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  • 21 Aug, 2019

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Gliese 900
Gliese 900 (GJ 900, BD+00 5017) is a triple star system, located 68 light-years from Earth in the constellation Pisces. It is made up of three main sequence stars: one is a K-type star, the two others are M-dwarf stars. The two M-dwarfs form a binary system with a period of 36 years, and this system has a period of 80 years around the primary component. With an apparent magnitude of 9.546, Gliese 900 is not visible to the naked eye. A widely separated planet has been detected around the system.

Stellar system

Location of Gliese 900 (circled)
Location of Gliese 900 (circled)

Gliese 900 is a hierarchical star system, made up of three main sequence stars: The primary component (Gliese 900 A) is a K5-K7 type star, that has 0.64–0.67 times the mass of the Sun, 0.72 times its radius, and 12% its luminosity. A light curve from the Transiting Exoplanet Survey Satellite (TESS) shows that its rotational period is 12 days. Gliese 900 A has a high level of chromospheric and coronal activity, although its apparent brightness presents little variation. The other components are red dwarf stars. Gliese 900 B has a spectral type of M3–M4 and a mass between 0.24 and 0.34 solar masses. Gliese 900 C has a spectral type of M5–M6 and a mass between 0.16 and 0.24 solar masses.

The system is young, about 200 million years old, and is a likely member (99.7% probability) of the nearby moving group Carina-Near. It is a source of X-ray emission, with an observed flux of 9.13×10 mW M, and is also a source of ultraviolet emission. The emission of X-rays is typical of young stars, and classifies it as one. The TESS light curve identifies stellar flares on this star.

Orbit

Gliese 900 B and C form an inner pair (named Gliese 900 BC) with an orbital period of around 36 years. Gliese 900 BC and Gliese 900 A orbit the system's center of mass with a period of 80 years. As of November 2004, B was separated from A by 751 milliarcseconds and C was separated from A by 708 mas. This separation changes over time. It was identified as a multiple star system in 2002 by Eduardo L. Martín, using adaptive optics-corrected images at the 8.2 m Subaru Telescope. When first observed, the A–B and A–C separations were of 0.51 and 0.76 arcsecs respectively. A further study by Malogolovets et al. (2007) identified this system as a hierarchical triple.

Other stars in the system

Malogolovets et al. (2007) reported two other objects in 2MASS images (potentially late red dwarfs) that would be the components D and E and make the system quintuple, being "very likely" to be bound to the system. However, these faint stars haven't been confirmed as members of the GJ 900 system, and are likely not associated.

Motion

Gliese 900 is located 68 light-years from Earth, based on parallax measurements by the Gaia spacecraft. The BP-RP spectra suggest a distance of 67.7 ly. The space velocity components of this system are U = −28.7, V = −15 and W = 0.2. Gliese 900 is part of the thin disk population of the Milky Way. It was once classified as part of the IC 2602 supercluster. A newer analysis using kinematics from the Gaia spacecraft suggest that Gliese 900 has a 99.7% chance of being a member of the Carina-Near moving group and a 0.3% chance of being a field star, i.e. not associated to any star cluster or stellar association.

Planetary system

A 2024 study led by Austin Rothermich identified CWISE J233531.55+014219.6 (abbreviated to CW2335+0142) as a proper motion companion to Gliese 900, with 99.5% probability. This object, also called Gliese 900 b or Gliese 900 (ABC)b, is a planetary-mass object that has 10.5 times the mass of Jupiter (or 0.01 times the mass of the Sun) and a spectral type T9. It was found to be at an angular separation of 587" from Gliese 900. At the estimated distance to this system, it translates to a projected separation of 12,000 astronomical units.

As of 2024, Gliese 900 b has the largest observed separation of any known planet, and assuming a circular orbit, the longest orbital period. The orbital period is estimated at 1.27 million years based on the projected separation. Due to the similar spectral type, orbital separation and age, CW2335+0142 has been compared to COCONUTS-2b by the discovery team.

A study in 2024 using data from the Wide-field Infrared Survey Explorer found a red W2-W3 color, which the researchers interpret as a sign of low gravity for T-dwarfs. Low gravity is often seen as an indicator of a young age and a low mass.

Gliese 900 planetary system
Companion
(in order from star) 		Mass Projected separation
(AU) 		Orbital period (10 Myr) Eccentricity Inclination Radius
b 10.5 MJ 12,000 1.27  –  – 1.11 RJ (estimate)

See also

Notes

  1. ^ Obtained with a right ascension of 23 35 00.27674 and a declination of +01° 36′ 19.4347″ on this website.
  2. ^ Using the apparent magnitude and distance from Earth, Gliese 900's absolute magnitude can be calculated.
    9.546+5−5*log(20.85) = 7.95.
  3. ^ Using the angular separation and the parallax (both in milliarcseconds), the physical separation (in AU) can be obtained.
    444/48.17 = 9.217 AU.
  4. ^ Out of objects with a planetary mass (<13 MJ). Exoplanet databases list a few brown dwarfs at larger separations.

