1000 Sentences With "apparent magnitude" | Random Sentence Generator

In this specific photo, which was taken on September 2, the probe's apparent magnitude was around 25, about as bright in the night sky as Saturn's tiny, 4-kilometer wide moon Fenrir.

The asteroid came to opposition 175 degrees from the Sun on 17 May 2019 when it had an apparent magnitude of 27. Such a faint apparent magnitude would require a 10 hour image to detect with the largest 8-meter class telescopes in the world. Pan-STARRS is a 1.8-meter class telescope and with 30 second images has a limiting apparent magnitude of around 22. ATLAS has a limiting apparent magnitude closer to 19.

The primary member, component A, is a white-hued A-type main sequence star with an apparent magnitude of +5.02. Its companion, component B, has an apparent magnitude of +7.39.

Comet White–Ortiz–Bolelli in 1970 reached an apparent magnitude of 1. In December 2011, Kreutz sungrazer C/2011 W3 (Lovejoy) survived its perihelion passage and had an apparent magnitude of −3.

D Centauri (D Cen) is a double star in the constellation Centaurus. The system has a combined apparent magnitude of +5.31 and is approximately 570 light years from Earth. The system is classified as an orange K-type giant. The brighter component has an apparent magnitude of +5.31, while the apparent magnitude of the optical companion is +6.8.

Delta Tucanae A is a main sequence star of spectral type B9.5V and an apparent magnitude of 4.49. The companion has an apparent magnitude of 9.3. The Kappa Tucanae system shines with a combined apparent magnitude of 4.25, and is located around 68 light-years from the Solar System. The brighter component is a yellowish star, known as Kappa Tucanae A with an apparent magnitude of 5.33 and spectral type F6V, while the fainter lies 5 arcseconds to the northwest.

The asteroid did not become brighter than apparent magnitude 23 until 19 June when it was about 4 million km from Earth. The asteroid was detected by ATLAS when it was apparent magnitude 18.1.

It is approximately away from Earth. Its apparent magnitude is 6.3.

The apparent magnitude of the cluster is 6.7 and can be seen with 10x50 binoculars around a 7th magnitude star, which is not however member of the cluster. The brightest member of the cluster has apparent magnitude 9,3.

A fourth component C, 69.6 arcseconds away, has an apparent magnitude of 10.4.

By 3 January 2014 the asteroid was becoming dimmer than apparent magnitude 20.

Supernova SN 1986J was discovered on August 21, 1986 at apparent magnitude 14.

The primary component, σ Cassiopeiae A, is a B2 subgiant with an apparent magnitude of +5.0. Its companion, σ Cassiopeiae B, is a B5 main sequence dwarf with an apparent magnitude of +7.1. The two stars are three arcseconds apart.

Q Centauri (Q Cen) is a binary star in the constellation Centaurus. It has a combined apparent magnitude of +4.99 and is approximately 270 light years from Earth. The primary component, Q Centauri A, is a blue-white B-type main sequence dwarf with an apparent magnitude of +5.7. Its companion, Q Centauri B, is a white A-type main sequence dwarf with an apparent magnitude of +7.1.

Huya has a visual absolute magnitude (H) of 5.04 and a low geometric albedo of 0.083. Its apparent magnitude, the brightness as seen from Earth, varies from 19.8 to 21.6 magnitudes. Huya comes to opposition in June of each year at a visual apparent magnitude of 19.8. At wavelengths of the R-band range, Huya appears brighter in red light, with its R-band apparent magnitude reaching 19.11 magnitudes at opposition.

HD 185435 is a star in the constellation Cygnus. Its apparent magnitude is 6.42.

6 Aurigae is a star in the constellation Auriga. Its apparent magnitude is 6.48.

It is not visible to the naked eye with an apparent magnitude of 8.

NGC 5897 has a diameter of 12.6 arcminutes and an apparent magnitude of 8.5.

HD 110956 is a star in the constellation Crux. Its apparent magnitude is 4.61.

It has an apparent magnitude (V) of 9.55 and a spectral type of O8e C.

19 Camelopardalis (19 Cam) is a star in the constellation Camelopardalis. Its apparent magnitude is 6.17.

20 Camelopardalis (20 Cam) is a star in the constellation Camelopardalis. Its apparent magnitude is 7.45.

HD 77258 is a spectroscopic binary star in the constellation Vela. Its apparent magnitude is 4.47.

68 Cancri (68 Cnc) is a star in the constellation Cancer. Its apparent magnitude is 7.38.

Gliese 3634 has an apparent magnitude of 11.95. It cannot be seen with the naked eye.

80 Cancri (80 Cnc) is a star in the constellation Cancer. Its apparent magnitude is 6.87.

11 Leonis Minoris has a red dwarf companion of spectral type M5V and apparent magnitude 13.0. 20 Leonis Minoris is a multiple star system away from the Sun. The main star is another yellow star, this time a dwarf of spectral type G3Va and apparent magnitude 5.4.

Kepler-11 has an apparent magnitude of 14.2, and thus cannot be seen with the naked eye.

It is too faint to be see with the naked eye, having an apparent magnitude of 18.80.

It has an apparent magnitude of 16.2 and is located about 5 degrees northwest of Alpha Trianguli.

The data and models support a less than 0.05 apparent magnitude internal extinction of a galaxy's PNe.

Based on its spectrum, HD 154672 is not a very active star. The apparent magnitude (v) of HD 154672 is 8.22, which means that it is not visible to the naked eye. It is slightly dimmer than Neptune, which has an apparent magnitude of 7.78 at its brightest.

On average, metal-rich stars tend to be more likely to have planets and planetary systems. The star, as seen from Earth, has an apparent magnitude of 13.8. It is not visible with the naked eye. In comparison, Pluto's apparent magnitude at its brightest is slightly brighter, at 13.65.

Lambda1 is itself a binary star, with two components—a yellow-white star of spectral type F7IV-V and an apparent magnitude of 6.22, and a yellow main sequence star of spectral type G1V and an apparent magnitude of 7.28. The system is 186 light-years distant. Lambda2 is an orange subgiant of spectral type K2III that is expanding and cooling and has left the main sequence. Of apparent magnitude 5.46, it is approximately 220 light-years distant from Earth.

During the 2020 apparition the comet has brightened to about apparent magnitude 10.7 and should reach magnitude 9.

In 2134, Halley is expected to pass within of Earth. Its apparent magnitude is expected to be −2.0.

The star has an apparent magnitude of 12.9. It cannot be seen from Earth with the naked eye.

Vizier catalog entry Component C has reported type K2III-IV, apparent magnitude 9.65, and separation about 85". Vizier catalog entry Recent observations indicate the presence of additional smaller companions D (about 50" from A), E (about 8" from C), and F (about 40" from C) all around apparent magnitude 14.

HD 201298 is a K-type star in the constellation of Equuleus. It has an apparent magnitude of 6.14.

HD 50235 is a class K5III (orange giant) star located approximately 811 light years away, in the constellation Puppis. Its apparent magnitude is 4.99. HD 50235 made its closest approach to the Sun 7.8 million years ago, at the distance of 137 light years, during which it had an apparent magnitude of 1.13.

The fainter companion star is located at an angular separation of 98.3 arcseconds and has an apparent magnitude of 8.8.

9 Sagittarii (9 Sgr) is a massive binary star in the constellation Sagittarius. It has an apparent magnitude of 5.97.

The primary component, HR 2554 A, is a yellow G-type bright giant with a mean apparent magnitude of +4.4.

It is part of a triple association with NGC 1871 and NGC 1873. It has an apparent magnitude of 14.0.

Apep is located in the constellation of Norma, at a right ascension of and declination of , The system can be resolved into two components, the "central engine" Wolf–Rayet binary, and the "northern companion" supergiant. The total apparent magnitude of the system is 17.5, with the apparent magnitude of a resolved central engine and northern companion being 19.0 and 17.8 respectively. Its infrared spectral energy distribution (SED) is unique, with brightness ranging from an apparent magnitude of 6.4 at 2.2 µm to −2.4 at 22 µm. Surveys conducted with the European Southern Observatory (ESO)'s SINFONI instrument on the Very Large Telescope measured the apparent magnitude in the infrared J band for the central engine as , and for the northern companion as .

A low probability asteroid occultation of star UCAC2 17967364 with an apparent magnitude of +13.8 was possible on 11 February 2009. Another such event involving a star with an apparent magnitude of +12.9 occurred on 10 April 2014 at about 10:46 Universal Time, visible for observers in the southwest US and western Mexico.

HD 105382 (also known as V863 Centauri) is a star in the constellation Centaurus. Its apparent magnitude is 4.47. From parallax measurements, it is located 130 parsecs (440 light years) from the sun. HD 105382 is a variable star whose apparent magnitude varies with an amplitude of 0.012 over a period of 1.295 days.

Image mosaic by , 1974 Mercury's apparent magnitude is calculated to vary between −2.48 (brighter than Sirius) around superior conjunction and +7.25 (below the limit of naked-eye visibility) around inferior conjunction. The mean apparent magnitude is 0.23 while the standard deviation of 1.78 is the largest of any planet. The mean apparent magnitude at superior conjunction is −1.89 while that at inferior conjunction is +5.93. Observation of Mercury is complicated by its proximity to the Sun, as it is lost in the Sun's glare for much of the time.

Until 18 January 2015 18:00 UT the small dim asteroid either had an elongation less than 45 degrees from the Sun or was significantly fainter than apparent magnitude 23. On 18 January 2015 13:36 UT the asteroid passed from the Moon and at 17:09 UT passed from Earth. The asteroid was not discovered until 9 days later on 27 January 2015 by Pan- STARRS at an apparent magnitude of 21 using a Ritchey–Chrétien telescope. Two precovery images from 19 January 2015 when the asteroid was apparent magnitude 16 were then located.

Lying halfway between Beta and Gamma, Epsilon Trianguli Australis is an optical double. The brighter star, Epsilon Trianguli Australis A, is an orange K-type sub-giant of spectral type K1.5III with an apparent magnitude of +4.11. The optical companion, Epsilon Trianguli Australis B (or HD 138510), is a white main sequence star of spectral type A9IV/V which has an apparent magnitude of +9.32. Zeta Trianguli Australis appears as a star of apparent magnitude +4.91 and spectral class F9V, but is actually a spectroscopic binary with a near companion, probably a red dwarf.

SN 1895B was a supernova in the galaxy NGC 5253. It reached a maximum brightness of apparent magnitude 8.0 before fading.

This one had an apparent magnitude of 12.2 and was located 33 arcseconds north and 44 arcseconds west of its nucleus.

HD 153950 cannot be seen from Earth with the naked eye because the star has an apparent magnitude (V) of 7.39.

The apparent magnitude of Kepler-22 is 11.5, which means it is too dim to be seen with the naked eye.

V1668 Cygni was a nova that appeared in the constellation Cygnus in 1978 with a maximum brightness of 6th apparent magnitude.

It is apparent magnitude 14.5 and has a redshift of 0.012029. This galaxy is located about 48 megaparsecs from the Earth.

NGC 6167 is an open cluster in the constellation of Norma, viewed from Earth it has an apparent magnitude of 6.7.

Zeta Coronae Australis is a rapidly rotating main sequence star with an apparent magnitude of 4.8, 221.7 light years from Earth. The star has blurred lines in its hydrogen spectrum due to its rotation. Its spectral type is B9V. Theta Coronae Australis lies further to the west, a yellow giant of spectral type G8III and apparent magnitude 4.62.

HD 117440, also known by its Bayer designation d Centauri (d Cen), is a binary star in the constellation Centaurus. It is approximately 900 light years from Earth. Both components are yellow G-type giant stars. The primary, d Centauri A, has an apparent magnitude of +4.5, while the secondary, d Centauri B, has an apparent magnitude of +4.7.

The constellations Phoenix, Grus, Pavo and Tucana, are known as the Southern Birds. The brightest star, Alpha Phoenicis, is named Ankaa, an Arabic word meaning 'the Phoenix'. It is an orange giant of apparent magnitude 2.4. Next is Beta Phoenicis, actually a binary system composed of two yellow giants with a combined apparent magnitude of 3.3.

The brighter component, Nu Scorpii Aa, has a spectral type of B3V implying a B-type main sequence star. The fainter component, Nu Scorpii Ab, is thought to have an apparent magnitude of 6.90. Nu Scorpii Ac is the third component of the Nu Scorpii A subsystem. 63 milliarcseconds away, it has an apparent magnitude of 6.62.

It has a similar radius as the Sun and slightly more mass. Two reported additional components, C (apparent magnitude 12.93) and D (apparent magnitude 6.94), are believed to be optical doubles rather than part of the Mu Cygni system. Component D is the more distant spectroscopic binary HD 206874 (HIP 107326), consisting of two early F-type subgiants.

In mid March 2021 the comet is expected to come to opposition in the constellation of Crater at around apparent magnitude 20.9.

45 Aquarii is a star in the zodiac constellation of Aquarius. 45 Aquarii is its Flamsteed designation. Its apparent magnitude is 5.96.

NGC 119 is a lenticuluar galaxy of type E/SA0? pec with an apparent magnitude of 13.0 located in the constellation Phoenix.

170P/Christensen is a periodic comet in the Solar System. It came to perihelion in September 2014 at about apparent magnitude 18.

HD 96660 is an orange giant star located approximately 560 light years away, in the constellation Centaurus. Its apparent magnitude is 6.44.

HD 97413 is a white main-sequence star located 293 light years away, in the constellation Centaurus. Its apparent magnitude is 6.27.

HD 98176 is a white main-sequence star approximately 343 light years away, in the constellation Centaurus. Its apparent magnitude is 6.46.

HD 63399 is an orange giant star located approximately 445 light years away, in the constellation Puppis. Its apparent magnitude is 6.46.

It last came to perihelion in April 2015, and was expected to reach about apparent magnitude 16.7 near opposition in September 2015.

The primary is given the type F8-G0III giant and the secondary is a type A7m dwarf. Their combined apparent magnitude is +3.52.

75 Aquarii (abbreviated 75 Aqr) is a star in the constellation Aquarius. 75 Aquarii is its Flamsteed designation. Its apparent magnitude is 6.86.

This is a list of titleholders of being the dimmest (apparent magnitude) red dwarf as seen from Earth, and its succession over time.

Venus as seen from Mars (when near the maximum elongation from the Sun of 31.7°) would have an apparent magnitude of about −3.2.

NGC 118 is a spiral galaxy of type S (rs)a? pec with an apparent magnitude of 13.6 located in the constellation Cetus.

V Crucis is a carbon star in the constellation Crux. A Mira variable, its apparent magnitude ranges from 8.7 to 11.1 over ays.

Asteroid 65 Cybele and two stars, with their magnitudes labeled 'Apparent magnitude (') is a measure of the brightness of a star or other astronomical object observed from Earth. An object's apparent magnitude depends on its intrinsic luminosity, its distance from Earth, and any extinction of the object's light caused by interstellar dust along the line of sight to the observer. The word magnitude in astronomy, unless stated otherwise, usually refers to a celestial object’s apparent magnitude. The magnitude scale dates back to the ancient astronomer Ptolemy, whose star catalog listed stars from 1st magnitude (brightest) to 6th magnitude (dimmest).

While apparent magnitude is a measure of the brightness of an object as seen by a particular observer, absolute magnitude is a measure of the intrinsic brightness of an object. Flux decreases with distance according to an inverse-square law, so the apparent magnitude of a star depends on both its absolute brightness and its distance (and any extinction). For example, a star at one distance will have the same apparent magnitude as a star four times brighter at twice that distance. In contrast, the intrinsic brightness of an astronomical object, does not depend on the distance of the observer or any extinction.

Psi1 Piscium (Psi1 Psc, ψ1 Piscium, ψ1 Psc) is binary star in constellation of Pisces. It is approximately 280 light years from Earth, based on its parallax. The two components of Psi1 Piscium are both A-type main-sequence stars. The primary has an apparent magnitude of 5.273, while the secondary is slightly dimmer, with an apparent magnitude of 5.455.

One nox (nx) equals 1 millilux (1 mlx). In astronomy, apparent magnitude is a measure of the illuminance of a star on the Earth's atmosphere. A star with apparent magnitude 0 is 2.54 microlux outside the earth's atmosphere, and 82% of that (2.08 microlux) under clear skies. A magnitude 6 star (just barely visible under good conditions) would be 8.3 nanolux.

Nu Scorpii CD is also a triple star system. The primary component of the system, Nu Scorpii C, is a late B-type giant with a spectral type of B9III. With an apparent magnitude of 6.90, it outshines its fainter companion, Nu Scorpii D, which only has an apparent magnitude of 7.39. The two are separated by about 2 arcseconds.

65 Aquarii (abbreviated 65 Aqr) is a star in the constellation of Aquarius. 65 Aquarii is its Flamsteed designation. Its apparent magnitude is 7.04.

72 Aquarii (abbreviated 72 Aqr) is a star in the constellation of Aquarius. 72 Aquarii is the Flamsteed designation. Its apparent magnitude is 7.00.

85 Aquarii (abbreviated 85 Aqr) is a star in the constellation of Aquarius. 85 Aquarii is its Flamsteed designation. Its apparent magnitude is 6.69.

87 Aquarii (abbreviated 87 Aqr) is a star in the constellation of Aquarius. 87 Aquarii is the Flamsteed designation. Its apparent magnitude is 7.37.

84 Aquarii (abbreviated 84 Aqr) is a star in the constellation of Aquarius. 84 Aquarii is its Flamsteed designation. Its apparent magnitude is 7.08.

23 Arietis (abbreviated 23 Ari) is a star in the constellation of Aries. 23 Arietis is the Flamsteed designation. Its apparent magnitude is 6.83.

50 Arietis (abbreviated 50 Ari) is a star in the constellation of Aries. 50 Arietis is the Flamsteed designation. Its apparent magnitude is 6.80.

The star's apparent magnitude, or how bright it appears from Earth's perspective, is 4.09. Therefore, Upsilon Andromedae can be seen with the naked eye.

3C 273 lies at the center of a giant elliptical galaxy with an apparent magnitude of 16 and an apparent size of 30 arc seconds.

Although closer to the Sun than the dwarf planet Eris, Gonggong appears dimmer, as Eris has a higher albedo and an apparent magnitude of 18.8.

160P/LINEAR is a periodic comet in the Solar System. The comet came to perihelion on 18 September 2012, and reached about apparent magnitude 17.

V381 Cephei (HR 8164) is a triple star system in the northern constellation of Cepheus. Its apparent magnitude is slightly variable between 5.5 and 5.7.

37 Aquarii (abbreviated 37 Aqr) is a star in the equatorial constellation of Aquarius. 37 Aquarii is its Flamsteed designation. Its apparent magnitude is 6.64.

41 Ursae Majoris is a red giant star in the constellation Ursa Major. It is 690 light years from Earth. The apparent magnitude is 6.34.

On July 2, 2016 a type 1a supernova designated as SN 2016cyt was discovered in NGC 7033. It had a maximum apparent magnitude of 18.0.

Its apparent magnitude has been recently recalibrated at 4.6767 yielding an absolute magnitude of -1.56, almost as bright as its neighbor Alpha Ceti at -1.62.

The azimuthal equatorial velocity may be . It is a suspected Gamma Cassiopeiae type (GCAS) variable star, with its apparent magnitude varying from 2.62m to 2.66m.

HD 36041 is giant star in the northern constellation Auriga. It has an apparent magnitude of 6.37, making it faintly visible to the naked eye.

Eta Persei A belongs to spectral class K3 and has an apparent magnitude of +3.76. It radiates with 35,000 times the luminosity of the Sun.

152P/Helin–Lawrence is a periodic comet in the Solar System. The comet came to perihelion on 9 July 2012, and reached about apparent magnitude 17.

The star is at an apparent magnitude of 9 and is visible through binoculars or a telescope in the constellation of Pictor, in the southern sky.

The star's apparent magnitude, or how bright it appears from Earth's perspective, is 18.8. Therefore, it is too dim to be seen with the naked eye.

The NGC 1528 is clearly visible with 10x50 binoculars. 165 stars are recognised as members of NGC 1528, the brightest of which has apparent magnitude 8.7.

It appears in Pegasus, near Alpha Pegasi (Markab). It has been known to occasionally outburst, brightening to a peak apparent magnitude of 13.4 in June 2014.

68 Aquilae (abbreviated 68 Aql) is a double star in the equatorial constellation of Aquila. 68 Aquilae is its Flamsteed designation. Its apparent magnitude is 6.12.

The star's apparent magnitude, or how bright it appears from Earth's perspective, is 15. Therefore, it is too dim to be seen with the naked eye.

A possible third component with an apparent magnitude of +9.5, detected by studying the star during occultation, is located 0.052 arcseconds away from the A component.

The star's apparent magnitude, or how bright it appears from Earth's perspective, is 13.426. Therefore, it is too dim to be seen with the naked eye.

The star's apparent magnitude, or how bright it appears from Earth's perspective, is 14.976. Therefore, it is too dim to be seen with the naked eye.

The star's apparent magnitude, or how bright it appears from Earth's perspective, is 13.75. Therefore, it is too dim to be seen with the naked eye.

WASP-36 is a yellow main sequence star of spectral class G2, similar to the Sun. It has an unconfirmed stellar companion with apparent magnitude 14.03.

The star's apparent magnitude, or how bright it appears from Earth's perspective, is 15.474. Therefore, it is too dim to be seen with the naked eye.

The apparent magnitude of the star, or how bright it appears from Earth, is around 5. Therefore, it is only just visible to the unaided eye.

The binary system's apparent magnitude, or how bright it appears from Earth's perspective, is 24. It is far too dim to be seen with the naked eye.

Apparent magnitude is a logarithmic measure of apparent brightness. The distance determined by luminosity measures can be somewhat ambiguous, and is thus sometimes called the luminosity distance.

44 Cancri (44 Cnc) is an orange-to-red star located in the constellation Cancer. It has an apparent magnitude of 8.04 and its radius is about .

TU Muscae, also known as HD100213, is an eclipsing binary star in the constellation Musca. Its apparent magnitude ranges from 8.17 to 8.75 over around 1.4 days.

HD 220466 is a F-type subgiant or main sequence star in the constellation Aquarius. It has apparent magnitude 6.47 and is about 200 light-years away. In 1913, an apparent visual companion of apparent magnitude 10.3 was observed 1.9 arcseconds away from the star,CCDM 23241-2146, database entry, Catalog of Components of Double and Multiple Stars, CDS ID I/211. Accessed on line July 22, 2008.

Both components are blue-white B-type main-sequence stars. The brighter member, component A, has an apparent magnitude of +5.5, while its companion, component B, has an apparent magnitude of +5.8. The two stars are separated by 0.6 arcseconds and complete one orbit around their common centre of mass about once every 250 years. The primary displays an infrared excess, possibly due to a debris disk or other orbiting material.

Its brightest stars have an apparent magnitude of around 8. There are 84 member stars with an apparent magnitude brighter than 12. NGC 6067 is located in the Norma Star Cloud in the Norma Arm of the Milky Way and is 15 to 20 times as rich as the Pleiades and about the same age. It is thought to be around 102 million years old, and contain 893 solar masses.

HD 82886 is an evolved giant star in the constellation Leo Minor. With an apparent magnitude 7.63, it is too faint to be seen with the unaided eye.

V419 Cephei (BD+59°2342 or HIP 104719) is an irregular variable star in the constellation of Cepheus with an apparent magnitude that varies between 6.54 and 6.89.

The regolith is highly porous and has a radar-estimated density of only . Escape velocity from Deimos is 5.6 m/s. The apparent magnitude of Deimos is 12.45.

Binoculars or a small telescope will identify this cluster as non-stellar, while larger telescopes will resolve individual stars, of which the brightest are of apparent magnitude 13.1.

Gaia16cfr was a supernova imposter that occurred in NGC 2442 on 1 December 2016. It reached a Gaia apparent magnitude of 19.3 and absolute magnitude of about −12.

HR 3830 is an orange giant star, type K0III, in the southern hemisphere constellation of Antlia. It is 311 light years from Earth. Its apparent magnitude is 5.68.

On April 13, 2009, SN 2009dd was discovered in NGC 4088. At apparent magnitude 13.8, it became the third-brightest supernova of 2009. In 1991 there was SN1991G.

HD 79940 is a star in the constellation Vela. Its apparent magnitude is 4.64. It has a projected rotational velocity of and an effective temperature of 6,397 K.

With an apparent magnitude of 12.4, WASP-43 cannot be seen with the unaided eye. The star is located approximately 80 parsecs (260 light years) away from Earth.

The apparent magnitude of the star, or how bright it appears from Earth, is around 5. Therefore, it is just visible to the unaided eye to most observers.

Orbital diagram: close approach of on 5 March 2014 came to opposition (furthest elongation in the sky from the Sun) on 15 February 2014, but the asteroid had a very faint apparent magnitude of about 23 and was only 10 degrees from the full moon. The asteroid was discovered on 28 February 2014 by Pan-STARRS at an apparent magnitude of 20 using a Ritchey–Chrétien telescope. On 5 March 2014 at 21:00 UT the asteroid passed from Earth and reached about apparent magnitude 15. At 22:22 UT it passed from the Moon. By 6 March 2014 18:00 UT, the asteroid was less than 30 degrees from the Sun and dimming significantly.

HD 165634 is a class G7III (yellow giant) star in the constellation Sagittarius. Its apparent magnitude is 4.56 and it is approximately 339 light years away based on parallax.

HD 189831 is a class K5III (orange giant) star in the constellation Sagittarius. Its apparent magnitude is 4.77 and it is approximately 366 light years away based on parallax.

HD 34989 is a blue-white star in the main sequence, of apparent magnitude 5.80, in the constellation of Orion. It is 1700 light-years from the solar system.

HD 18970 is a class G9.5III (yellow giant) star in the constellation Perseus. Its apparent magnitude is 4.77 and it is approximately 211 light years away based on parallax.

HD 59890 is a class G3Ib (yellow supergiant) star in the constellation Puppis. Its apparent magnitude is 4.65 and it is approximately 1500 light years away based on parallax.

HD 63744 is a class K0III (orange giant) star in the constellation Puppis. Its apparent magnitude is 4.71 and it is approximately 232 light years away based on parallax.

HD 53811 is a class A4IV (white subgiant) star in the constellation Puppis. Its apparent magnitude is 4.92 and it is approximately 198 light years away based on parallax.

HD 51799 is a class M1III (red giant) star in the constellation Puppis. Its apparent magnitude is 4.95 and it is approximately 860 light years away based on parallax.

Its mass is about , with a surface temperature of 125,000 ± 5,000 K. Currently it is 200 times more luminous than the Sun, but its apparent magnitude is only +15.75.

HD 44131 is a class M1III (red giant) star in the constellation Orion. Its apparent magnitude is 4.91 and it is approximately 465 light years away based on parallax.

23 July 2015. The star's apparent magnitude, or how bright it appears from Earth's perspective, is 13.426; therefore, it is too dim to be seen with the naked eye.

With an apparent magnitude of 11.7, the star cannot be seen by the naked eye, but is visible with a telescope in a dark sky with little light pollution.

NGC 62 is a spiral galaxy in the constellation Cetus. It is located at RA 00h 17m 05.4s, dec −13° 29′ 15″, and has an apparent magnitude of 13.5.

NGC 63 is a spiral galaxy in the constellation Pisces. It is located at RA 00h 17m 45.5s, dec −11° 27′ 01″, and has an apparent magnitude of 12.63.

HD 15524 is a wide binary star in the northern zodiac constellation of Aries. Located approximately away, the primary, a yellow-white subgiant or main sequence star has an apparent magnitude of 5.97, meaning that it can be viewed with the naked eye under good conditions. The secondary, separated from the primary by 12.4 arcseconds, has an apparent magnitude of 10.4. This system is the likely source of X-ray emission coming from these coordinates.

C/2011 J2 (LINEAR) is an Oort cloud comet discovered on 4 May 2011 by LINEAR at an apparent magnitude of 19.7 using a Reflecting telescope. As of September 2014 the comet is around apparent magnitude 17. C/2011 J2 came to perihelion (closest approach to the Sun) on 25 December 2013 at a distance of 3.4 AU from the Sun. On 27 August 2014 an 18th magnitude fragment CK11J02b was detected.

Albireo A and B Beta Cygni is about away from the Sun. When viewed with the naked eye, Albireo appears to be a single star. However, in a telescope it resolves into a double star consisting of β Cygni A (amber, apparent magnitude 3.1), and β Cygni B (blue-green, apparent magnitude 5.1). Separated by 35 seconds of arc,Entry, The Washington Double Star Catalog, identifier 19307+2758, discoverer identifier STFA 43.

TU Corvi is a Delta Scuti variable—a class of short period (six hours at most) pulsating stars that have been used as standard candles and as subjects to study astroseismology. It varies by 0.025 of a magnitude around apparent magnitude 6.53 over 59 minutes. Three star systems have confirmed planets. HD 103774 is a young yellow-white main-sequence star of apparent magnitude 7.12 that is 181 ± 5 light-years distant from Earth.

Vizier catalog entry The primary, with an apparent magnitude of 4.69, is an F-type main-sequence star with a stellar classification of F6V. It has 35% more mass than the Sun and 188% of the Sun's radius. The star is spinning with a projected rotational velocity of 9.6 km/s. The secondary companion, with an apparent magnitude of 6.12, is a G-type main- sequence star with a class of G2V.

Epsilon Sculptoris (ε Scl, ε Sculptoris) is a binary star in the constellation Sculptor. It is approximately 91.7 light years from Earth. The primary component, Epsilon Sculptoris A, is a yellow-white F-type main-sequence star with an apparent magnitude of +5.29. Orbiting it with a separation of 4.6 arcseconds, or at least 125 Astronomical Units, is Epsilon Sculptoris B, a yellow G-type main sequence dwarf with an apparent magnitude of +8.6.

HD 167818 is a class K3II (orange bright giant) star in the constellation Sagittarius. Its apparent magnitude is 4.66 and it is approximately 760 light years away based on parallax.

HD 20468 is a class K2II (orange bright giant) star in the constellation Perseus. Its apparent magnitude is 4.82 and it is approximately 1180 light years away based on parallax.

HD 70060 is a class A8V (white main-sequence) star in the constellation Puppis. Its apparent magnitude is 4.45 and it is approximately 93.4 light years away based on parallax.

As of 2018, it is 63 AU from the Sun. It will make its closest approach to the Sun in 2093, when it will reach an apparent magnitude of 21.2.

HD 65810 is a class A2V (white main-sequence) star in the constellation Puppis. Its apparent magnitude is 4.61 and it is approximately 241 light years away based on parallax.

HD 64740 is a class B1.5V (blue main-sequence) star in the constellation Puppis. Its apparent magnitude is 4.63 and it is approximately 760 light years away based on parallax.

HD 61772 is a class K3II (orange bright giant) star in the constellation Puppis. Its apparent magnitude is 4.98 and it is approximately 700 light years away based on parallax.

HD 91312 (HR 4132, HIP 51658) is a star in the constellation Ursa Major. Its apparent magnitude is 4.73. It is the brightest star of Ursa Major without Flamsteed designation.

775 Lumière is a minor planet orbiting the Sun. The apparent magnitude is 10.40. The diameter is 33.58 kilometers. Its rotational period is 6.103 hours, and the albedo is .108.

In the early 1970s PAGEOS varied from 2nd apparent magnitude to beyond visibility over a period of a few minutes. In 2016, one of the largest fragments of PAGEOS de-orbited.

HD 61831 (d1 Puppis) is a class B2.5V (blue dwarf) star in the constellation Puppis. Its apparent magnitude is 4.84 and it is approximately 556 light years away based on parallax.

126 Tauri (126 Tau) is a blue subgiant star in the constellation Taurus. Its apparent magnitude is 4.83. It is also a binary star, with an orbital period of 111 years.

HD 29697 (Gliese 174, V834 Tauri) is a variable star of BY Draconis type in the constellation Taurus. It has an apparent magnitude around 8 and is approximately 43 ly away.

NGC 120 is a lenticular galaxy of type SB0? pec? with an apparent magnitude of 13.4 located in the constellation Cetus. It was discovered on 27 September 1880 by Wilhelm Tempel.

It has a class of B9.5V with an apparent magnitude of +6.58. As of 2010, the secondary had an angular separation of from the primary along a position angle of 76°.

Its luminosity () is 80% that of the Sun. The star's apparent magnitude, or how bright it appears from Earth's perspective, is 4.74. Therefore, it can be seen with the naked eye.

HD 102839 is a class G6Ib (yellow supergiant) star in the constellation Musca. Its apparent magnitude is 4.98 and it is approximately 950 light years away from Earth based on parallax.

9 Aquarii (abbreviated 9 Aqr) is a yellow giant with a spectral type of G8III and an apparent magnitude of 6.55 in the constellation Aquarius. 9 Aquarii is the Flamsteed designation.

This name was later connected by Allen with 46 Leonis Minoris—an error perpetuated by subsequent astronomers. The original "Praecipua", 37 Leonis Minoris, has an apparent magnitude of 4.69, but is a distant yellow supergiant of spectral type G2.5IIa and absolute magnitude of −1.84, around distant. Leo Minor as seen by the naked eye Beta Leonis Minoris is a binary star system. The primary is a giant star of spectral class G8 and apparent magnitude of 4.4.

The primary component, designated 48 Cassiopeiae A, is a white A-type main-sequence star with a stellar classification of A2 V and an apparent magnitude of +4.65. It has a companion, component B, which is an F-type main-sequence star of class F2 V and an apparent magnitude of +6.74. This pair orbit around their common centre of mass once every 61.1 years. They have a semimajor axis of 0.614 arcseconds and an eccentricity of 0.355.

Curious spiral around red giant star R Sculptoris. No stars brighter than 3rd magnitude are located in Sculptor. This is explained by the fact that Sculptor contains the south galactic pole where stellar density is very low. Overall, there are 56 stars within the constellation's borders brighter than or equal to apparent magnitude 6.5. The brightest star is Alpha Sculptoris, an SX Arietis-type variable star with a spectral type B7IIIp and an apparent magnitude of 4.3.

Mu Tucanae was dropped by Francis Baily, who felt the star was too faint to warrant a designation, and Kappa's two components came to be known as Kappa1 and Kappa2. The layout of the brighter stars of Tucana has been likened to a kite. Within the constellation's boundaries are around 80 stars brighter than an apparent magnitude of 7. At an apparent magnitude of 2.86, Alpha Tucanae is the brightest star in the constellation and marks the toucan's head.

Theta Coronae Borealis, Latinized from θ Coronae Borealis, is a binary star system in the constellation Corona Borealis. It shines with a combined apparent visual magnitude (V band) of 4.13. There are two components: Theta Coronae Borealis A is of apparent magnitude 4.16, while Theta Coronae Borealis B lies around 1 arcsecond distant and has an apparent magnitude of 6.29. The system is located around 375 light-years from Earth, as estimated from its parallax of 8.69 milliarcseconds.

The two components are yellow main sequence stars. The brighter component (designated Xi Ursae Majoris A), has a mean apparent magnitude of +4.41. The companion star (Xi Ursae Majoris B) has an apparent magnitude of +4.87. The orbital period of the two stars is 59.84 years, and they are currently separated by 1.2 arcseconds, or at least 10 AU. Orbit of Xi Ursae Majoris Each component of this double star is itself a single-lined spectroscopic binary.

W Coronae Borealis (W CrB) is a Mira-type long period variable star in the constellation Corona Borealis. Its apparent magnitude varies between 7.8 and 14.3 over a period of 238 days.

Both stars have a surface temperature of 8,000 kelvins. Theta Serpentis C is a yellow G-type star with an apparent magnitude of +6.71. It is separated by 7 arcminutes from θ².

HD 70555 (w Puppis) is a class K2.5II-III (orange giant) star in the constellation Puppis. Its apparent magnitude is 4.83 and it is approximately 1,010 light years away based on parallax.

M Carinae (M Car) is a star in the constellation Carina. It is a white A-type giant with an apparent magnitude of +5.154. It is approximately 308 light- years from Earth.

Its luminosity () is 8.7 times that of the Sun. The star's apparent magnitude, or how bright it appears from Earth's perspective, is 3. Therefore, it can be seen with the naked eye.

Eta Lyrae belongs to spectral class B2.5IV and has apparent magnitude of +4.40. It is a single-lined spectroscopic binary, with a very small radial velocity variation of . The orbital period is .

Pluto was easiest to find because it has the highest apparent magnitude of all known trans-Neptunian objects. It also has a lower inclination to the ecliptic than most other large TNOs.

56 Ursae Majoris (56 UMa) is a star in the constellation Ursa Major. Its apparent magnitude is 5.03. It is a single-lined spectroscopic binary with an orbital period of about 45 years.

HII regions are observed in the arms. The brightest stars of the galaxy have apparent magnitude around 22. Its nucleus is small and bright.Sandage, A., Bedke, J. (1994), The Carnegie Atlas of Galaxies.

NGC 957 (also known as Collinder 28) is a loosely bound open cluster located in the constellation Perseus. It has an apparent magnitude of 7.6 and an approximate size of 11 arc-minutes.

