The GD-1 stellar stream perturber as a core-collapsed self-interacting dark matter halo
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| Format: | Preprint |
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2024
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| _version_ | 1866917880679890944 |
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| author | Zhang, Xingyu Yu, Hai-Bo Yang, Daneng Nadler, Ethan O. |
| author_facet | Zhang, Xingyu Yu, Hai-Bo Yang, Daneng Nadler, Ethan O. |
| contents | The GD-1 stellar stream exhibits spur and gap structures that may result from a close encounter with a dense substructure. When interpreted as a dark matter subhalo, the perturber is denser than predicted in the standard cold dark matter (CDM) model. In self-interacting dark matter (SIDM), however, a halo could evolve into a phase of gravothermal collapse, resulting in a higher central density than its CDM counterpart. We conduct high-resolution controlled N-body simulations to show that a collapsed SIDM halo could account for the GD-1 perturber's high density. We model a progenitor halo with a mass of $3\times10^8~M_\odot$, motivated by a cosmological simulation of a Milky Way analog, and evolve it in the Milky Way's tidal field. For a cross section per mass of $σ/m\approx30-100~{\rm cm^2~g^{-1}}$ at $V_{\rm max }\sim10~{\rm km~s^{-1}}$, the enclosed mass of the SIDM halo within the inner $10~{\rm pc}$ can be increased by more than an order of magnitude compared to its CDM counterpart, leading to a good agreement with the properties of the GD-1 perturber. Our findings indicate that stellar streams provide a novel probe into the self-interacting nature of dark matter. |
| format | Preprint |
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arxiv_https___arxiv_org_abs_2409_19493 |
| institution | arXiv |
| publishDate | 2024 |
| record_format | arxiv |
| spellingShingle | The GD-1 stellar stream perturber as a core-collapsed self-interacting dark matter halo Zhang, Xingyu Yu, Hai-Bo Yang, Daneng Nadler, Ethan O. Astrophysics of Galaxies High Energy Physics - Phenomenology The GD-1 stellar stream exhibits spur and gap structures that may result from a close encounter with a dense substructure. When interpreted as a dark matter subhalo, the perturber is denser than predicted in the standard cold dark matter (CDM) model. In self-interacting dark matter (SIDM), however, a halo could evolve into a phase of gravothermal collapse, resulting in a higher central density than its CDM counterpart. We conduct high-resolution controlled N-body simulations to show that a collapsed SIDM halo could account for the GD-1 perturber's high density. We model a progenitor halo with a mass of $3\times10^8~M_\odot$, motivated by a cosmological simulation of a Milky Way analog, and evolve it in the Milky Way's tidal field. For a cross section per mass of $σ/m\approx30-100~{\rm cm^2~g^{-1}}$ at $V_{\rm max }\sim10~{\rm km~s^{-1}}$, the enclosed mass of the SIDM halo within the inner $10~{\rm pc}$ can be increased by more than an order of magnitude compared to its CDM counterpart, leading to a good agreement with the properties of the GD-1 perturber. Our findings indicate that stellar streams provide a novel probe into the self-interacting nature of dark matter. |
| title | The GD-1 stellar stream perturber as a core-collapsed self-interacting dark matter halo |
| topic | Astrophysics of Galaxies High Energy Physics - Phenomenology |
| url | https://arxiv.org/abs/2409.19493 |