Iota Persei

ι Persei, Latinized as Iota Persei, is a single star in the northern constellation Perseus. This object is visible to the naked eye as a faint, yellow-white hued point of light with an apparent visual magnitude of 4.1. It is located 34 light years from the Sun based on parallax, and is drifting further away with a radial velocity of +49 km/s. Iota Persei has a relatively high proper motion across the sky.
This is a late F- or early G-type main-sequence star with a stellar classification of around G0V. It is about 3–4 billion years old and is spinning slowly with a projected rotational velocity of 4 km/s. The star has 1.4 times the mass of the Sun and 1.4 times the Sun's radius. It is radiating more than double the luminosity of the Sun from its photosphere at an effective temperature of 5,963 K.
There is a 12.4-magnitude line-of-sight companion star that is not believed to be gravitationally associated with Iota Persei. This object is located at an angular separation of from the primary along a position angle of 125°, as of 2014.
Naming.
In Chinese, (), meaning "Mausoleum", refers to an asterism consisting of ι Persei, 9 Persei, τ Persei, κ Persei, β Persei, ρ Persei, 16 Persei and 12 Persei. Consequently, the Chinese name for ι Persei itself is (, ).


KQ Puppis

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.
The KQ Puppis system consists of a fairly typical M2 supergiant, in orbit with a hotter less luminous star. The hotter star is surrounded by a disc of material being transferred from the cool supergiant. This type of binary is referred to a VV Cephei system, although in this case there are no eclipses of either star. A portion of the disc does appear to be eclipsed and this is detected as a strong drop in far-ultraviolet radiation for about a third of the orbit.
The red supergiant primary star has been compared to Betelgeuse. It shows small amplitude irregular pulsations, and also some variation associated with the orbital motion. The nature of the secondary is less certain. The spectrum shows high excitation features that would indicate an early B or hotter spectral type, but these may be associated with the disc rather than that star itself. Other studies have found a spectrum similar to an A supergiant, but this is thought to be an artefact of a B-type shell star.
KQ Puppis has been catalogued as an outlying member of the open cluster Messier 47 (NGC 2422) and would be the brightest member of that cluster. Membership is uncertain as it appears to be more distant than the other stars in the cluster.


NGC 4230

NGC 4230 is a loosely scattered open cluster in the constellation of Centaurus. It was discovered by John Herschel on April 5, 1837.
ESO catalog (and SIMBAD database) misidentify ESO 171-SC14 as NGC 4230.


X Carinae

X Carinae is a Beta Lyrae variable in the constellation Carina. It ranges between magnitudes 7.9 and 8.65 over a period of approximately 1.08 days.


NGC 6239

NGC 6239 is a barred spiral galaxy located in the constellation Hercules with a distinct core. It is designated as SB(s)B in the galaxy morphological classification scheme and was discovered by the German-born British astronomer William Herschel on 12 April 1788. The galaxy is approximately 42 million light years away from Earth.<ref name="NASA/IPAC"></ref>


NGC 5985

NGC 5985 is a spiral galaxy located in the northern constellation Draco. NGC 5985 was discovered by William Herschel in 1788.


Zubenhakrabi

Zubenhakrabi (or Zuben Hakrabi) is the traditional name for some stars in the constellation Libra.
It can refer to:


42 Aquilae

42 Aquilae, abbreviated 42 Aql, is a single star in the equatorial constellation of Aquila. "42 Aquilae" is its Flamsteed designation. It is a dim star but visible to the naked eye under suitable viewing conditions, having an apparent visual magnitude of 5.45. 42 Aql is located some 104.6 light years away, as determined from its annual parallax shift of . it is moving closer to the Earth with a heliocentric radial velocity of −38 km/s, and is predicted to come to within of the Sun in around 752,000 years.
The stellar classification of this star is F3 IV/V, which matches an F-type star with blended spectral traits of a main sequence star and a subgiant star. It is around 1.3 billion years old with a relatively high rate of rotation, having a projected rotational velocity of 87 km/s. The star has 1.26 times the mass of the Sun and is radiating 5.76 times the Sun's luminosity from its photosphere at an effective temperature of 6,749 K. These coordinates are a source of X-ray emission, which is most likely (99.3% chance) coming from the star.


Hickson 44

Hickson 44 (HCG 44) is a group of galaxies in the constellation Leo. As Arp 316, a part of this group is also designated as group of galaxies in the Atlas of Peculiar Galaxies.


NGC 2040

NGC 2040 is an open star cluster located 160,000 light years away in the constellation of Dorado. It is a young group of stars in one of the largest star formation regions of the Large Magellanic Cloud.


Lambda Normae

λ Normae, Latinised as Lambda Normae, is a binary star system in the southern constellation of Norma, located near the northern constellation boundary with Scorpius. It is visible to the naked eye as a dim, white-hued point of light that shines with a combined apparent visual magnitude of 5.44. The system is located approximately 350 light years distant from the Sun based on parallax, but is drifting closer with a radial velocity of about −15 km/s.
The pair have an orbital period of 67.5 years with a high eccentricity of 0.788. Both components are A-type main-sequence stars that are generating energy through core hydrogen fusion. The primary component has a visual magnitude of 5.83, and is of class A0V. The fainter secondary is class A3V with a magnitude 6.86.


47 Cygni

47 Cygni is a triple star system in the northern constellation of Cygnus, and is located around 4,000 light years from the Earth. It is visible to the naked eye with a combined apparent visual magnitude of 4.61. The system is moving closer to the Earth with a heliocentric radial velocity of −4.6 km/s.
The dual nature of this system was recognized by Annie Cannon in 1912, and she assigned the pair separate Henry Draper Catalogue identifiers. They orbit each other with a period of around . The primary component is itself a spectroscopic binary in a near circular orbit with a period of around . The "a" sin "i" value for the primary is , where "a" is the semimajor axis and "i" is the orbital inclination. It has been repeatedly resolved by speckle interferometery since 1973. Radio emission was detected from this system in 1985/86.
The supergiant primary is a slow irregular variable with an amplitude of about 0.1 magnitudes. Its close companion has 57% of the mass of the Sun. The secondary is a hot B-type main-sequence star, but still 2.5 magnitudes fainter than the primary.


Delta Coronae Borealis

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. Its luminosity and spectrum suggest it has just crossed the Hertzsprung gap, having finished burning core hydrogen and just begun burning hydrogen in its shell. It is a strong source of X-rays due to its hot corona.
In 1989, it was noticed that the brightness of δ Coronae Borealis is not constant. Approximately every 45 days, its brightness changes sinusoidally between 4.57 and 4.69, too small to be noticed without close monitoring. The evolutionary state of the star and its probably rotation period mean that the variations may be due to its rotation with different parts of the surface having spots or different temperatures. This would make it an RS Canum Venaticorum variable. The period has since been refined to 59 days and this is now accepted as the star's rotation period.


Omicron Herculis

Omicron Herculis, Latinized from o Herculis, is a multiple star system in the constellation Hercules. It used to be called Masym ("the wrist"), but this name was transferred to Lambda Herculis.
Properties.
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.
Omicron Herculis is an eruptive variable of the Gamma Cassiopeiae class, which are rapidly rotating B-class stars with mass outflow. It has a projected rotational velocity of 194 km/s.
Omicron Herculis is both a spectroscopic and an interferometric binary star with a separation of 0.1 arcsec.
Omicron Hercules is notable for residing close to the coordinates of the solar apex, the direction towards which the Sun is moving. This was first noticed by William Herschel in 1783, although in his first calculation he identified this point with Lambda Herculis. It will eventually become the brightest star in the sky in approximately 3 million years from today, at -0.4, slightly less bright than Canopus today.


R Canum Venaticorum

R Canum Venaticorum is a Mira variable star in the constellation Canes Venatici. It ranges between magnitudes 6.5 and 12.9 over a period of approximately 329 days.


Pisces-Eridanus stellar stream

Pisces-Eridanus stellar stream is a close stellar stream, between 80 and 226 parsecs away, and stretching 120° across the sky, an open cluster that was stretched apart by past gravitational interactions. By analysis of the highest mass member stars, it is estimated to be only 120 million years old, a similar age to the Pleiades.
Stars.
The stream includes at least 5 naked eye stars: Lambda Tauri at 3.5 magnitude star, 148 parsecs, Omicron Aquarii at 4.7 magnitude, 134 parsec distance, 106 Aquarii at 5.2 magnitude, 114 parsec distance, 108 Aquarii at 5.2 magnitude 98 parsec distance, Tau1 Aquarii at 5.7 magnitude, 97 parsec distance and Nu Fornacis at 4.7 magnitude and 114 parsec distance.


List of stars in Ophiuchus

This is the list of notable stars in the constellation Ophiuchus, sorted by decreasing brightness. Although the Sun travels through Ophiuchus, it is not listed here because it does not stay in the constellation.


NGC 283

NGC 283 is a spiral galaxy in the constellation Cetus. It was discovered on October 2, 1886 by Francis Leavenworth.


HAT-P-7

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.
Planetary system.
This star has only one known planet, HAT-P-7b. This star system was within the initial field of view of the Kepler planet-hunting spacecraft.


Kepler-6

Kepler-6 is a yellow giant situated in the constellation Cygnus. The star lies within the field of view of the Kepler Mission, which discovered it as part of a NASA-led mission to discover Earth-like planets. The star, which is slightly larger, more metal-rich, slightly cooler, and more massive than the Sun, is orbited by at least one extrasolar planet, a Jupiter-sized planet named Kepler-6b that orbits closely to its star.
Nomenclature and history.
Kepler-6 was named for the Kepler Mission, a NASA project launched in 2009 that aims to discover Earth-like planets that transit, or cross in front of, their home stars with respect to Earth. Unlike stars like the Sun or Sirius, Kepler-6 does not have a common and colloquial name. The discovery of Kepler-6b was announced by the Kepler team on January 4, 2010 at the 215th meeting of the American Astronomical Society along with planets around Kepler-4, Kepler-5, Kepler-7, and Kepler-8. It was the third planet to be discovered by the Kepler spacecraft; the first three planets to be verified by data from Kepler had been previously discovered. These three planets were used to test the accuracy of Kepler's measurements.
The discovery of Kepler-6 was confirmed by follow-up observations made using the Hobby Eberly and Smith telescopes in Texas; the Keck 1 telescope in Hawaii; the Hale and Shane telescopes in southern California; the WIYN, MMT, and Tillinghast telescopes in Arizona; and the Nordic Optical Telescope in the Canary Islands.
Characteristics.
Kepler-6 is a star that is approximately 1.209 Msun, or some five-fourths the mass of the Sun. It is also wider than the sun, with a radius of 1.391 Rsun, or seven-fifths of that of the Sun. The star is approximately 3.8 billion years old, and has an effective temperature of 5647 K (9,705 °F). In comparison, the Sun has a slightly warmer temperature of 5778 K. Kepler-6 has a metallicity of [Fe/H] = +0.34, making it 2.2 times more metallic than the Sun. 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.
Planetary system.
Kepler-6 has one confirmed extrasolar planet; it is a gas giant named Kepler-6b. The planet is approximately .669 MJ, or some two-thirds the mass of planet Jupiter. It is also slightly more diffuse than Jupiter, with a radius of approximately 1.323 RJ. Kepler-6b orbits at an average distance of .0456 AU from its star, and completes an orbit every 3.234 days. The eccentricity of the planet's orbit is assumed to be 0, which is that of a circular orbit.


