Unravelling the interplay between SIDM and baryons in MW haloes: defining where baryons dictate heat transfer

Rose, Jonah C.; Torrey, Paul; Vogelsberger, Mark; O'Neil, Stephanie

doi:10.1093/mnras/stac3634

Cited by 9 publications

(12 citation statements)

References 89 publications

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“…The MW host halo exhibits a ∼1 kpc core in our SIDM simulation, which is expected given that our cross section is greater than ∼0.1 cm 2 g −1 at the MW halo velocity scale (e.g., Nadler et al 2020a). Note that this core is not expected to remain in a full hydrodynamic setting because SIDM efficiently responds to a baryon-dominated central gravitational potential, thus regenerating a cusp (Kaplinghat et al 2014;Sameie et al 2018;Robles et al 2019;Rose et al 2023).…”

Section: Cosmological Zoom-in Simulationsmentioning

confidence: 99%

“…In future work, it will be particularly interesting to perform hydrodynamic simulations in the presence of core collapse. We expect that the cuspy density profiles of collapsed halos remain resilient to feedback as self-interactions can redistribute energy rapidly (e.g., see Sameie et al 2021;Rose et al 2023 for studies of MW-mass SIDM halos). This may provide a mechanism to form compact dwarf galaxies in SIDM even when feedback is strong.…”

Section: Future Workmentioning

confidence: 99%

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Strong Dark Matter Self-interactions Diversify Halo Populations within and surrounding the Milky Way

Yang

Nadler

2023

ApJ

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We perform a high-resolution cosmological zoom-in simulation of a Milky Way (MW)–like system, which includes a realistic Large Magellanic Cloud analog, using a large differential elastic dark matter self-interaction cross section that reaches ≈100 cm2 g−1 at relative velocities of ≈10 km s−1, motivated by the diverse and orbitally dependent central densities of dwarf galaxies within and surrounding the MW. We explore the effects of dark matter self-interactions on satellite, splashback, and isolated halos through their abundance, central densities, maximum circular velocities, orbital parameters, and correlations between these variables. We use an effective constant cross section model to analytically predict the stages of our simulated halos’ gravothermal evolution, demonstrating that deviations from the collisionless R max – V max relation can be used to select deeply core-collapsed halos, where V max is a halo’s maximum circular velocity, and R max is the radius at which it occurs. We predict that a sizable fraction (≈20%) of subhalos with masses down to ≈108 M ⊙ is deeply core collapsed in our SIDM model. Core-collapsed systems form ≈10% of the isolated halo population down to the same mass; these isolated, core-collapsed halos would host faint dwarf field galaxies with extremely steep central density profiles. Finally, most halos with masses above ≈109 M ⊙ are core-forming in our simulation. Our study thus demonstrates how self-interactions diversify halo populations in an environmentally dependent fashion within and surrounding MW-mass hosts, providing a compelling avenue to address the diverse dark matter distributions of observed dwarf galaxies.

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Section: Cosmological Zoom-in Simulationsmentioning

confidence: 99%

Section: Future Workmentioning

confidence: 99%

Strong Dark Matter Self-interactions Diversify Halo Populations within and surrounding the Milky Way

Yang

Nadler

2023

ApJ

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“…It has been shown that for galaxies with Milky Way-like masses and above the interplay of baryons and self-interactions can lead to cuspier density profiles than in CDM (e.g. Despali et al 2019;Rose et al 2022). In principle, baryons could also affect the ability to constrain the angular dependence with the abundance of satellites.…”

Section: Discussionmentioning

confidence: 99%

“…Such studies were performed not only with DM-only (DMO) simulations but also within hydrodynamical cosmological simulations (e.g. Vogelsberger et al 2014;Robertson et al 2019Robertson et al , 2020Rose et al 2022;Mastromarino et al 2023;Rahimi et al 2023). They are well-motivated for different angular dependencies, including forward-enhanced crosssections from light mediator models (e.g.…”

Section: Introductionmentioning

confidence: 99%

Cosmological simulations with rare and frequent dark matter self-interactions

Fischer

Brüggen

Schmidt-Hoberg

et al. 2022

Monthly Notices of the Royal Astronomical Society

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Dark matter (DM) with self-interactions is a promising solution for the small-scale problems of the standard cosmological model. Here we perform the first cosmological simulation of frequent DM self-interactions, corresponding to small-angle DM scatterings. The focus of our analysis lies in finding and understanding differences to the traditionally assumed rare DM (large-angle) self scatterings. For this purpose, we compute the distribution of DM densities, the matter power spectrum, the two-point correlation function and the halo and subhalo mass functions. Furthermore, we investigate the density profiles of the DM haloes and their shapes. We find that overall large-angle and small-angle scatterings behave fairly similarly with a few exceptions. In particular, the number of satellites is considerably suppressed for frequent compared to rare self-interactions with the same cross-section. Overall we observe that while differences between the two cases may be difficult to establish using a single measure, the degeneracy may be broken through a combination of multiple ones. For instance, the combination of satellite counts with halo density or shape profiles could allow discriminating between rare and frequent self-interactions. As a by-product of our analysis, we provide - for the first time - upper limits on the cross-section for frequent self-interactions.

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“…For smaller self-interacting cross sections, the velocity distribution is non-Maxwellian, while for the velocity-dependent models, the velocity distribution is close to those extracted from collision-less DM-only simulations. High resolution SIDM simulations including baryons have recently become available [44][45][46]. Yet, a study of the local DM distribution and its implications for DM direct detection using such simulations had not been performed and is the aim of this work.…”

Section: Introductionmentioning

confidence: 99%

The local dark matter distribution in self-interacting dark matter halos

Rahimi

Vienneau²,

Bozorgnia³

et al. 2023

J. Cosmol. Astropart. Phys.

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We study the effects of dark matter self-interactions on the local dark matter distribution in selected Milky Way-like galaxies in the EAGLE hydrodynamical simulations. The simulations were run with two different self-interacting dark matter models, a constant and velocity-dependent self-interaction cross-section. We find that the local dark matter velocity distribution of the Milky Way-like halos in the simulations with dark matter self-interactions and baryons are generally similar to those extracted from cold collisionless dark matter simulations with baryons. In both cases, the local dark matter speed distributions agree well with their best fit Maxwellian distributions. Including baryons in the simulations with or without dark matter self-interactions increases the local dark matter density and shifts the dark matter speed distributions to higher speeds. To study the implications for direct detection, we compute the dark matter halo integrals obtained directly from the simulations and compare them to those obtained from the best fit Maxwellian velocity distribution. We find that a Maxwellian distribution provides a good fit to the halo integrals of most halos, without any significant difference between the results of different dark matter self-interaction models.

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Unravelling the interplay between SIDM and baryons in MW haloes: defining where baryons dictate heat transfer

Cited by 9 publications

References 89 publications

Strong Dark Matter Self-interactions Diversify Halo Populations within and surrounding the Milky Way

Strong Dark Matter Self-interactions Diversify Halo Populations within and surrounding the Milky Way

Cosmological simulations with rare and frequent dark matter self-interactions

The local dark matter distribution in self-interacting dark matter halos

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