References

  1. ^ "GJ 900". SIMBAD. Centre de données astronomiques de Strasbourg.
  2. ^ Malogolovets, E. V.; Balega, Yu. Yu.; Rastegaev, D. A.; Hofmann, K. -H.; Weigelt, G. (2007-06-01). "GJ 900: A new hierarchical system with low-mass components". Astrophysical Bulletin. 62 (2): 117–124. arXiv:0707.2193. Bibcode:2007AstBu..62..117M. doi:10.1134/S1990341307020034.
  3. ^ Hünsch, M.; Schmitt, J. H. M. M.; Sterzik, M. F.; Voges, W. (1999-03-01). "The ROSAT all-sky survey catalogue of the nearby stars". Astronomy and Astrophysics Supplement Series. 135 (2): 319–338. Bibcode:1999A&AS..135..319H. doi:10.1051/aas:1999169. ISSN 0365-0138. Gliese 900's database entry at VizieR.
  4. ^ 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.
  5. ^ Stassun, Keivan G.; Oelkers, Ryan J.; Paegert, Martin; Torres, Guillermo; Pepper, Joshua; De Lee, Nathan; Collins, Kevin; Latham, David W.; Muirhead, Philip S.; Chittidi, Jay; Rojas-Ayala, Bárbara; Fleming, Scott W.; Rose, Mark E.; Tenenbaum, Peter; Ting, Eric B. (2019-10-01). "The Revised TESS Input Catalog and Candidate Target List". The Astronomical Journal. 158 (4): 138. arXiv:1905.10694. Bibcode:2019AJ....158..138S. doi:10.3847/1538-3881/ab3467. ISSN 0004-6256. Gliese 900's database entry at VizieR.
  6. ^ Mann, Andrew W.; Dupuy, Trent; Kraus, Adam L.; Gaidos, Eric; Ansdell, Megan; Ireland, Michael; Rizzuto, Aaron C.; Hung, Chao-Ling; Dittmann, Jason; Factor, Samuel; Feiden, Gregory; Martinez, Raquel A.; Ruíz-Rodríguez, Dary; Thao, Pa Chia (2019-01-01). "How to Constrain Your M Dwarf. II. The Mass-Luminosity-Metallicity Relation from 0.075 to 0.70 Solar Masses". The Astrophysical Journal. 871 (1): 63. arXiv:1811.06938. Bibcode:2019ApJ...871...63M. doi:10.3847/1538-4357/aaf3bc. ISSN 0004-637X. Gliese 900 BC's database entry at VizieR.
  7. ^ Rothermich, Austin; Faherty, Jacqueline K.; Bardalez-Gagliuffi, Daniella; Schneider, Adam C.; Kirkpatrick, J. Davy; Meisner, Aaron M.; Burgasser, Adam J.; Kuchner, Marc; Allers, Katelyn; Gagné, Jonathan; Caselden, Dan; Calamari, Emily; Popinchalk, Mark; Suárez, Genaro; Gerasimov, Roman (2024-06-01). "89 New Ultracool Dwarf Comoving Companions Identified with the Backyard Worlds: Planet 9 Citizen Science Project". The Astronomical Journal. 167 (6): 253. arXiv:2403.04592. Bibcode:2024AJ....167..253R. doi:10.3847/1538-3881/ad324e. ISSN 0004-6256.
  8. ^ Martín, Eduardo L. (2003-08-01). "A New Multiple Stellar System in the Solar Neighborhood". The Astronomical Journal. 126 (2): 918–920. arXiv:astro-ph/0305289. Bibcode:2003AJ....126..918M. doi:10.1086/376742. ISSN 0004-6256.
  9. ^ Zuckerman, B.; Bessell, M. S.; Song, Inseok; Kim, S. (2006-10-01). "The Carina-Near Moving Group". The Astrophysical Journal. 649 (2): L115–L118. arXiv:astro-ph/0609041. Bibcode:2006ApJ...649L.115Z. doi:10.1086/508060. ISSN 0004-637X.
  10. ^ Hinkel, Natalie R.; Mamajek, Eric E.; Turnbull, Margaret C.; Osby, Ella; Shkolnik, Evgenya L.; Smith, Graeme H.; Klimasewski, Alexis; Somers, Garrett; Desch, Steven J. (2017-10-01). "A Catalog of Stellar Unified Properties (CATSUP) for 951 FGK-Stars within 30 pc". The Astrophysical Journal. 848 (1): 34. arXiv:1709.04465. Bibcode:2017ApJ...848...34H. doi:10.3847/1538-4357/aa8b0f. ISSN 0004-637X. Gliese 900's database entry at VizieR.
  11. ^ "GJ 900 Overview". NASA Exoplanet Archive. Retrieved June 17, 2024.
  12. ^ "The Extrasolar Planet Encyclopaedia — GJ 900 (ABC)b". Extrasolar Planets Encyclopaedia. Paris Observatory.
  13. ^ Martin, Pierre-Yves (1995). "Catalogue of Exoplanets". exoplanet.eu. Retrieved 2024-06-20.
  14. ^ "Planetary Systems Composite Data". NASA Exoplanet Archive. Retrieved 25 June 2024.
  15. ^ "GJ 900 b - NASA Science". science.nasa.gov. Retrieved 2024-06-20.
  16. ^ Leggett, S. K.; Tremblin, Pascal (5 Nov 2024). "Redshifting the Study of Cold Brown Dwarfs and Exoplanets: the Mid-Infrared Wavelength Region as an Indicator of Surface Gravity and Mass". arXiv:2411.03549 [astro-ph].
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