The XMM Cluster Survey: Present status and latest results

Viana, P. T. P.; Mehrtens, Nicola; Harrison, Craig; Romer, A. K.; Collins, Chris; Hilton, Matthew; Hoyle, B.; Kay, Scott T.; Liddle, Andrew R.; Mayers, Julian A.; Miller, Christopher J.; Rooney, Philip; Sahlén, Martin; Stott, John P.

doi:10.1002/asna.201211881

Cited by 4 publications

(5 citation statements)

References 19 publications

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“…The XCS-SV cluster sample is a product from the XMM Cluster Survey (Lloyd-Davies et al 2011;Mehrtens et al 2012;Viana et al 2013), which searches for galaxy cluster candidates (extended Xray emissions) in the XMM-Newton archival data. The X-ray selected cluster candidates (about 300 in number) are later confirmed with the DES-SV optical images, and have their photometric redshifts estimated using the DES-SV photometric data set.…”

Section: The Xcs-sv Cluster Samplementioning

confidence: 99%

Galaxies in X-ray selected clusters and groups in Dark Energy Survey data – II. Hierarchical Bayesian modelling of the red-sequence galaxy luminosity function

Zhang

Miller

Rooney

et al. 2019

Monthly Notices of the Royal Astronomical Society

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Using ∼ 100 X-ray selected clusters in the Dark Energy Survey Science Verification data, we constrain the luminosity function (LF) of cluster red sequence galaxies as a function of redshift. This is the first homogeneous optical/X-ray sample large enough to constrain the evolution of the luminosity function simultaneously in redshift (0.1 < z < 1.05) and cluster mass (13.5 ≤ log 10 (M 200crit ) ∼< 15.0). We pay particular attention to completeness issues and the detection limit of the galaxy sample. We then apply a hierarchical Bayesian model to fit the cluster galaxy LFs via a Schecter function, including its characteristic break (m * ) to a faint end power-law slope (α). Our method enables us to avoid known issues in similar analyses based on stacking or binning the clusters. We find weak and statistically insignificant (∼ 1.9σ) evolution in the faint end slope α versus redshift. We also find no dependence in α or m * with the X-ray inferred cluster masses. However, the amplitude of the LF as a function of cluster mass is constrained to ∼ 20% precision. As a by-product of our algorithm, we utilize the correlation between the LF and cluster mass to provide an improved estimate of the individual cluster masses as well as the scatter in true mass given the X-ray inferred masses. This technique can be applied to a larger sample of X-ray or optically selected clusters from the Dark Energy Survey, significantly improving the sensitivity of the analysis.Galaxy clusters are special for both cosmology and astrophysics studies. As the structures that correspond to the massive end of halo mass function, they are sensitive probes of the ΛCDM cos-

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Section: The Xcs-sv Cluster Samplementioning

confidence: 99%

Galaxies in X-ray selected clusters and groups in Dark Energy Survey data – II. Hierarchical Bayesian modelling of the red-sequence galaxy luminosity function

Zhang

Miller

Rooney

et al. 2019

Monthly Notices of the Royal Astronomical Society

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“…The XMM Cluster Survey serendipitously searches for galaxy cluster (and group) candidates in the XMM-Newton archive (Lloyd-Davies et al 2011;Mehrtens et al 2012;Viana et al 2013). The cluster candidates are then verified with optical/infrared imaging data, which confirm the existence of red sequence galaxies.…”

Section: The Des-xcs Cluster and Group Samplementioning

confidence: 99%

GALAXIES IN X-RAY SELECTED CLUSTERS AND GROUPS IN DARK ENERGY SURVEY DATA. I. STELLAR MASS GROWTH OF BRIGHT CENTRAL GALAXIES SINCE z ∼ 1.2

Zhang

Miller

McKay

et al. 2016

ApJ

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Using the science verification data of the Dark Energy Survey (DES) for a new sample of 106 X-Ray selected clusters and groups, we study the stellar mass growth of Bright Central Galaxies (BCGs) since redshift 1.2. Compared with the expectation in a semi-analytical model applied to the Millennium Simulation, the observed BCGs become under-massive/under-luminous with decreasing redshift. We incorporate the uncertainties associated with cluster mass, redshift, and BCG stellar mass measurements into analysis of a redshiftdependent BCG-cluster mass relation, m * ∝ ( M200 1.5×10 14 M⊙ ) 0.24±0.08 (1 + z) −0.19±0.34 , and compare the observed relation to the model prediction. We estimate the average growth rate since z = 1.0 for BCGs hosted by clusters of M 200,z = 10 13.8 M ⊙ , at z = 1.0: m * ,BCG appears to have grown by 0.13 ± 0.11 dex, in tension at ∼ 2.5σ significance level with the 0.40 dex growth rate expected from the semi-analytic model. We show that the buildup of extended intra-cluster light after z = 1.0 may alleviate this tension in BCG growth rates.