Beta Delphini

Beta Delphini (β Delphini, abbreviated Beta Del, β Del) is a binary star in the constellation of Delphinus. It is the brightest star in Delphinus.
The two components of the system are designated Beta Delphini A (officially named Rotanev , which is historically the name of the system) and B.
Nomenclature.
"β Delphini" (Latinised to "Beta Delphini") is the binary's Bayer designation. The designations of the two components as "Beta Delphini A" and "B" derive from the convention used by the Washington Multiplicity Catalog (WMC) for multiple star systems, and adopted by the International Astronomical Union (IAU).
Beta Delpini bore an historical name, "Rotanev", which arose as follows: Niccolò Cacciatore was the assistant to Giuseppe Piazzi, and later his successor as Director of the Palermo Observatory. The name first appeared in Piazzi's Palermo Star Catalogue. When the Catalogue was published in 1814, the unfamiliar names "Sualocin" and "Rotanev" were attached to "Alpha" and "Beta Delphini", respectively. Eventually the Reverend Thomas Webb, a British astronomer, puzzled out the explanation. Cacciatore's name, "Nicholas Hunter" in English translation, would be Latinized to "Nicolaus Venator". Reversing the letters of this construction produces the two names. They have endured, the result of Cacciatore's little practical joke of naming the two after himself. How Webb arrived at this explanation 45 years after the publication of the catalogue is still a mystery.
In 2016, the International Astronomical Union organized a Working Group on Star Names (WGSN) to catalogue and standardize proper names for stars. The WGSN decided to attribute proper names to individual stars rather than entire multiple systems. It approved the name "Rotanev" for the component Beta Delphini A on 12 September 2016 and it is now so included in the List of IAU-approved Star Names.
In Chinese, (), meaning "Good Gourd", refers to an asterism consisting of Beta Delphini, Alpha Delphini, Gamma2 Delphini, Delta Delphini, and Zeta Delphini.
Properties.
Beta Delphini was found to be a binary star system in 1873 by the American astronomer S. W. Burnham. The system consists of a pair of F-type stars that orbit each other with a period of 26.66 years and an eccentricity of 0.36. The plane of the orbit is inclined by an angle of 61° to the line of sight from the Earth. The two stars have an angular separation of about 0.44 arcseconds, making them a challenge to resolve with a telescope. The larger member of the pair is a giant star with 1.75 times the mass and 24 times the luminosity of the Sun, while the secondary component is a subgiant star that has 1.47 times the Sun's mass and around 8 times the Sun's luminosity. The system is around 1.8 billion years old.


Mu Virginis

Mu Virginis (μ Vir, μ Virginis) is a star in the zodiac constellation of Virgo. It was listed in the "Calendarium" of Al Achsasi al Mouakket as "rijl al-‘awwā’", Arabic رجل العواء, meaning "The foot of the barking (dog)". With an apparent visual magnitude of 3.88, it is bright enough to be seen with the naked eye. The position of the star near the celestial equator means it is visible from most of the Earth. Based upon parallax measurements, Mu Virginis is located some 59.6 light years from the Sun.
Rijl al Awwa is an F-type main sequence star with a stellar classification of F2 V, although it does show some evidence of being a more evolved star. It has an effective temperature of 6,751 K in its outer atmosphere. The estimated age of the star is 1.5 billion years, and it has a relatively high 47.0 km/s projected rotational velocity. A 1990 study of the star gave it a giant star classification, and modeled it with 1.7 times the mass of the Sun, 2.1 times the Sun's radius, and shining with 9.8 times the Sun's luminosity.
Past observations of this star appear to show some indications of short term chromospheric variability as well as radial velocity variations. It has a candidate common proper motion companion at a projected separation of 770 AU. This object has a J band magnitude of 10.72.


Nu Scorpii

Nu Scorpii (ν Scorpii, abbreviated Nu Sco, ν Sco) is a multiple star system in the constellation of Scorpius. It is most likely a septuple star system, consisting of two close groups (designated Nu Scorpii AB and CD) that are separated by 41 arcseconds. Based on parallax measurements, it is approximately 470 light-years from the Sun.
The component Nu Scorpii Aa is formally named Jabbah .
Location.
Nu Scorpii is the system that causes the reflection nebula cataloged as IC 4592 and known as the Blue Horsehead nebula. Reflection nebulae are actually made up of very fine dust that normally appears dark but can look quite blue when reflecting the light of energetic nearby stars.
Since it is near the ecliptic, Nu Scorpii can be occulted by the Moon and, very rarely, by planets. Mercury occulted it on 14 December 1821, but will not occult it again until 2 December 2031. The last occultation by Venus took place on 27 December 1852 and the next will take place on 30 December 2095. On 29 July 1808 there was an occultation by Neptune.
Nomenclature.
"ν Scorpii" (Latinised to "Nu Scorpii") is the system's Bayer designation. The designations of its two constituent groups as "Nu Scorpii AB" and "CD"; of the component "Nu Scorpii Aa", and of other components similarly lettered, derive from the convention used by the Washington Multiplicity Catalog (WMC) for multiple star systems, and adopted by the International Astronomical Union (IAU).
Nu Scorpii bore the traditional name "Jabbah", possibly from the Arabic "Iklīl al Jabhah" (إكليل الجبهة 'the crown of the forehead'). In 2016, the IAU organized a Working Group on Star Names (WGSN) to catalog and standardize proper names for stars. The WGSN decided to attribute proper names to individual stars rather than entire multiple systems. It approved the name "Jabbah" for the component Nu Scorpii Aa on 30 June 2017 and it is now so included in the List of IAU-approved Star Names.
In Chinese astronomy, Nu Scorpii is called 鍵閉, Pinyin: Jiànbì, meaning "Door Bolt", because it is marking itself and standing alone in the "Door Bolt" asterism, Room mansion (see : Chinese constellations). 鍵閉 (Jiànbì), westernized into "Keen Pi", but that name (meaning "the Two Parts of a Lock") was ascribed to the pair Lambda Scorpii (Shaula) and Upsilon Scorpii (Lesath) by R.H. Allen.
Multiplicity.
Hierarchy of orbits in the ν Scorpii system
Nu Scorpii is a septuple star system. It is one of only two known systems, the other being AR Cassiopeiae. Higher-multiplicity star systems are uncommon because they are less stable than their simpler counterparts, and often decay into smaller systems.
Nu Scorpii is split into two groups, Nu Scorpii AB and Nu Scorpii CD. Nu Scorpii CD is located 41 arcseconds away from Nu Scorpii A, and is also known as HR 6026.
Nu Scorpii A.
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. The main component of Nu Scorpii A is known as Nu Scorpii Aab, and it is a single-lined spectroscopic binary. Its components cannot be resolved but the stars' movements cause periodic Doppler shifts in their spectra. "Single-lined" means that light from only one of the stars can be detected. The pair has an orbital period of 5.5521 days and an eccentricity of 0.11, and an estimated separation of about 1.057 milliarcseconds. 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.
Nu Scorpii B.
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.
Nu Scorpii CD.
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.
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.


Eta Scorpii

Eta Scorpii, Latinized from η Scorpii, is a star in the southern zodiac constellation of Scorpius. With an apparent visual magnitude of 3.33, this is one of the brighter members of the Scorpius and is the furthest south of the constellation stars with a Bayer designation. The distance to this star can be estimated using parallax measurements, yielding a value of with a 0.4% margin of error.
The stellar classification of this star has undergone some revision over time, with the star being classified anywhere from an F-type main sequence star to a giant star. In 2006, the NStars program assigned it a class of F5 IV, where the luminosity class of 'IV' indicates this is a subgiant star that is exhausting the supply of hydrogen at its core and is in the process of evolving into a giant star. It has around 175% of the Sun's mass with an estimated age of 1.1 billion years. The star is radiating about 18 times the luminosity of the Sun from its outer atmosphere at an effective temperature of 6,533 K. It is this heat that gives it a yellow-white hue that is typical for an F-type star.
Eta Scorpii is rotating rapidly, with a projected rotational velocity of . This is causing the star to spin on its axis with a period of less than a day. It is an X-ray emitter with its stellar corona giving off an X-ray luminosity of . In 1991 it was identified as a possible barium star, as it displays an enhanced abundance of the element barium in its spectrum. Overall, the abundance of elements other than hydrogen and helium, what astronomers term the star's metallicity, is similar to the abundance in the Sun.


Delta Lyrae cluster

Delta Lyrae cluster is a sparse open cluster of stars located about 1,220 light years away in the northern constellation of Lyra. Centered on the member star Delta2 Lyrae for which it is named.
This cluster was first suspected in 1959 by American astronomer Charles B. Stephenson, then was later concluded not to exist by German astronomer Werner Bronkalla in 1963. However, subsequent photometric observations at the Palomar and Mount Wilson observatories led American astronomer Olin J. Eggen to demonstrate that there was an actual cluster, at least for the observed stars down to absolute magnitude +5.5. Eggen's study found at least 33 members.
The cluster has a visual magnitude of 3.8 and spans an angular diameter of 20 arc minutes. The tidal radius of the cluster is and it has an estimated combined mass of 589 times the mass of the Sun. Based upon its estimated age and motion through space, it may be associated with the Gould Belt. It includes an Algol variable star, BD+36° 3317, discovered in 2007 from Spain: this is a spectroscopic binary star system that undergoes regular eclipses because the orbital plane is nearly aligned with the line of sight to the Earth.


NGC 6975

NGC 6975, also known as NGC 6976, is a spiral galaxy in the constellation Aquarius. The object was discovered on 12 July 1864 by the German astronomer Albert Marth.
NGC 6975 is part of Hickson Compact Group 88, along with NGC 6977, NGC 6978, and MCG-01-53-014. The group is at a distance of about 273 million light years (84 million parsecs). In 2012, supernova SN 2012ga was discovered within NGC 6975.


