Gliese 758

Gliese 758 is a star in the northern constellation of Lyra. At about magnitude 6 it is a challenge to view with the naked eye even in good seeing conditions, but can be easily seen through a small telescope or binoculars. Parallax measurements from the Hipparcos mission give it an estimated distance of around from Earth.
Properties.
This is a Sun-like star with 97% of the Sun's mass and 88% of the radius of the Sun. The spectrum matches a stellar classification of G8V, identifying it as a G-type main sequence star that is generating energy through the nuclear fusion of hydrogen at its core. It is radiating this energy into space from its outer envelope at an effective temperature of . Estimates of its age put it at about 7.7–8.7 billion years old, although some measurements give it an age as low as 720 million years. The abundance of elements other than hydrogen and helium, what astronomers term the star's metallicity, are 51% higher than in the Sun.
System.
In November 2009, a team using the HiCIAO instrument of the Subaru Telescope imaged a substellar companion orbiting the star. This object, designated Gliese 758 B, was estimated to be of approximately 10-40 Jupiter masses. A second candidate object was also detected, which was given the designation Gliese 758 C. Follow-up studies of the system suggested the mass range of Gliese 758 B, indicating it to be a companion with approximately 30 to 40 Jupiter masses and revealed that Gliese 758 C is a background star which is not physically associated with the Gliese 758 system. On the other hand, a younger age was suggested from the kinematic stellar grouping.
Orbit.
Gliese 758 B is on an eccentric orbit with a semimajor axis of Astronomical units and an orbital period of years, which takes it within 9 astronomical units of its host star at its closest approach.


67 Ophiuchi

67 Ophiuchi (67 Oph) is a class B5 Ib (blue supergiant) star in the constellation Ophiuchus. Its apparent magnitude is 3.93 and it is approximately 1200 light years away based on parallax. It is considered to be a member of the open cluster Collinder 359 (Melotte 186).
67 Oph has four companions. The closest is a magnitude 13.7 B1 main sequence star at 8.29", designated B. Component C (BD+02°3459) is the brightest close companion, a magnitude 8.1 B2 main sequence star at 54.32". Component D is a magnitude 12.5 star 8.37" from component C. Component E is a magnitude 10.9 star 46.53" from 67 Oph A.


Epsilon Lyrae

Epsilon Lyrae (ε Lyr, ε Lyrae), also known as the Double Double, is a multiple star system of at least five stars approximately 162 light-years away in the constellation of Lyra.
Star System.
The widest two components of the system are easily separated when viewed through binoculars, or even with the naked eye under excellent conditions.
The northern component is called ε1 (ADS 11635 AB in multiple star notation) and the southern ε2 (ADS 11635 CD); they lie around 160 light years from Earth and orbit each other over hundreds of thousands of years. Their separation of is about one hundred times that of the subcomponents. When viewed at higher magnifications, each intuitively likely "star" proves to be a set of shorter-term, close-orbiting binary stars. Ability to view these sub-components is a common benchmark for the resolving power of telescopes, since they are so close together: the stars of ε1 were 2.35 arc-seconds apart in 2006, those of ε2 were separated by about the same amount in that year. Since the first high-precision measurements of their orbit in the 1980s, both binaries have moved only a few degrees in position angle.
The component stars of ε1 have magnitudes of 4.7 and 6.2 separated by 2.6" and have an orbital period that can only be crudely estimated at 1200 years, which places them at roughly 140 AU apart. Main components of ε2 have magnitudes 5.1 and 5.5 separated by 2.3", and orbit in perhaps half that period. ε1 and ε2 are more than 0.16 light years apart. An observer at one pair would see the other as strongly as a quarter (also known as half) Moon (which is about mv = −5.0), less than a degree away from each other.
The fifth component of this system, orbiting one of the ε2 pair, was detected by speckle interferometry in 1985 and confirmed in two later observations. No orbit can be prepared from such limited data, but its rapid motion suggests a period of a few tens of years. Its maximum observed separation of 0.2 arc-seconds precludes direct visual observation.
A further five nearby dimmer stars are also listed in multiple star catalogues:


NGC 7320c

NGC 7320c is a galaxy member of the Stephan's Quintet located in the constellation Pegasus.


SU Aurigae

SU Aurigae is a T Tauri-type variable star in the constellation Auriga. It is located about 500 light-years (150 parsecs) away in the Taurus-Auriga Star Forming Region. Its apparent magnitude is 9.30, which is dim enough that it cannot be seen with the unaided eye.
SU Aurigae's spectral type of G2IIIne means that it is a G-type star with an effective temperature similar to the Sun. The III in the spectral type refers to its luminosity, which is much higher than normal G-type main sequence stars and would put it in the giant star class. However, it is only about 4 million years old, which is relatively young for a star - young protostars like SU Aurigae are luminous because they are larger, not condensing into a normal size until they are older.
SU Aurigae is known to have a circumstellar protoplanetary disk surrounding it, which is typical of many T Tauri stars. SU Aurigae's disk has a high inclination of 62° and is nearly perpendicular to the plane of sky, so orbiting protoplanets or comets may be the cause of why there are drops in the amount of light detected. SU Aurigae's proper motion and distance is similar to AB Aurigae, a better known pre-main-sequence star, meaning that the two may form a very wide binary system; if not, they are still in the same star association.


27 Hydrae

27 Hydrae is a member of a triple star system system in the equatorial constellation of Hydra, located 222 light years away from the Sun. It is visible to the naked eye as a faint, orange-hued star with a combined apparent visual magnitude of 4.82. The system is moving further from the Earth with a heliocentric radial velocity of +25.6 km/s.
The magnitude 4.91 primary, component A, is an aging giant star with a stellar classification of K0 III. It is a red clump giant, which indicates it is on the horizontal branch and is generating energy through helium fusion at its core. The star is 1.9 billion years old with 2.17 times the mass of the Sun. It has swelled to 11 times the Sun's radius and is radiating 57.5 times the Sun's luminosity from its enlarged photosphere at an effective temperature of 4,965 K. The star is suspected to host a low-mass companion.
The stellar companions to this star, designated components B and C, lie at an angular separation of from the primary, and form a binary pair with a separation of 9.20″ as of 2015. The brighter member of the pair, component B, is a seventh magnitude F-type main-sequence star with a class of F4 V, while its companion is an eleventh magnitude K-type main-sequence star with a class of K2 V.
Substellar companion.
The Okayama Planet Search team published a paper in late 2008 reporting investigations into radial velocity variations observed for a set of evolved stars, showing hints of a substellar companion orbiting the primary member of the wide binary system 27 Hydrae. Its orbital period is estimated at 9.3 years, but no planet has been confirmed yet.


53 Aurigae

53 Aurigae is a binary star system in the northern constellation of Auriga. It is visible to the naked eye as a dim star with a combined apparent visual magnitude of 5.74. Parallax estimates put it at a distance of away. The system is receding from the Earth with a heliocentric radial velocity of 13 km/s.
The two components of 53 Aurigae orbit each other every 39 years with an eccentricity of 0.557. The primary component, 53 Aurigae A, is chemically peculiar since it contains higher-than-normal amounts of manganese, but also europium, chromium, and mercury. It is a B-type main-sequence star, while the secondary component, 53 Aurigae B, is an early F-type main-sequence star. The total mass of the system is estimated to be .


Kappa Herculis

Kappa Herculis (κ Herculis, abbreviated Kappa Her, κ Her) is an optical double star in the constellation of Hercules. The two components, Kappa Herculis A (Marsic , the traditional name of the system) and B, were 27.3 arc seconds apart in 2000. Based on parallax measurements from the Hipparcos mission, κ Her A is about 113 parsecs (370 light-years) from the Sun and κ Her B is 600 parsecs (2,000 light-years); more recent parallax measurements suggest that B is around 5% more distant than A.
A faint third component Kappa Herculis C is just over 1 arc-minute away. It is at the same distance as κ Her A and has an almost-identical space motion.
The star 8 Herculis forms a naked-eye pair with Kappa Herculis away.
Nomenclature.
κ Herculis (Latinised to "Kappa Herculis") is the system's Bayer designation. The designations of the components as "Kappa Herculis A", "B" and "C" derive from the convention used by the Washington Multiplicity Catalog (WMC) for multiple star systems, and adopted by the International Astronomical Union (IAU).
The system bore the traditional names of "Marsic", "Marfik" or "Marfak", all of which come from the Arabic لمرفق "Al-Mirfaq" meaning "the elbow", a name (or some derivative of which) it shared with Lambda Ophiuchi. The Working Group on Star Names (WGSN) approved the name "Marsic" for the component Kappa Herculis A on February 1, 2017, and "Marfik" for the primary component of Lambda Ophiuchi on September 12, 2016, and they are both now so included in the List of IAU-approved Star Names.
In Chinese, (), meaning "Right Wall of Heavenly Market Enclosure", refers to an asterism which represents eleven old states in China and marks the right borderline of the enclosure, consisting of Kappa Herculis, Beta Herculis, Gamma Herculis, Gamma Serpentis, Beta Serpentis, Delta Serpentis, Alpha Serpentis, Epsilon Serpentis, Delta Ophiuchi, Epsilon Ophiuchi and Zeta Ophiuchi. Consequently, the Chinese name for Kappa Herculis itself is (, ), representing the state of Jin (晉) (or Tsin), together with 36 Capricorni in "Twelve States" (asterism).
Properties.
Kappa Herculis A is a giant star with stellar classification G8III. With a mass of and radius that is , the star boasts a bolometric luminosity that is . Its slightly companion is cooler and about a third of the luminosity.
Kappa Herculis is a suspected variable star with a reported magnitude range of 4.70 to 5.02.


