Measuring the low mass end of the M• - σ relation
We show that high quality laser guide star (LGS) adaptive optics (AO) observations of nearby early-type galaxies are possible when the tip-tilt correction is done by guiding on nuclei while the focus compensation due to the changing distance to the sodium layer is made 'open loop'. We achi...
| Main Authors: | , , , |
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| Format: | Journal article |
| Language: | English |
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2010
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| _version_ | 1797101735224803328 |
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| author | Krajnović, D McDermid, R Cappellari, M Davies, R |
| author_facet | Krajnović, D McDermid, R Cappellari, M Davies, R |
| author_sort | Krajnović, D |
| collection | OXFORD |
| description | We show that high quality laser guide star (LGS) adaptive optics (AO) observations of nearby early-type galaxies are possible when the tip-tilt correction is done by guiding on nuclei while the focus compensation due to the changing distance to the sodium layer is made 'open loop'. We achieve corrections such that 40% of flux comes from R<0.2 arcsec. To measure a black hole mass (M•) one needs integral field observations of both high spatial resolution and large field of view. With these data it is possible to determine the lower limit to M• even if the spatial resolution of the observations are up to a few times larger than the sphere of influence of the black hole. © 2010 American Institute of Physics. |
| first_indexed | 2024-03-07T05:56:04Z |
| format | Journal article |
| id | oxford-uuid:ea89d1a1-0d50-47ae-9ea4-1653f700cde9 |
| institution | University of Oxford |
| language | English |
| last_indexed | 2024-03-07T05:56:04Z |
| publishDate | 2010 |
| record_format | dspace |
| spelling | oxford-uuid:ea89d1a1-0d50-47ae-9ea4-1653f700cde92022-03-27T11:03:04ZMeasuring the low mass end of the M• - σ relationJournal articlehttp://purl.org/coar/resource_type/c_dcae04bcuuid:ea89d1a1-0d50-47ae-9ea4-1653f700cde9EnglishSymplectic Elements at Oxford2010Krajnović, DMcDermid, RCappellari, MDavies, RWe show that high quality laser guide star (LGS) adaptive optics (AO) observations of nearby early-type galaxies are possible when the tip-tilt correction is done by guiding on nuclei while the focus compensation due to the changing distance to the sodium layer is made 'open loop'. We achieve corrections such that 40% of flux comes from R<0.2 arcsec. To measure a black hole mass (M•) one needs integral field observations of both high spatial resolution and large field of view. With these data it is possible to determine the lower limit to M• even if the spatial resolution of the observations are up to a few times larger than the sphere of influence of the black hole. © 2010 American Institute of Physics. |
| spellingShingle | Krajnović, D McDermid, R Cappellari, M Davies, R Measuring the low mass end of the M• - σ relation |
| title | Measuring the low mass end of the M• - σ relation |
| title_full | Measuring the low mass end of the M• - σ relation |
| title_fullStr | Measuring the low mass end of the M• - σ relation |
| title_full_unstemmed | Measuring the low mass end of the M• - σ relation |
| title_short | Measuring the low mass end of the M• - σ relation |
| title_sort | measuring the low mass end of the m• σ relation |
| work_keys_str_mv | AT krajnovicd measuringthelowmassendofthemsrelation AT mcdermidr measuringthelowmassendofthemsrelation AT cappellarim measuringthelowmassendofthemsrelation AT daviesr measuringthelowmassendofthemsrelation |