scholarly journals Constraints on the Self‐Interaction Cross Section of Dark Matter from Numerical Simulations of the Merging Galaxy Cluster 1E 0657−56

2008 ◽  
Vol 679 (2) ◽  
pp. 1173-1180 ◽  
Author(s):  
Scott W. Randall ◽  
Maxim Markevitch ◽  
Douglas Clowe ◽  
Anthony H. Gonzalez ◽  
Marusa Bradač
Keyword(s):  
Dark Matter ◽  
Numerical Simulations ◽  
Cross Section ◽  
Galaxy Cluster ◽  
The Self ◽  
Interaction Cross Section

Direct Constraints on the Dark Matter Self‐Interaction Cross Section from the Merging Galaxy Cluster 1E 0657−56

2004 ◽  
Vol 606 (2) ◽  
pp. 819-824 ◽  
Author(s):  
M. Markevitch ◽  
A. H. Gonzalez ◽  
D. Clowe ◽  
A. Vikhlinin ◽  
W. Forman ◽  
...  
Keyword(s):  
Dark Matter ◽  
Cross Section ◽  
Galaxy Cluster ◽  
Interaction Cross Section

NEW LIMITS ON THE WIMP COLD DARK MATTER INTERACTION CROSS SECTION FROM THE UK EXPERIMENT

COSMO-97 ◽  
1998 ◽  
Author(s):  
T. Ali ◽  
T. J. Sumner ◽  
J. J. Quenby ◽  
A. Bewick ◽  
N. J. T. Smith ◽  
...  
Keyword(s):  
Dark Matter ◽  
Cross Section ◽  
Cold Dark Matter ◽  
Interaction Cross Section ◽  
Matter Interaction ◽  
The Uk

scholarly journals Inferring the dark matter velocity anisotropy to the cluster edge

2020 ◽  
Vol 500 (3) ◽  
pp. 3151-3161
Author(s):  
Jacob Svensmark ◽  
Steen H Hansen ◽  
Davide Martizzi ◽  
Ben Moore ◽  
Romaine Tessier
Keyword(s):  
Dark Matter ◽  
Numerical Simulations ◽  
Galaxy Cluster ◽  
Dynamical Property ◽  
Large Error ◽  
New Method ◽  
Bright Galaxy ◽  
X Ray ◽  
Velocity Anisotropy ◽  
Error Bars

ABSTRACT Dark matter (DM) dominates the properties of large cosmological structures such as galaxy clusters, and the mass profiles of the DM have been inferred for these equilibrated structures for years by using cluster X-ray surface brightnesses and temperatures. A new method has been proposed, which should allow us to infer a dynamical property of the DM, namely the velocity anisotropy. For the gas, a similar velocity anisotropy is zero due to frequent collisions; however, the collisionless nature of DM allows it to be non-trivial. Numerical simulations have for years found non-zero and radially varying DM velocity anisotropies. Here we employ the method proposed by Hansen & Piffaretti, and developed by Høst et al. to infer the DM velocity anisotropy in the bright galaxy cluster Perseus, to near five times the radii previously obtained. We find the DM velocity anisotropy to be consistent with the results of numerical simulations, however, still with large error bars. At half the virial radius, we find the DM velocity anisotropy to be non-zero at 1.7$\, \sigma$, lending support to the collisionless nature of DM.

scholarly journals Dark matter self-interactions from spin-2 mediators

2021 ◽  
Vol 81 (10) ◽  
Author(s):  
Yoo-Jin Kang ◽  
Hyun Min Lee
Keyword(s):  
Dark Matter ◽  
Cross Section ◽  
Scattering Cross Section ◽  
The Self ◽  
Leading Order ◽  
Resonance Effects ◽  
Scattering Cross ◽  
Born Cross Section ◽  
Massive Spin ◽  
Type Potential

AbstractWe propose a new mechanism for rendering dark matter self-interacting in the presence of a massive spin-2 mediator. The derived Yukawa-type potential for dark matter is independent of the spins of dark matter in the leading order of the momentum expansion, so are the resulting non-perturbative effects for the dark matter self-scattering. We find that both the Born cross section and relatively mild resonance effects assist to make the self-scattering cross section velocity-dependent. We discuss how to evade the current indirect bounds on dark matter annihilations and show that the model is marginally compatible with perturbative unitarity in the ghost-free realization of the massive spin-2 particle.

Structure of dark matter haloes of Milky Way satellite galaxies in SIDM universes

2018 ◽  
Vol 14 (S344) ◽  
pp. 498-501
Author(s):  
Takashi Okamoto
Keyword(s):  
Dark Matter ◽  
Cross Section ◽  
Galaxy Formation ◽  
Luminosity Function ◽  
Milky Way ◽  
Dwarf Galaxies ◽  
Interaction Cross Section ◽  
Large Cross Section ◽  
Stellar Feedback ◽  
Satellite Galaxies

AbstractSelf-interacting dark matter (SIDM) can create sufficiently large cores in dark matter haloes of dwarf galaxies if the self-interaction cross-section is sufficiently large on scales of dwarf galaxies. Such a large cross-section can be realized without changing the densities and shapes of cluster-size haloes by introducing a velocity dependent cross-section. Lowering the central densities of dwarf-size haloes, however, may change the strength of stellar feedback required to reproduce observed properties of dwarf galaxies such as the luminosity function of the Milky Way’s satellite galaxies. We perform simulations of galaxy formation by employing such a velocity dependent self-interaction cross-section to investigate the coupled effect of SIDM and feedback.

