X-Ray Groups of Galaxies in the Aegis Deep and Wide Fields

Erfanianfar, G.; Finoguenov, A.; Tanaka, Masaomi; Lerchster, M.; Nandra, K.; Laird, E. S.; Connelly, Jennifer L.; Bielby, R. M.; Mirkazemi, M.; Faber, S. M.; Kocevski, D.; Cooper, Michael C.; Newman, J. A.; Jeltema, T.; Coil, Alison L.; Brimioulle, F.; Davis, Marc; McCracken, H. J.; Willmer, C. N. A.; Gerke, Brian F.; Cappelluti, N.; Gwyn, Stephen

doi:10.1088/0004-637x/765/2/117

Cited by 33 publications

(57 citation statements)

References 69 publications

(53 reference statements)

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“…We estimate the galaxy velocity dispersion σ x (v) using the virial mass of groups (estimated from the X-ray luminosity), as introduced in Erfanianfar et al (2013). In Table 1 we present the values of R 200 and σ x (v) for each galaxy group.…”

Section: Red-sequence Methodsmentioning

confidence: 99%

“…Column 7 lists L x,0.1−2.4 in the rest-frame 0.1−2.4 keV energy range. Column 8 presents the galaxy velocity dispersion in km s −1 , estimated from L X using the scaling relations (Erfanianfar et al 2013). Column 9 shows group's R 200c in degrees.…”

Section: Catalog Of Identified Groupsmentioning

confidence: 99%

“…In the absence of spectroscopic group membership, the calculation using red sequence galaxies may be contaminated by dusty star forming galaxies (DSFGs). We examine the impact of contamination of group members by DSFGs using the X-ray galaxy group catalog in the redshift range 0.066 < z < 1.544 presented in Erfanianfar et al (2013) and the data of galaxies in the AEGIS Herschel survey located within a CFHTLS field covering the redshift range 0.05 < z < 1.10. We define as DSFGs those galaxies which have star formation rate above ≈100 M yr −1 as inferred from FIR observations by Herschel space telescope (Erfanianfar et al 2014).…”

Section: Contamination Of Group Membershipmentioning

confidence: 99%

“…To examine the effect of the contamination by DSFGs on the magnitude gap calculation, we use data of nine galaxy groups with spectroscopic membership from the AEGIS X-ray groups catalog within the redshift range of 0.65 < z < 1.1 (Erfanianfar et al 2013(Erfanianfar et al , 2014. The redshift range of these groups of galaxies covers the range where the contamination by DSFGs is the highest.…”

Section: Contamination Of Group Membershipmentioning

confidence: 99%

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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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Section: Red-sequence Methodsmentioning

confidence: 99%

Section: Catalog Of Identified Groupsmentioning

confidence: 99%

Section: Contamination Of Group Membershipmentioning

confidence: 99%

Section: Contamination Of Group Membershipmentioning

confidence: 99%

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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

Self Cite

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“…Sensitivities and redshift ranges vary slightly from field to field and are discussed in Finoguenov et al (2015); Erfanianfar et al (2013);Finoguenov et al (2010); Erfanianfar et al (2014) for CDFS, EGS, UDS and HDFN, respectively (see Fig. 3).…”

Section: Datasets and Map Productionmentioning

confidence: 99%

Probing Large-scale Coherence between Spitzer IR and Chandra X-Ray Source-subtracted Cosmic Backgrounds

Cappelluti

Arendt

Kashlinsky

et al. 2017

ApJL

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We present new measurements of the large scale clustering component of the cross-power spectra of the source-subtracted Spitzer-IRAC Cosmic Infrared Background (CIB) and Chandra-ACIS Cosmic Xray Background (CXB) surface brightness fluctuations. Our investigation uses data from the Chandra Deep Field South (CDFS), Hubble Deep Field North (HDFN), EGS/AEGIS field and UDS/SXDF surveys, comprising 1160 Spitzer hours and ∼ 12 Ms of Chandra data collected over a total area of 0.3 deg 2 . We report the first (>5σ) detection of a cross-power signal on large angular scales > 20 ′′ between [0.5-2] keV and the 3.6 and 4.5µm bands, at ∼5σ and 6.3σ significance, respectively. The correlation with harder X-ray bands is marginally significant. Comparing the new observations with existing models for the contribution of the known unmasked source population at z <7, we find an excess of about an order of magnitude at 5σ confidence. We discuss possible interpretations for the origin of this excess in terms of the contribution from accreting early black holes, including both direct collapse black holes and primordial black holes, as well as from scattering in the interstellar medium and intra-halo light.

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Ultra-deep catalog of X-ray groups in the ExtendedChandraDeep Field South

Finoguenov

Tanaka

Cooper

et al. 2015

A&A

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Aims. We present the detection, identification and calibration of extended sources in the deepest X-ray dataset to date, the Extended Chandra Deep Field South (ECDF-S). Methods. Ultra-deep observations of ECDF-S with Chandra and XMM-Newton enable a search for extended X-ray emission down to an unprecedented flux of 2 × 10 −16 ergs s −1 cm −2 . By using simulations and comparing them with the Chandra and XMM data, we show that it is feasible to probe extended sources of this flux level, which is 10 000 times fainter than the first X-ray group catalogs of the ROSAT all sky survey. Extensive spectroscopic surveys at the VLT and Magellan have been completed, providing spectroscopic identification of galaxy groups to high redshifts. Furthermore, available HST imaging enables a weak-lensing calibration of the group masses.Results. We present the search for the extended emission on spatial scales of 32 in both Chandra and XMM data, covering 0.3 square degrees and model the extended emission on scales of arcminutes. We present a catalog of 46 spectroscopically identified groups, reaching a redshift of 1.6. We show that the statistical properties of ECDF-S, such as log N− log S and X-ray luminosity function are broadly consistent with LCDM, with the exception that dn/dz/dΩ test reveals that a redshift range of 0.2 < z < 0.5 in ECDF-S is sparsely populated. The lack of nearby structure, however, makes studies of high-redshift groups particularly easier both in X-rays and lensing, due to a lower level of clustered foreground. We present one and two point statistics of the galaxy groups as well as weak-lensing analysis to show that the detected low-luminosity systems are indeed low-mass systems. We verify the applicability of the scaling relations between the X-ray luminosity and the total mass of the group, derived for the COSMOS survey to lower masses and higher redshifts probed by ECDF-S by means of stacked weak lensing and clustering analysis, constraining any possible departures to be within 30% in mass. Conclusions. Ultra-deep X-ray surveys uniquely probe the low-mass galaxy groups across a broad range of redshifts. These groups constitute the most common environment for galaxy evolution. Together with the exquisite data set available in the best studied part of the Universe, the ECDF-S group catalog presented here has an exceptional legacy value.

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X-Ray Groups of Galaxies in the Aegis Deep and Wide Fields

Cited by 33 publications

References 69 publications

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

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

Probing Large-scale Coherence between Spitzer IR and Chandra X-Ray Source-subtracted Cosmic Backgrounds

Ultra-deep catalog of X-ray groups in the ExtendedChandraDeep Field South

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