The undisturbed apparent magnitude is around 12.7, but the star is rarely at that level. The eclipses are believed to be caused by dust formed from expelled material, not by the companion star.

G Scorpii (abbreviated G Sco), also named Fuyue, is a giant star in the constellation of Scorpius. It has an apparent magnitude of +3.19. It is approximately 126 light-years from the Sun.

V357 Carinae (a Car, a Carinae) is an astrometric and spectroscopic binary in the constellation Carina. It is approximately 419 light years from Earth. The mean apparent magnitude of the system is +3.43.

NGC 1662 (also known as Collinder 55) is a loosely bound open cluster located in the constellation Orion. It has an apparent magnitude of 7.6 and an approximate size of 20 arc-minutes.

RS Persei is a red supergiant variable star located in the Double Cluster in Perseus. The star's apparent magnitude varies from 7.82 to 10.0, meaning it is never visible to the naked eye.

It is classified a blue-white B-type giant star and has an apparent magnitude of +4.35. (The individual components are classified as B6IV and B8.) The binary system has an orbital period of 14.1683 days. The binary's companion, Epsilon Volantis B, is 6.05 arcseconds away and has an apparent magnitude of +8.1. It too is a spectroscopic binary, consisting of two A-type main sequence stars with stellar classifications of A2 V and an orbital period of "a few days".

The comet last reached perihelion on 24 March 2013. For much of 2012, observation of Lemmon remained limited to CCD imagery, but steadily brightened throughout the course of the year. In late-November 2012, the comet became bright enough for telescopic viewing, and had an apparent magnitude estimated at +9 by the year's end. Brightening continued into the early months of 2013 before peaking at an apparent magnitude of +5 in late March, though viewing was mostly limited to the Southern Hemisphere.

Delta Apodis (δ Aps, δ Apodis) is the Bayer designation for a double star in the southern constellation of Apus. The brighter star, δ¹ Apodis, is a M-type red giant and has an apparent magnitude that varies from magnitude +4.66 to +4.87. It is classified as a semiregular variable with pulsations of multiple periods of 68.0, 94.9 and 101.7 days. At an angular separation of 102.9 arcseconds is δ² Apodis, an orange K-type giant with an apparent magnitude of +5.27.

It contains a Sun-like star and a white dwarf. Because of their close proximity and the larger mass of the white dwarf, the latter draws matter from the larger, less massive star. The influx of matter on the white dwarf's surface causes periodic thermonuclear explosions to occur. The usual apparent magnitude of this star system is 15.5, but there have been observed eruptions with maximal apparent magnitude of about 7.0 in the years 1890, 1902, 1920, 1944, 1966 and 2011.

As of 2007, the two stars had an angular separation of 1.206 arcseconds at a position angle of 35°. The components are main sequence stars of similar size and appearance. The primary component, β Muscae A, has an apparent magnitude of 3.51, a stellar classification of B2 V, and about 7.35 times the Sun's mass. The secondary component, β Muscae B, has an apparent magnitude of 4.01, a stellar classification of B3 V, and is about 6.40 times the mass of the Sun.

NGC 102 is a lenticular galaxy estimated to be about 330 million light-years away in the constellation of Cetus. It was discovered by Francis Leavenworth in 1886 and its apparent magnitude is 14.

NGC 105 is a spiral galaxy estimated to be about 240 million light-years away in the constellation of Pisces. It was discovered by Édouard Stephan in 1884 and its apparent magnitude is 14.1.

NGC 106 is a lenticular galaxy estimated to be about 270 million light-years away in the constellation of Pisces. It was discovered by Francis Leavenworth in 1886 and its apparent magnitude is 14.5.

NGC 83 is an elliptical galaxy estimated to be about 260 million light-years away in the constellation of Andromeda. It was discovered by John Herschel in 1828 and its apparent magnitude is 14.2.

NGC 96 is a lenticular galaxy estimated to be about 290 million light-years away in the constellation of Andromeda. It was discovered by Guillaume Bigourdan in 1884 and its apparent magnitude is 17.

NGC 97 is an elliptical galaxy estimated to be about 230 million light-years away in the constellation of Andromeda. It was discovered by John Herschel in 1828 and its apparent magnitude is 13.5.

Its luminosity () is 15% that of the Sun. The star's apparent magnitude, or how bright it appears from Earth's perspective, is 14.3. Therefore, it is too dim to be seen with the naked eye.

Its luminosity () is 11% that of the Sun. The star's apparent magnitude, or how bright it appears from Earth's perspective, is 14.76. Therefore, it is too dim to be seen with the naked eye.

It brightened to roughly apparent magnitude 19.3 around mid-March 2014. One radar Doppler observation of was made in 2014. The October–November 2015 Earth approach was studied by the Goldstone Deep Space Network.

Epsilon Equulei, Latinized from ε Equulei, is a star system of apparent magnitude +5.23 in the constellation of Equuleus. It is located 180 light years away from the Solar System, based on its parallax.

Its luminosity (L☉) is 0.05% of that of the Sun. The star's apparent magnitude, or how bright it appears from Earth's perspective, is 18.8, too dim to be seen with the naked eye.

Melotte 186 (also known as Collinder 359) is a large, loosely bound open cluster located in the constellation Ophiuchus. It has an apparent magnitude of 3.0 and an approximate size of 240 arc-minutes.

Its luminosity () is 21% that of the Sun. The star's apparent magnitude, or how bright it appears from Earth's perspective, is 13.65. Therefore, it is too dim to be seen with the naked eye.

NGC 79 is an elliptical galaxy estimated to be about 240 million light-years away in the constellation of Andromeda. Its apparent magnitude is 14.9. It was discovered on 14 November 1884 by Guillaume Bigourdan.

Phi Velorum (φ Vel, φ Velorum) is a star in the constellation Vela. It is a blue-white B-type supergiant with an apparent magnitude of +3.53. It is approximately 1,590 light years from Earth.

HD 72561 is a star in the constellation Hydra. Its apparent magnitude is 5.867. Based on parallax, it is located about 1,600 light-years (500 parsecs) away. HD 72561 is a G-type giant star.

HD 54893 is a class B2IV (blue subgiant) star in the constellation Puppis. Its apparent magnitude is 4.83 and it is approximately 730 light years away based on parallax. It is a Beta Cephei variable.

NGC 500 (also known as PGC 5013) is a type E-SO lenticular galaxy located in the Pisces constellation. It has an apparent size of .8 by .6 arcminutes and an apparent magnitude of 14.2.

HIP 57274 is a K-type main-sequence star in the constellation Ursa Major. It has an apparent magnitude of 8.96 and is both smaller and less luminous than the sun. Three planets orbit it.

NGC 4302 has hosted one supernova, a Type IIL supernova designated as SN 1986E. The supernova was discovered by G. Candeo at the Asiago Observatory on April 13, 1986 with an apparent magnitude of 14.5.

Tau1 Capricorni (τ1 Cap, τ1 Capricorni) is a star in the constellation Capricornus. τ1 Capricorni is an orange K-type giant with an apparent magnitude of +6.76. It is approximately 884 light years from Earth.

V533 Carinae (V533 Car, y Car, y Carinae) is a white A-type supergiant variable star with a mean apparent magnitude of +4.59 in the constellation Carina. It is over 10,000 light years from Earth.

HD 92036 is a single star in the equatorial constellation of Hydra. Its apparent magnitude is 4.87. This is an aging red giant star on the asymptotic giant branch with a stellar classification of M1III:Ba0.5.

During the perihelic oppositions of 2003–04, Chariklo had an apparent magnitude of +17.7. , Chariklo was 14.8 AU from the Sun. Chariklo orbits within 0.09 AU of the 4:3 mean-motion resonance with Uranus.

WASP-95 is a star in the constellation Grus. With an apparent magnitude of 10.1, it is not visible to the naked eye. Its spectral type of G2 means it is a yellow sunlike star.

One of the novae, M81 2007 3, grew very luminous, reaching the quite extraordinary absolute magnitude of −10 and apparent magnitude of 17.6 six days later. It was the brightest nova ever discovered in M81.

HD 5789 and HD 5788 is a pair of stars comprising a binary star system in the northern constellation of Andromeda. Located approximately away, the primary is a hot, massive blue star with an apparent magnitude of 6.06 while the secondary is slightly smaller and cooler, with an apparent magnitude of 6.76. Both stars are main-sequence stars, meaning that they are currently fusing hydrogen into helium in their cores. As of 2016, the pair had an angular separation of along a position angle of 195°.

Three supernovae have been observed in the Whirlpool Galaxy: In 1994, SN 1994I was observed in the Whirlpool Galaxy. It was classified as type Ic, indicating that its progenitor star was very massive and had already shed much of its mass, and its brightness peaked at apparent magnitude 12.91. In June 2005 the type II supernova SN 2005cs was observed in the Whirlpool Galaxy, peaking at apparent magnitude 14. On 31 May 2011 a type II supernova was detected in the Whirlpool Galaxy, peaking at magnitude 12.1.

C/2013 V5 (Oukaimeden) is a retrograde Oort cloud comet discovered on 12 November 2013 by Oukaimeden Observatory at an apparent magnitude of 19.4 using a reflecting telescope. From 5 May 2014 until 18 July 2014 it had an elongation less than 30 degrees from the Sun. By late August 2014 it had brighten to apparent magnitude 8 making it a small telescope and high-end binoculars target for experienced observers. It crossed the celestial equator on 30 August 2014 becoming a southern hemisphere object.

The brighter component, ζ Aquarii A (also called ζ2 Aquarii), is a yellow-white-hued F-type main sequence star with an apparent magnitude of +4.42. Its companion, ζ Aquarii B (also called ζ1 Aquarii), is a yellow-white-hued F-type subgiant with an apparent magnitude of +4.51. The fact that their brightness is so similar makes the pair easy to measure and resolve. Zeta Aquarii A is known to be an astrometric binary system, as it undergoes regular perturbations from its orbit.

It ranges in apparent magnitude from 1.59 to 1.64. The spectral types for O and early B stars were defined more rigorously in 1971 and Bellatrix was used as a standard for the B2 III type. The expected brightness of Bellatrix from this spectral type is about one magnitude brighter than calculated from its apparent magnitude and Hipparcos distance. Analysis of the observed characteristics of the star indicate that it should be a B2 main sequence star, not the giant that it appears from its spectral type.

The comet came to perihelion on 1 October 2012, and was expected to reach about apparent magnitude 15.2, but due to an outburst the comet reached apparent magnitude 8. As a result of the outburst of gas and dust, the comet was briefly more than 500 times brighter than it would have been without the outburst. On 19 October 2012, images by the Virtual Telescope Project showed a dust cloud trailing the nucleus. Images by the Faulkes Telescope North on 26 October 2012 confirm a fragmentation event.

Its companion, almost 3 arcminutes away, is a 13th-magnitude star which may or may not be in orbit around Beta. The remaining member of the triangle is Gamma Trianguli Australis with an apparent magnitude of 2.87. It is an A-type main sequence star of spectral class A1 V, which lies away. Located outside the triangle near Beta, Delta Trianguli Australis is the fourth-brightest star at apparent magnitude +3.8. It is a yellow giant of spectral type G2Ib-II and lies away.

Thuban , designation Alpha Draconis (α Draconis, abbreviated Alpha Dra, α Dra), is a star (or star system) in the constellation of Draco. A relatively inconspicuous star in the night sky of the Northern Hemisphere, it is historically significant as having been the north pole star from the 4th to 2nd millennium BCE. Even though Johann Bayer gave Thuban the designation Alpha, its apparent magnitude of 3.65 means it is 3.7 times fainter than the brightest star in the constellation, Gamma Draconis (Eltanin), whose apparent magnitude is 2.24.

57 Cancri is a double star in the zodiac constellation of Cancer, located around 460 light years away from the Sun. They are visible to the naked eye as a faint star with a combined apparent visual magnitude of +5.40. The brighter member, designated component A. is a yellow-hued giant star with a stellar classification of G7 III and an apparent magnitude of +6.09. Its companion, component B, is an orange-hued giant with a class of K0 III and an apparent magnitude of +6.37.

On 1 September 2014 the asteroid passed about from Earth, but at that time the asteroid had an apparent magnitude of 25 and was roughly 25 degrees from the Sun. It was discovered on 11 December 2014 by the Mount Lemmon Survey at an apparent magnitude of 20 using a reflecting telescope. The asteroid has an observation arc of 35 days with an uncertainty parameter of 6. The asteroid was last observed on 15 January 2015, and is still being actively observed to better constrain the orbit.

NGC 86 is a lenticular galaxy estimated to be between 275 and 300 million light-years away in the constellation of Andromeda. It was discovered by Guillaume Bigourdan in 1884 and its apparent magnitude is 14.9.

HD 110458 (Bayer designation w Cen / w Centauri) is a star in the constellation Centaurus. It is an orange K-type giant with an apparent magnitude of +4.66 and is approximately 191 light years from Earth.

78 Aquarii (abbreviated 78 Aqr) is a star in the constellation of Aquarius. 78 Aquarii is its Flamsteed designation. It is a k3iii giant star, indicating an orange to red color. Its apparent magnitude is 6.20.

N Scorpii (N Sco) is a blue giant star in the constellation Scorpius. Its apparent magnitude is 4.23. It was initially given the Bayer designation Alpha Normae by Lacaille but later moved from Norma to Scorpius.

However the planet orbits at a distance of 2.7 AU, which prediction says is too close for disk instability to occur. The low apparent magnitude, of MK = 14.3 ± 0.1, suggests that it formed via core accretion.

RW Cygni is a semiregular variable star in the constellation Cygnus, about a degree east of 2nd magnitude γ Cygni. Its apparent magnitude varies between 8.05 and 9.70 and its spectral type between M3 and M4.

HD 89307 is a yellow main-sequence star located approximately 108 light-years away in the constellation of Leo. The apparent magnitude is 7.06. The mass of the star is identical in value to the Sun.

NGC 166 (also known as PGC 2143) is a spiral galaxy located around 2.6 million light-years away in the constellation Cetus, with an apparent magnitude of 15.18. It was discovered by Francis Preserved Leavenworth in 1886.

R Leonis Minoris (R LMi) is a Mira variable type star in the constellation Leo Minor. It ranges between apparent magnitude 6.3 and 13.2, and spectral types M6.5e to M9.0e (Tc:), over a period of 372 days.

The comet made a return appearance in 1992, when it was rediscovered by Japanese astronomer Tsuruhiko Kiuchi and became visible with binoculars. In 2126 it will be a bright naked- eye comet reaching about apparent magnitude 0.7.

OGLE-TR-111 is a yellow dwarf star approximately 5,000 light-years away in the constellation of Carina (the Keel). Having an apparent magnitude of about 17, this distant and dim star has not yet been cataloged.

AS 314, also known as V452 Scuti, is a white hypergiant star and luminous blue variable candidate located in the constellation of Scutum. It has an apparent magnitude of 9.85 and can be seen with small telescopes.

V382 Carinae, also known as x Carinae (x Car), is a yellow hypergiant in the constellation Carina. It is a G-type star with a mean apparent magnitude of +3.93, and a variable star of low amplitude.

690 Wratislavia is a minor planet orbiting the Sun. Wratislavia was discovered on October 16, 1909. IRAS data shows it is about 135 km in diameter. Asteroid 690 Wratislavia (apparent magnitude 12.9) near the galaxy NGC 6941.

This is a double-lined spectroscopic binary star system. The spectrum matches a B-type main-sequence star with a stellar classification of B2.5 V. There is a faint visual companion with an apparent magnitude of 12.49.

Below is a list of stars arranged in order of decreasing luminosity (increasing bolometric magnitude). Accurate measurement of stellar luminosities is quite difficult in practice, even when the apparent magnitude is measured accurately, for four reasons: #The distance d to the star must be known, to convert apparent to absolute magnitude. Absolute magnitude is the apparent magnitude a star would have if it were 10 parsecs away from the viewer. Since apparent brightness decreases as the square of the distance (i.e. as 1/d2), a small error (e.g.

HD 2767 is the primary component of a double star located away in the constellation Andromeda. It is a red giant with a spectral type of K1III and an apparent magnitude of 5.88, thus is visible by the naked eye under favourable conditions. The secondary is named BD+32 81, has an apparent magnitude of 9.28, and is an F-type star; it shares radial velocity, parallax and proper motion with the primary component. The distance from the primary is estimated as 6,536 AU, while their separation in the sky is 56 arcseconds.

He numbered 89 stars (now with Flamsteed designations), though 6 and 11 turned out to be stars in Aquarius. Within the constellation's borders there are 177 stars of apparent magnitude 6.5 or greater. Epsilon Pegasi, also known as Enif, marks the horse's muzzle. The brightest star in Pegasus, is an orange supergiant of spectral type K21b that is around 12 times as massive as the Sun and is around 690 light-years distant from Earth. It is an irregular variable, its apparent magnitude varying between 2.37 and 2.45.

To apply this method, one must measure the apparent magnitude of the star and know the spectral type of the star. The spectral type can be determined by observing the star's spectrum. If the star lies on the main sequence, as determined by its luminosity class, the spectral type of the star provides a good estimate of the star's absolute magnitude. Knowing the apparent magnitude (m) and absolute magnitude (M) of the star, one can calculate the distance (d, in parsecs) of the star using m - M = 5 \log (d/10) (see distance modulus).

The brighter star, ι Cancri A, is a yellow G-type giant with an apparent magnitude of +4.02. It is a mild barium star, thought to be formed by mass transfer of enriched material from an asymptotic giant branch star onto a less evolved companion. No such donor has been detected in the ι Cancri system, but it is assumed that there is an unseen white dwarf. The fainter of the two stars, ι Cancri B, is a white A-type main sequence dwarf with an apparent magnitude of +6.57.

Both visible components are white-hued A-type main-sequence stars. The primary, component A, sometimes called ο1 Capricorni, has an apparent magnitude of +5.94, while the companion, component B or ο2 Capricorni, has an apparent magnitude of +6.74. The two stars are currently separated by 21.91 arcseconds − corresponding to a projected separation of around 2,100 AU. At the estimated age of around 118 million years old, both components are spinning rapidly: component A has a projected rotational velocity of 276 km/s, while component B is 136 km/s.

Photometric measurements are made in the ultraviolet, visible, or infrared wavelength bands using standard passband filters belonging to photometric systems such as the UBV system or the Strömgren uvbyβ system. Absolute magnitude is a measure of the intrinsic luminosity of a celestial object rather than its apparent brightness and is expressed on the same reverse logarithmic scale. Absolute magnitude is defined as the apparent magnitude that a star or object would have if it were observed from a distance of . When referring to just "magnitude", apparent magnitude rather than absolute magnitude is normally intended.

Polaris, the brightest star in the constellation, is a yellow-white supergiant and the brightest Cepheid variable star in the night sky, ranging from an apparent magnitude of 1.97 to 2.00. Beta Ursae Minoris, also known as Kochab, is an aging star that has swollen and cooled to become an orange giant with an apparent magnitude of 2.08, only slightly fainter than Polaris. Kochab and magnitude 3 Gamma Ursae Minoris have been called the "guardians of the pole star". Planets have been detected orbiting four of the stars, including Kochab.

Pleiades and Hyades with κ Tauri as the very close pair at lower centre (north is approximately to the left) The system is dominated by a visual double star, κ1 Tauri and κ2 Tauri. κ1 Tauri is a white A-type subgiant with an apparent magnitude of +4.22. It is emitting an excess of infrared radiation at a temperature indicating there is a circumstellar disk in orbit at a radius of 67 AU from the star. κ2 Tauri is a white A-type main sequence star with an apparent magnitude of +5.24.

HD 1185 is a double star in the northern constellation of Andromeda. The primary, with an apparent magnitude of 6.15, is a white main-sequence star of spectral type A1Si, indicating it has stronger silicon absorption lines than usual, thus making it also an Ap star. The secondary companion, which is 9.08 arcseconds away, is not visible to the naked eye at an apparent magnitude of 9.76, and is also an A-type star. It shares common proper motion and parallax with the primary star but orbital parameters are still unknown.

HD 2942 is a triple star system in the constellation Andromeda located approximately away. The primary component, a red giant of spectral type K0III, has an apparent magnitude of 6.33, meaning that it is barely visible with the naked eye under good conditions. The secondary component is much fainter, with an apparent magnitude 11.26, and is located 8.6 arcseconds away. It is a double-lined spectroscopic binary, where two very similar G-type main sequence stars of spectral types G6V and G8V orbit around their common center of mass in 7.489 days.

It orbits every 919 days inclined at 50°, and is 1.76 AU from the host star. The host star, HD 128311, is a K0V-type star located 16.6 parsecs from Earth. It is smaller than the Sun, with a mass of and a radius of ; it also appears below the threshold of naked-eye visibility at an apparent magnitude of 7.51. There are several single-planet systems in Boötes. HD 132406 is a Sun-like star of spectral type G0V with an apparent magnitude of 8.45, 231.5 light-years from Earth.

Epsilon Phoenicis is a star in the constellation Phoenix. Its apparent magnitude is 3.87. Located around distant, it is an orange giant of spectral type K0III, a star that has used up its core hydrogen and has expanded.

HD 103774 is a young yellow-white main-sequence star of apparent magnitude 7.12 that is 181 ± 5 light-years distant from Earth. It is 1.335 ± 0.03 times as massive and 3.5 ± 0.3 as luminous as the Sun.

Both stars are F-type main sequence stars. The first component has an apparent magnitude of 6.20; the second is magnitude 6.34. They are orbiting each other with a period of 21.84 years with an eccentricity of 0.388.

HD 85951, also designated HR 3923 and formally named Felis , is a star in the constellation of Hydra. Its apparent magnitude is 4.95. Based on parallax measurements it is about 530 light-years (162 parsecs) from the Sun.

TT Cygni is a carbon star. It is away in Cygnus. It has an apparent magnitude of 7.44. It is called a carbon star because it has a high ratio of carbon to oxygen in its surface layers.

NGC 654 is an open cluster in the constellation Cassiopeia. It was discovered by William Herschel in 1787. With apparent magnitude 6.5, it can be observed by binoculars. It is located 2,5° northeast of the star Delta Cassiopeiae.

The luminosity varies slightly from magnitude +2.01 to +2.10. Based upon parallax measurements, it is roughly from the Sun. Its apparent magnitude is reduced by 0.06 by extinction due to gas and dust along the line of sight.

NGC 3005 is an edge-on spiral galaxy in the constellation of Ursa Major, discovered by Bindon Stoney on January 25th, 1851. It has an apparent magnitude of 16.00, at a distance of 141 Kpc from the sun.

NGC 1934 (also known as ESO 56-SC109) is an emission nebula located in the Dorado constellation and part of the Large Magellanic Cloud. It was discovered by John Herschel on November 23 1834. Its apparent magnitude is 10.50.

The most favorable apparition of 10P/Tempel 2 was in 1925 when it came within of Earth with an apparent magnitude of 6.5. On August 3, 2026, comet Tempel 2 will have another close pass within about of Earth.

41P was recovered on November 10, 2016 at apparent magnitude 21 by Pan-STARRS. On April 1, 2017 the comet passed from the Earth. The comet was expected to brighten to around magnitude 7 and be visible in binoculars.

The apparent magnitude of the star, or how bright it appears from Earth, is around 5. Therefore, it is just visible to the unaided eye. Star HD 219134 (circled) lies just off the "W" shape of the constellation Cassiopeia.

HD 194244 is a variable Be star in the equatorial constellation of Aquila. With an apparent magnitude of 6.14, according to the Bortle scale it is faintly visible to the naked eye from rural skies on a dark night.

16 Arietis (abbreviated 16 Ari) is a star in the northern constellation of Aries. 16 Arietis is the Flamsteed designation. Its apparent magnitude is 6.01. Based upon the annual parallax shift of , this star is approximately distant from Earth.

Bayer-designated stars in Cassiopeia. Sigma Cassiopeiae is circled. Sigma Cassiopeiae (σ Cas, σ Cassiopeiae) is a binary star in the constellation Cassiopeia. It is approximately 5000 light years from Earth and has a combined apparent magnitude of +4.88.

Orbit of After it had been unobservable for almost three years, was recovered on 7 October 2018 by L. Buzzi at Schiaparelli Observatory (observatory code 204), at apparent magnitude 21. The 11 November 2018 flyby was about from Earth.

HD 93607 (HR 4222) is a star in the constellation Carina. Its apparent magnitude is 4.87. Its parent cluster is IC 2602. HD 93607 is a B4 main sequence star, although older spectral studies classified it as a subgiant.

HD 125351 or A Boötis (A Boo) is spectroscopic binary in the constellation Boötes. The system has an apparent magnitude of +4.97, with a spectrum matching a K-type giant star. It is approximately 233 light years from Earth.

On 11 January 2011, it was at opposition (coinciding with Hamilton's 72nd birthday) at a distance of 2.476 AU. Given the moderately elliptical orbit, this asteroid can on rare occasions reach an apparent magnitude from Earth of about 10.9.

HD 24480 is a double star in the northern constellation of Camelopardalis. The brighter component is a giant star with a stellar classification of K4III and an apparent magnitude of 5.20. The pair have an angular separation of 1.71″.

HD 130917 is a single star in the northern constellation of Boötes. It is an A-type main sequence star with a stellar classification of A4V. At an apparent magnitude of 5.80, it is visible to the naked eye.

Castor C is believed to be in orbit around Castor AB, but with an extremely long period of several thousand years. It is 73″ distant from the bright components. The combined apparent magnitude of all six stars is +1.58.

Despite its relative proximity to the Sun at 42 light-years, HD 40307 is not visible to the naked eye, given its apparent magnitude of 7.17. It came within 6.4 light-years of the Sun about 413,000 years ago.

N119 has an associated open cluster called NGC 1910 (also known as ESO 56-SC99). Its apparent magnitude is 11.2 and its apparent size is 1.54 arcminutes. It is inside N119 with a right ascension of and a declination of .

It had an apparent magnitude of 8.3 during a perihelic opposition on 25 December 2015. It is the parent body of the Euterpe family (), a stony inner-belt asteroid family of nearly 400 known members. Euterpe has been studied by radar.

It also has the other designation 6C B0014+8120, from the Sixth Cambridge Survey of Radio Sources by the University of Cambridge. The host galaxy of S5 0014+81 is a giant elliptical starburst galaxy, with the apparent magnitude of 24.

HD 113703, also known as f Centauri (f Cen), is a star in the constellation Centaurus. It is approximately 390 light years from Earth. f Centauri is a blue-white B-type main sequence dwarf with an apparent magnitude of +4.71.

Integrating the orbital solution shows the asteroid passed from Earth on 8 June 1975 with an apparent magnitude of about 13.9. The next notable close approach will be 27 May 2221, when the asteroid will pass Earth at a distance of .

28 Andromedae (abbreviated 28 And) is a Delta Scuti variable star in the constellation Andromeda. 28 Andromedae is the Flamsteed designation. It also bears the variable star name GN Andromedae. Its apparent magnitude is 5.214, varying by less than 0.1 magnitudes.

HD 111968, also known by the Bayer designation n Centauri (n Cen), is a star in the constellation Centaurus. n Centauri is a white A-type giant with an apparent magnitude of +4.25. It is approximately 149 light years from Earth.

On March 25, 2008, SN 2008bk was discovered in NGC 7793. At apparent magnitude 12.5, it became the 2nd brightest supernova of 2008. The progenitor of this supernova was a Red Supergiant, observed only 547 days prior to the explosion.

HD 129456, also known by its Bayer designation c1 Centauri (c1 Cen), is a star in the constellation Centaurus. c¹ Centauri is an orange K-type giant with an apparent magnitude of +4.06. It is approximately 209 light years from Earth.

IC 1517 is an elliptical galaxy, of apparent magnitude +13.8, in the constellation Pisces. The galaxy is south and west of Gamma Piscium, just south of the ecliptic, and north of the constellation Aquarius. It has a redshift of 0.02449.

HD 62166 has an exceptionally high surface temperature of about 200,000 kelvins and a luminosity 1,100 times that of the Sun. This dense star, with an estimated 0.6 solar mass and 0.028 solar radius, has an apparent magnitude of 17.5.

RV Corvi is an eclipsing binary star system in the constellation Corvus, ranging from apparent magnitude 8.6 to 9.16 over 18 hours. The system is composed of stars of spectral types F0 and G0, which orbit each other every 0.7473 days.

The "Very Large Telescope" at the European Southern Observatory in Northern Chile observed a possible optical counterpart of this neutron star. The object has an apparent magnitude that is (X ≤ 27.8). No companions have been discovered in orbit around this object.

HD 35619 is a double star in the northern constellation of Auriga. It has an apparent magnitude of 8.572, which is too faint to be viewed with the naked eye. The companion is 12th magnitude and 2 arc-seconds away.

U Equulei (U Equ / IRAS 20547 +0247) is a variable star in the Equuleus constellation with an apparent magnitude of +14.50 in the B band. It lies at an estimated distance of 5,000 light-years (1,500 parsecs ) from the Solar System.

HD 93194 (HR 4205) is a star in the constellation Carina. Its apparent magnitude is 4.79. Its parent cluster is IC 2602. HD 93607 is a B4 main sequence star, notable for "nebulous" absorption lines caused by its rapid rotation.

HD 149143, formally named Rosalíadecastro, is a star located in Ophiuchus constellation that has spectral type of G0 located at a distance of 240 ly from us. Its apparent magnitude is 7.9 (a binocular object) and the absolute magnitude is 3.9.

Gamma Cancri A presents as a white A-type subgiant with an apparent magnitude of +4.67. Located around 181 light-years from the Sun, it shines with a luminosity approximately 36 times greater and has a surface temperature of 9108 K.

HD 111915, also known by the Bayer designation e Centauri (e Cen), is a star in the constellation Centaurus. e Centauri is an orange K-type giant with an apparent magnitude of +4.33. It is approximately 294 light years from Earth.

NGC 1985 (also known as 2MASS J05374779+3159200) is a small, bright reflection nebula located in the Auriga. It was discovered by William Herschel on December 13, 1790. It has an Apparent Magnitude of 12.8 and its size is 0.68.

It is bright enough to be seen with the naked eye and can be found around 9° to the east-southeast of the Large Magellanic Cloud. The brighter component, designated γ2 Volantis, is an orange K-type giant star with a stellar classification of K0 III and an apparent magnitude of +3.62, making this the brightest star in the constellation. Its companion, γ1 Volantis, is an F-type main-sequence star of classification F2 V and an apparent magnitude of +5.70. As of 2002, the pair were at an angular separation of 14.1″ along a position angle of 296°.

AG Persei is another Algol variable in Perseus, whose primary component is a B-type main sequence star with an apparent magnitude of 6.69. Phi Persei is a double star, although the two components do not eclipse each other. The primary star is a Be star of spectral type B0.5, possibly a giant star, and the secondary companion is likely a stellar remnant. The secondary has a similar spectral type to O-type subdwarfs. With the historical name Mirfak (Arabic for elbow) or Algenib, Alpha Persei is the brightest star of this constellation with an apparent magnitude of 1.79.

At the time of discovery, was located in the constellation Taurus, at a very faint apparent magnitude of 24.6, approaching the lowest detectable magnitude limit for most telescopes. The very slow movement and low apparent magnitude of indicated that it is very distant, which prompted additional follow-up observations to constrain its orbit and distance. The object was reobserved in December 2018 with the 6.5-meter Magellan-Baade telescope at the Las Campanas Observatory in Chile, with observation times spanning ten days. However, due to 's slow motion, its orbit could not be accurately calculated from the short observation arc.

Varuna's apparent magnitude, its brightness as seen from Earth, varies from 19.5 to 20 magnitudes. At opposition, its apparent magnitude can reach up 20.3 magnitudes. Combined thermal measurements from the Spitzer Space Telescope and the Herschel Space Observatory in 2013 obtained a visual absolute magnitude (HV) of 3.76, comparable to that of the similarly-sized Kuiper belt object (HV=3.83). Varuna is among the twenty brightest trans- Neptunian objects known, despite the Minor Planet Center assuming an absolute magnitude of 3.6. The surface of Varuna is dark, with a measured geometric albedo of 0.127 based on thermal observations in 2013.

From mid November 2013 until 1 January 2014 15:00 UT the small dim asteroid had an elongation less than 45 degrees from the Sun with an undetectable apparent magnitude of around 30. While less than 18 degrees from the Sun any dim asteroid can be lost in astronomical twilight. On 1 January 2014 10:00 UT the asteroid passed from the Moon and at 16:13 UT passed from Earth. The asteroid was then discovered on 2 January 2014 by the Catalina Sky Survey at an apparent magnitude of 18.9 using a Schmidt–Cassegrain telescope.

Alpha Centauri A, also known as Rigil Kentaurus, is the principal member, or primary, of the binary system. It is a solar-like main-sequence star with a similar yellowish colour, whose stellar classification is spectral type G2 V; it is slightly larger and more luminous than the Sun. Alpha Centauri A is about 10 percent more massive than the Sun, with a radius about 22 percent larger. When considered among the individual brightest stars in the sky (excluding the Sun), it is the fourth brightest at an apparent magnitude of −0.01, being slightly fainter than Arcturus at an apparent magnitude of −0.05.

Lacaille gave twelve stars Bayer designations, labelling them Alpha through to Kappa, including two stars next to each other as Delta and another two stars near each other as Kappa. Within the constellation's borders, there are 39 stars brighter than or equal to apparent magnitude 6.5. Beta, Gamma and Delta Apodis form a narrow triangle, with Alpha Apodis lying to the east. The five brightest stars are all red-tinged, which is unusual among constellations. Alpha Apodis is an orange giant of spectral type K3III located 430 ± 20 light-years away from Earth, with an apparent magnitude of 3.8.

The primary member of 2 Camelopardalis, designated component A, is an A-type main-sequence star with a spectral type of A8V. It has an apparent magnitude of 5.86, and has a secondary with an apparent magnitude of 7.35, designated component B. The two orbit each other on a very eccentric orbit with a period of 26.65 years. Further out, there is an eight- magnitude companion (designated component C), orbiting once every few hundred years. Because the third star is relatively massive for its luminosity, it is possible that it may be a binary star itself.

Of apparent magnitude 5.11, the yellow bright giant Kappa Trianguli Australis of spectral type G5IIa lies around distant from the Solar System. Eta Trianguli Australis (or Eta1 Trianguli Australis) is a Be star of spectral type B7IVe which is from Earth, with an apparent magnitude of 5.89. Lacaille named a close-by star as Eta as well, which was inconsistently followed by Francis Baily, who used the name for the brighter or both stars in two different publications. Despite their faintness, Benjamin Gould upheld their Bayer designation as they were closer than 25 degrees to the south celestial pole.

Delta Coronae Borealis, Latinized from δ Coronae Borealis, is a variable star in the constellation Corona Borealis. Its apparent magnitude varies regularly between apparent magnitude 4.57 and 4.69, and it is around 170 light-years distant. δ Coronae Borealis is a yellow giant star of spectral type G3.5III that is around 2.4 times as massive as the Sun and has swollen to 7.4 times its radius. It has a surface temperature of 5180 K. For most of its existence, Delta Coronae Borealis was a blue-white main sequence star of spectral type B before it ran out of hydrogen fuel in its core.

Beta¹ Capricorni is the more complex of the pair and has a spectrum that is difficult to interpret. Its dominant pair of stars are the orange K-type bright giant Beta Capricorni Aa, with an apparent magnitude of +3.08, and the blue-white B-Type main sequence dwarf Beta Capricorni Ab1 with an apparent magnitude of +7.20. They are separated by 0.05 arcseconds (5 AU) and have an orbital period of 3.77 years. The Aa component has a surface temperature of 4900 kelvins, a radius 35 times that of the Sun, and a luminosity 600 times that of the Sun.

The yellow-white hued primary, component A, has an apparent magnitude of +6.32 and stellar classification of F2 IV/V, showing mixed traits of an F-type main-sequence star and a subgiant. It is classified as a Delta Scuti type variable star and its brightness varies from magnitude +6.28 to +6.39 with a period of 3.25 hours. A 2000 observing campaign identified at least six independent pulsation modes for this variation. The companion star, component B, has an apparent magnitude of +9.65 and, as of 2000, is at an angular separation of along a position angle of 183°.

HD 5319 is an 8th magnitude star approximately 397 light years away in the constellation Cetus. It is a subgiant star of spectral type K3, having run out of hydrogen in its core. When it was main-sequence, the spectral type was early F or late A. The absolute magnitude (apparent magnitude at 10 parsecs) is 3.05, which would translate to easy naked eye visibility, but its distance is ten times greater, so its apparent magnitude is 8.05 (100 times fainter than its absolute magnitude), it is not visible to the naked eye and binoculars are needed.

