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Globular cluster ejection, infall, and the host dark matter halo of the Pegasus dwarf galaxy

Citation

Leaman, R and Ruiz-Lara, T and Cole, AA and Beasley, MA and Boecker, A and Fahrion, K and Bianchini, P and Falcon-Barroso, J and Webb, J and Sills, A and Mastrobuono-Battisti, A and Neumayer, N and Sippel, AC, Globular cluster ejection, infall, and the host dark matter halo of the Pegasus dwarf galaxy, Monthly Notices of the Royal Astronomical Society, 492, (4) pp. 5102-5120. ISSN 0035-8711 (2020) [Refereed Article]


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Copyright Statement

Copyright 2020 The Authors. This article has been accepted for publication in Monthly Notices of the Royal Astronomical Society : 2020 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society. All rights reserved.

DOI: doi:10.1093/mnras/staa004

Abstract

Recent photometric observations revealed a massive, extended (MGC ≳ 105M; Rh ∼ 14pc) globular cluster (GC) in the central region (D3D ≲ 100pc) of the low-mass (M* ∼ 5נ106M) dwarf irregular galaxy Pegasus. This massive GC offers a unique opportunity to study star cluster inspiral as a mechanism for building up nuclear star clusters, and the dark matter (DM) density profile of the host galaxy. Here, we present spectroscopic observations indicating that the GC has a systemic velocity of ΔV= 38km s−1 relative to the host galaxy, and an old, metal-poor stellar population. We run a suite of orbital evolution models for a variety of host potentials (cored to cusped) and find that the GCs observed tidal radius (which is ∼3times larger than the local Jacobi radius), relaxation time, and relative velocity are consistent with it surviving inspiral from a distance of Dgal ≳ 700pc (up to the maximum tested value of Dgal= 2000pc). In successful trials, the GC arrives to the galaxy centre only within the last ∼1.41Gyr. Orbits that arrive in the centre and survive are possible in DM haloes of nearly all shapes, however to satisfy the GCs structural constraints a galaxy DM halo with mass MDM ≃ 62נ109 M, concentration c ≃ 13.70.6, and an inner slope to the DM density profile of −0.9 ≤ γ ≤ −0.5 is preferred. The gas densities necessary for its creation and survival suggest the GC could have formed initially near the dwarfs centre, but then was quickly relocated to the outskirts where the weaker tidal field permitted an increased size and relaxation time with the latter preserving the former during subsequent orbital decay.

Item Details

Item Type:Refereed Article
Keywords:galaxies: evolution; galaxies: star formation; galaxies: stellar content
Research Division:Physical Sciences
Research Group:Astronomical sciences
Research Field:Cosmology and extragalactic astronomy
Objective Division:Expanding Knowledge
Objective Group:Expanding knowledge
Objective Field:Expanding knowledge in the physical sciences
UTAS Author:Cole, AA (Associate Professor Andrew Cole)
ID Code:139069
Year Published:2020
Deposited By:Physics
Deposited On:2020-05-25
Last Modified:2020-06-17
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