Iota Pictoris
| Observation data Epoch J2000.0 Equinox J2000.0 (ICRS) | |
|---|---|
| Constellation | Pictor |
| ι Pic A | |
| Right ascension | 04h 50m 55.32684s[1] |
| Declination | −53° 27′ 41.2300″[1] |
| Apparent magnitude (V) | 5.63[2] |
| ι Pic B | |
| Right ascension | 04h 50m 56.49825s[1] |
| Declination | −53° 27′ 34.9159″[1] |
| Apparent magnitude (V) | 6.47[2] |
| Characteristics | |
| ι Pic A | |
| Spectral type | F0 V[2] |
| U−B color index | 0.06[2] |
| B−V color index | 0.32[2] |
| ι Pic B | |
| Spectral type | F4 V[2] |
| B−V color index | 0.37[2] |
| Astrometry | |
| ι Pic A | |
| Radial velocity (Rv) | 8.6±3.4[3] km/s |
| Proper motion (μ) | RA: −98.707[1] mas/yr Dec.: +80.769[1] mas/yr |
| Parallax (π) | 24.9211 ± 0.1559 mas[1] |
| Distance | 130.9 ± 0.8 ly (40.1 ± 0.3 pc) |
| Absolute magnitude (MV) | 2.50[2] |
| ι Pic B | |
| Radial velocity (Rv) | 23.3±1.0[3] km/s |
| Proper motion (μ) | RA: −98.707[1] mas/yr Dec.: +66.139[1] mas/yr |
| Parallax (π) | 25.6610 ± 0.4106 mas[1] |
| Distance | 127 ± 2 ly (39.0 ± 0.6 pc) |
| Absolute magnitude (MV) | 3.30[2] |
| Details | |
| ι Pic A | |
| Mass | 1.51[4] M☉ |
| Radius | 1.80+0.23 −0.11[1] R☉ |
| Luminosity | 7.2±0.1[1] L☉ |
| Surface gravity (log g) | 4.28±0.14[4] cgs |
| Temperature | 7,331±249[4] K |
| Age | 696[4] Myr |
| ι Pic B | |
| Mass | 2.76[4] M☉ |
| Radius | 1.48+0.04 −0.06[1] R☉ |
| Luminosity | 3.4±0.06[1] L☉ |
| Surface gravity (log g) | 4.24±0.14[4] cgs |
| Temperature | 6,435±219[4] K |
| Age | 516[4] Myr |
| Other designations | |
| ι Pic A: HD 31203, HIP 22531, HR 1563, SAO 233709 | |
| ι Pic B: HD 31204, HIP 22534, HR 1564, SAO 233710 | |
| Database references | |
| SIMBAD | data |
ι Pictoris, Latinized from Iota Pictoris, is a suspected multiple star system[6] in the southern Pictor constellation. It is visible to the naked eye as a dim, yellow-white-hued point of light with a combined apparent visual magnitude of 5.28.[6] The two resolvable components have an angular separation of 8.2 arcseconds, equivalent to a physical projected separation of around 450 AU.[7] They are located at a distance of around 127–131 light-years from the Sun, based on parallax.[1]
The two visible components appear as F-type main-sequence stars: the magnitude 5.63 component A has a stellar classification of F0 V, while the cooler, fainter secondary is of class F4 V.[2] Both are themselves are suspected spectroscopic binary stars consisting of roughly equal components.[6] Component B actually has a higher estimated mass than Component A, although the radius of B is smaller. They are both more luminous than the Sun, and have an estimated age of around 500–600 million years.[4]
References
- ^ a b c d e f g h i j k l m n o Brown, A. G. A.; et al. (Gaia collaboration) (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics. 616. A1. arXiv:1804.09365. Bibcode:2018A&A...616A...1G. doi:10.1051/0004-6361/201833051.
- ^ a b c d e f g h i j Corbally, C. J. (1984), "Close visual binaries. I - MK classifications", Astrophysical Journal Supplement Series, 55: 657, Bibcode:1984ApJS...55..657C, doi:10.1086/190973.
- ^ a b de Bruijne, J. H. J.; Eilers, A.-C. (October 2012), "Radial velocities for the HIPPARCOS-Gaia Hundred-Thousand-Proper-Motion project", Astronomy & Astrophysics, 546: 14, arXiv:1208.3048, Bibcode:2012A&A...546A..61D, doi:10.1051/0004-6361/201219219, S2CID 59451347, A61.
- ^ a b c d e f g h i David, Trevor J.; Hillenbrand, Lynne A. (2015), "The Ages of Early-Type Stars: Strömgren Photometric Methods Calibrated, Validated, Tested, and Applied to Hosts and Prospective Hosts of Directly Imaged Exoplanets", The Astrophysical Journal, 804 (2): 146, arXiv:1501.03154, Bibcode:2015ApJ...804..146D, doi:10.1088/0004-637X/804/2/146, S2CID 33401607.
- ^ "iot Pic". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2017-06-21.
{{cite web}}: CS1 maint: postscript (link) - ^ a b c 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.
- ^ Tokovinin, Andrei; et al. (August 2010), "Subsystems in Nearby Solar-type Wide Binaries", The Astronomical Journal, 140 (2): 510–517, arXiv:1006.1253, Bibcode:2010AJ....140..510T, doi:10.1088/0004-6256/140/2/510, S2CID 73629363.
