Scattering, damping, and acoustic oscillations: Simulating the structure of dark matter halos with relativistic force carriers

Buckley, Matthew R.; Zavala, Jesús; Cyr-Racine, Francis-Yan; Sigurdson, Kris; Vogelsberger, Mark

doi:10.1103/physrevd.90.043524

Cited by 118 publications

(156 citation statements)

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“…4.2), and this has in fact been the initial motivation for introducing SIDM models [350]. Although the extra damping (through selfinteraction [351] or collisions with standard particles such as radiation [352]) is a feature of various dark matter models, the existing large-scale structure constraints so far favor no observable deviations from the standard cold dark matter picture. Such deviations on very small scales may however be observable in the CMB [353], and can be looked for using future small-scale CMB experiments.…”

Section: New Particles and Structure Formationmentioning

confidence: 99%

BeyondΛCDM: Problems, solutions, and the road ahead

Bull

Akrami

Adamek

et al. 2016

Physics of the Dark Universe

420

210

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Despite its continued observational successes, there is a persistent (and growing) interest in extending cosmology beyond the standard model, ΛCDM. This is motivated by a range of apparently serious theoretical issues, involving such questions as the cosmological constant problem, the particle nature of dark matter, the validity of general relativity on large scales, the existence of anomalies in the CMB and on small scales, and the predictivity and testability of the inflationary paradigm. In this paper, we summarize the current status of ΛCDM as a physical theory, and review investigations into possible alternatives along a number of different lines, with a particular focus on highlighting the most promising directions. While the fundamental problems are proving reluctant to yield, the study of alternative cosmologies has led to considerable progress, with much more to come if hopes about forthcoming high-precision observations and new theoretical ideas are fulfilled.Keywords: cosmology -dark energy -cosmological constant problem -modified gravitydark matter -early universe Cosmology has been both blessed and cursed by the establishment of a standard model: ΛCDM. On the one hand, the model has turned out to be extremely predictive, explanatory, and observationally robust, providing us with a substantial understanding of the formation of large-scale structure, the state of the early Universe, and the cosmic abundance of different types of matter and energy. It has also survived an impressive battery of precision observational tests -anomalies are few and far between, and their significance is contentious where they do arise -and its predictions are continually being vindicated through the discovery of new effects (B-mode polarization [1] and lensing [2,3] of the cosmic microwave background (CMB), and the kinetic Sunyaev-Zel'dovich effect [4] being some recent examples). These are the hallmarks of a good and valuable physical theory.On the other hand, the model suffers from profound theoretical difficulties. The two largest contributions to the energy content at late times -cold dark matter (CDM) and the cosmological constant (Λ) -have entirely mysterious physical origins. CDM has so far evaded direct detection by laboratory experiments, and so the particle field responsible for it -presumably a manifestation of "beyond the standard model" particle physics -is unknown. Curious discrepancies also appear to exist between the predicted clustering properties of CDM on small scales and observations. The cosmological constant is even more puzzling, giving rise to quite simply the biggest problem in all of fundamental physics: the question of why Λ appears to take such an unnatural value [5,6,7]. Inflation, the theory of the very early Universe, has also been criticized for being fine-tuned and under-predictive [8], and appears to leave many problems either unsolved or fundamentally unresolvable. These problems are indicative of a crisis.From January 14th-17th 2015, we held a conference in Oslo, Norway to surve...

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Section: New Particles and Structure Formationmentioning

confidence: 99%

BeyondΛCDM: Problems, solutions, and the road ahead

Bull

Akrami

Adamek

et al. 2016

Physics of the Dark Universe

420

210

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“…A range of alternatives to vanilla CDM have also been proposed e.g. warm DM (Schaeffer & Silk 1988), interacting DM (Boehm et al 2001;Boehm & Schaeffer 2005;Cyr-Racine & Sigurdson 2013;Chu & Dasgupta 2014), selfinteracting DM (Spergel & Steinhardt 2000;Rocha et al 2013;Vogelsberger et al 2014;Buckley et al 2014), decaying DM (Wang et al 2014) and late-forming DM (Agarwal et al 2015). These "beyond CDM" models generally exhibit a cut-off in the linear matter power spectrum at small scales (high wavenumbers) that translates into a reduced number of low-mass DM haloes compared to collisionless CDM at late times.…”

Section: Introductionmentioning

confidence: 99%

Dark matter–radiation interactions: the structure of Milky Way satellite galaxies

Schewtschenko

Baugh

Wilkinson

et al. 2016

Mon. Not. R. Astron. Soc.

