Constraints on the interactions between dark matter and baryons from the x-ray quantum calorimetry experiment

An extraordinarily rich zoo of non-baryonic Dark Matter candidates has been proposed over the last three decades. Here we present a 10-point test that a new particle has to pass, in order to be considered a viable DM candidate: I.) Does it match the appropriate relic density? II.) Is it cold? III.) Is it neutral? IV.) Is it consistent with BBN? V.) Does it leave stellar evolution unchanged? VI.) Is it compatible with constraints on self-interactions? VII.) Is it consistent with direct DM searches? VIII.) Is it compatible with gamma-ray constraints? IX.) Is it compatible with other astrophysical bounds? X.) Can it be probed experimentally?

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“…[161,162] and (more recently and with substantial changes with respect to previous analyses) in Ref. [163].…”

Section: It Results That Champs With Masses Below 10mentioning

confidence: 96%

Dark matter candidates: a ten-point test

Taoso

Bertone

Masiero

2008

J. Cosmol. Astropart. Phys.

173

151

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“…[22,23]. There is also a body of work on direct detection [24][25][26][27][28][29], gravitational lensing [30], gas temperature in clusters [31], big-bang nucleosynthesis [32], cosmic rays [33,34], and cosmic gamma rays [36]. If DM annihilates, then constraints on the Earth's heat flow [35,36] become important, though this constraint disappears if annihilation is absent as could be the case for asymmetric dark matter [6,7].…”

Section: Introductionmentioning

confidence: 99%

Constraining dark matter-baryon scattering with linear cosmology

2014

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We derive constraints on elastic scattering between baryons and dark matter using the cosmic microwave background (CMB) data from the Planck satellite and the Lyman-α forest data from the Sloan Digital Sky Survey. Elastic scattering allows baryons and dark matter to exchange momentum, affecting the dynamics of linear density perturbations in the early Universe. We derive constraints to scattering cross sections of the form σ ∝ v n , allowing for a wide range of velocity dependencies with −4 ≤ n ≤ 2. We improve and correct previous estimates where they exist, including velocityindependent cross section as well as dark matter millicharge and electromagnetic dipole moments. Lyman-α forest data dominates the constraints for n > −3, where the improvement over CMB data alone can be several orders of magnitude. Dark matter-baryon scattering cannot affect the halo mass function on mass scales M > 10 12 M⊙. Our results imply, model-independently, that a baryon in the halo of a galaxy like our own Milky Way, does not scatter from dark matter particles during the age of the galaxy. Contents

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“…The case where the dark particle is stable and identified as dark matter has been treated in a dedicated companion paper, Ref. [6], where a complementarity with low-mass direct detection bounds (like XQC [9][10][11]) has been found. Searches for dark sectors via loops of virtual dark particles include Refs.…”

Section: Introductionmentioning

confidence: 99%

Bounding quantum dark forces

2018

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Dark sectors lying beyond the Standard Model and containing sub-GeV particles which are bilinearly coupled to nucleons would induce quantum forces of the Casimir-Polder type in ordinary matter. Such new forces can be tested by a variety of experiments over many orders of magnitude. We provide a generic interpretation of these experimental searches and apply it to a sample of forces from dark scalars behaving as 1=r 3 , 1=r 5 , 1=r 7 at short range. The landscape of constraints on such quantum forces differs from the one of modified gravity with Yukawa interactions and features, in particular, strong short-distance bounds from molecular spectroscopy and neutron scattering.

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Constraints on the interactions between dark matter and baryons from the x-ray quantum calorimetry experiment

Cited by 104 publications

References 82 publications

Dark matter candidates: a ten-point test

Dark matter candidates: a ten-point test

Constraining dark matter-baryon scattering with linear cosmology

Bounding quantum dark forces

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