EDGE – Dark matter or astrophysics? Breaking dark matter heating degeneracies with H I rotation in faint dwarf galaxies
Low-mass dwarf galaxies are expected to reside within dark matter haloes that have a pristine, ‘cuspy’ density profile within their stellar half-light radii. This is because they form too few stars to significantly drive dark matter heating through supernovadriven outflows. Here, we study such simul...
| Autores: | , , , , , , , , |
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| Tipo de recurso: | artículo |
| Estado: | Versión publicada |
| Fecha de publicación: | 2024 |
| País: | España |
| Institución: | Consejo Superior de Investigaciones Científicas (CSIC) |
| Repositorio: | DIGITAL.CSIC. Repositorio Institucional del CSIC |
| OAI Identifier: | oai:digital.csic.es:10261/357273 |
| Acceso en línea: | http://hdl.handle.net/10261/357273 |
| Access Level: | acceso abierto |
| Palabra clave: | Methods: numerical Galaxies: structure Galaxies: evolution Dark matter |
| Sumario: | Low-mass dwarf galaxies are expected to reside within dark matter haloes that have a pristine, ‘cuspy’ density profile within their stellar half-light radii. This is because they form too few stars to significantly drive dark matter heating through supernovadriven outflows. Here, we study such simulated faint systems (104 ≤ M ≤ 2 × 106 M) drawn from high-resolution (3 pc) cosmological simulations from the ‘Engineering Dwarf Galaxies at the Edge of galaxy formation’ (EDGE) project. We confirm that these objects have steep and rising inner dark matter density profiles at z = 0, little affected by galaxy formation effects. But five dwarf galaxies from the suite also showcase a detectable H I reservoir (MH I ≈ 105 − 106 M), analogous to the observed population offaint, H I-bearing dwarf galaxies. These reservoirs exhibit episodes of ordered rotation, opening windowsforrotation curve analysis. Within actively star-forming dwarfs, stellar feedback easily disrupts the tenuous H I discs (vφ,g ≈ 10 km s−1), making rotation short-lived (<< 150 Myr) and more challenging to interpret for dark matter inferences. In contrast, we highlight a long-lived (≥ 500 Myr) and easy-to-interpret H I rotation curve extending to ≈ 2 r1/2,3D in a quiescent dwarf, that has not formed new stars since z = 4. This stable gas disc is supported by an oblate dark matter halo shape that drives high-angular momentum gas flows. Our results strongly motivate further searches for H I in rotation curves in the observed population of H I-bearing low-mass dwarfs, that provide a key regime to disentangle the respective roles of dark matter microphysics and galaxy formation effects in driving dark matter heating. |
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