Located 42 million light- years away, it is moving away from the Solar System at a rate of 616 km per second. In 2000, a star within the galaxy brightened to magnitude 17.4, and has since been determined to be a luminous blue variable and supernova impostor. NGC 3003, a SBbc barred spiral galaxy with an apparent magnitude of 12.3 and an angular size of 5.8 arcminutes, is seen almost edge-on. NGC 3344, 25 million light-years distant, is face-on towards Earth. Measuring 7.1 by 6.5 arcminutes in size, it has an apparent magnitude of 10.45. NGC 3504 is a starburst barred spiral galaxy of apparent magnitude 11.67 and measuring 2.1 by 2.7 arcminutes. It has hosted supernovae in 1998 and 2001. It and the spiral galaxy NGC 3486 are also almost face-on towards Earth; the latter is of magnitude 11.05 and measures 7.1 by 5.2 arcminutes. NGC 2859 is an SB0-type lenticular galaxy.

It has been reported to show eclipses of less than 0.1 magnitudes with a period of 2 years and 1 month., but this has never been confirmed. It is 99.4 ± 0.4 light-years from Earth. Epsilon Cassiopeiae has an apparent magnitude of 3.3.

After analysis of HD 205739's spectrum, it can be concluded that HD 205739's chromosphere (its outermost layer) is not active. HD 205739 cannot be seen from Earth with the naked eye because the star has an apparent magnitude (V) of 8.56.

HD 88218 is a binary star in the southern constellation of Antlia. With an apparent magnitude of 6.16, the system is faintly visible to the naked eye from dark skies. The pair orbit each other with a period of about 86 years.

M47 on the left. KQ Puppis (KQ Pup) is a spectroscopic binary variable star in the constellation Puppis. A red supergiant star and a hot main sequence star orbit each other every 9,742 days. Its apparent magnitude varies between 4.82 and 5.17.

20 Ophiuchi is a class F6IV (yellow-white subgiant) star in the constellation Ophiuchus. Its apparent magnitude is 4.64 and it is approximately 104 light years away based on parallax. It lies near the star Zeta Ophiuchi. 20 Ophiuchi is an astrometric binary.

HD 37756 is a class B2IV (blue subgiant) star in the constellation Orion. Its apparent magnitude is 4.95 and it is approximately 900 light years away based on parallax. It is a spectroscopic binary, with a period of 27 days and eccentricity 0.72.

HD 2421 is a double-lined spectroscopic binary with a class A main-sequence primary and a class F main-sequence secondary in the constellation Andromeda. Its apparent magnitude is 5.18 and it is approximately 290 light years away based on parallax.

Its orbital period is 760 years; the two components are currently moving farther apart. θ Aquarii, sometimes called Ancha, is a G8 spectral type star with an apparent magnitude of 4.16 and an absolute magnitude of 1.4. κ Aquarii, also called Situla.

NGC 6388 is a globular cluster located in the constellation Scorpius. The cluster was discovered by Scottish astronomer James Dunlop on May 13, 1826 using a reflector telescope. Due to its moderate apparent magnitude (+6.72), a telescope is required to see it.

NGC 6440 is a globular cluster in the constellation Sagittarius and was discovered by William Herschel on 28 May 1786. It has an apparent magnitude of about 10, with a diameter of about 6 arcminutes, and its Shapley–Sawyer Concentration Class is V.

HD 65750 is located about 900 light years away, and has an apparent magnitude that varies between 6.2 and 7.1 and a metallicity just of the Sun. It is part of the Diamond Cluster moving group. The star has a radial velocity of .

Nova in Andromeda Galaxy Novae are relatively common in the Andromeda Galaxy (M31). Approximately several dozen novae (brighter than about apparent magnitude 20) are discovered in M31 each year. The Central Bureau for Astronomical Telegrams (CBAT) tracked novae in M31, M33, and M81.

Alchiba belongs to the spectral class F1V and has apparent magnitude +4.00. This star exhibits periodic changes in its spectrum over a three-day period, which suggests it is either a spectroscopic binary or (more likely) a pulsating Gamma Doradus-type variable.

The star is slightly dimmer than planet Neptune as perceived with the naked eye, which has an apparent magnitude of 7.78 at its brightest. The star's actual brightness is measured with an absolute magnitude of 4.12, similar to that of the Sun.

In comparison, the Sun is about 4.6 billion years old and has a surface temperature of 5778 K. The star's apparent magnitude, or how bright it appears from Earth's perspective, is 3.53. Therefore, Epsilon Tauri can be seen with the naked eye.

Gamma Trianguli (Gamma Tri, γ Trianguli, γ Tri) is a star in the constellation Triangulum located approximately 112 light years from Earth. It has an apparent magnitude of +4.01 and forms an optical (line-of-sight) triple with Delta Trianguli and 7 Trianguli.

Psi2 Draconis is a solitary giant star in the northern circumpolar constellation of Draco, also designated 34 Draconis. It lies about a degree east of the brighter Psi1 Draconis. Psi2 Draconis has an apparent magnitude of 5.45. and is located around away.

In comparison, the Sun is 4.6 billion years old and has a surface temperature of 5778 K. The star's apparent magnitude, or how bright it appears from Earth's perspective, is 14.3. Therefore, it is too dim to be seen with the naked eye.

It is also the basis for computing the geometrical albedo and the Bond albedo of the body. In ephemeris generation, the phase curve is used in conjunction with the distances from the object to the Sun and the Earth to calculate the apparent magnitude.

NGC 2326 (also known as PGC 20218) is a barred spiral galaxy in the Lynx constellation. It was discovered by William Herschel on 9 February, 1788. Its apparent magnitude is 14.3 and its size is 2.71 arc minutes. It is located near NGC 2326A.

HD 190007, also known as Gliese 775, is a star in the constellation of Aquila. Its apparent magnitude is 7.48. Parallax measurements by Gaia put the star at a distance of 41.5 light-years (12.74 parsecs) away. HD 190007 is a BY Draconis variable.

55 Ursae Majoris (55 UMa) is a triple star system in the constellation Ursa Major. Its apparent magnitude is 4.80. Two stars form a close spectroscopic binary with an orbital period of 2.55 days. The third star orbits the central pair every 1873 days.

NGC 6086 is an elliptical galaxy in the constellation of Corona Borealis. It has an apparent magnitude of 12.7. A Type-cD galaxy, it is the brightest cluster galaxy in the cluster Abell 2162. In 2010, a supermassive black hole was discovered in NGC 6086.

HIP 41378 is a star located 348 light-years away in the constellation of Cancer. The star has an apparent magnitude of 8.92. This F-type main sequence dwarf has a mass of and a radius of . It has a surface temperature of about .

The NGC 5866 Group is a small group of galaxies located in the constellation Draco. The group is named after NGC 5866, the galaxy with the highest apparent magnitude in the group, although some galaxy group catalogs list NGC 5907 as the brightest member.

Iota Cassiopeiae (ι Cas, ι Cassiopeiae) is a star system in the constellation Cassiopeia. The system has a combined apparent magnitude of 4.53, making it visible to the naked eye. Based on its parallax, it is located about 133 light-years (41 parsecs) from Earth.

WD 1337+705 is a star in the constellation Ursa Minor. Shining with an apparent magnitude of 12.8, it is white dwarf 0.59 times as massive as the Sun. It is 86.5 light-years distant from Earth. It has 3% of the Sun's luminosity.

This star type varies in luminosity due to non-radial pulsations. Its apparent magnitude varies from 4.93 to 5.03 over a period of 1.25804 days. For that reason it has been given the variable star designation V398 Aurigae. 9 Aurigae is a multiple star system.

Gliese 167 is a star in the constellation Dorado. It has an apparent magnitude of 7.634. Based on parallax measurements by Gaia, the star is known to be located 42.5 light-years (13.02 parsecs) away. The star is a K-type main- sequence star.

Omicron Andromedae (ο And, ο Andromedae) is a star system in the constellation Andromeda. It is approximately 692 light years from Earth. The system as a whole is classified as a blue-white B-type giant, with a mean combined apparent magnitude of +3.62.

EZ Canis Majoris (abbreviated to EZ CMa, also designated as WR 6) is binary system in the constellation of Canis Major. The primary is a Wolf-Rayet star and it is one of the ten brightest Wolf-Rayet stars, brighter than apparent magnitude 7.

Omicron Herculis is a B9.5V star approximately 106 pc from the Earth. It has an apparent magnitude of 3.83. The star radiates with a bluish-white hue, and has a luminosity approximately 355 times as bright as the Sun. Omicron Herculis is 3.49 solar masses.

It is found in a region often called the Sea due to its profusion of constellations with watery associations such as Cetus the whale, Pisces the fish, and Eridanus the river. At apparent magnitude 2.9, Beta Aquarii is the brightest star in the constellation.

In comparison, the Sun is about 4.6 billion years old and has a surface temperature of 5778 K. The star's apparent magnitude, or how bright it appears from Earth's perspective, is 8.19. Therefore, HD 240237 is too dim to be seen with the naked eye.

The primary component, Atlas A, is a blue-white B-type giant with an apparent magnitude of +3.62. It is a binary star whose components have magnitudes of 3.84 and 5.46. The binary makes one orbit every 290 days, and the eccentricity is about 0.24.

HD 190647 is a yellow subgiant star located approximately 178 light years away in the constellation of Sagittarius. The apparent magnitude is 8 and absolute magnitude is 4. It is also called HIP 99115. In 2007, a planet was found to be orbiting the star.

HD 190228 is a star located in the constellation Vulpecula. Its apparent magnitude is 7.31 and the absolute magnitude is 3.34. The distance is 205 light years from Earth. The star is definitely old with age over 10 billion years and it is metal-poor.

Based on its spectrum, WASP-44 is not active in its chromosphere (outer layer). The star was also not found to demonstrate a high rate of rotation. With an apparent magnitude of 12.9, WASP-44 cannot be seen with the unaided eye from Earth.

In 1910 Hans Rosenberg published a diagram plotting the apparent magnitude of stars in the Pleiades cluster against the strengths of the calcium K line and two hydrogen Balmer lines. These spectral lines serve as a proxy for the temperature of the star, an early form of spectral classification. The apparent magnitude of stars in the same cluster is equivalent to their absolute magnitude and so this early diagram was effectively a plot of luminosity against temperature. The same type of diagram is still used today as a means of showing the stars in clusters without having to initially know their distance and luminosity.

Located about 97 light-years away from Earth, Alpha Pictoris is the brightest star in the constellation; it is a white main-sequence star with an apparent magnitude of 3.3, and spectral type A8VnkA6. A rapidly spinning star with a projected rotational velocity estimated at 206 km/s, it has a shell of circumstellar gas. Beta Pictoris is another white main sequence star of spectral type A6V and apparent magnitude 3.86. Located around 63.4 light-years distant from Earth, it is a member of the Beta Pictoris moving group—a group of 17 star systems around 12 million years old moving through space together.

Tombaugh continued searching for over a decade after the discovery of Pluto, and the lack of further discoveries left him satisfied that no other object of a comparable apparent magnitude existed near the ecliptic. No more trans-Neptunian objects were discovered until 15760 Albion in 1992. However, more recently the relatively bright object has been discovered. It has a relatively high orbital inclination, but at the time of Tombaugh's discovery of Pluto, Makemake was only a few degrees from the ecliptic near the border of Taurus and Aurigabased on Minor Planet Center online Minor Planet Ephemeris Service: March 1, 1930: RA: 05h51m, Dec: +29.0 at an apparent magnitude of 16.

A.R. Gibbs of the Mount Lemmon Observatory in Arizona discovered the comet based on images acquired by the sky survey's 1.5-m reflecting telescope on 23 March 2012. However, Gibbs did not recognize its cometary appearance and was listed as an asteroid on the Minor Planet Center's Near Earth Object confirmation page. At the time, the apparent magnitude of the comet was estimated between +20.6 and +20.8. Shortly after initial discovery, amateur astronomer Peter Birtwhistle in Great Shefford observed the comet using a 40-cm refracting telescope and CCD images, estimating an apparent magnitude of +20.1 and a diameter stretching 5 arc seconds across.

Makemake (apparent magnitude 16.9) with edge on galaxy IC 3587 Makemake's orbit outside of Neptune is similar to Haumea's. The positions are as of 1 January 2018. Makemake is currently visually the second-brightest Kuiper belt object after Pluto, having a March opposition apparent magnitude of 17.0 it will pass from its present constellation Coma Berenices to Boötes in December 2027. It is bright enough to be visible using a high-end amateur telescope. Combining the detection in infrared by the Spitzer Space Telescope and Herschel Space Telescope with the similarities of spectrum with Pluto yielded an estimated diameter from 1,360 to 1,480 km.

The primary, component A, is a B-type giant with a stellar classification of B6III and an apparent magnitude of +5.8. It has five times the mass of the Sun and is spinning rapidly with a projected rotational velocity of 170 km/s. The star is radiating 1,893 times the luminosity of the Sun from its photosphere at an effective temperature of 15,439 K. At an angular separation of only 0.34 arcseconds is the companion, component B, a B-type subgiant star with a class of B6IV and an apparent magnitude of +6.3. These two stars orbit around their common centre of mass once every 420 years.

The object's position and cometary appearance was confirmed by several other unaffiliated observers, and as such the comet was named ISON, after the international observational project and in accordance with International Astronomical Union naming guidelines. Comet ISON was precovered in analysis of Mount Lemmon Observatory imagery by G. V. Williams and Pan-STARRS imagery in Haleakalā. Precovery images from Mount Lemmon were first taken on 28 December 2011 and indicated that the comet had an estimated apparent magnitude ranging from 19.5 to 19.9. Images from Pan-STARRS were taken on 28 January 2012 and in those images the comet had an estimated apparent magnitude ranging from 19.8 to 20.6.

With an apparent visual magnitude of −0.05, Arcturus is the brightest star in the northern celestial hemisphere and the fourth-brightest star in the night sky, after Sirius (−1.46 apparent magnitude), Canopus (−0.72) and α Centauri (combined magnitude of −0.27). However, α Centauri AB is a binary star, whose components are both fainter than Arcturus. This makes Arcturus the third-brightest individual star, just ahead of α Centauri A (officially named Rigil Kentaurus), whose apparent magnitude . The French mathematician and astronomer Jean-Baptiste Morin observed Arcturus in the daytime with a telescope in 1635, a first for any star other than the Sun and supernovae.

The absolute magnitude , of a star or astronomical object is defined as the apparent magnitude it would have as seen from a distance of . The absolute magnitude of the Sun is 4.83 in the V band (visual), 4.68 in the Gaia satellite's G band (green) and 5.48 in the B band (blue). In the case of a planet or asteroid, the absolute magnitude rather means the apparent magnitude it would have if it were from both the observer and the Sun, and fully illuminated at maximum opposition (a configuration that is only theoretically achievable, with the observer situated on the surface of the Sun).

Fenrir , or Saturn XLI (provisional designation S/2004 S 16), is a natural satellite of Saturn. Its discovery was announced by Scott S. Sheppard, David C. Jewitt, Jan Kleyna, and Brian G. Marsden on May 4, 2005, from observations taken between December 13, 2004, and March 5, 2005. Fenrir has an apparent magnitude of 25, making it one of the faintest known moons in the Solar System, and was discovered using some of the largest telescopes in the world. It is even too dark to be observed by the Cassini spacecraft in orbit around Saturn, for which it never gets brighter than approximately 17th apparent magnitude.

LSS 4067, also known as CD−38°11748, is an O-type blue supergiant star located in the constellation Scorpius, very close to the galactic plane. It is part of the open cluster HM 1, although its distance is not well known; it may be anywhere between 9,500 and 12,700 light years (2900 to 3900 parsecs) away from the Earth. Despite being a blue supergiant, it is extremely reddened by interstellar extinction, so its apparent magnitude is brighter for longer- wavelength passbands. Without the extinction, it is estimated that LS 4067 would be 5.8 magnitudes brighter, a naked eye star with an apparent magnitude of 5.3.

Alnitak (ζ Orionis) is a triple star system at the eastern end of Orion's belt and is 1,260 light-years from the Earth. Alnitak B is a 4th-magnitude B-type star which orbits Alnitak A every 1,500 years. The primary (Alnitak A) is itself a close binary, comprising Alnitak Aa (a blue supergiant of spectral type O9.7 Ibe and an apparent magnitude of 2.0) and Alnitak Ab (a blue dwarf of spectral type O9V and an apparent magnitude of about 4). Alnitak Aa is estimated as being up to 28 times as massive as the Sun, and to have a diameter 20 times greater.

Known as Kappa Tucanae B, it has an apparent magnitude of 7.58 and spectral type K1V. Five arcminutes to the northwest is a fainter star of apparent magnitude 7.24 —actually a pair of orange main sequence stars of spectral types K2V and K3V, which can be seen individually as stars one arcsecond apart with a telescope such as a Dobsonian with high power. Most of the Small Magellanic Cloud lies within Tucana. Lambda Tucanae is an optical double—that is, the name is given to two stars (Lambda1 and Lambda2) which appear close together from our viewpoint, but are in fact far apart in space.

Epsilon Canis Majoris (Latinised from ε Canis Majoris, abbreviated Epsilon CMa, ε CMa) is a binary star and, despite being designated ε (epsilon), the second-brightest object in the constellation of Canis Major and one of the brightest stars in the night sky with an apparent magnitude of 1.50. About 4.7 million years ago, it was the brightest star in the sky, with an apparent magnitude of −3.99. Based upon parallax measurements obtained during the Hipparcos mission, it is about 430 light-years distant from the Sun. The two components are themselves designated ε Canis Majoris A (also officially named Adhara , the traditional name of the system) and B.

The asteroid was discovered on 20 November 2007 by Andrea Boattini of the NASA-funded Catalina Sky Survey on Mount Lemmon, near Tucson, Arizona, United States, using a 1.5-meter telescope. It was discovered in the constellation Taurus at an apparent magnitude of +20. This is about 400,000 times fainter than most people can see with the naked eye on a dark night far from city lights. It was discovered nineteen days after passing near the Earth. By the time it arrived at Mars it had an apparent magnitude of roughly +26 and therefore appeared over 100 times fainter than at the time of discovery.

Gliese 146 is a K5V class star located in the constellation Horologium. At 44.4 light years, GJ 146 has an apparent magnitude of +8.57. Gliese 146 is also known as HD 22496, HIP 16711, SAO-216392, and LHS 1563.K stars within 100 light-years - SolStation.

NGC 953 (also PGC 9586, UGC 1991, MCG 5-7-1, GWT GWT 504 104 or 505.1) is an elliptical galaxy in the constellation Triangulum. It has an apparent magnitude of 14.5. It was discovered by the German astronomer Heinrich Louis d'Arrest on September 26, 1865.

The reddened light from the center of the galaxy appears yellowish due to the intervening gas and dust located within the outer arms of NGC 2683. Its apparent magnitude is 10.6 making it not visible to the human eye without the aid of a small telescope.

HD 16028 is a star in the constellation Andromeda. Its apparent magnitude is 5.71. Located approximately distant, it is an orange giant of spectral type K3III, a star that has used up its core hydrogen and has expanded. Double star catalogues list two stars as optical companions.

The distance from the anode (source of X-rays) to the image receptor greatly influences the apparent magnitude of the anode heel effect. The shorter the distance, the less space the beam has to diverge. The effect is less noticeable at larger source-image distances (SID).

One supernova has been observed in NGC 3393, SN 2018aqi. The supernova was discovered by ASAS-SN on April 6, 2018, and had an apparent magnitude of 16.4 at discovery. By its spectrum, it was identified as a type Ia supernova 6 days before maximum brightness.

The Romans named it after their god Jupiter. When viewed from Earth, Jupiter can reach an apparent magnitude of −2.94, bright enough for its reflected light to cast shadows, and making it on average the third-brightest object in the night sky after the Moon and Venus.

Gliese 393 is a red dwarf star in the constellation Sextans. At apparent magnitude 9.65, it is much too faint to be seen with the unaided eye. A small star, it has around 41% the mass and radius of the Sun, but only 2.35% its luminosity.

NGC 1058 is a Seyfert Type 2 galaxy in the NGC 1023 Group, located in the Perseus constellation. It is approximately 27.4 million light years from Earth and has an apparent magnitude of 11.82. It is receding from Earth at , and at relative to the Milky Way.

The wind is being effected by the star's rapid rotation, resulting in an enhanced outflow along the equator. Gamma Arae has an optical companion located at an angular separation of 17.9 arcseconds, which is an A-type main sequence star with an apparent magnitude of 10.5.

HD 135944 is a star in the northern constellation of Boötes. With an apparent magnitude of 6.5, it is at the limits of naked eye visibility. There is a magnitude 8.94 companion at an angular separation of 67.3″ along a position angle of 102° (as of 2011).

CoRoT-7 (TYC 4799-1733-1) is a G-type main sequence star, slightly smaller and cooler than the Sun. It has an apparent magnitude 11.67, fainter than Proxima Centauri (mag. 11.05), the nearest star to the Sun. This star is located in the Monoceros constellation.

LP 944-20 is a dim brown dwarf of spectral class M9 located about 21 light- years from the Solar System in the constellation of Fornax. With a visual apparent magnitude of 18.69, it has one of the dimmest visual magnitudes listed on the RECONS page.

It is more magnetically active than Alpha Centauri A, showing a cycle of compared to 11 years for the Sun, and about half the minimum-to-peak variation in coronal luminosity of the Sun. Alpha Centauri B has an apparent magnitude of +1.35, slightly dimmer than Mimosa.

HD 160529 (V905 Scorpii) is a luminous blue variable (LBV) star located in the constellation of Scorpius. With an apparent magnitude of around +6.8 cannot be seen with the naked eye except under very favourable conditions, but it's easy to see with binoculars or amateur telescopes.

Additionally, with a luminosity of 2.25, HD 8574 releases more than twice the energy released by the Sun. The star has an apparent magnitude of 7.12, and is thus extremely faint (if visible at all) as seen from the unaided eye of an observer on Earth.

WASP-24 has a metallicity similar to that measured in the Sun. The star's estimated age is 3.8 billion years old, although the star's age is not well-constrained. WASP-24 has an apparent magnitude of 11.3. It cannot be seen from Earth with the naked eye.

QU Vulpeculae was a nova, which occurred in 1984 in the constellation Vulpecula and which reached a brightness of 5.2 mag. Peter Collins an amateur astronomer from Cardiff, California discovered this nova on December 22, 1984. The apparent magnitude was 6.8 at the time of discovery.

On 17 March 2013, an object hit the lunar surface in Mare Imbrium and exploded in a flash of apparent magnitude 4. The crater could be as wide as 20 meters. This was the brightest impact recorded since NASA's lunar impact team began monitoring in 2005.

R Serpentis is a Mira variable type star in the equatorial constellation of Serpens. It ranges between apparent magnitude 5.16 and 14.4, and spectral types M5e to M8e, over a period of 356.41 days. The variability of this star was discovered in 1826 by Karl Ludwig Harding.

Gamma1 Fornacis (γ1 For) is a star in the constellation Fornax. Its apparent magnitude is 6.15. It is a yellow giant that has swollen and brightened to around 80 times as luminous as the Sun. γ1 Fornacis has three companions listed in the Washington Double Star Catalog.

NGC 2460 has an absolute magnitude of 11.7, and an apparent magnitude of 12.1. Several arms extend for long distances from the central galaxy, perhaps as a result of an interaction with nearby galaxy PGC 213434. The galaxy has a radial velocity of 1443 km/s.

M Centauri (M Cen) is a binary star in the constellation Centaurus. It is approximately 260 light years from Earth. M Centauri is a yellow G-type giant with an apparent magnitude of +4.64. It is a spectroscopic binary with an orbital period of 437 days.

NGC 77 (also known as PGC 1290, NPM1G -22.0006 or PGC 198147) is a lenticular galaxy located 780 million light-years away in the constellation of Cetus. It was discovered by Frank Muller in 1886 and its apparent magnitude is 14.8. This galaxy is around 360,000 light-years across.

NGC 85 is an interacting spiral or lenticular galaxy estimated to be about 200 million light-years away in the constellation of Andromeda. It was discovered by Ralph Copeland in 1873 and its apparent magnitude is 15.7. The galaxy appears to be interacting with the companion spiral IC 1546.

KELT is dedicated to discovering transiting exoplanets orbiting stars in the apparent magnitude of 8 < V < 10 magnitude. This is the regime just fainter than the set of stars comprehensively surveyed for planets by the radial-velocity surveys, but brighter than those typically observed by most transit surveys.

The 21 May 2014 Earth close approach of should allow a refinement to the orbit. From 7 May 2014 until 2 June 2014 the asteroid will be brighter than apparent magnitude 20. The asteroid will come to opposition on 18 May 2014 when it will be up all night.

This structure is thought to be the remnants of a smaller galaxy that was torn apart by tidal forces as it collided with NGC 4013. Supernova SN 1989Z was discovered on December 30, 1989 at apparent magnitude 12. NGC 4013 is a member of the Ursa Major Cluster.

NS Puppis (NS Pup) is an irregular variable star in the constellation Puppis. Its apparent magnitude varies between 4.4 and 4.5. NS Puppis is a naked eye star, given the h1 and the Bright Star Catalogue number 3225. It was considered to be a stable star until 1966.

HD 208177 is a double star system in the equatorial constellation of Aquarius. They are faintly visible to the naked eye with an apparent magnitude of 6.20. The pair have an angular separation of 19.113″. The primary component is an evolved subgiant star with a stellar classification of F5IV.

HD 183143 (HT Sagittae) is a blue hypergiant star located in the constellation of Sagitta. This star has an apparent magnitude of 6.86, meaning that can be seen with the naked eye under very dark skies and that is an easy target for binoculars or a small telescope.

It was removed from the Sentry Risk Table on 21 December 2013. It may be possible to recover the asteroid in late September 2017, but it will have an apparent magnitude of about 22. It has an observation arc of 35 days with an uncertainty parameter of 6.

NGC 3244 is a spiral galaxy in the Antlia constellation discovered by John Herschel on April 22, 1835. A supernova was detected in NGC 3244 on June 27, 2010, designated SN 2010ev. With an apparent magnitude of about 14, it was the third-brightest supernova observed in 2010.

28 Monocerotis is a class K4III (orange giant) star in the constellation Monoceros. Its apparent magnitude is 4.69 and it is approximately 450 light years away based on parallax. It is an FK Comae Berenices variable, with a magnitude varying by 0.02 with a period of 0.21 days.

Xi Andromedae (ξ Andromedae, abbreviated Xi And, ξ And), officially named Adhil , is a solitary star in the northern constellation of Andromeda. It has an apparent magnitude of +4.9. Based on parallax measurements obtained during the Hipparcos mission, it lies at a distance of roughly from the Sun.

The galaxy is close enough so as its stars can be resolved. The brightest of them have apparent magnitude about 21.5.Sandage, A., Bedke, J. (1994), The Carnegie Atlas of Galaxies. Volume I, Carnegie Institution of Washington One ultra- luminous X-ray source has been detected in the galaxy.

See: of spectral type C6,4(Nb) with a prominent red hue. Located in the west of the constellation and depicting the peacock's tail are Eta and Xi Pavonis. At apparent magnitude 3.6, Eta is a luminous orange giant of spectral type K2II some 350 light years distant from Earth.

171P/Spahr is a periodic comet in the Solar System. 171P/Spahr was recovered on 20–24 October 2011 at apparent magnitude 20.6 using the Faulkes Telescope South. 171P/Spahr is peaked at about magnitude 18 in 2012. During the 1999 passage the comet brightened to about magnitude 13.5.

HD 93833 is a star in the constellation of Sextans. Its apparent magnitude is 5.842, but interstellar dust makes it appear 0.202 magnitudes dimmer than it should be. It is located some 340 light-years (104 parsecs) away, based on parallax. HD 93833 is a K-type giant star.

NGC 1994 (also known as ESO 56-SC136) is an open cluster in the Dorado constellation which is located in the Large Magellanic Cloud. It was discovered by John Herschel on 16 December 1835. It has an apparent magnitude is 9.8 and its size is 0.60 arc minutes.

Delta Trianguli Australis (δ TrA, δ Trianguli Australis) is a single, yellow- hued star in the constellation Triangulum Australe. It is approximately 606 light years (182 parsecs) from Earth. This is a G-type giant star with a stellar classification of G5II and an apparent magnitude of +3.86.

47 Tucanae, 47 Tuc (or NGC 104) is a globular cluster located in the constellation Tucana. It is about away from Earth, and 120 light years across. 47 Tuc can be seen with the naked eye, with an apparent magnitude of 4.1. It appears about 50 arcminutes across.

Gamma1 Caeli, Latinized from γ1 Caeli, is a double star in the constellation Caelum. It is approximately 185 light years from Earth. The brighter component is an orange K-type giant with an apparent magnitude of +4.55. The companion is an eighth magnitude star located 3.1 arcseconds away.

It is a semiregular variable star of the Mu Cephei type, whose apparent magnitude varies between 3.3 and 4.0 with periods of 50, 120 and 250 days. The Double Cluster contains three even larger stars, each over 700 solar radii: S, RS, and SU Persei are all semiregular pulsating M-type supergiants. The stars are not visible to the naked eye; SU Persei, the brightest of the three, has an apparent magnitude of 7.9 and thus is visible through binoculars. AX Persei is another binary star, the primary component is a red giant in an advanced phase of stellar evolution, which is transferring material onto an accretion disc around a smaller star.

Although of a similar distance—around 302 light- years—to the stars of the Lower Centaurus Crux subgroup, it is moving much faster at around 100 km/s and does not share a common origin. To the northwest lies Mu Muscae, an orange giant of spectral type K4III that varies between apparent magnitude 4.71 and 4.76, and has been classified as a slow, irregular variable. Near Mu is Lambda Muscae, the third-brightest star in the constellation and a white main-sequence star of spectral type A7V around 128 light-years distant from Earth. Located near Alpha is R Muscae, a classical Cepheid variable ranging from apparent magnitude 5.93 to 6.73 over 7.5 days.

Following discovery, Lemmon remained a dim object but steadily brightened over the next few months. The comet was last sighted on 14 June 2012 with an apparent magnitude estimated at +19.0 before it was lost in the sun's glare. On 25 August, the comet was analyzed to have passed an apparent 0.7 degrees from the sun. The comet was re-sighted on 14 October utilizing the RAS (Remote Astronomical Society) Observatory of New Mexico in Mayhill, with an apparent magnitude estimated to have brightened to +15.3. The first confirmed visual observation of the comet without the use of CCD imagery was conducted by Juan Jose Gonzalez Suarez in Cantabria, Spain using a 20-cm reflector on 22 November.

Ankaa is the brightest star in the constellation. It is an orange giant of apparent visual magnitude 2.37 and spectral type K0.5IIIb, 77 light years distant from Earth and orbited by a secondary object about which little is known. Lying close by Ankaa is Kappa Phoenicis, a main sequence star of spectral type A5IVn and apparent magnitude 3.90. Located centrally in the asterism, Beta Phoenicis is the second brightest star in the constellation and another binary star. Together the stars, both yellow giants of spectral type G8, shine with an apparent magnitude of 3.31, though the components are of individual apparent magnitudes of 4.0 and 4.1 and orbit each other every 168 years.

Within the constellation's borders, there are 47 stars brighter than or equal to apparent magnitude 6.5. Traditionally representing the mouth of the fish, Fomalhaut is the brightest star in the constellation and the 19th brightest star in the night sky, with an apparent magnitude of 1.16. Located 25.13 ± 0.09 light- years away, it is a white main sequence star that is 1.92 ± 0.02 times as massive and 16.63±0.48 as luminous as the Sun. Its companion Fomalhaut b was thought to be the first extrasolar planet ever detected by a visible light image, thanks to the Hubble Space Telescope, but infrared observations have since retracted this claim: it is instead a spherical cloud of dust.

Simulated image of the β Tucanae system The two brightest stars, Beta-1 Tucanae and Beta-2 Tucanae, also referred to as Beta Tucanae A and Beta Tucanae C, are 27 arcseconds, or at least 1100 astronomical units (AU) apart. They are both main sequence dwarfs, Beta-1 a blue-white B-type star with an apparent magnitude of +4.36, and Beta-2 a white A-type star with an apparent magnitude of +4.53. Both of these bright stars have at least one closer main sequence companion. Beta Tucanae B is a magnitude +13.5 M3-type star which is a close companion to Beta-1, being 2.4 arcseconds, or at least 100 AU away.

This is a flare star of the type known as a BY Draconis variable. It varies slightly in apparent magnitude, ranging from 6.44 to 6.49 over a 10.3 day period. While smaller than the Sun, it is relatively large for a flare star. Most flare stars are red M-type dwarfs.

On 9 February 2018, the asteroid passed about from Earth, traveling relative to Earth and briefly reaching apparent magnitude 13. It was observed by the Goldstone Observatory, which constrained its size to no more than 20 meters. During the flyby its period was changed from 1.48 years to 1.67 years.

S Scuti is a carbon star located in the constellation Scutum. Parallax measurements by Hipparcos put it at a distance of approximately 1,300 light- years (390 parsecs). Its apparent magnitude is 6.80, making it visible to the naked eye only under excellent conditions. S Scuti is a semiregular variable star.

QW Puppis (QW Pup) is a class F3V (yellow-white dwarf) star in the constellation Puppis. Its apparent magnitude is 4.49 and it is approximately 69.9 light years away based on parallax. It is a Gamma Doradus variable, ranging from 4.5 to 4.47 magnitude with a period of 0.96 days.

The galaxy PGC 16052 is not a NGC object, nor is it physically associated with NGC 1573, but is often called NGC 1573A. It is an intermediate spiral galaxy with an apparent magnitude of about 14.0. In 2010, a supernova was discovered in PGC 16052 and was designated as SN 2010X.

28 Aurigae (28 Aur) is a star in the constellation Auriga. Its apparent magnitude is 6.80. It is a giant star which has exhausted its core hydrogen and expanded to ten times the size of the Sun. Despite being slightly cooler than the sun at it is 73 times more luminous.

M Puppis (M Pup, HR 2789, HD 57197) is a blue giant or bright giant star (spectral type B8II/III) in the constellation Puppis. Its apparent magnitude is 5.84, which means it is visible with the naked eye under optimal conditions. It is approximately 590 light years away based on parallax.

Are Comets 42P/Neujmin 3 and 53P/Van Biesbroeck Parts of one Comet? The orbit of 53P/Van Biesbroeck has a Jupiter Minimum orbit intersection distance (MOID) of only . The next perihelion passage is on Christmas Eve 24 December 2028. The comet is expected to brighten to about apparent magnitude 14.

HAT-P-7 is a F-type main sequence star located about 1123 light-years away in the constellation Cygnus. The apparent magnitude of this star is 10.5, which means it is not visible to the naked eye but can be seen with a small telescope on a clear dark night.

R Apodis (R Aps) is a star in the constellation Apus. R Apodis is an orange K-type giant with an apparent magnitude of +5.34. It is approximately 386 light years from Earth. It was earlier suspected to be a variable star and given the variable star designation R Apodis.

40 Arietis is a probable binary star system in the northern constellation of Aries. 40 Arietis is the Flamsteed designation. Their combined apparent magnitude is 5.82, putting the system near the limit of naked eye visibility. Based upon an annual parallax shift of just , it is away from the Sun.

Image taken by ESO's VISTA of the Globular Cluster VVV CL001. On the right lies the globular star cluster UKS 1 and on the left lies a much less conspicuous new discovery, VVV CL001. This is a list of globular clusters. The apparent magnitude does not include an extinction correction.

Holmberg II is a dwarf galaxy in the constellation Ursa Major. Its apparent magnitude is 11,1m and it is 11 million light years away from Earth. The galaxy is dominated by huge glowing gas bubbles, which are regions of star formation. Holmberg II also hosts an ultraluminous X-ray source.

Cor Caroli seen from northern England on March 1, 2011. Alpha Canum Venaticorum is a binary star with a combined apparent magnitude of 2.81. The two stars are 19.6 arcseconds apart in the sky and are easily resolved in small telescopes. The system lies approximately 110 light years from the Sun.

In addition, Kepler-4 has an effective temperature of 5781 (± 76) K, which is almost identical, within the errors, to that of the Sun, which is 5778 K. As seen from Earth, Kepler-4 has an apparent magnitude of 12.7. It is, as a result, not visible with the naked eye.

The Great Comet of 1819, officially designated as C/1819 N1, also known as Comet Tralles, was an easily visible brilliant comet, approaching an apparent magnitude of 1–2, discovered July 1, 1819 by Johann Georg Tralles in Berlin, Germany. It was the first comet analyzed using polarimetry, by François Arago.

The primary component of is a magnitude 6.47 giant star with a stellar classification of G8 III:. A companion star at an angular separation of 1.437 arcseconds is an A-type main sequence star with a classification of A1 V. It is slightly fainter, with an apparent magnitude of 6.75.

Pi Mensae (π Men), also known as HD 39091, is a yellow dwarf star in the constellation of Mensa. This star has a high proper motion. The apparent magnitude is 5.67, which can be visible to the naked eye in exceptionally dark, clear skies. It is nearly 60 ly away.

HD 128093 is a double star in the constellation Boötes. The brighter component is an F-type main sequence star with a stellar classification of F5V and an apparent magnitude of 6.33. It has a magnitude 11.33 companion at an angular separation of 28.1 along a position angle of 318°.

Rotating ellipsoidal variables are a class of variable star. They are close binary systems whose components are ellipsoidal. They are not eclipsing, but fluctuations in apparent magnitude occur due to changes in the amount of light emitting area visible to the observer. Typical brightness fluctuations do not exceed 0.1 magnitudes.

