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http://hdl.handle.net/2445/213432
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DC Field | Value | Language |
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dc.contributor.author | Foote, Hayden R. | - |
dc.contributor.author | Besla, Gurtina | - |
dc.contributor.author | Mocz, Philip | - |
dc.contributor.author | Garavito-Camargo, Nicolás | - |
dc.contributor.author | Lancaster, Lachlan | - |
dc.contributor.author | Sparre, Martin | - |
dc.contributor.author | Cunningham, Emily C. | - |
dc.contributor.author | Vogelsberger, Mark | - |
dc.contributor.author | Gómez, Facundo A. | - |
dc.contributor.author | Laporte, Chervin F. P. | - |
dc.date.accessioned | 2024-06-19T19:07:45Z | - |
dc.date.available | 2024-06-19T19:07:45Z | - |
dc.date.issued | 2023 | - |
dc.identifier.issn | 0004-637X | - |
dc.identifier.uri | http://hdl.handle.net/2445/213432 | - |
dc.description.abstract | The Large Magellanic Cloud (LMC) will induce a dynamical friction (DF) wake on infall to the Milky Way (MW). The MW's stellar halo will respond to the gravity of the LMC and the dark matter (DM) wake, forming a stellar counterpart to the DM wake. This provides a novel opportunity to constrain the properties of the DM particle. We present a suite of high-resolution, windtunnel-style simulations of the LMC's DF wake that compare the structure, kinematics, and stellar tracer response of the DM wake in cold DM (CDM), with and without self-gravity, versus fuzzy DM (FDM) with ma = 10−23 eV. We conclude that the self-gravity of the DM wake cannot be ignored. Its inclusion raises the wake's density by ∼10%, and holds the wake together over larger distances (∼50 kpc) than if self-gravity is ignored. The DM wake's mass is comparable to the LMC's infall mass, meaning the DM wake is a significant perturber to the dynamics of MW halo tracers. An FDM wake is more granular in structure and is ∼20% dynamically colder than a CDM wake, but with comparable density. The granularity of an FDM wake increases the stars' kinematic response at the percent level compared to CDM, providing a possible avenue of distinguishing a CDM versus FDM wake. This underscores the need for kinematic measurements of stars in the stellar halo at distances of 70–100 kpc. | - |
dc.format.extent | 1 p. | - |
dc.format.mimetype | application/pdf | - |
dc.language.iso | eng | - |
dc.publisher | Institute of Physics (IOP) | - |
dc.relation.isformatof | Reproducció del document publicat a: https://doi.org/10.3847/1538-4357/ace533 | - |
dc.relation.ispartof | Astrophysical Journal, 2023 | - |
dc.relation.uri | https://doi.org/10.3847/1538-4357/ace533 | - |
dc.rights | (c) American Astronomical Society, 2023 | - |
dc.source | Articles publicats en revistes (Física Quàntica i Astrofísica) | - |
dc.subject.classification | Halos (Meteorologia) | - |
dc.subject.classification | Matèria fosca (Astronomia) | - |
dc.subject.classification | Cinemàtica | - |
dc.subject.classification | Núvols | - |
dc.subject.other | Halos (Meteorology) | - |
dc.subject.other | Dark matter (Astronomy) | - |
dc.subject.other | Kinematics | - |
dc.subject.other | Clouds | - |
dc.title | Structure, Kinematics, and Observability of the Large Magellanic Cloud's Dynamical Friction Wake in Cold versus Fuzzy Dark Matter | - |
dc.type | info:eu-repo/semantics/article | - |
dc.type | info:eu-repo/semantics/publishedVersion | - |
dc.identifier.idgrec | 742275 | - |
dc.date.updated | 2024-06-19T19:07:50Z | - |
dc.rights.accessRights | info:eu-repo/semantics/openAccess | - |
Appears in Collections: | Articles publicats en revistes (Institut de Ciències del Cosmos (ICCUB)) Articles publicats en revistes (Física Quàntica i Astrofísica) |
Files in This Item:
File | Description | Size | Format | |
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841733.pdf | 2.77 MB | Adobe PDF | View/Open |
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