NGC 3367

NGC 3367 is a barred spiral galaxy located in the constellation Leo. It is located at a distance of circa 120 million light years from Earth, which, given its apparent dimensions, means that NGC 3367 is about 85,000 light years across. It was discovered by William Herschel on March 19, 1784.
Characteristics.
NGC 3367 is a barred spiral galaxy with an asymmetric shape seen nearly face-on, with an inclination of 25 degrees. The inner arms begin at the ends of the bar, forming a ring with a major axis of 0.9 arcseconds, and after half of a revolution start to branch, creating a multiple-arm structure. They are studded with many bright HII regions. The star formation rate in NGC 3367 is nearly 3 per year. The outer arms form a semi-circular arch towards the south, at a distance of 50 arcseconds from the centre, more visible in the ultraviolet.
Usually, asymmetry in a galaxy is caused by interaction with other galaxies, but no large satellite has been detected near NGC 3367. The cause of the asymmetry is assumed to be a minor merger or mass accretion that took place in the last billion years. Because no low surface brightness structures, like plumes and star streams, have been detected near NGC 3367, and nor is gas seen in HI imaging near the galaxy, it is believed that the galaxy accreted of cold gas in the past million years. This gas accretion resulted in increased star formation and nuclear activity.
NGC 3367 features a strong bar. The bar pattern speed was estimated to be 43 ± 6 km s−1 kpc−1 using the Tremaine-Weinberg method. The bar of the galaxy is more prominent in the near infrared, suggesting the dominance of an old population of stars in that region. There is also a knot at the eastern end of the bar, where there is a non-negligible population of red giants and asymptotic giant branch stars.
Nucleus.
NGC 3367 has been categorised as a HII region or a type 2 Seyfert galaxy. However, optically there is no hint of an Active Galactic Nucleus (AGN). The spectrum of NGC 3367 features unusually broad lines (FWHM of 490 m/s for Hβ) and a blue asymmetry. The spectrum looks like one produced from Wolf-Rayet stars. There is no clear evidence of H-alpha emission. The spectrum is also dominated by starburst features like low [Fe II] 1.2567 μm/Paβ line ratio. The galaxy was observed by the Spitzer Space Telescope and [Ne v] 14.3 and 24.3 μm lines, consistent with the existence of a weak AGN were detected. Observed by the XMM-Newton telescope, the galaxy's X-ray luminosity in 2-10 keV was 2.0 × 1040 erg s−1 dominated by a power law. This value is consistent with low-luminosity AGNs.
When observed in radio waves, the galaxy features two radio lobes extending from a nuclear source, a feature common to Seyfert 2 galaxies. The emission of the southwest lobe is polarised, indicating it is above the plain of the disk, while the northeast is depolarised. The southwest lobe extends 26" from the nucleus and the northeast 33". The total extent of the source is approximately 12 kpc at the distance of the galaxy. More detailed observations by the Very Large Array revealed a radio jet connecting the nucleus with the southwest lobe and a circumnuclear structure with a radius of nearly 300 pc.
In the centre of the galaxy lies a supermassive black hole whose mass is estimated to be (107.2) based on Ks bulge luminosity. The X-ray spectra of the galaxy suggested the mass of the supermassive black hole to be in the range of 105 to 107 .
Around the nucleus, at a radius of circa 2 arcseconds, has been detected using CO(1-0) emission a significant amount of molecular gas. The total mass of molecular gas in that region is estimated to be and in the central 5 arcseconds the mass of molecular gas is . The presence of a such large mass could obscure the optical emission lines from an active galactic nucleus. The CO emission has an elongated shape, maybe due to the forces created by the stellar bar.
Supernovae.
Five supernovae have been observed in NGC 3367 in the last 30 years; SN 1986A (type Ia, mag 14.0), SN 1992C (type II, mag 16.5), SN 2003aa (type Ic, mag 17.6), SN 2007am (type II, mag 17.8), and SN 2018kp (type Ia). SN 1992c was discovered by ESO astronomer Hans van Winckel on January 28, 1992. He found it on a photographic plate obtained by Guido Pizarro during a search programme carried out with the ESO 1-metre Schmidt telescope at La Silla. Spectra of the supernova, obtained by Della Valle and Christoffel Waelkens (Astronomical Institute of Leuven, Belgium), with the 2.2-metre telescope at La Silla, showed it to be of type II and that the explosion must have happened between 10 and 20 days earlier. The expansion velocity was measured at about 7000 km/sec. SN 1992c was located southeast of the centre of the galaxy, at the tip of a spiral arm. SN 1986A was found on February 4, 1986 near the condensations in the spiral arms east of the centre of the galaxy.
Nearby galaxies.
NGC 3367 is the foremost member in a galaxy group known as the NGC 3367 group. Other members of the group include NGC 3391, and NGC 3419. A bit further away lie the galaxies NGC 3300, and NGC 3306. NGC 3367 lies in the same region of the sky as the Leo Group, whose redshift is about a third of NGC 3367. NGC 3377, a member of the Leo Group, lies 22 arcminutes to the north of NGC 3367.


R Carinae

R Carinae is a double star in the southern constellation of Carina. The brighter component is a variable star that can be viewed with the naked eye at peak brightness, but is usually too faint to be seen without a telescope, having an apparent visual magnitude that fluctuates around 7.43. This star is located at a distance of approximately 1,300 light years from the Sun based on parallax, and is drifting further away with a radial velocity of +28 km/s.
The main component is an aging red giant star on the asymptotic giant branch with a stellar classification of M6/7pe. It is classified as a pulsating Mira type variable star and its visual brightness varies with an average amplitude of 4.25 magnitudes over a period of . Its average maximum visual magnitude is , but the brightest observed maximum was magnitude 3.9 This star is surrounded by a dusty shell, with properties that are consistent with iron-poor silicates or corundum, extending from around three stellar radii outward.
The companion is a magnitude 11.30 star at an angular separation of along a position angle of 132° from the main star, as of 2015.


Xi Puppis

Xi Puppis (ξ Puppis, abbreviated Xi Pup, ξ Pup) is a multiple star system in the southern constellation of Puppis. With an apparent visual magnitude of 3.35, it is one of the brighter members of this constellation. Based on parallax measurements made during the Hipparcos mission, it is located approximately from the Sun, with a 7.5% margin of error.
The system consists of a spectroscopic binary, designated Xi Puppis A, together with a third companion star, Xi Puppis B. A's two components are themselves designated Xi Puppis Aa (formally named Azmidi ) and Ab.
Nomenclature.
"ξ Puppis" (Latinised to "Xi Puppis") is the system's Bayer designation. The designations of the two constituents as "Xi Puppis A" and "B", and those of "A's" components - "Xi Puppis 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).
The system was sometimes known as "Asmidiske" ("Azmidiske"), a misspelling and misplacement of "Aspidiske" (from the Greek for 'little shield), the traditional name of Iota Carinae. 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 "Azmidi" for the component Xi Puppis Aa on 1 June 2018 and it is now so included in the List of IAU-approved Star Names.
Properties.
Because of the distance of this system from the Earth, its visual magnitude is reduced by 0.73 as a result of extinction from the intervening gas and dust.
Xi Puppis A presents as a yellow supergiant of spectral class G6 with a luminosity 8,300 times that of the Sun.
The 13th-magnitude companion, Xi Puppis B, is about 5 arcseconds distant and is a Sun-like star that orbits at least 2000 AU away with an orbital period of at least 26,000 years.


NGC 338

NGC 338 is a spiral galaxy in the constellation Pisces. It was discovered in 1877 by Wilhelm Tempel. It was described by Dreyer as "very faint, very small, irregular figure, brighter middle."


Zeta2 Scorpii

Zeta2 Scorpii (Zeta2 Sco, ζ2 Scorpii, ζ2 Sco) is a K-type orange giant star in the constellation of Scorpius. It has an apparent visual magnitude which varies between 3.59 and 3.65, and is located near the blue-white supergiant star ζ1 Scorpii in Earth's sky. In astronomical terms, ζ2 is much closer to the Sun and unrelated to ζ1 except for line-of sight co-incidence. ζ1 is 5,700 light-years away and probably an outlying member of open star cluster NGC 6231 (also known as the "northern jewel box" cluster), whereas ζ2 is a mere 132 lightyears distant and thus much less luminous in real terms. ζ2 can also be distinguished from its optical partner, ζ1, because of its orangish colour especially in long-exposure astrophographs.


Ghost (Chinese constellation)

The Ghost mansion () is one of the Twenty-eight mansions of the Chinese constellations. It is one of the southern mansions of the Vermilion Bird.


NGC 2439

NGC 2439 is a sparse open cluster of stars in the constellation Puppis. It has an apparent visual magnitude of 6.9, an angular size of 10 arcminutes, and is visible using a small telescope. This is a young cluster with age estimates in the range of 20–300 million years. It has a tidal radius of approximately 82 light years. No chemically peculiar stars have been found.
Distance estimates to this cluster vary widely. Piskunov and associates (2008) gave an estimate of . A value in the range 3–4 kpc means the cluster lies well below the Galactic Plane. It is positioned in a hole in the Milky Way's gas and dust, with the reduced absorption resulting in a lower than expected extinction of 1.27 in visual magnitude. This result raises the question of whether this cluster actually exists. It is positioned along the same line of sight as two groups of B-type supergiant stars. The nearer group is located at a distance of 1.03 kpc, while the second group is at 3.2 kpc.


Eta2 Pictoris

η2 Pictoris, Latinised as Eta2 Pictoris, is a solitary star in the southern constellation of Pictor. It is visible to the naked eye as a dim, orange-hued star with an apparent visual magnitude of 5.02. With an annual parallax shift of as seen from the Earth, it is located around 418 light years from the Sun. It is a member of the HR 1614 moving group of stars that share a common motion through space.
This is an evolved K-type giant star with a stellar classification of K5 III, having exhausted the supply of hydrogen at its core, then cooled and expanded off the main sequence. At present it has 41 times the girth of the Sun. It is radiating an estimated 363.5 times the Sun's luminosity from its photosphere at an effective temperature of 4,136 K. This is a member of the old disk population and is a suspected variable star.


94 Ceti

94 Ceti (HD 19994) is a trinary star system approximately 73 light-years away in the constellation Cetus.
94 Ceti A is a yellow-white dwarf star with about 1.3 times the mass of the Sun while 94 Ceti B and C are red dwarf stars.
An infrared excess has been detected around the primary, most likely indicating the presence of a circumstellar disk at a radius of 95 AU. The temperature of this dust is 40 K.
Stellar system.
This system is a hierarchical triple star system with 94 Ceti A being orbited by 94 Ceti BC, a pair of M dwarfs, in 2000 years. 94 Ceti B and C meanwhile orbit each other in a 1-year orbit.
Planetary system.
On 7 August 2000, a planet was announced by the Geneva Extrasolar Planet Search team as a result of radial velocity measurements taken with the Swiss 1.2-metre Leonhard Euler Telescope at La Silla Observatory in Chile. It is most stable if its inclination is either 65 or 115, ± 3.


20 Persei

20 Persei is a visual binary star in the northern constellation of Perseus, a few degrees from Pi Persei. It is visible to the naked eye as a dim, yellow-white hued point of light with a combined apparent visual magnitude of 5.343. The system is located around away from the Sun, based on its parallax. It is receding from the Earth with a heliocentric radial velocity of +6 km/s.
The orbit of the two stars has been calculated from the secondary changing its position relative to the primary. The two orbit each other every 31.6 years with an angular semimajor axis of 0.22 arcseconds and an eccentricity of 0.7560. The combined spectrum of 20 Persei matches that of an F-type main-sequence star, and the two stars are thought to have equal masses, 1.5 times that of the Sun. A ninth-magnitude star, designated 20 Persei C, may be associated with the pair.


