WD 0806−661 (L 97-3, GJ 3483), formally named Maru,[9] is a DQwhite dwarf with an extremely cold Y-typesubstellar companion (designated "B"), located in the constellation Volans at 62.7 light-years (19.2 parsecs) from Earth. The companion was discovered in 2011, and is the only known Y-type companion to a star or stellar remnant. At the time of its discovery WD 0806-661 B had the largest actual (2500 AU) and apparent separation (more than 2 arcminutes) of any known planetary-mass object, as well as being the coldest directly imaged substellar object then known.
WD 0806−661 / Maru
The right side shows an image taken by ESO's VLT HAWK-I in near-infrared. The white dwarf is marked with an arrow. The left side shows an image taken by the NASA/ESA HST WFC3 also in near-infrared wavelengths. The sub-brown dwarf appears as green pixels (2014) and purple pixels (2015) in an insert.
Component WD 0806-661 B was discovered in 2011 with the Spitzer Space Telescope. Its discovery paper is Luhman et al., 2011. The secondary has a mass between 7 and 9 MJ and a temperature between 325–350 Kelvin (52-77 °C; 125-170 °F).[7] At the time of its discovery, WD 0806−661 B was the coldest "brown dwarf" that has ever been found.[8] The object is too faint to acquire a spectrum even with the Hubble Space Telescope, however the spectral type of this object was estimated to be Y1 based on its detection in Hubble images at near-infrared wavelengths.[5] The photometric colors of this object suggest that it is metal-poor. The metal-poor composition of the companion could explain the DQ spectral type of the primary white dwarf.[7] Hydrogen-deficient AGB stars might evolve into DB white dwarfs and then into DQ white dwarfs as they cool down.[10]
In August 2022, WD 0806-661 and its planetary-mass companion were included among 20 systems to be named by the third NameExoWorlds project.[11] The approved names, proposed by a team from South Korea, were announced in June 2023. WD 0806-661 is named Maru and its companion is named Ahra, after Korean words meaning "sky" and "ocean".[9]
^ abcdVallenari, 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.
^Holberg, J. B.; Sion, E. M.; Oswalt, T.; McCook, G. P.; Foran, S.; Subasavage, John P. (2008). "A New Look at the Local White Dwarf Population". The Astronomical Journal. 135 (4): 1225–1238. Bibcode:2008AJ....135.1225H. doi:10.1088/0004-6256/135/4/1225. S2CID 122855486.
^Sion, Edward M.; Holberg, J. B.; Oswalt, Terry D.; McCook, George P.; Wasatonic, Richard (2009). "The White Dwarfs Within 20 Parsecs of the Sun: Kinematics and Statistics". The Astronomical Journal. 138 (6): 1681–1689. arXiv:0910.1288. Bibcode:2009AJ....138.1681S. doi:10.1088/0004-6256/138/6/1681. S2CID 119284418.
^ abLeggett, S. K.; Morley, Caroline V.; Marley, M. S.; Saumon, D. (January 2015). "Near-infrared Photometry of Y Dwarfs: Low Ammonia Abundance and the Onset of Water Clouds". The Astrophysical Journal. 799 (1): 37. arXiv:1411.2020. Bibcode:2015ApJ...799...37L. doi:10.1088/0004-637X/799/1/37. ISSN 0004-637X. S2CID 118530454.
^ abcdefghGiammichele, N.; Bergeron, P.; Dufour, P. (2012). "Know Your Neighborhood: A Detailed Model Atmosphere Analysis of Nearby White Dwarfs". The Astrophysical Journal Supplement. 199 (2): 29. arXiv:1202.5581. Bibcode:2012ApJS..199...29G. doi:10.1088/0067-0049/199/2/29. S2CID 118304737.
^ abcdefghiLeggett, S. K.; Tremblin, P.; Esplin, T. L.; Luhman, K. L.; Morley, Caroline V. (June 2017). "The Y-type Brown Dwarfs: Estimates of Mass and Age from New Astrometry, Homogenized Photometry, and Near-infrared Spectroscopy". The Astrophysical Journal. 842 (2): 118. arXiv:1704.03573. Bibcode:2017ApJ...842..118L. doi:10.3847/1538-4357/aa6fb5. ISSN 0004-637X. S2CID 119249195.