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“…However, it is possible to discover thousands of clusters through Xray archival data searching. The XMM cluster survey (Lloyd-Davies et al, 2011;Mehrtens et al, 2012;Viana et al, 2013) is a project that conducts this kind of searching.…”

Section: Multi-wavelength Datamentioning

confidence: 99%

“…The XCS-SV cluster sample is a product from the XMM Cluster Survey (Lloyd-Davies et al, 2011;Mehrtens et al, 2012;Viana et al, 2013), which searches for galaxy cluster candidates in XMM-Newton archival data. The XCS-SV sample refers to the confirmed clusters with the DES-SV optical data (Miller et al in prep., henceforce referenced as M15).…”

Section: The Xcs-sv Cluster Samplementioning

confidence: 99%

Looking Wider and Further: The Evolution of Galaxies Inside Galaxy Clusters

Zhang¹

2016

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The road leading to this dissertation was not free from stress or problems, but many people have helped making the journey fulfilling and entertaining. First and Foremost, I want to thank my advisor, Tim McKay, for the training and the guidance. I had no previous experience in astronomy or astrophysics, but Tim took me on without hesitation. Over the years, I learned a great deal from his words and deeds: how to do research, how to write and speak about research results, and how to establish fruitful collaborations. I also feel lucky that Tim helped me raising awareness about work-life balance and being practical while being a perfectionist.I have been working with Chris Miller a lot since 2013. In the past a couple of years, he treated me as one of his own students and taught me many research skills without any reservation. He was keen on making me to pursue extra research, collaboration and observation opportunities. I would have missed many of them if it wasn't him.I learned a lot about cosmology theories and simulations from the weekly meetings organized by Gus and Dragan. Gus is alway pressing me for my latest proposals and paper drafts, and offered many insightful feedbacks. Dave and Greg mentored my research with the DES collaboration, and helped to make sure that I communicate with people about my work. Michigan postdocs Joerg and Jeeseon supervised me when I was a junior graduate student. Michigan alumni Adam and Tomasz offered many helpful dicussions while they were here.The bonds with the DES collaboration and the XCS collaboration (the XMM Cluster Survey) have benefitted me enormously. The feedbacks from the DES cluster working group, the DES galaxy evolution working group and the XCS collaboration are critical in shaping my DES and XCS projects. Many collaborators have generously provided their code and catalogs, or patiently answered my questions about data and simulations. More than twenty people have commented on my paper drafts at different stages of preparation. The telephone discussions within the two collaborations are always inspiring and motivating. This section would become too long if I list the people that have helped on various issues, but at least let me thank Kathy Romer here for supervising my participation in both the DES and the XCS collaborations.My friends have helped to make the past five years fruitful and unforgettable: Scott,ii Tom, Paul and Arina, Ping, Zhao, Mijin, Arya and many others. I especially want to thank Jia Xu for taking care of me after an exercise accident. I am grateful that my family has always stood with me. My brother across the Pacific ocean helped me staying connected to different sides of life. My parents were understanding, cheerful, and eagerly helpful. I've become interested in mathematical and physical science since childhood. However, being a female, it took some extra courage to push it through. My parents were firm that women deserve any kinds of excellence and happiness with any kinds of career choice. This dissertation is dedicated to my mother an...

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The XMM Cluster Survey: Present status and latest results

Cited by 4 publications

References 19 publications

Galaxies in X-ray selected clusters and groups in Dark Energy Survey data – II. Hierarchical Bayesian modelling of the red-sequence galaxy luminosity function

Galaxies in X-ray selected clusters and groups in Dark Energy Survey data – II. Hierarchical Bayesian modelling of the red-sequence galaxy luminosity function

GALAXIES IN X-RAY SELECTED CLUSTERS AND GROUPS IN DARK ENERGY SURVEY DATA. I. STELLAR MASS GROWTH OF BRIGHT CENTRAL GALAXIES SINCE z ∼ 1.2

Looking Wider and Further: The Evolution of Galaxies Inside Galaxy Clusters

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