Omicron Ursae Majoris

Omicron Ursae Majoris (ο Ursae Majoris, abbreviated Omicron UMa, ο UMa), formally named Muscida , is a star system in the northern circumpolar constellation of Ursa Major. It has an apparent visual magnitude of +3.35 and is located at a distance of around from the Sun. In 2012, an extrasolar planet, designated Omicron Ursae Majoris Ab was found to be orbiting the primary.
Nomenclature.
"ο Ursae Majoris" (Latinised to "Omicron Ursae Majorise") is the star's Bayer designation.
The traditional name "Muscida" was shared with the optical double star Pi Ursae Majoris. In 2016, the International Astronomical Union organized a Working Group on Star Names (WGSN) to catalog and standardize proper names for stars. The WGSN's first bulletin of July 2016 included a table of the first two batches of names approved by the WGSN; which included "Muscida" for this star.
In Chinese, (), meaning "Inner Steps", refers to an asterism consisting of ο Ursae Majoris, 16 Ursae Majoris, 6 Ursae Majoris, 23 Ursae Majoris, 5 Ursae Majoris and 17 Ursae Majoris. Consequently, the Chinese name for ο Ursae Majoris itself is (, .).
Properties and observations.
The stellar classification of this star, G4 II–III, places it midway between the giant and bright giant stages of its evolution. The interferometry-measured angular diameter of this star is about 2.42 mas, which, at its estimated distance, equates to a physical radius of about 14 times the radius of the Sun. It has about three times the mass of the Sun and radiates 138 times the Sun's luminosity from its outer atmosphere at an effective temperature of 5,282 K, giving it the yellowish hue of a G-type star.
In 1963, East German astronomer Gerhard Jakisch reported this star as a variable with a period of 358 days and an amplitude of 0.08 magnitude. The 1982 edition of the "New Catalogue of Suspected Variable Stars" listed it with a variability from 3.30 to 3.36 in the visual band. However, in 1992 American astronomer Dorrit Hoffleit noted that the two comparison stars used to determine the variability may themselves be variable. Hence the actual variability of this star may be suspect.
Muscida has a magnitude 15.2 common proper motion companion at an angular separation of 7.1 arcseconds. With a probability of 99.4%, this companion is the source for the X-ray emission from the system. Omicron Ursae Majoris is sometimes listed with two more companions, but, based on proper motion data, these appear to be optical companions. No other companions were detected by 2016.
This system is a member of the thin disk population and is following an orbit through the Milky Way galaxy with an eccentricity of 0.12. It comes as close to the Galactic Center as and as distant as . This orbit carries it no more than about 330 ly (100 pc) above the galactic plane. It is considered a runaway star because it has a high peculiar velocity of 35.5 km s−1 relative to the typical motion of stars in its vicinity.
The star has no detectable magnetic fields.
Planetary system.
In 2012, an extrasolar planet designated Omicron Ursae Majoris b and orbiting the primary at 3.9 astronomical units, was found. This gas giant (4.1 times as massive as Jupiter) completes an orbit in 1630 days.
References.
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NGC 6208

NGC 6208 is an open cluster in the southern constellation of Ara. With an age of 1.17 Gigayears, it is one of the oldest known open clusters.


Gliese 588

Gliese 588 is a nearby red dwarf star of spectral type M2.5, located in the constellation Lupus at 19.34 light-years from Earth. It emits a very stable light flux, with no detectable pulsations.
History of observations.
According to "Luyten's (1979)" (catalogue LHS, as well as NLTT), this object was discovered by Innes. In 1903–1927 Innes was the director of the Union Observatory (UO), South Africa.
However, in the "Ci 20" catalogue (see number 934) this star was designated as "CD -40 7021", not "UO". This may indicate that GJ 588 was first catalogued earlier, in the "Cordoba Durchmusterung" by John M. Thome in 1894. Note: the real CD designation of Gliese 588 is "CD-40 9712", not "CD -40 7021": GJ 588 has a RA of 15 hours, but the real CD -40 7021 has a RA of 11 hours.
Planetary system.
On 11 June 2019 two planets were detected by radial velocity around Gliese 588 among other 118 planets around M dwarf stars.


U Coronae Borealis

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


46 Aquilae

46 Aquilae is a star in the constellation of Aquila, located to the north of Tarazed (γ Aquilae). "46 Aquilae" is its Flamsteed designation. It is a dim, blue-white hued star that is a challenge to view with the naked eye, having an apparent visual magnitude of 6.33. This object is located approximately 830 light years from the Sun, based on parallax. It is moving closer to the Earth with a heliocentric radial velocity of −25 km/s.
This body has a stellar classification of B9 III, matching a late B-type giant star. It is a chemically peculiar star of a weak Mercury-Manganese type (CP3), and is the most chromium–deficient star known. The star may possess a magnetic field with a strength greater than . It is radiating 180 times the luminosity of the Sun from its photosphere at an effective temperature of 12,900 K.


Epsilon Microscopii

Epsilon Microscopii, Latinized from ε Microscopii, is a single, white-hued star in the southern constellationof Microscopium. It is faintly visible to the naked eye with an apparent visual magnitude of 4.71. The annual parallax shift of the star is 19.7054 mas as measured from Earth, which yields a distance estimate of around 166 light years. It is moving further from the Sun with a radial velocity of +7 km/s.
This star has a stellar classification of A1 V, indicating it is an A-type main-sequence star that is generating energy through hydrogen fusion at its core. The spectrum displays an overabundance of silicon in the atmosphere, but the abundance of iron is the same as in the Sun. The star has 2.2 times the mass of the Sun and 2.2 times the Sun's radius. It is around a half billion years old and is spinning rapidly with a projected rotational velocity of 127 km/s. Epsilon Microscopii is radiating about 36 times the Sun's luminosity from its photosphere at an effective temperature of 9,126 K.
Epsilon Microscopii was a latter designation of 4 Piscis Austrini.
This star was the brightest star in Globus Aerostaticus, the obsolete constellation.


Z Canis Majoris

Z Canis Majoris (Z CMa) is a B-type star in the constellation of Canis Major. It has an average apparent visual magnitude of approximately 9.85, though has brightened by 1-2 magnitudes in irregular outbursts in 1987, 2000, 2004 and 2008.
The star is a complex binary system only 300,000 years old with two main components separated by an estimated 100 astronomical units (AU) or 0.1" as seen from Earth. The southeast component is an FU Orionis star (a type of pre-main-sequence star in a phase of very high mass accretion resulting in an accretion disk which dominates the optical spectrum) that is 1300 times as luminous as the Sun, has 3 times its mass and 13 times its diameter and a surface temperature of 10,000 K. The northwest component is a Herbig Ae/Be star that has been calculated to be 12 times as massive as the Sun with 1690 times its diameter, and shining with 2400 times its luminosity, though there is some uncertainty about its properties. It is enveloped in an irregular roughly spherical cocoon of dust that has an inner diameter of 20 and outer diameter of 50 AU. The cocoon has a hole in it through which light shines that covers an angle of 5 to 10 degrees of its circumference. Both stars are surrounded by a large envelope of in-falling material that left over from the original cloud that formed the system. Both stars are emitting jets of material, that of the Herbig Ae/Be star being much larger - up to 11.7 light-years (3.6 parsecs) long.
It is unclear whether the most recent (and brightest) brightening in 2008 was due to the Herbig Ae/Be star increasing in luminosity or a hole appearing in the cocoon.


TY Pyxidis

TY Pyxidis is an eclipsing binary star in the constellation Pyxis. The apparent magnitude ranges from 6.85 to 7.5 over 3.2 days.
The two components are both of spectral type G5IV, have a mass of 1.2 solar masses and revolve around each other every 3.2 days. Each star is around 2.2 times the diameter of the Sun.
The system is classified as either a RS Canum Venaticorum variable or a BY Draconis variable, stars that vary on account of prominent starspot activity, and lies 184 ± 5 light years away. The system emits X-rays, and analysing the emission curve over time led Pres and colleagues to conclude that there was a loop of material arcing between the two stars.


NGC 3008

NGC 3008 is a lenticular galaxy with an active galactic nucleus in the constellation of Ursa Major, discovered by William Parsons and his assistants. It is about 40 thousand light years across, and with a recessional velocity of about 4,785 kilometers per second, is at a distance of 240 million light-years from the Sun.
It is a member of the NGC 2998 group, which also includes NGC 2998, NGC 3002, NGC 3005, NGC 3006, and a few others. Among these galaxies, it has the lowest star formation rate, at per year.


NGC 5559

NGC 5559 is a barred spiral galaxy, located 240 million light-years away in the constellation of Boötes. It was discovered on April 10, 1785 by the astronomer William Herschel.
In 2001, a type Ib supernova was detected within NGC 5559, and was subsequently designated SN 2001co. The supernova was a calcium-rich supernova, as it had strong spectral lines characteristic of calcium. The progenitors of these calcium-rich supernovae are still a mystery.


Gliese 526

GJ 526 (Lalande 25372, Wolf 498) is a red dwarf star in the northern constellation of Boötes. It has an apparent visual magnitude of 8.5, which is too faint to be seen with the naked eye. Based upon an annual parallax shift of 0.184 arc seconds as measured by the Hipparcos satellite, this system is from Earth.
History of observations.
This star is known at least from 1801, when it was included to Lalande's stellar catalogue "Histoire Céleste Française". In 1847 edition of Lalande's catalogue by Francis Baily it was assigned number 25372, since it sometimes designated as "Lalande 25372" or "LAL 25372".
High proper motion of this star and its large parallax were known at least from 1911, when Frank Schlesinger published a paper where he announced its parallax and mentioned its proper motion value of 2.3 arcsec. In 1919, German astronomer Max Wolf included GJ 526 in his catalogue of high proper motion stars, giving it the identifier 498.
Properties.
GJ 526 is a flare star, which means it undergoes sporadic increases in brightness of up to 1–6 magnitudes. It is a main sequence red dwarf with a stellar classification of M1.5 V. GJ 526 is smaller than the Sun, with 28% of the mass and 58.2% of the radius. It shines with just 1.1% of the luminosity of the Sun, with its stellar atmosphere radiating at an effective temperature of 3,474 K.
GJ 526 has been examined for an excess of radiation in the infrared. The presence of an infrared excess can be taken as an indication of a debris disk orbiting the star. However, no such excess was discovered around GJ 526.


Eta Herculis

Eta Herculis (η Her, η Herculis) is a fourth-magnitude star in the constellation Hercules.
Properties.
Eta Herculis is a G-Type star. With a stellar classification G7.5IIIb, it is yet considerably larger having a mass that is 2.3 times solar and a radius 9.8 times. Though it only shines with an apparent magnitude of 3.48, it is part of the "Keystone" asterism, visible overhead in the mid-summer night sky to northern observers, allowing it to be easily recognized. Eta Herculis is 50 times more luminous than the Sun. The Hipparcos satellite mission estimated its distance at roughly 34.4 parsecs from Earth, or 112 light years away.
If one follows the line connecting Eta Herculis with Zeta Herculis one comes across one of the earliest and most stunning globular clusters in the nighttime sky, M13, discovered in 1714 by Edmond Halley.
Eta Herculis is a double star once thought to be part of a binary star system.