^ abcdLuhman, K. L.; Burgasser, Adam J.; Bochanski, J. J. (2011). "Discovery of a Candidate for the Coolest Known Brown Dwarf". The Astrophysical Journal Letters. 730 (1): L9. arXiv:1102.5411. Bibcode:2011ApJ...730L...9L. doi:10.1088/2041-8205/730/1/L9. S2CID 54666396.
^ ab"2022 Approved Names". nameexoworlds.iau.org. IAU. Retrieved 7 June 2023.
^Althaus, L. G.; Serenelli, A. M.; Panei, J. A.; Córsico, A. H.; García-Berro, E.; Scóccola, C. G. (May 2005). "The formation and evolution of hydrogen-deficient post-AGB white dwarfs: The emerging chemical profile and the expectations for the PG 1159-DB-DQ evolutionary connection". Astronomy and Astrophysics. 435 (2): 631–648. arXiv:astro-ph/0502005. Bibcode:2005A&A...435..631A. doi:10.1051/0004-6361:20041965. ISSN 0004-6361.
^"List of ExoWorlds 2022". nameexoworlds.iau.org. IAU. 8 August 2022. Retrieved 27 August 2022.
External linksedit
Simbad — component b
WD 0806-661 on Solstation.com
April 30, 2024
0806, 3483, formally, named, maru, white, dwarf, with, extremely, cold, type, substellar, companion, designated, located, constellation, volans, light, years, parsecs, from, earth, companion, discovered, 2011, only, known, type, companion, star, stellar, remna. WD 0806 661 L 97 3 GJ 3483 formally named Maru 9 is a DQ white dwarf with an extremely cold Y type substellar companion designated B located in the constellation Volans at 62 7 light years 19 2 parsecs from Earth The companion was discovered in 2011 and is the only known Y type companion to a star or stellar remnant At the time of its discovery WD 0806 661 B had the largest actual 2500 AU and apparent separation more than 2 arcminutes of any known planetary mass object as well as being the coldest directly imaged substellar object then known WD 0806 661 MaruThe right side shows an image taken by ESO s VLT HAWK I in near infrared The white dwarf is marked with an arrow The left side shows an image taken by the NASA ESA HST WFC3 also in near infrared wavelengths The sub brown dwarf appears as green pixels 2014 and purple pixels 2015 in an insert Observation dataEpoch J2000 1 Equinox J2000 1 Constellation Volans Right ascension 08h 06m 53 75366s 2 Declination 66 18 16 7011 2 Characteristics Spectral type DQ4 2 3 4 Y1 5 Apparent magnitude B 13 74 6 Apparent magnitude V 13 71 6 Apparent magnitude R 13 64 6 Apparent magnitude I 13 60 6 Apparent magnitude J 13 704 0 023 1 25 42 7 Apparent magnitude H 13 739 0 025 1 25 29 7 Apparent magnitude K 13 781 0 043 1 AstrometryProper motion m RA 335 519 16 mas yr 2 Dec 288 994 17 mas yr 2 Parallax p 51 9970 0 0141 mas 2 Distance62 73 0 02 ly 19 232 0 005 pc Absolute magnitude MV 12 30 6 DetailsComponent AMass0 58 0 03 6 M Surface gravity log g 8 00 0 05 6 cgsTemperature10205 390 6 KAge1 5 2 7 7 GyrComponent BMass7 9 7 MJupSurface gravity log g 4 2 4 3 7 cgsTemperature325 350 7 KMetallicity lt 0 7 Position relative to A ComponentBAngular distance130 2 0 2 8 Position angle104 2 0 2 8 Projected separation2500 AU 8 Other designationsMaru GJ 3483 BPM 4834 L 97 3 LAWD 27 LTT 3059 NLTT 19008 WD 0806 661 WD 0806 66 GSC 08936 01284 2MASS J08065373 6618167 GEN 6 00204834 uvby98 986097003 WG 12 1 Database referencesSIMBADdata Contents 1 WD 0806 661 B 2 See also 3 References 4 External linksWD 0806 661 B editMain article WD 0806 661 B Component WD 0806 661 B was discovered in 2011 with the Spitzer Space Telescope Its discovery paper is Luhman et al 2011 The secondary has a mass between 7 and 9 MJ and a temperature between 325 350 Kelvin 52 77 C 125 170 F 7 At the time of its discovery WD 0806 661 B was the coldest brown dwarf that has ever been found 8 The object is too faint to acquire