Spectral analysis of high resolution near-infrared spectra of ultra cool dwarfs
Aims.We present an analysis of high resolution spectra in the J band of five ultra cool dwarfs from M6 to L0. Methods.We make use of a new ab initio water vapour line list and existing line lists of FeH and CrH for modelling the observations. Results.We find a good fit for the Mn I 12 899.76 Å line....
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| Veröffentlicht in: | Astronomy and astrophysics (Berlin) 2007-10, Vol.473 (1), p.257-264 |
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| container_title | Astronomy and astrophysics (Berlin) |
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| creator | Lyubchik, Y. Jones, H. R. A. Pavlenko, Y. V. Martin, E. McLean, I. S. Prato, L. Barber, R. J. Tennyson, J. |
| description | Aims.We present an analysis of high resolution spectra in the J band of five ultra cool dwarfs from M6 to L0. Methods.We make use of a new ab initio water vapour line list and existing line lists of FeH and CrH for modelling the observations. Results.We find a good fit for the Mn I 12 899.76 Å line. This feature is one of the few for which we have a reliable oscillator strength. Other atomic features are present but most of the observed features are FeH and H2O lines. While we are uncertain about the quality of many of the atomic line parameters, the FeH and CrH line lists predict a number of features which are not apparent in our observed spectra. We infer that the main limiting factor in our spectral analysis is the FeH and CrH molecular spectra. |
| doi_str_mv | 10.1051/0004-6361:20065386 |
| format | Article |
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R. A. ; Pavlenko, Y. V. ; Martin, E. ; McLean, I. S. ; Prato, L. ; Barber, R. J. ; Tennyson, J.</creator><creatorcontrib>Lyubchik, Y. ; Jones, H. R. A. ; Pavlenko, Y. V. ; Martin, E. ; McLean, I. S. ; Prato, L. ; Barber, R. J. ; Tennyson, J.</creatorcontrib><description>Aims.We present an analysis of high resolution spectra in the J band of five ultra cool dwarfs from M6 to L0. Methods.We make use of a new ab initio water vapour line list and existing line lists of FeH and CrH for modelling the observations. Results.We find a good fit for the Mn I 12 899.76 Å line. This feature is one of the few for which we have a reliable oscillator strength. Other atomic features are present but most of the observed features are FeH and H2O lines. While we are uncertain about the quality of many of the atomic line parameters, the FeH and CrH line lists predict a number of features which are not apparent in our observed spectra. 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While we are uncertain about the quality of many of the atomic line parameters, the FeH and CrH line lists predict a number of features which are not apparent in our observed spectra. We infer that the main limiting factor in our spectral analysis is the FeH and CrH molecular spectra.</description><subject>Astronomy</subject><subject>brown dwarfs</subject><subject>Earth, ocean, space</subject><subject>Exact sciences and technology</subject><subject>line: identification</subject><subject>stars: atmospheres</subject><subject>stars: late-type</subject><subject>stars: low-mass</subject><issn>0004-6361</issn><issn>1432-0746</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2007</creationdate><recordtype>article</recordtype><recordid>eNpFkE1LxDAQhoMouK7-AU-96K06-WjSehPxCxYVXRG8hGw6cauxWZMuuv_elvXjNDPM8w7MQ8g-hSMKBT0GAJFLLukJA5AFL-UGGVHBWQ5KyE0y-gO2yU5Kr_3IaMlH5PZhgbaLxmemNX6VmpQFl82bl3kWMQW_7JrQZi2amDetiyZinaV1ZACXfmhsCD6rP010aZdsOeMT7v3UMXm8OJ-eXeWT28vrs9NJbnkFXU5tXVXWSVsLoxRVziA1bKaKsmS0QEeVAooVzpCDdFALqGsUTDmFxgoHfEwO13cXMXwsMXX6vUkWvTcthmXSDLiQtDcwJmwN2hhSiuj0IjbvJq40BT2404MaPajRv-760MHPdZOs8f3frW3Sf7ICKZikPZevuSZ1-PW3N_FNS8VVoUt40tXz9OH-7oZryr8BuIF-Ug</recordid><startdate>20071001</startdate><enddate>20071001</enddate><creator>Lyubchik, Y.</creator><creator>Jones, H. 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J.</creatorcontrib><creatorcontrib>Tennyson, J.</creatorcontrib><collection>Istex</collection><collection>Pascal-Francis</collection><collection>CrossRef</collection><collection>Meteorological & Geoastrophysical Abstracts</collection><collection>Meteorological & Geoastrophysical Abstracts - Academic</collection><jtitle>Astronomy and astrophysics (Berlin)</jtitle></facets><delivery><delcategory>Remote Search Resource</delcategory><fulltext>fulltext</fulltext></delivery><addata><au>Lyubchik, Y.</au><au>Jones, H. R. A.</au><au>Pavlenko, Y. V.</au><au>Martin, E.</au><au>McLean, I. S.</au><au>Prato, L.</au><au>Barber, R. J.</au><au>Tennyson, J.</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>Spectral analysis of high resolution near-infrared spectra of ultra cool dwarfs</atitle><jtitle>Astronomy and astrophysics (Berlin)</jtitle><date>2007-10-01</date><risdate>2007</risdate><volume>473</volume><issue>1</issue><spage>257</spage><epage>264</epage><pages>257-264</pages><issn>0004-6361</issn><eissn>1432-0746</eissn><coden>AAEJAF</coden><abstract>Aims.We present an analysis of high resolution spectra in the J band of five ultra cool dwarfs from M6 to L0. Methods.We make use of a new ab initio water vapour line list and existing line lists of FeH and CrH for modelling the observations. Results.We find a good fit for the Mn I 12 899.76 Å line. This feature is one of the few for which we have a reliable oscillator strength. Other atomic features are present but most of the observed features are FeH and H2O lines. While we are uncertain about the quality of many of the atomic line parameters, the FeH and CrH line lists predict a number of features which are not apparent in our observed spectra. We infer that the main limiting factor in our spectral analysis is the FeH and CrH molecular spectra.</abstract><cop>Les Ulis</cop><pub>EDP Sciences</pub><doi>10.1051/0004-6361:20065386</doi><tpages>8</tpages><oa>free_for_read</oa></addata></record> |
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| source | Bacon EDP Sciences France Licence nationale-ISTEX-PS-Journals-PFISTEX; EDP Sciences; EZB-FREE-00999 freely available EZB journals |
| subjects | Astronomy brown dwarfs Earth, ocean, space Exact sciences and technology line: identification stars: atmospheres stars: late-type stars: low-mass |
| title | Spectral analysis of high resolution near-infrared spectra of ultra cool dwarfs |
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