Rho2 Cephei

Rho2 Cephei, Latinized from ρ2 Cephei, or simply ρ Cephei, is a solitary star in the northern constellation of Cepheus. With an apparent visual magnitude of 5.50, it is faintly visible to the naked eye, forming an optical pair with Rho1 Cephei. Based upon an annual parallax shift of 13.31 mas as seen from the Earth, it is located about 245 light years from the Sun.
Rho2 Cephei is an A-type main sequence star with a stellar classification of A3 V, estimated to be 85 million years old. It has a high rate of rotation, showing a projected rotational velocity of 133 km/s. The effective temperature of its photosphere is and its bolometric luminosity, the total amount of radiation it emits at all wavelengths, is .


Rho2 Cancri

Rho2 Cancri (ρ2 Cancri) is a solitary, yellow-hued star in the constellation Cancer. With an apparent visual magnitude of 5.22, it is visible to the naked eye on a dark night. Based upon an annual parallax shift of 6.70 mas as seen from Earth, this star is located around 490 light years from the Sun. At that distance, the visual magnitude is diminished by an extinction factor of 0.06 due to interstellar dust.
At the age of about 234 million years, is an evolved, G-type giant star with a stellar classification of G8 III. It has an estimated 3.6 times the mass of the Sun and has expanded to 24 times the Sun's radius. It is radiating 310 times the Sun's luminosity from its photosphere at an effective temperature of 4,994 K.


HR 2096

HR 2096, also known as HD 40325 is a double star in the constellation Auriga. It is composed of two ageing orange giants of spectral types K0III and K2III. It is not a member of any known moving group of stars.


Chariot (Chinese constellation)

The Chariot mansion () is one of the Twenty-eight mansions of the Chinese constellations. It is one of the southern mansions of the Vermilion Bird.


NGC 4424

NGC 4424 is an unbarred spiral galaxy located 30 million light years is the constellation of Virgo.


Z Carinae

Z Carinae and z Carinae are designations referring to stars in the constellation Carina.
The Bayer designation z Carinae (z Car) is shared by two stars in the constellation Carina:
They are separated by 0.53° on the sky.
The variable star designation Z Carinae is used by the star HD 88946, a 10.20m Mira variable.


HD 330075 b

HD 330075 b is an extrasolar planet approximately 164 light-years away in the constellation of Norma. This planet orbits the star HD 330075. It was discovered by the Geneva Extrasolar Planet Search team at ESO's La Silla Observatory using the HARPS spectrograph.
The planet has a mass about three quarters that of Jupiter. Its orbital distance from the star is less than 1/23rd Earth's distance from the Sun, which makes HD 330075 b an example of a hot Jupiter. One orbit around the star takes a little more than 3 Earth days to complete, as compared to one year for the Earth around the Sun.


SX Corvi

SX Corvi is an eclipsing binary star system in the constellation Corvus, ranging from apparent magnitude 8.99 to 9.25 over 7.5 hours. The system is a contact binary also known as a W Ursae Majoris variable, where the two component stars orbit closely enough to each other for mass to have been transferred between them—in this case the secondary having transferred a large amount of mass to the primary.
Yildiz and colleagues estimated the age of the system at 7.32 ± 0.97 billion years based on study of the properties of the system and estimated rate of mass transfer. They found the current masses of the primary and secondary to be 1.25 ± 0.04 and 0.10 ± 0.01 solar masses respectively, from their original masses of 0.72 ± 0.02 and 1.68 ± 0.05 solar masses.


HD 208527

HD 208527 is a star located in the northern constellation of Pegasus. It has a reddish hue and is dimly visible to the naked eye with an apparent visual magnitude of +6.39. The star is located at a distance of approximately 1,300 light years from the Sun based on parallax, and is drifting further away with a radial velocity of +4.8 km/s.
This was once catalogued as a K-type main-sequence star with a stellar classification of K5V, but is now known as an aging red giant with a class of M1III, based on its dimensions and low surface gravity. This indicates that the two-billion year old star has exhausted the supply of hydrogen at its core then cooled and expanded off the main sequence. It has an estimated 1.6 times the mass of the Sun but has swollen to 51 times the Sun's radius.
Planetary system.
From September 2008 to June 2012, the team B.-C. Lee, I. Han and M.-G. Park observed HD 208527 with "the high-resolution spectroscopy of the fiber-fed Bohyunsan Observatory Echelle Spectrograph (BOES) at Bohyunsan Optical Astronomy Observatory (BOAO)".
In 2012, a long-period, wide-orbiting planet was deduced by radial velocity. This was published in November, gaining the designation HD 208527 b. Along with HD 220074 b this is one of the first two planets proposed around a red giant.


Mu Leporis

Mu Leporis, Latinized from μ Leporis, is a star in the southern constellation of Lepus. The apparent visual magnitude is 3.259, making the star visible to the naked eye at night from the southern hemisphere. Parallax measurements yield an estimated distance of from the Earth. It is moving further from the Sun with a radial velocity of +27.7 km/s.
The stellar classification of this star is B9 IV:HgMn, although the ':' indicates an uncertain spectral value. The luminosity class of IV indicates that this is a subgiant that has exhausted the hydrogen at its core and it is in the process of evolving into a giant star. At present it has about 3.4 times the Sun's radius, 3.45 times the mass of the Sun, and is radiating 251 times the Sun's luminosity from its photosphere at an effective temperature of 12,800 K.
Mu Leporis is a suspected Alpha² Canum Venaticorum variable with a period of about two days, although this has not been confirmed. The stellar spectrum of this star shows overabundances of mercury and manganese, as indicated by the HgMn in the stellar class. X-ray emission has been detected coming from a location at an angular separation of 0.93 arcseconds from this star. At the estimated distance of Mu Leporis, this equals a projected distance of 52 Astronomical Units. The source may be a stellar companion: either a star that has not yet reached the main sequence or a small, low-temperature star. The X-ray luminosity of this object is .


RY Sagittarii

RY Sagittarii is a yellow supergiant and an R Coronae Borealis type variable star in the constellation Sagittarius. Although it ostensibly has the spectrum of a G-type star, it differs markedly from most in that it has almost no hydrogen and much carbon.
Discovery.
Colonel Ernest Elliott Markwick first came across what became known as RY Sagittarii during searches for variable stars while posted in Gibraltar. He recorded it dimming from magnitude 7 in July 1893 to fainter than 11 by 23 October that year, and brightening to magnitude 6.4 by November 1894. Edward Charles Pickering wrote that it was a "remarkable object", and "nearly got away". The spectrum was first noted to be peculiar at the time, and by 1953 it was classified as a R Coronae Borealis variable, along with a handful of other stars.
Mystified by its origins, Danziger postulated possible explanations as forming from a helium cloud, an aged star that had exhausted its hydrogen, or a star that had somehow thrown off its hydrogen envelope, though noted there was no evidence of such an envelope. He conceded that knowledge of star evolution was not advanced enough to come up with an explanation.
Variability.
It is one of the three brightest R Coronae Borealis stars visible to Earth observers, along with R Coronae Borealis and V854 Centauri, and the brightest in the southern hemisphere. It is also a pulsating variable, with a semiregular period of 38 days. Its light curve has been studied for over a hundred years and is typical for the class, characterised by a sudden drop in brightness of several magnitudes over a few weeks before gradually brightening over the following several months. The timing between these dimmings is irregular. The cause of the drop in magnitude is the presence of dust clouds of carbon obscuring (and most likely ejected from) the star, though the mechanism how this might occur is not known. Extensive clouds have been detected with ESO's Very Large Telescope Interferometer.
Properties.
The star is so remote that its parallax, distance and hence luminosity were impossible to calculate with any accuracy. The Hipparcos satellite calculated its parallax at 1.29 milliarcseconds, yielding a distance of from Earth. Its parallax from the Gaia EDR3 is much smaller at , indicating a much larger distance consistent with non-parallax estimates of the distance. The distance derived indirectly by comparison with similar stars, is around 2,000 parsecs. Its effective temperature has been calculated at 7,250 K and its size at based on an assumed luminosity of .


NGC 6357

NGC 6357 is a diffuse nebula near NGC 6334 in the constellation Scorpius. The nebula contains many proto-stars shielded by dark discs of gas, and young stars wrapped in expanding "cocoons" or expanding gases surrounding these small stars. It is also known as the Lobster Nebula and the Madokami Nebula by some fans of the Japanese anime "Madoka Magica" due to its resemblance to the main character from the anime, and a popular fan petition to rename it.
This nebula was also given the name War and Peace Nebula by the Midcourse Space Experiment scientists because of its appearance, which, in infrared images the bright, western part resembles a dove, while the eastern part looks like a skull.
It is located about ~5,500 light years away from Earth.
Associated open clusters.
Pismis 24.
This nebula includes the open cluster Pismis 24, which is home to several massive stars. One of the brightest stars in the cluster, Pismis 24-1, was thought possibly to be the most massive on record, approaching 300 solar masses, until it was discovered to be a multiple system of at least three stars; component stars would still remain near 100 solar masses each, making them among the more massive stars on record.
G353.2+0.7.
The young stellar cluster G353.2+0.7 lies east of Pismis 24 and was revealed by a Chandra X-ray image showing approximately 800 stars.
G353.1+0.6.
The young stellar cluster G353.1+0.6 lies southeast of Pismis 24 and also contains approximately 800 stars detected by X-ray. The region includes several O-type stars, including [BDSB2003] 10.
Massive stars.
NGC 6357 is one of the most prominent sites of massive-star formation in our neighborhood of the Milky Way. A variety of early O-type stars reside in this nebula, blowing the bubbles around the star clusters that can be seen in the molecular cloud.


Encampment (Chinese constellation)

The Encampment mansion () is one of the Twenty-eight mansions of the Chinese constellations. It is one of the northern mansions of the Black Tortoise.


NGC 3359

NGC 3359 is a barred spiral galaxy located 59 million light-years from Earth, in the constellation of Ursa Major. It was discovered on November 28, 1793 by the astronomer William Herschel. The central bar is approximately 500 million years old.
NGC 3559 is "devouring" the much smaller galaxy, nicknamed the Little Cub.


