Adaptive Optics Integral Field Spectroscopy of the Young Stellar Objects in LkH_alpha 225
Progress in understanding the embedded stars in LkHa225 has been hampered by their variability, making it hard to compare data taken at different times, and by the limited resolution of the available data, which cannot probe the small scales between the two stars. In an attempt to overcome these dif...
| Main Authors: | , , , , , , , |
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| Format: | Journal article |
| Language: | English |
| Published: |
Institute of Physics Publishing
2001
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| _version_ | 1797051388117647360 |
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| author | Davies, R Tecza, M Looney, L Eisenhauer, F Tacconi-Garman, L Thatte, N Ott, T Rabien, S |
| author_facet | Davies, R Tecza, M Looney, L Eisenhauer, F Tacconi-Garman, L Thatte, N Ott, T Rabien, S |
| author_sort | Davies, R |
| collection | OXFORD |
| description | Progress in understanding the embedded stars in LkHa225 has been hampered by their variability, making it hard to compare data taken at different times, and by the limited resolution of the available data, which cannot probe the small scales between the two stars. In an attempt to overcome these difficulties, we present new near-infrared data on this object taken using the ALFA adaptive optics system with the MPE 3D integral field spectrometer and the near-infrared camera Omega-Cass. The stars themselves have K-band spectra which are dominated by warm dust emission, analagous to class I-II for low mass YSOs, suggesting that the stars are in a phase where they are still accreting matter. On the other hand, the ridge of continuum emission between them is rather bluer, suggestive of extincted and/or scattered stellar light rather than direct dust emission. The compactness of the CO emission seen toward each star argues for accretion disks (which can also account for much of the K-band veiling) rather than a neutral wind. In contrast to other YSOs with CO emission, LkHa225 has no detectable Br_gamma emission. Additionally there is no H_2 detected on the northern star, although we do confirm that the strongest H_2 emission is on the southern star, where we find it is excited primarily by thermal mechanisms. A second knot of H_2 is observed to its northeast, with a velocity shift of -75kms and a higher fraction of non-thermal emission. This is discussed with reference to the H2O maser, the molecular outflow, and [S II] emission observed between the stars. |
| first_indexed | 2024-03-06T18:18:50Z |
| format | Journal article |
| id | oxford-uuid:059223f7-2645-4328-acf4-d122e54d387c |
| institution | University of Oxford |
| language | English |
| last_indexed | 2024-03-06T18:18:50Z |
| publishDate | 2001 |
| publisher | Institute of Physics Publishing |
| record_format | dspace |
| spelling | oxford-uuid:059223f7-2645-4328-acf4-d122e54d387c2022-03-26T08:57:54ZAdaptive Optics Integral Field Spectroscopy of the Young Stellar Objects in LkH_alpha 225Journal articlehttp://purl.org/coar/resource_type/c_dcae04bcuuid:059223f7-2645-4328-acf4-d122e54d387cEnglishSymplectic Elements at OxfordInstitute of Physics Publishing2001Davies, RTecza, MLooney, LEisenhauer, FTacconi-Garman, LThatte, NOtt, TRabien, SProgress in understanding the embedded stars in LkHa225 has been hampered by their variability, making it hard to compare data taken at different times, and by the limited resolution of the available data, which cannot probe the small scales between the two stars. In an attempt to overcome these difficulties, we present new near-infrared data on this object taken using the ALFA adaptive optics system with the MPE 3D integral field spectrometer and the near-infrared camera Omega-Cass. The stars themselves have K-band spectra which are dominated by warm dust emission, analagous to class I-II for low mass YSOs, suggesting that the stars are in a phase where they are still accreting matter. On the other hand, the ridge of continuum emission between them is rather bluer, suggestive of extincted and/or scattered stellar light rather than direct dust emission. The compactness of the CO emission seen toward each star argues for accretion disks (which can also account for much of the K-band veiling) rather than a neutral wind. In contrast to other YSOs with CO emission, LkHa225 has no detectable Br_gamma emission. Additionally there is no H_2 detected on the northern star, although we do confirm that the strongest H_2 emission is on the southern star, where we find it is excited primarily by thermal mechanisms. A second knot of H_2 is observed to its northeast, with a velocity shift of -75kms and a higher fraction of non-thermal emission. This is discussed with reference to the H2O maser, the molecular outflow, and [S II] emission observed between the stars. |
| spellingShingle | Davies, R Tecza, M Looney, L Eisenhauer, F Tacconi-Garman, L Thatte, N Ott, T Rabien, S Adaptive Optics Integral Field Spectroscopy of the Young Stellar Objects in LkH_alpha 225 |
| title | Adaptive Optics Integral Field Spectroscopy of the Young Stellar Objects
in LkH_alpha 225 |
| title_full | Adaptive Optics Integral Field Spectroscopy of the Young Stellar Objects
in LkH_alpha 225 |
| title_fullStr | Adaptive Optics Integral Field Spectroscopy of the Young Stellar Objects
in LkH_alpha 225 |
| title_full_unstemmed | Adaptive Optics Integral Field Spectroscopy of the Young Stellar Objects
in LkH_alpha 225 |
| title_short | Adaptive Optics Integral Field Spectroscopy of the Young Stellar Objects
in LkH_alpha 225 |
| title_sort | adaptive optics integral field spectroscopy of the young stellar objects in lkh alpha 225 |
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