Sigma Puppis

Sigma Puppis (Sigma Pup, σ Puppis, σ Pup) is a binary star system in the southern constellation of Puppis. It has an apparent visual magnitude of 3.25, which is bright enough to be visible to the naked eye at night from the southern hemisphere. Through a telescope, it appears as a bright, orange-hued star with a nearby white companion. Parallax measurements indicate this star is located at a distance of about from Earth.
This is a spectroscopic binary system, consisting of an orbiting pair of stars that have not been individually resolved with a telescope. Their orbital period is 257.8 days and the eccentricity is 0.17. The pair form an eclipsing binary of the Beta Lyrae type and a period of 130.5 days, or one half of their orbital period. The eclipse of the primary component causes a decline of 0.04 magnitudes, while the secondary eclipse reduces the magnitude by 0.03.
The combined stellar classification is K5 III, which matches the spectrum of a giant star. The measured angular diameter of the primary star is . At the estimated distance of this system, this yields a physical size of about 107 times the radius of the Sun. The primary component shows the behavior of a slow irregular variable.
In addition to its binary components, Sigma Puppis has a more distant companion that has a matching proper motion, suggesting that it may be gravitationally bound to the binary. This magnitude 8.5 star is at an angular separation of 22.4 arcseconds with a position angle of 74° from Sigma Puppis, which is equivalent to a projected separation of 1,200 Astronomical Units. In 1970, American astronomer Olin J. Eggen suggested that Sigma Puppis belonged to a moving group of stars that share a similar motion through space, and thereby a common origin. It served as the eponym for this, the σ Puppis group. The existence of this group was later brought into question.
References.
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29 Cygni

29 Cygni is a single star in the northern constellation of Cygnus. It is dimly visible to the naked eye as a white-hued star with an apparent visual magnitude of 4.93. The distance to 29 Cyg, as estimated from an annual parallax shift of , is 131 light years. The star is moving closer to the Earth with a heliocentric radial velocity of −17 km/s. It is a member of the 30–50 million year old Argus Association of co-moving stars.
This is an A-type main-sequence star with a stellar classification of A2 V. Rodríguez et al. (2000) classify it as a Delta Scuti variable with a frequency of 0.0267 cycles per day. It is a Lambda Boötis class chemically peculiar star and the first such star to be classified as a pulsating variable. 29 Cyg is multi-periodic, small-amplitude variable with a magnitude change of about 0.02 and a dominant period of 39 minutes. A magnetic field has been detected with an averaged quadratic field of . The star has a moderate rate of rotation, showing a projected rotational velocity of 65 km/s. It has double the mass of the Sun and is radiating 25 times the Sun's luminosity from its photosphere at an effective temperature of roughly 8,790 K.
29 Cygni is listed in multiple star catalogs as having several companions within , including the yellow 7th magnitude HD 192661. All are background objects not physically associated with 29 Cygni itself. The naked-eye stars b1 Cygni and b2 Cygni, respectively about one and two degrees away, also lie at different distances to 29 Cygni.


S Ori 70

S Ori 70 or S Ori J053810.1-023626 is a mid-T type astronomical object in the foreground of the σ Orionis cluster, which is approximately 1,150 light-years from Earth. It was discovered on November 24, 2002 by M. R. Zapatero Osorio and E. L. Martin's team at the Roque de los Muchachos Observatory. It has yet to be determined if it is a field brown dwarf or a 3-million-year-old planet that is part of a cluster. Near-infrared spectroscopy images taken 3 years after its discovery led to the first motion measurements for the object. Its behavior is significantly different from what may be expected; it was further described as either a low-gravity atmosphere or an atmosphere with metallicity. The object's small proper motion suggests that it is farther away than expected if it were a single field T dwarf.
Discovery.
The σ Orionis open cluster has been the focus of Osorio's team observations due to the age of the cluster (approximately 3 to 8 million years). The cluster also has low extinction, its distance is convenient, and it is observed to be rich and dense. Using the William Herschel Telescope in a pencil-beam deep mini-survey measuring 55 square minutes of arc at a sensitivity of 21 magnitudes in the J and H Bands allowed the team to find S Ori 70. The raw data collected was reduced to IRAF (an acronym for Image Reduction and Analysis Facility), a standard technique used with near-infrared images; after subtracting the sky background and dark current, an extracted object spectrum was derived. It was the faintest and coolest member found in the cluster and was named S Ori 70.
Argument of the initial study.
Adam J. Burgasser examined the claims of Osorio's T-type brown dwarf discovery and its spectroscopically verified low-mass. A comparison of the J band spectrum between S Ori 70 and other field objects was done. The J band spectrum revealed a distinct triangular-shaped spectral morphology which was previously explained by Osorio and Martin was due to the surface's low gravity. In order to see if similar discrepancies occurred in the T dwarf's behavior, Burgasser's team compared data from the claims of Osorio to that of standard COND models. Identical wavelength scales interpolated through both empirical and model spectra were Gaussian smoothed; this showed that best-fit spectral models can yield skewed gravities for late-type field T dwarfs which resulted in the underestimation of age and mass. Burgasser concluded that S Ori 70 is not a member of the Sigma Ori cluster but is rather a foreground field brown dwarf. Further study of the object suggest that the low gravity was not from the field T dwarf but rather a nearby background star. As of 2009 no direct scientific data have dispelled nor confirmed either conclusion.
It could be the first "free floating" non-stellar planet discovered with a mass of 3 MJ, but needs confirmation.


29 Arietis

29 Arietis is a triple star system in the northern constellation of Aries. "29 Arietis" is the Flamsteed designation. Its annual parallax shift of indicates a distance of about from Earth. The system is barely visible to the naked eye with an apparent visual magnitude of 6.0; it is 0.02 degree north of the ecliptic. It is moving further from Earth with a heliocentric radial velocity of 9 km/s.
The core of the system is formed by a close spectroscopic binary with an angular separation of 3.892 mas, a semimajor axis of , an orbital period of 19.4 days, and an eccentricity of 0.4. The larger member of this pair has 114% of the mass of the Sun, while its companion has 88% of the Sun's mass. Orbiting the pair at an angular separation of 1.422 arcseconds over a period of 164 years, the tertiary component has 52% of the Sun's mass.


Upsilon3 Eridani

Upsilon³ Eridani (υ³ Eridani, abbreviated Upsilon³ Eri, υ³ Eri), officially named Beemim , is a star in the constellation of Eridanus. It is visible to the naked eye with an apparent visual magnitude of 3.96 The distance to this star, based upon an annual parallax shift of 11.01 mas, is around 296 light-years.
This is an evolved K-type giant star with a stellar classification of K4 III. It has about 54 times the radius of the Sun and radiates 426 times the solar luminosity from its outer atmosphere at an effective temperature of 3,990 K.
Nomenclature.
"υ³ Eridani" (Latinised to "Upsilon³ Eridani") is the star's Bayer designation.
This star bore the traditional name "Beemim" (also rendered "Beemin", "Theemim" and "Theemin" -- see Theemin). In 2016, the International Astronomical Union organized a Working Group on Star Names (WGSN) to catalog and standardize proper names for stars. The WGSN approved the name "Beemim" for this star on 30 June 2017 and it is now so included in the List of IAU-approved Star Names.
In Chinese, (), meaning "Celestial Orchard", refers to an asterism consisting of Upsilon³ Eridani, Chi Eridani, Phi Eridani, Kappa Eridani, HD 16754, HD 23319, Theta Eridani, HD 24072, HD 24160, Upsilon⁴ Eridani, Upsilon² Eridani and Upsilon¹ Eridani. Consequently, the Chinese name for Upsilon³ Eridani itself is (, ).


NGC 3048

NGC 3048 is a pair of spiral galaxies located in the constellation Leo. It was discovered on April 27, 1864, by German astronomer Albert Marth. The object consists of a visual pair of galaxies, PGC 1509261 and PGC 28595. PGC 1509261 is likely a physical pair with a much fainter galactic object not a part of the New General Catalogue, J095458+162726.


47 Arietis

47 Arietis is a single star in the northern constellation of Aries. The designation is from the star catalogue of English astronomer John Flamsteed, first published in 1712. It is faintly visible to the naked eye with an apparent visual magnitude of 5.80. It has an annual parallax shift of , which is equivalent to a physical distance of approximately from Earth.
The star is moving further from the Sun with a radial velocity of +26.6 km/s. It has a relatively high proper motion, traversing the celestial sphere at the rate of 0.237 arc seconds per year. The combination of these movements indicate this star is a member of the Hyades supercluster.
Li et al. (2000) categorized this as an F-type main-sequence star with a stellar classification of F5 V(e). Previously, Cowley (1976) listed a class of F5 IV, which would indicate it is a subgiant star. It is most likely (97.8% chance) the source of X-ray emission that is detected at these coordinates, and it is a radio source. The star has 1.55 times the mass of the Sun and is radiating 4.43 times the Sun's luminosity from its photosphere at an effective temperature of roughly 6,633 K.
47 Arietis has a red dwarf companion at an angular separation of 14.8 arc seconds along a position angle of 113°, as of 1998. This star has a class of M3.5 and an infrared J-band magnitude of 10.47.


V345 Carinae

V345 Carinae is a star in the constellation Carina. It has the Bayer designation "E Carinae"; "V345 Carinae" is the variable star designation. The star has a blue-white hue and is faintly visible to the naked eye with an apparent visual magnitude that fluctuates around +4.66. Its actual brightness varies from magnitude +4.67 to +4.78 with a period of 137.7 days. Based on parallax measurements, it is located at a distance of approximately 1,010 light years from the Sun. It is drifting further away with a radial velocity of around +19 km/s.
This star has a stellar classification of B2(IV)n, matching a suspected B-type subgiant star. The 'n' notation indicates "nebulous" lines caused by rapid rotation: the star is spinning with a projected rotational velocity of 140 km/s. It is a Be star having a circumstellar disk of hot, decreted gas that is inserting emission lines into the spectrum. The star is 20 million years old with 9.6 times the mass of the Sun and 8.7 times the Sun's radius. It is radiating 2,540 times the luminosity of the Sun from its photosphere at an effective temperature of 19,000 K.
The star displays a complex luminosity variation with a periods of 1.13028 and 137.7 days. Although thought to be a single star, Carrier et al. (2002) suggested the longer period may be caused by some sort of binary interaction with the circumstellar disk or perhaps a light reflecting effect. However, no companion has been detected via radial velocity variations. This suggests that the companion would need to either have less than 1.7 times the mass of the Sun or it is being viewed from nearly pole-on. The short-term variations may be from non-radial pulsations similar to those of ω CMa.


Gamma Normae

The Bayer designation γ Normae, which is Latinized as gamma Normae and abbreviated γ Nor, is shared by two stars in the southern constellation of Norma:
The pair form a double star that can be resolved with the naked eye.


