The black hole in NGC 3379: a comparison of gas and stellar dynamical mass measurements with HST and integral-field data
| Autor: | Kristen L. Shapiro, Karl Gebhardt, Michele Cappellari, Tim de Zeeuw, Richard M. McDermid, Remco C. E. van den Bosch, Thomas S. Statler |
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| Rok vydání: | 2006 |
| Předmět: |
Physics
Stellar kinematics 010308 nuclear & particles physics Astrophysics::High Energy Astrophysical Phenomena Astrophysics (astro-ph) FOS: Physical sciences Perturbation (astronomy) Sigma Astronomy and Astrophysics Astrophysics::Cosmology and Extragalactic Astrophysics Kinematics Astrophysics 01 natural sciences Galaxy Black hole General Relativity and Quantum Cosmology Stars Space and Planetary Science 0103 physical sciences Elliptical galaxy Astrophysics::Earth and Planetary Astrophysics 010303 astronomy & astrophysics Astrophysics::Galaxy Astrophysics |
| Zdroj: | Monthly Notices of the Royal Astronomical Society. 370:559-579 |
| ISSN: | 1365-2966 0035-8711 |
| DOI: | 10.1111/j.1365-2966.2006.10537.x |
| Popis: | We combine Hubble Space Telescope spectroscopy and ground-based integral-field data from the SAURON and OASIS instruments to study the central black hole in the nearby elliptical galaxy NGC 3379. From these data, we obtain kinematics of both the stars and the nuclear gaseous component. Axisymmetric three-integral models of the stellar kinematics find a black hole of mass 1.4 (+2.6 / -1.0) x 10^8 M_sun (3 sigma errors). These models also probe the velocity distribution in the immediate vicinity of the black hole and reveal a nearly isotropic velocity distribution throughout the galaxy and down to the black hole sphere of influence R_BH. The morphology of the nuclear gas disc suggests that it is not in the equatorial plane; however the core of NGC 3379 is nearly spherical. Inclined thin-disc models of the gas find a nominal black hole of mass 2.0 (+/- 0.1) x 10^8 M_sun (3 sigma errors), but the model is a poor fit to the kinematics. The data are better fit by introducing a twist in the gas kinematics (with the black hole mass assumed to be 2.0 x 10^8 M_sun), although the constraints on the nature and shape of this perturbation are insufficient for more detailed modelling. Given the apparent regularity of the gas disc's appearance, the presence of such strong non-circular motion indicates that caution must be used when measuring black hole masses with gas dynamical methods alone. Comment: 22 pages, 19 figures. Accepted for publication in MNRAS. A version with full resolution figures is available at http://astro.berkeley.edu/~shapiro/Papers/shapiro2006_N3379.pdf |
| Databáze: | OpenAIRE |
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