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Iota Serpentis
	Location of ι Serpentis (circled)
Observation data; Epoch J2000 Equinox J2000
Constellation	Serpens
Right ascension	15h 41m 33.05469s
Declination	19° 40′ 13.4380″
Apparent magnitude (V)	4.51
Characteristics
Evolutionary stage	main sequence
Spectral type	B9V + A1V
B−V color index	+0.062±0.003
Astrometry
Radial velocity (Rv)	−17.20 km/s
Proper motion (μ)	RA: -60.86 mas/yr ; Dec.: -43.69 mas/yr
Parallax (π)	17.16 ± 0.67 mas
Distance	190 ± 7 ly ; (58 ± 2 pc)
Absolute magnitude (MV)	+0.69
Orbit
Period (P)	8015.0±6.3 d
Semi-major axis (a)	0.21033±0.00047″
Eccentricity (e)	0.0941±0.0028
Inclination (i)	83.608±0.043°
Longitude of the node (Ω)	69.684±0.033°
Periastron epoch (T)	54,180±33 HMJD
Argument of periastron (ω); (secondary)	80.5±1.8°
Details
A
Mass	1.999 M☉
B
Mass	1.984 M☉
Other designations
	ι Ser, 21 Serpentis, BD+20° 3138, GC 21102, HD 140159, HIP 76852, HR 5842, SAO 101682, ADS 9744, CCDM J15416+1940
Database references
SIMBAD	data

ι Serpentis, Latinized as Iota Serpentis and abbreviated Iot Ser, is a triple star^[7] system in the constellation Serpens, in its head (Serpens Caput). It is approximately 190 light years from Earth.^[1]

At the centre of the system is a spectroscopic binary, Iota Serpentis A and B. These are both white main sequence dwarfs and both have apparent magnitudes of +5.3. This binary has an orbital period variously reported as 11^[8] or 22^[5] years. First discovered as an astrometric binary, the pair have now been resolved and visual orbits have been derived.^[5]

There are two visual companions, Iota Serpentis C, a 13th magnitude star 143 arcseconds away and Iota Serpentis D, a 12th magnitude star 151 arcseconds distant.

References

^ ^a ^b ^c ^d ^e ^f van Leeuwen, F. (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. S2CID 18759600. Vizier catalog entry
^ ^a ^b ^c 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, S2CID 119257644.
^ ^a ^b ^c Martin, C.; et al. (1998). "Mass determination of astrometric binaries with Hipparcos. III. New results for 28 systems". Astronomy and Astrophysics Supplement. 133 (2): 149. Bibcode:1998A&AS..133..149M. doi:10.1051/aas:1998459.
^ Evans, D. S. (June 20–24, 1966). "The Revision of the General Catalogue of Radial Velocities". In Batten, Alan Henry; Heard, John Frederick (eds.). Determination of Radial Velocities and their Applications, Proceedings from IAU Symposium no. 30. Vol. 30. University of Toronto: International Astronomical Union. p. 57. Bibcode:1967IAUS...30...57E.
^ ^a ^b ^c Muterspaugh, Matthew W.; et al. (2010). "The Phases Differential Astrometry Data Archive. II. Updated Binary Star Orbits and a Long Period Eclipsing Binary". The Astronomical Journal. 140 (6): 1623–1630. arXiv:1010.4043. Bibcode:2010AJ....140.1623M. doi:10.1088/0004-6256/140/6/1623. S2CID 6030289.
^ "iot Ser". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2019-09-09.
^ Eggleton, P. P.; Tokovinin, A. A. (September 2008), "A catalogue of multiplicity among bright stellar systems", Monthly Notices of the Royal Astronomical Society, 389 (2): 869–879, arXiv:0806.2878, Bibcode:2008MNRAS.389..869E, doi:10.1111/j.1365-2966.2008.13596.x, S2CID 14878976.
^ van den Bos, W. H. (1965). "Note on the Double Star Iota Serpentis". Monthly Notes of the Astronomical Society of Southern Africa. 24: 123. Bibcode:1965MNSSA..24..123V.