On the ejection of dark matter from globular clusters

Hurst, Travis J; Zentner, Andrew R.

doi:10.1093/mnras/staa1065

Cited by 3 publications

(2 citation statements)

References 37 publications

(21 reference statements)

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“…see Moore 1996;Saitoh et al 2006;Creasey et al 2019) and internal dynamical processes (e.g. see Bromm & Clarke 2002;Mashchenko & Sills 2005;Hurst & Zentner 2020) as well as feedback processes (Pontzen & Governato 2012; Davis et al 2014). It could be possible that some remnant of the DM halo is still preserved in the peripheries of present-day GCs (e.g.…”

Section: Introductionmentioning

confidence: 99%

The First Billion Years project: Finding infant globular clusters at z = 6

Phipps

Khochfar

Varri

et al. 2020

A&A

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Aims. We aim to conduct an assessment of the demographics of substructures in cosmological simulations to identify low-mass stellar systems at high redshift, with a particular focus on globular cluster (GC) candidates. Methods. We explored a suite of high-resolution cosmological simulations from the First Billion Years Project (FiBY) at z ≥ 6. All substructures within the simulations have been identified with the SUBFIND algorithm. From our analysis, two distinct groups of objects emerge. We hypothesise that the substructures in the first group, which appear to have a high baryon fraction (fb ≥ 0.95), are possible infant GC candidates. Objects belonging to the second group have a high stellar fraction (f* ≥ 0.95) and show a potential resemblance to infant ultra-faint dwarf galaxies. Results. The high baryon fraction objects identified in this study are characterised by a stellar content similar to the one observed in present-day GCs, but they still contain a high gas fraction (fgas ∼ 0.95) and a relatively low amount of dark matter. They are compact systems, with densities higher than the average population of FiBY systems at the same stellar mass. Their sizes are consistent with recent estimates based on the first observations of possible proto-GCs at high redshifts. These types of infant GC candidates appear to be more massive and more abundant in massive host galaxies, indicating that the assembly of galaxies via mergers may play an important role in building several GC-host scaling relations. Specifically, we express the relation between the mass of the most massive infant GC and its host stellar mass as log(Mcl) = (0.31 ± 0.15) log (M*, gal + (4.17 ± 1.06). We also report a new relation between the most massive infant GC and the parent specific star formation rate of the form log(Mcl) = (0.85 ± 0.30) log (sSFR)+α that describes the data at both low and high redshift. Finally, we assess the present-day GC mass (GC number) – halo mass relation offers a satisfactory description of the behaviour of our infant GC candidates at high redshift, suggesting that such a relation may be set at formation.

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Section: Introductionmentioning

confidence: 99%

The First Billion Years project: Finding infant globular clusters at z = 6

Phipps

Khochfar

Varri

et al. 2020

A&A

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“…However, such over-dense DM cores in a globular cluster are quite speculative and not yet well established. It has in fact been shown that globular clusters do not have any DM over-densities [85][86][87][88]. Hence, the explanation of a sub-Chandrasekhar or O(1) M BH due to a PBH transit hinges on the contentious assumption of a high DM density in globular clusters, and remains uncertain until the provenance of globular clusters is settled.…”

Section: Excluded From Existence Of Psr J0437-4715mentioning

confidence: 99%

Low Mass Black Holes from Dark Core Collapse

Dasgupta,

Laha,

Ray

2020

Preprint

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Unusual masses of the black holes being discovered by gravitational wave experiments pose fundamental questions about the origin of these black holes. Black holes with masses smaller than the Chandrasekhar limit ≈ 1.4 M are essentially impossible to produce through stellar evolution. We propose a new channel for production of sub-Chandrasekhar mass black holes: stellar objects can catastrophically accrete non-annihilating dark matter in dense regions of the Universe, owing to interactions of dark matter and ordinary matter, and the dark core subsequently collapses. The wide range of allowed dark matter masses allows a smaller effective Chandrasekhar limit, and thus smaller mass black holes. We point out several avenues to test our proposal.

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