The XMM Cluster Survey: optical analysis methodology and the first data release

Mehrtens, Nicola; Romer, A. K.; Hilton, Matthew; Lloyd-Davies, E. J.; Miller, Christopher J.; Stanford, S. A.; Hosmer, Mark; Hoyle, B.; Collins, Chris; Liddle, Andrew R.; Viana, P. T. P.; Nichol, R. C.; Stott, John P.; Dubois, E. N.; Kay, Scott T.; Sahlén, Martin; Young, Owain; Short, Chris; Christodoulou, L.; Watson, William A.; Davidson, M.; Harrison, Craig; Baruah, L.; Smith, M.; Burke, Claire; Mayers, Julian A.; Deadman, Paul James; Rooney, Philip; Edmondson, Edward M.; West, Michael J.; Campbell, H.; Edge, A. C.; Mann, Robert; Sabirli, Kivanc; Wake, David A.; Benoist, Christophe; Costa, L. N. da; Maia, M. A. G.; Ogando, R. L. C.

doi:10.1111/j.1365-2966.2012.20931.x

Cited by 159 publications

(188 citation statements)

References 93 publications

(131 reference statements)

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“…In the next subsections, we compare our new results with the common clusters from (a) the XMM Cluster Survey (Mehrtens et al 2012); (b) the MCXC catalogue (Piffaretti et al 2011); and (c) the Paper I sample. We then proceed to derive an updated L X − T relation based on this new sample.…”

Section: Resultsmentioning

confidence: 99%

“…The largest published catalogue of X-ray clusters so far, based on the entire XMM-Newton archive, was compiled by the XMM Cluster Survey team (XCS, Romer et al 2001;Lloyd-Davies et al 2011;Mehrtens et al 2012). The catalogue consists of 503 optically confirmed clusters.…”

Section: Comparison With the Xcs Samplementioning

confidence: 99%

“…Several other projects are being conducted to detect galaxy clusters from the observations of the XMM-Newton, Chandra, and the X-ray Telescope A&A 558, A75 (2013) on board of the Swift satellite (e.g. Barkhouse et al 2006; Kolokotronis et al 2006;Finoguenov et al 2007Finoguenov et al , 2010Adami et al 2011;Fassbender et al 2011;Takey et al 2011;Mehrtens et al 2012;Clerc et al 2012;Tundo et al 2012;de Hoon et al 2013).…”

Section: Introductionmentioning

confidence: 99%

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The 2XMMi/SDSS Galaxy Cluster Survey

Takey

Schwope

Lamer

2013

A&A

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Aims. We compile a sample of X-ray-selected galaxy groups and clusters from the XMM-Newton serendipitous source catalogue (2XMMi-DR3) with optical confirmation and redshift measurement from the Sloan Digital Sky Survey (SDSS). We present an analysis of the X-ray properties of this new sample with particular emphasis on the X-ray luminosity-temperature (L X − T ) relation. Methods. The X-ray cluster candidates were selected from the 2XMMi-DR3 catalogue in the footprint of the SDSS-DR7. We developed a finding algorithm to search for overdensities of galaxies at the positions of the X-ray cluster candidates in the photometric redshift space and to measure the redshifts of the clusters from the SDSS data. For optically confirmed clusters with good quality X-ray data we derived the X-ray flux, luminosity, and temperature from proper spectral fits, while the X-ray flux for clusters with low-quality X-ray data was obtained from the 2XMMi-DR3 catalogue. Results. The detection algorithm provides the photometric redshift of 530 galaxy clusters. Of these, 310 clusters have a spectroscopic redshift for at least one member galaxy. About 75 percent of the optically confirmed cluster sample are newly discovered X-ray clusters. Moreover, 301 systems are known as optically selected clusters in the literature while the remainder are new discoveries in X-ray and optical bands. The optically confirmed cluster sample spans a wide redshift range 0.03−0.70 (median z = 0.32). In this paper, we present the catalogue of X-ray-selected galaxy groups and clusters from the 2XMMi/SDSS galaxy cluster survey. The catalogue has two subsamples: (i) a cluster sample comprising 345 objects with their X-ray spectroscopic temperature and flux from the spectral fitting; and (ii) a cluster sample consisting of 185 systems with their X-ray flux from the 2XMMi-DR3 catalogue, because their X-ray data are insufficient for spectral fitting. For each cluster, the catalogue also provides the X-ray bolometric luminosity and the cluster mass at R 500 based on scaling relations and the position of the likely brightest cluster galaxy (BCG). The updated L X − T relation of the current sample with X-ray spectroscopic parameters is presented. We found the slope of the L X − T relation to be consistent with published ones. We see no evidence for evolution in the slope and intrinsic scatter of the L X − T relation with redshift when excluding the low-luminosity groups.