H Puppis

The Bayer designations h Puppis and H Puppis are distinct. They can refer to three stars in the constellation Puppis:


Pi2 Ursae Minoris

Pi2 Ursae Minoris, which is Latinized from π2 UMi Ursae Minoris, is a binary star system in the northern circumpolar constellation of Ursa Minor. The pair have a combined apparent visual magnitude of 6.89, which can be viewed with a pair of binoculars. They are located at a distance of approximately 400 light years from the Sun based on parallax, but are drifting closer with a radial velocity of −32 km/s.
This star was found to be a double system by O. Struve in 1832, and the pair have now completed a full orbit. There is a lot of scatter in the data though, so the grade of the orbital elements is rated as poor. The system has a high eccentricity of 0.96 and they orbit each other with a period of roughly 172 years. The magnitude 7.32 primary is an F-type main-sequence star with a stellar classification of F1V. The fainter secondary has a magnitude of 8.15 and is G-type star.


HD 85622

HD 85622 is a binary star system in the southern constellation of Vela. It is visible to the naked eye with an apparent visual magnitude of 4.58. The distance to HD 85622 can be estimated from its annual parallax shift of , yielding a value of 750 light years. It is moving further from the Earth with a heliocentric radial velocity of +8 km/s.
This is a single-lined spectroscopic binary with a circular orbit and a period of 329.3 days. The "a" sin "i" value is , where "a" is the semimajor axis and "i" is the orbital inclination to the line of sight. This value provides a lower bound on the actual semimajor axis. The system shows a micro-variability in its brightness, and is a source of X-ray emission with an apparent flux of .
The visible component is a supergiant star with a stellar classification of G5 Ib or G6 IIa. It is about 64 million years old with a projected rotational velocity of 19 km/s. The star has 6.2 times the mass of the Sun and is radiating 1,908 times the Sun's luminosity from its photosphere at an effective temperature of 4,796 K.


R Ursae Minoris

R Ursae Minoris is a star in the constellation Ursa Minor. A red giant of spectral type M7IIIe, it is a semiregular variable ranging from magnitude 8.5 to 11.5 over a period of 325 days.


XZ Tauri

XZ Tauri is a binary system approximately away in the constellation Taurus. The system consists of two T Tauri stars orbiting each other about 6 billion kilometers apart (roughly the same distance as Pluto is from the Sun). The system made news in 2000 when a superflare was observed in the system.


29 Orionis

29 Orionis is a single star located around 157 light years away from the Sun in the equatorial constellation of Orion. In Bayer's "Uranometria", this star is one of two stars (the other being Upsilon Orionis) marking the top of Orion's right boot. It has the Bayer designation e Orionis, while "29 Orionis" is the Flamsteed designation. This object is visible to the naked eye as a faint, yellow-hued point of light with an apparent visual magnitude of 4.13. It is moving closer to the Earth with a heliocentric radial velocity of -18 km/s.
This is an aging giant star with a stellar classification of G8IIIFe-0.5, having exhausted the supply of hydrogen at its core and evolved away from the main sequence. The suffix notation indicates a mild underabundance of iron in the spectrum. It is a red clump giant, which means it is on the horizontal branch and is generating energy through helium fusion at its core. The star has 2.33 times the mass of the Sun and has expanded to 10.36 times the Sun's radius. It is radiating 71 times the Sun's luminosity from its enlarged photosphere at an effective temperature of 4,852 K.


Rho Persei

Rho Persei (Rho Per, ρ Persei, ρ Per) is a star in the northern constellation of Perseus. It has the traditional name Gorgonea Tertia , being the third member of the quartet called the Gorgonea in reference to the Gorgons from the legend of Perseus. An apparent visual magnitude of +3.39 makes it visible to the naked eye, but a challenge to view from a well-lit urban environment. Based upon parallax measurements, it is located at a distance of roughly from Earth.
Rho Persei is a semiregular variable star, whose apparent magnitude varies between 3.3 and 4.0 with periods of 50, 120 and 250 days. The star has reached the asymptotic giant branch of its evolution. It is a bright giant star with a stellar classification of M4 II. The outer envelope has an effective temperature of 4,111 K, giving it the red-orange hue of an M-type star.
This star has a mass five times the mass of the Sun, while its radius has expanded to 150 times solar. It is radiating some 2,290 times the Sun's luminosity. Rho Persei is losing mass at the rate of solar masses per year, or the equivalent of the Sun's mass every 83 million years. It is about 440 million years in age.
Naming.
In Chinese, (), meaning "Mausoleum", refers to an asterism consisting of ρ Persei, 9 Persei, τ Persei, ι Persei, κ Persei, β Persei, 16 Persei and 12 Persei. Consequently, the Chinese name for ρ Persei itself is (, .).


NGC 207

NGC 207 is a spiral galaxy roughly 178 million light-years from the Solar System in the constellation Cetus. It was discovered on December 7, 1857, by R. J. Mitchell.


Sigma Sagittarii

Sigma Sagittarii (σ Sagittarii, abbreviated Sigma Sgr, σ Sgr), formally named Nunki , is the second-brightest star in the constellation of Sagittarius. It has an apparent magnitude of +2.05, making it readily visible to the naked eye. The distance to this star, determined using parallax measurements from the Hipparcos astrometry satellite, yields an estimated value of from the Sun.
Properties.
Sigma Sagittarii has a spectrum matching a stellar classification of B2.5 V, which indicates this is a B-type main-sequence star. Its total luminosity is 3300 times that of the Sun while it has a surface temperature of 18,890 K. X-ray emission has been detected from this star, which has an estimated X-ray luminosity of .
It has a 10th magnitude optical companion located 5.2 arcminutes away.
It is 3.45 degrees south of the ecliptic, so it can be occulted by the Moon and rarely by planets. The last occultation by a planet took place on November 17, 1981, when it was occulted by Venus. This is the brightest star that can be principally occulted by an exterior planet between 5000 BC and 5000 AD. However, only Mars can do this, and only rarely; the last time was on September 3, 423.
Nomenclature.
"σ Sagittarii" (Latinised to "Sigma Sagittarii") is the star's Bayer designation.
It bore the traditional name of "Nunki", which was an Assyrian or Babylonian name recovered by archaeologists and made public by R. H. Allen. In 2016, the International Astronomical Union organized a Working Group on Star Names (WGSN) to catalogue and standardize proper names for stars. The WGSN approved the name "Nunki" for this star on 21 August 2016 and it is now so included in the List of IAU-approved Star Names.
This star, together with :
Zeta Sagittarii and Pi Sagittarii may have been the Akkadian "Gu-shi-rab‑ba", the Yoke of the Sea.
In the catalogue of stars in the "Calendarium" of Al Achsasi al Mouakket, this star was designated "Thanih al Sadirah", which was translated into Latin as "Secunda τού al Sadirah", meaning "second returning ostrich".
In Chinese, (), meaning "Dipper", refers to an asterism consisting of Sigma Sagittarii, Phi Sagittarii, Lambda Sagittarii,
Mu Sagittarii, Tau Sagittarii and Zeta Sagittarii. Consequently,the Chinese name for Sigma Sagittarii itself is (, .)


Gamma2 Fornacis

Gamma2 Fornacis, a name Latinized from γ2 Fornacis, is a single star in the southern constellation Fornax. It has a white hue and is faintly visible to the naked eye at night with an apparent visual magnitude of 5.4. The distance to Gamma2 Fornacis is approximately 520 light years based on parallax. It is drifting further away with a radial velocity of 24 km/s. Gamma1 Fornacis is a 6th magnitude star about four degrees to the north.
The stellar classification of Gamma2 Fornacis is A1 V, which is notation for an A-type main-sequence star that, like the Sun, is generating energy through core hydrogen fusion. Comparison of its properties to theoretical models suggest an age of about 400 million years old. It has a high rate of spin, showing a projected rotational velocity of 149 km/s. The star has 2.4 times the mass of the Sun and 4.5 times the Sun's radius. It is radiating 117 times the luminosity of the Sun from its photosphere at an effective temperature of roughly 9,000 K.


XO-2 (star)

XO-2 is a binary star. It consists of two components: XO-2S (Also known as XO-2A) and XO-2N (Also known as XO-2B).
This system is located approximately 500 light-years away from Earth in the Lynx constellation. Both of these stars are slightly cooler than the Sun and are nearly identical to each other. The system has a magnitude of 11 and cannot be seen with the naked eye but is visible through a small telescope. These stars are also notable for their large proper motions.
XO-2N and XO-2S have a separation of approximately AU.
Planetary systems.
There are two known exoplanets orbiting XO-2N. XO-2Nb (or rarely XO-2Bb), which is classified as a hot Jupiter, was discovered by the XO Telescope using the transit method orbiting XO-2N (XO-2B) in 2007 and XO-2Nc was discovered in 2015 using the radial velocity method.
Two planets were reported to orbit around XO-2S in 2014 using radial velocity method. One of them is Jupiter-mass and another has a mass comparable to Saturn.
Both stars also show RV-trends, which may indicate the presence of additional long-periodic jovians or brown dwarfs around each of them.


Zeta Delphini

Zeta Delphini (ζ Delphini) is a star in the constellation of Delphinus. With an apparent magnitude of about 4.6, it is faintly visible to the naked eye. Parallax measurements of the system made by the Hipparcos spacecraft put it at a distance of about 220 light-years, or 67 parsecs.
Zeta Delphini has a spectral type of A3V, implying it is an A-type main-sequence star. These types of stars are bluish-white colored, and have effective temperatures between 7100 and 11500 K: Zeta Delphini has a temperature of 8336 K. Its age is estimated to be around 500 million light years, considerably younger than the Sun.
In 2014, the discovery of a brown dwarf around Zeta Delphini was announced. Zeta Delphini B is a brown dwarf with a spectral type of L5 (but may be from L3 to L7), and has a mass of about 55 Jupiters. At over 13 arcseconds away, this brown dwarf is separated at least 910 AU from Zeta Delphini.


Theta Delphini

Theta Delphini, a name Latinized from θ Delphini, is a single star in the northern constellation of Delphinus. It has an apparent visual magnitude of about 5.7, meaning that it is just barely visible to the naked eye under excellent viewing conditions. The distance to this star is approximately 2,050 light years from the Sun based on parallax. It is drifting closer with a radial velocity of −15 km/s.
The stellar classification of Theta Delphini is K3Ib, which means it is a K-type supergiant. These types of stars form when relatively massive (10 to ) stars like B-type main sequence stars run out of hydrogen to fuse and start cooling down. It has been described as a super-metal-rich star because of its high metallicity.


Gamma Sagittae

Gamma Sagittae, Latinized from γ Sagittae, is the brightest star in northern constellation of Sagitta. A single star, it is visible to the naked eye with an apparent visual magnitude of +3.47. Based upon an annual parallax shift of 12.62 mas as seen from Earth, it is located about 258 light years from the Sun. It is moving closer to the Sun with a radial velocity of −34 km/s.
This is a red giant star with a stellar classification of M0 III. It is most likely (94% chance) on the red-giant branch of its evolutionary lifespan, fusing hydrogen along a shell to generate energy. The star is around 2.35 billion years old with roughly 55 times the Sun's radius. Mass estimates range from 0.9 to 1.8 times the mass of the Sun. It is radiating about 562 times the Sun's luminosity from its enlarged photosphere at an effective temperature of 3,862 K.
Naming.
In Chinese, (), meaning "Left Flag", refers to an asterism consisting of γ Sagittae, α Sagittae, β Sagittae, δ Sagittae, ζ Sagittae, 13 Sagittae, 11 Sagittae, 14 Sagittae and ρ Aquilae. Consequently, the Chinese name for γ Sagittae itself is (, ).


