Dark matter halo properties from galaxy–galaxy lensing★

Brimioulle, F.; Seitz, S.; Lerchster, M.; Bender, Ralf; Snigula, J.

doi:10.1093/mnras/stt525

Cited by 78 publications

(133 citation statements)

References 126 publications

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“…As far as the signal-to-noise ratio of the stacked haloes is concerned, these effects counterbalance each other and lensing results are comparable (Johnston et al 2007;Mandelbaum, Seljak & Hirata 2008;Mandelbaum et al 2013;Brimioulle et al 2013;Hudson et al 2015;Covone et al 2014;Ford et al 2014Ford et al , 2015Velander et al 2014;Oguri 2014). A similar choice of data-sets for a joint analysis of galaxy clustering and galaxy-galaxy lensing was recently made by More et al (2014).…”

Section: Datamentioning

confidence: 90%

New constraints on σ8 from a joint analysis of stacked gravitational lensing and clustering of galaxy clusters

Sereno¹,

Veropalumbo²,

Marulli³

et al. 2015

Monthly Notices of the Royal Astronomical Society

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The joint analysis of clustering and stacked gravitational lensing of galaxy clusters in large surveys can constrain the formation and evolution of structures and the cosmological parameters. On scales outside a few virial radii, the halo bias, b, is linear and the lensing signal is dominated by the correlated distribution of matter around galaxy clusters. We discuss a method to measure the power spectrum amplitude σ 8 and b based on a minimal modelling. We considered a sample of ∼ 120000 clusters photometrically selected from the Sloan Digital Sky Survey in the redshift range 0.1 < z < 0.6. The auto-correlation was studied through the two-point function of a subsample of ∼ 70000 clusters; the matter-halo correlation was derived from the weak lensing signal of the subsample of ∼ 1200 clusters with CanadaFrance-Hawaii Lensing Survey data. We obtained a direct measurement of b, which increases with mass in agreement with predictions of the ΛCDM paradigm. Assuming Ω M = 0.3, we found σ 8 = 0.78 ± 0.16. We used the same clusters for measuring both lensing and clustering and the estimate of σ 8 did require neither the mass-richness relation, nor the knowledge of the selection function, nor the modelling of b. With an additional theoretical prior on the bias, we obtained σ 8 = 0.75 ± 0.08.

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Section: Datamentioning

confidence: 90%

New constraints on σ8 from a joint analysis of stacked gravitational lensing and clustering of galaxy clusters

Sereno¹,

Veropalumbo²,

Marulli³

et al. 2015

Monthly Notices of the Royal Astronomical Society

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“…The completeness limits and image quality of the photometric survey data are important for the detection of the optical counterparts of the X-ray sources and for the accuracy of the photometric redshift of galaxies (e.g., Mirkazemi et al 2014;Brimioulle et al 2008;Bordoloi et al 2012).…”

Section: Photometric and Spectroscopic Datamentioning

confidence: 99%

“…In this paper, we use the photometric redshift catalogs of the CFHTLS survey by Brimioulle et al (2008Brimioulle et al ( , 2013. The XMM-CFHTLS W1 field, has a good spectroscopic coverage of ∼0.64 degrees 2 with the VIMOS-VLT Deep Survey (VVDS; Le Fèvre et al 2004Fèvre et al , 2005 and the targeted cluster follow-up of Adami et al (2011).…”

Section: Photometric and Spectroscopic Datamentioning

confidence: 99%

Mining the gap: evolution of the magnitude gap in X-ray galaxy groups from the 3-square-degree XMM coverage of CFHTLS

