HD 175167
Observation data
Epoch J2000.0      Equinox J2000.0
Constellation Pavo
Right ascension 19h 00m 00.83509s[1]
Declination −69° 56′ 39.2647″[1]
Apparent magnitude (V) 8.01[2]
Characteristics
Spectral type G5IV/V[3]
Apparent magnitude (B) 8.761[2]
Apparent magnitude (J) 6.713±0.019[2]
Apparent magnitude (H) 6.381±0.018[2]
Apparent magnitude (K) 6.288±0.018[2]
B−V color index 0.751±0.002[2]
Astrometry
Radial velocity (Rv)4.58±0.12[1] km/s
Proper motion (μ) RA: -7.234 mas/yr[1]
Dec.: -191.895 mas/yr[1]
Parallax (π)14.0421 ± 0.0229 mas[1]
Distance232.3 ± 0.4 ly
(71.2 ± 0.1 pc)
Absolute magnitude (MV)3.88[2]
Details
Mass1.17±0.09[4] M☉
Radius1.75±0.04[5] R☉
Luminosity2.857[6] L☉
Surface gravity (log g)4.09±0.09[4] cgs
Temperature5,635±28[4] K
Metallicity [Fe/H]+0.28±0.02[4] dex
Rotational velocity (v sin i)2.6[7] km/s
Other designations
CD−70°1658, HD 175167, HIP 93281, PPM 363703, LTT 7516, NLTT 47212[8]
Database references
SIMBADdata
Exoplanet Archivedata

HD 175167 is a star with an exoplanet companion in the southern constellation of Pavo. It is too faint to be visible with the naked eye at an apparent visual magnitude of 8.01.[2] The system is located at a distance of 232 light-years from the Sun based on parallax measurements, and it is drifting further away with a radial velocity of 5 km/s.[1] It shows a high proper motion, traversing the celestial sphere at an angular rate of 0.190 arcsec yr−1.[9]

This yellow-hued star has a stellar classification of G5IV/V,[3] which, together with the star's absolute magnitude of 3.88,[2] is consistent with a star that is in the early stages of evolving off the main sequence.[10] It has a high metallicity and is spinning with a projected rotational velocity of 2.6 km/s.[7] The star has 1.2[4] times the mass of the Sun and 1.75[5] times the Sun's girth. It is radiating 2.9[6] times the Sun's luminosity from its photosphere at an effective temperature of 5,635 K.[4]

Planetary system

A Jovian planetary companion was discovered in 2010 by a team of the Magellan Planet Search Program, led by Pamela Arriagada. Designated HD 175167 b, their Doppler velocity data (taken over a five year period) indicates the planet has an orbital period of 3.5 years at a distance of 2.40 AU (359 Gm) from the host star with an eccentricity (ovalness) of 0.54.[10] Since the inclination of the orbital plane was initially unknown, it was only possible to deduce a lower bound on the planet's mass. It is at least 7.8 times as massive as Jupiter.[10] In a 2013 paper, Robert A. Wittenmyer and colleagues reviewed the data of this and many other systems with one or two planets for possible additional planets, but were unable to find any evidence of any.[11]

An astrometric measurement of the planet's inclination and true mass was published in 2022 as part of Gaia DR3.[12] A number of subsequent studies in 2022 and 2023 have determined astrometric orbits for HD 175167 b,[13] estimating masses ranging from 6.4 MJ[14] to 15 MJ,[15][16] the latter of which would put it at the borderline of being a brown dwarf. The most recent and accurate mass measurement is 10 MJ, making it a massive super-Jovian planet.[17]

The HD 175167 planetary system[17]
Companion
(in order from star) 		Mass Semimajor axis
(AU) 		Orbital period
(days) 		Eccentricity Inclination Radius
b 10.2±0.4 MJ 2.44±0.07[13] 1275.8±0.4 0.529±0.002 38.6±1.7° —