Psi Hydrae (ψ Hydrae) is a star in the equatorial constellation of Hydra. Based upon an annual parallax shift of 14.09 mas as seen from Earth, it is located around 231 light years away from the Sun. It is faintly visible to the naked eye with an apparent magnitude of 4.97.

Pi Cephei (π Cephei) is a trinary star located in the constellation Cepheus. With a combined apparent magnitude of about 4.4, the system is faintly visible to the naked eye. The inner pair of stars orbits in 1.5 years while the outer companion completes one orbit in about 160 years.

Kronk, G. W. Cometography: A Catalog of Comets, I, Cambridge: Cambridge University Press, 1999, p. 408. The comet brightened steadily as it approached perihelion. By February 18, 1744, it reportedly was as bright as the planet Venus (with an apparent magnitude of -4.6) and at this time displayed a double tail.

NGC 6624 is a globular cluster in the constellation Sagittarius. It was discovered on 24 June 1784 by the astronomer William Herschel. It is given an apparent magnitude of 7.6 to 8.5.It is given a diameter of 6 to 8.5 arcminutes, and class VI with stars magnitude 14 and dimmer.

HD 100307 is a suspected variable star in the constellation of Hydra. Its apparent magnitude is 6.16, but interstellar dust makes it appear 0.346 magnitudes dimmer than it should be. It is located some 340 light-years (104 parsecs) away, based on parallax. HD 100307 is a M-type red giant.

HD 95808 is a double star in the constellation of Crater. Its apparent magnitude is 5.50, but interstellar dust makes it appear 0.11 magnitudes dimmer than it should be. It is located some 340 light-years (104 parsecs) away, based on parallax. HD 95808 is a G-type giant star.

NGC 1992 (also known as PGC 17466) is a lenticular galaxy located in the Columba constellation. It was discovered by John Herschel on November 19, 1835. It is about 473 million light years from the Milky Way, Its apparent magnitude is 14.65 and its size is 1.10 x 0.7 arc minutes.

NGC 1993 (also known as ESO 554-14) is a lenticular galaxy located in the Lepus constellation. It was discovered by John Herschel on February 6, 1835. It is about 143 million light years from the Milky Way, Its apparent magnitude is 13.39 and its size is 1.5 arc minutes.

HD 30963 is a star in the constellation of Eridanus. With an apparent magnitude of 7.23, it cannot be seen with the naked eye. Parallax measurements made by Hipparcos put the star at a distance of around 900 light-years (280 parsecs) away. HD 30963 is a late B-type star.

NGC 7048 is a planetary nebula in the constellation of Cygnus. The bright star to the lower left of the nebula is a magnitude 10.5 star, designated TYC 3589-4652-1. The nebula is slightly brighter along the west and east sides. This planetary nebula has an apparent magnitude of 12.1.

NGC 6522 is a globular cluster in the constellation Sagittarius. It is apparent magnitude 8.3, and diameter 16.4 arc minutes, and class VI with stars 16th magnitude and dimmer. It was discovered by William Herschel on June 24, 1784. It is centered in a region of the sky known as Baade's Window.

The three brightest stars—Alpha, Beta and Nu Fornacis—form a flattened triangle facing south. With an apparent magnitude of 3.91, Alpha Fornacis is the brightest star in Fornax. Six star systems have been found to have exoplanets. The Fornax Dwarf galaxy is a small faint satellite galaxy of the Milky Way.

HD 49798 is binary star in the constellation Puppis about 650 parsecs from Earth. It has an apparent magnitude of 8.3. HD 49798 was discovered in 1964 to be a rare hydrogen-deficient O class subdwarf. This was identified as a binary star, but the companion could not be detected visually or spectrscopically.

Gliese 69 is a star located in the constellation of Cassiopeia. It has an apparent magnitude of 8.40. Parallax measurements by Hipparcos put it at a distance of 44.3 light-years (13.6 parsecs) away. Gliese 69 is a K-type main- sequence star that is smaller and less massive than the Sun.

HD 210434 is a subgiant star in the equatorial constellation of Aquarius. According to the Bortle scale, an apparent magnitude of six means this star is faintly visible to the naked eye from dark rural skies. It is an estimated 630 million years old with 2.4 times the mass of the Sun.

In February 2008, a rotational lightcurve of Begzhigitova at an apparent magnitude of only 17 was obtained from photometric observations at Modra Observatory in the Czech Republic. Lightcurve analysis gave a rotation period of 5.341 hours with a brightness amplitude of 0.3 magnitude (). However a longer period can not be ruled out.

HD 109271 is a star in the constellation of Virgo. With an apparent magnitude of 8.05, it cannot be seen with the naked eye. Parallax measurements made by Gaia put the star at a distance of 182 light-years (56.0 parsecs) away. HD 109271 is a typical G-type main-sequence star.

The two stars passed their periastron in 1920. Finally, it is thought that Epsilon Equulei A may be, in turn, a spectroscopic binary. The orbital period of the latter would be 2.03133 days. Approximately 10 arcseconds away from A and B is Epsilon Equulei C (HIP 103571), with an apparent magnitude of 7.35.

V Puppis (V Pup) is a star system in the constellation Puppis. Its apparent magnitude is 4.41. There is a binary star system at the center with a B1 dwarf orbiting a B3 subgiant star. They have an orbital period of 1.45 days and a distance of only 15 solar radii apart.

QZ Puppis (QZ Pup, b Pup) is a class B2.5V (blue main-sequence) star in the constellation Puppis. Its apparent magnitude is 4.49 and it is approximately 650 light years away based on parallax. It is an ellipsoidal variable, ranging from 4.54 to 4.47 magnitude, with a reported period of 1.1 days.

HD 61330 (f Puppis) is a class B8IV (blue subgiant) star in the constellation Puppis. Its apparent magnitude is 4.53 and it is approximately 360 light years away based on parallax. It is a multiple star, with a secondary component C, with magnitude 6.07 in an 81-year orbit with eccentricity 0.64.

HD 213429 is a spectroscopic binary system in the equatorial constellation of Aquarius. It has a combined apparent magnitude of 6.16 and is located around 83 light years away. The pair orbit each other with a period of 631 days, at an average separation of 1.74 AU and an eccentricity of 0.38.

17 December 2014. Retrieved 17 July 2016. It has a surface temperature of 5394 K and is 10.6 billion years old. In comparison, the Sun is 4.6 billion years old and has a surface temperature of 5778 K. The star's apparent magnitude, or how bright it appears from Earth's perspective, is 5.47.

' is an Apollo near-Earth asteroid around in diameter. It is the largest asteroid known to have passed closer than the Moon. On 17 September 1918 the asteroid passed from Earth with a peak apparent magnitude of around 8.4. The 1918 close approach distance is known with an accuracy of roughly ± 200 km.

31P/Schwassmann–Wachmann, also known as Schwassmann–Wachmann 2, is a periodic comet in the Solar System. It was discovered on January 17, 1929, at an apparent magnitude of 11. (Cometography Home Page) The comet has been seen at every apparition. The comet nucleus is estimated to be 6.2 kilometers in diameter.

33 Arietis (abbreviated 33 Ari) is a binary star in the northern constellation of Aries. 33 Arietis is the Flamsteed designation. The combined apparent magnitude of 5.33 is bright enough to be seen with the naked eye. Based upon an annual parallax shift of 14.09 mas, the distance to this system is approximately .

The much more distant third companion is an orange (class K) twelfth magnitude star, and only two thirds as massive. The two main stars together appear with a spectral type of A0 IV. As seen from Earth, the entire triple star system of Delta Cygni shines at a combined apparent magnitude of 2.87.

Theta1 Orionis A (θ1 Ori A) is a variable trinary star in the constellation Orion. Its apparent magnitude range is 6.72 to 7.65 with a period of 65.432 days. It is one of the main stars in The Trapezium in Orion, along with B, C, and D, as well as the fainter E.

HD 186302 (also designated HIP 97507) is a star in the constellation of Pavo. It is about away from Earth, with an apparent magnitude of 8.76. It was identified in November 2018 as a potential solar sibling to the Sun. It is very similar to the Sun; the Sun is a G2V star.

67 Ophiuchi (67 Oph) is a class B5 Ib (blue supergiant) star in the constellation Ophiuchus. Its apparent magnitude is 3.93 and it is approximately 1200 light years away based on parallax. It is considered to be a member of the open cluster Collinder 359 (Melotte 186). 67 Oph has four companions.

T Antliae (also abbreviated T Ant) is a Classical Cepheid variable star that is between 10 and 12,000 light-years away from the Sun in the constellation of Antlia. A yellow-white supergiant with a spectral type of F6Iab, it ranges between apparent magnitude 8.86 and 9.76 over a period of 5.89820 days.

TT Corvi (TT Crv) is a semiregular variable star in the constellation Corvus. It is a red giant of spectral type M3III and average apparent magnitude 6.48 around 923 light years distant. It shines with a luminosity approximately 993 times that of the Sun and has a surface temperature of 3630 K.

The inner spectroscopic binary consists of two F-type stars, a subgiant and a main-sequence star. There is a companion star which is a white A-type main- sequence star, with an apparent magnitude of 5.76. It is separated 0.361 arcseconds from the primary and has an orbital period of 16.651 years.

Kidger, M. Comet Hale-Bopp Light Curve, NASA Jet Propulsion Laboratory, accessed 17-11-08 Its apparent magnitude may have reached as high as -7, leading it to be classified among what are called the "Great Comets". This comet is noted especially for developing a 'fan' of six tails after reaching its perihelion.

It is classified as an S-type asteroid and has an estimated size of 154.34 km. The spectrum of 354 Eleonora reveals the strong presence of the mineral olivine, a relatively rarity in the asteroid belt. During favorable oppositions, such as in 1968 and 2010, Eleonora can reach an apparent magnitude of +9.31.

NGC 6717 is a globular cluster in the constellation Sagittarius, which was discovered by William Herschel on August 7, 1784. It is located of 7100 parsecs away from Earth. The globular cluster, which has an apparent magnitude of 9.28 and diameter of 9.9 arcminutes. Is located just south of the star ν2 Sagittarii.

At a distance of about 840 light-years, Zeta Cephei has an apparent magnitude (m) of 3.4 and an absolute magnitude (M) of -4.7. The star has a metallicity approximately 1.6 times that of the Sun; i.e., it contains 1.6 times as much heavy-element material as the Sun. Hekker et al.

HD 21749 is a star that is approximately 68% the mass of and 76% the radius of the Sun. It has a surface temperature of 4571 K. In comparison, the Sun has a surface temperature of 5778 K. The star's apparent magnitude, or how bright it appears from Earth's perspective, is 8.143.

Redshift information is also important in separating the background source population from other galaxies in the foreground, or those associated with the mass responsible for the lensing. With no redshift information, the foreground and background populations can be split by an apparent magnitude or a color cut, but this is much less accurate.

Alpha Vulpeculae (α Vulpeculae, abbreviated Alpha Vul, α Vul), officially named Anser , is the brightest star in the constellation of Vulpecula. It is approximately 297 light-years from Earth. It forms a wide optical binary with 8 Vulpeculae. Alpha Vulpeculae is a red giant of spectral class M1 and has apparent magnitude +4.4.

NGC 1986 (also known as ESO 56-SC134) is an open cluster which is located in the Mensa constellation which is part of the Large Magellanic Cloud. It was discovered by James Dunlop on September 27, 1826. It has an apparent magnitude of 11.31 and its size is 2.80 by 2.40 arc minutes.

Supernova 1945A is the only supernova that has been detected within NGC 5195. The supernova was found 10″ northwest of the nucleus on April 6, 1945 by Milton L. Humason using the telescope at Mount Wilson Observatory. The supernova, classified as a Type I supernova, reached a peak apparent magnitude of 14.0.

VB 10 has an extremely low luminosity with a baseline absolute magnitude of nearly 19 and an apparent magnitude of 17.3 (somewhat variable), making it very difficult to see. Mathematical formulae for calculating apparent magnitude show that, if VB 10 occupied the place of the Sun, it would shine on Earth's sky at a magnitude of −12.87—approximately the same magnitude of that of the full moon. Later researchers also noted that its mass, at 0.08 solar mass (), is right at the lower limit needed to create internal pressures and temperatures high enough to initiate nuclear fusion and actually be a star rather than a brown dwarf. At the time of its discovery it was the lowest-mass star known.

This small dim asteroid approached Earth in opposition, having an elongation from the Sun of over 160 degrees from mid November 2015. However, due to its absolute magnitude even though it had a very low phase angle during the approach it was too dim for contemporary telescopes to spot it so early, as it was significantly fainter than apparent magnitude 23. However it got brighter as it approached and a few weeks later, on 6 December 2015 it was spotted by Pan- STARRS at an apparent magnitude of 21.5 using a Ritchey–Chrétien telescope. On 15 December 2015 at 13:52 UT, the asteroid passed from the Earth and three and a half hours later at 17:17 UT passed from the Moon.

UGC 9405 (also known as PGC 52142) is a faint dwarf irregular galaxy situated in the constellation of Ursa Major. It is the member of the M101 Group, a group containing the several galaxies orbiting the largest, Pinwheel Galaxy (M101). UGC 9405 is also the faintest member of M101 Group, with apparent magnitude of 17.

Gliese 282 is a triple star system in the equatorial constellation of Monoceros. At a distance of 36 light years, this star has an apparent magnitude of 7.26 when viewed from Earth. It is not visible to the naked eye. The Gl 282AB star system is composed of two K- type main-sequence stars.

The star's metallicity, which is measured by iron content, is placed roughly at [Fe/H] = 0, similar to that of the Sun. Also, the star's estimated effective temperature is 5826 K, slightly warmer than the Sun. Gloas has an apparent magnitude of 10.42, making it invisible to the unaided eye as seen from Earth.

The asteroid was last observed on 20 January 2018 at apparent magnitude 24 by T14 Mauna Kea. As the asteroid is becoming very faint, further observations during this approach are difficult. The next good chance to recover the asteroid will be between March and late April 2022 when the asteroid will pass about from Earth.

Most of these stars lie in Hydra. The three brightest stars—Delta, Alpha and Gamma Crateris—form a triangle located near the brighter star Nu Hydrae in Hydra. Within the constellation's borders, there are 33 stars brighter than or equal to apparent magnitude 6.5. Delta Crateris is the brightest star in Crater at magnitude 3.6.

The tertiary is not visible in telescopes. AA Ceti is an eclipsing variable star; the tertiary star passes in front of the primary and causes the system's apparent magnitude to decrease by 0.5 magnitudes. UV Ceti is an unusual binary variable star. 8.7 light-years from Earth, the system consists of two red dwarfs.

It was discovered on 24 January 2011, by a team of astronomers at Pan-STARRS, the Panoramic Survey Telescope and Rapid Response System at Haleakala Observatory on Hawaii, United States. The discovery was made using a 1.8-meter Ritchey–Chrétien telescope. At the time of discovery, the object had an apparent magnitude of 22.

HD 120987 (y Centauri or y Cen) is a star system located in the constellation Centaurus. HD 120987 is a quintuple star system located 50 pc (163 light years) from the Sun. The system has an apparent magnitude of 5.565. Based on the system's parallax, it is located some 172 light-years (52 parsecs) away.

NGC 1929 (also known as ESO 56-EN107) is an open cluster associated with the emission nebula located within the N44 nebula in the Dorado constellation and part of the Large Magellanic Cloud. It was discovered by James Dunlop on August 3 1826. Its apparent magnitude is 14.0, and its size is 0.8 arc minutes.

HD 88836 is a double star in the southern constellation of Antlia. With an apparent magnitude of 6.35, it is faintly visible to the naked eye from dark skies. The brighter component is a giant star with a stellar classification of G8III. It is radiating energy at a luminosity 58 times that of the Sun.

HD 64440, also known as a Puppis, is a spectroscopic binary star in the constellation Puppis. Its apparent magnitude is 3.71. Located around distant, the primary is a bright giant of spectral type K1.5II and the secondary is an early A-type star. They orbit with a period just under 7 years and eccentricity 0.38.

HD 220766 is a double star in the equatorial constellation of Aquarius. The primary is a K-type giant star with a stellar classification of K0III and an apparent magnitude of 6.44. It has a faint, magnitude 12 companion, located at an angular separation of 5.0″ along a position angle of 132° (as of 1933).

It crossed the celestial equator on 5 May 2015 and became easiest to see from the Northern Hemisphere. Even right after perihelion when it was in the constellation of Gemini, it only brightened to about apparent magnitude 12, and required a telescope to be seen. , the comet had a total magnitude of about 20.

Iota Cassiopeiae is known to be a quintuple star system. The brightest star system, ι Cassiopeiae A, contains a white-colored A-type main-sequence star with a mean apparent magnitude of +4.61. The primary component is a tighter binary star system itself. The two stars themselves were resolved by adaptive optics, revealing two stars.

Theta Muscae (θ Muscae) is a multiple star system in the southern constellation Musca ("the Fly") with an apparent magnitude of 5.5. It is the second-brightest Wolf–Rayet star in the sky, although much of the visual brightness comes from the massive companions and it is not one of the closest of its type.

Zeta Cassiopeiae (ζ Cassiopeiae, abbreviated Zet Cas, ζ Cas), officially named Fulu , is a variable star in the constellation of Cassiopeia. It has a blue- white hue and is classified as a B-type subgiant with an apparent magnitude of +3.66. Based upon parallax measurements, it is approximately 590 light-years from the Sun.

' is a near-Earth asteroid of the Aten group, approximately in diameter. On 3 June 2014 around 17:38 UT (± 3 hours), it is crudely estimated to have passed about from Earth. The asteroid was discovered on 2 June 2014 by the Mount Lemmon Survey at an apparent magnitude of 21 using a reflecting telescope.

HD 56577 or 145 Canis Majoris is a single K giant or supergiant star in the southern constellation of Canis Major. Its apparent magnitude is 4.84. It has a visual companion. It is often referred to as The Winter Albireo as it is quite similar in appearance to the well-known double Albireo in Cygnus.

HD 73390, also called e1 Carinae, is a binary star system in the constellation Carina. It is approximately 870 light years from Earth. The primary is a blue- white B-type main sequence dwarf with an apparent magnitude of +5.27. It displays an infrared excess and is a candidate host of an orbiting debris disk.

WR 46 (DI Crucis) is a Wolf-Rayet star in the constellation of the Southern Cross of apparent magnitude +10.8. It is located at 55 arcmin north of Theta2 Crucis. The star is a member of the distant stellar association OB4 Cru, and is around 2,900 parsecs or 9,300 light years from the Solar System.

V433 Aurigae is a variable star in the constellation Auriga. It is a Slowly pulsating B star (SPB) that ranges from apparent magnitude 6.02 to 6.06 over 4.6 days. Located around 324 parsecs distant, it shines with a luminosity approximately 322 times that of the Sun and has a surface temperature of 7400 K.

The apparent magnitude of the eclipsing binary varies from 5.65 to 6.05 with a period of 4.4672 days. Combined, they appear to have a spectral type of A2IV. The binary has a dimmer (magnitude 9.7 according to Norton, or 10.5 by SIMBAD) companion of 0.8 orbiting with a period of about 86 580 years.

AZ Phoenicis (HR 239) is a variable star in the constellation of Phoenix. It has an average visual apparent magnitude of 6.47, so it is at the limit of naked eye visibility. From parallax measurements by the Gaia spacecraft, it is located at a distance of from Earth. Its absolute magnitude is calculated at 1.65.

BP Circini is a star in the constellation Circinus. A Cepheid variable, its apparent magnitude ranges from 7.37 to 7.71 over 2.39810 days. It is a yellow- white supergiant of spectral type F2 or F3II. A spectroscopic binary, it has a 4.7 solar mass () companion that is a blue-white star of spectral type B6.

NGC 5634 is a globular cluster in the constellation Virgo (constellation), located about 82,200 light years (25.2 kiloparsecs) away. NGC 5634 has an apparent magnitude of about 10 and a diameter of 4 or 5 arcminutes. Its Shapley–Sawyer Concentration Class is IV, meaning the cluster shows intermediate rich concentrations. with stars 19th magnitude.

HD 211392 is a suspected variable star in the equatorial constellation of Aquarius, positioned about 370 light-years away. With an apparent magnitude close to six, according to the Bortle scale it is just visible to the naked eye from dark, rural skies. It is a giant star with a stellar classification of K3III.

' is a kilometer-length near-Earth asteroid and potentially hazardous asteroid of the Apollo group. It was discovered by LINEAR on 13 January 1999. On 7 August 2027, this asteroid will pass at about of the Earth. During the close approach, it should peak at about apparent magnitude 7.3, and will be visible in binoculars.

HD 131399 is a star system in the constellation of Centaurus. Based on the system's electromagnetic spectrum, it is located around 351 light-years (107.9 parsecs) away. The total apparent magnitude is 7.07, but because of interstellar dust between it and the Earth, it appears 0.22 ± 0.09 magnitudes dimmer than it should be.See Interstellar extinction.

NGC 5023 is an edge-on spiral galaxy located in the constellation Canes Venatici. It is considered a member of the M51 Group although it is actually relatively isolated from other galaxies. It is approximately 15 kiloparsecs (49,000 light-years) across and contains more than 200 stars with an apparent magnitude of greater than 23.5.

The star system has a combined apparent magnitude of 2.9. The system is 39 light years away from the Sun. Gamma Virginis is 2.8 degrees north of the ecliptic, so it can be occulted by the Moon and (rarely) by planets. In June 2011 Saturn passed a quarter of a degree south of Porrima.

AK Pictoris is a star system in the constellation Pictor. Its combined apparent magnitude is 6.182. Based on the system's parallax, it is located 69 light-years (21.3 parsecs) away. AK Pictoris is a member of the AB Doradus moving group, a group of stars with similar motions that are thought to be associated.

Tau1 Eridani, Latinized from τ1 Eridani, is a binary star system in the constellation Eridanus. It has an apparent magnitude of 4.46, making it visible to the naked eye in suitably dark conditions. This a spectroscopic binary with an orbital period of 958 days. It is located about 46 light years from the Earth.

This is particularly odd for a star as old as HD 164922. Its luminosity () is 70% of the solar luminosity. The star's apparent magnitude, or how bright it appears from Earth's perspective, is 7.01. Therefore, HD 164922 is too dim to be seen with the naked eye, but can be viewed using good binoculars.

Theta Tauri B is the dimmer constituent. Its primary component, Theta Tauri Ba, is an orange K-type giant with an apparent magnitude of +3.84. The secondary, Theta Tauri Bb, is of the 7th-magnitude. It has a mass of and orbits the primary every 16.26 years on a fairly eccentric (at 0.570) orbit.

Delta Ursae Majoris (δ Ursae Majoris, abbreviated Delta UMa, δ UMa), formally named Megrez , is a star in the northern circumpolar constellation of Ursa Major. With an apparent magnitude of +3.3, it is the dimmest of the seven stars in the Big Dipper asterism. Parallax measurements yield a distance estimate of from the Sun.

Delta Herculis (δ Herculis, abbreviated Delta Her, δ Her) is a multiple star system in the constellation of Hercules. Its light produces to us apparent magnitude 3.12, as such the third-brightest star in the large, fairly dim constellation. Based on parallax measurement taken during the Hipparcos mission, it is approximately from the Sun.

16 Tauri is a blue-white B-type subgiant with an apparent magnitude of +5.45. It is approximately 430 light years from the Sun; about the same distance as the Pleiades. The interstellar extinction of this star is fairly small at 0.05 magnitudes. The projected rotational velocity of the equator is 185 km/s.

Kappa Trianguli Australis (κ Trianguli Australis) is a star in the constellation Triangulum Australe. Kappa Trianguli Australis is a yellow G-type supergiant with an apparent magnitude of +5.08. It is around 1,200 light years from Earth. It is not generally listed as a variable star but Hipparcos photometry showed small amplitude brightness changes.

NGC 1983 (also known as ESO 56-SC133) is an open cluster associated with an emission nebula which is located in the Dorado constellation and part of the Large Magellanic Cloud. It was discovered by John Herschel on 11 November 1836. It has an apparent magnitude of 9.9 and its size is 1.0 arc minutes.

The white dwarf sucks matter from the other star onto an accretion disc and periodically erupts, reaching apparent magnitude 8.4 in superoutbursts, 9.0 in normal outbursts and remaining at magnitude 14.4 when quiet. Normal outbursts occur every 27.3 days and last for 1.4 days, while superoutbursts happen 179 days and last for 12.6 days.

V744 Centauri, is a semi-regular variable pulsating star in the constellation Centaurus. Located 3 degrees north north east of Epsilon Centauri, It ranges from apparent magnitude 5.1 to 6.7 over 90 days. It is unusual in that it is a red star with a high proper motion (greater than 50 milliarcseconds a year).

Kepler-432 is a binary star system composed of a K-type giant star (Kepler-432 A) and a red dwarf star (Kepler-432 B). The apparent magnitude of the system, or how bright it appears from Earth's perspective, is about 15.8. Therefore, it is too dim to be seen with the naked eye.

In the Washington Double Star Catalog HR 8768 has a faint optical companion star with an apparent magnitude of 9.88, from HR 8768. The separation has decreased from when it was discovered as a double in 1828. The two stars share the same Hipparcos identifier HIP 113802, and have very similar parallaxes and proper motions.

HD 171028 is a yellow main-sequence star in the constellation of Ophiuchus. The apparent magnitude is +8.31, visible in good binoculars. Unlike most planet-harboring stars, it does not have a Hipparcos number, though the distance was estimated at 90±7.8 parsecs. In the summer of 2007, a planet was discovered orbiting this star.

M9 has an apparent magnitude of 7.9, an angular size of 9.3′, and can be viewed with a small telescope. It is one of the nearer globular clusters to the center of the Milky Way Galaxy with a separation of around 5,500 light-years from the Galactic Core. Its distance from Earth is 25,800 light-years.

X Crucis is a classical Cepheid variable star in the southern constellation of Crux. X Crucis is a pulsating variable star with am extremely regular amplitude and period. Its apparent magnitude varies from 8.1 to 8.7 every 6.22 days. This type of variable is known as a Cepheid after δ Cephei, the first example to be discovered.

X Sagittarii is a bright giant Cepheid variable star in the constellation Sagittarius. This variable star changes in apparent magnitude from 4.90 to 4.20 magnitude with a period of 7.01 days. Its change in brightness is accompanied by a change in spectral classification, from G2 to F5. It is approximately 990 light years away based on parallax.

10 Per is the bright star below and right of the Double Cluster 10 Persei is a blue supergiant star in the constellation Perseus. Its apparent magnitude is 6.26 although it is slightly variable. 10 Persei is located around distant in the Perseus OB1 stellar association. It lies close to the Double Cluster and is considered a cluster member.

Delta Pictoris (δ Pic) is a class B3III (blue giant) star in the constellation Pictor. Its apparent magnitude is 4.72 and it is approximately 1300 light years away based on parallax. It is a β Lyrae variable, a type of eclipsing binary, which ranges in brightness from 4.90 to 4.65 magnitude with a period of 1.67 days.

Omicron Velorum (ο Vel, ο Velorum) is a star in the constellation Vela. It is the brightest member of the loose naked eye open cluster IC 2391, also known as the ο Velorum Cluster. Omicron Velorum is a blue-white B-type subgiant with a mean apparent magnitude of +3.60. It is approximately 495 light years from Earth.

U Coronae Borealis (U CrB) is an Algol-type eclipsing binary star system in the constellation Corona Borealis. Its apparent magnitude varies between 7.66 and 8.79 over a period of 3.45 days The component stars are a blue-white main sequence star of spectral type B6V and a cooler yellow-white subgiant star of spectral type F8III-IV.

In Bayer's 1603 work Uranometria, Procyon is located on the dog's belly, and Gomeisa on its neck. Gamma, Epsilon and Eta Canis Minoris lie nearby, marking the dog's neck, crown and chest respectively. Although it has an apparent magnitude of 4.34, Gamma Canis Minoris is an orange K-type giant of spectral class K3-III C, which lies away.

The primary component has a spectral type of M4.5 and a red apparent magnitude of 14.2. Both components seem to be accreting mass from their stellar disks, as shown by their emission lines. The four stars have a total mass of only 26% of the Sun, making it the quadruple star system with the lowest mass known.

Y Sagittarii is a variable star in the constellation of Sagittarius. It is a Cepheid variable in apparent magnitude +5.77. This star is the third-brightest in this constellation after X Sagittarii and W Sagittarii. The measure of its parallax by Hubble Space Telescope puts Y Sagittarii to 1,293 light-years away from the Solar System.

HD 205765 is a star in the equatorial constellation of Aquarius. It is an A-type main sequence star with an apparent magnitude of 6.2, which, according to the Bortle scale, makes it faintly visible to the naked eye from dark rural skies. This star is spinning rapidly with a projected rotational velocity of 172 km/s.

MX Puppis (MX Pup) is a class B1.5IV (blue subgiant) star in the constellation Puppis. Its apparent magnitude varies irregularly between magnitude 4.6 and 4.9 and it is classified as a Gamma Cassiopeiae variable. It is approximately 930 light years away based on parallax. It is a γ Cas variable, ranging from 4.92 to 4.60 magnitude.

It has a temperature of 15900 K and its cooling age is 175 million years. In comparison, the Sun is 4.6 billion years old and has a surface temperature of 5778 K. The star's apparent magnitude, or how bright it appears from Earth's perspective, is 17. Therefore, it is far too dim to be seen with the naked eye.

Kepler-11 has six known planets in orbit: Kepler-11b, Kepler-11c, Kepler-11d, Kepler-11e, Kepler-11f, and Kepler-11g. Kepler-11's five inner planets orbit closely to their host star, and their orbits would fit within that of Mercury's. With an apparent magnitude of 14.2, Kepler-11 cannot be seen with the naked eye.

The close approach distance is now known with an accuracy of roughly ± 1000 km. This is the largest asteroid to pass closer than the Moon this year and possibly the largest since in November 2011. The asteroid makes close approaches to Mercury, Venus, Earth, and Mars. It will be brighter than apparent magnitude 24 until 18 July 2020.

PAGEOS data has been tracked 11 times. PAGEOS' predecessors in satellite triangulation were the balloons Echo 1 (1960, 30 m) and Echo 2 (1964, 40 m) which were also used for passive telecommunication. Their apparent magnitude (brightness) was 1 mag, that of Pageos 2 mag (like Polaris) due to its higher orbit. Pageos could therefore be observed simultaneously e.g.

When it comes to opposition in May 2020, when it is still 3.5 AU from the Sun, it will likely have an apparent magnitude around 16.9. But during the 2021 perihelion passage the comet will be on the opposite side of the Sun as the Earth. The comet is not known for bright outbursts of activity.

HU Delphini, also known as Gliese 791.2, is a star system in the constellation of Delphinus. Its apparent magnitude is 13.07. With a trigonometric parallax of 113.4 ± 0.2 mas, it is about 28.76 light-years (8.82 parsecs) away from the Solar System. HU Delphini is a binary star with a well-defined period of 538.6 days.

Gliese 1214 is a dim M4.5 red dwarf in the constellation Ophiuchus with an apparent magnitude of 14.7. It is located at a distance of approximately 47 light years from Earth. The star is about one-fifth the radius of the Sun with a surface temperature estimated to be . Its luminosity is only 0.33% that of the Sun.

Lambda Pegasi (λ Peg, λ Pegasi) is a fourth-magnitude star in the constellation Pegasus. λ Pegasi is a yellow giant with stellar classification G8II-III. With a mass of and radius that is , the star boasts a bolometric luminosity that is roughly . Its apparent magnitude was calibrated in 1983 at 3.96, yielding an absolute magnitude of -1.45.

HD 147513 (62 G. Scorpii) is a star in the southern constellation of Scorpius. It was first catalogued by Italian astronomer Piazzi in his star catalogue as "XVI 55".Piazzi, G., (ed.) the Palermo Catalogue, 1814. With an apparent magnitude of 5.38, according to the Bortle scale it is visible to the naked eye from suburban skies.

MY Apodis, also known as L 19-2 or WD 1425-811, is a pulsating white dwarf or ZZ Ceti star located in the far southern constellation Apus. Shining with an apparent magnitude of 13.75, it is white dwarf 0.71 times as massive as the Sun with a spectral type DA4.1 and surface temperature of 12330 K.

The brighter component has a stellar classification of B9 V and an apparent magnitude 5.90, while the second member is a B9.5 V star with a magnitude of 6.46. The pair have an angular separation of 0.091 arcseconds with an estimated orbital period of 59.32 years. They are about 3.89 and 3.45 times as massive as the Sun.

Gliese 638 is a main sequence star in the constellation of Hercules. It is located about 31.9 light years from the Earth. This is a suspected variable star with a measured apparent magnitude that ranges from 8.09-8.11. As a K-class star, it has a lower mass than the Sun, and consequently is less luminous.

52 Arietis (abbreviated 52 Ari) is a triple star system in the northern constellation of Aries. 52 Arietis is the Flamsteed designation. The combined apparent magnitude is +5.46, which is bright enough to be faintly visible to the naked eye. Based upon an annual parallax shift of 6.05 mas, the system is roughly distant from the Earth.

The brighter member of this system has an apparent magnitude of 4.81. It is an A-type main sequence star with a stellar classification of A0 V. This star is spinning rapidly with a projected rotational velocity of 1 km/s. The fainter companion is a magnitude 7.43 star at an angular separation of 0.840 arcseconds.

63 Andromedae (abbreviated 63 And) is an Alpha2 Canum Venaticorum (α2 CVn) variable star in the constellation Andromeda. Its variable star designation is PZ Andromedae. With an apparent magnitude of about 5.6, it is bright enough to be seen by naked eye. Based upon an annual parallax shift of , it is located 413 light years away.

44 Boötis or i Boötis is a triple star system in the constellation Boötes. It is approximately 41.6 light years from Earth. The primary component, 44 Boötis A, is a yellow-white G-type main sequence dwarf with a mean apparent magnitude of +4.83. The companion component, 44 Boötis B, is a W Ursae Majoris variable spectroscopic binary.

Sigma Boötis (σ Boo, σ Boötis) is a star in the constellation Boötes. Sigma Boötis is a yellow-white F-type main sequence dwarf with an apparent magnitude of +4.47. It is approximately 50.4 light years from Earth. In Chinese, (), meaning Celestial Lance, refers to an asterism consisting of σ Boötis, ε Boötis and ρ Boötis.

From the population of about 100 stars, this open cluster features a prominent yellow giant with the apparent magnitude +7.9 and spectral type G0 as its brightest member. This corresponds to an absolute magnitude of -1.5, or a luminosity of 900 Suns. For comparison, the Sun would appear as a faint magnitude +15.3 star from the distance of M38.

The structure is now classed as a bipolar planetary nebula (BPNe). Distance to M76 is currently estimated as 780 parsecs or 2,500 light years, making the average dimensions about 0.378 pc. (1.23 ly.) across. The total nebula shines at the apparent magnitude of +10.1 with its central star or planetary nebula nucleus (PNN) at +15.9v (16.1B) magnitude.

In astronomy, limiting magnitude is the faintest apparent magnitude of a celestial body that is detectable or detected by a given instrument. (retrieved Jan 28 2016) In some cases, limiting magnitude refers to the upper threshold of detection. In more formal uses, limiting magnitude is specified along with the strength of the signal (e.g., "10th magnitude at 20 sigma").

LHS 6343 is a star system in the northern constellation of Lyra. It appears exceedingly faint with a combined apparent magnitude of 13.435. Based on its stellar properties, the system is thought to be about 119.4 light-years (36.6 parsecs) away. LHS 6343 is a binary star with two red dwarfs, designated LHS 6343 A and B, respectively.

During closest approach to Earth the asteroid reached about apparent magnitude 10, which is much too faint to be seen by the naked eye. Even at peak brightness, the asteroid was a challenging target for amateur astronomers with small telescopes, best seen in the Northern hemisphere. The glare from an 80% waning gibbous Moon also hindered observations.

HD 88366 (S Carinae) is a star in the constellation Carina. HD 88366 is an M-type red giant with a mean apparent magnitude of +6.94. It is approximately 1,620 light years from Earth. It is classified as a Mira type variable star and its brightness varies between magnitude +4.5 and +10.0 with a period of 149.49 days.

The apparent magnitude of Venus is as bright as −7.7. The Earth and the Moon are also very prominent, their apparent magnitudes being about −5 and −1.2, respectively. The maximum apparent distance between the Earth and the Moon is about 15′. All other planets are visible just as they are on Earth, but somewhat less bright at opposition.

One supernova has been observed in IC 5201, SN 1978G. It was first reported by J. C. Blades, of the Anglo-Australian Observatory, and R. E. Griffiths, of Center for Astrophysics, on November 24.5 UTC, with apparent magnitude at discovery 13.5. The supernova was detected in its early stages. Spectroscopic observations revealed it was a type II supernova.

Similarly, the magnitude of each maximum and minimum varies. The mean apparent magnitude is 11.6, with a mean maximum magnitude of 9.9. The brightest recorded maxima are at magnitude 9.0, and the faintest minima at magnitude 15.0. The rise to maximum brightness is faster than the fall to minimum, taking on average 40% of the period.

