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Kappa2 Sagittarii (κ2 Sagittarii) is a binary star system in the zodiac constellation of Sagittarius. It is visible to the naked eye with a combined apparent visual magnitude of +5.64. Based upon an annual parallax shift of 10.47 mas as seen from Earth, this system is located around 310 light years from the Sun. They are receding with a radial velocity of +2.6 km/s.
Epsilon Sculptoris is a binary star in the constellation Sculptor. It is approximately 91.7 light years from Earth.
Kappa1 Sculptoris is a binary star system in the southern constellation of Sculptor. It is faintly visible to the naked eye, with a combined apparent visual magnitude of +5.51. Based upon an annual parallax shift of 12.91 mas as measured from Earth, it is located roughly 250 light years from the Sun.
Gamma Sextantis, Latinized as γ Sextantis, is a binary star system in the equatorial constellation of Sextans. The combined apparent visual magnitude of the system is 5.05, which means it is faintly visible to the naked eye. The annual parallax shift is 11.75 mas, indicating a distance of around 280 light years.
Iota Trianguli Australis is a binary star system in the constellation Triangulum Australe. It is visible to the naked eye with a combined apparent visual magnitude of +5.27. Based upon an annual parallax shift of 25.77 mas as seen from the Earth, it is located around 127 light years from the Sun. The system appears to be moving closer to the Sun with a radial velocity of around −6 km/s.
Theta Volantis, Latinized from θ Volantis, is a solitary star in the southern constellation of Volans. Based upon parallax measurements, is approximately 240 light years from the Sun. It has an apparent visual magnitude of 5.19, which is bright enough to be faintly visible to the naked eye.
48 Cassiopeiae is a triple star system in the northern constellation of Cassiopeia. It is visible to the naked eye with a combined apparent visual magnitude of 4.49. With an annual parallax shift of 28.36±0.44 mas as seen from Earth's orbit, it is located approximately 115 light years away. The system is moving closer with a heliocentric radial velocity of −12.4 km/s.
38 Lyncis is a multiple star system in the northern constellation of Lynx. It located about 125 light-years from the Sun, based on parallax.
HR 3082 is a double star in the northern circumpolar constellation of Camelopardalis. It is faintly visible to the naked eye with an apparent visual magnitude of 5.39. The system is moving closer to the Sun with a heliocentric radial velocity of +2.7 km/s. It is currently at a distance of around 323 light years, based upon an annual parallax shift of 10.10±0.24 mas.
HD 21447 is a probable binary star system located in the constellation Camelopardalis. The star is also known as HR 1046. It can be viewed with the naked eye, having an apparent visual magnitude of 5.09. Based upon an annual parallax shift of 16.42±0.29 mas, it is located some 199 light years from the Sun. It is a candidate for membership in the Ursa Major Moving Group.
Theta Piscis Austrini, Latinized as θ Piscis Austrini, is a binary star system in the southern constellation of Piscis Austrinus. It is faintly visible to the naked eye with a combined apparent visual magnitude of +5.01. Based upon an annual parallax shift of 10.16 mas as seen from the Earth, the system is located around 320 light years from the Sun. The system is drifting further away with a radial velocity of +13 km/s.
Delta Horologii is a binary star system in the constellation Horologium. It is visible to the naked eye with a combined apparent visual magnitude of 4.93. As of 2014, the pair had an angular separation of 0.20 arc seconds along a position angle of 24°. Based upon an annual parallax shift of 18.24 mas as seen from Earth, it is located 179 ± 4 light years from the Sun.
Tau1 Hydrae is a triple star system in the equatorial constellation of Hydra. Based upon the annual parallax shift of the two visible components as seen from Earth, they are located about 18 parsecs (59 ly) from the Sun. The system has a combined apparent visual magnitude of +4.59, which is bright enough to be visible to the naked eye at night.
Theta Indi is a binary star in the constellation Indus. Its apparent magnitude is 4.40 and it is approximately 98.8 light years away based on parallax. The smaller companion, B, has a spectral type of G0V and an apparent magnitude of 7.18 at a separation of 6.71". Recent observations suggest the primary is itself a binary with components Aa and Ab orbiting at 0.0617", estimated period about 1.3 years.
ξ Oph, Latinized as Xi Ophiuchi, is a visual binary star system in the equatorial constellation of Ophiuchus. It has a yellow-white hue and is faintly visible to the naked eye with a combined apparent visual magnitude of 4.39. The system is located approximately 56.6 light years away from the Sun based on parallax, but is drifting closer with a radial velocity of -9 km/s.
34 Persei is a binary star system in the northern constellation of Perseus. It is visible to the naked eye as a faint, blue-white hued point of light with a combined apparent visual magnitude of 4.67. The system is located approximately 540 light years away from the Sun based on parallax, but it is drifting closer with a radial velocity of −3.5 km/s. It is a likely member of the Alpha Persei Cluster.
52 Sagittarii is a binary star system in the southern constellation of Sagittarius. It has the Bayer designation h2 Sagittarii, while 52 Sagittarii is the Flamsteed designation. This system is visible to the naked eye as a faint, blue-white hued point of light with an apparent visual magnitude of 4.59. It is located approximately 190 light years away based on parallax, but is drifting closer with a radial velocity of −19 km/s.
43 Persei is a binary star system in the northern constellation Perseus. It is visible to the naked eye as a dim, yellow-white hued star with an apparent visual magnitude of 5.28. The system is located around 38.5 parsecs (125.4 ly) distant from the Sun, based on parallax.
Sigma2 Gruis is a binary star system in the southern constellation of Grus. Its apparent visual magnitude is 5.86. The pair had an angular separation of 2.7 arc seconds along a position angle of 265°, as of 1991. Located around 215 ly (66 pc) distant, the white-hued primary component is an A-type main-sequence star of spectral type A1V, a star that is currently fusing its core hydrogen.
HD 24141, also known as HR 1192, is a star located in the northern constellation Camelopardalis, the giraffe. It is faintly visible to the naked eye as a white-hued point of light with an apparent magnitude of 5.79. The object is located relatively close at a distance of 176 light-years based on Gaia DR3 parallax measurements and it is slowly drifting closer with a heliocentric radial velocity of −0.2 km/s. At its current distance, HD 24141's brightness is diminished by 0.17 magnitudes due to interstellar extinction and it has an absolute magnitude of +2.28.
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