Iota Pavonis
| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| Constellation | Pavo |
| Right ascension | 18h 10m 26.15370s[1] |
| Declination | −62° 00′ 07.9922″[1] |
| Apparent magnitude (V) | 5.47[2] |
| Characteristics | |
| Spectral type | G0V[3] |
| Apparent magnitude (B) | 6.07[4] |
| Apparent magnitude (J) | 4.43±0.31[5] |
| Apparent magnitude (H) | 4.02±0.24[5] |
| Apparent magnitude (K) | 4.130±0.266[5] |
| Astrometry | |
| Radial velocity (Rv) | 30.20±0.14[6] km/s |
| Proper motion (μ) | RA: −76.952±0.159 mas/yr[1] Dec.: 222.452±0.188 mas/yr[1] |
| Parallax (π) | 56.1961±0.2674 mas[1] |
| Distance | 58.0 ± 0.3 ly (17.79 ± 0.08 pc) |
| Absolute magnitude (MV) | 4.24±0.02[7] |
| Orbit[8] | |
| Period (P) | 8304.32±15.34 d |
| Semi-major axis (a) | 8.56+0.29 −0.31 au |
| Eccentricity (e) | 0.43430±0.00160 |
| Inclination (i) | 79.55+0.59 −0.60° |
| Argument of periastron (ω) (secondary) | 203.74+0.38 −0.40° |
| Semi-amplitude (K1) (primary) | 1.355±0.003 km/s |
| Details | |
| ι Pavonis A | |
| Mass | 1.03+0.10 −0.06[9] M☉ |
| Radius | 1.26+0.02 −0.03[9] R☉ |
| Luminosity | 1.85+0.13 −0.11[9] L☉ |
| Surface gravity (log g) | 4.29±0.07[10] cgs |
| Temperature | 5951±29[10] K |
| Metallicity [Fe/H] | −0.07±0.06[10] dex |
| Rotational velocity (v sin i) | 2.5[11] km/s |
| Age | 7.221+2.747 −1.990[12] Gyr |
| ι Pavonis B | |
| Mass | 141±10[8] MJup |
| Other designations | |
| ι Pav, CD−62 1190, GJ 9616, HD 165499, HIP 89042, HR 6761, SAO 254157, LTT 7205, 2MASS J18102614-6200078[13] | |
| Database references | |
| SIMBAD | data |
Iota Pavonis (Latinized from ι Pavonis) is a binary star[14] in the southern constellation of Pavo. It is located at a distance of 58.0 light-years (17.79 parsecs) from the Sun based on its parallax.[1] It has an apparent visual magnitude of 5.47,[2] making it very faintly visible to the naked eye from the southern hemisphere.
Iota Pavonis consists of a solar-type primary star and a low-mass stellar companion detected by radial velocity and astrometry.[8]
Nomenclature
ι Pavonis (Latinized to Iota Pavonis) is the star's Bayer designation, abbreviated Iota Pav or ι Pav. It is also known by its Henry Draper Catalogue designation HD 165499, as well as several other catalogue designations.[13]
Properties
The primary star has a stellar classification of G0 V,[3] indicating that it is a G-type main sequence star. It is similar to the Sun, having a similar mass, slightly hotter effective temperature, and slightly lower metallicity; but is somewhat larger and more luminous.[9] At an age of about 7 billion years, it is significantly older than the Sun.[12]
Radial velocity and astrometric measurements suggest that the low-mass stellar companion has a mass of around 0.13 solar masses, and orbits the primary star in a moderately eccentric orbit at a distance of around 9 AU.[8]
Iota Pavonis is not listed in the Washington Double Star Catalog, and hence is included in the NASA Exoplanet Exploration Program (ExEP) Mission Star List (EMSL),[15] despite the separation between the two stars being less than 1 arcsecond, whereas the EMSL intended to exclude binaries with stellar companion separated by less than 3 arcseconds.[16]
See also
References
- ^ a b c d e Vallenari, A.; et al. (Gaia collaboration) (2023). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy and Astrophysics. 674: A1. arXiv:2208.00211. Bibcode:2023A&A...674A...1G. doi:10.1051/0004-6361/202243940. S2CID 244398875. Gaia DR3 record for this source at VizieR.
- ^ a b Lund, Mikkel N.; et al. (2025). "Luminaries in the sky: The TESS legacy sample of bright stars". Astronomy & Astrophysics. 701. EDP Sciences: A285. arXiv:2508.08699. Bibcode:2025A&A...701A.285L. doi:10.1051/0004-6361/202555485. ISSN 0004-6361.
