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Date and Time of the Query: 2019-03-19 T12:58:31 PDT
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For refcode 2009ApJ...692..856B:
Retrieve 177 NED objects in this reference.
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Copyright by American Astronomical Society. Reproduced by permission
2009ApJ...692..856B Upper Limits on the Masses of 105 Supermassive Black Holes from Hubble Space Telescope/Space Telescope Imaging Spectrograph Archival Data Beifiori, A.; Sarzi, M.; Corsini, E. M.; Bonta, E. Dalla; Pizzella, A.; Coccato, L.; Bertola, F. Abstract. Based on the modeling of the central emission-line width measured over subarcsecond apertures with the Hubble Space Telescope, we present stringent upper bounds on the mass of the central supermassive black hole, M_blackhole_, for a sample of 105 nearby galaxies (D < 100 Mpc) spanning a wide range of Hubble types (E-Sc) and values of the central stellar velocity dispersion, {sigma}_c_ (58-419 km s^-1^). For the vast majority of the objects, the derived M_blackhole_ upper limits run parallel and above the well-known M_blackhole_-{sigma}_c_ relation independently of the galaxy distance, suggesting that our nebular line-width measurements trace rather well the nuclear gravitational potential. For values of {sigma}_c_ between 90 and 220 km s^-1^, 68% of our upper limits falls immediately above the M_blackhole_-{sigma}_c_ relation without exceeding the expected M_blackhole_ values by more than a factor 4.1. No systematic trends or offsets are observed in this {sigma}_c_ range as a function of the galaxy Hubble type or with respect to the presence of a bar. For 6 of our 12 M_blackhole_ upper limits with {sigma}_c_ <90 km s^-1^, our line-width measurements are more sensitive to the stellar contribution to the gravitational potential, either due to the presence of a nuclear stellar cluster or because of a greater distance compared to the other galaxies at the low-{sigma}_c_ end of the M_blackhole_-{sigma}_c_ relation. Conversely, our M_blackhole_ upper bounds appear to lie closer to the expected M_blackhole_ in the most massive elliptical galaxies with values of {sigma}_c_ above 220 km s^-1^. Such a flattening of the M_blackhole_-{sigma}_c_ relation at its high-{sigma}_c_ end would appear consistent with a coevolution of supermassive black holes and galaxies driven by dry mergers, although better and more consistent measurements for {sigma}_c_ and K-band luminosity are needed for these kinds of objects before systematic effects can be ruled out. Key words: black hole physics, galaxies: kinematics and dynamics, galaxies: structure
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