NGC 4800

NGC 4800 is an isolated spiral galaxy in the constellation Canes Venatici, located at a distance of from the Milky Way. It was discovered by William Herschel on April 1, 1788. The morphological classification of this galaxy is SA(rs)b, indicating a spiral galaxy with no visual bar at the nucleus (SA), an incomplete ring structure (rs), and moderately-tightly wound spiral arms (b). The galactic plane is inclined to the line of sight by an angle of 43°, and the long axis is oriented along a position angle of 25°. There is a weak bar structure at the nucleus that is visible in the infrared.
The galaxy has a low-luminosity active galactic nucleus with an HII region at the core. The circumnuclear zone contains a double ring structure of "ultra-compact nuclear rings"; the inner ring has a radius of 30 pc and the outer ring's radius is about 130 pc. The upper limit on the mass of the central Supermassive Black Hole is estimated as , or 20 million times the mass of the Sun.


NGC 3382

NGC 3382 is the name for two stars in the constellation Leo Minor. The object was discovered on April 5, 1874 by the Irish astronomer Lawrence Parsons.


KjPn 8

KjPn 8 is a bipolar planetary nebula which was discovered by M.A. Kazaryan and Eh. S. Parsamyan in 1971 and independently by Luboš Kohoutek in 1972.
Very little was published about this nebula until 1995, when it was realized that KjPn 8 sits in the center of a very large filamentary nebula, 14 by 4 arc minutes in size. This is the largest known bipolar structure associated with a planetary nebula. Narrow band images centered at Hα and forbidden line transitions of nitrogen, sulphur, and oxygen reveal pairs of bow shocks at differing position angles, indicating the presence of episodic ejection of material along a precessing jet, similar to what is seen in Fleming 1, but much larger (in angular extent).
The physical size of this extended nebula is approximately 4.1 by 1.2 parsecs, much larger than a typical planetary nebula, while the core nebula known prior to 1995 is only about 0.2 parsecs in diameter.
The envelope of KjPn 8 is expanding rapidly enough to allow the proper motion of features in the nebula to be measured. In 1997 John Meaburn compared images of the nebula taken in 1954 (as part of the Palomar Sky Survey) and 1991.He measured a proper motion of 34±3 milliarcseconds per year for two knots in the nebula. Combining this proper motion with an expansion velocity derived from spectral line profile widths allowed Meaburn to derive a distance to the nebula of 1600±230 parsecs, and a kinematic age of 3400±300 years.
Microwave emission from carbon monoxide reveals the presence of a dense disk of molecular gas 30 arcseconds in diameter expanding at about 7 km/sec, with a mass ≥ 0.03 M⊙. The disk is aligned with the youngest and fastest bipolar jet, which has an expansion velocity of about 300 km/sec. The central star has begun to ionize the central region of this disk.
Hubble Space Telescope observations suggest that KjPn 8 might be a very rare object, formed by a binary system in which both stars had similar masses, which reached the end of the Asymptotic Giant Branch phase within 10 to 20 thousand years of each other, and entered the planetary nebula formation stage nearly simultaneously.


V450 Aquilae

V450 Aquilae is semi-regular pulsating star in the constellation Aquila. Located around 660 light-years distant, it shines with a luminosity approximately 2172 times that of the Sun and has a surface temperature of 3326 K.


Tau Sculptoris

Tau Sculptoris (τ Scl, τ Sculptoris) is a binary star system in the southern constellation of Sculptor, about 8° to the east-southeast of Alpha Sculptoris. It is faintly visible to the naked eye with a combined apparent visual magnitude of +5.69. Based upon an annual parallax shift of 14.42 mas as seen from Earth, it is located around 230 light years from the Sun.
The binary nature of this system was discovered by English astronomer John Herschel in 1835. The current orbital elements are based upon a fraction of a single orbit, as the estimated orbital period is around 1,503 years. The system has a semimajor axis of 3.2 arc seconds and an eccentricity of 0.6. The primary member, component A, is a yellow-white hued F-type main sequence star with an apparent magnitude of +6.06 and a stellar classification of F2 V. The companion, component B, is a magnitude 7.35 star.


Gamma Sculptoris

Gamma Sculptoris, Latinized from γ Sculptoris, is a single, orange-hued star in the constellation Sculptor. Based upon an annual parallax shift of 17.90 mas as seen from Earth, this star is located about 182 light years from the Sun. It is bright enough to be visible to the naked eye with an apparent visual magnitude of 4.41. It is moving away from the Sun with a radial velocity of +15.6 km/s.
This is an evolved K-type giant star with a stellar classification of K1 III. At the age of 2.47 billion years it is a red clump star on the horizontal branch, which means it is generating energy through helium fusion at its core. The star has 1.60 times the mass of the Sun and it has expanded to 12 times the Sun's radius. It is radiating 72 times the Sun's luminosity from its enlarged photosphere at an effective temperature of 4,578 K


NGC 469

NGC 469 is a spiral galaxy in the constellation Pisces. With its distance being approximately 167 million light-years from Earth, it was discovered by Albert Marth in 1864.


NGC 5078

NGC 5078 is a spiral galaxy in the Hydra constellation, approximately 94 million light-years away from Earth. It has a diameter of 127,000 light-years and is probably a member of the NGC 5061 group. The dust lane of NGC 5078 is warped, probably by interaction with the nearby galaxy IC 879, which is itself distorted into an 'S' shape by the interaction. At the presumed distance the two galaxies would have a minimal separation of about 61,000 light-years. For comparison, the Large Magellanic Cloud is about 160,000 light-years from the Milky Way.


45 Aurigae

45 Aurigae or PLX 1468.2 is a binary star system in the northern constellation of Auriga. It has an apparent visual magnitude of 5.34, making it visible to the naked eye under suitable viewing conditions. An annual parallax shift of 16.89 mas as seen from Earth's orbit indicates the system is located about 193 light years from the Sun.
This is a close, single-lined spectroscopic binary with a circularized orbit with a short period of 6.5 days. They have a mean angular separation of 0.963 mas. The visible component has a stellar classification of F5 V, matching an F-type main-sequence star that is generating energy through hydrogen fusion at it core. It is about 1.6 billion years old and is spinning with a projected rotational velocity of 14 K. It has 1.2 times the mass of the Sun and is radiating 22 times the Sun's luminosity from its photosphere at an effective temperature of around 6,489 K. The secondary has a minimum mass of 42% of the Sun's mass.


HR 6902

HR 6902 (also designated V2291 Oph) is a binary system located 790 light years away from the Sun in the Ophiuchus constellation. The system includes an orange bright giant star and a B-type main sequence star, forming an eclipsing binary of Zeta Aurigae type. The system is also surrounded by a warm circumstellar envelope and the spectra show silicon and carbon absorption up to a distance of 3.3 giant radii.


DG Tauri B

DG Tauri B, near the T Tauri star DG Tauri, is a young stellar object located 450 light-years (140 parsecs) from Earth, within the Taurus constellation. Observations of DG Tauri B were first made in October, and later December 1995 at the 6 element Owens Valley millimeter wave array. Its most notable characteristics are its bipolar jets of molecular gas and dust emanating from either side of the object. Red-shifted carbon monoxide emissions extend out 6,000 AU to the northwest of the object from the undetermined source, and are symmetrically distributed about the jet, while blue-shifted CO emissions are confined to a region with a roughly 500 AU radius.


Epsilon Cygni

Epsilon Cygni (ε Cygni, abbreviated Epsilon Cyg, ε Cyg) is multiple star system in the constellation of Cygnus. With an apparent visual magnitude of 2.48, it is readily visible to the naked eye at night as one of the brighter members of Cygnus. Based upon parallax measurement, Epsilon Cygni is about 73 light-years from the Sun.
The system has three constituents: a spectroscopic binary (designated Epsilon Cygni A); an optical companion (B) and a single star (C). A's two components are themselves designated Epsilon Cygni Aa (officially named Aljanah ) and Ab.
Nomenclature.
"ε Cygni" (Latinised to "Epsilon Cygni") is the system's Bayer designation. The designations of the three constituents as "Epsilon Cygni A", "B" and "C", and those of "A's" components - "Epsilon Cygni 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).
Epsilon Cygni bore the traditional name "Gienah" from the Arabic "al janāħ" () meaning "the wing". However that name was more usually applied to Gamma Corvi. For reasons of disambiguation it was sometimes called Gienah Cygni. 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 "Aljanah" for the component Epsilon Cygni Aa on 30 June 2017. It had previously approved the name "Gienah" for Gamma Corvi A on 6 November 2016. Both are now so included in the List of IAU-approved Star Names.
In Chinese astronomy, the "Celestial Ford" () refers to an asterism consisting of Epsilon Cygni, Gamma Cygni, Delta Cygni, 30 Cygni, Alpha Cygni, Nu Cygni, Tau Cygni, Upsilon Cygni and Zeta Cygni. Consequently, the Chinese name for Epsilon Cygni Cygni itself is "the Ninth Star of Celestial Ford" ().
Companions.
Epsilon Cygni A has an optical companion, Epsilon Cygni B, with which it is not physically associated, and a 13th magnitude candidate common proper motion companion, Epsilon Cygni C, at an angular separation of 78 arcseconds. If the latter star is gravitationally bound to Epsilon Cygni A, then they are currently separated by 1700 AU or more, and have an orbital period of at least 50,000 years.
Properties.
Epsilon Cygni A is a single-lined spectroscopic binary. Radial velocity observations suggest a possible companion with an orbital period of at least 15 years. It presents as a giant star with a stellar classification of K0 III. This indicates that the star has left the main sequence and has begun the final stages in its stellar evolution. The effective temperature of its photosphere is 4,710 K, giving an orange hue that is a characteristic of K-type stars. It has nearly 11 times the solar radius and is about 62 times the luminosity of the Sun.
Since 1943, the spectrum of Epsilon Cygni A has served as one of the stable anchor points by which other stars are classified.
Veil Nebula.
ε Cygni lies about three degrees north of the Veil nebula, a probable ancient supernova remnant. The nebula is far more distant than the star.


Necklace Nebula

The Necklace Nebula (PN G054.2-03.4) is a 19-trillion-kilometre-wide ( light-year-wide) planetary nebula located about 15,000 light-years away in the northern constellation Sagitta. It was discovered in 2005 from the Isaac Newton Telescope Photometric H-alpha Survey (IPHAS), a ground-based H-alpha planetary nebula study of the North Galactic Plane.
The Necklace Nebula is the exploded aftermath of a giant star that came too close to its Sun-like binary companion. The two stars that produced the Necklace Nebula are in a relatively small orbit about each other. They have a period of 1.2 days and a separation on the order of 5 times the radius of the Sun.
About 10,000 years ago one of the aging stars ballooned to the point where it engulfed its companion star. The smaller star continued orbiting inside its larger companion, increasing the giant's rotation rate.
The bloated companion star spun so fast that a large part of its gaseous envelope expanded into space. Due to centrifugal force, most of the gas escaped along the star's equator, producing a ring. The embedded bright knots are dense gas clumps in the ring.


