MOCCA-Survey Database I. Unravelling black hole subsystems in globular clusters

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MOCCA-Survey Database I. Unravelling black hole subsystems in globular clusters. / Arca Sedda, Manuel; Askar, Abbas; Giersz, Mirek.

I: Monthly Notices of the Royal Astronomical Society, Vol. 479, Nr. 4, 01.07.2018, s. 4652-4664.

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TY - JOUR

T1 - MOCCA-Survey Database I. Unravelling black hole subsystems in globular clusters

AU - Arca Sedda, Manuel

AU - Askar, Abbas

AU - Giersz, Mirek

PY - 2018/7/1

Y1 - 2018/7/1

N2 - In this paper, we discuss how the structural and observational properties of globular clusters (GCs) can be used to infer the presence of a black hole system (BHS) inhabiting their inner regions. We propose a novel way to define the BHS size as the radius from the GC centre within which half of the mass is in stellar mass BHs and the remaining half is in other stars. Using this definition, similar to the well-known concept of ‘influence radius’, we found a ‘fundamental plane’ connecting the BHS typical density with the GC central surface density profile, total luminosity and observational half-mass radius. Our approach allows us to define a unique way to connect the observational GCs parameters with their dark content. Comparing our results with observed Milky Way GCs, we found that many of them likely host, at the present time, as many as several hundreds of BHs. These BHS are characterized by a relatively low typical density, pc−3 and composed of relatively massive BHs, with average masses in the range m BHS =14−22M ⊙ mBHS=14−22M⊙⁠. We also show that a similar approach can be used to find Milky Way GCs potentially hosting an intermediate-mass black hole.

AB - In this paper, we discuss how the structural and observational properties of globular clusters (GCs) can be used to infer the presence of a black hole system (BHS) inhabiting their inner regions. We propose a novel way to define the BHS size as the radius from the GC centre within which half of the mass is in stellar mass BHs and the remaining half is in other stars. Using this definition, similar to the well-known concept of ‘influence radius’, we found a ‘fundamental plane’ connecting the BHS typical density with the GC central surface density profile, total luminosity and observational half-mass radius. Our approach allows us to define a unique way to connect the observational GCs parameters with their dark content. Comparing our results with observed Milky Way GCs, we found that many of them likely host, at the present time, as many as several hundreds of BHs. These BHS are characterized by a relatively low typical density, pc−3 and composed of relatively massive BHs, with average masses in the range m BHS =14−22M ⊙ mBHS=14−22M⊙⁠. We also show that a similar approach can be used to find Milky Way GCs potentially hosting an intermediate-mass black hole.

U2 - 10.1093/mnras/sty1859

DO - 10.1093/mnras/sty1859

M3 - Article

VL - 479

SP - 4652

EP - 4664

JO - Monthly Notices of the Royal Astronomical Society

T2 - Monthly Notices of the Royal Astronomical Society

JF - Monthly Notices of the Royal Astronomical Society

SN - 1365-2966

IS - 4

ER -