K2-72

K2-72 (also designated EPIC 206209135) is a cool red dwarf star of spectral class M2.7V located about away from the Earth in the constellation of Aquarius. It is known to host four planets, all similar in size to Earth, with one of them residing within the habitable zone.
Nomenclature and history.
K2-72 also has the 2MASS catalogue number J22182923-0936444. Its EPIC (Ecliptic Plane Input Catalog) number is 206209135.
The star's planetary companions were discovered by NASA's Kepler Mission, a mission tasked with discovering planets in transit around their stars. The transit method that Kepler uses involves detecting dips in brightness in stars. These dips in brightness can be interpreted as planets whose orbits move in front of their stars from the perspective of Earth. The name K2-72 derives directly from the fact that the star is the catalogued 72nd star discovered by the "K2" mission to have confirmed planets.
The designation "b", "c", "d", and "e" derives from the order of discovery. The designation of "b" is given to the first planet orbiting a given star, and "e" to the last. In the case of K2-72, there were four planets, so only letters "b" to "e" are used. At first the planets were all thought to be smaller than Earth. However, in 2017, new analysis by Martinez "et al." and Courtney Dressing found that K2-72 was significantly larger than previous estimates, and found that the planets were all larger than Earth, although all are still expected to be rocky.
Stellar characteristics.
K2-72 is a M-type star that is approximately 27% the mass of and 33% the radius of the Sun, according to the analysis done by Dressing "et al." The results found by Martinez "et al." suggest a larger star, with about 36% the radius and mass of the Sun. Both give a luminosity estimate between 0.013 and 0.015 solar luminosities. 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.
Planetary system.
The star is known to host four planets, all likely to be rocky. Only one (K2-72e) is currently known to reside inside the habitable zone, although K2-72c may straddle the inner edge.


23 Arietis


33 Cygni

33 Cygni is a single star located 159 light years away in the northern constellation Cygnus. Its is visible to the naked eye as a white-hued star with an apparent visual magnitude of 4.28. The star is moving closer to the Earth with a heliocentric radial velocity of −16 km/s. Eggen (1995) listed it as a proper motion candidate for membership in the IC 2391 supercluster.
This star has a stellar classification of A3 IV–Vn, showing a spectrum with traits intermediate between an A-type main-sequence star and an evolving subgiant star. The 'n' suffix indicates "nebulous" absorption lines due to rapid rotation. It is about 400 million years old with a high projected rotational velocity of 243 km/s. This rate of spin is giving the star an oblate shape with a pronounced equatorial bulge that is an estimated 28% wider than the polar radius.
33 Cyg has 2.33 times the mass of the Sun and 2.76 times the Sun's radius. The star is radiating 44 times the Sun's luminosity from its photosphere at an effective temperature of 8,395 K. It displays an infrared excess that suggests an orbiting debris disk with a temperature of 500 K at a mean distance of from the host star.


U Carinae

The Bayer designations U Carinae and u Carinae are distinct. Due to technical limitations, both designations link here. For the star


Holmberg II

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. One hypothesis suggests that is caused by an intermediate mass black hole that is pulling surrounding material.
Holmberg II was discovered by Erik Bertil Holmberg.


PU Aurigae

PU Aurigae is an irregular variable star located in the constellation Auriga. A red giant, it varies by 0.1 magnitude around magnitude 5.64. Located around 560 light-years distant, it shines with a luminosity approximately 1,523 times that of the Sun and has a surface temperature of 3,482 K.


Kappa Centauri

Kappa Centauri (κ Cen, κ Centauri) is a binary star in the southern constellation of Centaurus. With an apparent visual magnitude of +3.14, it can be viewed with the naked eye on a dark night. Parallax measurements place it at an estimated distance of from Earth.
This is a spectroscopic binary system where the presence of an orbiting companion is revealed by shifts in the absorption lines caused by the Doppler effect. The primary component is a huge star, with about seven times the Sun's mass and four times the Sun's radius. It has a stellar classification of B2 IV, indicating that it is in the subgiant stage of its stellar evolution. An effective temperature of 19,800 K in the outer envelope is what gives it the blue-white hue of a B-type star.
The primary is a candidate Beta Cephei variable that shows line-profile variations in its spectrum. However, the nature of the variability remains uncertain because of the binary nature of the system. As of 2007, the secondary component was separated from the primary by 0.128 arcseconds at a position angle of 156°. It has about 68% of the mass of the primary. This system is a proper motion member of the Upper-Centaurus Lupus sub-group in the Scorpius-Centaurus OB association, the nearest such co-moving association of massive stars to the Sun.
In Chinese, (), meaning "Imperial Guards", refers to an asterism consisting of κ Centauri, γ Lupi, δ Lupi, β Lupi, λ Lupi, ε Lupi, μ Lup, π Lupi, ο Lupi and α Lupi. Consequently, the Chinese name for κ Centauri itself is (, .). From this Chinese name, the name Ke Kwan has appeared.


Tau Piscis Austrini

Tau Piscis Austrini (τ Piscis Austrini) is a solitary, yellow-white hued star in the southern constellation of Piscis Austrinus. It is visible to the naked eye with an apparent visual magnitude of +4.9. Based upon an annual parallax shift of 54.71 mas as seen from the Earth, the star is located 59.6 light years from the Sun.
This is an F-type main sequence star with a stellar classification of F6 V. It is about 1.3 billion years old with a projected rotational velocity of 14 km/s and exhibits a low level of activity. The star has an estimated 1.34 times the mass of the Sun and 1.45 times the Sun's radius. It is radiating 2.82 times the solar luminosity from its photosphere at an effective temperature of 6,324 K. This star is a candidate for hosting a debris disk, as it displayed an initial near infrared excess that faded with further observations.
Naming.
In Chinese, (), meaning "Celestial Money", refers to an asterism consisting of refers to an asterism consisting of τ Piscis Austrini, 13 Piscis Austrini, θ Piscis Austrini, ι Piscis Austrini and μ Piscis Austrini. Consequently, the Chinese name for τ Piscis Austrini itself is (, .)


98 Herculis

98 Herculis is a single star located approximately 590 light years from the Sun in the northern constellation Hercules. It is visible to the naked eye as a dim, red-hued point of light with an apparent visual magnitude of 4.96. The brightness of the star is diminished by an extinction of 0.19 due to interstellar dust. The star is moving closer to the Earth with a heliocentric radial velocity of −19 km/s.
This is an aging red giant star on the asymptotic giant branch with a stellar classification of M3-SIII, where the suffix notation indicating this is an S-type star. It is a mild barium star with an intensity class of 0.2, and is a suspected variable star, although Percy and Shepherd (1992) were unable to confirm this. With the hydrogen at its core exhausted, the star has expanded to around 85 times the Sun's radius. It is radiating 1,330 times the luminosity of the Sun from its swollen photosphere at an effective temperature of 3,772 K.


Fomalhaut C

Fomalhaut C or its original name, LP 876-10 is the distant third star of the Fomalhaut system. It is about five degrees from Fomalhaut, roughly halfway between it and the Helix Nebula. It is currently 2.5 light years (0.77 pc) from Fomalhaut A, and 3.2 light years away from Fomalhaut B (0.987 pc). The entire system is only around 25 light years (7.7 parsecs) from our solar system. It was originally catalogued as a lone red dwarf, until October 2013, when Eric Mamajek announced that the star had a distance, velocity and color-magnitude position consistent with it being part of the Fomalhaut system. It was most likely catalogued with no relation to Fomalhaut due to the fact that it is in the Aquarius constellation, while the rest of the system are in the Piscis Austrinus constellation.
Discovery and observation.
Fomalhaut C was catalogued as a high-proper-motion star by Willum Luyten in 1979, and later, in October 2013, was discovered to be part of the Fomalhaut system, giving it the name Fomalhaut C. The star has a mass of 0.2 solar masses, (0.2 "M☉") while Fomalhaut A is 1.9 "M☉", and Fomalhaut B is 0.7"M☉". The magnitude of this star has been recorded as 12.6. With this third star being so distant, the entire Fomalhaut system may be the widest-spanning star system that has ever been discovered. In the sky, Fomalhaut C would appear very far away from Fomalhaut, which is part of the fact of how close this system is. The distance in the night sky would be 5.5°, or around 11 full moons. Due to its magnitude, you would require a telescope to observe it at home. The entire system of Fomalhaut is around 440 million years old, which is roughly a tenth of the Solar System's age.
Debris disc.
In December 2013, a debris disc was discovered around this star. This is the second debris disc in the system, as a first one was discovered around Fomalhaut A. The debris disc was discovered with the Herschel Space Telescope, and with the telescope the debris disc's temperature has been estimated at 24 kelvins. The distance from the star was originally thought to be around 10 AU, but since it is hypothesized that it is mainly small grains, which trap more heat, it may be further. However, if it were beyond 40 AU, it would have been already cataloged, which gives it a radius between 10 and 40 AU.
Comets.
In part with the debris disc, there are also comets orbiting Fomalhaut C. The debris disc orbiting C is sometimes referred to as a comet belt, due to some very elliptical orbits. The disc around Fomalhaut A is also thought to have many comets, as it is also elliptical, along with Fomalhaut b (the planet, not to be confused with Fomalhaut B, the star). The Fomalhaut A belt is thought to possibly be due to a close encounter with either an undiscovered exoplanet, Fomalhaut B, or Fomalhaut C. With both A and C having comet belts, the absence of one around B is a mystery. Not only does the presence of comets make the belt more elliptical, it also makes it brighter which takes a part in its discovery.
With Fomalhaut b being hidden in the comets, this leads to a hypothesis that C could have hidden exoplanets within its comets and asteroids. There is another theory that A & C have interacted which could have formed C's comet belt if the interaction involved A giving up comets and debris. With Fomalhaut B not having any discs or belts around it, it could have been unaffected by the encounter between them.
Orbit.
The orbit of Fomalhaut C around A is estimated to take 20 million years to complete. Due to the age of the three stars being 440 million years, and the distance of 2.5 light years, this would mean that Fomalhaut C has only completed a full orbit around Fomalhaut A 22 times. The tidal radius of the Fomalhaut system is 6.2 light years (1.9 parsecs), which makes Fomalhaut C well within it, which further proves the Fomalhaut system as trinary.


PGC 54493

PGC 54493 is a barred spiral galaxy located about 490 million light-years away in the constellation Serpens. It is part of a galaxy group called Abell 2052. It has an estimated diameter of 140,000 light-years.


