A Detailed Study of the Most Relaxed SPT-selected Galaxy Clusters: Properties of the Cool Core and Central Galaxy

McDonald, Michael; Allen, S. W.; Hlavacek-Larrondo, J.; Mantz, Adam; Bayliss, M.; Benson, B. A.; Brodwin, M.; Bulbul, Esra; Canning, Rebecca; Chiu, I.; Forman, W.; Garmire, G. P.; Gupta, N.; Khullar, Gourav; Mohr, J. J.; Reichardt, C. L.; Schrabback, T.

doi:10.3847/1538-4357/aaf394

Cited by 15 publications

(10 citation statements)

References 99 publications

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“…The Hogan et al (2017) clusters shown in the top panel were chosen mainly for their brightness, and are hence relatively representative of cool-core clusters. The bottom panel shows model fits to four objects from McDonald et al (2019a), which were selected to be the most dynamicallyrelaxed clusters out of the 100 clusters in the South Pole Telescope sample (SPT, Bleem et al 2015). The entropy profiles at 30 − 160 kpc of these clusters is steeper than in the sample shown in the top panel, and similar to the slope predicted by the cooling flow solution, especially in the Phoenix and SPT-CLJ2043-5035 clusters.…”

Section: Clustersmentioning

confidence: 77%

Cooling flow solutions for the circumgalactic medium

Stern

Fielding

Faucher-Giguère

et al. 2019

Monthly Notices of the Royal Astronomical Society

102

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ABSTRACT In several models of galaxy formation feedback occurs in cycles or mainly at high redshift. At times and in regions where feedback heating is ineffective, hot gas in the galaxy halo is expected to form a cooling flow, where the gas advects inward on a cooling timescale. Cooling flow solutions can thus be used as a benchmark for observations and simulations to constrain the timing and extent of feedback heating. Using analytic calculations and idealized 3D hydrodynamic simulations, we show that for a given halo mass and cooling function, steady-state cooling flows form a single-parameter family of solutions, while initially hydrostatic gaseous haloes converge on one of these solutions within a cooling time. The solution is thus fully determined once either the mass inflow rate ${\dot{M}}$ or the total halo gas mass are known. In the Milky Way halo, a cooling flow with ${\dot{M}}$ equal to the star formation rate predicts a ratio of the cooling time to the free-fall time of ∼10, similar to some feedback-regulated models. This solution also correctly predicts observed $\rm{O\,{\small VII}}$ and $\rm{O\,{\small VIII}}$ absorption columns, and the gas density profile implied by $\rm{O\,{\small VII}}$ and $\rm{O\,{\small VIII}}$ emission. These results suggest ongoing heating by feedback may be negligible in the inner Milky-Way halo. Extending similar solutions out to the cooling radius however underpredicts observed $\rm{O\,{\small VI}}$ columns around the Milky-Way and around other low-redshift star-forming galaxies. This can be reconciled with the successes of the cooling flow model with either a mechanism which preferentially heats the $\rm{O\,{\small VI}}$-bearing outer halo, or alternatively if $\rm{O\,{\small VI}}$ traces cool photoionized gas beyond the accretion shock. We also demonstrate that the entropy profiles of some of the most relaxed clusters are reasonably well described by a cooling flow solution.

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Section: Clustersmentioning

confidence: 77%

Cooling flow solutions for the circumgalactic medium

Stern

Fielding

Faucher-Giguère

et al. 2019

Monthly Notices of the Royal Astronomical Society

102

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“…In order to compare the observed luminosity function with the expectations of different cosmological models, we need to adopt a mass calibration. At the moment, the 0.3 < z < 0.6 part of the CODEX scaling relations are not yet tightly constrained, while the available studies extending to a redshift of one argue in favor of the self-similar scaling for these relations outside of the cool core (McDonald et al 2019). Therefore, in this work we consider whether the observed lack of evolution of XLF can be explained by a combination of self-similar evolution of scaling relations and a change in some basic cosmological parameters, limiting the study to Ω M and σ 8 .…”

