A deep survey of brown dwarfs in Orion with Gemini
We report the results of a deep near-infrared (JHK) survey of the outer parts of the Trapezium Cluster with Gemini South/Flamingos. 396 sources were detected in a 26 arcmin 2 area, including 138 brown dwarf candidates, defined as M < 0.075 M ⊙ for an assumed age of 1 Myr. Only 33 of the brown...
| Główni autorzy: | , , |
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| Format: | Journal article |
| Język: | English |
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2005
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| _version_ | 1826279555834314752 |
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| author | Lucas, P Roche, P Tamura, M |
| author_facet | Lucas, P Roche, P Tamura, M |
| author_sort | Lucas, P |
| collection | OXFORD |
| description | We report the results of a deep near-infrared (JHK) survey of the outer parts of the Trapezium Cluster with Gemini South/Flamingos. 396 sources were detected in a 26 arcmin 2 area, including 138 brown dwarf candidates, defined as M < 0.075 M ⊙ for an assumed age of 1 Myr. Only 33 of the brown dwarf candidates are planetary mass candidates with estimated masses in the range 0.003 < M < 0.012 M ⊙. In an extinction-limited sample (A v < 5) complete to approximately 0. 005 M ⊙ (5 M Jup) the mass function appears to drop by a factor of 2 at the deuterium burning threshold, i.e. at planetary masses. After allowing for background contamination it is likely that planetary mass objects at 3-13 M Jup number < 10 per cent of the cluster population, with an upper limit of 13 per cent. Analysis of the spatial distribution of stars and brown dwarf candidates suggests that brown dwarfs and very low-mass stars (M < 0.1 M ⊙) are less likely than more massive stars to have wide (> 150 au) binary companions. This result has modest statistical significance (96 per cent) in our data but is supported at 93 per cent confidence by analysis of a completely independent sample taken from the Subaru data of Kaifu et al. There is a statistically very significant excess of both stars and brown dwarfs with small separations from each other (<6 arcsec or 2600 au). This appears to be due to the presence of small-N subgroups, which are likely to be dynamically unstable in the long term. Hence these results are consistent with the 'ejected stellar embryo' hypothesis for brown dwarf formation. We also report the discovery of two new bipolar nebulae, which are interpreted as Class I protostars. © 2005 RAS. |
| first_indexed | 2024-03-07T00:00:30Z |
| format | Journal article |
| id | oxford-uuid:75c62b1b-9906-443c-a54e-a3c64e382d06 |
| institution | University of Oxford |
| language | English |
| last_indexed | 2024-03-07T00:00:30Z |
| publishDate | 2005 |
| record_format | dspace |
| spelling | oxford-uuid:75c62b1b-9906-443c-a54e-a3c64e382d062022-03-26T20:11:32ZA deep survey of brown dwarfs in Orion with GeminiJournal articlehttp://purl.org/coar/resource_type/c_dcae04bcuuid:75c62b1b-9906-443c-a54e-a3c64e382d06EnglishSymplectic Elements at Oxford2005Lucas, PRoche, PTamura, MWe report the results of a deep near-infrared (JHK) survey of the outer parts of the Trapezium Cluster with Gemini South/Flamingos. 396 sources were detected in a 26 arcmin 2 area, including 138 brown dwarf candidates, defined as M < 0.075 M ⊙ for an assumed age of 1 Myr. Only 33 of the brown dwarf candidates are planetary mass candidates with estimated masses in the range 0.003 < M < 0.012 M ⊙. In an extinction-limited sample (A v < 5) complete to approximately 0. 005 M ⊙ (5 M Jup) the mass function appears to drop by a factor of 2 at the deuterium burning threshold, i.e. at planetary masses. After allowing for background contamination it is likely that planetary mass objects at 3-13 M Jup number < 10 per cent of the cluster population, with an upper limit of 13 per cent. Analysis of the spatial distribution of stars and brown dwarf candidates suggests that brown dwarfs and very low-mass stars (M < 0.1 M ⊙) are less likely than more massive stars to have wide (> 150 au) binary companions. This result has modest statistical significance (96 per cent) in our data but is supported at 93 per cent confidence by analysis of a completely independent sample taken from the Subaru data of Kaifu et al. There is a statistically very significant excess of both stars and brown dwarfs with small separations from each other (<6 arcsec or 2600 au). This appears to be due to the presence of small-N subgroups, which are likely to be dynamically unstable in the long term. Hence these results are consistent with the 'ejected stellar embryo' hypothesis for brown dwarf formation. We also report the discovery of two new bipolar nebulae, which are interpreted as Class I protostars. © 2005 RAS. |
| spellingShingle | Lucas, P Roche, P Tamura, M A deep survey of brown dwarfs in Orion with Gemini |
| title | A deep survey of brown dwarfs in Orion with Gemini |
| title_full | A deep survey of brown dwarfs in Orion with Gemini |
| title_fullStr | A deep survey of brown dwarfs in Orion with Gemini |
| title_full_unstemmed | A deep survey of brown dwarfs in Orion with Gemini |
| title_short | A deep survey of brown dwarfs in Orion with Gemini |
| title_sort | deep survey of brown dwarfs in orion with gemini |
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