C Capricorni

c Capricorni can refer to two different stars:


HD 240429/240430

HD 240429 (nicknamed Krios) and HD 240430 (Kronos) is a wide binary star system in the constellation of Cassiopeia. Both components of the system are yellow G-type main-sequence stars. HD 240430 is a Sun-like star in appearance, but it seems to have eaten its own planets, for which it is given the nickname Kronos, after the Greek god and the leader of the first generation of Titans. Its unusual properties were described by a team of astrophysicists at Princeton University in 2017, led by Semyeong Oh.
Kronos and Krios are about 350 light years away from Earth. Formed around four billion years ago, they originated from the same interstellar cloud. They are moving together through space and are assumed to orbit each other slowly, with an estimated period of about 10,000 years. Kronos has a higher abundance of elements such as lithium, magnesium and iron in its atmosphere than in that of Krios. They are the most chemically different binary stars to have been discovered to date. The unusual and rich chemical composition leads scientists to the conclusion that Kronos has destroyed many of its orbiting planets. According to estimates, it might have absorbed at least 15 Earth masses.


FG Sagittae

FG Sagittae is a supergiant star in the constellation Sagitta at a distance of 4000 light-years. When first noted in 1943, it was identified to be a variable star, and it was found to be a hot, blue star of stellar spectral type B in 1955. Since then it has expanded and cooled, becoming a yellow G-type star by 1991, and then further cooling to become an orange K-type star. It started to pulsate when becoming an A-type star with a period of 15 days. This period later increased to over 100 days.
Since 1992 the star has exhibited fadings and recoveries similar to that of a R Coronae Borealis variable star; this behavior is emphasized by a hydrogen deficiency typical for this class of stars. It has been proposed that this star has undergone a late thermal pulse (LTP) of helium fusion after having left the asymptotic giant branch (AGB) to move towards the hottest end of the "white dwarf cooling track". This thermal pulse is believed to have revived this aged star to once again, for a short time, behave as an AGB star.
FG Sagittae is the central star of the planetary nebula Henize 1-5.
Observations.
In 1943, a star designated AN 377.1943 was discovered to be a previously-unknown variable star. It was designated CSV 5066 as a suspected variable, and then FG Sagittae as a confirmed variable star. At the time, its variations were described as being irregular, but it was soon noted that the average brightness was steadily increasing. It brightened by about two magnitudes between 1943 and 1970, and then began to fade. Examination of old photographic observations found that the star had been brightening since at least 1900, with extrapolations suggesting that the minimum had occurred around 1880. As it faded, FG Sagittae began to show periodic variations, at first a period of 80 days, but increasing to 130 days. In 1992, the periodic variations ceased and the brightness decreased by five magnitudes in only two months. Since then, it has continued to show occasional deep fading events, appearing much like an R Coronae Borealis star.
The spectrum of FG Sagittae when it was first noted as a variable star was that of a blue supergiant. The first reliable spectral class is B0 in 1930. Extrapolation of the brightness and colour indices suggest it may have been an O3 star in 1890. It then steadily cooled, with the spectral class becoming as late as K2 in the 1980s. The spectral class has since stayed as a G or K type supergiant, but there have been dramatic changes. The abundances of various elements have either increased or decreased: s-process elements became at least 25 times more abundant between 1967 and 1974; iron peak elements became less visible; and carbon-rich dust became strongly visible after 1992. Observations of the spectrum after 1992 are hindered by the dust formation, but the s-process and rare earth elements appear to have continued becoming more abundant.
Planetary nebula.
There is a very faint visible planetary nebula, Henize 1-5, around FG Sagittae, around visual magnitude 23. This formed when FG Sagittae first left the asymptotic giant branch. FG Sagittae is now losing mass at about every million years and a dust shell has formed around the star. This may form a second planetary nebula.
Evolution.
The effective temperature of FG Sagittae in 1930 would have been about , possibly as hot as in 1890, then cooling to about by 1975. Detailed analysis of the spectral energy distribution during the 1980s show a slow decrease in temperature to as low as . During the deep fades since 1992, even lower temperatures have been calculated, but these may represent observations of obscuring dust rather than the surface of the star itself.
The bolometric luminosity of FG Sagittae increased steadily from around at the end of the 19th century to over by 1965. The luminosity then became more or less stable until 1992. As the star cooled and became more luminous, its radius increased from around in 1900 to about by 1992.
When the star faded in 1992, it was obscured by dust formation and comparisons of temperature and luminosity became more difficult. The visual luminosity dropped by about five magnitudes, but the infrared brightness increased by a comparable amount. Models of the dust around the star suggest that the luminosity dropped sharply for a few hundred days as dust formed and was heated, but the underlying stellar luminosity was essentially constant and remained constant until at least 2001.
The underlying properties of FG Sagittae changed on a timescale almost unheard-of for a star, from a small very hot post-asymptotic giant branch star becoming a white dwarf, to a hot supergiant and then a cool supergiant. This is believed to have been due to a helium flash in a shell that had previously been inactive since the star left the asymptotic giant branch. This is known as a late thermal pulse or very late thermal pulse, depending on the exact timing. Models approximate the behaviour of FG Sagittae although there are still detailed discrepancies.


Beta Piscium

Beta Piscium (β Piscium, abbreviated Beta Psc, β Psc), formally named Fumalsamakah , is a blue-white hued star in the zodiac constellation of Pisces. Its apparent magnitude is 4.40, meaning it can be faintly seen with the naked eye. Based on parallax measurements taken during the Hipparcos mission, it is about 410 light-years (125 parsecs) distant from the Sun.
Nomenclature.
"β Piscium" (Latinised to "Beta Piscium") is the star's Bayer designation.
It bore the traditional name "Fum al Samakah" from the Arabic فم السمكة "fum al-samakah" "mouth of the fish" (compare Fomalhaut). 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 "Fumalsamakah" for this star on 1 June 2018 and it is now so included in the List of IAU-approved Star Names.
In Chinese, (), meaning "Thunderbolt", refers to an asterism consisting of Beta Piscium and Gamma, Theta, Iota and Omega Piscium. Consequently, the Chinese name for Beta Piscium itself is (, ).
Properties.
Beta Piscium is a Be star, a special class of B-type stars with emission lines in their spectra. With a spectral type of B6Ve its mass is estimated to be about , and its radius is about . It is suspected to be a variable star. Beta Piscium is radiating 524 times the Sun's luminosity from its photosphere at an effective temperature of 15,500 K. The star has a high rate of spin, showing a projected rotational velocity of around 90 km/s.


Tau Lupi

The Bayer designation τ Lupi (Tau Lupi) is shared by two star systems in the constellation Lupus:


Phi Ursae Majoris

Phi Ursae Majoris, Latinized from φ Ursae Majoris, is binary star system in the northern constellation of Ursa Major. It is white-hued and is visible to the naked eye with a combined apparent visual magnitude of +4.60; the primary is magnitude 5.28 while the secondary is magnitude 5.39. The system is located at a distance of approximately 510 light years from the Sun based on parallax, but is drifting closer with a radial velocity of −14.7 km/s. It should make its closest approach at a distance of around in about 4.7 million years.
As of 2017, the components had an angular separation of along a position angle of 304°. They are orbiting each other with a period of 105.4 years and eccentricity of 0.44. Both of components are A-type subgiant stars with a stellar classification of A3 IV.
Phi Ursae Majoris is moving through the Galaxy at a speed of 21.6 km/s relative to the Sun. Its projected Galactic orbit carries it between 24,000 and 46,000 light years from the center of the Galaxy.
Naming.
With τ, h, υ, θ, e, and f, it composed the Arabic asterism "Sarīr Banāt al-Na'sh", the Throne of the daughters of "Na'sh", and "Al-Haud", the Pond. According to the catalogue of stars in the "Technical Memorandum 33-507 - A Reduced Star Catalog Containing 537 Named Stars", "Al-Haud" were the title for seven stars : f as "Alhaud I", τ as "Alhaud II", e as "Alhaud III", h as "Alhaud IV", θ as "Alhaud V", υ as "Alhaud VI" and this star (φ) as "Alhaud VII".
In Chinese, (), meaning "Administrative Center", refers to an asterism consisting of φ Ursae Majoris, υ Ursae Majoris, θ Ursae Majoris, 15 Ursae Majoris and 18 Ursae Majoris. Consequently, the Chinese name for φ Ursae Majoris itself is known as (, ).


NGC 483

NGC 483 is a spiral galaxy in the constellation Pisces. It is located approximately 192 million light-years from Earth and was discovered on November 11, 1827 by astronomer John Herschel.


R Aquilae

R Aquilae is a variable star in the equatorial constellation of Aquila. It is located approximately 780 light years distant from the Sun based on parallax, and is drifting further away with a radial velocity of 35 km/s. This is a thermally-pulsating Mira variable that ranges in brightness from 5.3 down to 12.0 with a period of 269.84 days. The period was over 300 days when first observed, and has declined steadily since – decreasing from 320 in 1915 down to 264 in 2010, at an average rate of 0.4 days per year. The amplitude of the variation has also decreased by about a magnitude since discovery. The peak magnitude is bright enough for the star to be visible to the naked eye as a dim, red-hued star.
R Aquilae is an aging red giant on the asymptotic giant branch with a stellar classification that varies over time, between M5e and M9e, where the 'e' suffix indicates emission features in the spectrum. The cooler spectral types occur near the minimum visual magnitude, and the hottest near maximum. The star may have recently undergone a helium flash. It is oxygen-rich in abundance with the same mass as the Sun but has expanded to 259 times the Sun's radius. On average, the star is radiating 3,470 K times the luminosity of the Sun from its swollen photosphere at an effective temperature of 3000 K or so. It is losing mass at the rate of , forming a dusty silicate shell.


39 Draconis

39 Draconis is a wide binary star system in the northern circumpolar constellation of Draco. It has the Bayer designation b Draconis, while "39 Draconis" is the Flamsteed designation. This system is visible to the naked eye as a dim, white-hued point of light with an apparent visual magnitude of 5.0. Parallax measurements made by the Hipparcos spacecraft put it at a distance of 184 light-years, or 56 parsecs away from the Sun. The system is moving closer to the Earth with a heliocentric radial velocity of -24.5 km/s.
The two components of 39 Draconis have an angular separation of and take almost 4,000 years to orbit each other. The primary star is an early A-type main-sequence star, having 2.12 times the mass of the Sun with a visual magnitude of 5.06 The secondary is a magnitude 8.07 F-type main-sequence star, and has 1.18 times the mass of the Sun.
The 8th-magnitude star HD 238865 is listed in double star catalogues as component C. It is separated from the other two stars by and lies at about the same distance. It is itself a spectroscopic binary with an F8 primary and a red dwarf secondary orbiting every 2.7 days.


