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M∙ − σ relation in spherical systems

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dc.contributor.author Bhattacharyya, D
dc.contributor.author Mangalam, A
dc.date.accessioned 2020-11-11T01:43:34Z
dc.date.available 2020-11-11T01:43:34Z
dc.date.issued 2018-02
dc.identifier.citation Journal of Astrophysics and Astronomy, Vol. 39, No. 1, 4 en_US
dc.identifier.issn 0250-6335
dc.identifier.uri http://prints.iiap.res.in/handle/2248/6899
dc.description Open Access © Indian Academy of Sciences; http://www.ias.ac.in/describe/article/joaa/039/01/0004||https://doi.org/10.1007/s12036-017-9493-2 en_US
dc.description.abstract To investigate the M∙−σ relation, we consider realistic elliptical galaxy profiles that are taken to follow a single power-law density profile given by Ï (r)=Ï 0(r/r0)−γ or the Nuker intensity profile. We calculate the density using Abel’s formula in the latter case by employing the derived stellar potential; in both cases. We derive the distribution function f(E) of the stars in the presence of the supermassive black hole (SMBH) at the center and hence compute the line-of-sight (LoS) velocity dispersion as a function of radius. For the typical range of values for masses of SMBH, we obtain M∙∠σp for different profiles. An analytical relation p=(2γ+6)/(2+γ) is found which is in reasonable agreement with observations (for γ=0.75−1.4, p=3.6−5.3). Assuming that a proportionality relation holds between the black hole mass and bulge mass, M∙=fMb, and applying this to several galaxies, we find the individual best fit values of p as a function of f; also by minimizing χ2, we find the best fit global p and f. For Nuker profiles, we find that p=3.81±0.004 and f=(1.23±0.09)×10−3 which are consistent with the observed ranges. en_US
dc.language.iso en en_US
dc.publisher Indian Academy of Sciences en_US
dc.subject Galaxies: bulges en_US
dc.subject Galaxies: nuclei en_US
dc.subject Galaxies: elliptical en_US
dc.subject Galaxies: kinematics and dynamics en_US
dc.subject Galaxies: structure en_US
dc.title M∙ − σ relation in spherical systems en_US
dc.type Article en_US


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