HD 40657

HD 40657 is a single star in the equatorial constellation of Orion, near the constellation border with Monoceros. It has an orange hue and is faintly visible to the naked eye with an apparent visual magnitude of 4.52. The star is located at a distance of approximately 289 light years from the Sun based on parallax. It is drifting further away with a radial velocity of +26 km/s.
This is an aging giant star with a stellar classification of K1.5III-IIIb CN-1, where the suffix notation indicates an underabundance of cyanogen in the spectrum. Having exhausted the supply of hydrogen at its core, this star cooled and expanded off the main sequence. At present it has 25 times the radius of the Sun.
HD 40657 is a suspected variable star with a brightness that has been measured ranging from magnitude 4.54 down to 4.58. It is an estimated 2.27 billion years old with 1.68 times the mass of the Sun and is spinning with a projected rotational velocity of 2.1 km/s. The star is radiating 196 times the Sun's luminosity from its swollen photosphere at an effective temperature of 4,317 K.


HD 28527

HD 28527 is a star in the constellation Taurus, and a member of the Hyades open cluster. It is faintly visible to the naked eye with an apparent visual magnitude of 4.78. The distance to this star, as determined from its parallax shift of , is . It is moving away from the Earth with a heliocentric radial velocity of .
Based upon a stellar classification of A6 IV by Cowley et al. (1969), this is an A-type subgiant star that has consumed the hydrogen at its core and is evolving away from the main sequence. Older studies had it classed as an A-type main-sequence star with a class of A7 V. At the age of 307 million years, it has a high rate of spin, revolving upon its axis once every 1.278 days. It is a Delta Scuti variable with 1.75 times the mass of the Sun and 2.2 times the Sun's radius. The star is radiating 19 times the Sun's luminosity from its photosphere at an effective temperature of 8,274 K.
Due to its location near the ecliptic, this star is subject to lunar occultations. These events have provided occasional, but not definitive, evidence of a close secondary companion. Eggleton and Tokovinin (2008) catalogue this as a possible triple star system, having the inner pair being similar stars with an angular separation of , and the outer component a magnitude 6.7 star of class F2 at a much wider separation of .


NGC 462

NGC 462 is an elliptical galaxy located in the Pisces constellation. It was discovered by Albert Marth on 23 October 1864. Dreyer, creator of the New General Catalogue, originally described it as "extremely faint, very small, stellar". The word stellar clearly suggests an initial misidentification of NGC 462 as a star.


NGC 4297

NGC 4297 is a lenticular galaxy located about 200 million light-years away in the constellation Virgo. It was discovered by astronomer William Herschel on April 13, 1784. It forms an interacting pair with NGC 4296.


Kappa Sagittarii

The Bayer designation Kappa Sagittarii (κ Sagittarii) is shared by two star systems, κ1 Sagittarii and κ2 Sagittarii, in the constellation Sagittarius. The two star systems are separated by 0.46° in the sky.


Delta Eridani

Delta Eridani, which is Latinized from δ Eridani, is a star in the equatorial constellation of Eridanus. It is sometimes called "Rana": "Rana" means "the frog" in Latin, but derivation of this name is uncertain. The star is visible to the naked eye and has been observed to vary in slightly brightness between magnitudes 3.51 and 3.56, although subsequent observations did not bear this out. It is relatively near to the Sun, with a distance of about 29.5 light years as determined from parallax. The star is drifting closer with a radial velocity of −6 km/s.
Structure.
The stellar classification of this star is K0 IV, matching a subgiant star that has exhausted its core hydrogen. This has caused the star to expand and become cooler than a comparable main sequence star. Stellar modelling indicates it is near the end of the subgiant stage and about to transition into a giant. It is an estimated six billion years old with 33% more mass than the Sun. The star has 2.3 times the girth of the Sun and is radiating three times the Sun's luminosity from its photosphere at an effective temperature of 4,986 K.
Delta Eridani is catalogued as a suspected RS Canum Venaticorum variable in 1983, but the activity level for the star is so low that this is considered doubtful. This class of variables occurs in close binary systems. A low projected rotational velocity of under 1 km/s and the lack of radial velocity variation suggests that this putative variable is being viewed from nearly pole-on. However, an examination of the star using interferometry does not detect the presence of a companion at the expected distance.
Chinese name.
In Chinese, (), meaning "Celestial Meadows", refers to an asterism consisting of δ Eridani, γ Eridani, π Eridani, ε Eridani, ζ Eridani, η Eridani, π Ceti, τ1 Eridani, τ2 Eridani, τ3 Eridani, τ4 Eridani, τ5 Eridani, τ6 Eridani, τ7 Eridani, τ8 Eridani and τ9 Eridani. Consequently, the Chinese name for δ Eridani itself is (, .)


NGC 4666

NGC 4666 is a spiral galaxy in the equatorial constellation of Virgo, located at a distance of approximately from the Milky Way. It was discovered by the German-born astronomer William Herschel on February 22, 1784. John L. E. Dreyer described it as "bright, very large, much extended 45°±, pretty suddenly brighter middle". It is a member of an interacting system with NGC 4668 and a dwarf galaxy, and belongs to a small group that also includes NGC 4632.
The morphological classification of this galaxy is SABc, which indicates a weak bar around the nucleus with moderately wound spiral arms. Viewed nearly edge-on, its galactic plane is inclined at an angle of to the line of sight from the Earth, with the major axis aligned along a position angle of 40°. There is an active galactic nucleus that shows a modest level of activity and is most likely heavily obscured by gas and dust. The central point source has been detected in the radio and X-ray bands.
This is a starburst galaxy that is noteworthy for its vigorous star formation, which creates an unusual superwind of out-flowing gas. This wind is not visible at optical wavelengths, but is prominent in X-rays, and has been observed by the ESA XMM-Newton space telescope. The estimated star formation rate is  yr–1, with a density of  yr−1 kpc−2. Unlike in many other starburst galaxies, the star formation is spread across the disk rather than being more concentrated.
A type Ia supernova was detected in NGC 4666 on 9 December 2014; ASASSN-14lp is located from the center of NGC 4666. A type Ib supernova, SN 2019yvr, was detected on 27 December 2019. It has a 0.005 redshift. Images of the location of the supernova before the explosion showed the progenitor star was ~19.


LHS 3003


NGC 289

NGC 289 is a spiral galaxy in the southern constellation of Sculptor, located at a distance of from the Milky Way. It was discovered on September 27, 1834 by John Herschel. The compiler of the New General Catalogue, John Louis Emil Dreyer noted that NGC 289 was "pretty bright, large, extended, between 2 considerably bright stars". The plane of the galaxy is inclined by an angle of 45° to the line of sight from the Earth.
This is a Type II Seyfert galaxy with an active galactic nucleus. A dust lane is seen crossing the nucleus, and there are indications of recent starburst activity nearby. NGC 289 is a giant, gas-rich, low surface brightness galaxy with a small bulge at the nucleus, a small central bar, and two inner spiral arms. These arms split into multiple parts as they extend into the outer disk. The galaxy has a dark matter halo that has an estimated 3.5 times the mass of the gaseous and stellar components. There is a dwarf elliptical companion to the north of the galaxy, designated Arp 1981, that may be having a perturbing influence.


HD 40979

HD 40979 is a triple star system in the northern constellation of Auriga. The combined brightness of this group lies below the typical limit of visibility to the naked eye at an apparent visual magnitude of 6.74. It is located at a distance of approximately 108 light years from the Sun based on parallax. The system is receding with a radial velocity of +32 km/s. It has a relatively high rate of proper motion, traversing the celestial sphere at the rate of per year.
The primary, designated component A, is an F-type main-sequence star with a stellar classification of F7V. It is an estimated 2.51 billion years old and is spinning with a projected rotational velocity of 9.1 km/s. The star has 1.21 times the mass of the Sun and 1.26 times the Sun's radius. It has a higher metallicity than the Sun – what astronomers term the relative abundance of elements with a higher atomic number than helium. The star is radiating 1.96 times the luminosity of the Sun from its photosphere at an effective temperature of 6,077 K. As of 2002, there is one extrasolar planet known to be orbiting around this star. An infrared excess suggests a debris disk is orbiting the star at a separation of with a mean temperature of 80 K.
The magnitude 9.11 secondary, component B, is a co-moving companion at an angular separation of from the primary, which corresponds to a projected separation of around . It has 83% of the mass of the Sun. This star in turn has a magnitude 12.00 companion, component C, at a separation of along a position angle of , as of 2015. This equates to a projected separation of . The star has an estimated 0.38 times the Sun's mass.
Planetary system.
In 2003, the detection of a giant planet orbiting the primary was announced. It was discovered using the radial velocity method, which allow selected orbital elements of this object to be determined.


64 Aquilae

64 Aquilae, abbreviated 64 Aql, is a star in the equatorial constellation of Aquila. "64 Aquilae" is its Flamsteed designation. It is a faint star that requires good viewing conditions to see, having an apparent visual magnitude of 5.97. The distance to 64 Aql, as determined from its annual parallax shift of 2, is 152.2 light years. At that distance, the visual magnitude of the star is diminished by an extinction of 0.029 due to interstellar dust. It is moving closer to the Earth with a heliocentric radial velocity of −3.6 km/s.
This is an evolved giant star currently on the red giant branch with a stellar classification of K1 III/IV. The luminosity class of 'III/IV' indicates the spectrum shows a blend of features matching a subgiant and giant star. It is around 6.2 billion years old with 1.17 times the mass of the Sun and has expanded to 4.5 times the Sun's radius. The star is radiating 11 times the Sun's luminosity from its enlarged photosphere at an effective temperature of 4,786 K.


J Puppis

The Bayer designations j Puppis and J Puppis are distinct. Due to , both designations link here. For the star
See also.
QW Puppis (I Puppis)


36 Draconis

36 Draconis is a star in the northern constellation Draco. It is faintly visible to the naked eye with an apparent visual magnitude of 4.99. Based upon an annual parallax shift of 43.63 mas, it is located about 74.8 light years away. At that distance, the visual magnitude is diminished by an extinction of 0.129 due to interstellar dust. The star has a relatively high proper motion, traversing the celestial sphere at the rate of 0.353 arc seconds per year. It is moving closer to the Sun with a radial velocity of −35.6 km/s.
This is an ordinary F-type main-sequence star with a stellar classification of F5 V. It has 1.23 times the mass of the Sun and 1.64 times the Sun's radius. The star is around three billion years old and is spinning with a projected rotational velocity of 8 km/s. It is radiating 4.7 times the Sun's luminosity from its photosphere at an effective temperature of 6,638 K.
Observations carried out in 2010 and 2012 detected a faint companion at an angular separation of 3.3 arcseconds. Judging by the age and magnitude, this is a red dwarf of class M3.


