The Evolution of Galaxies in X‐Ray–luminous Groups

Jeltema, T.; Mulchaey, John S.; Lubin, Lori M.; Fassnacht, C. D.

doi:10.1086/511852

Cited by 52 publications

(78 citation statements)

References 93 publications

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“…For instance, have studied a sample of 12 nearby poor galaxy groups and found significant variations (up to a factor 2) in the fraction of early-type galaxies. Similar variations in the galaxy population from group to group have been obtained by Jeltema et al (2007) at intermediate redshifts. Therefore, we do not probe the same fraction of group members for each object in our sample.…”

Section: Richness and Optical Luminositysupporting

confidence: 80%

“…3.2, using the same COSMOS data, George et al (2012) confirmed the findings of Jeltema et al (2007) about the BGG/BCG in groups and clusters: an early-type galaxy, but not necessarily a dominant one, and with observed shifts up to 100 kpc with respect to the X-ray peak (see also Hoekstra et al 2012, and their sample of 50 massive galaxy clusters). In our study of the SARCS sample, we observed the same behaviour in some specific cases such as the multi-modal groups where there is not a single early-type galaxy dominating the light distribution, and/or where the strong-lensing system is not associated to the brightest member.…”

Section: Comparison With Previous Worksupporting

confidence: 76%

“…However, the brightest galaxy is not always a cD at rest in the gravitational potential well, but rather a large elliptical galaxy that is not necessarily located at the centre of the mass distribution. For instance, Jeltema et al 2007 have studied a sample of seven X-ray-loud galaxy groups at intermediate redshifts (0.2 < z < 0.6), and for two of them, the brightest galaxy presents an offset ∼100 h −1 70 kpc with the X-ray emission peak. They also found two groups where no dominant elliptical galaxy is present, but rather several ones with comparable luminosities (see also the more recent work by George et al 2012, of the COSMOS X-ray-selected groups).…”

Section: Choice Of the Centrementioning

confidence: 99%

“…From the X-ray point of view, Jeltema et al (2006Jeltema et al ( , 2007 present the analysis of a sample of nine X-ray emitting galaxy groups at intermediate redshifts . In particular they find that these intermediate-redshift groups present similar properties as local groups, thus excluding strong nonstandard redshift evolution.…”

Section: Comparison With Previous Workmentioning

confidence: 99%

“…On the other hand, a precise characterization of group and cluster masses provides a unique way to probe relevant mechanisms, such as galaxy harassment, ram pressure stripping, or galaxy starvation/strangulation, which drive the evolution of the galaxy properties (stellar mass, size, star formation rate, spectral/morphological type, etc.) as a function of their local environment, from field galaxies to the core of massive clusters (Smail et al 1998;Balogh et al 1999;Tran et al 2003;Treu et al 2003;Dressler et al 2004;Poggianti 2004;Boselli & Gavazzi 2006;Poggianti et al 2006;Balogh et al 2007;De Lucia et al 2007;Jeltema et al 2007;Popesso et al 2007;Huertas-Company et al 2009;Lubin et al 2009;Stott et al 2009;Wilman et al 2009;Balogh et al 2011b;Carollo et al 2013). It is, therefore, very important to use representative group and cluster samples that cover a wide range in mass and redshift to study and constrain the galaxy and ICM properties along with robust and direct mass estimates of the parent halo.…”

Section: Introductionmentioning

confidence: 99%

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SARCS strong-lensing galaxy groups

