1RXS J160929.1−210524

1RXS J160929.1−210524 (also known as GSC 6213-1358 or PZ99 J160930.3−210459) is a pre-main-sequence star approximately 456 light-years away in the constellation of Scorpius.

1RXS J160929.1-210524
Observation data
Epoch J2000      Equinox J2000
Constellation Scorpius
Right ascension 16h 09m 30.3076s[1]
Declination −21° 04′ 58.9453″[1]
Characteristics
Spectral type K7V[2]
Variable type T Tauri star
Astrometry
Proper motion (μ) RA: −10.274±0.112[1] mas/yr
Dec.: −23.204±0.083[1] mas/yr
Parallax (π)7.1595 ± 0.0676[1] mas
Distance456 ± 4 ly
(140 ± 1 pc)
Details
Mass0.85+0.20
−0.10[2] M☉
Radius1.35[2] R☉
Temperature4060+300
−200[2] K
Age5 million[2] years
Other designations
2MASS J16093030-2104589, GSC 06213-01358, 1RXS J160929.1−210524[3]
Database references
SIMBADdata

The star was identified as a member of the Upper Scorpius subgroup of the Scorpius–Centaurus Association by Thomas Preibisch and coauthors in 1998,[4] and originally assigned an age of 5 million years old based on its group membership. A more recent analysis of the ages of the stars in the Upper Scorpius group pegs its average age at 11 million years.[5]

Stellar characteristics

This star was identified as a young object belonging to the Upper Scorpius subgroup of the Scorpius–Centaurus Association in two papers published in 1998 and 1999, based on its lithium abundance, X-ray emission, and position in the H–R diagram.[6][4] The spectrum of 1RXS J160929.1-210524 reveals it to be cooler than the Sun with a spectral type that has been estimated at K7[2] or M0,[7] so the star can be considered an orange dwarf or a red dwarf. The star is estimated to be around 0.85 times as massive as the Sun and to have an effective temperature of 4,060 K.[2] The Upper Scorpius association is quite young and only stars earlier (hotter) than type A3 have reached the main sequence; less massive stars, such as 1RXS J160929.1−210524, are still in the process of contraction during the pre-main sequence phase. Originally, the association was estimated to be around 5 million years old, but a recent 2012 paper made a significant revision of this value to 11 million years, which is therefore considered to be the age of 1RXS J160929.1-210524.[5]

Planetary system

On 8 September 2008, it was announced that astronomer David Lafrenière and collaborators used the Gemini Observatory to take pictures of the star which appeared to show a planet (designated 1RXS J160929.1-210524 b). The apparent planet is very large—about eight times the mass of Jupiter,[8] orbiting the star at a distance of 330 AU (roughly 50 billion kilometres or 31 billion miles).[9] The orbital status of the companion planet was confirmed in a paper submitted on 15 June 2010 to The Astrophysical Journal.[10][11] This made it the smallest known exoplanet orbiting its host at such a distance. It is also the second announced directly imaged exoplanet orbiting a sun-like star (after GQ Lup b), and the 2nd directly imaged exoplanet to have spectrum taken (after 2M1207b).[8]

The discoverers note that the object's location far from its star presents serious challenges to current models of planetary formation: the timescale to form a planet by core accretion at this distance from the star would be longer than the age of the system itself. One possibility is that the planet may have formed closer to the star and migrated outwards as a result of interactions with the disk or with other planets in the system. An alternative is that the planet formed in situ via the disk instability mechanism, where the disk fragments because of gravitational instability, though this would require an unusually massive protoplanetary disk.[2]

With the upward revision in the age of the Upper Scorpius group from 5 million to 11 million years, the estimated mass of 1RXS J1609b is approximately 14 Jupiter masses, i.e. above the deuterium-burning limit.[5] An older age for the J1609 system implies that the luminosity of J1609b is consistent with a much more massive object, making more likely that J1609b may be simply a brown dwarf which formed in a manner similar to that of other low-mass and substellar companions.[12]