Iota Pictoris

ι Pictoris, Latinized from Iota Pictoris, is a suspected multiple star system in the southern Pictor constellation. It is visible to the naked eye as a dim, yellow-white hued point of light with a combined apparent visual magnitude of 5.28. The two resolvable components have an angular separation of , equivalent to a physical projected separation of around . They are located at a distance of around 127–131 light years from the Sun, based on parallax.
The two visible components appear as F-type main-sequence stars: the magnitude 5.63 component A has a stellar classification of F0 V, while the cooler, fainter secondary is of class F4 V. Both are themselves are suspected spectroscopic binary stars consisting of roughly equal components. Component B actually has a higher estimated mass than Component A, although the radius of B is smaller. They are both more luminous than the Sun, and have an estimated age of around 500–600 million years.


Psi Orionis

The Bayer designation Psi Orionis (ψ Ori / ψ Orionis) is shared by two stars in the constellation Orion:


V382 Carinae

V382 Carinae, also known as x Carinae (x Car), is a yellow hypergiant in the constellation Carina. It is a G-type star with a mean apparent magnitude of +3.93, and a variable star of low amplitude.
Variability.
The radial velocity of V382 Carinae has long been known to be variable, but variations in its brightness were unclear. Brightness variations were detected by some observers, but others found it to be constant. It was formally named as a variable star in 1981, listed in the General Catalogue of Variable Stars as a possible δ Cephei variable. It has been described as a "pseudo-Cepheid", a supergiant with pulsations similar to a Cepheid but less regular.
Analysis of Hipparcos photometry showed clear variation with a maximum range of 0.12 magnitudes and the star was treated as an α Cygni variable. A period of 556 days was suggested, but it is not entirely consistent. It is now generally treated as a semiregular or irregular supergiant.
Properties.
V382 Car is the brightest yellow hypergiant in the night sky, easily visible to the naked eye and brighter than Rho Cassiopeiae although not visible from much of the northern hemisphere. It is 6,200 light years from Earth and around 500 times the radius of the Sun. The large size means that V382 Car is over 200,000 times as luminous as the sun. The low infrared excess suggest that V382 Carinae may be cooling towards a red supergiant phase, less common than yellow hypergiants evolving towards hotter temperatures.


Former constellation

Former constellations are old historical western constellations that for various reasons are no longer widely recognised or are not officially recognised by the International Astronomical Union (IAU). Prior to 1930, many of these defunct constellations were traditional in one or more countries or cultures. Some only lasted decades but others were referred to over many centuries. All are now recognised only for having classical or historical value. Many former constellations had complex Latinised names after objects, people, or mythological or zoological creatures. Others with unwieldy names were shortened for convenience. For example, Scutum Sobiescianum was reduced to Scutum, Mons Mensae to Mensa, and Apparatus Sculptoris to Sculptor.
Some of the northern sky's former constellations were placed in the less populated regions between the traditional brighter constellations just to fill gaps. In the southern skies, new constellations were often created from about the 15th century by voyagers who began journeying south of the equator. European countries like England, France, the Netherlands, German or Italian states, etc., often supported and popularised their own constellation outlines. In some cases, different constellations occupied overlapping areas and included the same stars. These former constellations are often found in older books, star charts or star catalogues.
The eighty-eight modern constellation names and boundaries were standardised by Eugene Delporte for the IAU in 1930, under an international agreement, removing any possible astronomical ambiguities between astronomers from different countries. Nearly all former or defunct constellations differ in their designated boundaries inasmuch as they have outlines that do not follow the exact lines of right ascension and declination.
Noteworthy former constellations.
Argo Navis.
Argo Navis is the only constellation from Ptolemy's original list of 48 constellations that is no longer officially recognized. Due to its large size, it was split into three constellations by Nicolas Louis de Lacaille: Carina (the keel), Puppis (the poop deck), and Vela (the sails). The new constellations were introduced in the 1763 star catalog "Coelum Australe Stelliferum", which was published soon after de Lacaille's death.
Quadrans Muralis.
Quadrans Muralis was originally created in 1795, placed in the northern skies between the still-accepted constellations Boötes and Draco. The Quadrantids meteor shower is named after this former constellation.


NGC 7074

NGC 7074 is an edge-on lenticular galaxy located about 140 million light-years away in the constellation of Pegasus. NGC 7074 was discovered by astronomer Albert Marth on October 16, 1863.


OGLE-TR-56

OGLE-TR-56 is a dim, distant, magnitude 17 Sun-like star located approximately 1500 parsecs away in the constellation of Sagittarius.
This star is listed as an eclipsing type variable star with the eclipse due to the passage of the planet as noted in the discovery papers.
Planetary system.
In 2002, a possible planet was discovered transiting the star, and after additional observations to rule out false positives, it was confirmed. At the time of discovery it was the shortest period planet.


UX Lyncis

UX Lyncis is a variable star in the faint northern constellation of Lynx, positioned about 3° to the south of the 4th magnitude star 10 Ursae Majoris. This is a red-hued star near the lower threshold of visibility to the naked eye, having an apparent visual magnitude that fluctuates around 6.70. It is located at a distance of approximately 900 light years from the Sun based on parallax, and is drifting further away with a radial velocity of +39 km/s.
The stellar classification of this star is M3III, while the infrared spectrum matches a class of M6III. It is an aging red giant on the asymptotic giant branch that has exhausted the supply of both hydrogen and helium in its core, then cooled and expanded. At present it has 128 times the radius of the Sun, which is equivalent to or 60% of the distance from the Sun to the Earth. On average, it radiates a luminosity approximately 1,766 times that of the Sun from its swollen photosphere at an effective temperature of 3,302 K. Infrared observations show little or no evidence for an oxygen-rich dusty shell around the star.
The variability of this star was reported by R. L. Walker in 1970 from the U.S. Naval Observatory. UX Lyncis has been classified as a semiregular variable ranging from magnitude 6.6 down to 6.78. Its changes in brightness are complex, with a shorter period of 37.3 days due to the star's pulsations, and a longer period of 420 days possibly due to the star's rotation or convectively induced oscillatory thermal (COT) mode. There is some evidence for an additional weak variability with a 29 day period.


Bharani

Bharani (Devanagari: भरणी) is the second nakshatra in Hindu astronomy, corresponding to 35, 39, and 41 Arietis all together. In Jyotiṣa, Bharani is ruled by Shukra (the planet Venus).
Also, it is classified as a Cruel or Active nakshatra, meaning that, under electional astrological beliefs, works of a harmful or deceptive nature are best conducted while the moon is Bharani.
Bharani is seen as being under the domain of Yama, the god of death or Kālī.
Traditional Hindu given names are determined by which pada (quarter) of a nakshatra the Ascendant/Lagna was in at the time of birth. The given name would begin with the following syllables:


W Carinae

The designations W Carinae and w Carinae are distinct and refer to two different stars:


Gliese 436

Gliese 436 is a red dwarf approximately away in the zodiac constellation of Leo. It has an apparent visual magnitude of 10.67, which is much too faint to be seen with the naked eye. However, it can be viewed with even a modest telescope of aperture. In 2004, the existence of an extrasolar planet, Gliese 436b, was verified as orbiting the star. This planet was later discovered to transit its host star.
Properties.
Gliese 436 is a M2.5V star, which means it is a red dwarf. Stellar models give an estimated size of about 42% of the Sun's radius. The same model predicts that the outer atmosphere has an effective temperature of 3,318 K, giving it the orange-red hue of an M-type star. Small stars such as this generate energy at a low rate, giving it only 2.5% of the Sun's luminosity.
Gliese 436 is older than the Sun by several billion years and it has an abundance of heavy elements (with masses greater than helium-4) equal to 48% that of the Sun. The projected rotation velocity is 1.0 km/s, and the chromosphere has a low level of magnetic activity. Gliese 436 is a member of the "old-disk population" with velocity components in the galactic coordinate system of "U"=+44, "V"=−20 and "W"=+20 km/s.
Planetary system.
The star is orbited by one known planet, designated Gliese 436 b. The planet has an orbital period of 2.6 Earth days and transits the star as viewed from Earth. It has a mass of 22.2 Earth masses and is roughly 55,000 km in diameter, giving it a mass and radius similar to the ice giant planets Uranus and Neptune in the Solar System. In general, Doppler spectroscopy measurements do not measure the true mass of the planet, but instead measure the product m sin i, where m is the true mass and i is the inclination of the orbit (the angle between the line-of-sight and the normal to the planet's orbital plane), a quantity that is generally unknown. However, for Gliese 436 b, the transits enable the determination of the inclination, as they show that the planet's orbital plane is very nearly in the line of sight (i.e. that the inclination is close to 90 degrees). Hence the mass quoted is the actual mass. The planet is thought to be largely composed of hot ices with an outer envelope of hydrogen and helium, and is termed a "hot Neptune".
GJ 436 b's orbit is likely misaligned with its star's rotation. In addition the planet's orbit is eccentric. Because tidal forces would tend to circularise the orbit of the planet on short timescales, this suggested that Gliese 436 b is being perturbed by an additional planet orbiting the star.
Possible second planet.
In 2008, a second planet, designated "Gliese 436 c" was claimed to have been discovered, with an orbital period of 5.2 days and an orbital semimajor axis of 0.045 AU. The planet was thought to have a mass of roughly 5 Earth masses and have a radius about 1.5 times larger than the Earth's. Due to its size, the planet was thought to be a rocky, terrestrial planet. It was announced by Spanish scientists in April 2008 by analyzing its influence on the orbit of Gliese 436 b. Further analysis showed that the transit length of the inner planet is not changing, a situation which rules out most possible configurations for this system. Also, if it did orbit at these parameters, the system would be the only "unstable" orbit on UA's Extrasolar Planet Interactions chart. The existence of this "Gliese 436 c" was thus regarded as unlikely, and the discovery was eventually retracted at the Transiting Planets conference in Boston, 2008.
Despite the retraction, studies concluded that the possibility that there is an additional planet orbiting Gliese 436 remained plausible. With the aid of an unnoticed transit automatically recorded at NMSU on January 11, 2005, and observations by amateur astronomers, it has been suggested that there is a trend of increasing inclination of the orbit of Gliese 436 b, though this trend remains unconfirmed. This trend is compatible with a perturbation by a planet of less than 12 Earth masses on an orbit within about 0.08 AU of the star.
Two sub-Earth candidates.
In July 2012, NASA announced that astronomers at the University of Central Florida, using the Spitzer Space Telescope, strongly believed they had observed a second planet. This candidate planet was given the preliminary designation UCF-1.01, after the University of Central Florida. It was measured to have a radius of around two thirds that of Earth and, assuming an Earth-like density of 5.5 g/cm3, was estimated to have a mass of 0.3 times that of Earth and a surface gravity of around two thirds that of Earth. It orbits at 0.0185 AU from the star, every 1.3659 days. The astronomers also believe they have found some evidence for an additional planet candidate, UCF-1.02, which is of a similar size, though with only one detected transit its orbital period is unknown. Follow up observations with the Hubble Space Telescope as well as a reanalysis of the Spitzer Space Telescope data were unable to confirm these planets.