Sigma Librae

Sigma Librae (σ Librae, abbreviated Sigma Lib, σ Lib) is a binary star in the constellation of Libra. The apparent visual magnitude is +3.29, making it visible to the naked eye. Based upon parallax measurements, this system is at a distance of roughly from the Sun, with a 2% margin of error. At that distance, the visual magnitude is diminished by 0.20 ± 0.17 from extinction caused by intervening gas and dust.
The two components are designated Sigma Librae A (officially named Brachium , the traditional name for the system) and B.
Nomenclature.
"σ Librae" (Latinised to "Sigma Librae") is the system's current Bayer designation (the star originally bore the designation Gamma Scorpii) and did not receive its current designation until the new designation was agreed upon by Commission 3 of the International Astronomical Union (IAU) on July 31, 1930.) The designations of the two components as "Sigma Librae A" and "B" derives from the convention used by the Washington Multiplicity Catalog (WMC) for multiple star systems, and adopted by the International Astronomical Union (IAU).
It bore the traditional Latin names "Brachium" (arm) and "Cornu" (horn), and the non-unique minor Arabic names "Zuben el Genubi" (southern claw) (shared with Alpha Librae); "Zuben Hakrabi" (shared with Gamma Librae and Eta Librae, also rendered as "Zuban Alakrab"), and "Ankaa" (shared with Alpha Phoenicis). In 2016, the IAU organized a Working Group on Star Names (WGSN) to catalog and standardize proper names for stars. The WGSN decided to attribute proper names to individual stars rather than entire multiple systems. It approved the name "Brachium" for the primary component Sigma Librae A on 5 September 2017. "Ankaa" had previously been approved as the name for Alpha Phoenicis on 29 July 2016. Both are now so included in the List of IAU-approved Star Names.
In Chinese, (), meaning "Executions (asterism)", refers to an asterism consisting of σ Librae, 50 Hydrae, 3 Librae, 4 Librae and 12 Librae. Consequently, the Chinese name for σ Librae is (, ).
Properties.
The primary, Sigma Librae A, has a spectral class M2.5 III, which places it in the red giant stage of its evolution. This is a semi-regular variable star with a single pulsation period of 20 days. It shows small amplitude variations in magnitude of 0.10–0.15 on time scales as brief as 15–20 minutes, with cycles of repetition over intervals of 2.5–3.0 hours. This form of variability indicates that the star is on the asymptotic giant branch and is generating energy through the nuclear fusion of hydrogen and helium along concentric shells surrounding an inert core of carbon and oxygen.
The companion, Sigma Librae B, is of the 16th magnitude and over an arc minute away.


K Puppis

k Puppis (k Pup, k Puppis) is a Bayer designation given to an optical double star in the constellation Puppis, the two components being k1 Puppis and k2 Puppis.
Bayer designation.
Note that the Bayer designation for this star is "k" not "kappa" (κ). In Bayer's original Uranometria, k Puppis was listed as ρ (rho) Navis. When Lacaille broke apart the large constellation Argo Navis into Carina, Puppis, and Vela, he re-designated the stars with Greek letters in a single sequence across all three constellations. Additionally, Lacaille used Latin letters for many additional stars. κ (kappa) is in the constellation of Vela and so there is no kappa in Puppis. The confusion also extends to the proper name Markab which properly applies to κ Velorum (and other stars) but which has also been used for k Puppis when it is called κ Puppis.
Description.
Both k1 Puppis and k2 Puppis are bright blue B-type stars of nearly equal brightness, +4.50 and +4.62, respectively. To the naked eye, the pair has a combined magnitude of +3.80. On the sky, the two stars are separated by approximately 9.9 seconds of arc along PA 318°. The optical pair can be distinguished easily with a small telescope. The component k1 Puppis is a binary star system in its own right, while k2 Puppis is a variable star. Each star within the k Puppis optical pair is between 450 and 470 light years from Earth.
k Puppis is listed in the General Catalogue of Variable Stars as a suspected variable star, but the range and type are not stated. The "International Bulletin of Variable Stars" has since published research showing that k2 Puppis is the variable component. 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. All of its spectral lines show variability, probably due to variations in the chemical makeup of its atmosphere as it rotates.
External links.


NGC 268

NGC 268 is a spiral galaxy located in the constellation Cetus. It was discovered on November 22, 1785 by William Herschel.


Nu Canis Majoris

The Bayer designation Nu Canis Majoris (ν CMa / ν Canis Majoris) is shared by three star systems, in the constellation Canis Major:
They are separated by the different asterism in Chinese astronomy. ν¹ Canis Majoris was not any member of asterism. ν² Canis Majoris was stand alone in asterism 野雞 (Yě Jī), "Wild Cockerel". ν³ Canis Majoris was member of asterism 軍市 (Jūn Shì), "Market for Soldiers". Both of asterisms were lied in "Well" mansion.


MACHO-98-BLG-35

MACHO-98-BLG-35 was a gravitational microlensing event that occurred in July 1998 in the constellation Sagittarius. The red dwarf star causing the lens may have a planet, according to one study.


H Carinae

The Bayer designations h Carinae and H Carinae are distinct.


Kappa Leonis

Kappa Leonis, Latinized from κ Leonis, is a double star in the constellation Leo. It was called "Al-minħar al-asad", meaning the Lion's nose. The name is corrupted as "Al Minliar al Asad" in the Yale "Bright Star Catalogue". This star is visible to the naked eye with an apparent visual magnitude of 4.46. It has an annual parallax shift of 16.20 mas as seen from Earth, which provides a distance estimate of about 201 light years. Kappa Leonis is moving away from the Sun with a radial velocity of +28 km/s.
The primary component is an evolved K-type giant star with a stellar classification of K2 III. It is about the same age as the Sun with an estimated 144% of the Sun's mass and has expanded to 17 times the Sun's girth. It is radiating 89 times the luminosity of the Sun from its enlarged photosphere at an effective temperature of 4,400 K.
Kappa Leonis has a magnitude 10.4 companion at an angular separation of 2.1 arc seconds. The pair most likely form a binary star system. The companion is a suspected variable star.


Lambda Pictoris

λ Pictoris, Latinised as Lambda Pictoris, is a solitary, orange-hued star in the southern constellation of Pictor. It is visible to the naked eye, having an apparent visual magnitude of +5.29. With an annual parallax shift of 8.71 mas as seen from the Earth, it is located around 374 light years from the Sun. At the estimated age of 2.24 billion years old, it is an evolved K-type giant star with a stellar classification of K0/1 III. Lambda Pictoris has 2.2 times the mass of the Sun and is radiating 112 times the Sun's luminosity from its photosphere at an effective temperature of 4,581 K.


Phi Pegasi

φ Pegasi, Latinised as Phi Pegasi, is a solitary, reddish hued star in the northern constellation of Pegasus. With an apparent visual magnitude of around 5.1, it is a faint star that can be seen with the naked eye. Based upon an annual parallax shift of 7.05 mas as seen from Earth, the system is located around 460 light years distant from the Sun. At that distance, the visual magnitude of the star is diminished by an extinction factor of 0.15 due to interstellar dust.
This is an evolved red giant star with a stellar classification of M2.5 IIIb. It is a semiregular variable that ranges between magnitudes 5.11 and 5.17. Hipparcos mission photometry gives an amplitude variation of 0.0148 in magnitude with a frequency of 11.4 cycles per day.
In terms of its right ascension coordinates, φ Pegasi is located very near the line of the vernal equinox and will cross over around the year 3030, due to the precession of the Earth's axis.


HD 83095

HD 83095 is a single star in the southern constellation of Carina. It has the Bayer designation H Carinae; "HD 83095" is the identifier from the "Henry Draper Catalogue". This object has an orange hue and is dimly visible to the naked eye with an apparent visual magnitude of 5.46. The star is located at a distance of approximately 710 light years from the Sun based on parallax, and is drifting further away with a radial velocity of +14 km/s. It has an absolute magnitude of −1.45.
This is an aging K-type giant star with a stellar classification of K4III, having exhausted the supply of hydrogen at its core then cooled and expanded off the main sequence. At present it has about 60 times the radius of the Sun and is radiating 769 times the Sun's luminosity from its swollen photosphere at an effective temperature of 3,940 K.


Tau Cassiopeiae

Tau Cassiopeiae (τ Cassiopeiae) is a solitary, orange hued star in the northern constellation of Cassiopeia. It is bright enough to be seen with the naked eye, having an apparent visual magnitude of +4.86. Based upon an annual parallax shift of 18.75 mas as seen from Earth, this system is located about 174 light years from the Sun.
The spectrum of this star indicates it is an evolved, K-type giant star with a stellar classification of K1 IIIa. It is a suspected variable star of unknown type. Tau Cassiopeiae is 3.9 billion years old with about 1.44 times the mass of the Sun and 10 times the Sun's radius. It is radiating 40 times the Sun's luminosity from its expanded photosphere at an effective temperature of around 4,617 K.
Naming.
In Chinese, (), meaning "Flying Serpent", refers to an asterism consisting of τ Cassiopeiae, α Lacertae, 4 Lacertae, π2 Cygni, π1 Cygni, HD 206267, ε Cephei, β Lacertae, σ Cassiopeiae, ρ Cassiopeiae, AR Cassiopeiae, 9 Lacertae, 3 Andromedae, 7 Andromedae, 8 Andromedae, λ Andromedae, κ Andromedae, ι Andromedae, and ψ Andromedae. Consequently, the Chinese name for τ Cassiopeiae itself is (, )


Legs (Chinese constellation)

The Legs mansion (奎宿, pinyin: Kuí Xiù) is one of the Twenty-eight mansions of the Chinese constellations. It is one of the western mansions of the White Tiger.
Cultural significance.
In East Asian cultures, the Legs mansion (Kuí Xiù) represents wisdom, scholarship and literature. A notable example is a structure known as "Kuiwen Pavilion" (奎文閣) in the many Confucius temples in China and other East Asian countries.


NGC 5886

NGC 5886 is an +14 magnitude elliptical galaxy in the constellation Boötes. It was originally discovered by John Herschel in 1828 with an 18.7 inch reflector.


K2-28

K2-28 is a metal rich M4-type main sequence star. One confirmed transiting exoplanet is known to orbit this star. There is another star 5.2 arcseconds to the north–east of K2-28 however this star has a different proper motion and is therefore physically unrelated and probably a background star.
Planetary system.
Discovery.
K2-28b was first noticed as a candidate extrasolar planet by Vanderburg et al. in 2016, who, in a search of 59,174 stars from the Kepler space telescope's first year of K2 observations, found 234 planetary candidates. Shortly thereafter the K2-ESPRINT Project confirmed that the candidate was a super-Earth sized planet in a close orbit around a red dwarf star.
Characteristics.
K2-28b is a sub-Neptune sized planet orbiting its star in only 2.26 days. Despite its short orbital period the equilibrium temperature of the planet is a relatively low 500 Kelvin due to the low luminosity of the parent star. Because of the very small size of the parent star this planet is a particularly favorable target for transmission spectroscopy by the James Webb Space Telescope which should be able to determine if the atmosphere is cloudy or clear by observing roughly 5 transits. Among a group of small and cool planets orbiting relatively bright M-dwarfs its predicted secondary eclipse depth of 230 parts-per-million is second only to Gliese 1214 b.


