X-ray morphology of cluster-mass haloes in self-interacting dark matter

Abstract

We perform cosmological zoom-in simulations of $19$ relaxed cluster-mass haloes with the inclusion of adiabatic gas in the cold dark matter (CDM) and self-interacting dark matter (SIDM) models. These clusters are selected as dynamically relaxed clusters from a parent simulation with $M_{200}\simeq 1-3\times 10^{15}{\mathrm{M}}_{\odot }$. Both the dark matter and the intracluster gas distributions in SIDM appear more spherical than their CDM counterparts. Mock X-ray images are generated based on the simulations and are compared to the real X-ray images of $84$ relaxed clusters selected from the Chandra and ROSAT archives. We perform ellipse fitting for the isophotes of mock and real X-ray images and obtain the ellipticities at cluster-centric radii of $r\simeq 0.1-0.2R_{200}$. The X-ray isophotes in SIDM models with increasing cross-sections are rounder than their CDM counterparts, which manifests as a systematic shift in the distribution function of ellipticities. Unexpectedly, the X-ray morphology of the observed non-cool-core clusters agrees better with SIDM models with cross-section $(\sigma /m)=0.5-1{\mathrm{cm}}^2/\mathrm{g}$ than CDM and SIDM with $(\sigma /m)=0.1{\mathrm{cm}}^2/\mathrm{g}$. Our statistical analysis indicates that the latter two models are disfavored at the $68\%$ confidence level (as conservative estimates). This conclusion is not altered by shifting the radial range of measurements or applying temperature selection criterion. However, the primary uncertainty originates from the lack of baryonic physics in the adiabatic model, such as cooling, star formation and feedback effects, which still have the potential to reconcile CDM simulations with observations.

Accepted by MNRAS

References in corpus (49)

• The EAGLE project: Simulating the evolution and assembly of galaxies and their environments
• A direct empirical proof of the existence of dark matter
• Introducing the Illustris Project: Simulating the coevolution of dark and visible matter in the Universe
• In the Realm of the Hubble tension $-$ a Review of Solutions
• A Theory of Dark Matter
• Too big to fail? The puzzling darkness of massive Milky Way subhaloes
• Constraints on the Self-Interaction Cross-Section of Dark Matter from Numerical Simulations of the Merging Galaxy Cluster 1E 0657-5
• The non-gravitational interactions of dark matter in colliding galaxy clusters
• Dark Energy Survey Year 3 Results: Cosmology from Cosmic Shear and Robustness to Data Calibration
• Dark Matter and Dark Radiation
• High-resolution mass models of dwarf galaxies from LITTLE THINGS
• Dark Energy Survey Year 3 Results: Cosmology from Cosmic Shear and Robustness to Modeling Uncertainty
• Cores in Dwarf Galaxies from Dark Matter with a Yukawa Potential
• Is dark matter with long-range interactions a solution to all small-scale problems of ΛCDM cosmology?
• Cosmology and Astrophysics from Relaxed Galaxy Clusters II: Cosmological Constraints
• Dwarf galaxies in CDM and SIDM with baryons: observational probes of the nature of dark matter
• Searching for Cool Core Clusters at High redshift
• Is there a "too big to fail" problem in the field?
• GHASP : an H alpha kinematic survey of spiral and irregular galaxies. V. Dark matter distribution in 36 nearby spiral galaxies
• The Causes of Halo Shape Changes Induced by Cooling Baryons: Disks Versus Substructures
• Hydrodynamic Simulation of Non-thermal Pressure Profiles of Galaxy Clusters
• Interacting Dark Sector and Precision Cosmology
• High Resolution Optical Velocity Fields of 11 Low Surface Brightness Galaxies
• The moment of truth for WIMP Dark Matter
• Cosmology and Astrophysics from Relaxed Galaxy Clusters I: Sample Selection
• Scattering, Damping, and Acoustic Oscillations: Simulating the Structure of Dark Matter Halos with Relativistic Force Carriers
• Cosmology with self-interacting sterile neutrinos and dark matter - A pseudoscalar model
• M31 Satellite Masses Compared to LCDM Subhaloes
• Updated constraints on massive neutrino self-interactions from cosmology in light of the $H_0$ tension
• Interacting radiation after Planck and its implications for the Hubble Tension
• SIDM on FIRE: Hydrodynamical Self-Interacting Dark Matter simulations of low-mass dwarf galaxies
• A Step in Understanding the Hubble Tension
• The Onset of Gravothermal Core Collapse in Velocity Dependent Self-Interacting Dark Matter Subhaloes
• The Metallicity of the Intracluster Medium Over Cosmic Time: Further Evidence for Early Enrichment
• Cosmological constraints on multi-interacting dark matter
• Flavor-specific Interaction Favors Strong Neutrino Self-coupling in the Early Universe
• Long Range Interactions in Cosmology: Implications for Neutrinos
• Constraints on secret neutrino interactions after Planck
• The full Boltzmann hierarchy for dark matter-massive neutrino interactions
• Dissipative Dark Matter on FIRE: I. Structural and kinematic properties of dwarf galaxies
• Hints of dark matter-neutrino interactions in Lyman-$\alpha$ data
• Robust quantitative measures of cluster X-ray morphology, and comparisons between cluster characteristics
• SMBH Seeds from Dissipative Dark Matter
• Linear scale bounds on dark matter--dark radiation interactions and connection with the small scale crisis of cold dark matter
• ETHOS -- An effective parametrization and classification for structure formation: the non-linear regime at $z\gtrsim 5$
• ETHOS -- An Effective Theory of Structure Formation: Impact of Dark Acoustic Oscillations on Cosmic Dawn
• Projected Axis Ratios of Galaxy Clusters in the Horizon-AGN Simulation: Impact of Baryon Physics and Comparison with Observations
• Neutrino Interactions in the Late Universe
• SN-driven mechanism of cusp-core transformation: an appraisal

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• Introducing the AIDA-TNG project: galaxy formation in alternative dark matter models
• Gravothermal collapse of Self-Interacting Dark Matter halos as the Origin of Intermediate Mass Black Holes in Milky Way satellites
• Properties and observables of massive galaxies in self-interacting dark matter cosmologies
• Sensitivity of Halo Shape Measurements
• Core collapse in resonant self-interacting dark matter across two decades in halo mass