 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. | |
| Observation data Epoch 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] / - |
| Astrometry | |
| Proper motion (μ) |
RA: 335.519(16)
mas/
yr
[2] Dec.: −288.994(17) mas/ yr [2] |
| Parallax (π) | 51.9970 ± 0.0141 mas [2] |
| Distance | 62.73 ± 0.02
ly (19.232 ± 0.005 pc) |
| Absolute magnitude (MV) | 12.30 [6] / - |
| Details | |
| Component A | |
| Mass | 0.58 ± 0.03 [6] M☉ |
| Surface gravity (log g) | 8.00 ± 0.05 [6] cgs |
| Temperature | 10205 ± 390 [6] K |
| Age | 1.5–2.7 [7] Gyr |
| Component B | |
| Mass | 7–9 [7] MJup |
| Surface gravity (log g) | 4.2–4.3 [7] cgs |
| Temperature | 325–350 [7] K |
| Metallicity | <0 [7] |
| Position (relative to A) | |
| Component | B |
| Angular distance | 130.2 ± 0.2 ″ [8] |
| Position angle | 104.2 ± 0.2° [8] |
| Projected separation | 2500 AU [8] |
| Other designations | |
| Database references | |
| SIMBAD | data |
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 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 and 350 kelvins (52 and 77 °C; 125 and 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
- WISE 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 b
References
- ^ a b c d e f "GJ 3483 – White Dwarf". SIMBAD. Centre de données 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&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.; 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 links
| Stars |
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|---|---|---|---|---|---|---|---|---|---|---|---|
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| Galaxies |
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2011 in space | ||
|---|---|---|
2012 » | ||
Space probe launches
 |
|   .jpg) |
| Selected NEOs | ||
|
Exoplanets
|
| |
| Discoveries | ||
| Novae | ||
| Comets
| ||
| Space exploration | ||
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. | |
| Observation data Epoch 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] / - |
| Astrometry | |
| Proper motion (μ) |
RA: 335.519(16)
mas/
yr
[2] Dec.: −288.994(17) mas/ yr [2] |
| Parallax (π) | 51.9970 ± 0.0141 mas [2] |
| Distance | 62.73 ± 0.02
ly (19.232 ± 0.005 pc) |
| Absolute magnitude (MV) | 12.30 [6] / - |
| Details | |
| Component A | |
| Mass | 0.58 ± 0.03 [6] M☉ |
| Surface gravity (log g) | 8.00 ± 0.05 [6] cgs |
| Temperature | 10205 ± 390 [6] K |
| Age | 1.5–2.7 [7] Gyr |
| Component B | |
| Mass | 7–9 [7] MJup |
| Surface gravity (log g) | 4.2–4.3 [7] cgs |
| Temperature | 325–350 [7] K |
| Metallicity | <0 [7] |
| Position (relative to A) | |
| Component | B |
| Angular distance | 130.2 ± 0.2 ″ [8] |
| Position angle | 104.2 ± 0.2° [8] |
| Projected separation | 2500 AU [8] |
| Other designations | |
| Database references | |
| SIMBAD | data |
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 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 and 350 kelvins (52 and 77 °C; 125 and 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
- WISE 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 b
References
- ^ a b c d e f "GJ 3483 – White Dwarf". SIMBAD. Centre de données 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&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.; 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 links
| Stars |
| ||||||||||
|---|---|---|---|---|---|---|---|---|---|---|---|
| |||||||||||
| Galaxies |
| ||||||||||
| |||||||||||
2011 in space | ||
|---|---|---|
2012 » | ||
|
Space probe launches
|
| |
| Selected NEOs | ||
|
Exoplanets
|
| |
| Discoveries | ||
| Novae | ||
| Comets
| ||
| Space exploration | ||