WISEA J120037.79-784508.3: Difference between revisions
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== Disk == |
== Disk == |
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[[File:Nearby_young_brown_dwarf_disk_WISEA_J120037.79-784508.3.png|thumb|left|280px|Artist's depiction of brown dwarf W1200-7845. Note that observations of the disk around W1200-7845 showed that it probably does not have a large gap close to the brown dwarf.]]Three possible scenarios were considered for the disk: i) A blackbody disk (a disk with uniform temperature), ii) two blackbody disks (a disk with a gap) and iii) a power-law disk. |
[[File:Nearby_young_brown_dwarf_disk_WISEA_J120037.79-784508.3.png|thumb|left|280px|Artist's depiction of brown dwarf W1200-7845. Note that observations of the disk around W1200-7845 showed that it probably does not have a large gap close to the brown dwarf.]]Three possible scenarios were considered for the disk: i) A blackbody disk (a disk with uniform temperature), ii) two blackbody disks (a disk with a gap) and iii) a power-law disk.{{citation needed| reason=ref reqd| date=May 2024}} |
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The blackbody disk model has a temperature of 516 K (243°C; 469°F). The two-blackbodies model compromises of an inner disk with a temperature of 730 K (457°C; 854°F) and an outer disk with a temperature of 230 K (-43°C; -46°F). The best-fit model is a [[Power law|power-law]] disk with a power-law slope of α=-0.94, which is consistent with a [[Young stellar object#Classification by spectral energy distribution|class II disk]]. The close proximity of this system to the solar system makes this disk a good candidate to image the disk with [[Atacama Large Millimeter Array|ALMA]].<ref name="Paper" /> |
The blackbody disk model has a temperature of 516 K (243°C; 469°F). The two-blackbodies model compromises of an inner disk with a temperature of 730 K (457°C; 854°F) and an outer disk with a temperature of 230 K (-43°C; -46°F). The best-fit model is a [[Power law|power-law]] disk with a power-law slope of α=-0.94, which is consistent with a [[Young stellar object#Classification by spectral energy distribution|class II disk]]. The close proximity of this system to the solar system makes this disk a good candidate to image the disk with [[Atacama Large Millimeter Array|ALMA]].<ref name="Paper" /> |
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Revision as of 15:05, 3 May 2024
An editor has nominated this article for deletion. You are welcome to participate in the deletion discussion, which will decide whether or not to retain it. |
 WISE bands W1-W4 showing infrared excess around W1200-7845, indicating a primordial disk. | |
| Observation data Epoch J2000.0 Equinox J2000.0 | |
|---|---|
| Constellation | Chamaeleon |
| Right ascension | 12h 00m 37.712s[1] |
| Declination | −78° 45′ 08.378″[1] |
| Astrometry | |
| Proper motion (μ) | RA: -41.664 [0.080][1] mas/yr Dec.: -6.050 [0.074][1] mas/yr |
| Parallax (π) | 9.8383[1] ± 0.0714[1] mas |
| Distance | 333.73 ± 3.13[2] ly (102.32 ± 0.96[2] pc) |
| Details | |
| Mass | 42–58[2] MJup |
| Luminosity (bolometric) | 0.078[2] L☉ |
| Temperature | T eff, BD = 2784–2850[2]K |
| Metallicity | 0.7998 Fe abundance (from GSP using BP/RP spectra)[1] |
| Age | 3.7+4.6 −1.4[2] Myr |
| Database references | |
| SIMBAD | data |
WISEA J120037.79-784508.3, also called W1200-7845 or 2MASS J12003792-7845082, is a brown dwarf with a primordial disk 333.73 ± 3.13 lightyears from Earth in the 3.7+4.6
−1.4 Myr-old ε Chamaeleontis (ε Cha) association, currently making it the closest known brown dwarf with an associated circumstellar disk.[2] It was discovered by citizen scientists in 2020 volunteering for the Disk Detective project.[3]