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The full-text may be used and/or reproduced, and given to third parties in any format or medium, without prior permission or charge, for personal research or study, educational, or not-for-pro t purposes provided that:• a full bibliographic reference is made to the original source • a link is made to the metadata record in DRO • the full-text is not changed in any way The full-text must not be sold in any format or medium without the formal permission of the copyright holders.Please consult the full DRO policy for further details. ABSTRACTIn the thermal dark matter (DM) paradigm, primordial interactions between DM and Standard Model particles are responsible for the observed DM relic density. In Boehm et al. (2014), we showed that weak-strength interactions between DM and radiation (photons or neutrinos) can erase smallscale density fluctuations, leading to a suppression of the matter power spectrum compared to the collisionless cold DM (CDM) model. This results in fewer DM subhaloes within Milky Way-like DM haloes, implying a reduction in the abundance of satellite galaxies. Here we use very high resolution N -body simulations to measure the dynamics of these subhaloes. We find that when interactions are included, the largest subhaloes are less concentrated than their counterparts in the collisionless CDM model and have rotation curves that match observational data, providing a new solution to the "too big to fail" problem.

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“…Quantitatively [47], we have M cut 1.7 × 10 8 (T kd /keV) −3 M , such that T kd 0.5 keV suppresses formation of DM protohalos smaller than about 10 9 M , and eases the missing satellites problem [48]. It is important to note that the acoustic damping cut-off in our model is different in shape (oscillatory, with powerlaw envelope) [49,50], from the free-streaming cut-off in warm dark matter models (exponential). As a result, Lyman-α and other constraints on warm dark matter [51,52] cannot be applied directly [49,50].…”

mentioning

confidence: 99%

“…It is important to note that the acoustic damping cut-off in our model is different in shape (oscillatory, with powerlaw envelope) [49,50], from the free-streaming cut-off in warm dark matter models (exponential). As a result, Lyman-α and other constraints on warm dark matter [51,52] cannot be applied directly [49,50].…”

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confidence: 99%

Dark Radiation Alleviates Problems with Dark Matter Halos

Chu

Dasgupta

2014

Phys. Rev. Lett.

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We show that a scalar and a fermion charged under a global U (1) symmetry can not only explain the existence and abundance of dark matter (DM) and dark radiation (DR), but also imbue DM with improved scattering properties at galactic scales, while remaining consistent with all other observations. Delayed DM-DR kinetic decoupling eases the missing satellites problem, while scalarmediated self-interactions of DM ease the cusp vs. core and too big to fail problems. In this scenario, DM is expected to be pseudo-Dirac and have a mass 100 keV m χ 10 GeV. The predicted DR may be measurable using the primordial elemental abundances from big bang nucleosynthesis (BBN), and using the cosmic microwave background (CMB). Introduction.-Cosmological and astrophysical data now firmly point towards the existence of new nonrelativistic particles, dubbed dark matter (DM), and there is a vigorous experimental program underway to discover these particles and measure their properties. Dark radiation (DR), on the other hand, refers to new relativistic particles that contribute to the cosmological energy density but are otherwise decoupled from ordinary matter and radiation. There is neither clear evidence nor a definitive exclusion, but several independent analyses of cosmological data show tantalizing hints for DR [1][2][3][4][5], most recently to reconcile the results from the Planck Collaboration [6] with those from BICEP2 Collaboration [7].

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Scattering, damping, and acoustic oscillations: Simulating the structure of dark matter halos with relativistic force carriers

Cited by 118 publications

References 159 publications

BeyondΛCDM: Problems, solutions, and the road ahead

BeyondΛCDM: Problems, solutions, and the road ahead

Dark matter–radiation interactions: the structure of Milky Way satellite galaxies

Dark Radiation Alleviates Problems with Dark Matter Halos

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