CX Canis Majoris

CX CMa (CX Canis Majoris) is a blue variable star in the Canis Major constellation. Discovery of this variable is usually credited to German Astronomer Cuno Hoffmeister in 1931, although this remains uncertain.
It is an eclipsing binary of Algol (detached) whose magnitude varies between 9.9 and 10.4 with a period of 0.95462500 day (22.911000 hour). The variability was first discovered in 1931. Doubts arose because of scatter in the data and the small amplitude, but the discovery was confirmed by 1949. Its Algol-type light curve exhibits the O'Connell effect, meaning that there is a magnitude difference between subsequent maxima.
The temperature of the secondary star has been estimated at about 10,600 K and its mass at . The spectral type of the secondary star is estimated to be in the B8 to A0 range.


XX Trianguli

XX Trianguli, abbreviated XX Tri, is a variable star in the northern constellation of Triangulum, about 1.5° to the WNW of Beta Trianguli along the constellation border with Andromeda. It is classified as a RS Canum Venaticorum variable and ranges in brightness from magnitude 8.1 down to 8.7, which is too faint to be visible to the naked eye. The system is located at a distance of approximately 642 light years from the Sun based on parallax, but is drifting closer with a radial velocity of −26 km/s.
This is a single-lined spectroscopic binary with an orbital period of 23.96924 days. The visible component is an orange-hued K-type giant star with a stellar classification of K0 III, indicating it has exhausted the supply of hydrogen at its core then cooled and expanded off the main sequence. It is around eight billion years old with 26% more mass than the Sun and has expanded to 11 times the Sun's radius. It is radiating roughly 30 times the luminosity of the Sun from its photosphere at an effective temperature of 4,620 K.
The star is "covered with large high-latitude and even polar spots and with occasional small equatorial spots". XX Tri is notable for having a huge starspot larger than the diameter of the Sun, discovered using Doppler imaging. For its size, the star has a relatively rapid rotation rate of about 24 days. It has a weak, Sun-like differential rotation. The star appears to show a magnetic activity cycle of , although only a single cycle has been observed as of 2015.


LTT 3780

LTT 3780, also known as TOI 732 or LP 729-54, is the primary of the binary stellar system LDS 3977 in the constellation Hydra.
Characteristics.
LTT 3780 is an M-type main-sequence star. It is of similar age to Sun and relatively enriched in metals.
Planetary system.
In 2020, an analysis carried out by a team of astronomers led by astronomer Ryan Cloutier of the TESS project confirmed the existence of two planets on mildly eccentric orbits, the inner being a super-Earth and the outer a small gas giant about half the mass of Uranus.


Phi2 Orionis

Phi2 Orionis is a star in the constellation Orion, where it forms a small triangle on the celestial sphere with the nearby Meissa and Phi1 Orionis. This star is visible to the naked eye with an apparent visual magnitude of 4.081. Based upon an annual parallax shift of 27.76 mas, it is located around 117 light years from the Sun.
This is a G-type giant or subgiant star with a stellar classification of G8 III-IV that, at the age of 6.9 billion years, is evolving away from the main sequence. It has 1.07 times the mass of the Sun, but has expanded to 7.72 times the Sun's radius. The star shines with 31.6 times the solar luminosity from its outer atmosphere at an effective temperature of 4,856 K.


NGC 472

NGC 472 is a spiral galaxy located roughly 220 million lightyears from earth in the constellation Pisces. It was discovered on August 29, 1862 by Heinrich Louis d'Arrest.


HD 32309

HD 32309 is a single star in the southern constellation of Lepus. It has a blue-white hue and is visible to the naked eye with an apparent visual magnitude of 4.91. The distance to this object is 197 light years based on parallax. It is drifting further away from the Sun with a radial velocity of +24 km/s. This is a member of the Columba association of co-moving stars.
This is a B-type main-sequence star with a stellar classification of B9V. It is around 124 million years old and is spinning rapidly with a projected rotational velocity of about 300 km/s. Mass estimates range from 2.56 to 3.24 times the mass of the Sun and it has about 3.1 times the Sun's radius. The star is radiating 46.5 times the luminosity of the Sun from its photosphere at an effective temperature of 12,450 K.


87 Leonis

87 Leonis is a single star in the zodiac constellation of Leo, located approximately 480 light years away from the Sun. It has the Bayer designation e Leonis; "87 Leonis" is the Flamsteed designation. This object is visible by the naked eye as a faint orange-hued star with an apparent visual magnitude of 4.77. It is moving away from the Earth with a heliocentric radial velocity of 19 km/s. The star is positioned near the ecliptic and thus is subject to occultation by the Moon.
This is an aging K-type giant star with a stellar classification of , which means it has exhausted the hydrogen at its core and evolved away from the main sequence. The suffix notation indicates a mild underabundance of iron in the atmosphere. It has expanded to 37 times the Sun's radius and is radiating over a thousand times the Sun's luminosity from its photosphere at an effective temperature of 4,001 K.


Tau6 Eridani

Tau6 Eridani, Latinized from τ6 Eridani, is a single star in the equatorial constellation of Eridanus, located near the constellation border with Fornax. It has a yellow-white hue with an apparent visual magnitude of 4.22, which is bright enough to be seen with the naked eye. Based upon parallax measurements, the distance to this star is around 57.5 light years. It is drifting further away with a radial velocity of +8 km/s.
The spectrum of Tau6 Eridani matches a stellar classification of F5IV-V, indicating it is an F-type star that shows traits of both a main sequence star and a subgiant. It has an estimated 135% of the Sun's mass and about 1.8 time the radius of the Sun. The star is radiating 5.5 times the luminosity of the Sun at an effective temperature of 6,508 K, and it does not display any surface magnetic activity. The star has been examined for infrared excess emission that could indicate the presence of circumstellar matter, but none has been detected.


CO-0.40-0.22

CO-0.40-0.22 is a high velocity compact gas cloud near the centre of the Milky Way. It is 200 light years away from the centre in the central molecular zone. The cloud is in the shape of ellipse. The differences in the velocity, termed velocity dispersion, of the gas is unusually high at 100 km/s. The velocity dispersion was once thought to be due to an intermediate-mass black hole (IMBH) with a mass of about 100,000 solar masses. However, observations with the Atacama Large Millimeter/submillimeter Array were not consistent with such a large IMBH, and the features identified as signatures of IMBH-cloud interaction in previous studies turned out to be artifacts created by erroneous data reduction.
Subsequent theoretical studies of the gas cloud and nearby IMBH candidates have re-opened the possibility, though no observational evidence for existence of an IMBH has been reported so far.
The molecular cloud has a mass of 4,000 solar masses. It is located at −0.40°, −0.22° galactic longitude and latitude. The cloud is 0.2° away from Sgr C to the galactic southeast. The gas is moving away from Earth at speeds ranging from 20 to 120 km/s. The spectral lines of carbon monoxide reveal that the gas is dense, and warm and fairly opaque.
The gas cloud includes carbon monoxide and hydrogen cyanide molecules. Other molecules detected via microwave spectroscopy include cyanoacetylene, cyclopropenylidene, methanol, silicon monoxide, sulfur monoxide, carbon monosulfide, Thioformaldehyde, Hydrogen isocyanide, Formamide, and ions H2N+ and HCO+.
The name followed the precedent set by CO-0.02-0.02, which is another high velocity compact cloud in the central molecular zone. Another example of this naming convention is CO–0.30–0.07.


NGC 6027

NGC 6027 is a lenticular galaxy that is the brightest member of Seyfert's Sextet, a compact group of galaxies. Édouard Stephan discovered the galaxy in 1882.


T Antliae

T Antliae (also abbreviated T Ant) is a Classical Cepheid variable star that is between 10 and 12,000 light-years away from the Sun in the constellation of Antlia. A yellow-white supergiant with a spectral type of F6Iab, it ranges between apparent magnitude 8.86 and 9.76 over a period of 5.89820 days.
Variability.
T Antliae varies in brightness regularly every 5.89820 days. The light curve is extremely consistent and shows a rapid rise taking 23% of the period, with a slower decline. The maximum brightness of apparent magnitude 8.86 and the minimum of 9.76 are also extremely consistent.
The amplitude, light curve shape, period, and consistency, all mark T Antliae as a Cepheid variable. However, the exact sub-type has been debated. It has been considered a type II Cepheid, and old population II star, but is now thought to be a younger more massive Classical Cepheid variable, also known as a δ Cepheid.
The period has been calculated to be increasing by about half a second per year. The increasing period implies that the effective temperature of T Antliae is decreasing, something that would happen both during the initial crossing of the instability strip after a star has left the main sequence, and again following a blue loop. The first crossing of the instability strip is very rapid and T Antliae is judged to be crossing it for the third time (the second time occurs with increasing temperature at the start of the blue loop).
The brightness changes of Cepheid variables are caused by pulsations in their outer layers, causing both the temperature and radius to change. The radius of T Antliae has been calculated to vary by as it pulsates, around 10% of its radius. The temperature, and hence the spectral type, also vary. Spectral types between F6 and G5 have been published for T Antliae.
Stellar system.
The timing of the light variations of T Antliae show a small scatter which can be fitted to a sine curve. This has been proposed to be due to light travel time caused by orbital movement of the variable star. This is based on somewhat uncertain data from old photograph records, and there is no confirmation of a companion. A compatible orbit would take 42.4 years to complete, with a semimajor axis around 10.8 Astronomical Units.
A sparse open cluster lies around the position of T Antliae. Fitting of isochrones to the brighter stars shows a main sequence turnoff consistent with the position of T Antliae in the H-R diagram. The bluest stars in the cluster, and T Antliae itself, best match an isochrone of 100 million years. Fitting to redder stars in the cluster gives an age of around 79 million years.


RCW 34

RCW 34 (Gum 19) - H II region and the emission nebula located in the constellation Vela. It is located approximately 22,000 light years from Earth. Named after Australian astronomer Colin Stanley Gum.
The nebula RCW 34 is relatively dark. However, when observed using infrared wavelengths, two different areas are visible - one half of the nebula is bright, the other is dark. The bright side is the hydrogen illuminated by a nearby blue supergiant star, and dark is the place where new stars surround the central star on the other side.
The source of energy that stimulates the nebula RCW 34 to shine is a huge, extremely hot star V391 Velorum with a surface temperature of up to 30,000 °C. Because it is a variable star, it evokes violent phenomena, including discards of matter shells, affecting the composition and light emission of the RCW 34 nebula. Stars of the type V391 Velorum do not burn long enough to explode as supernovae. It can be expected that the explosion of the central star will completely change the RCW 34 nebula.


R Leonis

R Leonis is a red giant Mira-type variable star located approximately 370 light years away in the constellation Leo.
The apparent magnitude of R Leonis varies between 4.31 and 11.65 with a period of 312 days. At maximum it can be seen with the naked eye, while at minimum a telescope of at least 7 cm is needed. The star's effective temperature is estimated 2,890 kelvins and radius spans , roughly Mars's orbital zone.
Possible planet.
In 2009 Wiesemeyer et al. proposed that quasi-periodic fluctuations observed for the star R Leonis may be due to the presence of an evaporating substellar companion, probably an extrasolar planet. They have inferred a putative mass for the orbiting body of twice the mass of Jupiter, orbital period of 5.2 years and likely orbital separation of 2.7 astronomical units.
If confirmed such a planetary object could likely be an evaporating planet, with a long comet-like trail as hinted by intense SiO maser emissions.