Upsilon Centauri

The Bayer designation Upsilon Centauri (υ Cen / υ Centauri) is shared by two star systems, in the constellation Centaurus:
They are separated by 0.96° on the sky.
All of them were member of asterism 柱 (Zhǔ), "Pillars", "Horn" mansion.


Delta Herculis

Delta Herculis (δ Herculis, abbreviated Delta Her, δ Her) is a multiple star system in the constellation of Hercules. Its light produces to us apparent magnitude 3.12, as such the third-brightest star in the large, fairly dim constellation. Based on parallax measurement taken during the Hipparcos mission, it is approximately from the Sun.
Components.
It consists of a binary pair, designated Delta Herculis A, together with three potential companions, suffixed B, C and D. Furthermore B is believed to be an optical binary. A's components are designated Delta Herculis Aa (officially named Sarin , the traditional name of the system) and Ab.
Nomenclature.
"δ Herculis" (Latinised to "Delta Herculis") is the system's Bayer designation. The designations of the four constituents as "Delta Herculis A", "B", "C" and "D", and those of "A's" components - "Delta Herculis 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 "Sarin". 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 "Sarin" for the component Delta Herculis Aa on 12 September 2016 and it is now so included in the List of IAU-approved Star Names.
In the catalogue of stars in the "Calendarium" of Al Achsasi al Mouakket, this star was designated "Menkib al Jathi al Aisr", which was translated into Latin as "Humerus Sinister Ingeniculi", meaning "kneeler's left shoulder".
In Chinese, (), meaning "Left Wall of Heavenly Market Enclosure", refers to an asterism which represents eleven old states in China which is marking the left borderline of the enclosure, consisting of Delta Herculis, Lambda Herculis, Mu Herculis, Omicron Herculis, 112 Herculis, Zeta Aquilae, Theta1 Serpentis, Eta Serpentis, Nu Ophiuchi, Xi Serpentis and Eta Ophiuchi. Consequently, the Chinese name for Delta Herculis itself is (, ), and represents the state of Wei (魏), together with 33 Capricorni, according to Ian Ridpath version or Phi Capricorni and Chi Capricorni in R.H. Allen's version in "Twelve States" (asterism).
Properties.
Delta Herculis A presents as an A-type main-sequence subgiant with a stellar classification of A3IV. It has both a mass and radius that are roughly two times solar yielding a total luminosity of about


List of stars in Aquarius

This is the list of notable stars in the constellation Aquarius, sorted by decreasing brightness.


HD 39225

HD 39225, also known as HR 2028, is a variable star in the northern constellation Auriga, located around 620 light years away from the Sun. It is visible to the naked eye as a faint, red-hued star with an apparent visual magnitude of around 6.04. This is a suspected runaway star that is moving away from the Sun with a heliocentric radial velocity of 98 km/s.
Currently on the asymptotic giant branch, this is an evolved red giant star with a stellar classification of . The suffix notation indicates an underabundance of iron in the stellar atmosphere compared to similar stars of its class. It is suspected of varying in brightness between magnitudes 5.82 and 6.07. Having exhausted the hydrogen at its core, it has expanded to around 43 times the Sun's radius. It shines with a luminosity approximately 398.6 times that of the Sun and has a surface temperature of 3,934 K.


AR Aurigae

AR Aurigae (AR Aur), also known by its Flamsteed designation 17 Aurigae, is a binary star in the constellation Auriga. Based on parallax measurements made by the Hipparcos spacecraft, it is approximately 400 light-years from Earth.
Both components are blue-white B-type main-sequence stars that do not fill their Roche lobes. The system has a mean apparent magnitude of +6.15. However, the orbit of the stars are oriented in such a way that they periodically eclipse each other, so AR Aurigae is a variable star and its brightness varies from magnitude +6.15 to +6.82 with a period of 4.13 days.
The primary component of AR Aurigae is known to be a mercury-manganese star, also known as an HgMn star. As the name implies, these stars have over-abundances of the elements mercury and manganese, and also often xenon and other elements. Because AR Aurigae is an eclipsing binary (in fact, it is the only known eclipsing binary with a mercury-manganese star), accurate characterization of its parameters has been made possible. Based on the light-time effect observed from the stars, it is inferred that there is a third star with a mass of , orbiting at a separation of 13 au every 23.7 years.


37 Tauri

37 Tauri is a single, orange-hued star in the zodiac constellation of Taurus. It can be seen with the naked eye, having an apparent visual magnitude of 4.36. A magnitude 10.01 visual companion has an angular separation of on a position angle of 138.6°, as of 2003. Based on an annual parallax shift of , 37 Tauri is about 187 light years away. It is moving further from the Sun with a heliocentric radial velocity of 9.5 km/s.
This is an evolved K-type giant star with a stellar classification of K0 III-IIIb. At the age of 1.39 billion years, it has become a red clump giant, indicating that it is generating energy through helium fusion at its core. The star has around double the mass of the Sun and has expanded to 10 times the Sun's radius. It is radiating roughly 60 times the Sun's luminosity from its enlarged photosphere at an effective temperature of 4,732 K.
Chinese astronomy.
In Chinese astronomy, 37 Tauri is called 月, Pinyin: Yuè, meaning "Moon", because this star is marking itself and stand alone in "Moon" asterism, Hairy Head mansion (see : Chinese constellation).


NGC 236

NGC 236 is a spiral galaxy located in the constellation Pisces. It was discovered on August 3, 1864 by Albert Marth.


HAT-P-5

HAT-P-5 is a 12th magnitude star in the constellation Lyra, approximately 1,000 light years away from Earth. It is a spectral type G star, about 1.16 solar masses and radii greater than our Sun, and only 200 kelvins hotter. It is estimated to be 2.6 billion years old.
The star HAT-P-5 is named Chasoň. The name was selected in the NameExoWorlds campaign by Slovakia, during the 100th anniversary of the IAU. Chasoň is an ancient Slovak term for Sun.
Planetary system.
On October 9, 2007, a report was submitted to "The Astrophysical Journal Letters" telling of the discovery of an exoplanet transiting HAT-P-5. The planet was described as a Jupiter-like hot Jupiter, with a radius about one and one quarter times that of Jupiter, and nearly the same mass. Its density was reported as 0.66 ± 0.11 g/cm3, and its inclination 86.75 ± 0.44°.


HD 88522

HD 88522 is a double or multiple star. The component stars are two white stars of similar spectral type—A1V and A2V—and luminosity.


Lambda Ophiuchi

λ Ophiuchi, Latinized as Lambda Ophiuchi, is a triple star system in the equatorial constellation of Ophiuchus. It has the traditional name Marfik , which now applies exclusively to the primary component. The system is visible to the naked eye as a faint point of light with an apparent visual magnitude of 3.82. It is located approximately 173 light-years from the Sun, based on its parallax, but is drifting closer with a radial velocity of –16 km/s.
System.
The inner pair form a binary star system with an orbital period of 192 years and an eccentricity of 0.611. Both components are A-type main-sequence stars, indicating that they are generating energy through core hydrogen fusion. The brighter member of this pair, designated component A, is the primary for the system with a visual magnitude of 4.18 and a stellar classification of A0V. The secondary, component B, is magnitude 5.22 and class A4V.
Component C is magnitude 11.0 and lies at an angular separation of from the inner pair. It has a common proper motion and is at approximately the same distance as the other two stars, although any orbit would last for hundreds of thousands of years. It has a mass 72% of the Sun's, a radius 58% of the Sun's, a temperature of about , and 7% of the Sun's luminosity. It has an estimated spectral type of K6.
Nomenclature.
"λ Ophiuchi" is the system's Bayer designation. The designations of the three components as "Lambda Ophiuchi A", "B" and "C" 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 "Marfik" (or "Marsik"), from the Arabic مرفق "marfiq" "elbow". 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 "Marfik" for the component Lambda Ophiuchi A on 12 September 2016 and it is now so included in the List of IAU-approved Star Names.


NGC 6027a

NGC 6027a is a spiral galaxy that is part of Seyfert's Sextet, a compact group of galaxies, which is located in the constellation Serpens. In optical wavelengths, it has a strong resemblance to Messier 104, the Sombrero Galaxy, with which it shares a near equivalent orientation to observers on Earth.


Gliese 3470

GJ 3470 is a red dwarf star located in the constellation of Cancer, 30 parsecs away from Earth.
Properties.
The star has a mass of 0.539 solar masses and a radius of 0.547 solar radii. It is 1.6 billion years old, with a metallicity of 0.2 Fe/H. The star exhibits a strong stellar activity, with three ultraviolet flares detected by 2021.
Planetary system.
At least one exoplanet has been discovered orbiting at the distance of 0.031 astronomical units. The exoplanet, which is called GJ 3470 b, is a mini-Neptune with an orbital period of 3.3 days.
In July 2020, a group of amateur astronomers reported a new exoplanet candidate, which they hypothesize to be the size of Saturn and inside the system's habitable zone, along with twelve tentative transits from not yet characterized exoplanets in the same star system. If confirmed, GJ 3470 c would become the second exoplanet discovered by amateur astronomers, after KPS-1b, an exoplanet discovered by Ural State Technical University using amateur data. The new GJ 3470 candidate was discovered with amateur data and through a project led by amateur astronomers. However, it is important to note that the study in question has not been published in any scientific journal, nor has it been peer reviewed.


List of stars in Leo

This is the list of notable stars in the constellation Leo, sorted by decreasing brightness.


I Velorum

The Bayer designations i Velorum and I Velorum are distinct. Due to , both designations link here. For the star


Quadrans Muralis

Quadrans Muralis (Latin for "mural quadrant") was a constellation created by the French astronomer Jérôme Lalande in 1795. It depicted a wall-mounted quadrant with which he and his nephew Michel Lefrançois de Lalande had charted the celestial sphere, and was named Le Mural in the French atlas. It was between the constellations of Boötes and Draco, near the tail of Ursa Major, containing stars between β Bootis (Nekkar) and η Ursae Majoris (Alkaid).
Johann Elert Bode converted its name to Latin as "Quadrans Muralis" and shrank the constellation a little in his 1801 "Uranographia" star atlas, to avoid it clashing with neighboring constellations.
In 1922, Quadrans Muralis was omitted when the International Astronomical Union (IAU) formalised its list of officially recognized constellations.


R Lyrae

R Lyrae is a 4th magnitude semiregular variable star in the constellation Lyra, approximately 350 light years away from Earth. It is a red giant star of the spectral type M5III, meaning it has a surface temperature of under 3,500 kelvins. It is much larger and brighter, yet cooler, than the Sun. In the near-infrared J band, it is brighter than the nearby Vega.
R Lyrae is unusual in that it is a red star with a high proper motion, greater than 50 milliarcseconds a year.
The variability is not consistent and regular, but periods of 46, 64, 378, and 1,000 days have been reported, with the 46-day period being the strongest.
It is calculated that R Lyrae was a star on the main sequence. It is considered an oxygen-rich asymptotic giant branch star, with both hydrogen and helium shells fusing.