1 Ceti is a star in the constellation of Cetus. With an apparent magnitude of about 6.2, the star is barely visible to the naked eye (see Bortle scale). Parallax estimates put it at a distance of about away from the Earth. It is moving further from the Sun with a heliocentric radial velocity of 4 km/s.

NGC 1277 is a lenticular galaxy in the constellation of Perseus. It is a member of the Perseus Cluster of galaxies and is located approximately 73 Mpc (megaparsecs) or 220 million light years from the Milky Way. It has an apparent magnitude of about 14.7. It was discovered on December 4, 1875 by Lawrence Parsons, 4th Earl of Rosse.

HD 91496 (HR 4142) is a giant star in the constellation Carina, with an apparent magnitude is 4.92 and an MK spectral class of K4/5 III. It has been suspected of varying in brightness, but this has not been confirmed. HD 91496 has a faint companion, six magnitudes fainter and away. It is a distant background star.

RX Leporis (RX Lep) is a star in the constellation of Lepus. It is a red giant and is a semi-regular pulsating star. It has an apparent magnitude that varies from about 5 to 7.4. At its brightest it is dimly visible to the naked eye, and at its dimmest can be located with binoculars.

In 2008, NASA considered this asteroid as a possible target for a manned mission (Artemis 2) using the Orion spacecraft, prior to a projected 2030 push to Mars.Into the Beyond: A Crewed Mission to a Near-Earth Object – text slides Those plans were since abandoned. will be observable in April 2028 at an apparent magnitude of 19.

NGC 1755 (also known as ESO 56-SC28) is an open star cluster in the Large Magellanic Cloud in the Dorado constellation, It is about 120 light years across and due to its size could be a globular cluster. It has a diameter of 2.6′ and an apparent magnitude of 9.9. It was discovered by James Dunlop in 1826.

IC 4499 is a loose globular cluster in the medium-far galactic halo; its apparent magnitude is 10.6. The galaxies in the constellation are faint. IC 4633 is a very faint spiral galaxy surrounded by a vast amount of Milky Way line-of-sight integrated flux nebulae—large faint clouds thought to be lit by large numbers of stars.

Using observations with the Hubble Space Telescope, the discovery of a satellite of was reported in IAUC 8812 on 22 February 2007. The object was measured with a separation of 0.22 arcsec and an apparent magnitude difference of 5.0. , attempts to recover the satellite have failed. The unrecovered satellite is estimated to be about in diameter.

' is an Amor near-Earth asteroid. It was discovered on 5 December 2010 by the Catalina Sky Survey at an apparent magnitude of 19.7 using a Schmidt–Cassegrain telescope. Three precovery images are known from 1 July 1995. With an observation arc of 16 years, the orbit is well determined with an orbital uncertainty of 0.

Chandra Tempel 1 is not a bright comet; its brightest apparent magnitude since discovery has been 11, far below naked-eye visibility. Its nucleus measures . Measurements taken by the Hubble Space Telescope in visible light and the Spitzer Space Telescope in infrared light suggest a low albedo of only 4%. A two-day rotation rate was also determined.

Three stars comprise a small triangle that marks the head. The apex is marked by Meissa (Lambda Orionis), a hot blue giant of spectral type O8 III and apparent magnitude 3.54, which lies some 1100 light years distant. Phi-1 and Phi-2 Orionis make up the base. Also nearby is the very young star FU Orionis.

With an apparent magnitude of 2.59, Gamma Corvi—also known as Gienah—is the brightest star in the constellation. It is an aging blue giant around four times as massive as the Sun. The young star Eta Corvi has been found to have two debris disks. Three star systems have exoplanets, and a fourth planetary system is unconfirmed.

HD 100777 is an orange subgiant star located approximately 162 light years away in the constellation Leo. The apparent magnitude is 8.42 and absolute magnitude is 4.81. It is also called HIP 56572. The survey in 2015 have ruled out the existence of any additional stellar companions at projected distances from 18 to 369 astronomical units.

Gamma2 Fornacis (γ2 For) is a star in the constellation Fornax, with an apparent magnitude of 5.4. It is an A1 main sequence star 2.4 times as massive as the Sun and 120 times as luminous. Gamma1 Fornacis is a 6th magnitude star four degrees to the north. γ2 Fornacis is about from Earth and is receding at .

Alpha Coronae Australis belongs to the spectral class A2Va, making it an A-type star like Vega. Like the latter, it has excess infrared radiation, which indicates it may be ringed by a disk of dust. It has an apparent magnitude of +4.10. The star's mass and radius are estimated at 2.3 times the Sun's mass and radius.

The primary member, Nu Capricorni A, is a blue-white hued B-type main sequence or subgiant star with an apparent magnitude of +4.77. Its companion, Nu Capricorni B, is a magnitude 11.8 star at an angular separation of 54.1 arcseconds from the primary. Gaia Data Release 2 shows the companion to be much further away from Earth.

The brightness of a star, as seen from Earth, is measured with a standardized, logarithmic scale. This apparent magnitude is a numerical value that decreases in value with increasing brightness of the star. The faintest stars visible to the unaided eye are sixth magnitude, while the brightest in the night sky, Sirius, is of magnitude −1.46.

Sigma Sagittarii (σ Sagittarii, abbreviated Sigma Sgr, σ Sgr), formally named Nunki , is the second-brightest star in the constellation of Sagittarius. It has an apparent magnitude of +2.05, making it readily visible to the naked eye. The distance to this star, determined using parallax measurements from the Hipparcos astrometry satellite, yields an estimated value of from the Sun.

Nu Scorpii A is the brightest member of the system. It has an apparent magnitude from 4.35, meaning that it can be seen with the naked eye. However, Nu Scorpii AB and CD cannot be resolved using the naked eye, but it can be resolved using a telescope. Nu Scorpii A is itself a triple star system.

Nu Scorpii B is part of the Nu Scorpii AB sub-system and orbits Nu Scorpii A. It has an apparent magnitude of 5.40, but its spectral type is unknown. Nu Scorpii A and B are separated by 1.305 arcseconds; this translates to an orbital period of over 452 years, so no orbital motion has been detected.

DQ Herculis (or Nova Herculis 1934) was a slow, bright nova occurring in Hercules in December 1934. The nova was discovered on 13 December 1934 by J. P. M. Prentice from Stowmarket, Suffolk. It reached peak brightness on 22 December 1934 with an apparent magnitude of 1.5. The nova remained visible to the naked eye for several months.

HD 8673 is a binary star in the northern constellation of Andromeda. It has an apparent magnitude and absolute magnitude of 6.34 and 3.56 respectively. Based upon an annual parallax shift of , the system is located around 123.6 light years away. The system is moving further from the Earth with a heliocentric radial velocity of +19 km/s.

24 Cancri (abbreviated to 24 Cnc) is a triple star system in the constellation Cancer. The system is located about 260 light-years (80 parsecs) away, based on its parallax. The system has a combined apparent magnitude of 6.91. The primary component in the star system is designated 24 Cancri A. It is a F-type giant star.

RR Centauri is a variable star of apparent magnitude maximum +7.29. It is located in the constellation of Centaurus, approximately 320 light years distant from the solar system. The system is a contact binary of the W UMa type - two stars in physical contact whose two components share a gaseous envelope. Its spectral type is A9V or F0V.

HD 66141, also known as HR 3145 and 50 G. Canis Minoris, is star in the constellation Canis Minor. It is an orange K-type giant, approximately 254 light years from Earth. Its apparent magnitude is +4.39. When first catalogued it was in the Puppis constellation and was designated "13 Puppis", but it subsequently migrated to Canis Minor.

At the time the object was at 49 AU from the Sun and had an apparent magnitude of 21.1. The Pan-STARRS-1 survey at the Haleakala Observatory, Hawaii, in the United States also found precovery observations of 2013 FZ27 after 2013 FZ27 was announced and reported them to the Minor Planet Center at a later date.

Orbiting this pair at the much greater separation of 74 arcseconds, is the yellow G-type Delta Sculptoris C, which has an apparent magnitude of +9.4. Vizier catalog entry Vizier catalog entry This system is a candidate member of the AB Doradus moving group, an association of stars with similar ages that share a common heading through space.

Iota Eridani (ι Eri) is a solitary star in the constellation Eridanus. It is visible to the naked eye with an apparent magnitude of 4.11. With an annual parallax shift of 0.02165 arcseconds, it lies at an estimated distance of about 151 light years. This is an evolved red clump giant star with a stellar classification of K0 III.

Iota Virginis (ι Virginis, abbreviated Iota Vir, ι Vir) is a binary star in the constellation of Virgo. Its apparent magnitude is 4.08. Based on its parallax, it is assumed to be relatively nearby, at 72.5 light-years (22.24 parsecs). Its two components are designated Iota Virginis A (officially named Syrma , the traditional name for the system) and B.

Merope is a blue-white B-type subgiant with a mean apparent magnitude of +4.14. Richard Hinckley Allen described the star as lucid white and violet.Merope, Star Names and their Meanings, Richard Hinckley Allen, Dover Publications, 1963, p. 407. It has a luminosity of 630 times that of the Sun and a surface temperature of 14,000 kelvins.

This star has apparent magnitude +2.7 and belongs to spectral class B2 IV, with the luminosity class of 'IV' indicating it is a subgiant star. The star's luminosity is 12,300 times that of the Sun, while its surface temperature is 22,831 kelvins. The star has a radius of 6.1 times solar and 11 times the mass of the Sun.

Theta Eridani is a binary system with some evidence suggesting it is part of a multiple star system.NSV 01002, database entry, New Catalogue of Suspected Variable Stars, the improved version, Sternberg Astronomical Institute, Moscow, Russia. Accessed on line February 26, 2010. The main star, θ¹ Eridani, is of spectral class A4 with a +3.2 apparent magnitude.

19 Tauri A presents as a blue-white B-type subgiant with an apparent magnitude of +4.30. It is a spectroscopic binary, whose component stars have magnitudes of +4.6 and +6.1. They are separated by 0.012 arcseconds and complete one orbit every 1313 days. The 8th magnitude visual companion, 19 Tauri B, is 69 arcseconds away.

Zeta Cancri Ca is the brightest of the three components, having an apparent magnitude of +6.12. It appears to be a yellow G-type star, often reported as G5V, but now thought to be earlier, probably G0V. This star has around 1.15 solar masses. The tenth magnitude Zeta Cancri Cb is a close pair of red dwarfs.

WASP-66, also known as TYC 7193-1804-1, is an F-type star in the constellation Antlia. It has an apparent magnitude of 11.6, which is much too faint to be seen with the unaided eye. In 2012, a planet around WASP-66 was discovered. WASP-66b has a mass that is about 2.3 times that of Jupiter.

Kappa Ursae Majoris (κ Ursae Majoris, abbreviated Kappa UMa, κ UMa) is a binary star in the constellation of Ursa Major. With a combined apparent magnitude of +3.60, the system is approximately 358 light-years from Earth. The two components are designated Kappa Ursae Majoris A (officially named Alkaphrah , a traditional name of the system) and B.

Zeta Tucanae (ζ Tuc, ζ Tucanae) is a star in the constellation Tucana. It is a spectral class F9.5 main sequence star with an apparent magnitude of +4.23. Despite having a slightly lower mass, this star is more luminous than the Sun. Based upon parallax measurements by the Hipparcos spacecraft, it is approximately 28.0 light years from Earth.

Zeta Trianguli Australis (ζ TrA) is a spectroscopic binary in the constellation Triangulum Australe. It is approximately 39.5 light years from Earth. The binary's composite spectral class is F9V and its combined apparent magnitude is +4.90. The pair orbit each other once every 13 days, and the orbital eccentricity is a low 0.014, making it nearly circular.

SN 2010lt is about 20" west and 10" north of the galaxy center. It is a sub-luminous (1991bg-like) type Ia supernova and was discovered when near maximum light. The supernova could not be detected (detection limit approximately 18.5 of apparent magnitude) at its current position on images taken between October 2005 and March 2006.

Zeta Crucis, Latinized from ζ Crucis, is a binary star system in the southern constellation of Crux. It is visible to the naked eye with an apparent magnitude of 4.06m. ζ Crucis is located at about 360 light-years from the Sun. It is a member of the Lower Centaurus Crux subgroup of the Scorpius-Centaurus Association.

Theta2 Crucis, Latinized from θ2 Crucis, is a spectroscopic binary star in the constellation Crux. This pair of stars complete an orbit every 3.4280 days and they have a low orbital eccentricity that is close to 0.0. Theta2 Crucis is located at about 750 light-years from the Sun. The system has a combined mean apparent magnitude of +4.72m.

TY Pyxidis is an eclipsing binary star in the constellation Pyxis. The apparent magnitude ranges from 6.85 to 7.5 over 3.2 days. The two components are both of spectral type G5IV, have a mass of 1.2 solar masses and revolve around each other every 3.2 days. Each star is around 2.2 times the diameter of the Sun.

The tertiary and fifth component, Zeta Piscium C, is a magnitude 12.2 star at an angular separation 1.0 arc seconds from component B. Together the star system has an apparent magnitude of +4.9.John Pratt's stars re-publication by Dr J.P. Pratt (Doctor of Astronomy, University of Arizona) of sidereal coordinate data. Note: possibly a non-book published source.

V385 Andromedae is a variable star in the constellation Andromeda, about away. It is a red giant over a hundred times larger than the sun. It has an apparent magnitude around 6.4, just about visible to the naked eye in ideal conditions. V385 Andromedae was identified as a long-period variable in 1999 from analysis of Hipparcos photometry.

NGC 6925 is an unbarred spiral galaxy in the constellation Microscopium of apparent magnitude 11.3. It is lens-shaped, as it lies almost edge on to observers on Earth. It lies 3.7 degrees west-northwest of Alpha Microscopii. SN 2011ei, a Type II supernova in NGC 6925, was discovered by Stu Parker in New Zealand in July 2011.

14 Herculis or 14 Her is the Flamsteed designation of a K-type main-sequence star approximately 58.5 light-years away in the constellation Hercules. Because of its apparent magnitude, the star cannot be seen with the naked eye. As of 2006, it is thought that 14 Herculis has two extrasolar planets in orbit around the star.

Bedin I is located in the constellation Pavo, at a right ascension of and declination of . The galaxy is situated behind a group of unnamed foreground stars within the globular cluster NGC 6752. Bedin I measures around 20 by 8 arcseconds across and has an apparent magnitude of 19.94, although its visibility is significantly decreased by NGC 6752, one of the brightest globular clusters in the sky with an apparent magnitude of 5.4. Bedin I was accidentally discovered by a team researching white dwarfs in the cluster in an effort to better determine the cluster's age. The galaxy partially appeared in the field of view during program GO-15096 of the Hubble Space Telescope, led by principal investigator Luigi R. Bedin, which occurred between 7 and 18 September 2018.

The German cartographer Johann Bayer used the Greek letters alpha to theta to label the most prominent stars in the constellation, while his countryman Johann Elert Bode subsequently added iota to phi. Only lambda and pi remain in use, likely because of their proximity to the north celestial pole. Within the constellation's borders, there are 39 stars brighter than or equal to apparent magnitude 6.5. Marking the Little Bear's tail, Polaris, or Alpha Ursae Minoris, is the brightest star in the constellation, varying between apparent magnitude 1.97 and 2.00 over a period of 3.97 days. Located around 432 light-years away from Earth, it is a yellow- white supergiant that varies between spectral types F7Ib and F8Ib, and has around 6 times the Sun's mass, 2,500 times its luminosity and 45 times its radius.

HD 192699 is a yellow subgiant star located approximately 214 light-years away in the constellation of Aquila. It has the apparent magnitude of 6.45. Based on its mass of 1.68 solar, it was an A-type star when it was a main-sequence. In April 2007, a planet was announced orbiting the star, together with HD 175541 b and HD 210702 b.

HD 156279 has a stellar mass of 0.93 and a stellar radius of 0.95. It has a metallicity of 0.14 and an effective temperature of 5453 Kelvin. HD 156279 is 4 billion years old and based on the spectral type, K0, it is an orange colour. HD 156279 has an apparent magnitude of 8.167 and an absolute magnitude of 5.27.exoplanetkyoto.

83D/Russell (previously 83P/Russell) is a periodic lost comet in the Solar System with an orbital period of about 7.5 years. On the post-1988 orbit the comet probably does not get brighter than about apparent magnitude 21. The comet might come to perihelion in late May 2021, but the uncertainty in the comet's position is a few million km.

NGC 1955 (also known as ESO 56-SC121) is an open cluster associated with an emission nebula located in the Dorado constellation. This nebula is part of the H II region which is part of the Large Magellanic Cloud and was discovered by James Dunlop on August 3, 1826. Its apparent magnitude is 9.0, and its size is 1.8 arc minutes.

NGC 171 is a barred spiral galaxy with an apparent magnitude of 12, located around 3 million light-years away in the constellation Cetus. The galaxy has 2 main medium-wound arms, with a few minor arms, and a fairly bright nucleus and bulge. It was discovered on 20 October 1784 by William Herschel. It is also known as NGC 175.

It has 89% of the mass of the Sun and 104% of the Sun's radius. The star is radiating 63% of the Sun's luminosity from its photosphere at an effective temperature of 5,255 K. Its smaller companion, designated component B, is a red dwarf with spectral type M2V and apparent magnitude 12.33. It has a projected separation of from the primary.

HR 7578 (also known as V4200 Sagittarii) is a binary star in the constellation of Sagittarius. Their combined apparent magnitude is 6.18. Parallax measurements by the Gaia spacecraft put the system at 46.01 light-years (14.107 parsecs) away, making this a nearby system. The two stars of HR 7578 are fairly old, older than the Pleiades but possibly younger than the Hyades.

It is an Alpha2 Canum Venaticorum variable; its apparent magnitude varies from 4.70 down to 4.75 with a period of 12.5 days. A rotationally-modulated magnetic field has been measured, varying from to . It has an estimated rotation period of , although this is in need of further confirmation. The proper motion companion is a magnitude 12.8 star at an angular separation of .

NGC 1978 (also known as ESO 85-SC90) is an elliptical shaped globular cluster or open cluster in the constellation Dorado constellation. It is located within the Large Magellanic Cloud. It was discovered by James Dunlop on November 6, 1826, and its apparent magnitude is 9.9, and its size is 3.9 arcminutes. Its radial velocity is 293.1 ± 0.9 km/s.

NGC 2002 (also known as ESO 86-SC3) is an open cluster located in the Dorado constellation and is part of the Large Magellanic Cloud. It was discovered by James Dunlop on September 24, 1826. Its apparent magnitude is 10.1, and its size is 2.0 arc minutes. NGC 2002 contains five red supergiants, prominent in deep images of the cluster.

The system is about 360 million years old. The primary component is a giant star with an apparent magnitude of 2.7 and a stellar classification of G5 III. It is radiating about 107 times the luminosity of the Sun from an expanded atmosphere about 13 times the Sun's radius. The mass of this star is 3.3 times that of the Sun.

12 Persei (12 Per) is a double-lined spectroscopic binary star system in the northern constellation Perseus. Its combined apparent magnitude is 4.94, which means it can be viewed with the naked eye. Based upon parallax measurements, this system is about 79 light years away from the Sun. The magnitude difference between the two components is estimated to be 0.51.

HD 74180 is a binary star in the constellation Vela. It is approximately 3,200 light years from Earth. The primary component is a yellow-white F-type supergiant with a mean apparent magnitude of +3.81, with a 10th magnitude companion 37.5 arcseconds distant. b Velorum has been classified as a suspected α Cygni variable star which varies by only 0.06 magnitude.

NGC 7424 is a barred spiral galaxy with an apparent magnitude of 10.4. located around 4 degrees west of the Grus Triplet. Approximately 37.5 million light-years distant, it is about 100,000 light-years in diameter, has well defined spiral arms and is thought to resemble the Milky Way. Two ultraluminous X-ray sources and one supernova have been observed in NGC 7424.

Spiral galaxy NGC 3021 which lies about 100 million light-years away. In terms of deep-sky objects, Leo Minor contains many galaxies viewable in amateur telescopes. Located 3 degrees southeast of 38 Leonis Minoris, NGC 3432 is seen nearly edge on. Known as the knitting needle galaxy, it is of apparent magnitude 11.7 and measures 6.8 by 1.4 arcminutes.

Omicron1 Centauri (ο1 Cen, ο1 Centauri) is a star in the constellation Centaurus. It is approximately 6,000 light years from Earth. ο1 Centauri is a yellow G-type supergiant or hypergiant with a mean apparent magnitude of +5.13. It is classified as a semiregular variable star and its brightness varies from magnitude +5.8 to +6.6 with a period of 200 days.

Omicron2 Centauri (ο2 Cen, ο2 Centauri) is a star in the constellation Centaurus. ο2 Centauri is a white A-type supergiant with a mean apparent magnitude of +5.12. It is approximately 5000 light years from Earth. It is classified as an Alpha Cygni type variable star and its brightness varies from magnitude +5.12 to +5.22 with a period of 46.3 days.

HD 115404 is a binary star system located in the constellation Coma Berenices. Parallax measurements made by Hipparcos put the system at 36 light-years, or 11 parsecs, away. The combined apparent magnitude of the system is 6.52, with the magnitudes of the components being 6.66 and 9.50. The primary component, designated A, is a K-type main sequence star.

1 Camelopardalis (1 Cam) is a double star system in the constellation Camelopardalis. Its combined apparent magnitude is 5.56 and it is approximately away. The 1 Camelopardalis system is part of the Camelopardalis OB1 stellar association, which is 820 pc away. 1 Camelopardalis A is a hot massive star which has evolved away from the main sequence to become a giant.

NGC 1871 (also known as ESO 56-SC85) is an open cluster associated with an emission nebula located in the Dorado constellation within the Large Magellanic Cloud. It was discovered by James Dunlop on November 5, 1826. Its apparent magnitude is 10.21, and its size is 2.0 arc minutes. NGC 1871 is part of a triple association with NGC 1869 and NGC 1873.

The primary, component A, is a yellow-white hued bright giant with a stellar classification of F8 II, and it is a classical Cepheid variable. The combined apparent magnitude of the system ranges from 5.69 to 6.19 over 5.273 days. The secondary companion, component B, is a main sequence star with a class of B6 V and an absolute magnitude of about −0.12.

HR 4049, also known as HD 89353 and AG Antliae, is a binary post-asymptotic- giant-branch (post-AGB) star in the constellation Antlia. A very metal-poor star, it is surrounded by a thick unique circumbinary disk enriched in several molecules. With an apparent magnitude of about 5.5, the star can readily be seen under ideal conditions. It is located approximately distant.

MWC 480 is a single star, about 500 light-years away in the constellation of Auriga. It is located in the Taurus-Auriga Star-Forming Region. The name refers to the Mount Wilson Catalog of B and A stars with bright hydrogen lines in their spectra. With an apparent magnitude of 7.62, it is too faint to be seen with the naked eye.

NV Puppis (NV Pup), also known as υ1 Puppis, is a class B2V (blue main- sequence) star in the constellation Puppis. Its apparent magnitude is 4.67 and it is approximately 800 light years away based on parallax. It is a γ Cas variable, ranging from 4.78 to 4.58 magnitude. It is most likely an optical double with the nearby NW Puppis.

Based on an absolute magnitude of 19.4, the asteroid has an estimated diameter of about . is noted for a close approach to the Earth on 31 December 1914 at a distance of . It is one of the largest objects known to have come inside the orbit of the moon. During the 1914 close approach the asteroid reached about apparent magnitude 7.7.

NGC 3293 is an open cluster in the Carina constellation. It was discovered by Nicolas-Louis de Lacaille in 1751. It consists of more than 100 stars brighter than 14th magnitude in a 10 arc minute field, the brightest of which are blue supergiants of apparent magnitude 6.5 and 6.7. There is also a 7th magnitude pulsating red supergiant, V361 Carinae.

Rho Cygni, Latinized from ρ Cygni, is a yellow-hued star in the northern constellation of Cygnus. It is visible to the naked eye with an apparent magnitude of 4.02. The measured annual parallax shift is 26.39 milliarcseconds, which yields a distance estimate of 124 light years. It is moving further from the Sun with a radial velocity of +6.88.

It is visible to the naked eye with a slightly variable apparent magnitude of about 4.5. The primary component, ο Cassiopeiae A, is a spectroscopic binary, and its close companion completes one orbit every 2.83 years (1,031.55 days). The system has also been resolved with interferometry. The primary of this spectroscopic binary is a blue-white B-type giant star.

Theta Delphini (θ Del, θ Delphini) is a star in the constellation Delphinus. It has an apparent magnitude of about 5.7, meaning that it is just barely visible to the naked eye under excellent viewing conditions. This star is around 2,050 light years away from the Sun. Theta Delphini's spectral type is K3Ib, meaning it is a K-type supergiant.

AR Aurigae (AR Aur), also known by its Flamsteed designation 17 Aurigae, is a binary star in the constellation Auriga. Based on parallax measurements made by the Hipparcos spacecraft, it is approximately 400 light-years from Earth. Both components are blue-white B-type main-sequence stars that do not fill their Roche lobes. The system has a mean apparent magnitude of +6.15.

The two components of this system have an angular separation of 0.25 arcseconds. The brighter component is a giant star with a spectral classification of G8 III and an apparent magnitude of 4.79. The effective temperature of its outer atmosphere is 4,900 K, giving it the yellowish glow of a G-type star. The fainter component is a star of magnitude 6.77.

13 Boötis, also known by its variable star designation CF Boötis, is a variable star in the constellation Boötes. It is approximately 550 light-years from Earth, based on its parallax. 13 Boötis is a M-type red giant with a mean apparent magnitude of +5.26. It is classified as an irregular variable star and its brightness varies from magnitude +5.29 to +5.38.

The quasar lies 10 arcminutes north of NGC 3079, in the constellation Ursa Major. The astronomical data services SIMBAD and NASA/IPAC Extragalactic Database (NED) list several other names for this system. The Twin Quasar's two images are separated by 6 arcseconds. Both images have an apparent magnitude of 17, with the A component having 16.7 and the B component having 16.5.

Courier Corporation. p. 385. In 1867 he made the first measurement of the Sun's apparent magnitude, using a particular "telescope / photometer" he designed. The instrument was able to superimpose two images, one from a small telescope and the second from a reference lamp. During daytime he dimmed the image of the Sun (using polarizers and diaphragms) and compared it to the lamp.

Omega Aurigae, Latinized from ω Aurigae, is the Bayer designation for a double star in the northern constellation of Auriga. Its apparent magnitude is 4.95, which is bright enough to be seen with the naked eye. The distance to this system, as determined using parallax measurements, is approximately . The system is a member of the Columba group of co-moving stars.

On 25 August 1989 Castalia passed (within eleven lunar distances) of Earth, allowing it to be observed with radar from the Arecibo Observatory by Scott Hudson (Washington State University) and Steven J. Ostro (JPL). The data allowed Hudson et al. to produce a three-dimensional model of the object. During the 1989 passage Castalia peaked at an apparent magnitude of 12.

Optical, infrared, and X-ray observations taken by the Hubble Space Telescope between 14 and 59 days after the burst's detection revealed a blue galaxy with an apparent magnitude of 24.95 ± 0.11. Like several other gamma-ray burst hosts, Lyman alpha emission was detected from this galaxy, supporting the theory that the progenitors of gamma-ray burst tend to be metal-poor.

Revised calculations predicted the next perihelion would be on 28 November 1971 and Elizabeth Roemer of the University of Arizona successfully relocated the comet with the 154-cm reflector at Catalina. It was also observed in 1978, 1985, 1991-1992, and 1998-1999. The comet peaked at about apparent magnitude 16.3 in 2012. On 29 December 2077 the comet will pass from Mars.

Q Scorpii (Q Sco) is an orange giant star in the constellation Scorpius. Its apparent magnitude is 4.27. It lies in the tail of Scorpius, between the stars λ Scorpii and μ Scorpii, from the faint globular cluster Tonantzintla 2. Q Scorii is a suspected astrometric binary, a star whose position is seen to oscillate although no companion has been detected.

H Scorpii (H Sco) is a star in the constellation Scorpius. Its apparent magnitude is 4.18. It was initially given the Bayer designation Beta Normae by Lacaille but later moved from Norma to Scorpius. Located around 343 light- years distant, it shines with a luminosity approximately 576 times that of the Sun and has a surface temperature of 4000 K.

CoRoT-3 is a white-yellow dwarf main sequence star hotter than our Sun. This star is located approximately 2560 light-years away in the constellation of Aquila. The apparent magnitude of this star is 13, which means it is not visible to the naked eye but can be seen with a medium-sized amateur telescope on a clear dark night.

HD 45652 (Lusitânia) is a G8-K0 star located in the constellation Monoceros. It is approximately 114 light years (35 parsecs) from Earth with apparent magnitude 8.13. In May 2008, the discovery of an extrasolar planet, HD 45652 b, orbiting the star was announced. The planet was detected by the radial velocity method, using observations made from 2005 to 2007.

Theta Andromedae (θ And, θ Andromedae) is the Bayer designation for a binary star in the constellation Andromeda. It is approximately from Earth, with a visual magnitude of 4.6. On the Bortle Dark-Sky Scale, this makes it visible to the naked eye from outside urban regions. Theta Andromedae is a white A-type main sequence dwarf with an apparent magnitude of +4.61.

Kepler-138 is a red dwarf with approximately 57% the mass of and 54% the radius of the Sun. It has a surface temperature of 3871 ± 58 K. In comparison, the Sun has a surface temperature of 5778 K. Kepler-138's apparent magnitude (bright it appears from Earth's perspective) is 12.925, too dim to be seen with the naked eye.

This star has 55% more mass than the Sun. It shines with 6.6 times the Sun's luminosity at an effective temperature of 7,132 K. This heat gives it the yellow-white glow of an F-type star. It has a faint companion located 31 arcseconds away with an apparent magnitude of +11.3. Most likely this pair form a binary star system.

HR 3384 (11 G. Pyxidis) is solitary star in the southern constellation of Pyxis. It has an apparent magnitude of 6.38, indicating it is faintly visible to the naked eye. Based on the Bortle scale, the star can be viewed from dark rural skies. Astrometric measurements of the star by the Hipparcos spacecraft, give an estimated distance of about from Earth.

Students for the Exploration and Development of Space. Retrieved March 3, 2009 NGC 3982 is a part of the M109 Group. At an apparent magnitude of 12.0, NGC 3982 needs a telescope to be viewed. Using small telescopes, the galaxy appears as a very faint, diffuse patch of light with its central region appearing as a slightly brighter diffuse ball.

NGC 2353 is a loosely bound open cluster located in the constellation Monoceros. It has an apparent magnitude of 7.1 and an approximate size of 20 arc-minutes. The cluster is dominated by the magnitude 6.0 star HIP 34999, which lies at the southern edge of the cluster. The asterism NGC 2351 lies 19 arc-minutes southeast of NGC 2353.

Pi Aquarii, Latinized from π Aquarii, is the Bayer designation for a binary star in the equatorial constellation of Aquarius. This system has an apparent visual magnitude of a mean apparent magnitude of +4.57. Based upon parallax measurements, it is located at a distance of roughly from Earth. This is a binary star system with an orbital period of 84.1 days.

HD 34557 is a double star in the northern constellation of Auriga. The fainter star has an angular separation of 0.380″ from the primary component. They have a combined apparent magnitude of 5.52, making HD 34557 faintly visible to the naked eye from dark skies. Based upon parallax measurements made with the Hipparcos satellite, this system is roughly 280 light years away.

HIP 13044's mass is estimated to be 0.8 solar masses. Having a rotation period of 5–6 days, HIP 13044 is a fast-rotating star for its type. It is possible that this is because it has swallowed planets during its red-giant phase. HIP 13044 has an apparent magnitude of 9.94 and cannot be seen with the unaided eye.

118P/Shoemaker–Levy (also known as periodic comet Shoemaker–Levy 4) is a comet discovered by astronomers Carolyn and Eugene M. Shoemaker and David Levy. During the 2010 apparition the comet became as bright as apparent magnitude 11.5. The comet nucleus is estimated to be 4.8 kilometers in diameter. On December 3, 2015, comet Shoemaker–Levy 4 will pass from asteroid 4 Vesta.

Just shading Alpha, Beta Aquarii is the brightest star in Aquarius with an apparent magnitude of 2.91. It also has the proper name of Sadalsuud. Having cooled and swollen to around 50 times the Sun's diameter, it is around 2200 times as luminous as the Sun. It is around 6.4 times as massive as the Sun and around 56 million years old.

', provisionally known as 2003 EE16', is an Apollo near-Earth asteroid and potentially hazardous object. It was discovered on 8 March 2003 by LPL/Spacewatch II at an apparent magnitude of 20 using a reflecting telescope. It has an estimated diameter of . The asteroid was listed on Sentry Risk Table with a Torino Scale rating of 1 on 2 April 2003.

' is a sub-kilometer asteroid and fast rotator, classified as a near-Earth object of the Apollo group, approximately 50 meters in diameter. It was first observed on 30 September 2014, by the Mount Lemmon Survey at an apparent magnitude of 21 using a reflecting telescope. With an absolute magnitude of 24.3, the asteroid is about 37–85 meters in diameter.

The system has an apparent magnitude of 18.3, and is estimated to be between 3 and 10 billion years old. With a parallax of 166 mas (0.166 arcseconds), about 80 star systems are known to be closer to the Sun. It is a late discovery, as far as nearby stars go, because past efforts concentrated on high-proper-motion objects.

DL Crucis has a visual apparent magnitude of 6.3 so it is just visible with the unaided eye in dark skies. It lies in the small southern constellation of Crux, halfway between η Crucis and ζ Crucis and close to the constellation's brightest star α Crucis. This area of sky lies within the Milky Way and close to the Coalsack Nebula.

This is the original image of the Hubble Ultra-Deep Field. This is a list of UDF objects 1-500 from the Hubble Ultra Deep Field (UDF). The Hubble Ultra Deep Field is a small region of the sky in the constellation of Fornax. The data in these tables is from the SIMBAD Astronomical Database, and the apparent magnitude data is from Wikisky.

Consequently, the absolute magnitude of any object equals the apparent magnitude it would have if it were 10 parsecs away. The measurement of absolute magnitude is made with an instrument called a bolometer. When using an absolute magnitude, one must specify the type of electromagnetic radiation being measured. When referring to total energy output, the proper term is bolometric magnitude.

Note that right ascension, as used by astronomers, is 360° minus the sidereal hour angle. The final characteristic provided in the tables and star charts is the star's brightness, expressed in terms of apparent magnitude. Magnitude is a logarithmic scale of brightness, designed so that a body of one magnitude is approximately 2.512 times brighter than a body of the next magnitude.

Based on its light curve, Selene has an estimated rotation period of 0.3947±0.0004 days, or just under 9.5 hours. During each rotation, the apparent magnitude varies by 0.27. The approximate diameter of this asteroid is 46 km. (Some sources list a diameter of up to 56 km.) The albedo is about 7%, comparable to that of the Earth's Moon.

Upsilon Orionis (υ Ori, υ Orionis) is a star in the constellation Orion. It has the traditional name Thabit or Tabit (ﺛﺎﺑﺖ, Arabic for "the endurer"), a name shared with pi3 Orionis. It is a blue-white main sequence star of apparent magnitude 4.62 located over 3000 light-years distant from the Solar System. It is a suspected Beta Cephei variable.

The permanent designation "153P" was given to the comet. It has the longest known orbital period of any periodic comet (366.51 years). Its orbital speed around the Sun varies from 59 km/s at perihelion to 0.29 km/s at aphelion. The comet passed perihelion on March 18, 2002, and with apparent magnitude 3.5, it became the brightest comet since 1997.

Xi Draconis (ξ Draconis, abbreviated Xi Dra, ξ Dra) is a double or binary star in the northern circumpolar constellation of Draco. It has an apparent visual magnitude of 3.75. Based upon parallax measurements, it is located at a distance of from the Sun. At this distance, the apparent magnitude is diminished by 0.03 from extinction caused by intervening gas and dust.

In 2007, Floor van Leeuwen and his team calibrated the star's apparent magnitude at 3.9974 with an updated parallax of 22.04 ± 0.37 milliarcseconds, yielding a distance of 45.4 parsecs or approximately 148 light years from Earth. Given a surface temperature of 5,068 Kelvin, theoretical calculations would yield a total luminosity for the star of about 60 times the solar luminosity.

Iota Draconis (ι Draconis, abbreviated Iota Dra, ι Dra), also named Edasich , is a star in the northern circumpolar constellation of Draco. A visually unremarkable star of apparent magnitude 3.3, in 2002 it was discovered to have a planet orbiting it (designated Iota Draconis b, later named Hypatia). From parallax measurements, this star is located at a distance of about from the Sun.

Beta Piscium (β Piscium, abbreviated Beta Psc, β Psc), formally named Fumalsamakah , is a blue-white hued star in the zodiac constellation of Pisces. Its apparent magnitude is 4.40, meaning it can be faintly seen with the naked eye. Based on parallax measurements taken during the Hipparcos mission, it is about 410 light-years (125 parsecs) distant from the Sun.

