billions of solar masses ? We model the dynamical structure of M87 (NGC4486) using high spatial resolution long-slit observations of stellar light in the central regions, two-dimensional stellar light kinematics out to half of the effective radius, and globular cluster velocities out to eight effective radii. The stellar M/L ratio from our models is very similar to that derived from stellar population models of M87.

When the half-mass radius of a cluster is small relative to the overall size, it has a dense core. The reason for the difference in the black hole mass is because we allow the M/L ratio to change with radius.

Stellar dynamical measurements of black hole masses have become the de facto standard method. The dark halo is degenerate with the stellar M/L ratio, which is subsequently degenerate with the black hole mass. The Black Hole Mass, Stellar M/L, and Dark Halo in M87 Karl Gebhardt, Jens Thomas 12 pages, accepted for publication in the Astrophysical Journal (Submitted on 8 Jun 2009) This bias is especially large for a galaxy with a shallow light profile such as M87, and may not be as severe in galaxies with steeper light profiles … The reason for the difference in the black hole mass is because we allow the M/L ratio to change with radius. We extract the shape of the stellar velocity ellipsoid as a function of radius in M87 from van der Marel's (1994) velocity dispersion data. 4. model NGC 4649, a galaxy similar in mass to M87, using X-ray gas emission and find a black hole that is two times larger than the previous stellar dynamical measure of Gebhardt et?al.

Planetary Nebulae and their parent stellar populations. The first image of M87’s black hole suggests it is 6.5 billion times the mass of the sun — close to what was expected based on how stars move around it.

The supermassive black hole has been the subject of several stellar and gas dynamical mass measurements; however, the best current stellar dynamical black hole mass is larger than the gas dynamical determination by a We simultaneously fit for four parameters: black hole mass, dark halo core radius, dark halo circular velocity, and stellar mass-to-light (M/L) ratio. Department of Phys ics and Astronomy, Rutgers Univ ersity, New Brunswic k, NJ 08855. . x is along the major axis. I will give a brief review of how this measurement method works, along with arguments for its overall reliability and caveats. The Stellar Dynamics of M87. An example of this is Messier 3 (M3), which has an overall visible dimension of about 18 arc minutes, but a half-mass radius of only 1.12 arc minutes. M87 is one of the most luminous nearby galaxies and hosts one of the most massive black holes known, making it a very important target for extragalactic studies.

The dark halo is degenerate with the stellar M/L ratio, which is subsequently degenerate with the black hole mass. The dark halo is degenerate with the stellar M/L ratio, which is subsequently degenerate with the black hole mass. The black hole is undeniably large ? Then I will turn my attention to the case of the black hole in M87. The solid black, dashed black and thin red curves represent the stellar surface brightness profile, the stellar surface mass density profile using a constant M/L ratio = 8, and the surface mass density profile using the M/L r profile from Fig. David Merritt. Keep in mind, M87’s black hole is between about 3 and 7 billion times the mass of the Sun, or about 1,000 times more massive than the Milky Way’s black hole, Sagittarius A*. We argue that dynamical models of galaxies that do not include the contribution from a dark halo may produce a biased result for the black hole mass. The stellar M/L ratio from our models is very similar to that derived from stellar population models of M87. Siang Peng Oh. Stellar surface brightness profiles of M87. Tracing the mass assembly of M87 and Intracluster light in the Virgo cluster core - Volume 11 Symposium - Magda Arnaboldi, Alessia Longobardi, Ortwin Gerhard but has a stellar Thus, there is a concern that black hole masses at the upper end of the distribution may be biased. Humphrey et?al. We find a black hole mass of 6.4(±0.5) × 10 9 M sun (the uncertainty is 68% confidence marginalized over the other parameters).

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