KX Andromedae

KX Andromedae (often abbreviated to KX And) is a spectroscopic binary star in the constellation Andromeda. Its apparent visual magnitude varies between 6.88 and 7.28.
The primary component of the KX Andromedae system is a Be star with a spectral classification B3pe as in 2017, although on historical record it has varied from B1 to B7.
The secondary star is difficult to detect in the spectrum, but has been given a K1III spectral type. It is likely to be an asymptotic giant branch star that fills its Roche lobe.
The system is only about 25 million years old. The pair complete a circular orbit every 38.919 days at an inclination of .


HD 29573

HD 29573 is a binary star system in the constellation Eridanus. It has a combined apparent visual magnitude of 4.99, making it visible to the naked eye. Based upon an annual parallax shift of , it is located 217 light years from the Sun. The system is moving further away from Earth with a heliocentric radial velocity of +3 km/s.
The binary nature of this system was discovered through observations made with the Hipparcos spacecraft. The pair orbit each other with a period of 41 years and an eccentricity of 0.8. The magnitude 5.19 primary component has a class of A1, 2.28 times the mass of the Sun, and is a suspected chemically peculiar star. The secondary has magnitude 7.22, 1.56 times the Sun's mass, and a class of F2. The system has a possible infrared excess due to circumstellar dust.


EV Carinae

EV Carinae is a red supergiant and pulsating variable star of spectral type M4Ia in the constellation Carina. It is a semiregular variable star with its apparent magnitude varying between 7.4 and 9.0 in the visible band, making it only seen by binoculars or a telescope. Various periods have been identified, but the dominant one is around 347 days. It is an MK spectral standard star for the class M4.5Ia.
EV Car is one of the largest known stars although its properties depend on its distance. In the late of the 20th century, EV Carinae, based on an assumed distance of 4.2 kpc, was found to be an extremely luminous and large supergiant star with an unusual luminosity between 550,000 and 675,000 times that of the Sun (), which would imply radii of 2,880 to 3,190 times the Sun's radius () at a temperature of 2,930 K, making it larger than the orbit of Saturn.
More recently, new calculations of the distance derived closer distances below 3 kpc which would put EV Car part of the Carina OB2 association along the Carina Nebula and give the star lower luminosities below , higher temperatures, and correspondingly lower radius values, while calculation of the bolometric luminosity based on a Gaia Data Release 2 parallax of gives a luminosity below with a corresponding radius of , but that value is considered unreliable due to a very high level of astrometric noise.


Upsilon Andromedae c

Upsilon Andromedae c (υ Andromedae c, abbreviated Upsilon And c, υ And c), formally named Samh (a homophone with the star Salm), is an extrasolar planet orbiting the Sun-like star Upsilon Andromedae A every 241.3 days. Its discovery in April 1999 by Geoffrey Marcy and R. Paul Butler made this the first multiple-planet system to be discovered around a main-sequence star, and the first multiple-planet system known in a multiple star system. Upsilon Andromedae c is the second known planet in order of distance from its star.
Name.
In July 2014 the International Astronomical Union launched a process for giving proper names to certain exoplanets and their host stars. The process involved public nomination and voting for the new names. In December 2015, the IAU announced the winning name was Samh for this planet. The winning name was submitted by the Vega Astronomy Club of Morocco and honours the 11th Century astronomer Ibn al-Samh of Muslim Spain.
Discovery.
Upsilon Andromedae c was detected by measuring variations in its star's radial velocity as a result of the planet's gravity. This was done by making precise measurements of the Doppler shift of the spectrum of Upsilon Andromedae A. At the time of discovery, Upsilon Andromedae A was already known to host one extrasolar planet, the hot Jupiter Upsilon Andromedae b, however by 1999 it was clear that the inner planet could not explain the velocity curve.
In 1999, astronomers at both San Francisco State University and the Harvard-Smithsonian Center for Astrophysics independently concluded that a three-planet model best fit the data. The two new planets were designated Upsilon Andromedae c and Upsilon Andromedae d.
Orbit and mass.
Like the majority of long-period extrasolar planets, the orbit of Upsilon Andromedae c is eccentric, more so than any of the major planets in the Solar System (including Pluto). If placed in the Solar System, Upsilon Andromedae c would lie between the orbits of Earth and Venus.
The high orbital eccentricity may be the result of gravitational perturbations from the planet Upsilon Andromedae d. Simulations suggest that the orbit of Upsilon Andromedae c returns to its original circular state roughly once every 9,000 years.
One proposal is that interactions between Upsilon Andromedae d and a (now lost) outer planet moved Upsilon Andromedae d into an orbit closer to the star, where it gradually caused the orbit of Upsilon Andromedae c to become eccentric. If so, the rogue planet would have had to eject immediately.
A limitation of the radial velocity method used to detect Upsilon Andromedae c is that the orbital inclination is unknown, and only a lower limit on the planet's mass can be obtained. However, by combining radial velocity measurements from ground-based telescopes with astrometric data from the Hubble Space Telescope, astronomers have determined the orbital inclination as well as the actual mass of Upsilon Andromedae c, which is about 13.98 times the mass of Jupiter. The mutual inclination between c and d is 29.9 degrees.
Characteristics.
Given the planet's high mass, it is likely that Upsilon Andromedae c is a gas giant with no solid surface. Since the planet has only been detected indirectly through observations of its star, properties such as its radius, composition, and temperature are unknown.
Since its actual mass is approximately 14 times that of Jupiter, and its star's metallicity is similar to that of the Sun, Upsilon Andromedae c may actually be a small brown dwarf.


Xi Pegasi

Xi Pegasi (ξ Peg, ξ Pegasi) is the Bayer designation for a double star in the northern constellation of Pegasus, the winged horse. Located in the horse's neck, the primary component is an F-type main sequence star that is visible to the naked eye with an apparent visual magnitude of 4.2. It is 86% larger and 17% more massive that the Sun, radiating 4.5 times the solar luminosity. Based upon parallax measurements taken with the Hipparcos spacecraft, it is located 53.2 ± 0.2 light years from the Sun.
The primary has been examined for the presence of an infrared excess that might indicate the presence of a debris disk, but none has been discovered. The common proper motion companion, NLTT 54820, is a twelfth magnitude red dwarf located at an angular separation of 11.4″ along a position angle of 96.9°. This corresponds to a projected physical separation of 192.3 AU.


K2-33

K2-33 is an extremely young pre-main-sequence star located about away from the Earth in the constellation of Scorpius. It is known to host one planet, a super-Neptune, named K2-33b. It is also notable for its young age.
Nomenclature and history.
K2-33 also has the 2MASS catalogue number J16101473-1919095 and EPIC designation 205117205.
Planetary candidates were detected around the star by NASA's Kepler Mission on its "K2" 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 pass in front of their stars from the perspective of Earth, although other phenomenon can also be responsible which is why the term planetary candidate is used.
Following the acceptance of the discovery paper, the Kepler team provided an additional moniker for the system of "K2-33". The discoverers referred to the star as K2-33, which is the normal procedure for naming the exoplanets discovered by the spacecraft. Hence, this is the name used by the public to refer to the star and its planet.
Candidate planets that are associated with stars studied by the Kepler Mission are assigned the designations ".01" etc. after the star's name, in the order of discovery. If planet candidates are detected simultaneously, then the ordering follows the order of orbital periods from shortest to longest. Following these rules, there was only one candidate planet were detected, with an orbital period of 5.424865 days.
The designation of "b" is given to the first planet orbiting a given star, followed by the other letters of the alphabet. In the case of K2-33, there was only one planet, so only the letter "b" are used. The name K2-33 derives directly from the fact that the star is the catalogued 33rd star discovered by "K2" to have confirmed planets.
Stellar characteristics.
This star was identified as a young pre-main-sequence object that belongs to the Upper Scorpius subgroup of the Scorpius–Centaurus Association in a 2001 article, based on its high lithium content and position in the HR diagram. This is the nearest OB association and recent massive star formation region, with the Upper Scorpius subgroup having a mean distance of 145 parsecs (470 light-years). Direct parallax measurements, by the Gaia spacecraft, indicate that K2-33 is at a distance of 140 ± 2 pc, consistent with association to Upper Scorpius. The age of this subgroup is estimated at 11 ± 2 million years, while evolutionary models estimate to K2-33 an independent age of 9.3 million years.
K2-33's spectrum is best modelled with a spectral type of M3.3 and a visual extinction of 0.75 magnitudes, so the star can be considered to be a red dwarf. Its effective temperature has been measured at 3,540 K, which together with the apparent brightness of the star indicates a luminosity of 0.15 times the solar luminosity and a radius of 1.05 times the solar radius. This large size is typical of young stars and indicates that the star is still in the process of contracting towards the main sequence. The mass of this star is not known accurately, and has been estimated at 0.56 or 0.31 times the solar mass. The metallicity of K2-33 is consistent with being equal to the solar value ([Fe/H] = 0).
As a young star, K2-33 has a fast rotation, with a projected rotational velocity of 8.2 km/s. The rotation period of the star, 6.3 days, is known from the light curve obtained by the Kepler spacecraft, causing periodic variations of about 2% in the brightness of the star as star spots appear and disappear from Earth's line of sight. This stellar variability was removed for the analysis of the transit signal of the planet K2-33b.
K2-33 is almost certainly not a binary star. Radial velocity data obtained by the HIRES spectrograph, in the Keck I Telescope, do not show an acceleration larger than 2.6 km/s/yr, which excludes objects more massive than 0.14 solar masses at 3 AU or closer. Adaptive optics infrared observations by the NIRC2 imager, in the Keck II Telescope, can exclude companions more massive than 19 Jupiter masses at 3 AU or further, and 11-12 Jupiter masses at 6-23 AU. The combination of both observational limits only allows for the existence of brown dwarfs or very low mass stars at separations of 1-3 AU.
Planetary system.
The only known planet transits the star; this means that the planet's orbit appear to cross in front of their star as viewed from the Earth's perspective. Its inclination relative to Earth's line of sight, or how far above or below the plane of sight it is, vary by less than one degree. This allows direct measurements of the planet's periods and relative diameters (compared to the host star) by monitoring the planet's transit of the star.
K2-33b is known remarkably for its extremely young age, only one other planet is younger (V830 Tau b), with an age of around 2 million years, while K2-33b is only 9.3 million years old. Nonetheless, it is quite a discovery in the search of exoplanets.
Infrared measurements by the Spitzer Space Telescope show that there is still a disk of planetary debris, indicating that planet formation may not be finished yet.