Gozaliasl¹,

Finoguenov²,

Khosroshahi³

et al. 2014

A&A

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We present a catalog of 129 X-ray galaxy groups, covering a redshift range 0.04 < z < 1.23, selected in the ∼3 deg 2 part of the CFHTLS W1 field overlapping XMM observations performed under the XMM-LSS project. We carry out a statistical study of the redshift evolution out to redshift one of the magnitude gap between the first and the second brightest cluster galaxies of a well defined mass-selected group sample. We find that the slope of the relation between the fraction of groups and the magnitude gap steepens with redshift, indicating a larger fraction of fossil groups at lower redshifts. We find that 22.2 ± 6% of our groups at z ≤ 0.6 are fossil groups. We compare our results with the predictions of three semi-analytic models based on the Millennium simulation. The intercept of the relation between the magnitude of the brightest galaxy and the value of magnitude gap becomes brighter with increasing redshift. This trend is steeper than the model predictions which we attribute to the younger stellar age of the observed brightest cluster galaxies. This trend argues in favor of stronger evolution of the feedback from active galactic nuclei at z < 1 compared to the models. The slope of the relation between the magnitude of the brightest cluster galaxy and the value of the gap does not evolve with redshift and is well reproduced by the models, indicating that the tidal galaxy stripping, put forward as an explanation of the occurrence of the magnitude gap, is both a dominant mechanism and sufficiently well modeled.

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“…We used the code PHOTO-z (Bender et al 2001) to estimate the photometric redshifts, with a set of 31 SED templates (see Brimioulle et al 2008;Lerchster et al 2011, for details).…”

Section: Photometric Redshiftsmentioning

confidence: 99%

“…html 4 The full procedure of data reduction and calibration will be described in Brimioulle et al (in prep. ), see also Brimioulle et al (2008). illustrate the completeness of the X-ray selection technique as a method to identify clusters of galaxies.…”

Section: Galaxy Over-densitiesmentioning

confidence: 99%

Distant galaxy clusters in a deepXMM-Newtonfield within the CFTHLS D4

Hoon¹,

Lamer²,

Schwope³

et al. 2013

A&A

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Aims. The XMM-Newton distant cluster project (XDCP) aims at the identification of a well defined sample of X-ray selected clusters of galaxies at redshifts z ≥ 0.8. As part of this project, we analyse the deep XMM-Newton exposure covering one of the CFHTLS deep fields to quantify the cluster content. We validate the optical follow-up strategy as well as the X-ray selection function. Methods. We searched for extended X-ray sources in archival XMM-Newton EPIC observations. Multi-band optical imaging was performed to select high redshift cluster candidates among the extended X-ray sources. Here we present a catalogue of the extended sources in one the deepest ∼250 ks XMM-Newton fields targetting LBQS 2212-1759 covering ∼0.2 deg 2 . The cluster identification is based on deep imaging with the ESO VLT and from the CFHT legacy survey, among others. The confirmation of cluster candidates is done by VLT/FORS2 multi-object spectroscopy. Photometric redshifts from the CFHTLS D4 were utilised to confirm the effectiveness of the X-ray cluster selection method. The survey sensitivity was computed with extensive Monte-Carlo simulations. Results. At a flux limit of S 0.5−2.0 keV ∼ 2.5 × 10 −15 erg s −1 we achieve a completeness level higher than 50% in an area of ∼0.13 deg 2 . We detect six galaxy clusters above this limit with optical counterparts, of which 5 are new spectroscopic discoveries. Two newly discovered X-ray luminous galaxy clusters are at z ≥ 1.0, another two at z = 0.41, and one at z = 0.34. For the most distant X-ray selected cluster in this field at z = 1.45, we find additional (active) member galaxies from both X-ray and spectroscopic data. Additionally, we find evidence of large-scale structures at moderate redshifts of z = 0.41 and z = 0.34. Conclusions. The quest for distant clusters in archival XMM-Newton data has led to detection of six clusters in a single field, making XMM-Newton an outstanding tool for cluster surveys. Three of these clusters are at z ≥ 1, which emphasises the valuable contribution of small, yet deep surveys to cosmology. Beta models are appropriate descriptions of the cluster surface brightness when performing cluster detection simulations to compute the X-ray selection function. The constructed log N − log S tends to favour a scenario where no evolution in the cluster X-ray luminosity function (XLF) takes place.

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Dark matter halo properties from galaxy–galaxy lensing★

Cited by 78 publications

References 126 publications

New constraints on σ8 from a joint analysis of stacked gravitational lensing and clustering of galaxy clusters

New constraints on σ8 from a joint analysis of stacked gravitational lensing and clustering of galaxy clusters

Mining the gap: evolution of the magnitude gap in X-ray galaxy groups from the 3-square-degree XMM coverage of CFHTLS

Distant galaxy clusters in a deepXMM-Newtonfield within the CFTHLS D4

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