HD 60532

HD 60532 is a white (F-type) main sequence star located approximately 84 light-years away in the constellation of Puppis, taking its primary name from its Henry Draper Catalogue designation. It is calculated to be 1.44 times more massive than the Sun. The star is only 59% as old as our Sun (2.7 Gyr) and has metallicity of only 38% that of our Sun. In 2008, two extrasolar planets were discovered in orbit around it.
Planetary system.
In September 2008, two Jupiter-like planets were found orbiting the star. The orbital periods of these two planets appear to be in 3:1 resonance.


Theta Cancri

Theta Cancri, Latinized from θ Cancri, is a multiple star system in the zodiac constellation of Cancer. It is visible to the naked eye as a dim point of light with an apparent visual magnitude of +5.32. The system is located at a distance of approximately 450 light years away from the Sun, based on parallax, and is drifting further away with a radial velocity of +44 km/s. Since it is near the ecliptic, it can be occulted by the Moon and, very rarely, by planets.
The primary, designated component A, is K-type giant star with a stellar classification of K5 III, having exhausted the supply of hydrogen at its core, then cooled and expanded. At present it has 40 times the girth of the Sun. It is radiating 353 times the luminosity of the Sun at an effective temperature of 3,955 K.
In Chinese astronomy, "Ghost" () refers to an asterism consisting of Theta Cancri, Eta Cancri, Gamma Cancri and Delta Cancri. Theta Cancri is the first star of Ghost (), as it is also the determinative star for that asterism.


NGC 388

NGC 388 is an elliptical galaxy located in the constellation Pisces. It was discovered on November 4, 1850 by Bindon Stoney. It was described by Dreyer as "very faint, small, round." Along with galaxies NGC 375, NGC 379, NGC 382, NGC 383, NGC 384, NGC 385, NGC 386 and NGC 387, NGC 388 forms a galaxy cluster called Arp 331.


Omicron Cephei

Omicron Cephei, Latinized from ο Cephei, is a binary star in the constellation of Cepheus. It consists of a less massive F-type main sequence star in orbit with a more massive G-type giant star. The overall apparent visual magnitude of the system is 4.75.
The pair was first determined to be binary by F. G. W. Struve in 1832. Since then, the secondary has been seen to revolve approximately 45 degrees around the primary. A number of orbits have been computed, the most recent giving a period of approximately 1500 years.
Visual companion.
There is a visual companion, "CCDM J23186+6807C", to the binary star. It has an approximate apparent visual magnitude of 12.8 and is located approximately 45 arcseconds away from it.


58 Ophiuchi

58 Ophiuchi is a single star in the equatorial constellation of Ophiuchus. It is visible to the naked eye as a faint, yellow-white hued star with an apparent visual magnitude of 4.86. This object is approximately 57.6 light years away based on parallax, and is drifting further from the Earth with a heliocentric radial velocity of +10 km/s.
This is an ordinary F-type main-sequence star with a stellar classification of F5V. It is 2.7 billion years old with a projected rotational velocity of 12 km/s. The star has an estimated 1.26 times the mass of the Sun and 1.3 times the Sun's radius. It is radiating three times the luminosity of the Sun from its photosphere at an effective temperature of 6,447 K.


R Hydrae

R Hydrae, also known as R Hya, is a Mira-type variable star in the constellation Hydra.
The magnitude of R Hydrae varies over a period of 389 days, between 3.5 and 10.9. The period of R Hydrae changes slowly.
At maximum brightness the star can be seen with the naked eye, while at minimum a telescope of at least 5 cm is needed.
R Hydrae is approximately 700 light years from Earth. Its spectral class is M6e/M9e:.


Omicron Leonis

Omicron Leonis (ο Leonis, abbreviated Omicron Leo, ο Leo) is a multiple star system in the constellation of Leo, west of Regulus, some 130 light-years from the Sun, where it marks one of the lion's forepaws.
It consists of a binary pair, designated Omicron Leonis A and an optical companion, Omicron Leonis B. A's two components are themselves designated Omicron Leonis Aa (officially named Subra , the traditional name for the system) and Ab.
Nomenclature.
"ο Leonis" (Latinised to "Omicron Leonis") is the star's Bayer designation. The designations of the two constituents as "Omicron Leonis A" and "B", and those of "A's" components—"Omicron Leonis Aa" and "Ab"—derive from the convention used by the Washington Multiplicity Catalog (WMC) for multiple star systems, and adopted by the International Astronomical Union (IAU).
It bore the traditional name "Subra", from the Arabic زبرة "zubra" (upper part of the back), originally applied to Delta and Theta Leonis.
In 2016, the International Astronomical Union organized a Working Group on Star Names (WGSN) to catalogue and standardize proper names for stars. The WGSN decided to attribute proper names to individual stars rather than entire multiple systems. It approved the name "Subra" for the component Omicron Leonis Aa on 12 September 2016 and it is now so included in the List of IAU-approved Star Names.
Properties.
The primary is given the type F8-G0III giant and the secondary is a type A7m dwarf. Their combined apparent magnitude is +3.52.


43 Aurigae

43 Aurigae is a star located 382 light years away from the Sun in the northern constellation of Auriga. It is just bright enough to be barely visible to the naked eye with an apparent visual magnitude of 6.33. The star is moving closer to the Earth with a heliocentric radial velocity of −3.4 km/s.
This is an aging giant star with a stellar classification of K2 III, having exhausted the hydrogen at its core and expanded off the main sequence. Roughly three billion years old, this star has 1.43 times the mass of the Sun and 11 times the Sun's radius. It is radiating 49 times the luminosity of the Sun from its swollen photosphere at an effective temperature of 4,552 K.


NGC 2293

NGC 2293 is a lenticular galaxy located in the constellation Canis Major. It is located at a distance of circa 100 million light years from Earth, which, given its apparent dimensions, means that NGC 2293 is about 160,000 light years across. It was discovered by John Herschel on January 20, 1835. NGC 2293 forms a pair with NGC 2292 and has an HI ring that surrounds both galaxies.
Characteristics.
NGC 2293 is a lenticular galaxy with hints of a spiral structure. The old stars that make it give the galaxy an orange color. Located 0.8 arcminutes away from NGC 2292 lies NGC 2293. Both galaxies appear to share a common envelope and a complete ring of neutral hydrogen gas (HI) has been found to encircle both galaxies. The ring apparently has a color change to the southwestern view, that has been attributed to the presence of star formation. On the other hand, there is a marked absence of HI near the centre of the two galaxies. The total HI mass is .
It is possible that the ring is the result of an ongoing merger between the two galaxies, that would result in a giant elliptical galaxy. Various models have been suggested for the formation of the ring. The most likely model is the collision between one of the two galaxies and one more galaxy that swept gas away, with the star formation region on the ring been created by a density wave or it is a population that was stripped by the intruder galaxy. It hasn't been ruled out that the positioning is an projection effect of two galaxies separated by a few million light years.
Based on far infrared observations there is an extensive amount of cold dust at the pair, with temperature 13 K, which is lower that dust temperature found in spiral and interacting galaxies. The temperature indicates however that it isn't of primordial origin.
Nearby galaxies.
NGC 2292/2293 pair belongs to a galaxy group known as LGG 138. Other members of the group are the spiral galaxy NGC 2280, NGC 2295, ESO 490−G010 and ESO 490−G045. Because of its large angular diameter, about one degree, the group was identified when redshift information were available, by Garcia et al. in 1993.


NGC 399

NGC 399 is a barred spiral galaxy located in the constellation Pisces. It was discovered on October 7, 1874 by Lawrence Parsons. It was described by Dreyer as "very faint, small, round."


Lambda Orionis Cluster

The Lambda Orionis Cluster (also known as the Collinder 69) is an open star cluster located north-west of the star Betelgeuse in the constellation of Orion. It is about five million years old and roughly away from the Sun. Included within the cluster is a double star named Meissa. With the rest of Orion, it is visible from the middle of August in the morning sky, to late April before Orion becomes too close to the Sun to be seen well. It can be seen from both the northern hemisphere and the southern hemisphere.
Description.
The cluster is following an orbit through the Milky Way that has a period of 227.4 million years with an ellipticity of 0.06, carrying it as far as from the Galactic Center, and as close as . The inclination of the orbit carries it up to away from the galactic plane. On average it crosses the plane every 33.3 million years.
The star cluster is young and contains a large number of low-mass stars, some T Tauri stars and brown dwarfs. One notable member is LOri167, which is a wide binary consisting of a potential planetary-mass object and a brown dwarf. Observations of the star cluster with the Spitzer Space Telescope have shown that 25% of the low-mass stars and 40% of the substellar objects are surrounded by a circumstellar disk. Two of these being actively photoevaporated by Meissa.
Molecular ring and cluster evolution.
The cluster might have formed in the central region of an elongated cloud, which is supported by the distribution of pre-main-sequence star candidates, which are concentrated in the cluster and nearby regions in an elongated shape. Massive OB stars and low-mass stars formed in the central regions of these clouds. The low-mass stars closest to the massive stars likely lost their circumstellar disks due to photoevaporation. Many low-mass stars parsecs away were unaffected by this and represent the current population of low-mass stars with a circumstellar disk. The cluster is surrounded by a large molecular ring, called the Lambda Orionis ring. This was interpreted as a remnant of a supernova that exploded one Million years ago. The supernova blast encountered the clouds and gas in the region and the blast dispersed the parent core, creating the molecular ring.
See also.
Other celestial bodies included in the constellation Orion:


40 Cancri

40 Cancri is a binary star system in the zodiac constellation of Cancer, located about 614 light years from the Sun in the Beehive Cluster (NGC 2632). It is a challenge to view with the naked eye, having an apparent visual magnitude of 6.61. The system is moving further from the Earth with a heliocentric radial velocity of 34 km/s.
The primary component appears to be a normal A-type main-sequence star with a stellar classification of A1 V, showing neither an organized magnetic field nor a chemical peculiarity. However, it has an excessive temperature for its luminosity, and thus is considered an extreme blue straggler. This is a second generation star formed through a collision of two low mass stars some 5–350 million years ago. The collision was either between two separate cluster members or the coalescence of a binary star system.
With an effective temperature of 9,382 K, this is the hottest star in the cluster by about 1,200 K. It has 2.46 times the mass of the Sun and 2.72 times the Sun's radius. The star has an unusually slow rotation for an A1V star, with a projected rotational velocity of 10 km/s. It is radiating 74 times the Sun's luminosity from its photosphere.
40 Cancri has a common proper motion companion, located at an angular separation of along a position angle of , as of 1983. This object is about dimmer than the primary, and is most likely an F-type star with a mass of about . The projected separation between the pair is , so their orbital period is 450 years or greater.