NGC 502

NGC 502, also occasionally referred to as PGC 5034 or UGC 922, is a lenticular galaxy in the constellation Pisces. It is located approximately 113 million light-years from the Solar System and was discovered on 25 September 1862 by German astronomer Heinrich Louis d'Arrest.
When the Morphological Catalogue of Galaxies was published between 1962 and 1974, the identifications of NGC 502 and NGC 505 were reversed. In reality, NGC 502 is equal to MGC +01-04-041 and not MCG +01-04-043 as noted in the catalogue.
Observation history.
Arrest discovered NGC 502 using an 11" reflecting telescope in Copenhagen. His position, which he measured on four separate nights, matches with both UGC 922 and PGC 5034. John Louis Emil Dreyer, creator of the New General Catalogue, described the galaxy as "considerably bright, small, round, brighter middle and nucleus".


DU Lyncis

DU Lyncis is a single variable star in the constellation Lynx. It is a faint star but visible to the naked eye with an apparent visual magnitude of 5.15. With an annual parallax shift of , it is located some 350 light years from the Sun. The star is moving closer with a heliocentric radial velocity of −37 km/s.
This is an aging red giant star with a stellar classification of M3 III, indicating that it has consumed the hydrogen at its core and evolved away from the main sequence. Eggen lists it as being on the asymptotic giant branch. It has been classified as a semiregular variable of type SRb, ranging from magnitude 5.18 down to 5.31 with periods of 360 and possibly 22 days. It shines with a luminosity approximately 536 times that of the Sun and has an effective temperature of 3,779 K.


30 Monocerotis

30 Monocerotis is a single star in the equatorial constellation of Hydra, located 122 light years away from the Sun. It has the Bayer designation C Hydrae; "30 Monocerotis" is the Flamsteed designation and was assigned when it belonged to the Monoceros constellation. The object is visible to the naked eye as a white-hued star with an apparent visual magnitude of 3.90. It is moving away from the Earth with a heliocentric radial velocity of +10 km/s.
This is an A-type main-sequence star with a stellar classification of A0 Va. It is around 162 million years old with a high rate of spin, showing a projected rotational velocity of 129 km/s. The star has 2.36 times the mass of the Sun and about 2.7 times the Sun's radius. It is radiating 40 times the luminosity of the Sun from its photosphere at an effective temperature of 10,281 K.
A statistically significant infrared excess has been detected, indicating a debris disk is orbiting from the host star with a blackbody temperature of . It is comparable in size to the asteroid belt. An unexplained X-ray emission has also been detected coming from these coordinates – stars of this class are not normally expected to show X-ray emission, so it may be coming from a background source or an unseen companion.


9 Puppis

9 Puppis is a binary star system in the southern constellation of Puppis. It was originally designated 9 Argus, being part of the now defunct Argo Navis constellation. The system is faintly visible to the naked eye as a point of light with a combined apparent visual magnitude of 5.16. The magnitude difference between the two stars is 0.65. Parallax measurements yield a distance estimate to 9 Puppis of approximately 54 light years from the Sun, with the dynamic and trigonometric parallaxes for the system being in close agreement. It is drifting closer with a systemic radial velocity of –21 km/s. The motion of the system through space is predicted to bring it as close as in about 292,000 years.
The binary nature of this system was discovered by S. W. Burnham in 1873, and it now has the discovery code BU 101 (originally: β 101). Early efforts at computing orbital elements were made by Burnham (1894), Aitken (1914), and others. The latest refined elements show an orbital period of 22.7 years with a large eccentricity (ovalness) of 0.74. The orbital plane is highly inclined to the line of sight at an angle of 80.4°.
The physical size of the system's semimajor axis is estimated to be . The large eccentricity of their orbit means a circumstellar planetary orbit would most likely only be stable over long periods with a semimajor axis inside from the primary and from the secondary. An outer circumbinary planet would have a stable orbit with a semimajor axis beyond about from the barycenter.
The stellar classification of the 9 Puppis system is G0V, matching a G-type main-sequence star like the Sun. The dynamic masses of the components are 1.06 and 0.90 times the mass of the Sun, yielding estimated individual stellar classes of G1 for the primary and G9 for the secondary, respectively. The system has been listed as a probable member of the Ursa Major Moving Group, but was excluded by Soderblom and Mayor (1993) due to low lithium abundance and low X-ray flux. Their age determined from chromospheric heating is around seven billion years.


Epsilon Cassiopeiae

Epsilon Cassiopeiae (ε Cassiopeiae, abbreviated Eps Cas, ε Cas), officially named Segin , is a star in the constellation of Cassiopeia. With an apparent visual magnitude of 3.4, this is one of the brightest stars in the constellation. The distance to this star has been determined directly using parallax measurements, yielding a value of around from the Sun.
Nomenclature.
"ε Cassiopeiae" (Latinised to "Epsilon Cassiopeiae") is the star's Bayer designation.
The star bore the traditional name "Segin", which probably originates from an erroneous transcription of "Seginus", the traditional name for Gamma Boötis, which itself is of uncertain origin. Different sources report varying pronunciations, with SEG-in the most common but the variants SAY-gin and seg-EEN also appearing. In 2016, the IAU organized a Working Group on Star Names (WGSN) to catalog and standardize proper names for stars. The WGSN approved the name "Segin" for this star on 5 September 2017 and it is now so included in the List of IAU-approved Star Names.
While some published reports incorrectly claim that this star was designated by NASA as "Navi" ('Ivan', backwards), in honor of astronaut Virgil Ivan "Gus" Grissom, one of the three astronauts who died in the Apollo 1 accident, the actual star so designated is Gamma Cassiopeiae in the center of the constellation.
In Chinese, (), meaning "Flying Corridor", refers to an asterism consisting of Epsilon Cassiopeiae, Iota Cassiopeiae, Delta Cassiopeiae, Theta Cassiopeiae, Nu Cassiopeiae and Omicron Cassiopeiae. Consequently, the Chinese name for Epsilon Cassiopeiae itself is (, .)
Properties.
Epsilon Cassiopeiae has a stellar classification of B3 V, indicating that it is a main sequence star fusing hydrogen in its core. Cote "et al." (2003) indicate that it displays the spectral properties of a Be star, even though it is not categorized as such. The presence of emission lines in the spectrum indicates the presence of a circumstellar shell of gas that has been thrown off by the star. The outer atmosphere has an effective temperature of , giving it the blue-white hue of a B-type star.
The interferometer-measured angular diameter is 0.43 milliarcseconds. At the estimated distance of this star, this yields a physical size of roughly 6 times the radius of the Sun.
Observation during the Hipparcos mission suggest that the star may undergo weak periodic variability. The amplitude of this variation is 0.0025 in magnitude with a frequency of 11.17797 times per day, or one cycle every 2.15 hours. The signal-to-noise ratio for this measured variation is 4.978. Hipparcos measurements of the space velocity components for this star suggest that it is a member of the Cas-Tau group of co-moving stars, with a 93% likelihood. This group may be kinematically associated with the alpha Persei Cluster, indicating that the Cas-Tau group, including Epsilon Cassiopeiae, may have been separated from the cluster through tidal interactions.
References.
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List of stars in Fornax

This is the list of notable stars in the constellation Fornax, sorted by decreasing brightness.


List of stars in Capricornus

This is the list of notable stars in the constellation Capricornus, sorted by decreasing brightness.


Three Stars (Chinese constellation)

The Three Stars mansion () is one of the twenty-eight mansions of the Chinese constellations. It is one of the western mansions of the White Tiger. This collection of seven bright stars is visible during winter in the Northern Hemisphere (summer in the Southern).


Beta Cephei

Beta Cephei (β Cephei, abbreviated Beta Cep, β Cep) is a triple star system of the third magnitude in the constellation of Cepheus. Based on parallax measurements obtained during the Hipparcos mission, it is approximately 690 light-years distant from the Sun. It is the prototype of the Beta Cephei variable stars.
It consists of a binary pair (designated Beta Cephei A) together with a third companion (B). The binary's two components are themselves designated Beta Cephei Aa (officially named Alfirk , the traditional name for the system) and Ab.
Nomenclature.
"β Cephei" (Latinised to "Beta Cephei") is the system's Bayer designation. The designations of the two constituents as "Beta Cephei A" and "B", and those of "A's" components - "Beta Cephei 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).
Beta Cephei bore the traditional name "Alfirk", derived from the Arabic الفرقة "al-firqah" "the flock" (of sheep). With Alpha Cephei (Alderamin) and Eta Cephei (Alkidr), they were "Al Kawākib al Firḳ" الكوكب الفرق "the stars of the flock" by Ulug Beg. In 2016, the IAU 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 "Alfirk" for the component Beta Cephei Aa on 21 August 2016 and it is now so included in the List of IAU-approved Star Names.
Visibility.
Like the star Epsilon Draconis in the constellation of Draco, Beta Cephei is visible primarily in the northern hemisphere, given its extreme northern declination of 70 degrees and 34 minutes. It is nevertheless visible to most observers throughout the world reaching as far south as cities like Harare in Zimbabwe, Santa Cruz de la Sierra in Bolivia or other settlements north ± 19° South latitude. It is circumpolar throughout all of Europe, northern Asia, and North American cities as far south as Guadalajara in west central Mexico. All other locations around the globe having a latitude greater than ± 20° North will notice that the star is always visible in the night sky. Because Beta Cephei is a faint third magnitude star, it may be difficult to identify in most light polluted cities, though in rural locations the star should be easily observable.
Pole Star.
Beta Cephei is a visible star located within 5° of the precessional path traced across the celestial sphere by the Earth's North pole. During the same period Iota Cephei will also be within 5° of the precessional path, on the other side so that both are in contention as pole stars, a title currently held by unambiguously by Polaris.
Properties.
Beta Cephei is a triple star comprising a spectroscopic binary with a magnitude 8 optical companion. Its magnitude varies between +3.16 and +3.27 with a period of 0.19048 days.
Beta Cephei Aa is a blue subgiant star with a stellar classification of B1 IV. It has previously been classified with either a main sequence or giant luminosity class. This star has a radius that has been estimated at and a mass of . Like most high-mass B-class stars, Beta Cephei Aa is a relatively young star with an estimated age of just a few million years. Like the majority of giant stars, it rotates slowly on its axis with a rotational velocity of 7 deg/day, a speed which takes the star approximately 51 days to make one complete revolution.
Beta Cephei Ab is a Be star in an 85-year orbit with the giant primary. It has been resolved using speckle interferometry at a distance of 0.25" in 1972.
B Cephei B is a magnitude 7.8 A2 main sequence star 13.6" distant.
Variability.
Beta Cephei pulsates regularly every 4 hours 34 minutes, producing a variation in its visual brightness of 0.11 magnitudes. It is the prototype of the Beta Cephei class of variables, hot main sequence and giant stars that pulsate analogously to Cepheid variables but with the pulsations driven by iron opacity rather than by helium.