List of stars in Circinus

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


C Scorpii

The Bayer designation c Scorpii is shared by two star systems in the constellation Scorpius:


72 Herculis

72 Herculis is a single star in the northern constellation of Hercules. The Flamsteed designation for this star comes from the publication "Historia Coelestis Britannica" by John Flamsteed. It is the 72nd star in Flamsteed's list of stars in Hercules. This star is faintly visible to the naked eye with an apparent visual magnitude of 5.4. Parallax measurements show this star to be located at a distance of about 47 light years from the Sun. It is drifting closer with a radial velocity of −78.6 km/s, and is predicted to come to within in around 98,000 years.
This is an ordinary G-type main-sequence star with a stellar classification of G0 V. It is similar in mass to the Sun, with a 13% larger radius. The star is radiating 1.3 times the luminosity of the Sun from its photosphere at an effective temperature of . The metallicity is much lower than in the Sun, with an [Fe/H] equal to . The star is an estimated 4–7 billion years old with a projected rotational velocity of 1 km/s. The level of chromospheric activity appears to be at or below that in the Sun.
As of 2010, no planetary companion had been detected orbiting this star. The "Washington Visual Double Star Catalog" for 1996 showed two visual companions of this star. The first is a visual magnitude 9.7 star located 289.1 arc seconds away. The second is only separated by 8.7 arc seconds, and is magnitude 12.9. It is unknown whether these visual companions are gravitationally-bound to 72 Her.


Kepler-59b

Kepler-59b is an exoplanet orbiting the star Kepler-59, located in the constellation Lyra. It was discovered by the "Kepler" telescope in August 2012. It completes an orbit around its parent star once every 11.9 days. It has a radius that is 1.1 times that of the Earth.


Lambda Horologii

λ Horologii, Latinised as Lambda Horologii, is a star in the southern constellation of Horologium. It is a yellow-white hued star that is dimly visible to the naked eye with an apparent visual magnitude of +5.35. Based upon parallax, this object is located 155 light years distance from the Sun. It is drifting further away with a radial velocity of +28 km/s. Although Eggleton and Tokovinin (2008) list this as a single star, according to Kunzli and North (1998) it may be a binary system with a long orbital period.
The visible component has a stellar classification of F2III, matching an evolved star that has, at the age of 1.4 billion years, become a giant. However, it has just 2.74 times the Sun's radius and shows a high rate of spin with a projected rotational velocity of +140 km/s. The star has 1.76 times the mass of the Sun and is radiating 13 times the Sun's luminosity from its photosphere at an effective temperature of 6,848 K.


S Normae

S Normae (S Nor) is a yellow supergiant variable star in the constellation Norma. It is the brightest member of the open cluster NGC 6087.
S Normae is a Classical Cepheid variable with a visual magnitude range of 6.12 to 6.77 and a period of 9.75411 days. The spectral type varies during the pulsation cycle from F8 to G0. Its mass has been measured at with reference to a close orbital companion, and it is over 3,000 times as luminous as the sun.
Companions.
S Normae is a spectroscopic binary, although the companion has now been resolved using the Hubble Space Telescope Wide Field Camera 3. The separation was 0.90" in April 2011, corresponding to 817 AU. This gives the rare opportunity for a direct determination of the mass of a Cepheid variable star and confirmation of other properties. It is a supergiant that is 6.3 times as massive as the Sun and 2,800 times as luminous. The companion a blue-white main sequence star of spectral type B9.5.
There is a more distant 10th magnitude companion at 30", unsurprising in the centre of an open cluster. It is TYC 8719-794-1, a chemically peculiar A or B class star. Three fainter companions have also been found: a 14th magnitude star at 14"; and two 16th magnitude stars at 20".


Kappa Velorum

Kappa Velorum (κ Velorum, abbreviated Kappa Vel, κ Vel; formally named Markeb ) is a binary star system in the southern constellation of Vela. The two components are designated Kappa Velorum A and B.
From parallax measurements, this system is located at a distance of roughly from the Sun. The apparent visual magnitude is 2.48, making it readily visible to the naked eye in the southern hemisphere. It forms part of an asterism known as the False Cross along with Delta Velorum, Iota Carinae and Epsilon Carinae, so called because it is sometimes mistaken for the Southern Cross, causing errors in astronavigation.
Nomenclature.
"κ Velorum" (Latinised to "Kappa Velorum") is the system's Bayer designation. The designations of the two components as "Kappa Velorum A" and "B" derives from the convention used by the Washington Multiplicity Catalog (WMC) for multiple star systems, and adopted by the International Astronomical Union (IAU).
The system bore has the traditional name "Markab", from the Arabic مركب, "markab" meaning "something to ride". It was often spelled "Markeb" to distinguish it from similarly named stars such as Alpha Pegasi. 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 "Markeb" for Kappa Velorum on 5 September 2017. "Markab" had previously been approved for Alpha Pegasi on 30 June 2016. Both are now so included in the List of IAU-approved Star Names.
In Chinese, (), meaning "Celestial Earth God's Temple", refers to an asterism consisting of Kappa Velorum, Gamma² Velorum, b Velorum and Delta Velorum. Consequently, Kappa Velorum itself is known as (), "the Fifth Star of Celestial Earth God's Temple".
Properties.
Kappa Velorum is a spectroscopic binary system consisting of a pair of stars that complete an orbit around each other with a period of 116.65 days and an eccentricity of 0.19. Because the individual stars have not been resolved, further details of the orbit have not yet been determined. The combined stellar classification of the pair is B2 IV, which matches the class of a B-type subgiant star that has exhausted the hydrogen at its core and begun to evolve into a giant. It has an estimated size of 6.9 times the Sun's radius.
The system is only a couple of degrees from the south celestial pole of Mars, so it could therefore be considered the southern polar star of that planet. Due to precession of the equinoxes, it will be the closest bright star of note to the south celestial pole of Earth in the period surrounding 9000 AD.
Interstellar medium.
Analysis of the spectrum of Kappa Velorum shows absorption lines due to the interstellar medium between Earth and the star. Observation of these features over many years has shown that the lines vary in strength, probably caused by a small dense cloud extending 10²–10³ au moving across the line of sight.


Pi2 Orionis

Pi2 Orionis (π2 Ori, π2 Orionis) is the Bayer designation for a solitary star in the equatorial constellation of Orion. Although the "Bright Star Catalogue" lists this as a spectroscopic binary star system, this does not appear to be the case. It is visible to the naked eye with an apparent visual magnitude of 4.35. Based upon an annual parallax shift of 14.53 mas, it is located roughly 224 light years away from the Sun.
This is an A-type main sequence star with a stellar classification of A1 Vn, where the 'n' indicates broad absorption lines due to rotation. It is spinning rapidly with a projected rotational velocity of 261.4 km/s. This is giving the star an oblate shape with an equatorial bulge that is 13% larger than the polar radius. It is shining with 70 times the solar luminosity from its outer atmosphere at an effective temperature of 9,457 K.


58 Hydrae

58 Hydrae is a single star in the equatorial constellation of Hydra, located around 290 light years away from the Sun based on parallax. It has the Bayer designation E Hydrae; "58 Hydrae" is the Flamsteed designation − a later designation of 6 Librae. It is visible to the naked eye as a faint, orange-hued star with an apparent visual magnitude of 4.42. This object is moving closer to the Earth with a heliocentric radial velocity of −9 km/s.
This is an aging giant star with a stellar classification of , most likely (98% chance) on the red giant branch. The suffix notation indicates an underabundance of iron in the spectrum, and some uncertainty about the classification. It is around 8.1 billion years old with 0.88 times the mass of the Sun. As a consequence of exhausting the hydrogen at its core, the star has expanded to 33.4 times the Sun's radius. It is radiating 310 times the luminosity of the Sun from its swollen photosphere at an effective temperature of 4,210 K.


58 Persei

58 Persei is a binary and possibly a triple star system in the northern constellation of Perseus. It has the Bayer designation e Persei, while "58 Persei" is the Flamsteed designation. This system is visible to the naked eye as a faint point of light with an apparent visual magnitude of 4.26. It is approximately 800 light years away from the Sun based on parallax, and is drifting further away with a radial velocity of +10 km/s.
This is a single-lined spectroscopic binary system with an orbital period of 28.7 years and an eccentricity of 0.65. The primary member, designated component A, is an orange-hued (K–type) bright giant with a stellar classification of K1II. The star is around 50 million years old with 7 times the mass of the Sun. Having exhausted the supply of hydrogen at its core, it has expanded to roughly 56 times the Sun's radius. It is radiating 1,698 times the luminosity of the Sun from its enlarged photosphere at an effective temperature of 5,173 K.
The secondary, component B, appears to be a B-type main-sequence star with a stellar classification of B7V. It is a suspected binary of unknown period with component masses of 3.3 and 1.2 times the mass of the Sun.


Mu Piscium

Mu Piscium (μ Piscium) is a solitary, orange-hued star in the zodiac constellation of Pisces. It is visible to the naked eye with an apparent visual magnitude of 4.84. Based upon an annual parallax shift of 10.73 mas as seen from Earth, it is located about 304 light years from the Sun. Given this distance, it has a relatively high proper motion, advancing 296 mas per year across the sky.
This is an evolved K-type giant star with a stellar classification of K4 III. It has an estimated 1.25 times the mass of the Sun and, at the age of 5.6 billion years, has expanded to about 37 times the Sun's radius. From this enlarged photosphere, it is radiating 186 times the Sun's luminosity at an effective temperature of 4,126 K. It has a magnitude 12.02 visual companion at an angular separation of 209.30 arc seconds along a position angle of 298°, as of 2012.
Naming.
In Chinese, (), meaning "Outer Fence", refers to an asterism consisting of refers to an asterism consisting of μ Piscium, δ Piscium, ε Piscium, ζ Piscium, ν Piscium, ξ Piscium and α Piscium. Consequently, the Chinese name for μ Piscium itself is (, .)


