Gamma1 Caeli

Gamma1 Caeli

Location of γ1 Caeli
Observation data
Epoch J2000      Equinox J2000
Constellation Caelum
Right ascension 05h 04m 24.40218s[1]
Declination −35° 28′ 58.7161″[1]
Apparent magnitude (V) 4.55[2]
Characteristics
Spectral type K2.5IIIb + G8IV[3]
U−B color index +1.20[4]
B−V color index +1.20[4]
Astrometry
Radial velocity (Rv)9.7 ± 2[5] km/s
Proper motion (μ) RA: 126.17[1] mas/yr
Dec.: −43.67[1] mas/yr
Parallax (π)17.99 ± 0.40[1] mas
Distance181 ± 4 ly
(56 ± 1 pc)
Absolute magnitude (MV)+0.83[6]
Other designations
γ1 Cae, CD−35° 2089, GC 6212, HD 32831, HIP 23595, HR 1652, SAO 195532, CCDM J05044-3529
Database references
SIMBADdata

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

References

  1. 1 2 3 4 5 van Leeuwen, F.; et al. (2007). "Validation of the new Hipparcos reduction". Astronomy and Astrophysics. 474 (2): 653–664. arXiv:0708.1752. Bibcode:2007A&A...474..653V. doi:10.1051/0004-6361:20078357.
  2. ↑ Ducati, J. R. (2002). "VizieR Online Data Catalog: Catalogue of Stellar Photometry in Johnson's 11-color system". CDS/ADC Collection of Electronic Catalogues. 2237. Bibcode:2002yCat.2237....0D.
  3. ↑ Corbally, C. J. (1984). "Close visual binaries. I - MK classifications". The Astrophysical Journal Supplement Series. 55: 657. Bibcode:1984ApJS...55..657C. doi:10.1086/190973.
  4. 1 2 Johnson, H. L. (1966). "UBVRIJKL Photometry of the Bright Stars". Communications of the Lunar and Planetary Laboratory. 4: 99. Bibcode:1966CoLPL...4...99J.
  5. ↑ Wilson, Ralph Elmer (1953). "General catalogue of stellar radial velocities". Washington. Bibcode:1953GCRV..C......0W.
  6. ↑ Anderson, E.; Francis, Ch. (2012), "XHIP: An extended hipparcos compilation", Astronomy Letters, 38 (5): 331, arXiv:1108.4971, Bibcode:2012AstL...38..331A, doi:10.1134/S1063773712050015.


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