Current limits on the cold dark matter interaction cross section obtained by the UK collaboration

1999 ◽  
Vol 70 (1-3) ◽  
pp. 74-78 ◽  
Author(s):  
T.J. Sumner ◽  
J.J. Quenby ◽  
A. Bewick ◽  
N.J.T. Smith ◽  
W.G. Jones ◽  
...  
Keyword(s):  
Dark Matter ◽  
Cross Section ◽  
Cold Dark Matter ◽  
Interaction Cross Section ◽  
Matter Interaction ◽  
The Uk

scholarly journals Multi-scalar signature of self-interacting dark matter in the NMSSM and beyond

2021 ◽  
Vol 2021 (9) ◽  
Author(s):  
Jinmian Li ◽  
Junle Pei ◽  
Cong Zhang
Keyword(s):  
Monte Carlo Simulation ◽  
Monte Carlo ◽  
Dark Matter ◽  
Cross Section ◽  
High Energy ◽  
The Self ◽  
Majorana Fermion ◽  
Scalar Boson ◽  
Analytical Expression

Abstract This work studies the self-interacting dark matter (SIDM) scenario in the general NMSSM and beyond, where the dark matter is a Majorana fermion and the force mediator is a scalar boson. An improved analytical expression for the dark matter (DM) self-interacting cross section which takes into account the Born level effects is proposed. Due to the large couplings and light mediator in SIDM scenario, the DM/mediator will go through multiple branchings if they are produced with high energy. Based on the Monte Carlo simulation of the showers in the DM sector, we obtain the multiplicities and the spectra of the DM/mediator from the Higgsino production and decay at the LHC for our benchmark points.

scholarly journals Velocity independent constraints on spin-dependent DM-nucleon interactions from IceCube and PICO

2020 ◽  
Vol 80 (9) ◽  
Author(s):  
M. G. Aartsen ◽  
◽  
M. Ackermann ◽  
J. Adams ◽  
J. A. Aguilar ◽  
...  
Keyword(s):  
Dark Matter ◽  
Velocity Distribution ◽  
Cross Section ◽  
Local Density ◽  
Bubble Chamber ◽  
High Energy ◽  
The Self ◽  
The Sun ◽  
The Galaxy ◽  
Spin Dependent Scattering

AbstractAdopting the Standard Halo Model (SHM) of an isotropic Maxwellian velocity distribution for dark matter (DM) particles in the Galaxy, the most stringent current constraints on their spin-dependent scattering cross-section with nucleons come from the IceCube neutrino observatory and the PICO-60 $$\hbox {C}_3\hbox {F}_8$$ C 3 F 8 superheated bubble chamber experiments. The former is sensitive to high energy neutrinos from the self-annihilation of DM particles captured in the Sun, while the latter looks for nuclear recoil events from DM scattering off nucleons. Although slower DM particles are more likely to be captured by the Sun, the faster ones are more likely to be detected by PICO. Recent N-body simulations suggest significant deviations from the SHM for the smooth halo component of the DM, while observations hint at a dominant fraction of the local DM being in substructures. We use the method of Ferrer et al. (JCAP 1509: 052, 2015) to exploit the complementarity between the two approaches and derive conservative constraints on DM-nucleon scattering. Our results constrain $$\sigma _{\mathrm{SD}} \lesssim 3 \times 10^{-39} \mathrm {cm}^2$$ σ SD ≲ 3 × 10 - 39 cm 2 ($$6 \times 10^{-38} \mathrm {cm}^2$$ 6 × 10 - 38 cm 2 ) at $$\gtrsim 90\%$$ ≳ 90 % C.L. for a DM particle of mass 1 TeV annihilating into $$\tau ^+ \tau ^-$$ τ + τ - ($$b\bar{b}$$ b b ¯ ) with a local density of $$\rho _{\mathrm{DM}} = 0.3~\mathrm {GeV/cm}^3$$ ρ DM = 0.3 GeV / cm 3 . The constraints scale inversely with $$\rho _{\mathrm{DM}}$$ ρ DM and are independent of the DM velocity distribution.

scholarly journals Neutron Stars and Dark Matter

Universe ◽  
2020 ◽  
Vol 6 (12) ◽  
pp. 222
Author(s):  
Antonino Del Popolo ◽  
Morgan Le Delliou ◽  
Maksym Deliyergiyev
Keyword(s):  
Dark Matter ◽  
Neutron Star ◽  
Neutron Stars ◽  
Cross Section ◽  
Galactic Center ◽  
Interaction Strength ◽  
Dark Matter Particle ◽  
Galactic Centre ◽  
Interaction Cross Section ◽  
Neutron Star Mass

Neutron stars change their structure with accumulation of dark matter. We study how their mass is influenced from the environment. Close to the sun, the dark matter accretion from the neutron star does not have any effect on it. Moving towards the galactic center, the density increase in dark matter results in increased accretion. At distances of some fraction of a parsec, the neutron star acquire enough dark matter to have its structure changed. We show that the neutron star mass decreases going towards the galactic centre, and that dark matter accumulation beyond a critical value collapses the neutron star into a black hole. Calculations cover cases varying the dark matter particle mass, self-interaction strength, and ratio between the pressure of dark matter and ordinary matter. This allow us to constrain the interaction cross section, σdm, between nucleons and dark matter particles, as well as the dark matter self-interaction cross section.

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