The black hole in the most massive ultracompact dwarf galaxy M59-UCD3
We examine the internal properties of the most massive ultracompact dwarf galaxy (UCD), M59-UCD3, by combining adaptive-optics-assisted near-IR integral field spectroscopy from Gemini/NIFS and Hubble Space Telescope (HST) imaging. We use the multiband HST imaging to create a mass model that suggests...
| Main Authors: | , , , |
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| Format: | Journal article |
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American Astronomical Society
2018
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| _version_ | 1826262623154339840 |
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| author | Ahn, C Seth, A Cappellari, M al., E |
| author_facet | Ahn, C Seth, A Cappellari, M al., E |
| author_sort | Ahn, C |
| collection | OXFORD |
| description | We examine the internal properties of the most massive ultracompact dwarf galaxy (UCD), M59-UCD3, by combining adaptive-optics-assisted near-IR integral field spectroscopy from Gemini/NIFS and Hubble Space Telescope (HST) imaging. We use the multiband HST imaging to create a mass model that suggests and accounts for the presence of multiple stellar populations and structural components. We combine these mass models with kinematics measurements from Gemini/NIFS to find a best-fit stellar mass-to-light ratio (M/L) and black hole (BH) mass using Jeans anisotropic models (JAMs), axisymmetric Schwarzschild models, and triaxial Schwarzschild models. The best-fit parameters in the JAM and axisymmetric Schwarzschild models have BHs between 2.5 and 5.9 million solar masses. The triaxial Schwarzschild models point toward a similar BH mass but show a minimum χ 2 at a BH mass of ~0. Models with a BH in all three techniques provide better fits to the central V rms profiles, and thus we estimate the BH mass to be ${4.2}_{-1.7}^{+2.1}\times {10}^{6}$ M ⊙ (estimated 1σ uncertainties). We also present deep radio imaging of M59-UCD3 and two other UCDs in Virgo with dynamical BH mass measurements, and we compare these to X-ray measurements to check for consistency with the fundamental plane of BH accretion. We detect faint radio emission in M59cO but find only upper limits for M60-UCD1 and M59-UCD3 despite X-ray detections in both these sources. The BH mass and nuclear light profile of M59-UCD3 suggest that it is the tidally stripped remnant of a ~109–1010 M ⊙ galaxy. |
| first_indexed | 2024-03-06T19:39:09Z |
| format | Journal article |
| id | oxford-uuid:200dd1c1-fdf7-41d0-85f6-2a50c0cd6dcb |
| institution | University of Oxford |
| last_indexed | 2024-03-06T19:39:09Z |
| publishDate | 2018 |
| publisher | American Astronomical Society |
| record_format | dspace |
| spelling | oxford-uuid:200dd1c1-fdf7-41d0-85f6-2a50c0cd6dcb2022-03-26T11:25:29ZThe black hole in the most massive ultracompact dwarf galaxy M59-UCD3Journal articlehttp://purl.org/coar/resource_type/c_dcae04bcuuid:200dd1c1-fdf7-41d0-85f6-2a50c0cd6dcbSymplectic Elements at OxfordAmerican Astronomical Society2018Ahn, CSeth, ACappellari, Mal., EWe examine the internal properties of the most massive ultracompact dwarf galaxy (UCD), M59-UCD3, by combining adaptive-optics-assisted near-IR integral field spectroscopy from Gemini/NIFS and Hubble Space Telescope (HST) imaging. We use the multiband HST imaging to create a mass model that suggests and accounts for the presence of multiple stellar populations and structural components. We combine these mass models with kinematics measurements from Gemini/NIFS to find a best-fit stellar mass-to-light ratio (M/L) and black hole (BH) mass using Jeans anisotropic models (JAMs), axisymmetric Schwarzschild models, and triaxial Schwarzschild models. The best-fit parameters in the JAM and axisymmetric Schwarzschild models have BHs between 2.5 and 5.9 million solar masses. The triaxial Schwarzschild models point toward a similar BH mass but show a minimum χ 2 at a BH mass of ~0. Models with a BH in all three techniques provide better fits to the central V rms profiles, and thus we estimate the BH mass to be ${4.2}_{-1.7}^{+2.1}\times {10}^{6}$ M ⊙ (estimated 1σ uncertainties). We also present deep radio imaging of M59-UCD3 and two other UCDs in Virgo with dynamical BH mass measurements, and we compare these to X-ray measurements to check for consistency with the fundamental plane of BH accretion. We detect faint radio emission in M59cO but find only upper limits for M60-UCD1 and M59-UCD3 despite X-ray detections in both these sources. The BH mass and nuclear light profile of M59-UCD3 suggest that it is the tidally stripped remnant of a ~109–1010 M ⊙ galaxy. |
| spellingShingle | Ahn, C Seth, A Cappellari, M al., E The black hole in the most massive ultracompact dwarf galaxy M59-UCD3 |
| title | The black hole in the most massive ultracompact dwarf galaxy M59-UCD3 |
| title_full | The black hole in the most massive ultracompact dwarf galaxy M59-UCD3 |
| title_fullStr | The black hole in the most massive ultracompact dwarf galaxy M59-UCD3 |
| title_full_unstemmed | The black hole in the most massive ultracompact dwarf galaxy M59-UCD3 |
| title_short | The black hole in the most massive ultracompact dwarf galaxy M59-UCD3 |
| title_sort | black hole in the most massive ultracompact dwarf galaxy m59 ucd3 |
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