Foëx¹,

Motta²,

Limousin³

et al. 2013

A&A

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We present the weak-lensing and optical analysis of the SL2S-ARCS (SARCS) sample of strong-lensing candidates. The sample is based on the Strong Lensing Legacy Survey (SL2S), a systematic search of strong-lensing systems in the photometric CanadaFrance-Hawaii Telescope Legacy Survey (CFHTLS). The SARCS sample focusses on arc-like features and is designed to contain mostly galaxy groups. We briefly present the weak-lensing methodology that we used to estimate the mass of the SARCS objects. Among 126 candidates, we obtained a weak-lensing detection (at the 1σ level) for 89 objects with velocity dispersions of the singular isothermal sphere mass model (SIS) ranging from σ SIS ∼ 350 km s −1 to ∼1000 km s −1 with an average value of σ SIS ∼ 600 km s −1 , corresponding to a rich galaxy group (or poor cluster). From the galaxies belonging to the bright end of the group's red sequence (M i < −21), we derived the optical properties of the SARCS candidates. We obtained typical richnesses of N ∼ 5−15 galaxies and optical luminosities of L ∼ 0.5−1.5 × 10 12 L (within a radius of 0.5 Mpc). We used these galaxies to compute luminosity density maps, from which a morphological classification reveals that a large fraction of the sample (∼45%) are groups with a complex light distribution, either elliptical or multi-modal, suggesting that these objects are dynamically young structures. We finally combined the lensing and optical analyses to define a sample of the 80 most secure group candidates, i.e. weak-lensing detection and over-density at the lens position in the luminosity map, to remove false detections and galaxy-scale systems from the initial sample. We use this reduced sample to probe the optical scaling relations in combination with a sample of massive galaxy clusters. We detect the expected correlations over the probed range in mass with a typical scatter of ∼25% in σ SIS at a given richness or luminosity, making these scaling laws interesting mass proxies.

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Section: Richness and Optical Luminositysupporting

confidence: 80%

Section: Comparison With Previous Worksupporting

confidence: 76%

Section: Choice Of the Centrementioning

confidence: 99%

Section: Comparison With Previous Workmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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SARCS strong-lensing galaxy groups

Foëx¹,

Motta²,

Limousin³

et al. 2013

A&A

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The Influence of Environment on Galaxy Evolution

Vollmer

2013

Planets, Stars and Stellar Systems

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J0454-0309: evidence of a strong lensing fossil group falling into a poor galaxy cluster

Schirmer¹,

Suyu²,

Schrabback

et al. 2010

A&A

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Aims. We have discovered a strong lensing fossil group (J0454) projected near the well-studied cluster MS0451-0305. Using the large amount of available archival data, we compare J0454 to normal groups and clusters. A highly asymmetric image configuration of the strong lens enables us to study the substructure of the system. Methods. We used multicolour Subaru/Suprime-Cam and CFHT/Megaprime imaging, together with Keck spectroscopy to identify member galaxies. A VLT/FORS2 spectrum was taken to determine the redshifts of the brightest elliptical and the lensed arc. Using HST/ACS images, we determined the group's weak lensing signal and modelled the strong lens system. This is the first time that a fossil group is analysed with lensing methods. The X-ray luminosity and temperature were derived from XMM-Newton data. Results. J0454 is located at z = 0.26, with a gap of 2.5 mag between the brightest and second brightest galaxies within half the virial radius. Outside a radius of 1.5 Mpc, we find two filaments extending over 4 Mpc, and within we identify 31 members spectroscopically and 33 via the red sequence with i < 22 mag. (BGG) is inconsistent with the dynamic centre of J0454. It strongly lenses a galaxy at z = 2.1 ± 0.3, and we model the lens with a pseudo-isothermal elliptical mass distribution. A high external shear, and a discrepancy between the Einstein radius and the weak lensing velocity dispersion requires that the BGG must be offset from J0454's dark halo centre by at least 90−130 kpc. The X-ray halo is offset by 24 ± 16 kpc from the BGG, shows no signs of a cooling flow and can be fit by a single β-model. With L X = (1.4 ± 0.2) × 10 43 erg s −1 J0454 falls onto standard cluster scaling relations, but appears cooler (T = 1.1 ± 0.1 keV) than expected (T ∼ 2.0 keV). Taken all together, these data indicate that J0454 consists of two systems, a sparse cluster and an infalling fossil group, where the latter seeds the brightest cluster galaxy. An alternative to the sparse cluster could be a filament projected along the line of sight mimicking a cluster, with galaxies streaming towards the fossil group.

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The Evolution of Galaxies in X‐Ray–luminous Groups

Cited by 52 publications

References 93 publications

SARCS strong-lensing galaxy groups

SARCS strong-lensing galaxy groups

The Influence of Environment on Galaxy Evolution

J0454-0309: evidence of a strong lensing fossil group falling into a poor galaxy cluster

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