Generalizes ultralight DM mass limits from MW satellite abundances to peaked power spectrum models, yielding m > 6e-18 eV scaled by k_* at 95% confidence for different k_* regimes.
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Prompt cusps delay core formation by a factor of ~2 in SIDM halos but later collapse tracks align after rescaling, with ~5% late-stage deviations depending on concentration and outer velocity dispersion.
Host galaxy potentials alone produce complex morphological features in most stellar streams, with pericentric distance as the strongest predictor of smoothness.
DESI data on the GD-1 stream identifies a thin cold core and a hot cocoon with 30% of members whose dispersion is consistent with 11 Gyr of dark matter subhalo heating.
MW-mass SIDM halos bypass core formation and enter immediate core collapse due to baryonic preconditioning, allowing the compact stellar disk and bulge to survive close pericenter passages while the diffuse halo is more easily disrupted.
citing papers explorer
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Warm, not Fuzzy: Generalized Ultralight Dark Matter Limits from Milky Way Satellites
Generalizes ultralight DM mass limits from MW satellite abundances to peaked power spectrum models, yielding m > 6e-18 eV scaled by k_* at 95% confidence for different k_* regimes.
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Role of prompt cusps in driving the core collapse of SIDM halos
Prompt cusps delay core formation by a factor of ~2 in SIDM halos but later collapse tracks align after rescaling, with ~5% late-stage deviations depending on concentration and outer velocity dispersion.
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No Stream Left Unscathed: The imprint of a host galaxy
Host galaxy potentials alone produce complex morphological features in most stellar streams, with pericentric distance as the strongest predictor of smoothness.
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Characterizing the GD-1 Stream with DESI DR2 Data: Thin Stream and Hot Cocoon
DESI data on the GD-1 stream identifies a thin cold core and a hot cocoon with 30% of members whose dispersion is consistent with 11 Gyr of dark matter subhalo heating.
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Bypassed Core Formation in Milky Way-Mass SIDM Halos: Implications for the Local Group Past-Pericenter Scenario
MW-mass SIDM halos bypass core formation and enter immediate core collapse due to baryonic preconditioning, allowing the compact stellar disk and bulge to survive close pericenter passages while the diffuse halo is more easily disrupted.