The hot gas mass fraction in halos. From Milky Way-like groups to massive clusters

Abstract

By using eROSITA data in the eFEDS area, we provide a measure of the hot gas fraction vs. halo mass relation over the largest halo mass range, from Milky Way-sized halos to massive clusters, and to the largest radii ever probed so far in local systems. To cope with the incompleteness and selection biases of the X-ray selection, we apply the stacking technique in eROSITA data of a highly complete and tested sample of optically selected groups. The method has been extensively tested on mock observations. In massive clusters, the hot gas alone provides a baryon budget within $R_{200}$ consistent with the cosmic value. At the same time, at the group mass scale, it accounts only for 20-40% of it. The hot gas fraction vs. halo mass relation is well-fitted by a power law, with a consistent shape and a normalization varying at maximum by a factor of 2 from $r_{500}$ to $r_{200}$. Such a relation is consistent with other works in the literature that consider X-ray survey data at the same depth as eFEDS. However, it provides a lower average gas fraction in the group regime than works based on X-ray bright group samples. The comparison of the observed relation with the predictions of several hydrodynamical simulations (BAHAMAS, FLAMINGO, SIMBA, Illustris, IllustrisTNG, MillenniumTNG, and Magneticum) shows that all simulations but Magneticum and SIMBA overpredict the gas fraction, with the largest discrepancy (up to a factor of 3) in the massive group-poor cluster halo mass range. We emphasize the need for mechanisms that can effectively expel gas to larger radii in galaxy groups without excessively quenching star formation in their member galaxies. Current hydrodynamical simulations face a significant challenge in balancing their subgrid physics: none can sufficiently evacuate gas from the halo virial region without negatively impacting the properties of the resident galaxy population.

submitted to A&A, 11 pages, 8 figures. Abstract reduced for ArXiv submission

References in corpus (44)

• The EAGLE project: Simulating the evolution and assembly of galaxies and their environments
• Simba: Cosmological Simulations with Black Hole Growth and Feedback
• Introducing the Illustris Project: the evolution of galaxy populations across cosmic time
• Galaxy Groups in the SDSS DR4: I. The Catalogue and Basic Properties
• A unified model for AGN feedback in cosmological simulations of structure formation
• The eROSITA Final Equatorial Depth Survey (eFEDS): The X-ray catalog
• Weighing the Giants IV: Cosmology and Neutrino Mass
• Scaling Properties of a Complete X-ray Selected Galaxy Group Sample
• The FLAMINGO project: cosmological hydrodynamical simulations for large-scale structure and galaxy cluster surveys
• The star formation main sequence and stellar mass assembly of galaxies in the Illustris simulation
• Galaxy And Mass Assembly (GAMA): Data Release 4 and the z < 0.1 total and z < 0.08 morphological galaxy stellar mass functions
• Calibration of the galaxy cluster M_500-Y_X relation with XMM-Newton
• Simulations of AGN feedback in galaxy clusters and groups: impact on gas fractions and the Lx-T scaling relation
• Unifying X-ray Scaling Relations from Galaxies to Clusters
• Quenched fractions in the IllustrisTNG simulations: comparison with observations and other theoretical models
• The MillenniumTNG Project: The hydrodynamical full physics simulation and a first look at its galaxy clusters
• Constraining the Scatter in the Mass-Richness Relation of maxBCG Clusters With Weak Lensing and X-ray Data
• The eROSITA Final Equatorial-Depth Survey (eFEDS): Catalog of galaxy clusters and groups
• Feedback from Active Galactic Nuclei in Galaxy Groups
• The Atacama Cosmology Telescope: Modeling the Gas Thermodynamics in BOSS CMASS galaxies from Kinematic and Thermal Sunyaev-Zel'dovich Measurements
• The eROSITA Final Equatorial-Depth Survey (eFEDS): Identification and characterization of the counterparts to the point-like sources
• The eROSITA Final Equatorial-Depth Survey (eFEDS): The AGN Catalogue and its X-ray Spectral Properties
• Simulating Groups and the IntraGroup Medium: The Surprisingly Complex and Rich Middle Ground Between Clusters and Galaxies
• Feedback reshapes the baryon distribution within haloes, in halo outskirts, and beyond: the closure radius from dwarfs to massive clusters
• LoCuSS: Scaling relations between galaxy cluster mass, gas, and stellar content
• The eROSITA Final Equatorial-Depth Survey (eFEDS): Galaxy Clusters and Groups in Disguise
• The eROSITA Final Equatorial-Depth Survey (eFEDS): X-ray Properties and Scaling Relations of Galaxy Clusters and Groups
• The physics inside the scaling relations for X-ray galaxy clusters: gas clumpiness, gas mass fraction and slope of the pressure profile
• SP(k) -- A hydrodynamical simulation-based model for the impact of baryon physics on the non-linear matter power spectrum
• Relative distribution of dark matter, gas, and stars around cosmic filaments in the IllustrisTNG simulation
• The eROSITA Final Equatorial-Depth Survey (eFEDS): Optical confirmation, redshifts, and properties of the cluster and group catalog
• The hot circumgalactic medium in the eROSITA All-Sky Survey II. Scaling relations between X-ray luminosity and galaxies' mass
• The morphology and kinematics of the gaseous circumgalactic medium of Milky Way mass galaxies -- II. comparison of IllustrisTNG and Illustris simulation results
• On the accretion history of galaxy clusters: temporal and spatial distribution
• Galaxy And Mass Assembly: search for a population of high-entropy galaxy groups
• Mapping "out-of-the-box" the properties of the baryons in massive halos
• Detecting Galaxy Groups and AGNs populating the local Universe in the eROSITA era
• The eROSITA Final Equatorial-Depth Survey (eFEDS): Presenting The Demographics of X-ray Emission From Normal Galaxies
• X-ray surface brightness and gas density profiles of galaxy clusters up to 3*R500c with SRG/eROSITA
• Simulation view of galaxy clusters with low X-ray surface brightness
• Detecting clusters and groups of galaxies populating the local Universe in large optical spectroscopic surveys
• Average X-ray properties of galaxy groups. From Milky Way-like halos to massive clusters
• The perils of stacking optically selected groups in eROSITA data. The Magneticum perspective
• The XXL Survey XLV. Linking the ages of optically selected groups to their X-ray emission

Cited by in corpus (3)

• MIGHTEE: The dark matter haloes, duty cycle and mechanical feedback from radio-AGN up to $z\sim 2.5$
• The SRG/eROSITA All-Sky Survey. Detection of shock-heated gas beyond the halo boundary into the accretion region
• Entropy plateaus can emerge from gas replacement at a characteristic halo mass in simulated groups and clusters of galaxies