HD 65750

HD 65750, also known as V341 Carinae is a bright red giant star in the constellation Carina. It is surrounded by a prominent reflection nebula, known as IC 2220, nicknamed the Toby Jug Nebula.
Characteristics.
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 .
Nebulae.
The nebulae is a mystery as the variations in nebulae brightness appear to be unrelated to the host star.
One theory is that rather than being an accreting protoplanetary disk the star may be an evolved star that is losing material.


NGC 3007

NGC 3007 is an edge-on, magnitude 13.4, lenticular galaxy in the constellation of Sextans, discovered by Édouard Stephan on March 16th, 1855. It is about 115 thousand light years across, and with a recessional velocity of 6,520 kilometers per second, is at a distance of over 300 million light-years from the Sun.


Palomar 6

Palomar 6 is a loose globular cluster in the constellation Ophiuchus that belongs to the halo of the Milky Way galaxy.
First discovered on the National Geographic Society – Palomar Observatory Sky Survey plates by Robert G. Harrington and Fritz Zwicky,
it was catalogued as a globular cluster, and is one of four globulars known to contain a planetary nebula.


Pi5 Orionis

Pi5 Orionis (π5 Ori, π5 Orionis) is a binary star system in the constellation Orion. It has an apparent visual magnitude of 3.69, which is bright enough to be visible to the naked eye on a clear night. Based upon an annual parallax shift of 2.43 mas, it is around 1,300 light years distant from the Sun.
This is a single-lined spectroscopic binary star system in a circular orbit with an orbital period of 3.7005 days. It is an ellipsoidal variable, which means the orbit is sufficiently close that the shapes of the components are being distorted by their mutual gravitation. This is causing the visual magnitude of the system to vary regularly by 0m.05 over the course of each orbit, as the orientation of the stars change with respect to the Earth.
The primary component is a B-type giant star with a stellar classification of B2 III. It is only 16 million years old and spins with a projected rotational velocity of 90 km/s. Pi5 Orionis has about 12.5 times the mass of the Sun and radiates 11,262 times the solar luminosity from its outer atmosphere at an effective temperature of 14,496 K.


NGC 2770

NGC 2770 is a spiral galaxy in the northern constellation of Lynx, near the northern constellation border with Cancer. It was discovered by German-born astronomer William Herschel on December 7, 1785. J. L. E. Dreyer described it as, "faint, large, much extended 150°, mottled but not resolved, 2 stars to north". NGC 2770 was the target for the first binocular image produced by the Large Binocular Telescope.
The morphological classification of SBc indicates a barred spiral with moderately-wound arms. The physical properties of this galaxy are similar to those of the Milky Way. The combined mass of stars in the galaxy is estimated at , and it has a star formation rate of  y−1. There are no apparent perturbations of the galaxy due to suspected interaction with the companion galaxy, NGC 2770B.
As of 2017, up to four supernovae events have been discovered in this galaxy. Three were of Type Ib: SN 1999eh, SN 2007uy, and SN 2008D. The last of these was the first supernova detected by the X-rays released very early on in its formation, rather than by the optical light emitted during the later stages, which allowed the first moments of the outburst to be observed. It is possible that NGC 2770's interactions with a suspected companion galaxy may have created the massive stars causing this activity. SN 2015bh, discovered in NGC 2770 in February 2015, was either a Type II supernova or the hyper-eruption of a luminous blue variable.


Gamma Sagittarii

The Bayer designation γ Sagittarii (Gamma Sagittarii) is shared by two stars in the constellation Sagittarius:
The two stars are separated by slightly under one degree.


K2-229b

K2-229b (previously designated EPIC 228801451.01) is an extremely hot, solid, iron-rich exoplanet in a close orbit around the active K-dwarf K2-229 in the constellation Virgo, 335 light years away from Earth.
Characteristics.
Mass, radius, and temperature.
K2-229b is a relatively Earth-sized planet, first identified using the transit method, where a planet passes in front of its host star and blocks a tiny fraction of its light. When the planet was first discovered, only its radius was known. It was determined to be 1.165 , or about 16.5% larger than Earth. A planet of this size is most likely rocky with a solid surface, like Earth itself. However, radial velocity measurements using the HARPS spectrograph revealed that K2-229b was far denser and more massive than initially expected. The planet has a mass of 2.59 and an extremely high density of about 8.9 g/cm3, giving it about 91% more surface gravity than Earth. The unusually high mass and density of K2-229b indicates a Mercury-like composition dominated by an iron core taking up about 70% of the planet's mass.
Due to its extremely tight orbit, K2-229b is one of the hottest planets yet found. It has an equilibrium temperature of , hot enough to melt iron. The day side has an even higher temperature in excess of .
Orbit and Rotation.
K2-229b has one of the shortest orbital periods known, with one full orbit taking just 0.584 days (14 hours) to complete. The planet orbits its host star at a distance of 0.012888 AU, nearly 100 times closer in than Earth. For comparison, our Solar System's innermost planet, Mercury, takes 88 days to orbit at 0.39 AU. K2-229b has an orbital eccentricity of 0 and is most likely tidally locked with its host star.
Host star.
K2-229b orbits the orange dwarf star K2-229, which is about 79% the radius and 84% the mass of the Sun, with a temperature of 5185 K and an age of about 5.4 billion years. For comparison, the Sun has a temperature of 5778 K and is 4.5 billion years old. K2-229 has a visual magnitude of 10.985, too faint to be seen without a telescope. It is noted for being extremely active.
Formation, composition, and conditions.
The discovery of the high mass and density of K2-229b was unexpected. "When we saw this planet that was Earth-sized, we thought it would have an Earth-like composition. But it turns out it's more like Mercury", astrophysicist Jessie Christiansen, who was not part of the team which discovered K2-229b, told "Newsweek". The unusual Mercury-like composition of K2-229b is believed to offer insight into how it and other high-density, Mercury-like planets could have formed.
There are multiple hypotheses on how K2-229b became so dense, with one stating that much of the planet's atmosphere was eroded away by stellar radiation from its nearby, active star. Another hypothesis suggests that K2-229b was formed when two planets in the system collided, much like the theory on how the Moon was created from a collision between Earth and another planet. As of March 2018, all these theories are still in play, and there is not enough evidence to either prove or refute them.
Researchers also noted K2-229b's position in its planetary system. "Interestingly K2-229b is also the innermost planet in a system of at least 3 planets, though all three orbit much closer to their star than Mercury. More discoveries like this will help us shed light on the formation of these unusual planets, as well as Mercury itself", commented Dr. David Armstrong, one of the members of the team from the University of Warwick's Astronomy and Astrophysics Group which discovered the planet.
K2-229b is noted for being quite similar to Mercury, with about the same core-mass fraction of 68 %. However, the former is far closer to its host star and is more susceptible to mantle evaporation than the latter. With a day side temperature of over 2,330 K (assuming it is tidally locked with its host star), K2-229 is expected to have at least a thin atmosphere of silicate vapor created from the high temperatures on the star-facing side of the planet. Despite the high activity of K2-229, the planet is not expected to completely lose this atmosphere. If K2-229b has a magnetic field it can resist atmospheric erosion, meaning that mantle evaporation is extremely unlikely to have resulted in the planet's iron-rich composition. That, and K2-229b is estimated to only lose 1.3×10−5 per year, too little to remove any more than a few percent of its total mass over its lifetime.


Theta Capricorni

Theta Capricorni, Latinized from θ Capricorni, is a white-hued star in the southern constellation of Capricornus, 0.58° south of the ecliptic. Sometimes, this star is called by the name Dorsum, meaning "the back (of the goat)" in Latin. It can be seen with the naked eye, having an apparent visual magnitude of +4.07. Based upon an annual parallax shift of 20.11 mas as seen from the Earth, the star is about 162 light years from the Sun.
This is an A-type main sequence star with a stellar classification of A1 V. Radial velocity variations indicate it may be a binary star system, but when the system was examined in the infrared, no companion was detected. Theta Capricorni has an estimated 2.24 times the mass of the Sun and around 2.7 times the Sun's radius. It is 152 million years old and is spinning fairly rapidly with a projected rotational velocity of 104 km/s. It is radiating 65 times the solar luminosity from its photosphere at an effective temperature of around 10,000 K.
Night viewing.
The star or star system is almost eclipsed by the sun on about 3 February, when it will figure behind the sun's corona if there is a full solar eclipse. Thus the star can be viewed the whole night, crossing the sky, in early August (in the current epoch).
Chinese name.
In Chinese, (), meaning "Twelve States", refers to an asterism which represents twelve ancient states in the Spring and Autumn period and the Warring States period, consisting of θ Capricorni, φ Capricorni, ι Capricorni, 38 Capricorni, 35 Capricorni, 36 Capricorni, χ Capricorni, 30 Capricorni, 33 Capricorni, ζ Capricorni, 19 Capricorni, 26 Capricorni, 27 Capricorni, 20 Capricorni, η Capricorni and 21 Capricorni. Consequently, the Chinese name for θ Capricorni itself is (, ), meaning that this star (together with 30 Capricorni) and δ Serpentis in "Right Wall of Heavenly Market Enclosure" (asterism)) represents the state Qin () (or Tsin)


FF Aquilae

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. Analysis of its brightness over 122 years shows that its period is increasing by 0.072 ± 0.011 seconds per year. It has been estimated to be ± distant from Earth (by extrapolating from its angular diameter and estimated radius).
A yellow supergiant, FF Aql pulsates with varying temperature, diameter, and luminosity. Like all Cepheids, it has exhausted its core hydrogen fuel, cooled and expanded off the main sequence, and is rapidly evolving towards the Asymptotic Giant Branch.
FF Aql is a possible quadruple star system. Analysis of its spectrum shows that it is a spectroscopic binary system with the fainter companion calculated to be a main sequence star of spectral type A9V to F3V, orbiting every 3.92 years. A third star, revealed by speckle interferometry, is likely to be a cooler star that has evolved off the main sequence. A fourth star, that is of magnitude 11.4 and located 6 arcseconds away, is unlikely to be a member of the system.


TT Corvi

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.


