The influence of black holes on the binary population of the globular cluster Palomar 5

Author:

Wang Long12ORCID,Gieles Mark34ORCID,Baumgardt Holger5ORCID,Li Chengyuan12,Pang Xiaoying67,Tang Baitian12

Affiliation:

1. School of Physics and Astronomy, Sun Yat-sen University , Daxue Road, 519082 Zhuhai , China

2. CSST Science Center for the Guangdong-Hong Kong-Macau Greater Bay Area , 519082 Zhuhai , China

3. Institut de Ciències del Cosmos (ICCUB), Universitat de Barcelona (IEEC-UB) , Martí i Franquès 1, E-08028 Barcelona , Spain

4. ICREA , Pg. Lluís Companys 23, E-08010 Barcelona , Spain

5. School of Mathematics and Physics, The University of Queensland , St. Lucia, QLD 4072 , Australia

6. Department of Physics, Xi’an Jiaotong-Liverpool University , 111 Ren’ai Road, Suzhou Dushu Lake Science and Education Innovation District,   Suzhou Industrial Park, 215123 Suzhou , P. R. China

7. Shanghai Key Laboratory for Astrophysics, Shanghai Normal University , 100 Guilin Road, 200234 Shanghai , P. R. China

Abstract

ABSTRACT The discovery of stellar-mass black holes (BHs) in globular clusters (GCs) raises the possibility of long-term retention of BHs within GCs. These BHs influence various astrophysical processes, including merger-driven gravitational waves and the formation of X-ray binaries. They also impact cluster dynamics by heating and creating low-density cores. Previous N-body models suggested that Palomar 5, a low-density GC with long tidal tails, may contain more than 100 BHs. To test this scenario, we conduct N-body simulations of Palomar 5 with primordial binaries to explore the influence of BHs on binary populations and the stellar mass function. Our results show that primordial binaries have minimal effect on the long-term evolution. In dense clusters with BHs, the fraction of wide binaries with periods >105 d decreases, and the disruption rate is independent of the initial period distribution. Multi-epoch spectroscopic observations of line-of-sight velocity changes can detect most bright binaries with periods below 104 d, significantly improving velocity dispersion measurements. Four BH-MS binaries in the model with BHs suggests their possible detection through the same observation method. Including primordial binaries leads to a flatter inferred mass function because of spatially unresolved binaries, leading to a better match of the observations than models without binaries, particularly in Palomar 5’s inner region. Future observations should focus on the cluster velocity dispersion and binaries with periods of 104–105 d in Palomar 5’s inner and tail regions to constrain BH existence.

Funder

Sun Yat-sen University

Fundamental Research Funds for the Central Universities

National Natural Science Foundation of China

NSFC

China Manned Space

Spanish Ministry of Science and Innovation

Publisher

Oxford University Press (OUP)

Subject

Space and Planetary Science,Astronomy and Astrophysics

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