Section: Evolution Of Cluster X-ray Luminosity Functionmentioning

confidence: 96%

CODEX clusters

Finoguenov

Rykoff

Clerc

et al. 2020

A&A

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Context. Large area catalogs of galaxy clusters constructed from ROSAT All-Sky Survey provide the basis for our knowledge of the population of clusters thanks to long-term multiwavelength efforts to follow up observations of these clusters. Aims. The advent of large area photometric surveys superseding previous, in-depth all-sky data allows us to revisit the construction of X-ray cluster catalogs, extending the study to lower cluster masses and higher redshifts and providing modeling of the selection function. Methods. We performed a wavelet detection of X-ray sources and made extensive simulations of the detection of clusters in the RASS data. We assigned an optical richness to each of the 24 788 detected X-ray sources in the 10 382 square degrees of the Baryon Oscillation Spectroscopic Survey area using red sequence cluster finder redMaPPer version 5.2 run on Sloan Digital Sky Survey photometry. We named this survey COnstrain Dark Energy with X-ray (CODEX) clusters. Results. We show that there is no obvious separation of sources on galaxy clusters and active galactic nuclei (AGN) based on the distribution of systems on their richness. This is a combination of an increasing number of galaxy groups and their selection via the identification of X-ray sources either by chance or by groups hosting an AGN. To clean the sample, we use a cut on the optical richness at the level corresponding to the 10% completeness of the survey and include it in the modeling of the cluster selection function. We present the X-ray catalog extending to a redshift of 0.6. Conclusions. The CODEX suvey is the first large area X-ray selected catalog of northern clusters reaching fluxes of 10−13 ergs s−1 cm−2. We provide modeling of the sample selection and discuss the redshift evolution of the high end of the X-ray luminosity function (XLF). Our results on z < 0.3 XLF agree with previous studies, while we provide new constraints on the 0.3 < z < 0.6 XLF. We find a lack of strong redshift evolution of the XLF, provide exact modeling of the effect of low number statistics and AGN contamination, and present the resulting constraints on the flat ΛCDM.

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“…The systematic mass uncertainty amounts to 7.4%. Column 7: Chandra X-ray mass estimates computed by McDonald et al (2019) assuming the Y X -M scaling relation from Vikhlinin et al (2009). find any non-linear deviations of the multiplicative bias, but we note a shear dependence of the additive bias at |g| > 0.2.…”

Section: Discussionmentioning

confidence: 73%

“…To demonstrate the use of weak lensing measurements in the inner cluster and stronger shear regime we studied three clusters from the 2,500 deg 2 South Pole Telescope Sunyaev-Zel'dovich (SPT-SZ) Survey (Bleem et al 2015). According to their X-ray properties these three clusters are among the most relaxed clus-ters found in the SPT-SZ sample (McDonald et al 2019). These clusters are part of a larger sample of distant SPT-SZ clusters analysed using HST weak lensing data (S18a and S20).…”

Section: Hst Weak Lensing Measurements Of Three Highly Relaxed Cluste...mentioning

confidence: 99%

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Constraining the masses of high-redshift clusters with weak lensing: Revised shape calibration testing for the impact of stronger shears and increased blending

Hernandez-Martin

Schrabback

Hoekstra

et al. 2020

A&A

Self Cite

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Weak lensing measurements suffer from well-known shear estimation biases, which can be partially corrected for with the use of image simulations. In this work we present an analysis of simulated images that mimic Hubble Space Telescope/Advance Camera for Surveys observations of high-redshift galaxy clusters, including cluster specific issues such as non-weak shear and increased blending. Our synthetic galaxies have been generated to have similar observed properties as the background-selected source samples studied in the real images. First, we used simulations with galaxies placed on a grid to determine a revised signal-to-noise-dependent (S/NKSB) correction for multiplicative shear measurement bias, and to quantify the sensitivity of our KSB+ bias calibration to mismatches of galaxy or PSF properties between the real data and the simulations. Next, we studied the impact of increased blending and light contamination from cluster and foreground galaxies, finding it to be negligible for high-redshift (z > 0.7) clusters, whereas shear measurements can be affected at the ∼1% level for lower redshift clusters given their brighter member galaxies. Finally, we studied the impact of fainter neighbours and selection bias using a set of simulated images that mimic the positions and magnitudes of galaxies in Cosmic Assembly Near-IR Deep Extragalactic Legacy Survey (CANDELS) data, thereby including realistic clustering. While the initial SExtractor object detection causes a multiplicative shear selection bias of −0.028 ± 0.002, this is reduced to −0.016 ± 0.002 by further cuts applied in our pipeline. Given the limited depth of the CANDELS data, we compared our CANDELS-based estimate for the impact of faint neighbours on the multiplicative shear measurement bias to a grid-based analysis, to which we added clustered galaxies to even fainter magnitudes based on Hubble Ultra Deep Field data, yielding a refined estimate of ∼ − 0.013. Our sensitivity analysis suggests that our pipeline is calibrated to an accuracy of ∼0.015 once all corrections are applied, which is fully sufficient for current and near-future weak lensing studies of high-redshift clusters. As an application, we used it for a refined analysis of three highly relaxed clusters from the South Pole Telescope Sunyaev-Zeldovich survey, where we now included measurements down to the cluster core (r > 200 kpc) as enabled by our work. Compared to previously employed scales (r > 500 kpc), this tightens the cluster mass constraints by a factor 1.38 on average.

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A Detailed Study of the Most Relaxed SPT-selected Galaxy Clusters: Properties of the Cool Core and Central Galaxy

Cited by 15 publications

References 99 publications

Cooling flow solutions for the circumgalactic medium

Cooling flow solutions for the circumgalactic medium

CODEX clusters

Constraining the masses of high-redshift clusters with weak lensing: Revised shape calibration testing for the impact of stronger shears and increased blending

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