Impact of metallicity on the evolution of young star clusters

Mapelli, Michela; Bressan, A.

doi:10.1093/mnras/stt119

Cited by 31 publications

(19 citation statements)

References 81 publications

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“…The preponderance of metal-rich galaxies might have a major impact on the mass of BBH mergers, as metal-rich stars are expected to produce lower-mass BHs (Mapelli et al 2009;Belczynski et al 2010;Mapelli et al 2010;Mapelli & Bressan 2013;Spera et al 2015;Belczynski et al 2016b;Giacobbo et al 2018) and to lead to smaller merger efficiency Figure 1. Sketch of the procedure adopted to create the BBH catalog.…”

Section: Metallicity Distributionmentioning

confidence: 99%

“…This difference between the mass range of LVC BHs and BHs in X-ray binaries might be ascribed to the detectorʼs sensitivity, which is much higher for larger BH masses (see, for instance, , to other observational biases (e.g., X-ray binaries for which we have a dynamical mass measurement are within few Mpc in a predominantly metal-rich environment), to a predominantly different formation channel (Perna et al 2019), or to gravitational lensing (Broadhurst et al 2018). One of the critical parameters affecting the natal mass of BHs is the metallicity of their progenitors, Z, as metal-poor stars are expected to produce heavier BHs (Mapelli et al 2009(Mapelli et al , 2010Belczynski et al 2010;Mapelli & Bressan 2013;Spera et al 2015) and to have a higher merger efficiency than metal-rich stars (Dominik et al 2013;Askar et al 2017;Giacobbo et al 2018). Merging BBHs form either from isolated binary stellar evolution in galactic fields (Tutukov & Yungelson 1973;Portegies Zwart & McMillan 2000;Belczynski et al 2002Belczynski et al , 2010Belczynski et al , 2016aHurley et al 2002;Mapelli & Bressan 2013;Marchant et al 2016;Giacobbo et al 2018;Arca Sedda & Benacquista 2019;Spera et al 2019, and references therein), or through dynamical interactions in dense young massive clusters (Portegies Zwart & McMillan 2000;Banerjee et al 2010;Ziosi et al 2014;Mapelli 2016;Banerjee 2017Banerjee , 2018di Carlo et al 2019a;Rastello et al 2019), globular clusters (Sigurdsson & Phinney 1993;Lee 1995;Miller & Hamilton 2002;…”

Section: Introductionmentioning

confidence: 99%

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Fingerprints of Binary Black Hole Formation Channels Encoded in the Mass and Spin of Merger Remnants

Sedda¹,

Mapelli

Spera

et al. 2020

ApJ

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Binary black holes (BBHs) are thought to form in different environments, including the galactic field and (globular, nuclear, young, and open) star clusters. Here, we propose a method to estimate the fingerprints of the main BBH formation channels associated with these different environments. We show that the metallicity distribution of galaxies in the local universe along with the relative amount of mergers forming in the field or in star clusters determine the main properties of the BBH population. Our fiducial model predicts that the heaviest merger to date, GW170729, originated from a progenitor that underwent 2-3 merger events in a dense star cluster, possibly a galactic nucleus. The model predicts that at least one merger remnant out of a hundred BBH mergers in the local universe has mass <  M M 90 110 rem  , and one in a thousand can reach a mass as large as  M M 250 rem . Such massive black holes would bridge the gap between stellar-mass and intermediate-mass black holes. The relative number of low-and high-mass BBHs can help us unravel the fingerprints of different formation channels. Based on the assumptions of our model, we expect that isolated binaries are the main channel of BBH merger formation if~70% of the whole BBH population has remnants with masses < M 50  , whereas 6% of remnants having masses > M 75  points to a significant subpopulation of dynamically formed BBH binaries.

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Section: Metallicity Distributionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Fingerprints of Binary Black Hole Formation Channels Encoded in the Mass and Spin of Merger Remnants

Sedda¹,

Mapelli

Spera

et al. 2020

ApJ

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“…These black holes may well be slightly more massive than other Galactic stellar mass black holes, but further observations will be required to confirm this possibility (Strader et al 2012). Why no ULXs exist in Galactic globular clusters is so far unexplained, but it may be related to the metallicity (Mapelli & Bressan 2013) or simply because the Galactic globular cluster system is small and thus no such objects may be expected.…”

Section: Where Do Ulxs Reside?mentioning

confidence: 99%

Variability in Ultra-luminous X-ray Sources

Webb

Cseh

Kirsten

2014

Publ. Astron. Soc. Aust.

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Many upcoming surveys, particularly in the radio and optical domains, are designed to probe either the temporal and/or the spatial variability of a range of astronomical objects. In the light of these high resolution surveys, we review the subject of ultra-luminous X-ray (ULX) sources, which are thought to be accreting black holes for the most part. We also discuss the sub-class of ULXs known as the hyper-luminous X-ray sources, which may be accreting intermediate mass black holes. We focus on some of the open questions that will be addressed with the new facilities, such as the mass of the black hole in ULXs, their temporal variability and the nature of the state changes, their surrounding nebulae, and the nature of the region in which ULXs reside.

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“…"hyperstellar-mass black holes", as the authors coined, and previously discussed by e.g. also Heger et al 2003;Mapelli et al 2008;Zampieri & Roberts 2009;Mapelli et al 2010;Belczynski et al 2010a;Fryer et al 2012;Mapelli & Bressan 2013;Ziosi et al 2014;Spera et al 2015.…”

Section: Introductionmentioning

confidence: 99%

Stellar black hole binary mergers in open clusters

Rastello

Amaro-Seoane

Sedda

et al. 2018

Monthly Notices of the Royal Astronomical Society

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In this paper we study the evolution of a primordial black hole binary (BHB) in a sample of over 1500 direct-summation N−body simulations of small-and intermediatesize isolated star clusters as proxies of galactic open clusters. The BHBs have masses in the range of the first LIGO/Virgo detections. Some of our models show a significant hardening of the BHB in a relatively short time. Some of them merge within the cluster, while ejected binaries, typically, have exceedingly long merger timescales. The perturbation of stars around BHB systems is key to induce their coalescence. The BHBs which merge in the cluster could be detected with a delay of a few years between space detectors, as future LISA, and ground-based ones, due to their relatively high eccentricity. Under our assumptions, we estimate a BHB merger rate of R mrg ∼ 2 yr −1 Gpc −3 . We see that in many cases the BHB triggers tidal disruption events which, however, are not linked to the GW emission. Open cluster-like systems are, hence, a promising environment for GWs from BHBs and tidal disruptions. In this article we address the evolution of a BHB in an open cluster with a suit of 1500 direct-summation N−body simulations. We model the evolution of the BHB with properties similar to what can be expected to be detected by LIGO/Virgo (Amaro-Seoane & Chen 2016), using different representations of small-and intermediate-mass isolated open star clusters.Our cluster models are considered as a proxy of the

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Impact of metallicity on the evolution of young star clusters

Cited by 31 publications

References 81 publications

Fingerprints of Binary Black Hole Formation Channels Encoded in the Mass and Spin of Merger Remnants

Fingerprints of Binary Black Hole Formation Channels Encoded in the Mass and Spin of Merger Remnants

Variability in Ultra-luminous X-ray Sources

Stellar black hole binary mergers in open clusters

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