a spectrum even with the Hubble Space Telescope however the spectral type of this object was estimated to be Y1 based on its detection in Hubble images at near infrared wavelengths 5 The photometric colors of this object suggest that it is metal poor The metal poor composition of the companion could explain the DQ spectral type of the primary white dwarf 7 Hydrogen deficient AGB stars might evolve into DB white dwarfs and then into DQ white dwarfs as they cool down 10 In August 2022 WD 0806 661 and its planetary mass companion were included among 20 systems to be named by the third NameExoWorlds project 11 The approved names proposed by a team from South Korea were announced in June 2023 WD 0806 661 is named Maru and its companion is named Ahra after Korean words meaning sky and ocean 9 See also editWISE 0146 4234 a Y0 companion to a T9 brown dwarf WISE 1217 1626 B another Y0 companion to a T9 brown dwarf DT Virginis HD 106906 b GU Piscium bReferences edit a b c d e f GJ 3483 White Dwarf SIMBAD Centre de donnees astronomiques de Strasbourg Retrieved 2012 06 19 a b c d 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 amp A 674A 1G doi 10 1051 0004 6361 202243940 S2CID 244398875 Gaia DR3 record for this source at VizieR Holberg J B Sion E M Oswalt T McCook G P Foran S Subasavage John P 2008 A New Look at the Local White Dwarf Population The Astronomical Journal 135 4 1225 1238 Bibcode 2008AJ 135 1225H doi 10 1088 0004 6256 135 4 1225 S2CID 122855486 Sion Edward M Holberg J B Oswalt Terry D McCook George P Wasatonic Richard 2009 The White Dwarfs Within 20 Parsecs of the Sun Kinematics and Statistics The Astronomical Journal 138 6 1681 1689 arXiv 0910 1288 Bibcode 2009AJ 138 1681S doi 10 1088 0004 6256 138 6 1681 S2CID 119284418 a b Leggett S K Morley Caroline V Marley M S Saumon D January 2015 Near infrared Photometry of Y Dwarfs Low Ammonia Abundance and the Onset of Water Clouds The Astrophysical Journal 799 1 37 arXiv 1411 2020 Bibcode 2015ApJ 799 37L doi 10 1088 0004 637X 799 1 37 ISSN 0004 637X S2CID 118530454 a b c d e f g h Giammichele N Bergeron P Dufour P 2012 Know Your Neighborhood A Detailed Model Atmosphere Analysis of Nearby White Dwarfs The Astrophysical Journal Supplement 199 2 29 arXiv 1202 5581 Bibcode 2012ApJS 199 29G doi 10 1088 0067 0049 199 2 29 S2CID 118304737 a b c d e f g h i Leggett S K Tremblin P Esplin T L Luhman K L Morley Caroline V June 2017 The Y type Brown Dwarfs Estimates of Mass and Age from New Astrometry Homogenized Photometry and Near infrared Spectroscopy The Astrophysical Journal 842 2 118 arXiv 1704 03573 Bibcode 2017ApJ 842 118L doi 10 3847 1538 4357 aa6fb5 ISSN 0004 637X S2CID 119249195 a b c d Luhman K L Burgasser Adam J Bochanski J J 2011 Discovery of a Candidate for the Coolest Known Brown Dwarf The Astrophysical Journal Letters 730 1 L9 arXiv 1102 5411 Bibcode 2011ApJ 730L 9L doi 10 1088 2041 8205 730 1 L9 S2CID 54666396 a b 2022 Approved Names nameexoworlds iau org IAU Retrieved 7 June 2023 Althaus L G Serenelli A M Panei J A Corsico A H Garcia Berro E Scoccola C G May 2005 The formation and evolution of hydrogen deficient post AGB white dwarfs The emerging chemical profile and the expectations for the PG 1159 DB DQ evolutionary connection Astronomy and Astrophysics 435 2 631 648 arXiv astro ph 0502005 Bibcode 2005A amp A 435 631A doi 10 1051 0004 6361 20041965 ISSN 0004 6361 List of ExoWorlds 2022 nameexoworlds iau org IAU 8 August 2022 Retrieved 27 August 2022 External links editSimbad component b WD 0806 661 on Solstation com Retrieved from https en wikipedia org w index php title WD 0806 661 amp oldid 1197948916, wikipedia, wiki, book, books, library,