Alauda has been observed to occult stars on several occasions, providing important information on its size and shape. It produced occultations on 2001-07-12 and 2004-04-21. It may have occulted an apparent magnitude 9.5 star in the constellation of Gemini on 2009-10-17 at 08:18 UT. This event should have been visible from Uruguay, Argentina, and Chile.

One supernova has been observed in NGC 931, SN 2009lw. The supernova was discovered by W. Li, S. B. Cenko, and A. V. Filippenko during the Lick Observatory Supernova Search on 24.24 November 2009, when it had an apparent magnitude of 18.8. It was identified as a type-Ib or possibly a type-IIb supernova a few months past maximum light.

Xi Cephei A is a double-lined spectroscopic binary system with an orbital period of 810.9 days and an eccentricity of 0.46. The primary, component Aa, is a chemically peculiar Am star, a probable subgiant with an apparent magnitude of +4.29. Eight arcseconds away, Xi Cephei B is another spectroscopic binary. Xi Cephei C is a 13th magnitude star nearly two arcminutes away.

UZ Fornacis (abbreviated as UZ For) is a binary star in the constellation of Fornax. It appears exceedingly faint with a maximum apparent magnitude 17.0. Its distance, as measured by Gaia using the parallax method, is about 780 light-years (240 parsecs). The system consists of two stars, a white dwarf and a red dwarf, in close orbit around each other.

The solar constant includes all wavelengths of solar electromagnetic radiation, not just the visible light (see Electromagnetic spectrum). It is positively correlated with the apparent magnitude of the Sun which is −26.8. The solar constant and the magnitude of the Sun are two methods of describing the apparent brightness of the Sun, though the magnitude is based on the Sun's visual output only.

GJ 9827 is a star in the constellation of Pisces. It is a K-type main-sequence star with an apparent magnitude of 10.250. It is 97 light-years (30 parsecs) away, based on parallax. The rotation period of the star cannot be determined as in 2020, and can be either around 15 or 30 days, depending on interpretation of available data.

Venus, pictured center-right, is always brighter than all other planets or stars as seen from Earth. Jupiter is visible at the top of the image. To the naked eye, Venus appears as a white point of light brighter than any other planet or star (apart from the Sun). The planet's mean apparent magnitude is −4.14 with a standard deviation of 0.31.

Delta Canis Majoris (Latinised from δ Canis Majoris, abbreviated Delta CMa, δ CMa), officially named Wezen , is a star in the constellation of Canis Major. It is a yellow-white F-type supergiant with an apparent magnitude of +1.83. Since 1943, the spectrum of this star has served as one of the stable anchor points by which other stars are classified.

Beta Tauri (Latinised from β Tauri, abbreviated Beta Tau, β Tau), officially named Elnath (pronounced or , sometimes spelled Alnath), is the second- brightest star located in the constellation borders of Taurus and Auriga with an apparent magnitude of 1.65. It is a chemically peculiar B7 giant star, 134 light years away from Earth. It had a co-existing name Gamma Aurigae.

66 Eridani is a binary star in the constellation of Eridanus. The combined apparent magnitude of the system is 5.12 on average. Parallax measurements by Hipparcos put the system at some 309 light-years (95 parsecs) away. This is a spectroscopic binary: the two stars cannot be individually resolved, but periodic Doppler shifts in its spectrum mean there must be orbital motion.

Epsilon Microscopii lies 166 ± 5 light-years away, and is a white star of apparent magnitude 4.7, and spectral type A1V. Theta1 and Theta2 Microscopii make up a wide double whose components are splittable to the naked eye. Both are white A-class magnetic spectrum variable stars with strong metallic lines, similar to Cor Caroli. They mark the constellation's specimen slide.

NGC 1817 is an open cluster of stars in the constellation Taurus. It was discovered by English astronomer William Herschel in February 1784. With an apparent magnitude of 7 and spanning 17 arc minutes across the sky, it is separated from the NGC 1807 cluster by just a few degrees. Indeed, the two may actually be parts of a single extended cluster.

It has an apparent magnitude of 12.12, and thus cannot be seen with the unaided eye. Because Kepler-14 is so close-knit as seen from Earth, it was impossible for the discovery team to separate the two stars and analyze their characteristics as separate stars. The Kepler team analyzed their characteristics under the assumption that Kepler-14 was a single star.

HD 178911 is a triple star system in the constellation Lyra. The secondary star (designated as HD 178911 B) has an apparent magnitude of 6.74 and a spectral type of G1V, which is very similar to our Sun at a distance of 160 light years. The age of the star is slightly older and have significantly higher metallicity than our Sun.

6 Ceti is a single star in the equatorial constellation of Cetus. It is visible to the naked eye with an apparent magnitude of 4.89. The annual parallax shift as measured from Earth's orbit is 53.34 mas, which yields a distance estimate of 61.1 light years. The star is moving further from the Sun with a constant radial velocity of +16.70 km/s.

Zeta Sculptoris, Latinized from ζ Sculptoris, is a multiple star system in the constellation Sculptor. It is faintly visible to the naked eye with an apparent magnitude of 5.04. The annual parallax shift is 6.49 mas, which yields a distance estimate of about 500 light years from the Sun. It is moving further away with a radial velocity of +8.6 km/s.

31 Comae Berenices (31 Com) is a yellow giant star in the constellation Coma Berenices. Its apparent magnitude is about 4.9 and slightly variable. It is a rare FK Comae Berenices variable, a variable star that spins rapidly and has large starspots on its surface. It is currently in the Hertzsprung gap and its outer envelope has just begun convection.

' (prov. designation: ) is an asteroid on an eccentric orbit, classified as near-Earth object and potentially hazardous asteroid of the Apollo group, approximately in diameter. It was discovered on 20 August 2004 by the Siding Spring Survey at an apparent magnitude of 16.5 using the Uppsala Southern Schmidt Telescope. It is one of the largest potentially hazardous asteroids known to exist.

With an apparent magnitude of about 6.5, it is one of the few Wolf-Rayet stars that can be seen with the naked eye (although it can only be seen with the naked eye under excellent viewing conditions). Like most extremely massive stars, HD 151932 is losing mass via its stellar wind. The total rate of mass loss is /yr. The multiplicity (i.e.

Delta Trianguli (Delta Tri, δ Trianguli, δ Tri) is a spectroscopic binary star system approximately away in the constellation of Triangulum. The primary star is a yellow dwarf, while the secondary star is thought to be an orange dwarf. It has an apparent magnitude of +4.87 and forms an optical (line-of-sight) triple with Gamma Trianguli and 7 Trianguli.

NGC 1981 (also known as OCL 525) is an open cluster which is located in the Orion constellation. It was discovered by John Herschel on 4 January 1827. Its apparent magnitude is 4.2 and its size is 28.00 arc minutes. It lies to the north of the Orion Nebula, separated from it by the Sh2-279 region containing NGC 1973, 1975, and 1977.

Chi Ursae Majoris is an evolved, orange hued K-type giant with an apparent magnitude of +3.69. This star has times the radius of the Sun and 1.49 times the Sun's mass. The spiral galaxy in Ursa Major, NGC 3877 (= H I.201), type Sc, is best found from Chi Ursae Majoris, which is almost exactly 15 arcminutes north of the galaxy.

Chi Centauri (χ Cen, χ Centauri) is a star in the constellation Centaurus. χ Centauri is a blue-white B-type main sequence dwarf with a mean apparent magnitude of +4.36. It is approximately 510 light years from Earth. It is classified as a Beta Cephei type variable star and its brightness varies by 0.02 magnitudes with a period of 50.40 minutes.

Nu Herculis, Latinized from ν Herculis, is a binary and variable star in the constellation of Hercules. With an apparent magnitude of about 4.4, it is faintly visible to the naked eye. Parallax measurements made by the Hipparcos spacecraft put it at a distance of about 860 light years (260 parsecs). Nu Hercules is a binary with the two components separated by .

HD 132406 is a star in Boötes constellation. The spectrum is G0V, apparent magnitude +8.45, and the stellar distance 221 ly (68 pc). The star is 100K hotter, 1.8 Gya older, and 1.5 times more enrich in heavy elements [Fe/H] than our Sun. The star is unusual since it has one known planet, HD 132406 b, as of 2007.

LHS 2520, also known as Gliese 3707, is a red dwarf star in the constellation Corvus. With an apparent magnitude of 12.12. it is too faint to be seen with the unaided eye. A cool star of spectral type M3.5V, it has a surface temperature of 3024 K. The star was too faint to have had its parallax measured by the Hipparcos satellite.

The Great Comet of 2007: Watch it on the Web Yahoo News, January by Joe Rao of SPACE.com Skywatching Columnist. Accessed 16 January 2007 On 13 and 14 January 2007, the comet attained an estimated maximum apparent magnitude of −5.5. It was bright enough to be visible in daylight about 5°–10° southeast of the Sun from 12 to 14 January.

It consists of two B-type main sequence stars that orbit each other. The larger and brighter (Zeta Phoenicis Aa) is formally named Wurren . When one passes in front of one another, it blocks some of the other star's light. As a result, its apparent magnitude fluctuates between 3.9 and 4.4 with a period of 1.66977 days (its orbital period).

The limiting apparent magnitude of the survey is 19.5, covering objects with a redshift mostly within less than z=0.3 and a median redshift of 0.11. The volume of the Universe covered by the survey is approximately 108 h−1 Mpc3, where h corresponds to the value of the Hubble constant, H0, divided by 100. H0 is approximately 70 km/s/Mpc.

It is estimated to be roughly 63 meters in diameter. In 2015 it was known to have a 1 in 63,000 chance of impacting Earth on 27 November 2015. However, the nominal best-fit orbit showed that would be roughly from Earth on 27 November 2015 with an apparent magnitude of roughly +25 in the constellation of Virgo about 50 degrees from the Sun, and the same nominal orbit gave a distance of closest approach to Earth of a little under 0.4 AU a few weeks earlier. It was removed from the Sentry Risk Table on 17 September 2015, but was still listed at NEODyS with odds of 1 in 3 million for 27 November 2015 during the approach window. was discovered on 15 November 2007 by the Mount Lemmon Survey at an apparent magnitude of 20 using a reflecting telescope.

Iota Leonis, Latinized from ι Leonis, is a triple star system in the constellation Leo. The system is fairly close to the Sun, at only 79 light- years (24.2 parsecs) away, based on its parallax. The system has a combined apparent magnitude of 4.00 making it faintly visible to the naked eye. It is moving closer to the Sun with a radial velocity of −10 km/s.

The event was discovered on 22 February 2016 by the Panoramic Survey Telescope and Rapid Response System (Pan-STARRS) in Hawaii, with follow-up observations by the Hubble Space Telescope. The supernova occurred at a high z-value indicating a distance of 3.6 billion light-years. and is located in the constellation Draco. The maximum apparent magnitude was 18.11, the corresponding absolute magnitude -22.35.

The mean separation between them is approximately 10 AU, about the distance between the Sun and Saturn. The binary star has a visual companion, CCDM J13100+1732C, of apparent magnitude 10.2, located 89 arcseconds away along a position angle of 345°.Entry 13100+1732, discoverer code STF1728, components AB-C, The Washington Double Star Catalog , United States Naval Observatory. Accessed on line September 3, 2008.

The flash subsystem is an optical beacon allowing those on earth to visually track EQUiSat after launch. The beacon is an array of four extremely bright LEDs (~10,000 lumens each) that will be flashed for .1 seconds three times in rapid succession every minute when EQUiSat is in the night sky. The array will have an apparent magnitude of 3, approximately the same intensity as Polaris.

Adhafera is a giant star with a stellar classification of F0 III. Since 1943, the spectrum of this star has served as one of the stable anchor points by which other stars are classified. Its apparent magnitude is +3.44, making it relatively faint for a star that is visible to the naked eye. Nevertheless, it shines with 85 times the luminosity of the Sun.

Adhafera has about three times the Sun's mass and six times the radius of the Sun. Parallax measurements from the Hipparcos satellite yield an estimated distance to Adhafera of from the Sun. Adhafera forms a double star with an optical companion that has an apparent magnitude of 5.90. Known as 35 Leonis, this star is separated from Adhafera by 325.9 arcseconds along a position angle of 340°.

It is from Earth in the constellation of Perseus and less than 25 degrees from the Sun. It has an apparent magnitude of 7 and is too diffuse to be visible to the naked eye even from a dark site. The comet is also hidden by the glare of twilight, zodiacal light and atmospheric extinction. It was originally best seen from the Southern Hemisphere.

Nu¹ Sagittarii A is a spectral type K1 bright giant which has an apparent magnitude of +4.86. It is a microvariable with a frequency of 0.43398 cycles per day and an amplitude of 0.0078 magnitude. In 1982 it was found to have a hotter companion, Nu¹ Sagittarii B, a rapidly rotating B9 type star. The pair orbit with a period of around 370 days.

In addition, WASP-15 is most likely younger than the Sun, as it has an estimated age of 3.9 billion years. WASP-15 is approximately 3.09 times more luminous than the Sun. WASP-15 is located at a distance of approximately 290 parsecs (900 light years), and it has an estimated apparent magnitude of 10.9. It is, thus, not visible from Earth with the unaided eye.

They display an ellipsoidal variation of 0.03 in magnitude. The two stars are rotating rapidly, with projected rotational velocities of 108 and 87 km/s respectively. Their orbital period is 1.57 days and they are separated by an estimated distance of only 15 solar radii along a circular orbit. The primary is orbited by a smaller, more distant companion (B), which has an apparent magnitude of +12.2.

NGC 1624 is a very young open cluster located in the constellation Perseus inside an emission nebula. It was discovered by the German-British astronomer William Herschel in 1790. NGC 1624 is located at about 20,000 ly (6,000 pc) away and the latest estimates give an age of less than 4 million years. The apparent magnitude is 11.8, and apparent diameter is about 3.0 arc minutes.

In 1998, the Extreme Ultraviolet Explorer space telescope detected a strong flare that released an X-ray emission nearly equal to the output of the entire star. The quiescent X-ray luminosity of Mu Velorum A is about . The fainter companion, Mu Velorum B, is a main sequence star with an apparent magnitude of 6.4 and an assigned stellar classification of G2V. However, this classification is suspect.

Beta Phoenicis (β Phoenicis, β Phe) is a binary star in the constellation Phoenix. Its apparent magnitude is 3.30, meaning that it can be seen with the naked eye (see Bortle scale). The distance to Beta Phoenicis is poorly known. The original reduction of the Hipparcos satellite's data yielded a parallax value of 16 milliarcseconds, yet its standard error was larger than the parallax value itself.

QU Normae, also known as HR 6131, is a blue supergiant star in the constellation Norma. It is also a variable star, thought to be an α Cyg variable. The apparent magnitude of QU Normae varies somewhat irregularly between 5.27 and 5.41. The General Catalogue of Variable Stars quotes a period of 4.818 days, but other research only shows likely periods longer than 10 days.

C/2014 Q3 (Borisov) is a periodic comet discovered at apparent magnitude 17 on 22 August 2014 by amateur astronomer Gennadiy Borisov using a astrograph. It is the third comet discovered by Borisov. The comet is best viewed from the northern hemisphere. The comet was expected to reach about magnitude ~11 near perihelion (closest approach to the Sun), but brightened to around magnitude 10.

A photograph showing constellation Pictor as it can be seen by the naked eye (lines have been added that join up its three main stars). The bright star seen near Pictor is Canopus. Pictor is a faint constellation; its three brightest stars can be seen near the prominent Canopus. Within the constellation's borders, there are 49 stars brighter than or equal to apparent magnitude 6.5.

C/2007 E2 (Lovejoy) is a non-periodic comet discovered by Terry Lovejoy on 15 March 2007. Its perihelion was 27 March 2007, while its closest approach to Earth was 25 April 2007 in Hercules at a distance of 0.44 AU. Maximum apparent magnitude was approximately +8. The discovery was made using a Canon EOS 350D consumer grade digital camera, and not a CCD survey camera.

One supernova has been observed in NGC 1433, SN 1985 P, type II with apparent magnitude 13.5 at discovery, on 10 October 1985.Spectroscopy and photometry of a type II supernova 1985P in NGC1433 Workshop of ESO for SN 1987A, Garching, Federal Republic of Germany, 6-8 Ιουλίου 1987, Proceedings (A88-35301 14-90). Garching, Federal Republic of Germany, European Southern Observatory, 1987, p. 655-661.

Canes Venatici is one of the 88 official modern constellations. It is a small northern constellation that was created by Johannes Hevelius in the 17th century. Its name is Latin for 'hunting dogs', and the constellation is often depicted in illustrations as representing the dogs of Boötes the Herdsman, a neighboring constellation. Cor Caroli is the constellation's brightest star, with an apparent magnitude of 2.9.

The nebula surrounds the variable star RU Coronae Australis, which has an average apparent magnitude of 12.9 and is a WC class Wolf–Rayet star. IC 1297 is small, at only 7 arcseconds in diameter; it has been described as "a square with rounded edges" in the eyepiece, elongated in the north-south direction. Descriptions of its color encompass blue, blue-tinged green, and green-tinged blue.

Pi Chamaeleontis (π Cha) is a star located in the constellation Chamaeleon. Its apparent magnitude is 5.64. Parallax measurements by Hipparcos put the system at 135 light-years (41.5 parsecs) away. Pi Chamaeleontis is an A-type subgiant or F-type giant star with an effective temperature of about 6,900 K. It has an absolute magnitude of 2.56, a mass of , and a radius of .

36 Tauri (abbreviated to 36 Tau) is a binary star in the constellation of Taurus. Parallax measurements made by the Hipparcos spacecraft put it at a distance of over 1,000 light years (350 parsecs) from Earth. The combined apparent magnitude of the system is about 5.5, meaning it can barely be seen with the naked eye, according to the Bortle scale. 36 Tauri is a spectroscopic binary.

TZ Cassiopeaie (TZ Cas, HIP 117763, SAO 20912) is a variable star in the constellation Cassiopeia with an apparent magnitude of around +9 to +10. It is approximately 8,000 light-years away from Earth. The star is a red supergiant star with a spectral type of M3 and a temperature below . TZ Cassiopeiae was reported as being variable by Williamina Fleming and published posthumously in 1911.

HD 88809 is a star in a double star system in the constellation Antlia. The primary is an orange giant of spectral type K1III. Located around 480 light- years distant, it shines with a luminosity approximately 124 times that of the Sun and has a surface temperature of 4607 K. It has an apparent magnitude of 5.9, while the secondary star has a magnitude of 13.

Several other visual confirmations were made throughout the rest of the year. By the end of 2012, the comet had a coma 5-7 arc minutes across and an apparent magnitude estimated at +9. It was well placed for viewing in the southern hemisphere in January 2013 to observe it brightening, crossing Centaurus, Crux and Chamaeleon, and into February when it was circumpolar in Octans.

PU Puppis (PU Pup) is a class B8III (blue giant) star in the constellation Puppis. Its apparent magnitude is 4.69 and it is approximately 620 light years away based on parallax. It is a β Lyrae variable, ranging from 4.75 to 4.69 magnitude with a period of 2.58 days. The secondary is estimated at about 5.6 magnitude, although recent observations have failed to confirm it.

Cancer is one of the twelve constellations of the zodiac and is located in the Northern celestial hemisphere. Its name is Latin for crab and it is commonly represented as one. Its astrological symbol is♋. Cancer is a medium-size constellation with an area of 506 square degrees and its stars are rather faint, its brightest star Beta Cancri having an apparent magnitude of 3.5.

HD 64760 (J Puppis) is a class B0.5 supergiant star in the constellation Puppis. Its apparent magnitude is 4.24 and it is approximately 1,660 light years away based on parallax. The stellar wind structure of HD 64760 has been extensively studied. Its spectrum shows classic P Cygni profiles indicative of strong mass loss and high-velocity winds, but the spectral line profiles are also variable.

3 Puppis (3 Pup) is a supergiant star in the constellation Puppis. It is a very rare A[e] supergiant, referred to as a B[e] star despite its spectral classification, and its apparent magnitude is 3.93. 3 Puppis is surrounded by a disc of circumstellar dust, which is unusual for an A-type star. It is thought to be caused by a low mass companion.

HD 106112, also known as CO Camelopardalis, is a star in the constellation Camelopardalis. It has an apparent magnitude of about 5.1, meaning that it is just barely visible to the naked eye. Based upon parallax measurements made by the Hipparcos spacecraft, this star is around 177 light years away from the Sun. HD 106112's spectral type shows that it is an A-type giant star.

This is particularly odd as such low-mass stars near the boundary between brown dwarfs and hydrogen-fusing stars should be expected to have considerably less metal content than the Sun. Its luminosity () is 0.0522% of that of the Sun. The star's apparent magnitude, or how bright it appears from Earth's perspective, is 18.8. Therefore, it is too dim to be seen with the naked eye.

This is particularly odd as such low-mass stars near the boundary between brown dwarfs and hydrogen-fusing stars should be expected to have considerably less metal content than the Sun. Its luminosity () is 0.05% of that of the Sun. The star's apparent magnitude, or how bright it appears from Earth's perspective, is 18.8. Therefore, it is too dim to be seen with the naked eye.

On August 19 and 20, 2011, it became the fifteenth comet detected by ground radar telescope. During the 1995 perihelion passage, the comet was visible to Solar and Heliospheric Observatory (SOHO) on January 16, 1996, when the comet was around apparent magnitude 7 and 4.3° from the Sun. It is green because it emits diatomic carbon which glows green in the near vacuum of space.

1 Serpentis (1 Ser) is a red giant in the constellation Virgo with an apparent magnitude of 5.52. It is a red clump giant, a cool horizontal branch star that is fusing helium in its core. It has expanded to over 13 times the radius of the Sun and although it is cooler at it is 77 times more luminous. It is 322 light years away.

SX Centauri is a variable star in the constellation Centaurus. An RV Tauri variable, its light curve alternates between deep and shallow minima, varying its apparent magnitude from 9.1 to 12.4. From the period-luminosity relationship, it is estimated to be around 1.6 kpc (5200 light-years) from Earth. Gaia Data Release 2 gives a parallax of 0.2175 mas, corresponding to distance of about .

Ross 695, also known as Gliese 465, is a red dwarf star in the constellation Corvus. At apparent magnitude 11.27, it is much too faint to be seen with the unaided eye. A small star, it has around 23% the mass and radius of the Sun, but only 0.7% its luminosity. Investigation of its radial velocity failed to find any evidence of a planetary companion.

NGC 1342 is an open cluster in the constellation Perseus. It was discovered by William Herschel on 28 December 1799. It is located in the south of the constellation, almost halfway between Algol (β Persei) and ζ Persei, away from the plane of the Milky Way. NGC 1342 has an apparent size of 17' and an apparent magnitude of 6.7, marginally visible by naked eye.

The asteroid was discovered on 14 July 1999, by the Lincoln Near-Earth Asteroid Research (LINEAR) team at Lincoln Laboratory's Experimental Test Site, near Socorro, New Mexico, USA, at an apparent magnitude of 18, using a 1.0-meter reflector. Its first observation was made by the Catalina Sky Survey in June 1999, extending the asteroid's observation arc by one month prior to its official discovery observation.

It lies near the ecliptic and thus is subject to occultation by the Moon. One such event was observed September 3, 1991. This system forms a wide double star with an angular separation of along a position angle of 230°, as of 1991. The brighter star, component A, has an apparent magnitude of 4.99 while the fainter secondary, component B, is of magnitude 9.09.

104 Tauri (104 Tau) is the Flamsteed designation for a star in the equatorial constellation of Taurus. It has an apparent magnitude of 4.92, which is bright enough to be seen with the naked eye. Based upon parallax measurements, this star is located about 50 light years from the Sun. It is moving further from the Sun with a heliocentric radial velocity of +20 km/s.

Iota Delphini (ι Del, ι Delphini) is a star in the constellation Delphinus. It has an apparent magnitude of about 5.4, meaning that it is just barely visible to the naked eye. Based upon parallax measurements made by the Hipparcos spacecraft, this star is around 177 light years away from the Sun. Iota Delphini's spectral type is A1IV, meaning it is an A-type subgiant.

NGC 91 (PGC 3325956, GC 41, GC 5097, or NPD 68 22.9) is a star with an apparent magnitude of 14.4 in the constellation of Andromeda. The star is southwest of the galaxy NGC 90. Discovered in 1866 by Herman Schultz, there have been many arguments if this star exists or not. However, people have observed the star, and have confirmed that NGC 91 exists.

3360 Syrinx (originally designated 1981 VA) is an Apollo and Mars crosser asteroid discovered in 1981. It approaches Earth to within 40 Gm three times in the 21st century: 33 Gm in 2039, 40 Gm in 2070, and 24 Gm in 2085. On 2012-Sep-20 it passed from the Earth at apparent magnitude 17.0. In opposition on 23 November 2012, it brightened to magnitude 16.0.

47 Ophiuchi (47 Oph) is a binary star in the constellation Serpens. The combined apparent magnitude of the system is 4.54. The system is located about 98.1 light-years, or 30.1 parsecs away, based on its parallax as measured by Hipparcos. 47 Ophiuchi is a spectroscopic binary: that is, the two stars move fast enough that periodic Doppler shifts in the stars' spectra can be detected.

R Horologii is a red giant star approximately 1,000 light-years away in the southern constellation of Horologium. It is a Mira variable with a period of 404.83 days, ranging from apparent magnitude 4.7 to 14.3—one of the largest ranges in brightness known of stars in the night sky visible to the unaided eye. The star is losing mass at the rate of .

NGC 1977. (Mount Lemmon SkyCenter Schulman Telescope courtesy Adam Block 42 Orionis is a class B1V (blue main-sequence) star in the constellation Orion. Its apparent magnitude is 4.59 and it is approximately 900 light years away based on parallax. The primary star, Aa, has one spectroscopic companion Ab of magnitude 6.3 and separation 0.16", and a more distant companion B of 7.5 magnitude at 1.6" separation.

It was discovered on 23 May 2012 by the Mount Lemmon Survey at an apparent magnitude of 20.8 using a reflecting telescope. On 28 May 2012 at 15:20 UT, the asteroid passed from the center-point of Earth. The asteroid is estimated to be in diameter. It was removed from the Sentry Risk Table on 8 August 2013 after Sentry updated to planetary ephemeris (DE431).

7 Cancri (7 Cnc) is a giant star in the constellation Cancer. Its apparent magnitude is 6.84 and it is about away. The annual parallax of 7 Cancri determined from the Hipparcos satellite mission is , giving a distance of with an 11.5% margin of error. The more recent and more accurate Gaia Data Release 2 contains a parallax of , resulting in a closer distance of .

Two supernovae have been studied in the M58 galaxy. A type II supernova dubbed as SN 1988A was discovered by Kaoru Ikeya, Robert Evans, Christian Pollas and Shingo Horiguchi on January 18, 1988. It had an apparent magnitude of 13.5 and was located 40 arcseconds south of its center. A Type I supernova dubbed as SN 1989M was then found on June 28, 1989 by Kimeridze.

105P/Singer Brewster is a periodic comet in the Solar System. It was discovered in 1986, and received the name of 1986d under the old naming system. Because 105P/Singer Brewster only comes within 2 AU of the Sun, during the 2012 perihelion passage it is only expected to brighten to about apparent magnitude 17. The comet nucleus is estimated to be 2.2 kilometers in diameter.

13 Monocerotis (13 Mon) is a class A0 Ib (white supergiant) star in the constellation Monoceros. Its apparent magnitude is 4.5 and it is approximately away. 13 Mon lies within the Monoceros OB1 stellar association, halfway between the Rosette Nebula and NGC 2264, at a distance of about 780 parsecs. It is surrounded by a small reflection nebula listed as Van den Bergh 81 (VdB 81).

94P/Russell 4 is a periodic comet in the Solar System. It fits the definition of an Encke-type comet with (TJupiter > 3; a < aJupiter). It was discovered by Ken Rusell on photographic plates taken by M. Hawkins on March 7, 1984. In the discovery images, Russell estimated that the comet had an apparent magnitude of 13 and a noticeable tail of 5 arc minutes.

On July 2, Tralles found the comet to have a coma of 40″. On July 3, Friedrich Georg Wilhelm von Struve measured the nucleus at 8″ with a tail of several degrees. Heinrich Wilhelm Matthias Olbers reported that the nucleus had an apparent magnitude of 1–2 and a tail about 7–8° long. The comet was last sighted by Struve on October 25.

Discovered in 1956 by Olin Wilson and M.K. Vainu Bappu, the Wilson–Bappu effect utilizes the effect known as spectroscopic parallax. Many stars have features in their spectra, such as the calcium K-line, that indicate their absolute magnitude. The distance to the star can then be calculated from its apparent magnitude using the distance modulus. There are major limitations to this method for finding stellar distances.

Distance is not the only quantity relevant in determining the difference between absolute and apparent magnitude. Absorption is another important factor and it may even be a dominant one in particular cases (e. g. in the direction of the galactic center). Thus a distinction is made between distance moduli uncorrected for interstellar absorption (whose values would overestimate the distance if used naively) and absorption-corrected moduli.

V376 Carinae is a binary star system in the southern constellation of Carina. It has the Bayer designation b1 Carinae; V376 Carinae is the variable star designation. The system is visible to the naked eye as a faint point of light with a combined apparent magnitude of +4.69. The distance to this system from the Sun is approximately 650 light years based on parallax.

An Introduction to Mirages by Andy Young Here's how Jules Verne describes an inferior mirage sunset. : On very rare occasions the mirages of astronomical objects other than the Sun and the Moon might be observed. An apparent magnitude of an astronomical object should be low enough (that is, bright enough) in order to see it as not only a real object, but also a miraged one.

On 19 April 2017, it will reach its closest point to Earth of ~1.2 AU. At this point, it will be about apparent magnitude 8, and, assuming a size of 20 km, have an apparent size of 19 mas. It will come to perihelion (closest approach to the Sun) on 10 May 2017. It will not be 50 AU from the Sun until 2045.

The planet orbits a (K-type) star named Kepler-61. The star has a mass of 0.63 and a radius of 0.62 . It has a temperature of 4017 K and is about 1 billion years old. In comparison, the Sun is 4.6 billion years old and has a temperature of 5778 K. The star's apparent magnitude, or how bright it appears from Earth's perspective, is 15.

W Corvi is an eclipsing binary star system in the constellation Corvus, ranging from apparent magnitude 11.16 to 12.5 over 9 hours. Its period has increased by 1/4 second over a century. It is an unusual system in that its two stars are very close to each other yet have different surface temperatures and hence thermal transfer is not taking place as expected.

V352 Aurigae is a variable star in the northern constellation of Auriga. According to the Bortle scale, an apparent magnitude of 6.14 means that it is faintly visible to the naked eye from dark rural skies. It is a variable of Delta Scuti-type, which suggests that the variability is caused by the rotation of the host star in combination with localized regions of activity.

88 Tauri, also known as d Tauri, is a multiple star system in the constellation Taurus. It has an apparent magnitude of about 4.25, meaning that it is visible to the naked eye. Based upon parallax measurements made by the Hipparcos spacecraft, the star system is some from the Sun. 88 Tauri is a sextuple star system, meaning that it contains six stars in a hierarchical orbit.

This star is shining with 35 times the solar luminosity and has an effective temperature of 6,900 K. Its metallicity is high, with an overall metal abundance 25% greater the solar value. Gaia Data Release 2 discovered a star with the same proper motion and parallax as Rho Phoenicis. It has an apparent magnitude of 14.6 (G band) and is at a separation of 7.9 arcseconds.

1 Persei (1 Per) is an eclipsing binary star in the constellation Perseus. Its uneclipsed apparent magnitude is 5.49. The binary star consists of two B2 type main-sequence stars in a 25.9 day eccentric orbit. The stars are surrounded by a faint cloud of gas visible in mid-infrared, although whether they are the origin of the gas or simply passing through it is unclear.

At its brightest, Comet Lovejoy had an apparent magnitude of between and , which is about as bright as the planet Venus. It is the brightest sungrazing comet ever observed by SOHO, and the brightest comet to appear since Comet McNaught of 2007, which shone at visual magnitude . Nevertheless, Lovejoy was largely invisible to the naked eye during its peak brightness due to its proximity to the Sun.

35 Cygni is a spectroscopic binary star in the constellation Cygnus. Its apparent magnitude is 5.18. Located around distant, its primary is a yellow supergiant of spectral type F6Ib, a massive star that has used up its core hydrogen and is now fusing heavier elements. Yellow supergiants are usually variable, often Classical Cepheid variables, but 35 Cyg is notable for having an especially constant brightness.

There are 137 listed stars, but many are likely non- members, with only 36 having accurate photometric data. Total apparent magnitude of 5.3 and integrated spectral type of B1.7. NGC 3766 is relatively young that is estimated as log (7.160) or 14.4 million years, and approaching us at 14.8 km/s. This cluster contains eleven Be stars, two red supergiants and four Ap stars.

21 Leonis Minoris is a star in the constellation of Leo Minor. With an apparent magnitude of about 4.5, the star is faintly visible to the naked eye (see Bortle scale). Parallax estimates made by the Hipparcos spacecraft put it at a fairly close distance of about 92.1 light years (28.2 parsecs) away from the Earth. It is considered a member of the Sirius supercluster.

1.442 UT with a 0.35-m f/6.8 Schmidt-Cassegrain reflector. The supernova was located 56" east and 1" south of the center of NGC 691 and at the time of the discovery had an apparent magnitude of 15.2. Spectrographic observations indicated it was a type Ia supernova about a week before maximum. The peak magnitude of the supernova was 14.3, on February 10.759.

HD 137509, also known as NN Apodis, is a class B9p star in the constellation Apus. Its apparent magnitude is 6.87 and it is approximately 640 light years away based on parallax. It shines with a luminosity approximately 111 times that of the Sun and has a surface temperature of 12804 K. It has one of the strongest magnetic fields recorded for a chemically peculiar star.

HD 137388, named Karaka, is a class K2IV (orange subgiant) star in the constellation Apus. Its apparent magnitude is 8.70 and it is approximately 132 light years away based on parallax. It has a surface temperature of and is 58% as luminous and 93% as massive as the Sun, with 86% of its diameter, and is thought to be around 2.99 billion years old.

66P/du Toit is a periodic comet in the Solar System with a current orbital period of 14.78 years. It will next come to perihelion on 2018 May 19 at roughly apparent magnitude 12. It was discovered by Daniel du Toit at the Boyden Observatory, South Africa on 16 May 1944, who estimated its brightness at magnitude 10. Other observers estimated magnitude 11 and 12.5.

SN 2014J was a type-Ia supernova in Messier 82 (the 'Cigar Galaxy', M82) discovered in mid-January 2014. It was the closest type-Ia supernova discovered for 42 years, and none have been closer . The supernova was discovered by chance during an undergraduate teaching session at the University of London Observatory. It peaked on 31 January 2014, reaching an apparent magnitude of 10.5.

The angular diameter of Aldebaran has been measured many times. The value adopted as part of the Gaia benchmark calibration is . It is 44 times the diameter of the Sun, approximately 61 million kilometres. Aldebaran is a slightly variable star, assigned to the slow irregular type LB. The General Catalogue of Variable Stars indicates variation between apparent magnitude 0.75 and 0.95 from historical reports.

NGC 6540 is a globular cluster in the constellation Sagittarius. Its apparent magnitude is 9.3 and its diameter is about 9.5 arcminutes, with 12 faint stars visible. It is about 17,000 light years away from Earth and was discovered by Wilhelm Herschel on May 24, 1784 with an 18.7-inch mirror telescope, who described the cluster as "pretty faint, not large, crookedly extended, easily resolvable".

NGC 6553 is a globular cluster in the constellation Sagittarius. NGC 6553 has an apparent magnitude of about 8 magnitudes with an apparent diameter of 8.2 arcminutes. Its Shapley–Sawyer Concentration Class is XI, meaning the star concentration is very loose even at the center; it has stars of magnitude 20 and dimmer. It is located just over a degree southeast of Messier 8, the Lagoon Nebula.

Delphinus' five brightest stars form a distinctive asterism symbolizing a dolphin with four stars representing the body and one the tail. It is bordered (clockwise from north) by Vulpecula, Sagitta, Aquila, Aquarius, Equuleus and Pegasus. Delphinus is a faint constellation with only two stars brighter than an apparent magnitude of 4, Beta Delphini (Rotanev) at magnitude 3.6 and Alpha Delphini with a magnitude of 3.8.

Hercules is a constellation named after Hercules, the Roman mythological hero adapted from the Greek hero Heracles. Hercules was one of the 48 constellations listed by the second-century astronomer Ptolemy, and it remains one of the 88 modern constellations today. It is the fifth-largest of the modern constellations and is the largest of the 50 which have no stars brighter than apparent magnitude +2.5.

Calibrator stars close in the sky to the target are favoured (to avoid large differences in the atmospheric paths). If those stars have somewhat different zenith angles (altitudes) then a correction factor as a function of airmass can be derived and applied to the airmass at the target's position. Such calibration obtains the brightnesses as would be observed from above the atmosphere, where apparent magnitude is defined.