- ^ a b Gray, R. O.; et al. (2006). "Contributions to the Nearby Stars (NStars) Project: Spectroscopy of Stars Earlier than M0 within 40 pc--The Southern Sample". The Astronomical Journal. 132 (1): 161–170. arXiv:astro-ph/0603770. Bibcode:2006AJ....132..161G. doi:10.1086/504637. ISSN 0004-6256.
- ^ Tuchow, Noah W.; Stark, Christopher C.; Mamajek, Eric (2024). "HPIC: The Habitable Worlds Observatory Preliminary Input Catalog". The Astronomical Journal. 167 (3): 139. Bibcode:2024AJ....167..139T. doi:10.3847/1538-3881/ad25ec.
- ^ a b c Cutri, R. M.; et al. (June 2003). "The IRSA 2MASS all-sky point source catalog, NASA/IPAC infrared science archive". The IRSA 2MASS All-Sky Point Source Catalog. Bibcode:2003tmc..book.....C.
- ^ 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. Gaia DR2 record for this source at VizieR.
- ^ Holmberg, J.; Nordström, B.; Andersen, J. (2009-05-13). "The Geneva-Copenhagen survey of the solar neighbourhood. III. Improved distances, ages, and kinematics". Astronomy & Astrophysics. 501 (3). EDP Sciences: 941–947. arXiv:0811.3982. Bibcode:2009A&A...501..941H. doi:10.1051/0004-6361/200811191. ISSN 0004-6361. S2CID 118577511.
- ^ a b c d Barbato, D.; et al. (2023). "The CORALIE survey for southern extrasolar planets. XIX. Brown dwarfs and stellar companions unveiled by radial velocity and astrometry". Astronomy & Astrophysics. 674. EDP Sciences: A114. arXiv:2303.16717. Bibcode:2023A&A...674A.114B. doi:10.1051/0004-6361/202345874. ISSN 0004-6361.
- ^ a b c d Harada, Caleb K.; et al. (2024-06-01). "Setting the Stage for the Search for Life with the Habitable Worlds Observatory: Properties of 164 Promising Planet-survey Targets". The Astrophysical Journal Supplement Series. 272 (2): 30. arXiv:2401.03047. Bibcode:2024ApJS..272...30H. doi:10.3847/1538-4365/ad3e81. ISSN 0067-0049.
- ^ a b c Soubiran, C.; et al. (2022). "Assessment of [Fe/H] determinations for FGK stars in spectroscopic surveys". Astronomy & Astrophysics. 663. EDP Sciences: A4. arXiv:2112.07545. Bibcode:2022A&A...663A...4S. doi:10.1051/0004-6361/202142409. ISSN 0004-6361.
- ^ Chavero, C; et al. (2019-06-03). "Emerging trends in metallicity and lithium properties of debris disc stars". Monthly Notices of the Royal Astronomical Society. 487 (3). Oxford University Press (OUP): 3162–3177. arXiv:1905.12066. Bibcode:2019MNRAS.487.3162C. doi:10.1093/mnras/stz1496. ISSN 0035-8711.
- ^ a b Souza dos Santos, P V; et al. (2024-06-20). "Fine structure of the age–chromospheric activity relation in solar-type stars: II. Hα line". Monthly Notices of the Royal Astronomical Society. 532 (1). Oxford University Press (OUP): 563–576. arXiv:2406.12519. Bibcode:2024MNRAS.532..563S. doi:10.1093/mnras/stae1532. ISSN 0035-8711.
- ^ a b "iot Pav -- Spectroscopic Binary". SIMBAD. Centre de Données astronomiques de Strasbourg. Retrieved 2026-03-09.
- ^ Fuhrmann, K.; et al. (February 2017). "Multiplicity among Solar-type Stars". The Astrophysical Journal. 836 (1): 23. Bibcode:2017ApJ...836..139F. doi:10.3847/1538-4357/836/1/139. 139.
- ^ Harada, Caleb K.; et al. (2025-12-01). "SPORES-HWO. II. Companion Mass Limits and Updated Planet Properties for 120 Future Exoplanet Imaging Targets from 35 yr of Precise Doppler Monitoring". The Astronomical Journal. 170 (6): 343. arXiv:2409.10679. Bibcode:2025AJ....170..343H. doi:10.3847/1538-3881/ae0b62. ISSN 0004-6256.
- ^ Mamajek, Eric; Stapelfeldt, Karl (2024-02-19). "NASA Exoplanet Exploration Program (ExEP) Mission Star List for the Habitable Worlds Observatory (2023)". arXiv:2402.12414 [astro-ph.IM].