See also

References

  1. ^ a b c d e f 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.
  2. ^ a b c d e f g h i 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.
  3. ^ a b Houk, Nancy; Cowley, A. P. (1979). Michigan catalogue of two-dimensional spectral types for the HD stars. Ann Arbor, Michigan: Dept. of Astronomy, University of Michigan. Bibcode:1978mcts.book.....H.
  4. ^ a b c d e f Santos, N. C.; et al. (August 2013). "SWEET-Cat: A catalogue of parameters for Stars With ExoplanETs. I. New atmospheric parameters and masses for 48 stars with planets". Astronomy & Astrophysics. 556: 11. arXiv:1307.0354. Bibcode:2013A&A...556A.150S. doi:10.1051/0004-6361/201321286. S2CID 55237847. A150.
  5. ^ a b Stassun, Keivan G.; et al. (2016). "Accurate Empirical Radii and Masses of Planets and Their Host Stars with Gaia Parallaxes". The Astronomical Journal. 153 (3): 136. arXiv:1609.04389. Bibcode:2017AJ....153..136S. doi:10.3847/1538-3881/aa5df3. S2CID 119219062.
  6. ^ a b 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.
  7. ^ a b Jenkins, J. S.; et al. (July 2011). "Chromospheric activities and kinematics for solar type dwarfs and subgiants: analysis of the activity distribution and the AVR". Astronomy & Astrophysics. 531: 15. arXiv:1103.0584. Bibcode:2011A&A...531A...8J. doi:10.1051/0004-6361/201016333. S2CID 55800969. A8.
  8. ^ "HD 175167". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2020-10-11.
  9. ^ Luyten, W. J. (June 1995). "VizieR Online Data Catalog: NLTT Catalogue (Luyten, 1979)". VizieR Online Data Catalog. Bibcode:1995yCat.1098....0L.
  10. ^ a b c Arriagada, Pamela; et al. (2010). "Five Long-period Extrasolar Planets in Eccentric orbits from the Magellan Planet Search Program". The Astrophysical Journal. 711 (2): 1229–35. arXiv:1001.4093. Bibcode:2010ApJ...711.1229A. doi:10.1088/0004-637X/711/2/1229. S2CID 118682009.
  11. ^ Wittenmyer, Robert A.; et al. (2013). "Forever alone? Testing single eccentric planetary systems for multiple companions". The Astrophysical Journal Supplement Series. 208 (1): 2. arXiv:1307.0894. Bibcode:2013ApJS..208....2W. doi:10.1088/0067-0049/208/1/2. S2CID 14109907.
  12. ^ Collaboration, Gaia; et al. (2023). "Gaia Data Release 3". Astronomy & Astrophysics. 674: A34. arXiv:2206.05595. doi:10.1051/0004-6361/202243782. S2CID 249626026.
  13. ^ a b Xiao, Guang-Yao; Liu, Yu-Juan; et al. (May 2023). "The Masses of a Sample of Radial-Velocity Exoplanets with Astrometric Measurements". Research in Astronomy and Astrophysics. 23 (5): 055022. arXiv:2303.12409. Bibcode:2023RAA....23e5022X. doi:10.1088/1674-4527/accb7e. S2CID 257663647.
  14. ^ Feng, Fabo; Butler, R. Paul; et al. (August 2022). "3D Selection of 167 Substellar Companions to Nearby Stars". The Astrophysical Journal Supplement Series. 262 (21): 21. arXiv:2208.12720. Bibcode:2022ApJS..262...21F. doi:10.3847/1538-4365/ac7e57. S2CID 251864022.
  15. ^ Winn, Joshua N. (September 2022). "Joint Constraints on Exoplanetary Orbits from Gaia DR3 and Doppler Data". The Astronomical Journal. 164 (5): 196. arXiv:2209.05516. Bibcode:2022AJ....164..196W. doi:10.3847/1538-3881/ac9126. S2CID 252211643.
  16. ^ Unger, N.; Ségransan, D.; et al. (October 2023). "Exploring the Brown Dwarf Desert with Precision Radial Velocities and Gaia DR3 Astrometric Orbits". Astronomy & Astrophysics. arXiv:2310.02758. doi:10.1051/0004-6361/202347578. S2CID 263622019.
  17. ^ a b Gan, Tianjun (October 2023). "Gaia Astrometry and MIKE+PFS Doppler Data Joint Analysis Reveals that HD 175167b is a Massive Cold Jupiter". Research Notes of the AAS. 7 (10): 226. arXiv:2310.14568. Bibcode:2023RNAAS...7..226G. doi:10.3847/2515-5172/ad0643.


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