dc.contributor.author |
Safonova, M |
|
dc.contributor.author |
Shastri, P |
|
dc.date.accessioned |
2009-12-14T19:39:46Z |
|
dc.date.available |
2009-12-14T19:39:46Z |
|
dc.date.issued |
2010-01 |
|
dc.identifier.citation |
Astrophysics and Space Science, Vol. 325, No. 1, pp. 47 - 58 |
en |
dc.identifier.issn |
0004-640X |
|
dc.identifier.uri |
http://hdl.handle.net/2248/4937 |
|
dc.description |
The original publication is available at springerlink.com |
en |
dc.description |
Restricted Access |
|
dc.description.abstract |
Empirical evidence for both stellar mass black holes (M (aEuro cent)< 10(2) M (aS (TM))) and supermassive black holes (SMBHs, M (aEuro cent)> 10(5) M (aS (TM))) 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 sigma (c) , the M (aEuro cent)-sigma relation. On the other hand, evidence for "intermediate-mass" black holes (IMBHs, with masses in the range 100-10(5) M (aS (TM))) 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 (aEuro cent)-sigma 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 (aEuro cent)-sigma 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 (aEuro cent)-sigma relation. |
en |
dc.language.iso |
en |
en |
dc.publisher |
Springer |
en |
dc.relation.uri |
http://dx.doi.org/10.1007/s10509-009-0170-z |
en |
dc.rights |
© Springer |
en |
dc.subject |
Black holes |
en |
dc.subject |
Globular clusters |
en |
dc.title |
Extrapolating SMBH correlations down the mass scale: the case for IMBHs in globular clusters |
en |
dc.type |
Article |
en |