Astronomy:Iota Pictoris
| Observation data {{#ifeq:J2000.0|J2000.0 (ICRS)|Epoch J2000.0 Equinox J2000.0 (ICRS)| [[History:Epoch|Epoch J2000.0]] [[Astronomy:Equinox (celestial coordinates)|Equinox J2000.0}} | |
|---|---|
| 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[1] mas |
| 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[1] mas |
| 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: {{{names1}}} | |
| ι Pic B: {{{names2}}} | |
| 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 astronomical unit|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
- ↑ 1.00 1.01 1.02 1.03 1.04 1.05 1.06 1.07 1.08 1.09 1.10 1.11 1.12 1.13 1.14 Brown, A. G. A. (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics 616: A1. doi:10.1051/0004-6361/201833051. Bibcode: 2018A&A...616A...1G.
- ↑ 2.0 2.1 2.2 2.3 2.4 2.5 2.6 2.7 2.8 2.9 Corbally, C. J. (1984), "Close visual binaries. I - MK classifications", Astrophysical Journal Supplement Series 55: 657, doi:10.1086/190973, Bibcode: 1984ApJS...55..657C.
- ↑ 3.0 3.1 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, doi:10.1051/0004-6361/201219219, A61, Bibcode: 2012A&A...546A..61D.
- ↑ 4.0 4.1 4.2 4.3 4.4 4.5 4.6 4.7 4.8 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, doi:10.1088/0004-637X/804/2/146, Bibcode: 2015ApJ...804..146D.
- ↑ "iot Pic". SIMBAD. Centre de données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=iot+Pic.
- ↑ 6.0 6.1 6.2 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, doi:10.1111/j.1365-2966.2008.13596.x, Bibcode: 2008MNRAS.389..869E.
- ↑ Tokovinin, Andrei et al. (August 2010), "Subsystems in Nearby Solar-type Wide Binaries", The Astronomical Journal 140 (2): 510–517, doi:10.1088/0004-6256/140/2/510, Bibcode: 2010AJ....140..510T.
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