NGC 3393

NGC 3393 is a barred spiral galaxy located in the constellation Hydra. It is located at a distance of circa 180 million light years from Earth, which, given its apparent dimensions, means that NGC 3393 is about 140,000 light years across. It was discovered by John Herschel on March 24, 1835. It is a Type II Seyfert galaxy. The galaxy is known to host two supermassive black holes, which are the nearest known pair of supermassive black holes to Earth.
Characteristics.
The galaxy is characterised as a barred spiral galaxy. At both ends of the bar HII regions are present. There is also evidence of a fainter inner bar. The fainter outer arms of the galaxy form a nearly complete ring.
Active galactic nucleus.
NGC 3393 has been characterised as a Seyfert galaxy, a galaxy category which features bright point-like nuclei. NGC 3393 is a type II Seyfert galaxy. Its X ray spectrum is more consistent with a Compton-thick cold reflection source, which means that the source is hidden behind dense material, mainly gas and dust, and the X-rays observed have been reflected.
Supermassive black holes.
The source of activity in the active galactic nuclei is a supermassive black hole (SMBH) lying at the centre of the galaxy. Observations by the Chandra X-Ray Observatory revealed evidence for a pair of supermassive black holes in the centre of NGC 3393. The observation in hard X-rays, including emission from iron, showed two separate peaks, which were identified as black holes that are actively growing, generating X-ray emission as gas falls towards the black holes and becomes hotter. The obscured regions around both black holes block the copious amounts of optical and ultraviolet light produced by infalling material. They are the first pair of black holes found in a spiral galaxy like our Milky Way. The two black holes are separated by only 490 light years.
The two black holes in NGC 3393 are likely the remnant of a merger of two galaxies of unequal mass a billion or more years ago. Other evidence that supports the hypothesis of the galaxy merger include high pre-shock densities in the narrow-line region and low O/H and Mg/H abundances. However the N/H is more than predicted, probably due to the creation of Wolf–Rayet stars in the central region of the galaxy during the merger.
The total mass of the pair is estimated to be between 21 and 35 million .
Supernova.
One supernova has been observed in NGC 3393, SN 2018aqi. The supernova was discovered by ASAS-SN on April 6, 2018, and had an apparent magnitude of 16.4 at discovery. By its spectrum, it was identified as a type Ia supernova 6 days before maximum brightness.
Nearby galaxies.
NGC 3393 is the brightest galaxy in the NGC 3393 group, which also includes NGC 3369, NGC 3383, and ESO 501-086. NGC 3463 has also been proposed to be a member of the group. The group is part of the Hydra Supercluster.


NGC 394

NGC 394 is a lenticular galaxy located in the constellation Pisces. It was discovered on October 26, 1854 by R. J. Mitchell. It was described by Dreyer as "faint, small, 50 arcsec northeast of II 218.", with II 218 being NGC 392.


Kepler-20

Kepler-20 is a star 929 light-years from Earth in the constellation Lyra with a system of six known planets. The apparent magnitude of this star is 12.51, so it cannot be seen with the unaided eye. Viewing it requires a telescope with an aperture of or more. It is slightly smaller than the Sun, with 94% of the Sun's radius and about 91% of the Sun's mass. The effective temperature of the photosphere is slightly cooler than that of the Sun at , giving it the characteristic yellow hue of a stellar class G8 star. The abundance of elements other than hydrogen or helium, what astronomers term the metallicity, is approximately the same as in the Sun. It may be older than the Sun, although the margin of error here is relatively large.
Planetary system.
On December 20, 2011, the Kepler Space Telescope team reported the discovery of a five-planet system containing three small gas giants and the first two Earth-sized extrasolar planets, Kepler-20e (the first known extrasolar planet smaller than Earth orbiting a main-sequence star) and Kepler-20f, orbiting a Sun-like star. Although the planets are Earth-sized, they are not Earth-like in the respect that they are much closer to their star than Earth, and are hence not near the habitable zone, with expected surface temperatures of and , respectively. The three other Neptune-sized planets in the system, Kepler-20b, Kepler-20c, and Kepler-20d, all orbit similarly close to the star. Kepler-20g is a non-transiting Neptunian world.
The masses of e and f are expected masses. Their masses are uncertain as they are too small to detect via radial velocity with current technology.
All planets are at small near resonances; proceeding outwards, they are 3:2, 4:2, 2:1, 4:1. The planetary orbits in current form are highly sensitive to perturbations caused by outer planets, therefore assuming stability, no additional gas giant planets can be located closer than 30 AU from the parent star.


NGC 4454

NGC 4454 is a barred spiral galaxy located about 123 million light-years away in the constellation of Virgo. NGC 4454 was discovered by astronomer William Herschel on April 17, 1784.


F Hydrae

F Hydrae, also known as HD 74395, is a star in the constellation Hydra with an apparent magnitude is 4.64. It was catalogued as 31 Monocerotis, but this name is now rarely used since the star is now within the boundaries of Hydra. It is a low mass yellow supergiant around a thousand times brighter than the sun and five times as massive.
F Hya is a catalogued as a triple star, with 8th magnitude BD-06°2707 80" away and 13th magnitude companion at 57".


V344 Carinae

V344 Carinae is a single star in the southern constellation of Carina. It has the Bayer designation f Carinae, while "V344 Carinae" is its variable star designation. This star has a blue-white hue and is visible to the naked eye with an apparent visual magnitude that fluctuates around 4.50. Historically, it was mentioned in the "Almagest", suggesting that some time around 130 BCE it was brighter than its current magnitude. This object is located at a distance of approximately 610 light years from the Sun based on parallax. The star is drifting further away with a radial velocity of around +27 km/s.
This is a B-type main-sequence star with a stellar classification of B3V(n). It is a Be star; a rapidly-rotating star that is hosting a circumstellar disk of hot, decreted gas. It is a photometrically variable Be star, having a brightness that ranges from 4.4 down to 4.51 in visual magnitude, and has been classified as a Gamma Cassiopeiae variable. The star is 32 million years old and is spinning with a projected rotational velocity of 268 km/s. It has seven times the mass of the Sun and around 3.0 times the Sun's radius. The star is radiating 2,328 times the luminosity of the Sun from its photosphere at an effective temperature of 17,660 K.


HIP 56948

HIP 56948 (also known as HD 101364) is a solar twin star of type G5V. It is one of the most sun-like stars yet known in terms of size, mass, temperature, and chemical makeup. Our sun is about 4.6 billion years old, and HIP 56948 is believed to be about 7.1 billion years old. Both stars are between a third and a halfway through their life on the main sequence.
It is 208 light years away in the constellation of Draco, lying about halfway between Polaris and Dubhe on the celestial sphere. Astronomers have looked for planets in the system, so far without finding any. These observations suggest that the star does not have any hot Jupiters.
Jorge Meléndez of the Australian National University and Iván Ramírez of the University of Texas analysed the star in 2007 using the 2.7 metre Harlan J. Smith telescope at McDonald Observatory.
Most other solar analogs such as 18 Scorpii are unlike the sun in that they have several times the lithium abundance. HIP 56948 is among the best candidates for a solar twin because of the known possible contenders, its lithium abundance most resembles that of our own star. A 2009 high-dispersion spectroscopic study from the Astronomical Society of Japan confirms this.
In the abstract to their paper, the star's discoverers say:


NGC 5754

NGC 5754 is a barred spiral galaxy located 218 million light years away in the constellation Boötes. It is a member of the Arp 297 interacting galaxies group, which consists of NGC 5752, NGC 5753, NGC 5754, NGC 5755. Along with NGC 2718 and UGC 12158, NGC 5754 is often considered a Milky Way-twin.


Kappa Ursae Majoris

Kappa Ursae Majoris (κ Ursae Majoris, abbreviated Kappa UMa, κ UMa) is a binary star in the constellation of Ursa Major. With a combined apparent magnitude of +3.60, the system is approximately 358 light-years from Earth.
The two components are designated Kappa Ursae Majoris A (officially named Alkaphrah , a traditional name of the system) and B.
Nomenclature.
"κ Ursae Majoris" (Latinised to "Kappa Ursae Majoris") is the system's Bayer designation. The designations of the two components as "Kappa Ursae Majoris A" and "B" derives from the convention used by the Washington Multiplicity Catalog (WMC) for multiple star systems, and adopted by the International Astronomical Union (IAU).
The traditional name of the system is Alkafzah (corrupted to "Alkaphrah" or "El Koprah"), from the Arabic القفزة "al-qafzah" "the leap". (Cf. Alula Borealis and Alula Australis.)
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 "Alkaphrah" for the component Kappa Ursae Majoris A on 5 September 2017 and it is now so included in the List of IAU-approved Star Names.
In Chinese, (), meaning "Three Steps", refers to an asterism consisting of Kappa Ursae Majoris, Iota Ursae Majoris, Lambda Ursae Majoris, Mu Ursae Majoris, Nu Ursae Majoris and Xi Ursae Majoris. Consequently, the Chinese name for Kappa Ursae Majoris itself is (, ).
Properties.
Both components of the binary star are white A-type main sequence dwarfs. They have apparent magnitudes of +4.2 and +4.5. The orbital period of the binary is 35.6 years (13,007.2 days), and the two stars are separated by 0.18 arcseconds. An infrared excess indicates a debris disk with a mean temperature of 165 K is orbiting the primary at a separation of .


HD 330075

HD 330075 is a star in the southern constellation of Norma. It has a yellow hue and an apparent visual magnitude of 9.36, which makes it too faint to be seen with the naked eye – it is visible only with telescope or powerful binoculars. Parallax measurements provide a distance estimate of 148 light years from the Sun, and it is drifting further away with a radial velocity of 62 km/s. The star is estimated to have come as close as some 409 million years ago.
This object appears to be a slightly evolved dwarf with a spectral class of G5. That is, it is nearing the end of its main sequence lifetimes and is becoming a subgiant star. The star has very low chromospheric activity and is around five billion years old. It is smaller than the Sun with 86% of the Sun's mass and 85% of the solar radius. As a consequence, it is radiating just 39% of the luminosity of the Sun from its photosphere at an effective temperature of 4,967 K. It has a super-solar metallicity, which means the abundance of elements other than hydrogen and helium appears much higher than in the Sun.
Planetary system.
In 2004, the discovery of a hot Jupiter planet orbiting close to the star was announced. This is the first planet discovered by the then-new HARPS spectrograph.


40 Persei

40 Persei is a wide binary star system in the northern constellation of Perseus. It has the Bayer designation ο Persei, while "40 Persei" is the Flamsteed designation. The system is visible to the naked eye as a faint, blue-white hued point of light with an apparent visual magnitude of 4.97. It is located approximately 1060 light years away from the Sun based on parallax, and is drifting further away with a radial velocity of +22 km/s. The system is a member of the Perseus OB2 association of co-moving stars.
The primary component is a massive B-type main-sequence star with a stellar classification of B0.5V. It is about 7.2 million years old and has a very low projected rotational velocity for an early B-type star, measured at 10 km/s. This star has 12.5 times the mass of the Sun and is radiating 936 times the Sun's luminosity from its photosphere at an effective temperature of 29,330 K. The companion is magnitude 10.04, A-type main-sequence star with a class of A1Vn, and is located at an angular separation of from the primary.


NGC 282

NGC 282 is an elliptical galaxy in the constellation Pisces. It was discovered on October 13, 1879 by Édouard Stephan.


NGC 5999

NGC 5999 is an open cluster in the constellation Norma. Its brightest star is HIP 78355. It is 5310 light-years distant and thought to be around 400 million years old.


NGC 2294

NGC 2294 is an elliptical galaxy within the constellation Gemini, discovered by George Johnstone Stoney on February 22, 1849. The visual magnitude is 14, and the apparent size is 0.8 by 0.4 arc minutes.