HD 85859

HD 85859 is a single star in the equatorial constellation of Hydra. It has an apparent visual magnitude of 4.88, which is bright enough to be visible to the naked eye. The distance to this star, as estimated from its annual parallax shift of , is 259 light years. It is moving away from the Earth with a heliocentric radial velocity of 50.5 km/s.
The stellar classification of the visible component is , which matches an evolved K-type giant star with a mild overabundance of CN in the atmosphere. At the age of 4.34 billion years, it is a red clump star, which indicates it is on the horizontal branch and is generating energy through helium fusion at its core. The star has 1.55 times the mass of the Sun and is radiating 178 times the Sun's luminosity from its enlarged photosphere at an effective temperature of 4,415 K.


Upsilon Carinae

Upsilon Carinae, Latinized from υ Carinae, is a double star in the southern constellation of Carina. It is part of the Diamond Cross asterism in southern Carina. The Upsilon Carinae system has a combined apparent magnitude of +2.97 and is approximately 1,400 light years (440 parsecs) from Earth.
In Chinese, (), meaning "Sea Rock", refers to an asterism consisting of υ Carinae, ε Carinae, ι Carinae, HD 83183 and HD 84810. Consequently, υ Carinae itself is known as (, .)
The primary component, υ Carinae A, has a stellar classification of A8 Ib, making it a supergiant star that has exhausted the hydrogen at its core and evolved away from its brief main sequence lifetime as an O9 V star. With an apparent magnitude of +3.08, it has an effective temperature of about 7,600 K, giving it a white hue. The companion, υ Carinae B, is a giant star with a classification of B7 III, although Mandrini and Niemela (1986) suggested it may be a subgiant star with a classification of B4–5 IV. The outer envelope of this star has an effective temperature of around 23,000 K, resulting in the blue-white hue of a B-type star.
The two stars have an angular separation of 5.030 arcseconds. As a binary star system, they would have an estimated orbital period of at least 19,500 years and a present-day separation of around 2,000 Astronomical Units. This system is roughly 12 million years old.
In the next 7500 years, the south Celestial pole will pass close to this stars and Iota Carinae (8100 CE).


NGC 7686

NGC 7686 is a moderate-sized open cluster in the constellation Andromeda, containing about 80 stars. At magnitude 5.6, it is an easy target for binoculars and small telescopes.
According to Johnson et al. (1961), the "color-magnitude diagram shows merely a uniform scatter with no significant tendency to show a cluster main sequence". They conclude that this is not actually a star cluster.


Phi Tauri

Phi Tauri (φ Tauri) is a solitary, orange-hued star in the zodiac constellation of Taurus. It has an apparent visual magnitude of +4.96, which indicates the star is faintly visible to the naked eye. Based upon an annual parallax shift of 10.16 mas as seen from Earth, it is located roughly 321 light years distant from the Sun. At that distance, the visual magnitude of the star is diminished by an extinction factor of 0.27 due to interstellar dust.
This is an evolved, K-type giant star with a stellar classification of K1 III, currently (97% probability) on the red giant branch. It has an estimated 1.36 times the mass of the Sun and has expanded to 19 times the Sun's radius. At the age of roughly five billion years, it is radiating 131 times the Sun's luminosity from its inflated photosphere at an effective temperature of 4,479 K.
Phi Tauri has a magnitude 7.51 visual companion located at an angular separation of 48.80 arc seconds along a position angle of 258°, as of 2015. The pair form a yellow and blue double that is visible in small telescopes. A fainter, magnitude 12.27 companion lies at a separation of 118.10 arc seconds along a position angle of 25°, as of 2001.


HD 27894

HD 27894 is a 9th magnitude star located approximately 143 light years away in the constellation of Reticulum. It is an orange dwarf (spectral type K2V), a type dimmer and cooler than our Sun.
In 2005, the Geneva Extrasolar Planet Search Team announced some of the discoveries of an extrasolar planet orbiting the star. In 2017, the discovery of two additional exoplanets was announced. One is very close to the star like the one discovered earlier, while the other one orbits the star at a much larger distance. It is the first system where such a large gap between orbital distances has been found.


HD 77338

HD 77338 is a K-type subgiant star which has recently exhausted its hydrogen fuel and has started to expand. Its surface temperature is 5315 K. HD 77338 is enriched in its concentration of heavy elements compared to the Sun, with a metallicity Fe/H index of 0.16 but is much older at an age of 9.5 billion years.
HD 77338 is unusually enriched in heavy elements for a star of its age. The anomalously high abundance of ions of manganese may indicate the star has recently passed through the common shell stage (engulfed a planet).
Planetary system.
In 2012, one planet, named HD 77338b, was discovered by the radial velocity method on a tight orbit with uncertain eccentricity. Its equilibrium temperature is 954.8 K.


39 Leonis

39 Leonis is the Flamsteed designation for a star in the zodiac constellation of Leo. It has an apparent visual magnitude of 5.90, so, according to the Bortle scale, it is faintly visible from suburban skies at night. Measurements made with the Hipparcos spacecraft show an annual parallax shift of 0.04385″, which is equivalent to a distance of around from the Sun.
The stellar classification of 39 Leonis is F6 V, indicating it is a main sequence star. It shines with a luminosity more than double that of the Sun, although it has nearly the same mass and size. This is a mature star with an estimated age of 6.3 billion years. The abundance of elements other than hydrogen and helium is about half that in the Sun, making this a metal-poor star. The effective temperature of the stellar atmosphere is 6,118 K, giving it the yellow-white hued glow of an F-type star.
Observations made with the Akari satellite at a wavelength of 18 μm show an excess of infrared emission. This suggests the presence of an inner debris disk orbiting the star at a distance greater than four astronomical units (AU). There was no significant excess found at 22 μm.
A companion star is located at an angular separation of 7.72″ along a position angle of 302.7°—this corresponds to a projected separation of 175 AU. It is a red dwarf star with a classification of M1 and an apparent visual magnitude of 11.40.


24 Ursae Majoris

24 Ursae Majoris is a variable star in the northern circumpolar constellation of Ursa Major, located 101.5 light-years from the Sun. It has the variable star designation DK Ursae Majoris and the Bayer designation d Ursae Majoris; "24 Ursae Majoris" is the Flamsteed designation. This object is visible to the naked eye as a faint, yellow-hued star with an apparent visual magnitude of 4.54. It is moving closer to the Earth with a heliocentric radial velocity of −27 km/s, and is expected to come as close as in around 879,000 years.
Description.
24 Ursae Majoris has a stellar classification of G4 III-IV, which, at the estimated age of about one billion years, matches the spectrum of an aging giant star blended with features of a subgiant luminosity class. Based upon its position on the H–R diagram, this star has just passed through the Hertzsprung gap and is ready to begin its first ascent along the red-giant branch. It is a suspected RS Canum Venaticorum variable that changes in brightness by up to 0.058 in magnitude with a period of 0.9202 days, and is an X-ray source with a luminosity of .
This star has 1.9 times the mass of the Sun and has expanded to 4.6 times the Sun's radius. It is spinning with a rotation period of 10 days. The star is radiating 14.9 times the Sun's luminosity from its enlarged photosphere at an effective temperature of 5,335 K.
Nomenclature.
With π1, π2, σ1, σ2, ρ and 2 Ursae Majoris, it composed the Arabic asterism Al Ṭhibā᾽, the Gazelle. According to the catalogue of stars in the "Technical Memorandum 33-507 - A Reduced Star Catalog Containing 537 Named Stars", "Al Ṭhibā" were the title for seven stars : 2 Ursae Majoris as "Althiba I", π1 as "Althiba II", π2 as "Althiba III", ρ as "Althiba IV", σ1 as "Althiba V", σ2 as "Althiba VI", and this star (d) as "Althiba VII".


Sigma Persei

Sigma Persei (Sigma Per, σ Persei, σ Per) is an orange K-type giant with an apparent magnitude of +4.36. It is approximately 360 light years from Earth.
Sigma Persei is moving through the Galaxy at a speed of 17.4 km/s relative to the Sun. Its projected Galactic orbit carries it between 24,400 and 43,600 light years from the center of the Galaxy. It came closest to the Sun 5.1 million years ago when it had brightened to magnitude 3.11 from a distance of 202 light years.
It has one reported planet, b, with a period of 580 days and a mass approximately 6.5 times that of Jupiter.
Name and etymology.
This star, together with δ Per, ψ Per, α Per, γ Per and η Per, has been called "the Segment of Perseus".


Upsilon Geminorum

Upsilon Geminorum, Latinized from υ Geminorum, is a star in the constellation Gemini. It has an apparent visual magnitude of 4.04, which is bright enough to be seen with the naked eye. Based upon an annual parallax shift of 12.04 mas, it is around 270 light years from the Sun. There is a visual companion: a magnitude 13.20 star located at an angular separation of 55.20″ along a position angle of 40°, as of 2008.
This is an evolved red giant star with a stellar classification of M0 III. It is estimated to have 1.52 times the mass of the Sun, but has expanded to 44 times the Sun's radius. The star is spinning with a projected rotational velocity of 5.9 km/s and is about 3.53 billion years old. Upsilon Geminorum is radiating 417 times the solar luminosity from its outer atmosphere at an effective temperature of 3926 K.
Based upon the motion of this star through space, Upsilon Geminorum is a member of the Wolf 630 moving group. This is a set of stars centered on Wolf 630 that are moving nearly in parallel and have an age of around billion years. They may be former members of a dissolved open cluster.


NGC 7085

NGC 7085 is a spiral galaxy located about 365 million light-years away in the constellation of Pegasus. NGC 7085 was discovered by astronomer Albert Marth on August 3, 1864.


KT Lupi

KT Lupi is a visual binary star system in the constellation Lupus. It is visible to the naked eye with a combined apparent visual magnitude of 4.55. As of 1983, the pair had an angular separation of . Based upon an annual parallax shift of as seen from Earth's orbit, it is located 430 light years from the Sun. The system is moving further from the Earth with a heliocentric radial velocity of +6.5 km/s. It is a member of the Lower Centaurus Crux sub-group of the Scorpius–Centaurus Association.
The primary, component A, is a variable Be star, with the variation being modulated by rotation. It is visual magnitude 4.66 with a stellar classification of B3 V, matching a B-type main-sequence star. Hiltner et al. (1969) gave a class of B3 IVp, which is still used in some studies. It is a helium-weak chemically peculiar star showing an enhanced silicon patch near the equator and a silicon-weak region close to the pole. The star is about 21 million years old with nearly six times the mass of the Sun and three times the Sun's radius. It is radiating roughly 794 times the Sun's luminosity from its photosphere at an effective temperature of 18,400 K.
The secondary companion, component B, is of magnitude 6.62 with a class of B6 V. It has 2.79 times the Sun's mass.