The Effects of Dark Matter and Baryonic Physics on the Milky Way Subhalo Population in the Presence of the Large Magellanic Cloud

Given recent developments in our understanding of the Large Magellanic Cloud's (LMC) impact on the Milky Way's (MW) dark matter subhalo population, we compare the signatures of dark matter and baryonic physics on subhalos in MW systems with realistic LMC analogs. In particular, we study th...

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Bibliographic Details
Published in:Astrophysical journal. Letters 2021-10, Vol.920 (1), p.L11
Main Authors: Nadler, Ethan O., Banerjee, Arka, Adhikari, Susmita, Mao, Yao-Yuan, Wechsler, Risa H.
Format: Article
Language:English
Subjects:
Abundance
Analogs
Anisotropy
ASTRONOMY AND ASTROPHYSICS
Baryons
Dark matter
Disruption
Dwarf galaxies
Galactic disk
Galaxy abundances
Magellanic clouds
Milky Way
Milky Way dark matter halo
Physics
Radial distribution
Relative abundance
Satellite observation
Spatial distribution
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Summary:Given recent developments in our understanding of the Large Magellanic Cloud's (LMC) impact on the Milky Way's (MW) dark matter subhalo population, we compare the signatures of dark matter and baryonic physics on subhalos in MW systems with realistic LMC analogs. In particular, we study the effects of self-interacting dark matter (SIDM), warm dark matter (WDM), and the Galactic disk on the peak maximum circular velocity ( V peak ) function, radial distribution, and spatial distribution of MW and LMC-associated subhalos using cosmological dark matter-only zoom-in simulations of MW+LMC systems. For a fixed abundance of subhalos expected to host dwarf galaxies ( V peak ≳ 20 km s −1 ), SIDM and WDM can produce a similar mass-dependent suppression of the subhalo V peak function, while disk disruption is mass independent. Subhalos in the inner regions of the MW are preferentially disrupted by both self-interactions and the disk, while suppression in WDM is radially independent. The relative abundance of LMC-associated subhalos is not strongly affected by disk disruption or WDM, but is significantly suppressed in SIDM due to self-interactions with the LMC at early times and with the MW during LMC infall at late times, erasing spatial anisotropy in the MW subhalo population. These results provide avenues to distinguish dark matter and baryonic physics by combining properties of the MW and LMC subhalo populations probed by upcoming observations of satellite galaxies and stellar streams.
ISSN:2041-8205
2041-8213
DOI:10.3847/2041-8213/ac29c1