Measuring Ωmwith theROSATDeep Cluster Survey

Borgani, S.; Rosati, P.; Tozzi, P.; Stanford, S. A.; Eisenhardt, Peter; Lidman, C.; Holden, B.; Ceca, R. Della; Norman, C.; Squires, G.

doi:10.1086/323214

Cited by 276 publications

(297 citation statements)

References 60 publications

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“…Several X-ray cluster samples have been constructed from previous X-ray missions and have been used for a variety of astrophysical studies (e.g. Romer et al 1994;Forman et al 1978;Scharf et al 1997;Vikhlinin et al 1998;Böhringer et al 2000Böhringer et al , 2004Borgani et al 2001;Burenin et al 2007). The current generation of X-ray satellites, XMM-Newton, Chandra, and Suzaku, provided follow-up observations of individual clusters that allowed a precise determination of their spatially resolved spectra (e.g.…”

Section: Introductionmentioning

confidence: 99%

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: Introductionmentioning

confidence: 99%

The 2XMMi/SDSS Galaxy Cluster Survey

Takey

Schwope

Lamer

2013

A&A

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“…Being the most massive bound systems in the universe, they trace the latest stage of structure formation. Their abundance and mass as a function of redshift are thus highly indicative of how the growth of the cosmic density fluctuations occurs and can thus be used to constrain the matter content, the initial power spectrum normalisation and the expansion history of the universe (Eke et al 1998;Borgani et al 2001;Reiprich & Böhringer 2002;Allen et al 2003;Schuecker et al 2003;Henry 2004;Vikhlinin et al 2009;Mantz et al 2010;Rozo et al 2010;Sehgal & et al 2011;Planck Collaboration et al 2014a;Benson et al 2013;Mantz et al 2014). …”

Section: Introductionmentioning

confidence: 99%

Cosmology through arc statistics I: sensitivity to Ω_mand σ₈

Boldrin

Giocoli

Meneghetti

et al. 2016

Mon. Not. R. Astron. Soc.

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The next generation of large sky photometric surveys will finally be able to use arc statistics as a cosmological probe. Here we present the first of a series of papers on this topic. In particular, we study how arc counts are sensitive to the variation of two cosmological parameters: the (total) matter density parameter, Ω m , and the normalisation of the primordial power spectrum, expressed in terms of σ 8 . Both these parameters influence the abundances of collapsed structures and their internal structure. We compute the expected number of gravitational arcs with various length-to-width ratios in mock light cones, by varying these cosmological parameters in the ranges 0.1 Ω m 0.5 and 0.6 σ 8 1. We find that the arc counts dependence on Ω m and σ 8 is similar, but not identical, to that of the halo counts. We investigate how the precision of the constraints on the cosmological parameters based on arc counts depends on the survey area. We find that the constraining power of arc statistics degrades critically only for surveys covering an area smaller than 10% of the whole sky. Finally, we consider the case in which the search for arcs is done only in frames where galaxy clusters have been previously identified. Adopting the selection function for galaxy clusters expected to be detected from photometric data in future wide surveys, we find that less than 10% of the arcs will be missed, with only a small degradation of the corresponding cosmological constraints.

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“…The lesson from the previous calculation is that taking account of non-sphericity in collapse and the fact that massive clusters accrete matter quasi-continuously gives rise to a noteworthy change in the prediction of cosmological parameters, as Ω m . In order to check the previous trend, we have also estimated the value of Ω m following Borgani et al (2001). Analyzing the ROSAT Deep Cluster Survey (RDCS) and using the XLF to obtain constraints on cosmological parameters, Borgani et al (2001) found that Ω m = 0.35 +0.13 −0.10 .…”

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confidence: 99%

Constraints to cosmological parameters through cluster evolution

Popolo

Ercan

2004

IAU

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Abstract. In this paper, we revisit the constraints obtained by several authors (Reichart et al. 1999;Eke et al. 1998;Henry 2000) Firstly, using the quoted improvements, we re-derive an expression for the X-ray Luminosity Function (XLF), similarly to Reichart et al. (1999), and then we get some constraints to Ωm and n, by using the ROSAT BCS and EMSS samples and maximum-likelihood analysis. Then we re-derive the X-ray Temperature Function (XTF), similarly to Henry (2000), re-obtaining the constraints on Ωm, n, σ8. In the case of both the XLF and the XTF, the changes in the mass function and M-T relation produces an increase in Ωm of 20% and similar results in σ8 and n.

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Measuring Ω_mwith theROSATDeep Cluster Survey

Cited by 276 publications

References 60 publications

The 2XMMi/SDSS Galaxy Cluster Survey

The 2XMMi/SDSS Galaxy Cluster Survey

Cosmology through arc statistics I: sensitivity to Ω_mand σ₈

Constraints to cosmological parameters through cluster evolution

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Measuring Ωmwith theROSATDeep Cluster Survey

Cited by 276 publications

References 60 publications

The 2XMMi/SDSS Galaxy Cluster Survey

The 2XMMi/SDSS Galaxy Cluster Survey

Cosmology through arc statistics I: sensitivity to Ωmand σ8

Constraints to cosmological parameters through cluster evolution

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Measuring Ω_mwith theROSATDeep Cluster Survey

Cosmology through arc statistics I: sensitivity to Ω_mand σ₈