A 2013 study, using data from the Spitzer Space Telescope, detected a moderate excess of infrared radiation at 24 μm coming from this system, indicating the presence of a dusty debris disk, but could not determine whether the excess was coming from the star or the substellar companion (or both).[13] In 2015, observations with the Magellan Clay Telescope found evidence that the light from the substellar object is obscured and reddened by 4.5 visual magnitudes of circumstellar extinction, which indicated that the object is surrounded by a dusty disk responsible for the infrared excess. When considering the extinction in modeling the object's spectrum, its effective temperature was increased to 2,000 K and the spectral type to L2.[12]

The 1RXS J160929.1−210524 system
Companion MassObserved separation
(AU)
b8+4
−1,[2] 14+2
−3[5] MJ		~330[2]

See also

References
  1. 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.
  2. Lafrenière, David; Jayawardhana, Ray; Van Kerkwijk, Marten H. (2008). "Direct Imaging and Spectroscopy of a Planetary-Mass Candidate Companion to a Young Solar Analog". The Astrophysical Journal. 689 (2): L153. arXiv:0809.1424. Bibcode:2008ApJ...689L.153L. doi:10.1086/595870.
  3. "1RXS J160929.1-210524". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 17 January 2019.
  4. Preibisch, Thomas; Zinnecker, Hans (May 1999). "The History of Low-Mass Star Formation in the Upper Scorpius OB Association". Astronomical Journal. 117 (5): 2381. Bibcode:1999AJ....117.2381P. doi:10.1086/300842.
  5. Mark J. Pecaut; Eric E. Mamajek & Eric J. Bubar (February 2012). "A Revised Age for Upper Scorpius and the Star Formation History among the F-type Members of the Scorpius-Centaurus OB Association". Astrophysical Journal. 746 (2): 154. arXiv:1112.1695. Bibcode:2012ApJ...746..154P. doi:10.1088/0004-637X/746/2/154.
  6. Preibisch, Thomas (May 1998). "A lithium-survey for pre-main sequence stars in the Upper Scorpius OB association". Astronomy and Astrophysics. 333: 619–628. Bibcode:1998A&A...333..619P.
  7. Bowler, Brendan P.; Liu, Michael C.; Kraus, Adam L.; Mann, Andrew W. (March 2014). "Spectroscopic Confirmation of Young Planetary-mass Companions on Wide Orbits" (PDF). The Astrophysical Journal. 784 (1): article 65, 21 pp. arXiv:1401.7668. Bibcode:2014ApJ...784...65B. doi:10.1088/0004-637X/784/1/65.
  8. Fazekas, Andrew (30 June 2010). ""First" Picture of Planet Orbiting Sunlike Star Confirmed". National Geographic. Archived from the original on 3 July 2010. Retrieved 1 July 2010.
  9. "Exoplanet 'circles normal star'". BBC News. 15 September 2008. Archived from the original on 16 September 2008. Retrieved 17 September 2008.
  10. Lafrenière, David; Jayawardhana, Ray; van Kerkwijk, Marten H. (2010). "The Directly Imaged Planet around the Young Solar Analog 1RXS J160929.1-210524: Confirmation of Common Proper Motion, Temperature and Mass". The Astrophysical Journal. 719 (1): 497. arXiv:1006.3070. Bibcode:2010ApJ...719..497L. doi:10.1088/0004-637X/719/1/497.
  11. Kruesi, Liz (22 June 2010). "Astronomers verify directly imaged planet". Astronomy Magazine. Archived from the original on 30 June 2010. Retrieved 1 July 2010.
  12. Wu, Ya-Lin (July 2015). "New Extinction and Mass Estimates of the Low-mass Companion 1RXS 1609 B with the Magellan AO System: Evidence of an Inclined Dust Disk". The Astrophysical Journal Letters. 807 (1): artigo L13, 5 pp. arXiv:1506.05816. Bibcode:2015ApJ...807L..13W. doi:10.1088/2041-8205/807/1/L13.
  13. Bailey, Vanessa (April 2013). "A Thermal Infrared Imaging Study of Very Low Mass, Wide-separation Brown Dwarf Companions to Upper Scorpius Stars: Constraining Circumstellar Environments". The Astrophysical Journal. 767 (1): article 31, 13 pp. arXiv:1302.0582. Bibcode:2013ApJ...767...31B. doi:10.1088/0004-637X/767/1/31.

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