53 Ophiuchi

53 Ophiuchi is a multiple star system in the equatorial constellation of Ophiuchus. It is visible to the naked eye as a faint star with a combined apparent visual magnitude of 5.80. Located around 370 light years distant from the Sun based on parallax, it is moving closer to the Earth with a heliocentric radial velocity of −14 km/s. As of 2011, the visible components had an angular separation of along a position angle of 190°. The primary may itself be a close binary system with a separation of and a magnitude difference of 3.97 at an infrared wavelength of .
The magnitude 5.82 primary, designated component Aa, is an A-type main-sequence star with a stellar classification of A2 V. It has 2.5 times the mass of the Sun and about 1.7 times the Sun's radius. The star is radiating 56 times the Sun's luminosity from its photosphere at an effective temperature of 9,311 K. The widely spaced secondary, designated component B, is a magnitude 7.8 A-type subgiant star with a class of A8 IV.


NGC 400

NGC 400 is a star located in the constellation of Pisces. It was discovered on December 30, 1866 by Robert Ball.


AE Pictoris

AE Pictoris is an eclipsing binary star system in the southern constellation of Pictor. This dim, blue-white hued point of light is just barely visible to the naked eye; it has an apparent visual magnitude of 6.09, which drops to magnitude 6.14 during an eclipse. The system is located around 1,430 light years away from the Sun based on parallax, and it is receding with a radial velocity of 34 km/s.
This is a single-lined spectroscopic binary system with an orbital period of 2.97 days and an eccentricity of 0.10. The minimum value of the semimajor axis for the pair is . It is classed as a probable eclipsing binary variable (EB:), but with some uncertainty regarding the specific type. This is a candidate runaway star system, having a peculiar velocity of relative to its neighbors. The visible component is a B-type main-sequence star with a stellar classification of B3V. it is 28 million years old with seven times the mass of the Sun. The star is radiating 2,569 times the luminosity of the Sun from its photosphere at an effective temperature of 18,700 K.


Rho Cephei

The Bayer designation Rho Cephei (ρ Cephei / ρ Cep) is shared by two stars in the constellation Cepheus:


NGC 7303

NGC 7303 is a barred spiral galaxy around 170 million light-years from Earth in the constellation Pegasus. NGC 7303 was discovered by astronomer John Herschel on September 15, 1828.


HD 222399

HD 222399 is a double star in the northern constellation of Andromeda. The magnitude 6.57 primary is an F-type subgiant star with a stellar classification of F2IV. It has a magnitude 10.57 companion at an angular separation of 14.7″ along a position angle of 162° (as of 2002).


Delta Delphini

Delta Delphini, Latinized from δ Delphini, is a binary star in the northern constellation of Delphinus. It is visible to the naked eye with an apparent visual magnitude of 4.43. Based upon an annual parallax shift of 14.61 mas as seen from the Earth, the system is located about 223 light years from the Sun.
This is a double-lined spectroscopic binary system with an orbital period of 40.58 days. The two components are nearly identical chemically peculiar stars, having a combined stellar classification of kA7hF0mF0(IV-V). This notation indicates the calcium K line matches an A7 star, the hydrogen lines an F0 star, and the metal lines an F0 star. Each of the stars is a Delta Scuti variable, with the system having a dominant period of 0.1568 days and an amplitude of 0.0700 in magnitude. Delta Delphini forms the prototype of a class of metal-lined δ Scuti subgiant or giant stars.


66 Cancri

66 Cancri is a binary star system near the northern border of the zodiac constellation of Cancer, located 474 light years away from the Sun. It is visible to the naked eye as a faint, white-hued star with a combined apparent visual magnitude of 5.87. The pair are moving closer to the Earth with a heliocentric radial velocity of −13 light years. As of 2003, the magnitude 8.56 companion was located at an angular separation of along a position angle of 134° from the primary.
The brighter member of the system, designated component A, is an A-type main-sequence star with a stellar classification of A2 V. It is around 162 million years old with a high rate of spin, showing a projected rotational velocity of 183 km/s. Estimates of the mass of the star range from 1.7 up to 2.73 times the mass of the Sun. It is radiating 96 times the Sun's luminosity from its photosphere at an effective temperature of 8,974 K.


NGC 3738

NGC 3738 is a dwarf galaxy in the constellation of Ursa Major and belongs to the M81 Group of galaxies. NGC 3738 is 12 million light-years from the sun. The galaxy was first discovered by astronomer William Herschel in 1789. NGC 3738 is a blue compact dwarf, which is small compared to large spiral galaxies. The galaxy is about 10,000 light-years across. It is one-tenth the size of the Milky Way
Blue compact dwarf galaxies are blue in appearance because of the large cluster of hot massive stars. The galaxies are relatively dim and appear to be irregular in shape. They are typically chaotic in appearance.


27 Vulpeculae

27 Vulpeculae is a single, blue-white star in the northern constellation of Vulpecula. It is a dim star, visible to the naked eye, with an apparent visual magnitude of 5.59. An annual parallax shift of provides a distance estimate of about 306 light years. It is moving closer with a heliocentric radial velocity of −22 km/s, and will make perihelion passage at a distance of around in 3.75 million years.
This is a B-type main-sequence star with a stellar classification of B9 V. It is spinning rapidly, showing a projected rotational velocity of 335. The star has an estimated 2.77 times the mass of the Sun and about 3.1 times the Sun's radius. It is radiating 75 times the Sun's luminosity from its photosphere at an effective temperature of 10,789 K.


20 Puppis

20 Puppis is a solitary star in the southern constellation of Puppis. It is visible to the naked eye as a faint, yellow-hued star with an apparent visual magnitude of 4.99. The star lies approximately 990 light years away from the Sun based on parallax. It is receding from the Earth with a heliocentric radial velocity of +16.8 km/s.
This object has a stellar classification of G4 Ib-II, matching a G-type star with a luminosity class part way between a bright giant and a supergiant star. It is just 90 million years old with around five times the mass of the Sun. The star has expanded to 48 times the Sun's radius and is radiating 1,087 times as much luminosity as the Sun from its enlarged photosphere at an effective temperature of 4,804 K.


47 Aurigae

47 Aurigae is a star located around 680 light years away from the Sun in the northern constellation of Auriga. It is visible to the naked eye as a dim, orange-hued star with an apparent visual magnitude of 5.88. This object is moving closer to the Earth with a heliocentric radial velocity of −48 km/s, and is expected to come to within in around 3.6 million years.
This object is an aging giant star with a stellar classification of K4 III, having exhausted the hydrogen supply at its core then expanded to 36 times the Sun's radius. It is roughly two billion years old with 1.4 times the mass of the Sun. The star is radiating 358 times the luminosity of the Sun from its swollen photosphere at an effective temperature of 4,157 K.


S62 (star)

S62 is a star in the cluster surrounding Sagittarius A* (Sgr A*), the supermassive black hole in the center of the Milky Way. S62 orbits Sgr A* faster than any other star known as of August 2019. With an orbital period of only 9.9 years, it beats the previous record holder, the star S55, which circles Sgr A* in 12.8 years.
In addition, S62 has a highly eccentric orbit which makes it pass very close to Sgr A*, only , less than the distance between Uranus and the Sun. The star therefore passes only about 215 times the Schwarzschild radius of Sgr A* (the Schwarzschild radius of Sgr A* is approximately 0.082 AU, or 12 million km). It is closer to Sgr A* than the previous record, around 45 AU (6.7 billion km, 550 Schwarzschild radii) held by the star S175, and much closer than the more well-studied S2 (118 AU, 18 billion km, 1,440 Schwarzschild radii).
S62 passes so close to Sgr A* that its orbit has a very large precession: its orbit shifts by about 10° with each revolution. At closest approach its velocity is about 0.10c (10% of the speed of light) relative to Sgr A*. S62's next approach to Sgr A* is towards the end of 2022.
The discovery of S62 improved the bounds on the mass distribution in the center of the galactic center, showing that are concentrated within 16 AU of the center, fully compatible with Sgr A* being a supermassive black hole.


Kepler-39

Kepler-39 (2MASS J19475046+4602034) is an F-type main sequence star located in the constellation Cygnus. It is located about 3,560 light-years (1,090 parsecs) away. One known substellar companion orbits it, Kepler-39b.
Planetary system.
Kepler-39b is generally considered a brown dwarf rather than a planet since it does not meet the standard definition of planet. Some authorities such as the Extrasolar Planets Encyclopaedia and the NASA Exoplanet Archive include it among their list of confirmed planets.


NGC 2950

NGC 2950 is a lenticular galaxy in Ursa Major about 60 million light years from the Milky Way. It was discovered in 1790 by the Anglo-German astronomer William Herschel.
NGC 2950 is a field galaxy, it is not part of a galaxy cluster or galaxy group, and thus is gravitationally isolated. Measures that do not rely on redshift give a distance of 18,733 ± 3,210 Mpc (∼61,1 million astronomical units), which is within the distance calculated by redshift.
NGC 2950 hosts two nested stellar bars; the rotation frequency of the secondary bar is higher than that of the primary one.


Shravana

Shravana is the 22nd "nakshatra" (Devanagari नक्षत्र) or "lunar mansion" as used in Hindu astronomy, Hindu calendar and Hindu astrology. It belongs to the constellation Makara (Devanagari: मकर) or Capricorn.
Traditional Hindu given names are determined by which pada (quarter) of a nakshatra the Ascendant/Lagna was in at the time of birth. In the case of Shravana Nakshatra, the given name would begin with the following syllables:


A Velorum

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


Kepler-26e

Kepler-26e is an exoplanet orbiting the star Kepler-26, located in the constellation Lyra. It was discovered by the "Kepler" telescope in February 2014. It orbits its parent star at only 0.220 astronomical units and completes an orbit once every 46.8 days. It is potentially habitable.


Copeland Septet

Copeland Septet (also Copeland's Septet, Hickson Compact Group 57) is a group of galaxies in the constellation Leo that includes NGC 3748, NGC 3754, NGC 3750, NGC 3751, NGC 3745, NGC 3753 and NGC 3746. The group was discovered by British astronomer Ralph Copeland in 1874. The location of Copeland's Septet is R.A. 11h 38m / Decl. +22° (2000.0), about three degrees northwest of third magnitude star 93 Leonis.


Delta Fornacis

Delta Fornacis, Latinized from δ Fornacis, is a solitary, blue-white hued star near the middle of the southern constellation of Fornax. With an apparent visual magnitude of 5.00, it is faintly visible to the naked eye at night. The star has an annual parallax shift of , indicating it lies at a distance of approximately 790 light years from the Sun. It is drifting further away with a radial velocity of +26 km/s.
The stellar classification of Delta Fornacis is B5 III, matching an evolved B-type giant star. It has an angular diameter of , which, at the estimated distance of the star, yields a physical size of around 6 times the radius of the Sun. Around 63 million years old, the star is spinning rapidly with a projected rotational velocity of 185 km/s. It has an estimated 5.9 times the Sun's mass and radiates 1,291 times the solar luminosity from its outer atmosphere at an effective temperature of 16,230 K.
References.
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