The five brightest stars are all reddish in hue. Shading the others at apparent magnitude 3.8 is Alpha Apodis, an orange giant that has around 48 times the diameter and 928 times the luminosity of the Sun. Marginally fainter is Gamma Apodis, another ageing giant star. Delta Apodis is a double star, the two components of which are 103 arcseconds apart and visible with the naked eye.

However, it does not pose an impact risk for the foreseeable future. Its last notable close approach to Earth was on 11 March 1992 passing from Earth. The last notable close approach was on 21 March 2018 passing from Earth and shining at an apparent magnitude of +12.4. The next notable close approach will be on 14 September 2032 passing slightly closer at from Earth.

Criteria in the choice of stars includes their distribution across the celestial sphere, brightness, and ease of identification.Wright and Whitney, 1992, p. 273. Information for another 115 stars, known as "tabulated stars", is also available to the navigator. This list provides information on the name, approximate position in the celestial sphere, and apparent magnitude of the 58 selected stars in tabular form and by star charts.

53 Piscium, abbreviated as 53 Psc, is a star in the zodiac constellation of Pisces. With an apparent magnitude of about 5.9, it is just barely visible to the naked eye. parallax measurements made by the Hipparcos spacecraft place the star at a distance of about 1,040 light-years (320 parsecs) away. The spectral type of 53 Piscium is B2.5IV, meaning it is a B-type subgiant.

IC 2488 lies 30 arcminutes west of N Velorum, a 3rd magnitude star located near the False Cross asterism. Stephen James O'Meara estimates the overall apparent magnitude of the cluster to be 6.0. The cluster is coarse. The cluster can be spotted with 7x50 binoculars and with a 4 inches telescope the cluster can be resolved in 30 stars in a northwest-southeast direction.

HD 154672 is far older than the Sun, as its estimated gyrochronological age is estimated at 9.28 billion years. HD 154672's spectrum suggests that the star's chromosphere (its outer layer) is not active. HD 154672 is located 65.8 parsecs (214.6 light years) away from Earth. It has an apparent magnitude (V) of 8.22, making the star too dim to see from Earth with the naked eye.

Gliese 754 is a red dwarf star of spectral type M4.5V in the constellation Telescopium. It has an apparent magnitude of 12.23 and is around 19.3 light- years distant. It is one of the hundred closest stars to the Solar System. Calculations of its orbit around the Milky Way showed that it was eccentric, and indicate that it might be a thick disk object.

Octans is a very faint constellation; its brightest member is Nu Octantis, a spectral class K1 III giant star with an apparent magnitude 3.73. It is 63.3 ± 0.8 light-years distant from Earth. Beta Octantis is the second brightest star in the constellation. Sigma Octantis, the southern pole star, is a magnitude 5.4 star just over 1 degree away from the true South Celestial Pole.

These characteristics are understood to result from relativistic beaming of emission from a jet of plasma ejected from the vicinity of a supermassive black hole. BL Lac objects are also categorized as a type of blazar. BL Lacertae changes in apparent magnitude over fairly small time periods between values of 14 and 17. Its location in the sky for epoch 2000.0 is at RA , DEC .

HD 196050 is a triple star system located in the southern constellation of Pavo. This system has an apparent magnitude of 7.50 and the absolute magnitude is 4.01. It is located at a distance of 112 light years from the Sun based on parallax, and is drifting further away with a radial velocity of +61 km/s. It is also called by the Hipparcos number 101806.

RS Ophiuchi (RS Oph) is a recurrent nova system approximately 5,000 light- years away in the constellation Ophiuchus. In its quiet phase it has an apparent magnitude of about 12.5. It has been observed to erupt in 1898, 1933, 1958, 1967, 1985, and 2006 and reached about magnitude 5 on average. A further two eruptions, in 1907 and 1945, have been inferred from archival data.

Gamma1 is a blue-white star of spectral type B2III and apparent magnitude 4.3. The two pairs are separated by 41 arcseconds, easily separable in binoculars. Parallax measurements give a distance of 1,116 light-years, meaning that they are at least 12,000 AU apart. Further afield are 7.3-magnitude Gamma Velorum C and 9.4-magnitude Gamma Velorum D, lying 62 and 93 arcseconds south-southeast from Gamma2.

The white dwarf has a mass of 0.54 , a temperature of 10,530 ± 140 K and a log (g) of 7.86 ± 0.06. The apparent magnitude of the star, or how bright it appears from Earth's perspective, is about 18.4. Therefore, it is too dim to be seen with the naked eye. The star has been found to display deep, irregularly shaped transits suggestive of disrupted planetary debris.

Epsilon Tucanae traditionally marks the toucan's left leg. A B-type subgiant, it has a spectral type B9IV and an apparent magnitude of 4.49. It is approximately 373 light-years from Earth. It is around four times as massive as our Sun. Theta Tucanae is a white A-type star around 423 light- years distant from Earth, which is actually a close binary system.

It has an apparent magnitude of 10.3. Within it lies the triple star system HD 5980, each of its members among the most luminous stars known. Open star cluster NGC 299 is located within the Small Magellanic Cloud. The Tucana Dwarf galaxy, which was discovered in 1990, is a dwarf spheroidal galaxy of type dE5 that is an isolated member of the Local Group.

Another ageing star, Kappa Telescopii is a yellow giant with a spectral type G9III and apparent magnitude of 5.18. Around 1.87 billion years old, this star of around 1.6 solar masses has swollen to 11 times the Sun's diameter. It is approximately 293 light- years from Earth, and is another optical double. Xi Telescopii is an irregular variable star that ranges between magnitudes 4.89 and 4.94.

Location of HR 6819 the star system containing the black hole. Telescopium is also host to the first known visible star system with a black hole. QV Telescopii, also designated HR 6819, is a triple star system, which is visible to the unaided eye as a variable star with apparent magnitude 5.32 to 5.39. It is located in Telescopium near its SW corner with Ara and Pavo.

At an apparent magnitude of 1.94, this is the brightest star in Pavo. Based upon parallax measurements, this star is about distant from the Earth. It has an estimated six times the Sun's mass and 6 times the Sun's radius, but 2,200 times the luminosity of the Sun. The effective temperature of the photosphere is 17,700 K, which gives the star a blue-white hue.

25, p.245 Hipparchus, in the 1st century B.C., introduced the magnitude scale. He allocated first magnitude to the 20 brightest stars and the sixth magnitude to the faintest stars visible to the naked eye. In the 19th Century, this ancient scale of apparent magnitude was logarithmically defined—so that a star of 1.00 mag is exactly 100 times brighter than a star of 6.00 magnitude.

On 4 February 2018 at 21:31 UT, the asteroid passed about from Earth. The 2018 Earth approach distance was known with a 3-sigma accuracy of ±200 km. Goldstone is scheduled to observe the asteroid from 3 to 6 February. By 4 February 2018 11:00 UT, the asteroid brightened to apparent magnitude 14 and had a solar elongation of more than 100°.

It has a Jupiter-sized planet with an orbital period of 280 days that was discovered by the radial velocity method. WASP-7 is a star of spectral type F5V with an apparent magnitude of 9.54, about 1.28 times as massive as the Sun. Its hot Jupiter planet—WASP-7b—was discovered by transit method and found to orbit the star every 4.95 days.

Zeta Delphini (ζ Delphini) is a star in the constellation of Delphinus. With an apparent magnitude of about 4.6, it is faintly visible to the naked eye. Parallax measurements of the system made by the Hipparcos spacecraft put it at a distance of about 220 light-years, or 67 parsecs. Zeta Delphini has a spectral type of A3V, implying it is an A-type main-sequence star.

With a low-power telescope, Messier 13 looks like a comet or fuzzy patch. The cluster is visible throughout the year from latitudes greater than 36 degrees north, with the longest visibility during Northern Hemisphere spring and summer. It is located at right ascension 16h 41.7m, declination +36° 28'. With an apparent magnitude of 5.8, it is barely visible with the naked eye on clear nights.

13 Scorpii, also known by its Bayer designation c2 Scorpii, is a binary star in the constellation Scorpius. Its apparent magnitude is 4.57, meaning it can be faintly seen with the naked eye. Based on parallax estimates made by the Hipparcos spacecraft, the system is located about 480 light-years (147 parsecs) away. It is located within the Upper Scorpius subgroup of the Scorpius–Centaurus Association.

NGC 7582 is a spiral galaxy of the Hubble type SB(s)ab in the constellation Grus. It has an angular size of 5.0' × 2.1' and an apparent magnitude of 11.37. It is about 70 million light years away from Earth and has a diameter of about 100,000 light years. The galaxy is classified as a Seyfert 2 galaxy, a type of active galaxy.

Animation of the apparent retrograde motion of Mars in 2003 as seen from Earth. The mean apparent magnitude of Mars is +0.71 with a standard deviation of 1.05. Because the orbit of Mars is eccentric, the magnitude at opposition from the Sun can range from about −3.0 to −1.4. The minimum brightness is magnitude +1.86 when the planet is in conjunction with the Sun.

Comparison of its properties with model evolutionary tracks suggest that it is a main sequence star about three quarters of the way through its main sequence lifetime. The apparent magnitude varies from +4.33 to +4.36 with a period of 5.03 hours. Its pulsations cause its radius to vary by 1.0% to 1.5%. At the same time its effective temperature by about above and below its mean temperature.

UGC 9391 is a Magellanic spiral galaxy in constellation Draco. 130 milion light years from Earth, it is not a member of any group of galaxies, and is moving away from the Earth at 1939 km/s. The Hubble Space Telescope took a photo of Draco in 2016. In 2003, a supernova catalogued as SN 2003du was detected within the galaxy, with an apparent magnitude of 15.9.

Zeta Scuti, Latinized from ζ Scuti, is the Bayer designation for a star in the southern constellation of Scutum. It is a faint star but visible to the naked eye with an apparent magnitude of 4.66. The distance to this star, as determined via parallax measurement, is around 210 light years. It is moving closer to the Sun with a radial velocity of −5 km/s.

Delta Sculptoris (δ Scl, δ Sculptoris) is a triple star system in the constellation Sculptor. It is approximately 137.4 light years from Earth. The primary component, Delta Sculptoris A, is a white A-type main sequence dwarf with an apparent magnitude of +4.59. It has a faint, 11.6 magnitude companion, Delta Sculptoris B, 4 arcseconds, or more than 175 astronomical units, away from it.

Nu Eridani (ν Eri) is a star in the constellation Eridanus. It is visible to the naked eye with an apparent visual magnitude of 3.93. The distance to this star is roughly 520 light years, based upon an annual parallax shift of 0.00625 arcseconds. If the star were from the Sun, it would be the brightest star in the night sky with an apparent magnitude of −2.84.

HD 126053 is the Henry Draper Catalogue designation for a star in the equatorial constellation of Virgo. It has an apparent magnitude of 6.25, which means it is faintly visible to the naked eye. According to the Bortle scale, it requires dark suburban or rural skies to view. Parallax measurements made by the Hipparcos spacecraft provide an estimated distance of 57 light years to this star.

The planet orbits a (K-type) star named Kepler-1520. The star has a mass of 0.76 and a radius of 0.71 . It has a temperature of 4677 K and is 4.47 billion years old. In comparison, the Sun is 4.6 billion years old and has a surface temperature of 5778 K. The star's apparent magnitude, or how bright it appears from Earth's perspective, is 16.7.

Theta Tauri A has a mean apparent magnitude of +3.40. It is classified as a Delta Scuti type variable star and its brightness varies from magnitude +3.35 to +3.42 with a period of 1.82 hours. Its primary component, Theta Tauri Aa, is a white A-type giant. The secondary, Theta Tauri Ab, is of the 6th magnitude and is 0.005 arcseconds, or at least 2 AU, distant.

The brightening was insufficient to be a supernova, and is called a failed supernova. The star's coordinates were at RA and Dec . The brightness of the star, given by its apparent magnitude in different colour bands on 2 July 2005 is given by R = 21, V = 21, B = 22, U = 23. Prior to the optical outburst the star was about 100,000 times as bright as the sun.

Alpha Cancri is a fourth-magnitude star with an apparent magnitude of 4.20, making it barely visible to the naked eye under good lighting conditions. Nevertheless, it is 23 times more luminous than the Sun. Its stellar classification is A5m. The distance of Alpha Cancri calculated from the Gaia Data Release 2 parallax is roughly 50 parsecs from Earth, or approximately 164 light years away.

Theta Aquarii (θ Aquarii, abbreviated Theta Aqr, θ Aqr), officially named Ancha (distinguish Ankaa, with the same pronunciation), is a star in the equatorial constellation of Aquarius. Visible to the naked eye at apparent magnitude 4.175, it is located at a distance of around from the Sun. Since it is near the ecliptic it can be occulted by the Moon, or very rarely by planets.

S Microscopii is a star in the constellation Microscopium. It is a red giant star of spectral type M3e-M5.5 that is also a Mira variable, with an apparent magnitude ranging between 7.4 and 14.8 over 210 days. The Astronomical Society of Southern Africa in 2003 reported that observations of S Microscopii were very urgently needed as data on its light curve was incomplete.

HD 125823, also known as V761 Centauri or a Centauri, is a star in the constellation Centaurus. It is a blue-white B-type giant with a mean apparent magnitude of +4.41. It is approximately 460 light years from Earth. It is classified as an SX Arietis type variable star and its brightness varies from magnitude +4.38 to +4.43 with a period of 8.82 days.

J Centauri (J Cen) is a star in the constellation Centaurus. It is approximately 350 light years from Earth. J Centauri is a spectral class B3V main sequence star with a mean apparent magnitude of 4.5 and a luminosity 500 times that of the Sun. The temperature of the star's photosphere is nearly 24,000 K. The rotation velocity at the equator is at least 223 km/s.

The planet orbits an (F-type) star named Kepler-419. The star has a mass of 1.39 and a radius 1.75 . It has a surface temperatures of 6430 K and is 2.8 billion years old. In comparison, the Sun is about 4.6 billion years old and has a surface temperature of 5778 K. The star's apparent magnitude, or how bright it appears from Earth's perspective, is 13.

LkCa 15 is a T Tauri star in the Taurus-Auriga Star Forming Region. These types of stars are relatively young pre-main-sequence stars that show irregular variations in brightness. It has a mass that is about 97% of the Sun, an effective temperature of 4370 K, slightly cooler than the Sun. Its apparent magnitude is 11.91, meaning it is not visible to the naked eye.

The Trapezium is most readily identifiable by the asterism of four relatively bright stars for which it is named. The four are often identified as A, B, C, and D in order of increasing right ascension. The brightest of the four stars is C, or Theta1 Orionis C, with an apparent magnitude of 5.13. Both A and B have been identified as eclipsing binaries.

HD 7853 is a double star in the constellation Andromeda. With an apparent magnitude of 6.46, the stars can barely be seen with the naked eye even on the best of nights. The system is located approximately distant, and the brighter star is an Am star, meaning that it has unusual metallic absorption lines. The spectral type estimates of the primary range between A4 and A9.

171 Puppis (171 Pup) is a triple star system in the constellation of Puppis – the stern of Argo Navis – of apparent magnitude +5.38. Lacking a Bayer designation, it is instead known by its Gould designation. Based upon parallax measurements, the system is 49.6 light years away from the Solar System. The inner pair form a spectroscopic binary with an orbital period of around 10 years.

DD Microscopii, also known as CD-43 14304, is a binary star system in the constellation Microscopium. Its apparent magnitude is 11.0.SIMBAD, DD Microscopii (accessed 25 March 2015) It is a symbiotic star system composed of an orange giant of spectral type K2III and white dwarf in close orbit, with the smaller star ionizing the stellar wind of the larger star. The system is metal-poor.

Alpha Caeli (α Cae, α Caeli) is a double star system in the constellation Caelum. Alpha Caeli A is an F-type main sequence star with a stellar classification of F2V and an apparent magnitude of +4.44. It has 1.48 times the mass of the Sun and 1.3 times the solar radius. The projected rotational velocity at the stellar equator is 47.8 km/s.

Appearing to have moved off the main sequence as their core hydrogen supply is being or has been exhausted, they are enlarging and cooling to eventually become red giant stars. Markab has an apparent magnitude of 2.48, while Algenib is a Beta Cephei variable that varies between magnitudes 2.82 and 2.86 every 3 hours 38 minutes, and also exhibits some slow pulsations every 1.47 days. Eta and Omicron Pegasi mark the left knee and Pi Pegasi the left hoof, while Iota and Kappa Pegasi mark the right knee and hoof. Also known as Matar, Eta Pegasi is the fifth-brightest star in the constellation. Shining with an apparent magnitude of 2.94, it is a multiple star system composed of a yellow giant of spectral type G2 and a yellow-white main sequence star of spectral type A5V that are 3.2 and 2.0 times as massive as our Sun.

Even at this great distance this blazar has an apparent magnitude of about 15.5. Although 0.444 is used as the common redshift value, 0.3347 is a new strict lower limit "inferred through observing the far-UV absorption by the low-z IGM." 3C 66A underwent an optical outburst in 2007 August, as monitored by the Tuorla blazar monitoring program. The event was monitored by the Whole Earth Blazar Telescope project.

At the estimated distance of Eta Draconis, this yields a physical size of about 57 times the radius of the Sun. The companion, η Sagittarii B, was first noted by American astronomer S. W. Burnham in 1879. The two stars share a common proper motion and hence are probably gravitationally bound to each other. The secondary is likely an F-type main sequence star with an apparent magnitude of +7.77.

NGC 1987 (also known as ESO 56-SC131) is an open cluster or a globular cluster located in the Mensa constellation and part of the Large Magellanic Cloud. It was discovered by John Herschel on November 3, 1834. Its apparent magnitude is 12.1, and its size is 1.7 arc minutes. It is thought to be around 600 million years old and has a significant number of red ageing stars.

Spectroscopic analysis and calculation gave an estimate of 125 parsecs (407.5 light years). The system consists of a white dwarf and a donor star which orbit around a common centre of gravity every 1.5 hours. The white dwarf sucks matter from the other star onto an accretion disc and periodically erupts, reaching apparent magnitude 11.2 in superoutbursts, 12.1 in normal outbursts and remaining at magnitude 16.7 when quiet.

Ross 128 is a red dwarf in the equatorial zodiac constellation of Virgo, near β Virginis. The apparent magnitude of Ross 128 is 11.13, which is too faint to be seen with the unaided eye. Based upon parallax measurements, the distance of this star from Earth is , making it the twelfth closest stellar system to the Solar System. It was first cataloged in 1926 by American astronomer Frank Elmore Ross.

Using multiple bandpass filters with relative photometry is termed absolute photometry. A plot of magnitude against time produces a light curve, yielding considerable information about the physical process causing the brightness changes. Precision photoelectric photometers can measure starlight around 0.001 magnitude. The technique of surface photometry can also be used with extended objects like planets, comets, nebulae or galaxies that measures the apparent magnitude in terms of magnitudes per square arcsecond.

According to measurements from the Gaia spacecraft, HD 28185 has a parallax of 25.3642 milliarcseconds, which corresponds to a distance of 39.43 parsecs (128.6 light-years). Since the star is located further than 25 parsecs from Earth, it is not listed in the Gliese Catalogue of Nearby Stars. With an apparent magnitude of 7.81, the star is not visible with the naked eye, though it can be seen using binoculars.

HD 170657 is a star in the constellation Sagittarius. It is located at a distance of about 43 light years. It has 0.79 solar masses and is a suspected variable star that varies in apparent magnitude from 6.82−6.88. When observed with the Spitzer Space Telescope, this star did not display an excess emission of infrared radiation, which may otherwise indicate the presence of an orbiting debris disk.

Its luminosity in different bands of the thermal infrared in combination with its absolute magnitude—because of its known distance—was used to place it in context of different models; the best characterization of its brightness was in the W2 band of at an apparent magnitude of , though it was brighter into the deeper infrared. Infrared images taken with the Magellan Baade Telescope suggest evidence of water clouds.

138P/Shoemaker–Levy, also known as Shoemaker–Levy 7, is a faint periodic comet in the Solar System. The comet last came to perihelion on 11 June 2012, but only brightened to about apparent magnitude 20.5. There were 4 recovery images of 138P on 8 August 2018 by Pan-STARRS when the comet had a magnitude of about 21.5. The comet comes to perihelion on 2 May 2019.

X Trianguli Australis is a star in the southern constellation Triangulum Australe. It is a red-hued carbon star with an average apparent magnitude of +5.89. It is approximately 1173 light years (360 parsecs) from Earth, though this could vary by up to 200 light years. It is a semi-regular variable star with two periods of around 385 and 455 days, and is of spectral type C5.5(Nb).

Zeta Ursae Minoris (ζ UMi, ζ Ursae Minoris) is a star in the constellation Ursa Minor. It is a white stellar class A-type main sequence star with an apparent magnitude of +4.28. It is approximately 380 light years from Earth. Despite its classification as a main sequence dwarf star, Zeta UMi is 3.4 times the mass of the sun and its luminosity is about 200 solar luminosities.

Asteroids in the range of several meters in diameter are very hard to detect as they are too small to reflect much sunlight. For example, on 24 May 2018, the asteroid was still from Earth and only had an apparent magnitude of 25.5, much dimmer than any major modern surveys can detect using rapid-fire 30 second snapshots meant to cover as much of the sky as possible.

On 7 February 2018 it passed from the Earth when its apparent magnitude brightened to 14. Goldstone observed it until the following day. While this was an 8.1-million kilometer flyby, the next close flyby of 6.3 million km will occur on 5 February 2058, and another 7.6 million km on 8 February 2095. It will also have a 3.2 million km flyby of Mars on 26 September 2048.

A double star, it has a companion of magnitude 13; the two are separated by 11 arcseconds. Beta Pictoris Comparison Located about 1298 light-years from Earth, Delta Pictoris is an eclipsing binary of the Beta Lyrae type. Composed of two blue stars of spectral types B3III and O9V, the system has a period of 1.67 days, and is observed to dip from apparent magnitude 4.65 to 4.9.

Flamsteed's listing of Nu1, Nu2, Nu3, Xi1, Xi2, Omicron1 and Omicron2 have all remained in use. Canis Major as depicted in Urania's Mirror, a set of constellation cards published in London c.1825. Next to it are Lepus and Columba (partly cut off). Sirius is the brightest star in the night sky at apparent magnitude −1.46 and one of the closest stars to Earth at a distance of 8.6 light-years.

163P/NEAT is a periodic comet discovered on November 5, 2004 by Near-Earth Asteroid Tracking (NEAT) using the 1.2 meter Samuel Oschin telescope at Palomar Observatory. Precovery images of the comet were found by Maik Meyer in December 2004. There were two images from 1997, two images from 1991, and three images from 1990. During the 2005 perihelion passage the comet brightened to about apparent magnitude 16.

Epsilon Coronae Australis is an eclipsing binary belonging to a class of stars known as W Ursae Majoris variables. These star systems are known as contact binaries as the component stars are so close together they touch. Varying by a quarter of a magnitude around an average apparent magnitude of 4.83 every seven hours, the star system lies 98 light years away. Its spectral type is F4VFe-0.8+.

Theta Chamaeleontis, Latinized from θ Cha, is a single, orange-hued star located in the southern constellation of Chamaeleon. It is a dim star but visible to the naked eye with an apparent magnitude of 4.34. Parallax measurements by the Hipparcos spacecraft put the system at 155 light-years, or 47.6 parsecs away. It is moving away from the Sun with a radial velocity of +22 km/s.

62P/Tsuchinshan, also known as Tsuchinshan 1, is a periodic comet discovered on 1965 January 1 at Purple Mountain Observatory, Nanking. During the 2004 perihelion passage the comet brightened to about apparent magnitude 11. The comet was not observed during the 2011 unfavorable apparition since the perihelion passage occurred when the comet was on the far side of the Sun. On 2049 April 2 the comet will pass about from Mars.

BO Carinae, also known as HD 93420, is an irregular variable star in the constellation Carina. BO Car has a maximum apparent magnitude of +7.18. Its distance and membership is uncertain, but its possible membership to the star cluster Trumpler 15 allows a distance estimate of approximately (). The Gaia Data Release 2 parallax of suggests a closer distance, but the value is considered unreliable due to excess astrometric noise.

Cosmic dust clouds in Messier 78. In 1922, Edwin Hubble published the result of his investigations on bright nebulae. One part of this work is the Hubble luminosity law for reflection nebulae, which makes a relationship between the angular size (R) of the nebula and the apparent magnitude (m) of the associated star: :5 log(R) = -m + k where k is a constant that depends on the sensitivity of the measurement.

Along with Kepler-11c, Kepler-11 is host to the planets Kepler-11b, Kepler-11d, Kepler-11e, Kepler-11f, and Kepler-11g. The inner five planets' orbits would fit within the orbit of planet Mercury, while Kepler-11g orbits Kepler-11 at a much further distance in comparison to the inner components. With an apparent magnitude of 14.2, Kepler-11 cannot be seen from Earth with the naked eye.

It is the second-brightest natural object in the night sky after the Moon, reaching an apparent magnitude of −4.6, bright enough to cast shadows. Because Venus orbits within Earth's orbit it is an inferior planet. Venus is a terrestrial planet and is sometimes called Earth's "sister planet" because of their similar size, mass, proximity to the Sun, and bulk composition. It is radically different from Earth in other respects.

It was discovered on 27 May 1998, by astronomers of the Lincoln Near-Earth Asteroid Research (LINEAR) at Lincoln Laboratory's ETS near Socorro, New Mexico, at an apparent magnitude of 17.6 using a reflector. It was tracked through 9 June 1998. It was recovered on 28 December 2003 which extended the observation arc by 5 years. Two precovery images from January 1990 extended the observation arc by 8 years.

The primary component, 3 Camelopardalis Aa, is an orange K-type giant with a mean apparent magnitude of +5.07. It rotates once every 121 days, matching the orbital period with its close companion. It was thought to be a short period Cepheid variable when it was first investigated, but has since been classified as a probable RS Canum Venaticorum variable. The tital amplitude of its variations is less than 0.1 magnitudes.

TT Aquilae (TT Aql) is a Classical Cepheid (δ Cep) variable star in the constellation Aquila. The visual apparent magnitude of TT Aql ranges from 6.52 to 7.65 over 13.7546 days. The light curve is asymmetric, with the rise from minimum to maximum brightness only taking half the time of the fall from maximum to minimum. TT Aql is a yellow-white supergiant around five thousand times brighter than the sun.

Gliese 908 is a red dwarf star, located in constellation Pisces at 19.3 light- years from Earth. It is a BY Draconis variable star with a variable star designation of BR Piscium. Its apparent magnitude varies between magnitude 8.93 and magnitude 9.03 as a result of starspots and varying chromospheric activity. The variability of Gliese 908 was confirmed in 1994, although no period could be detected in its brightness changes.

The brightness changes are due to starspots and chromospheric activity combined with the rotation of the star. It has been given the variable star designation EE Leonis. Like the vast majority of stars in the Solar neighborhood, Gliese 402 is a dim red dwarf. With an apparent magnitude +11.66, it is far too dim to be seen with the naked eye; it can only be seen with a telescope.

HD 104304 (24 G. Virginis) is a binary star in the zodiac constellation Virgo. It has an apparent magnitude of 5.54, making it visible to the unaided eye under suitable viewing conditions. The stellar classification of G8 IV means that this is a subgiant star that has left the main sequence and has begun to evolve into a giant star. In 2007, a candidate planet was announced orbiting this star.

55 Cygni (55 Cyg) is a blue supergiant star in the constellation Cygnus. It is thought to be a member of the Cygnus OB7 stellar association at about 2,700 light years. Its apparent magnitude is 4.86, but this is slightly variable and the star is also called V1661 Cyg. When first analysed, it was classified as an irregular supergiant variable, but subsequent studies have treated it as an Alpha Cygni variable.

OU Puppis (OU Pup) is a class A0 (white main-sequence) star in the constellation Puppis. Its apparent magnitude is 4.87 and it is approximately 184.4 light years away based on parallax. It is an α² CVn variable, ranging from 4.93 to 4.86 magnitude with a period of 0.92 days. Unlike the majority of star pairs, the number attached to the Bayer designation 'L' is generally a subscript: L1.

Sigma Cygni, Latinised from σ Cygni, is a blue supergiant star in the constellation Cygnus. Its apparent magnitude is 4.2. It belongs to the Cygnus OB4 stellar association and is located approximately 3,300 light years away from Earth. Because of its location at the galactic disk, σ Cyg is obstructed by interstellar dust and is reddened by around 0.2 magnitudes and loses about 0.6 magnitudes at visual wavelengths.

It is an SX Arietis variable with a period of 1.9093 days which is also the rotational period of the star. The total amplitude is 0.015 apparent magnitude. k2 Puppis is a chemically peculiar star with a strong magnetic field. It is classified as a He-weak star and in addition to a deficit of helium in its spectrum, it shows an overabundance of many iron peak and rare earth elements.

S Trianguli Australis is a yellow-white hued variable star in the constellation Triangulum Australe. It is a dim star near the lower limit of visibility with the naked eye, having a typical apparent visual magnitude of 6.41. Based upon an annual parallax shift of , it is located 3,030 light years from the Earth. A Classical Cepheid variable, its apparent magnitude ranges from 5.95 to 6.81 over 6.32344 days.

Nebula IC 405 around AE Aurigae AE Aurigae is a blue O-type main sequence dwarf with a mean apparent magnitude of +6.0. It is classified as an Orion type variable star and its brightness varies irregularly between magnitudes +5.78 and +6.08. It is approximately 1,300 light-years from Earth. AE Aur is a runaway star that might have been ejected during a collision of two binary star groups.

24 Aquarii is a triple star system in the equatorial constellation of Aquarius. 24 Aquarii is the Flamsteed designation. The apparent magnitude of this system is 6.66, which, according to the Bortle Dark-Sky Scale, means it is a faint star that is just visible to the naked eye from dark, rural skies. It has an annual parallax shift of , which is equivalent to a distance of from Earth.

Theta Boötis has apparent magnitude +4.05 and belongs to the spectral class F7V. It is approximately 47 light years from Earth. From about 4300 BC until 3942 BC, it was the closest star to the celestial north pole visible to the naked eye, although it was still too dim to be regarded as a pole star. There is a nearby 11th magnitude optical companion star about 70 arcseconds away.

63 Aurigae is a single star located around 395 light years away from the Sun in the northern constellation of Auriga. It is visible to the naked eye as a faint, orange-hued star with an apparent magnitude of 4.91. It is moving closer to the Earth with a heliocentric radial velocity of −28 km/s. This is an evolved giant star with a stellar classification of K4 III.

9 Aurigae (9 Aur) is a star system in Auriga (constellation). It has an apparent magnitude of about 5, making it visible to the naked eye in many suburban skies. Parallax estimates made by the Hipparcos spacecraft put it at about 85.7 light-years (26.3 parsecs) from the solar system. It is a well- studied Gamma Doradus variable, and was one of the first stars to be so- classified.

65 Andromedae, abbreviated 65 And, is a single, orange-hued star in the northern constellation of Andromeda. With an apparent magnitude is 4.73, it is visible to the naked eye. The distance to 65 And can be derived from its annual parallax shift of , which yields a range of around 440 light years. At that distance, its brightness is diminished by an extinction of 0.16 magnitude due to interstellar dust.

19 Aquarii is a star in the zodiac constellation of Aquarius. With an apparent magnitude of about 5.7, the star is barely visible to the naked eye as a white-hued star (see Bortle scale). Parallax estimates put it at a distance of about 260 light years away from the Sun. The star is moving closer to the Earth with a heliocentric radial velocity of −21 km/s.

62 Andromedae, abbreviated 62 And, is a single star in the northern constellation Andromeda. 62 Andromedae is the Flamsteed designation; it also bears the Bayer designation of c Andromedae. It's bright enough to be seen by the naked eye, with an apparent magnitude is 5.31. Based upon parallax measurements made during the Gaia mission, it is at a distance of roughly 273 light-years (84 parsecs) from Earth.

The NGC 2841 group is a group of galaxies about 19.6 million light-years away from Earth. It includes the loose triplet NGC 2541, NGC 2500, and NGC 2552. NGC 2841 is the fourth-brightest galaxy in Ursa Major with an apparent magnitude of 9.2. It is 20' southeast of 3 Lyncis and just below the halfway point of an imaginary line between Theta and 15 Ursae Majoris.

By 1 November 2013, the comet was visible to the naked eye near the Beehive Cluster (M44), about halfway between Jupiter and Regulus. It became more impressive than comet ISON. In binoculars, the comet has the appearance of a green, unresolved globular cluster. C/2013 R1 made its closest approach to Earth on 19 November 2013 at a distance of , and reached an apparent magnitude of about 4.5.

Map of the constellation Mons Maenalus Mons Maenalus (Latin for Mount Maenalus) was a constellation created by Johannes Hevelius in 1687. It was located between the constellations of Boötes and Virgo, and depicts a mountain in Greece that the herdsman is stepping upon. It was increasingly considered obsolete by the latter half of the 19th century. Its brightest star is 31 Boötis, a G-type giant of apparent magnitude 4.86m.

Psi2 Aurigae (also known as 50 Aurigae), with an apparent magnitude of 4.8, was the brightest star in the constellation, Bode assigning it the designation 'a'. Located 420 ± 20 light-years distant from earth, Note: see VizieR catalogue I/311. it is an orange giant of spectral type K3III. Other stars belonging to the constellation include Psi4, Psi5, Psi7, 63, 64, 65 and 66 Aurigae, and Omicron Geminorum.

Mu2 Octantis (μ2 Oct) is a binary star system of two G-type main-sequence stars. It shares the designation μ with μ1 Octantis, from which it is separated by 50 arcminutes. The primary star (A) is HD 196067, whose data is in the starbox. The secondary star (B) is HD 196068 (HIP 102128, LTT 8160), another G-type main-sequence star with an apparent magnitude of 7.18.

Deneb () is a first-magnitude star in the constellation of Cygnus, the swan. Deneb is one of the vertices of the asterism known as the Summer Triangle and the "head" of the Northern Cross. It is the brightest star in Cygnus and the 19th brightest star in the night sky, with an average apparent magnitude of +1.25. A blue-white supergiant, Deneb rivals Rigel as the most luminous first magnitude star.

GJ 3379 (Giclas 99-49) is the nearest star in the Orion constellation, being around 17.5 lightyears away from the Sun. The main sequence star is a red dwarf with the spectral class M3.5V. It has an apparent magnitude of 11.33 and an absolute magnitude of 12.68, therefore, the star is not visible with the naked eye. It is located in the left upper part of the Orion constellation, below Betelgeuse.

In the naming citation, Enriqueta Basilio was recognized as the first woman torchbearer at the 1968 Summer Olympics, analogous to the role of heralds like Eurybates. Queta is very dim, with an apparent magnitude of ~26.77. It is at least 6,000 times fainter than Eurybates, suggesting that it is likely very small in size, less than in diameter. Assuming that Queta has the same albedo as Eurybates, its diameter would be .

The first ones are termed visual distance moduli and are denoted by {(m - M)}_{v} while the second ones are called true distance moduli and denoted by {(m - M)}_{0}. Visual distance moduli are computed by calculating the difference between the observed apparent magnitude and some theoretical estimate of the absolute magnitude. True distance moduli require a further theoretical step, that is the estimation of the interstellar absorption coefficient.

Relatively little is known about itself. With a size of about it is very small, on account of which it is seen from the Earth as a small point even with large telescopes, and can only be observed using highly sensitive CCD cameras. At the time of its closest approach in January 2003 it had an apparent magnitude of about 20.4. So far nothing concrete is known about the composition of .

110 Herculis (abbreviated to 110 Her) is a star in the northern constellation of Hercules. Its apparent magnitude is 4.19, and it can be faintly seen with the naked eye, according to the Bortle scale. Based on parallax estimates made by the Hipparcos spacecraft, the star is located fairly close, about 62.7 light-years (19.21 parsecs) away. 110 Herculis has a spectrum matching that of an F-type main-sequence star.

Iota Aquarii, Latinized from ι Aquarii, is the Bayer designation for a star in the equatorial constellation of Aquarius. It is visible to the naked eye with an apparent magnitude of +4.279. Based upon parallax measurements made during the Hipparcos mission, the distance to this star is around . The spectrum of this star fits a stellar classification of B8 V, showing that this is a B-type main sequence star.

It is a variable star, considered an Orion variable, with occasional fading and other variability caused by obscuration from the surrounding dust. The apparent magnitude varies irregularly between 10.2 and 10.7. The properties of the star are calculated based on its maximum brightness, assumed to be the least obscured. The secondary is a T Tauri star, detected by distinctive spectral lines that could not be produced by the hotter primary star.

Gliese 3685 is a star in the constellation of Leo. It is extremely faint; its apparent magnitude is 13.3, and can only be seen with a ten-inch (25 cm) telescope (see Limiting magnitude). Based on a parallax of 50.30 milliarcseconds, the system is located 65 light years (20 parsecs) away from the Earth. This is a part of a binary star system consisting of two components separated by 24″.

