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Intermediate-mass black holes in Galactic globular clusters

Published online by Cambridge University Press:  18 January 2010

Carolina Pepe  and
Leonardo J. Pellizza
Carolina Pepe
Affiliation:
Instituto de Astronomía y Física del Espacio, UBA–CONICET, C.C. 67, Suc. 28 (C1428ZAA), Buenos Aires, Argentina email: carolinap@iafe.uba.ar, pellizza@iafe.uba.ar
Leonardo J. Pellizza
Affiliation:
Instituto de Astronomía y Física del Espacio, UBA–CONICET, C.C. 67, Suc. 28 (C1428ZAA), Buenos Aires, Argentina email: carolinap@iafe.uba.ar, pellizza@iafe.uba.ar
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Abstract

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Over the last few years, different observations have suggested the existence of intermediate-mass (~103 M⊙) black holes in the centers of globular clusters. However, the issue is still a matter of debate, as current observations have alternative explanations. We previously developed a hydrodynamical model for the interstellar medium in these systems to explain the luminosity of the central X-ray source found in NGC 6388, assuming a black hole accreting from the insterstellar medium. Here, we explore the predictions of our model regarding the flow of the interstellar matter in the inner cluster regions and find that the density and velocity profiles could help to determine the presence of a central black hole as well as its mass.

Keywords

ISM: kinematics and dynamicsaccretionaccretion disks
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 5 , Symposium S266: Star clusters: basic galactic building blocks throughout time and space , August 2009 , pp. 491 - 494
Copyright
Copyright © International Astronomical Union 2010

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