Energy transfer from baryons to dark matter as a unified solution to small-scale structure issues of the 
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Popolo, A. Del; Pace, Francesco; Delliou, Morgan Le; Lee, Xi-Guo

doi:10.1103/physrevd.98.063517

Cited by 20 publications

(8 citation statements)

References 122 publications

(230 reference statements)

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“…A weakness of such arguments is that baryonic physics, such as supernovae or AGN activity, can alter the distribution of dark matter in galaxies and clusters in ways that are unaccounted for in dark matter-only simulations. Incorporating baryonic physics in simulations accurately is challenging, and may solve some or even all of the potential problems with ΛCDM on small scales [11][12][13][14][15][16].…”

Section: Jhep10(2020)191mentioning

confidence: 99%

Systematizing the effective theory of self-interacting dark matter

Agrawal¹,

Parikh²,

Reece³

2020

J. High Energ. Phys.

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If dark matter has strong self-interactions, future astrophysical and cosmological observations, together with a clearer understanding of baryonic feedback effects, might be used to extract the velocity dependence of the dark matter scattering rate. To interpret such data, we should understand what predictions for this quantity are made by various models of the underlying particle nature of dark matter. In this paper, we systematically compute this function for fermionic dark matter with light bosonic mediators of vector, scalar, axial vector, and pseudoscalar type. We do this by matching to the nonrelativistic effective theory of self-interacting dark matter and then computing the spin-averaged viscosity cross section nonperturbatively by solving the Schrödinger equation, thus accounting for any possible Sommerfeld enhancement of the low-velocity cross section. In the pseudoscalar case, this requires a coupled-channel analysis of different angular momentum modes. We find, contrary to some earlier analyses, that nonrelativistic effects only provide a significant enhancement for the cases of light scalar and vector mediators. Scattering from light pseudoscalar and axial vector mediators is well described by tree-level quantum field theory.

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Section: Jhep10(2020)191mentioning

confidence: 99%

Systematizing the effective theory of self-interacting dark matter

Agrawal¹,

Parikh²,

Reece³

2020

J. High Energ. Phys.

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“…Even though these problems might be solved invoking baryonic physics (e.g. [14][15][16][17][18][19][20][21][22][23][24][25][26][27][28][29][30][31]), this tension of observations with ΛCDM predictions on small scales makes modifications on these scales appealing.…”

Section: Introductionmentioning

confidence: 99%

Constraining Ultra-light Axions with Galaxy Cluster Number Counts

Diehl,

Weller

2021

Preprint

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In this paper we investigate the potential of current and upcoming cosmological surveys to constrain the mass and abundance of ultra-light axion (ULA) cosmologies with galaxy cluster number counts. ULAs, sometimes also referred to as Fuzzy Dark Matter, are well-motivated in many theories beyond the Standard Model and could potentially solve the ΛCDM small-scale crisis. Galaxy cluster counts provide a robust probe of the formation of structures in the Universe. Their distribution in mass and redshift is strongly sensitive to the underlying linear matter perturbations. In this forecast paper we explore two scenarios, firstly an exclusion limit on axion mass given a no-axion model and secondly constraints on an axion model. With this we obtain lower limits on the ULA mass on the order of m a 10 −24 eV. However, this result depends heavily on the mass of the smallest reliably observable clusters for a given survey. Cluster counts, like many other cosmological probes, display an approximate degeneracy in the ULA mass vs. abundance parameter space, which is dependent on the characteristics of the probe. These degeneracies are different for other cosmological probes. Hence galaxy cluster counts might provide a complementary window on the properties of ultra-light axions.

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“…In this paper, we aim to extend that study to galaxy clusters, including AGN feedback effects. That purpose will lead us to improve and extend the [136] model, using the [25] model for AGN feedback. Building a dwarf galaxies-cluster size halo mass range, including DM and baryonic effects, will enable for the first time the construction of a mass-dependent DM density profile set.…”

Section: Introductionmentioning

confidence: 99%

Cluster density slopes from Dark Matter-Baryons Energy Transfer

Del Popolo,

Delliou,

Deliyergiyev

2021

Preprint

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In this paper, we extend previous works on the relation between mass and the inner slope in dark matter density profiles. We calculate that relation in the mass range going from dwarf galaxies to cluster of galaxies. This was done thanks to a modeling of energy transfer via SN and AGN feedback, as well as via dynamical friction of baryon clumps. We show that, in the mass range above galaxy masses (Groups and clusters), the inner slopemass relation changes its trend. It flattens (towards less cuspy profile) around masses corresponding to groups of galaxies and steepens again for large galaxy cluster masses. The flattening is produced by the AGN outflows (AGN feedback). The one-σ scatter on α is approximately constant in all the mass range (∆α 0.3). This is the first paper extending the inner density profile slope-mass relationship to clusters of galaxies, accounting for the role of baryons. The result can be used to obtain a complete density profile, also taking baryons into account. Such kind of density profile was previously only available for galaxies.

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Energy transfer from baryons to dark matter as a unified solution to small-scale structure issues of the ΛCDM model

Cited by 20 publications

References 122 publications

Systematizing the effective theory of self-interacting dark matter

Systematizing the effective theory of self-interacting dark matter

Constraining Ultra-light Axions with Galaxy Cluster Number Counts

Cluster density slopes from Dark Matter-Baryons Energy Transfer

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