Black hole at the center of the globular cluster M15: Estimation of the mass and specific angular momentum

Kiselev, A. A.; Gnedin, Yu. N.; Shakht, N. A.; Grosheva, E. A.; Piotrovich, M. Yu.; Natsvlishvili, T. M.

doi:10.1134/s1063773708080033

Cited by 9 publications

(8 citation statements)

References 17 publications

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“…Though mass estimates for these two black holes are not from gas or stellar dynamics (the reason why AGN, for example, were excluded from GRG sample), these measurements were made by † a factor of two uncertainty has been assigned to this BH mass. ‡ the reported masses for this cluster range from 1 to 9 × 10 3 M ⊙ ; the listed mass is the most probable value, see latest (Kiselev et al 2008). multiple methods and are considered to be quite reliable.…”

Section: Constraints On the M • − σ Relation By Globular Clusters Canmentioning

confidence: 84%

Extrapolating SMBH correlations down the mass scale: the case for IMBHs in globular clusters

Safonova

Shastri

2009

Astrophys Space Sci

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Empirical evidence for both stellar mass black holes (M • < 10 2 M ⊙ ) and supermassive black holes (SMBHs,is well established. Moreover, every galaxy with a bulge appears to host a SMBH, whose mass is correlated with the bulge mass, and even more strongly with the central stellar velocity dispersion σ c , the M • − σ relation. On the other hand, evidence for "intermediate-mass" black holes (IMBHs, with masses in the range 100-10 5 M ⊙ ) is relatively sparse, with only a few mass measurements reported in globular clusters (GCs), dwarf galaxies and low-mass AGNs. We explore the question of whether globular clusters extend the M • − σ relationship for galaxies to lower black hole masses and find that available data for globular clusters are consistent with the extrapolation of this relationship. We use this extrapolated M • − σ relationship to predict the putative black hole masses of those globular clusters where existence of central IMBH was proposed. We discuss how globular clusters can be used as a constraint on theories making specific predictions for the low-mass end of the M • − σ relation.

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Section: Constraints On the M • − σ Relation By Globular Clusters Canmentioning

confidence: 84%

Extrapolating SMBH correlations down the mass scale: the case for IMBHs in globular clusters

Safonova

Shastri

2009

Astrophys Space Sci

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“…24, where it was used to calculate the orbit of the star S2 rotating about the center of the galaxy and to estimate the mass of a supermassive black hole at the center of the galaxy. The results obtained by this method were also compared there with the results obtained by methods based on the empirical relationship between the masses of black holes in the central region of galaxies and quasars and the luminosity of these regions in the radio and x-ray ranges.…”

Section: Determination Of the Orbitmentioning

confidence: 99%

Orbit determination and estimate of the component masses

et al. 2010

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Photographic observations of the visual binary star ADS 7251 were made from 1962 through 2006 on the 26-inch refractor at the Pulkovo Observatory. 206 plates were obtained and used to derive about 3000 relative positions. A uniform series of positions of the B-A components of ADS 7251 with errors in one annual average distance ρ and position angle θ of ±0".006 and ±0 o .02, respectively, have been used to determine the elements of the orbit and the sum of the masses of the components. The orbit has been determined using a method of apparent motion parameters developed at Pulkovo. The positions and motions of the components A and B relative to a system of reference stars have also been calculated from 146 of the plates; this made it possible to determine the position of the center of mass and the ratio of the masses of the components. The masses of A and B are 0.57 ¤ M and 0.53 ¤ M , respectively, a result that is consistent with their spectral classes and does not indicate the presence of significant excess mass.

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“…The search for black holes with intermediate masses ( The central objects of globular clusters are currently the most popular candidates for this class of objects [1][2][3][4][5].…”

Section: Introductionmentioning

confidence: 99%

Intermediate-mass black holes in globular clusters: constraints on the spin of a black hole

et al. 2011

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The spin of central black holes with intermediate masses in globular clusters is determined using the well known relationship between the kinetic power of a relativistic jet and the observed radio luminosity of the region closest to a central black hole. The estimate of the magnitude of the spin is based on the knownBlandford-Znajek mechanism. The magnetic field near the event horizon of a black hole is determined using a magnetic coupling mechanism that assumes equality between the densities of the magnetic and kinetic energies of the accreting gas (the Magnetic Coupling Model). The rate of accretion M is derived on the basis of the Bondi-Hoyle mechanism.

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Black hole at the center of the globular cluster M15: Estimation of the mass and specific angular momentum

Cited by 9 publications

References 17 publications

Extrapolating SMBH correlations down the mass scale: the case for IMBHs in globular clusters

Extrapolating SMBH correlations down the mass scale: the case for IMBHs in globular clusters

Orbit determination and estimate of the component masses

Intermediate-mass black holes in globular clusters: constraints on the spin of a black hole

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