| 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.