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Section: Resultsmentioning

confidence: 99%

Section: Comparison With the Xcs Samplementioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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The 2XMMi/SDSS Galaxy Cluster Survey

Takey

Schwope

Lamer

2013

A&A

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“…Though many recent photometric catalogs have focused on narrow but deep survey data (z 1, e.g., Gonzalez et al, 2001;Gladders and Yee, 2005; Note. -All cluster catalogs included above are drawn from ROSAT data, except for XCS, which is a serendipitous cluster search in XMM-Newton archival data (see Mehrtens et al, 2012, for the first data release). Wide/shallow survey catalogs refer to cluster searches in the ROSAT All-Sky Survey (RASS), whereas narrow/deep catalogs are drawn from pointed ROSAT or XMM-Newton observations.…”

Section: The Current State Of Playmentioning

confidence: 99%

Observational probes of cosmic acceleration

et al. 2013

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The accelerating expansion of the universe is the most surprising cosmological discovery in many decades, implying that the universe is dominated by some form of "dark energy" with exotic physical properties, or that Einstein's theory of gravity breaks down on cosmological scales. The profound implications of cosmic acceleration have inspired ambitious efforts to understand its origin, with experiments that aim to measure the history of expansion and growth of structure with percent-level precision or higher. We review in detail the four most well established methods for making such measurements: Type Ia supernovae, baryon acoustic oscillations (BAO), weak gravitational lensing, and the abundance of galaxy clusters. We pay particular attention to the systematic uncertainties in these techniques and to strategies for controlling them at the level needed to exploit "Stage IV" dark energy facilities such as BigBOSS, LSST, Euclid, and WFIRST. We briefly review a number of other approaches including redshift-space distortions, the Alcock-Paczynski effect, and direct measurements of the Hubble constant H 0 . We present extensive forecasts for constraints on the dark energy equation of state and parameterized deviations from General Relativity, achievable with Stage III and Stage IV experimental programs that incorporate supernovae, BAO, weak lensing, and cosmic microwave background data. We also show the level of precision required for clusters or other methods to provide constraints competitive with those of these fiducial programs. We emphasize the value of a balanced program that employs several of the most powerful methods in combination, both to cross-check systematic uncertainties and to take advantage of complementary information. Surveys to probe cosmic acceleration produce data sets that support a wide range of scientific investigations, and they continue the longstanding astronomical tradition of mapping the universe in ever greater detail over ever larger scales.

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“…As time has passed, new approaches for selecting clusters have been developed, most notably using X-ray emission due to thermal Bremsstrahlung radiation from the hot gas that makes up most of the baryonic matter in the cluster. X-ray cluster surveys include both the NORAS (Böhringer et al 2000) and REFLEX (Böhringer et al 2004) surveys, based on ROSAT satellite observations, which have been used as source catalogues for higherprecision observations by the Chandra and XMM-Newton satellites, as well as surveys with XMM-Newton, including the XMM Cluster Survey (XCS, Mehrtens et al 2012) and the XMM Large Scale Structure survey (XMM-LSS, Willis et al 2013).…”

Section: Introductionmentioning

confidence: 99%

Planck2013 results. XX. Cosmology from Sunyaev–Zeldovich cluster counts

Ade¹,

Aghanim²,

Arnaud³

et al. 2014

A&A

524

156

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We present constraints on cosmological parameters using number counts as a function of redshift for a sub-sample of 189 galaxy clusters from the Planck SZ (PSZ) catalogue. The PSZ is selected through the signature of the Sunyaev-Zeldovich (SZ) effect, and the sub-sample used here has a signal-to-noise threshold of seven, with each object confirmed as a cluster and all but one with a redshift estimate. We discuss the completeness of the sample and our construction of a likelihood analysis. Using a relation between mass M and SZ signal Y calibrated to X-ray measurements, we derive constraints on the power spectrum amplitude σ 8 and matter density parameter Ω m in a flat ΛCDM model. We test the robustness of our estimates and find that possible biases in the Y-M relation and the halo mass function are larger than the statistical uncertainties from the cluster sample. Assuming the X-ray determined mass to be biased low relative to the true mass by between zero and 30%, motivated by comparison of the observed mass scaling relations to those from a set of numerical simulations, we find that σ 8 = 0.75 ± 0.03, Ω m = 0.29 ± 0.02, and σ 8 (Ω m /0.27) 0.3 = 0.764 ± 0.025. The value of σ 8 is degenerate with the mass bias; if the latter is fixed to a value of 20% (the central value from numerical simulations) we find σ 8 (Ω m /0.27) 0.3 = 0.78 ± 0.01 and a tighter one-dimensional range σ 8 = 0.77 ± 0.02. We find that the larger values of σ 8 and Ω m preferred by Planck's measurements of the primary CMB anisotropies can be accommodated by a mass bias of about 40%. Alternatively, consistency with the primary CMB constraints can be achieved by inclusion of processes that suppress power on small scales relative to the ΛCDM model, such as a component of massive neutrinos. We place our results in the context of other determinations of cosmological parameters, and discuss issues that need to be resolved in order to make further progress in this field.

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The XMM Cluster Survey: optical analysis methodology and the first data release

Cited by 159 publications

References 93 publications

The 2XMMi/SDSS Galaxy Cluster Survey

The 2XMMi/SDSS Galaxy Cluster Survey

Observational probes of cosmic acceleration

Planck2013 results. XX. Cosmology from Sunyaev–Zeldovich cluster counts

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