Disk Detective's science team then cross-matched W1200-7845 with BANYAN Σ, a Bayesian analysis tool used to estimate the likelihood that an object is a member of a young moving group based on its position, proper motion, and parallax (using Gaia DR2 data, if available) and radial velocity. The analysis revealed (with 99.8% probability) that the brown dwarf was a member of the ε Cha young moving group association.[2][3]
Brown Dwarf
The brown dwarf has a mass of about 42-58 MJ and has a spectral type of about M6.0γ. The gamma (γ) signifies the low surface gravity of the object, which is typical for young brown dwarfs. No accretion was detected from paschen and brackett spectral lines.[2]
Later observations by Kubiak et al. 2021 found a strong H-alpha emission line, which indicates strong accretion of material. Named candidate #22 in their sample, it was the strongest accreting object in their entire sample.[4]
Disk
Three possible scenarios were considered for the disk: i) A blackbody disk (a disk with uniform temperature), ii) two blackbody disks (a disk with a gap) and iii) a power-law disk.[citation needed]
The blackbody disk model has a temperature of 516 K (243°C; 469°F). The two-blackbodies model compromises of an inner disk with a temperature of 730 K (457°C; 854°F) and an outer disk with a temperature of 230 K (-43°C; -46°F). The best-fit model is a power-law disk with a power-law slope of α=-0.94, which is consistent with a class II disk. The close proximity of this system to the solar system makes this disk a good candidate to image the disk with ALMA.[2]
See also
External links
- Disk Detective's Zooniverse blog at diskdetective.org
- Citizen scientists spot closest young brown dwarf disk yet from MIT News
References
- ^ a b c d e f g Sarro, L. M.; Berihuete, A; Smart, R. L.; Reylé, C.; Barrado, D.; García-Torres, M.; Cooper, W. J.; Jones, H. R. A.; Marocco, F.; Creevey, O. L.; Sordo, R.; Bailer-Jones, C. A. L.; Montegriffo, P.; Carballo, R.; Andrae, R.; Fouesneau, M.; Lanzafame, A. C.; Pailler, F.; Thévenin, F.; Lobel, A.; Delchambre, L.; Korn, A. J.; Recio-Blanco, A.; Schultheis, M. S.; De Angeli, F.; Brouillet, N.; Casamiquela, L.; Contursi, G.; de Laverny, P.; García-Lario, P.; Kordopatis, G.; Lebreton, Y.; Livanou, E.; Lorca, A.; Palicio, P. A.; Slezak-Oreshina, I.; Soubiran, C.; Ulla, A.; Zhao, H. (2022). "Ultracool dwarfs in Gaia DR3 (from table in VizieR)". Astronomy and Astrophysics. 669 (A193): 1–25. arXiv:2211.03641. Bibcode:2023A&A...669A.139S. doi:10.1051/0004-6361/202244507. S2CID 253383999.
- ^ a b c d e f g h i j k Schutte, Maria C.; Lawson, Kellen D.; Wisniewski, John P.; Kuchner, Marc J.; Silverberg, Steven M.; Faherty, Jacqueline K.; Gagliuffi, Daniella C. Bardalez; Kiman, Rocio; Gagné, Jonathan; Meisner, Aaron; Schneider, Adam C.; Bans, Alissa S.; Debes, John H.; Kovacevic, Natalie; Bosch, Milton K.D.; Luca, Hugo A. Durantini; Holden, Jonathan; Hyogo, Michiharu (2020-08-04). "Discovery of a Nearby Young Brown Dwarf Disk". The Astrophysical Journal. 160 (4): 156. arXiv:2007.15735v2. Bibcode:2020AJ....160..156S. doi:10.3847/1538-3881/abaccd. ISSN 1538-3881. S2CID 220920317.
- ^ a b Schutte, Maria (2020-08-12). "Our New Paper: Discovery of Nearby Young Brown Dwarf Disk!". DiskDetective.org. Retrieved 2023-09-23.
- ^ Kubiak, K.; Mužić, K.; Sousa, I.; Almendros-Abad, V.; Köhler, R.; Scholz, A. (2021-06-01). "New low-mass members of Chamaeleon I and ϵ Cha". Astronomy and Astrophysics. 650: A48. arXiv:2102.05589. Bibcode:2021A&A...650A..48K. doi:10.1051/0004-6361/202039899. ISSN 0004-6361. S2CID 231861868.