EO Aurigae is an eclipsing binary of Algol type in the northern constellation of Auriga. With a combined apparent magnitude of 7.71, it is too faint to be seen with the unaided eye. The eclipsing binary nature of the star was detected in 1943 by Sergei Gaposchkin at Harvard College Observatory. It consists of a pair of B-type main sequence stars orbiting each other with a period of 4.0656 days.

II Pegasi is a binary star system in the constellation of Pegasus with an apparent magnitude of 7.4 and a distance of 130 light years. It is a very active RS Canum Venaticorum variable (RS CVn), a close binary system with active starspots. The primary (II Pegasi A) is a cool subgiant, an orange K-type star. It has begun to evolve off the main sequence and expand.

The gas and dust between the Sun and HDE 226868 results in a reduction in the apparent magnitude of the star as well as a reddening of the hue—red light can more effectively penetrate the dust in the interstellar medium. The estimated value of the interstellar extinction (AV) is 3.3 magnitudes. Without the intervening matter, HDE 226868 would be a fifth-magnitude star and, thus, visible to the unaided eye.

SU Aurigae is a T Tauri-type variable star in the constellation Auriga. It is located about 500 light-years (150 parsecs) away in the Taurus-Auriga Star Forming Region. Its apparent magnitude is 9.30, which is dim enough that it cannot be seen with the unaided eye. SU Aurigae's spectral type of G2IIIne means that it is a G-type star with an effective temperature similar to the Sun.

Kepler-20 is a star 929 light-years from Earth in the constellation Lyra with a system of six known planets. The apparent magnitude of this star is 12.51, so it cannot be seen with the unaided eye. Viewing it requires a telescope with an aperture of or more. It is slightly smaller than the Sun, with 94% of the Sun's radius and about 91% of the Sun's mass.

Epsilon Eridani (Latinized from ε Eridani), formally named Ran, is a star in the southern constellation of Eridanus, at a declination of 9.46° south of the celestial equator. This allows it to be visible from most of Earth's surface. At a distance of from the Sun, it has an apparent magnitude of 3.73. It is the third-closest individual star or star system visible to the unaided eye.

The planet orbits a red subdwarf star named Kapteyn's Star. The star has a mass of 0.27 and a radius 0.29 . It has a surface temperatures of 3550 K and is roughly 11 billion years old. In comparison, the Sun is about 4.6 billion years old and has a surface temperature of 5778 K. The star's apparent magnitude, or how bright it appears from Earth's perspective, is 8.85.

The secondary star, HD 109749 B, is a K-type main sequence star with an apparent magnitude of 10.3. It has a mass of about and is located at a separation of 8.4 arcseconds, which corresponds to a projected separation of 490 AU. This star has the same proper motion as the primary and seems to be at the same distance, confirming they form a physical binary system.

The star normally has an apparent magnitude of 5.89, but every 7.64 days (7 days, 15 hours, and 22 minutes) its brightness decreases to magnitude 6.37, approximately two thirds as bright. Five days and 17 hours after each primary eclipse, there is a secondary eclipse when the brightness drops to magnitude 6.06, about 85% of the normal brightness. Each eclipse lasts for 220 minutes. Both eclipses are partial.

NGC 6558 is a globular cluster, located about 24,000 light years away in the constellation Sagittarius. Its apparent magnitude is about 11 and its apparent diameter is about 10 arcminutes. The globular cluster was discovered in 1784 by the astronomer William Herschel with his 18.7-inch telescope and the discovery was later catalogued in the New General Catalogue. It is located 1.5 degrees south-southeast of Gamma2 Sagittarii.

NGC 5927 is a globular cluster in the constellation Lupus. NGC 5927 has a diameter of about 12 arcminutes and an apparent magnitude of +8.86. Its Shapley–Sawyer Concentration Class is VIII, and it contains stars of magnitude 15 and dimmer. The globular cluster was discovered by the astronomer James Dunlop in 1826 with a 9-inch telescope and later by John Louis Emil Dreyer in the New General Catalog.

Kepler-69 is a G-type star that is approximately 81% the mass of and 93% the radius of the Sun. It has a surface temperature of 5638 ± 168 K. In comparison, the Sun has a surface temperature of 5778 K. The star's apparent magnitude, or how bright it appears from Earth's perspective, is 13.7. Therefore, Kepler-69 is too dim to be seen with the naked eye.

Lacaille gave nine stars Bayer designations, labelling them Alpha through to Theta, combining two stars next to each other as Zeta. Gould later added a tenth, Iota Antliae. Beta and Gamma Antliae (now HR 4339 and HD 90156) ended up in the neighbouring constellation Hydra once the constellation boundaries were delineated in 1930. Within the constellation's borders, there are 42 stars brighter than or equal to apparent magnitude 6.5.

Light curve for the Mira variable S Coronae Borealis over six years S Coronae Borealis (S CrB) is a Mira variable star in the constellation Corona Borealis. Its apparent magnitude varies between 5.8 and 14.1, with a period of 360 days—just under a year. Within the constellation, it lies to the west of Theta Coronae Borealis, and around 1 degree southeast of the eclipsing binary star U Coronae Borealis.

Tau3 Gruis is a solitary star in the southern constellation of Grus. Its apparent magnitude is 5.71, which is bright enough to be visible to the naked eye as a dim, white-hued star. The star is located around distant from the Sun based on parallax, and it is drifting further away with a radial velocity of 6 km/s. This is an Am star with a stellar classification of kA5hA7mF2.

Owing to its low luminosity, the star has the ability to live for up to 12 trillion years. It is metal-rich, with a metallicity ([Fe/H]) of 0.04, or 109% the solar amount. Its luminosity is 0.05% of that of the Sun (), most of which is emitted in the infrared spectrum, and with an apparent magnitude of 18.80 it is not visible to the naked eye from the Earth.

Nearby non-eclipsing binaries can also be photometrically detected by observing how the stars affect each other in three ways. The first is by observing extra light which the stars reflect from their companion. Second is by observing ellipsoidal light variations which are caused by deformation of the star's shape by their companions. The third method is by looking at how relativistic beaming affects the apparent magnitude of the stars.

The planet orbits an (F-type) star named Kepler-419. The star has a mass of 1.39 and a radius of 1.75 . It has a surface temperature of 6430 K and is 2.8 billion years old. In comparison, the Sun is about 4.6 billion years old and has a surface temperature of 5778 K. The star's apparent magnitude, or how bright it appears from Earth's perspective, is 12.

The two component stars orbit closely enough to each other for mass to have been transferred between them—in this case the secondary having transferred a large amount of mass to the primary. RV Corvi is another eclipsing binary. Its brightness varies from apparent magnitude 8.6 to 9.16 over 18 hours. The system is composed of stars of spectral types F0 and G0, which orbit each other every 0.7473 days.

Close to Gamma Corvi and visible in the same binocular field is R Corvi, a long period (Mira) variable star. It ranges in brightness from a magnitude of 6.7 to 14.4 with a period of approximately 317 days. TT Corvi is a semiregular variable red giant of spectral type M3III and apparent magnitude 6.48 around 923 light years distant. It is around 993 times as luminous as the Sun.

53 Eridani is a visual binary, where the orbit of the two stars is calculated from their orbital motions. The primary star, 53 Eridani A, is an evolved red giant with a spectral type of K1III. It is almost ten times as wide as the Sun and slightly more massive than the Sun. The secondary star, 53 Eridani B, has an apparent magnitude of 6.95 and its spectral type is unknown.

NGC 2423-3 is a red giant star approximately 2498 light-years away in the constellation of Puppis. The star is part of the NGC 2423 open cluster (hence the name NGC 2423-3). The star has an apparent magnitude of nine and an absolute magnitude of zero, with a mass of 2.4 times the Sun. As of 2007, it has been confirmed that an extrasolar planet orbits the star.

25 Serpentis is a star system in the constellation of Serpens Caput. With an apparent magnitude of 5.37, it is just barely visible to the naked eye. The system is estimated to be some 450 light-years (138 parsecs) based on its parallax. 25 Serpentis is a spectroscopic binary, meaning that the individual components are too close to be resolved, but periodic Doppler shifts in their spectra indicate orbital motion.

Gamma2 Normae, Latinized from γ2 Nor, is the brightest star in the southern constellation of Norma. Its apparent magnitude is 4.02 – making it a faint star but visible to the naked eye. Based upon an annual parallax shift of 25.33 mas as seen from Earth, this star is located roughly 129 light years from the Sun. It is moving closer to the Sun with a radial velocity of −29 km/s.

Kappa Normae, Latinized from κ Normae, is a solitary, yellow hued star in the southern constellation of Norma. Its apparent magnitude is 4.94, which is bright enough to be faintly visible to the naked eye. Based upon an annual parallax shift of as seen from Earth, the system is located about 440 light years from the Sun. It is drifting closer with a radial velocity of 13.5 km/s.

It is a hot massive main sequence or subgiant star, over a thousand times as luminous as the sun. μ2 Crucis is the fainter of the pair. Its apparent magnitude is 5.2 and it is a Be star, a star spinning so quickly that it has ejected a disc of material that creates emission lines in its spectrum. The disc is inclined at 36° to our line of sight.

WR 156 has a Hipparcos parallax of 3.16" indicating a distance of about a thousand light years, although with a fairly large margin of error. Other studies indicate that it is much more distant based on a very high luminosity and faint apparent magnitude. The Gaia DR1 parallax is 0.07". The margin of error is larger than the measured parallax, but still the indication is for a very large distance.

It has a surface temperature of between 3360 and 3370 K and its age is unknown. In comparison, the Sun is about 4.6 billion years old and has a surface temperature of 5778 K. The star's apparent magnitude, or how bright it appears from Earth's perspective, is 15.309. Therefore, it is too dim to be seen with the naked eye and can only be observed with a telescope.

Like the primary, the secondary star Gliese 667 B (GJ 667 B) is a K-type main-sequence star, although it has a slightly later stellar classification of K5V. This star has a mass of about 69% of the Sun, or 95% of the primary's mass, and it is radiating about 5% of the Sun's visual luminosity. The secondary's apparent magnitude is 7.24, giving it an absolute magnitude of around 8.02.

The human eye is easily fooled, and Hipparchus's scale has had problems. For example, the human eye is more sensitive to yellow and red light than to blue, and photographic film more to blue than to yellow/red, giving different values of visual magnitude and photographic magnitude. Apparent magnitude can also be affected by factors such as dust in the atmosphere or light cloud cover absorbing some of the light.

Plot from Leavitt's 1912 paper. The horizontal axis is the logarithm of the period of the corresponding Cepheid, and the vertical axis is its apparent magnitude. The lines drawn correspond to the stars' minimum and maximum brightness, respectively. Leavitt, a graduate of Radcliffe College, worked at the Harvard College Observatory as a "computer", tasked with examining photographic plates in order to measure and catalog the brightness of stars.

The comet reached its perihelion (the point that is closest to the Sun) on June 5, 2014, and then its perigee (the point that is closest to Earth) on July 10, 2014, at a distance of about 47 million kilometres. The comet peaked around apparent magnitude 9 and was visible in small telescopes. From late July 2014 until March 2015, as seen from Earth, the comet will appear near Arcturus.

The second-brightest star, the yellow-white subgiant star Alpha Trianguli (3.41m) with a close dimmer companion, is also known as Caput Trianguli or Ras al Muthallath, and is at the apex of the triangle. It lies around 7 degrees north-northwest of Alpha Arietis. Making up the triangle is Gamma Trianguli, a white main sequence star of spectral type A1Vnn of apparent magnitude 4.00 about 112 light-years from Earth.

HD 164595 is a G-type star located in the constellation of Hercules, from Earth that is notably similar to the Sun. With an apparent magnitude of 7.075, the star can be found with binoculars or a small telescope in the constellation Hercules. HD 164595 has one known planet, , which orbits HD 164595 every 40 days. It was detected with the radial velocity technique with the SOPHIE echelle spectrograph.

Nu Scorpii D, with an apparent magnitude of 7.39, is the faintest component of the Nu Scorpii system. It is one of a class of chemically peculiar stars known as Ap/Bp stars; in particular, it has strong silicon emission lines. It too is likely also another spectroscopic binary: Nu Scorpii Da is another B9III-type star, similar to Nu Scorpii C, but very little is known about Nu Scorpii Db.

' flew by Earth on 6 June 2020, passing from Earth. The asteroid had been recovered two days earlier on 4 June 2020. By 11 June 2020, the asteroid had brightened to apparent magnitude 14.4, which is roughly the brightness of Pluto. Being a member of the Aten asteroids, ' orbits the Sun at a distance of 0.50–1.26 AU once every 10 months (300 days; semi-major axis of 0.88 AU).

Kappa Draconis, Latinized from κ Draconis, is a blue giant star located in the northern circumpolar constellation of Draco. At an apparent magnitude of 3.88, it is barely visible to the naked eye when artificial lighting from cities is present. Nevertheless, it is a powerful star, approximately five time as massive as the Sun. It is about 490 light-years away, and is 1,400 times brighter than the Sun.

In November 2016, NASA reported finding a large amount of underground ice in the Utopia Planitia region. The volume of water detected has been estimated to be equivalent to the volume of water in Lake Superior. Mars can easily be seen from Earth with the naked eye, as can its reddish coloring. Its apparent magnitude reaches −2.94, which is surpassed only by Venus, the Moon and the Sun.

255P/Levy, formerly P/2006 T1 and P/2011 Y1, is a periodic comet with an orbital period of 5.25 years. It last came to perihelion (closest approach to the Sun) on 14 January 2012. During the 2006 passage the comet achieved an apparent magnitude of ~9.5. Levy (PK06T010) was believed to have been recovered on 3 June 2011 at magnitude 19.8, but other observatories were unable to confirm a recovery.

HD 193664 is the Henry Draper Catalogue designation for a star in the northern constellation of Draco. With an apparent magnitude of 5.93, according to the Bortle Scale it is visible to the naked eye from suburban skies. Parallax measurements by the Hipparcos spacecraft yield an estimated distance of 57.3 light years. It has a relatively large proper motion of 0.558 arc seconds per year across the sky.

Before being announced to the public, it was only tracked by Cerro Tololo Inter-American Observatory (807) and Las Campanas Observatory (304). It has an observation arc of about 5 years. Two precovery measurements from 22 October 2011 have been reported. A primary issue with observing it and finding precovery observations of it is that at an apparent magnitude of 23, it is too faint for most telescopes to easily observe.

20 Ceti is a single star located around 590 light years away in the equatorial constellation of Cetus. It is faintly visible to the naked eye with apparent magnitude is 4.76. The Bright Star Catalogue has this star classified as M0III, matching an aging red giant star that has consumed the hydrogen at its core and expanded. Houk and Swift (1999) listed an earlier class of K5 III.

Mu Persei (Mu Per, μ Persei, μ Per) is a binary star in the constellation of Perseus, with an apparent magnitude of +4.16. The primary component is a yellow G-type supergiant. It is approximately 900 light years from Earth. With an effective temperature of about 5400 kelvins and a radius of 53 solar radii, this star has the luminosity of about 2030 times that of the Sun.

The total mass of the galaxy is estimated to be . A total of 241 HII regions have been identified in the galaxy. One supernova has been observed in NGC 2906, SN 2005ip. The supernova was discovered by T. Boles on November 6, 2005, with a 0.35m refractor, with an estimated apparent magnitude 15.5 and was identified as a type II supernova, probably within a few weeks past explosion.

Chi Tauri (χ Tauri) is a star system in the constellation of Taurus. Parallax measurements made by the Hipparcos spacecraft put it at a distance of about 291 light years (89 parsecs) from Earth. The primary component has an apparent magnitude of about 5.4, meaning it is visible with the naked eye. The main component of the system is Chi Tauri A. It is a B-type main-sequence star.

Theta Tucanae (θ Tuc, θ Tucanae) is a star in the constellation Tucana. Like other stars in Tucana, it was given its Bayer designation by French explorer and astronomer Nicolas Louis de Lacaille in 1756. It was found to be variable in 1971. Theta Tucanae is a white A-type subgiant of spectral type A7IV with a mean apparent magnitude of +6.11, located approximately 423 light years from Earth.

It made a close approach to Earth of (0.1 lunar distances) around 18:02 UTC on 7 September 2014. The asteroid briefly brightened to about apparent magnitude 11.5, but it was still not visible to the naked eye or common binoculars. At the peak brightness the asteroid had a declination of –47, and was most easily visible over New Zealand. During 2014, asteroids 2014 AA and have come closer to Earth.

The 0.7 m telescope takes a week to complete a survey of the sky, detecting objects fainter than apparent magnitude 19. This combination of telescopes, one slow and one medium, has so far detected more near Earth Objects than any other single survey. This shows the need for a combination of different types of telescopes. CSS used to include a telescope in the Southern Hemisphere, the Siding Spring Survey.

The planet was discovered by the radial velocity method. WASP-23 is a star with one orbiting planet, WASP-23 b. The planet, discovered by the transit method in 2010, orbits every 2.944 very close to its Sun, at 0.0376 AU. It is smaller than Jupiter, at and . Its star is a K1V type star of apparent magnitude 12.7, far below naked-eye visibility, and smaller than the Sun at and .

Zeta1 Antliae is the Bayer designation for a binary star system in the southern constellation of Antlia. Based upon parallax measurements, the pair are located at a distance of roughly from Earth. They have apparent magnitudes of +6.20 and +7.01 and are separated by 8.042 arcseconds. The apparent magnitude of the combined system is +5.76, which is bright enough to be seen with the naked eye in suitably dark skies.

CS Camelopardalis (CS Cam) is a binary star in reflection nebula VdB 14, in the constellation Camelopardalis. It forms a group of stars known as the Camelopardalis R1 association, part of the Cam OB1 association. The near- identical supergiant CE Camelopardalis is located half a degree to the south. The primary component, CS Camelopardalis A, is a blue-white B-type supergiant with a mean apparent magnitude of 4.21m.

NGC 3239 is an irregular galaxy in the constellation of Leo. It is the host of SN 2012A, the first supernova of 2012. The galaxy, which was discovered in 1784 by William Herschel, is part of the New Galactic Catalogue, and with an apparent magnitude of 13.5, is not visible to the naked eye. It has been shown to have many HII regions, while also having some star formation regions.

Alpha Lyncis (α Lyn, α Lyncis) is the brightest star in the northern constellation of Lynx with an apparent magnitude of +3.13. Unusually, it is the only star in the constellation that has a Bayer designation. Based upon parallax measurements, this star is located about from the Earth. This is a giant star that has exhausted the hydrogen at its core and has evolved away from the main sequence.

The constellation does not lie on the galactic plane of the Milky Way, and there are no prominent star clusters. NGC 625 is a dwarf irregular galaxy of apparent magnitude 11.0 and lying some 12.7 million light years distant. Only 24000 light years in diameter, it is an outlying member of the Sculptor Group. NGC 625 is thought to have been involved in a collision and is experiencing a burst of active star formation. NGC 37 is a lenticular galaxy of apparent magnitude 14.66. It is approximately 42 kiloparsecs (137,000 light-years) in diameter and about 12.9 billion years old. Robert's Quartet (composed of the irregular galaxy NGC 87, and three spiral galaxies NGC 88, NGC 89 and NGC 92) is a group of four galaxies located around 160 million light-years away which are in the process of colliding and merging. They are within a circle of radius of 1.6 arcmin, corresponding to about 75,000 light-years.

The phase curve of the Moon compared to Mercury. The phase curve of the Moon approximately resembles that of Mercury due to the similarities of the surfaces and the lack of an atmosphere on either body. Clementine spacecraft data analyzed by J. Hillier, B. Buratti and K. Hill indicate a lunar opposition surge. The Moon's apparent magnitude at full phase is −12.7 while at quarter phase it is 21 percent as bright.

The total luminosity of this cluster is around 120,000 times that of the Sun, the absolute magnitude being -8.04. The brightest individual stars in M9 are of apparent magnitude 13.5, making them visible in moderately sized telescopes. There have been 24 variable stars found in M9: 21 RR Lyrae variables, plus a long-period variable, Type II Cepheid, and an eclipsing binary. No blue stragglers or SX Phoenicis variables have been discovered.

The variable luminosity of this system was discovered in 1784 by the British amateur astronomer John Goodricke. The orbital plane of this system is nearly aligned with the line of sight from the Earth, so the two stars periodically eclipse each other. This causes Beta Lyrae to regularly change its apparent magnitude from +3.2 to +4.4 over an orbital period of 12.9414 days. It forms the prototype of a class of ellipsoidal "contact" eclipsing binaries.

There are many binary stars in the system, as well as blue stragglers, which are likely to have been formed by collisions and mergers of smaller stars. The apparent magnitude of the cluster is 5.4, so it can be seen with the unaided eye. However this depends on good viewing conditions with a minimum of light pollution. With binoculars it can be seen to cover an area three quarters the size of the full moon.

It has around 18 times the mass of the Sun and 12 times the Sun's radius. This star is radiating about times the luminosity of the Sun from its outer envelope at an effective temperature of . This is a variable star of the Beta Cephei type, causing the apparent magnitude to vary between +2.86 and +2.94 with multiple periods of , , and 8.2 days. During each pulsation cycle, the temperature of the star varies by .

The system consists of a pair of binary stars separated by 66.6 arcseconds. The primary, component A, is a yellow-white F-type subgiant with an apparent magnitude of +4.25. It is classified as a Delta Scuti type variable star and its magnitude varies by 0.04 with a period of 0.1557 days. Its binary companion, component B, is also a F-type subgiant which is slightly dimmer, with a magnitude of +5.2.

FF Aquilae is a classical Cepheid variable star located in the constellation Aquila. It ranges from apparent magnitude 5.18 to 5.51 over a period of 4.470848 days, meaning it is faintly visible to the unaided eye in rural or suburban settings. Originally known as HR 7165, it was noted to be variable by Charles Morse Huffer in August 1927, who observed its Cepheid pattern. It then received the variable star designation FF Aquilae.

NGC 1873 (also known as ESO 85-SC54) is an open cluster associated with an emission nebula located in the Dorado constellation within the Large Magellanic Cloud. It was discovered by James Dunlop on September 24, 1826 and rediscovered by John Herschel on January 2, 1837. Its apparent magnitude is 10.4, and its size is 3.50 arc minutes. NGC 1873 is part of a triple association with NGC 1869 and NGC 1871.

Delta Velorum is a triple star system. The outer components, δ Velorum A and B, have a wide orbit with a 143-year period. The primary component A has an apparent magnitude of 2.00, while the secondary B is magnitude 5.54, with a combined magnitude measured at 1.96. As of 2013, the two stars were separated by 0.6", but they have an eccentric orbit and their average separation over the whole orbit is nearly 2".

R Leonis is a red giant Mira-type variable star located approximately 300 light years away in the constellation Leo. The apparent magnitude of R Leonis varies between 4.31 and 11.65 with a period of 312 days. At maximum it can be seen with the naked eye, while at minimum a telescope of at least 7 cm is needed. The star's effective temperature is estimated 2,890 kelvins and radius spans , roughly Mars's orbital zone.

It has an apparent magnitude of 12.1. Appearing undisturbed in visible light, it shows signs of having undergone a collision or merger when viewed at longer wavelengths, with disturbed patterns of ionized hydrogen including a filament of gas around 64,000 light-years long. It is part of a group of ten galaxies. NGC 7410 is a spiral galaxy discovered by British astronomer John Herschel during observations at the Cape of Good Hope in October 1834.

1 Scorpii, or b Scorpii, is a single star in the southern zodiac constellation of Scorpius. It has an apparent magnitude of 4.63, which is bright enough to be faintly visible to the naked eye on a dark night. The star shows an annual parallax shift of 6.59 mas from Earth's orbit, which equates to a distance of roughly 490 light years. It is a probable (89% chance) member of the Sco OB2 moving group.

Gamma Pictoris is an orange giant of spectral type K1III that has swollen to 1.4 times the diameter of the Sun. Shining with an apparent magnitude of 4.5, it lies 174 light-years distant from Earth. HD 42540, called 47 Pictoris by American astronomer Benjamin Apthorp Gould, is a slightly cooler orange giant, with a spectral type of K2.5III and average magnitude 5.04. It has also been suspected of being a variable star.

The globular cluster Arp-Madore 1 is the most remote known globular cluster in the Milky Way at a distance of from Earth. NGC 1512 is a barred spiral galaxy 2.1 degrees west-southwest of Alpha Horologii with an apparent magnitude of 10.2. About five arcmin (13.8 kpc) away is the dwarf lenticular galaxy NGC 1510. The two are in the process of a merger which has been going on for 400 million years.

With an apparent magnitude of 3.62, Delta is an orange giant of spectral type K2III located around 91 light-years away. Epsilon Muscae is a red giant of spectral type M5III and semiregular variable that ranges between magnitudes 3.99 and 4.31 over approximately 40 days. It has expanded to 130 times the Sun's diameter and 1800 to 2300 its luminosity. It was a star originally 1.5 to 2 times as massive as our Sun.

2009 RR micro-asteroid, classified as near-Earth object of the Apollo group. It was discovered on 11 September 2009 by the Catalina Sky Survey at an apparent magnitude of 19.5 using a Schmidt–Cassegrain telescope. was the only asteroid discovered before 2014 that was predicted to potentially pass inside the orbit of the Moon during 2014. The asteroid has an estimated diameter of and is listed on the Sentry Risk Table.

Eta Chamaeleontis, Latinized from η Chamaeleontis, is a star in the constellation Chamaeleon. It has an apparent magnitude of about 5.5, meaning that it is just barely visible to the naked eye. Based upon parallax measurements made by the Hipparcos spacecraft, this star is located some 310 light years (95 parsecs) away from the Sun. Eta Chamaeleontis has a spectral type of B8V, meaning it is a B-type main sequence star.

John Flamsteed did likewise with Nu Coronae Borealis; classed by Bayer as a single star, it was noted to be two close stars by Flamsteed. He named them 20 and 21 Coronae Borealis in his catalogue, alongside the designations Nu1 and Nu2 respectively. Chinese astronomers deemed nine stars to make up the asterism, adding Pi and Rho Coronae Borealis. Within the constellation's borders, there are 37 stars brighter than or equal to apparent magnitude 6.5.

Other cultures have likened the pattern to a turtle, ostrich nest, a tent, or even a hut belonging to a rock hyrax. Although fainter than its northern counterpart, the oval- or horseshoe-shaped pattern of its brighter stars renders it distinctive. Alpha and Beta Coronae Australis are the two brightest stars with an apparent magnitude of around 4.1. Epsilon Coronae Australis is the brightest example of a W Ursae Majoris variable in the southern sky.

75D/Kohoutek is a short-period comet discovered in February 1975, by Luboš Kohoutek. Not to be confused with the much better-known C/1973 E1 (Kohoutek), 75D is a repeat visitor to the inner Solar System, with a period of about seven years. It was placed on the discovery orbit when it passed from Jupiter on 28 July 1972. Apparitions have been dim, with the brightest being in 1988 at about apparent magnitude 13.

HD 221525 is a single star near the north celestial pole in the constellation Cepheus. At an apparent magnitude of 5.56, it can be seen with the naked eye under dark skies. It is about 30 times fainter than the nearby prominent star Polaris. Based upon parallax measurements, HD 221525 is located at a distance of approximately 317 light years from the Sun, but is drifting closer with a radial velocity of −11 km/s.

4 Centauri is a star in the constellation Centaurus. It is a blue-white B-type subgiant with an apparent magnitude of +4.75 and is approximately 640 light years from Earth. 4 Centauri is a hierarchical quadruple star system. The primary component of the system, 4 Centauri A, is a spectroscopic binary, meaning that its components cannot be resolved but periodic Doppler shifts in its spectrum show that it must be orbiting.

Upsilon Pegasi, Latinised from υ Pegasi, is a star within the great square in the northern constellation of Pegasus. It has the proper name Alkarab . This object has a yellow-white hue and is faintly visible to the naked eye with an apparent magnitude of 4.40. It is located at a distance of approximately 170 light-years from the Sun based on parallax, but is drifting closer with a radial velocity of −8.6 km/s.

As of November 2011 with an observation arc of 40 days, the JPL Small-Body Database showed that the uncertainty region of the asteroid during the 1976 close approach could result in a pass anywhere from 0.001 AU to 0.018 AU from Earth. During the 1976 close approach the asteroid reached about apparent magnitude 14. The asteroid will pass from Earth on 27 December 2022, allowing a refinement to the known trajectory.

The double star Zeta Reticuli is located in the western part of the small Reticulum constellation, about 25′ from the constellation's border with Horologium. In dark southern skies, the two stars can be viewed separately with the naked eye, or with a pair of binoculars. ζ1 Reticuli has an apparent magnitude of 5.52, placing it on the border between 5th and 6th magnitude stars. ζ2 Reticuli is slightly brighter at magnitude 5.22.

NGC 1984 (also known as ESO 56-SC132) is an open cluster associated with an emission nebula, it is located in the constellation Dorado in the Large Magellanic Cloud. It was discovered by John Herschel on 16 December 1835. The apparent magnitude is 9.9 and its size is 1.50 by 1.20 arc minutes. NGC 1984 contains a star called NGC 1984-16 which is at these co-ordinates 05 27 41.0 -69 08 06.

HD 166066 is a star in the constellation Telescopium, located about from Earth. It has an apparent magnitude of +8.11, allowing it to be viewed with binoculars under suitable viewing conditions. The stellar classification is G0V, which indicates that it is a main sequence star. The effective temperature of its chromosphere is 5,900 K,. It has an estimated lifespan of 8.9 billion years and has about the same mass as the Sun.

It has never been given a formal variable star designation, unlike L1 Puppis which is OU Puppis. L2 Puppis varies in apparent magnitude by about 2 magnitudes with a period of 140 days. The average brightness also varies slowly over several years so that the total range is given as magnitude 2.6 – 6.0. Since 1995 the average brightness has dropped so that the 140 day variations are now between about magnitude 6 and 8.

22 Vulpeculae is a binary star system in the northern constellation Vulpecula. Based on its parallax, it is located some 1,900 light-years away, and it has an apparent magnitude of about 5.176, making it visible to the naked eye. The system is moving closer to the Earth with a heliocentric radial velocity of −23 km/s. The pair have an orbital period of in what is assumed to be a circular orbit.

64 Aurigae is a single star located 312 light years away from the Sun in the northern constellation of Auriga. It is visible to the naked eye as a dim, white-hued star with an apparent magnitude of 5.87. The star is moving closer to the Earth with a heliocentric radial velocity of −10, and may come to within in around 5.3 million years. It is a member of the Sirius supercluster.

Its brightness varies from magnitude +4.9 to +7.0 in visual apparent magnitude. The period is given in the GCVS as 441 days, but there is also a strong variation with a period of 235 days. Using British Astronomical Association observations from 1971 to 1998, the periods are calculated as 439.4 and 233.1 days. The angular diameter of UU Aurigae has been measured at 12.07 ± 0.22 mas using very-long-baseline interferometry (VLBI).

66 Andromedae is a binary star system in the northern constellation of Andromeda, near the northern border with Perseus. The designation is from the star catalogue of English astronomer John Flamsteed, first published in 1712. It has a combined apparent magnitude of 6.16, which is near the lower limit of stars that are visible to the naked eye under good seeing conditions. An annual parallax shift of provides a distance estimate of 178 light years.

At its present distance, the visual magnitude is diminished by an extinction factor of 0.135 due to interstellar dust. Xi Cancri is a single-lined spectroscopic binary star system with an orbital period of 4.66 years, an eccentricity of 0.06, and a semimajor axis of 0.01 arcseconds. The primary, Xi Cancri A, is a yellow G-type giant with an apparent magnitude of +5.70. Its companion, Xi Cancri B, is of magnitude 6.20.

Older references give the star cloud's magnitude as 4.6, but more recent estimates place it a full two magnitudes brighter, at 2.5. HD 167356 is the brightest star within the Small Sagittarius Star Cloud, a white supergiant with an apparent magnitude of 6.05. This star is an Alpha-2 Canum Venaticorum variable, showing small changes in brightness as it rotates. There are three other stars in M24 with visual magnitudes between 6.5 and 7.0.

The member stars of M47 have been measured down to about red dwarfs at apparent magnitude 19. There are around 500 members, the brightest being HD 60855, a magnitude 5.7 Be star. The cluster is dominated by hot class B main sequence and giant stars, but a noticeable colour contrast comes from several bright red giants. M47 is located about a degree away from Messier 46, which is much older and much further away.

HD 66428 is a G-type main sequence star located approximately 179 light-years away in the constellation of Monoceros. This star is similar to our Sun with an apparent magnitude of 8.25, an effective temperature of 5705 ± 27 K and a solar luminosity 1.28. Its absolute magnitude is 11.1 while its U-V color index is 0.71. It is considered an inactive star and it is metal-rich ([Fe/H] = 0.310).

Light curve of T Antliae recorded by NASA's Transiting Exoplanet Survey Satellite (TESS) T Antliae varies in brightness regularly every 5.89820 days. The light curve is extremely consistent and shows a rapid rise taking 23% of the period, with a slower decline. The maximum brightness of apparent magnitude 8.86 and the minimum of 9.76 are also extremely consistent. The amplitude, light curve shape, period, and consistency, all mark T Antliae as a Cepheid variable.

The star's effective temperature is 5933 (± 44) K. In comparison, the 4.6 billion-year-old Sun releases less heat, with an effective temperature of 5778 K. A picture showing the relative sizes of the first five planets discovered by Kepler. Kepler-7b is the largest, highlighted in yellow. The star has an apparent magnitude of 13, meaning that it is extremely dim as seen from Earth. It cannot be seen with the naked eye.

The star also has an effective temperature of 6213 (± 150) K, meaning that it is hotter than the Sun, which has an effective temperature of 5778 K. The first five planets discovered by Kepler, compared by relative size. Kepler-8b is depicted in orange. Kepler-8 has an apparent magnitude of 13.9; in other words, as seen from Earth, Kepler-8 is an extremely dim star. It cannot be seen with the naked eye.

Zeta Andromedae (Zeta And, ζ Andromedae, ζ And) is a star system in the constellation Andromeda. It is approximately 189 light years from Earth. Zeta Andromedae is a spectroscopic binary whose primary is classified as an orange K-type giant with a mean apparent magnitude of +4.08. In addition to brightness variation due to the ellipsoidal shape of the giant primary star, the system is also an RS Canum Venaticorum type variable star.

The primary component is a yellow-white F-type subgiant with an apparent magnitude of +3.65. It has 1.9 times the Sun's mass, 2.9 times the Sun's radius and is emitting 15 times the luminosity of the Sun at an effective temperature of 6,651 K. Orbiting at an angular separation of 22.7 arcseconds is the 9th magnitude secondary companion. There is a magnitude +10.5 optical companion at an angular separation of 99.6 arcseconds.

A simulated circular orbit of 210-km-diameter moon at a distance of 4770 km The discovery of a minor-planet moon was reported in IAUC 8812 on 22 February 2007. The satellite was detected using the Hubble Space Telescope in August 2005. The satellite was found at 0.16 arcsec from the primary with an apparent magnitude difference of 2.5. It orbits the primary in days, at a distance of , yielding a system mass of .

104P/Kowal, also known as Kowal 2, is a periodic Jupiter-family comet discovered by Charles T. Kowal in 1979. The orbit was confirmed after new sightings in 1991 and 1998. In 2003, Gary Kronk and Brian Marsden noticed that an object observed by Leo Boethin in 1973 was actually 104P/Kowal. From Boethin's report, it was apparent that comet Kowal 2 had been in a short, major outburst to apparent magnitude 9.5 in 1973.

ESO - Model Image of Cepheid l Carinae HD 84810, also known as l Carinae (l Car), is a star in the southern constellation of Carina. Its apparent magnitude varies from about 3.4 to 4.1, making it readily visible to the naked eye and one of the brightest members of Carina. Based upon parallax measurements, it is approximately from Earth. From the characteristics of its spectrum, l Carinae has a stellar classification of G5 Iab/Ib.

Kappa Aquarii (κ Aquarii, abbreviated Kappa Aqr, κ Aqr) is a probable binary star in the equatorial constellation of Aquarius. This system is visible to the naked eye, but it is faint at an apparent magnitude of 5.03. Based upon parallax measurements made during the Hipparcos mission, it is around from the Sun. The two components are designated Kappa Aquarii A (formally named Situla , the traditional name for the system) and B.

W Hydrae is a Mira-type variable star in the constellation Hydra. The star is nearly located within the Solar neighborhood, between 75 and 120 parsecs, likely at 375 light years from the Sun. It has a visual apparent magnitude range of 5.6 to 10. In the near-infrared J band it has a magnitude of -1.7, is the 7th brightest star in the night sky, and is even brighter than Sirius.

BB Phoenicis is a variable star in the constellation of Phoenix. It has an average visual apparent magnitude of 6.17, being visible to the naked eye with excellent viewing conditions. From parallax measurements by the Gaia spacecraft, it is located at a distance of from Earth. Its absolute magnitude is calculated at 0.6. BB Phoenicis is a Delta Scuti variable, and shows stellar pulsations that cause brightness variations with an amplitude of 0.04 magnitudes.