Intrinsic Alignment of Cluster Galaxies: The Redshift Evolution

Hao, Jiangang; Kubo, Jeffrey M.; Feldmann, Robert; Annis, J.; Johnston, David; Lin, Huan; McKay, Timothy A.

doi:10.1088/0004-637x/740/1/39

Cited by 59 publications

(95 citation statements)

References 49 publications

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“…When galaxy ellipticities were measured from two-dimensional profile fits, a marginal detection of 3σ was observed. Hao et al (2011) measured the alignments of satellites around a highly pure sample of clusters in SDSS. Satellites were selected by red sequence color cuts around each cluster.…”

Section: Discussionmentioning

confidence: 99%

“…Color selections that isolate red sequence galaxies (Medezinski et al 2007) can also be applied to separate lensing from alignments. Hao et al (2011) applied this procedure to measure the alignments of satellites around clusters in SDSS in the same redshift range as probed in this work. However, due to the unconstrained evolution of the Butcher-Oemler (Butcher & Oemler 1978) effect, whereby cluster galaxies are increasingly blue at high redshift, it is important not to bias the cluster member selection when applying color cuts.…”

Section: Discussionmentioning

confidence: 99%

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Intrinsic alignments of group and cluster galaxies in photometric surveys

Chisari

Mandelbaum

Strauss

et al. 2014

Monthly Notices of the Royal Astronomical Society

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Intrinsic alignments of galaxies have been shown to contaminate weak gravitational lensing observables on linear scales, r > 10 h −1 Mpc, but studies of alignments in the non-linear regime have thus far been inconclusive. We present an estimator for extracting the intrinsic alignment signal of galaxies around stacked clusters of galaxies from multiband imaging data. Our estimator removes the contamination caused by galaxies that are gravitationally lensed by the clusters and scattered in redshift space due to photometric redshift uncertainties. It uses posterior probability distributions for the redshifts of the galaxies in the sample and it is easily extended to obtain the weak gravitational lensing signal while removing the intrinsic alignment contamination. We apply this algorithm to groups and clusters of galaxies identified in the Sloan Digital Sky Survey 'Stripe 82' coadded imaging data over ∼ 150 deg 2 . We find that the intrinsic alignment signal around stacked clusters in the redshift range 0.1 < z < 0.4 is consistent with zero. In terms of the tidal alignment model of Catelan et al. (2001), we set joint constraints on the strength of the alignment and the bias of the lensing groups and clusters on scales between 0.1 and 10. This constrains the contamination fraction of alignment to lensing signal to the range between [−18, 23] per cent below scales of 1 h −1 Mpc at 95 per cent confidence level, and this result depends on our photometric redshift quality and selection criteria used to identify background galaxies. Our results are robust to the choice of photometric band in which the shapes are measured (i and r) and to centring on the Brightest Cluster Galaxy or on the geometrical centre of the clusters.

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Section: Discussionmentioning

confidence: 99%

Section: Discussionmentioning

confidence: 99%

Intrinsic alignments of group and cluster galaxies in photometric surveys

Chisari

Mandelbaum

Strauss

et al. 2014

Monthly Notices of the Royal Astronomical Society

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“…Most recent studies in this field report no significant radial alignment (e.g. Sheldon et al 2009;Hao et al 2011;Schneider et al 2013;Chisari et al 2014;Sifón et al 2015), although some earlier work claimed that such an alignment exists (e.g. Pereira & Kuhn 2005;Faltenbacher et al 2007).…”

Section: Contaminationmentioning

confidence: 94%

Weak-lensing-inferred scaling relations of galaxy clusters in the RCS2: mass-richness, mass-concentration, mass-bias, and more

Uitert

Gilbank

Hoekstra

et al. 2016

A&A

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We study a sample of ∼10 4 galaxy clusters in the redshift range 0.2 < z < 0.8 with masses M 200 > 5 × 10 13 h −1 70 M , discovered in the second Red-sequence Cluster Survey (RCS2). The depth and excellent image quality of the RCS2 enabled us to detect the cluster-mass cross-correlation up to z ∼ 0.7. To obtain cluster masses, concentrations, and halo biases, we fit a cluster halo model simultaneously to the lensing signal and to the projected density profile of red-sequence cluster members, because the latter provides tight constraints on the cluster miscentring distribution. We parametrised the mass-richness relation as 70 M and α = 0.73 ± 0.07 at low redshift (0.2 < z < 0.35). At intermediate redshift (0.35 < z < 0.55), we find a higher normalisation, which points towards a fractional increase in the richness towards lower redshift caused by the buildup of the red sequence. The miscentring distribution is well constrained. Only ∼30% of our BCGs coincide with the peak of the dark matter distribution. The distribution of the remaining BCGs are modelled with a 2D-Gaussian, whose width increases from 0.2 to 0.4 h −1 70 Mpc towards higher masses. The ratio of width and r 200 is constant with mass and has an average value of 0.44 ± 0.01. The mass-concentration and mass-bias relations agree fairly well with literature results at low redshift, but have a higher normalisation at higher redshifts, possibly because of selection and projection effects. The concentration of the satellite distribution decreases with mass and is correlated to the concentration of the halo.

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“…Hirata et al 2004;Mandelbaum et al 2005a) who used galaxy moments. Siverd et al (2009) and Hao et al (2011) attribute the discrepancy to the different definitions of the position angle of a galaxy. As we measure the shapes of source galaxies using galaxy moments, we expect that intrinsic alignment only has a minor impact on the correction factor and hence can be safely ignored.…”

Section: Contamination Correctionmentioning

confidence: 99%

Galaxy-galaxy lensing constraints on the relation between baryons and dark matter in galaxies in the Red Sequence Cluster Survey 2

Uitert

Hoekstra

Velander

et al. 2011

A&A

101

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We present the results of a study of weak gravitational lensing by galaxies using imaging data that were obtained as part of the second Red Sequence Cluster Survey (RCS2). In order to compare to the baryonic properties of the lenses we focus here on the ∼300 square degrees that overlap with the data release 7 (DR7) of the Sloan Digital Sky Survey (SDSS). The depth and image quality of the RCS2 enables us to significantly improve upon earlier work for luminous galaxies at z ≥ 0.3. To model the lensing signal we employ a halo model which accounts for the clustering of the lenses and distinguishes between satellite and central galaxies. Comparison with dynamical masses from the SDSS shows a good correlation with the lensing mass for early-type galaxies. The correlation is less clear for late-type galaxies, possibly due to rotation. For low luminosity (stellar mass) early-type galaxies we find a satellite fraction of ∼40% which rapidly decreases to <10% with increasing luminosity (stellar mass). The satellite fraction of the late-types has a value in the range 0-15%, independent of luminosity or stellar mass. At high masses the satellite fraction is not well constrained, which we partly attribute to the modelling assumptions. To infer virial masses we apply simple models based on an independent satellite kinematics analysis to account for intrinsic scatter in the scaling relations. We find that early-types in the range 10 10 < L r < 10 11.5 L have virial masses that are about five times higher than those of late-type galaxies and that the mass scales as M 200 ∝ L 2.34 +0.09 −0.16 . For an early-type galaxy with a fiducal luminosity of 10 11 L r, , we obtain a mass M 200 = (1.93 +0.13 −0.14 ) × 10 13 h −1 M . We also measure the virial mass-to-light ratio, and find for L 200 < 10 11 L a value of M 200 /L 200 = 42 ± 10 for early-types, which increases for higher luminosities to values that are consistent with those observed for groups and clusters of galaxies. For late-type galaxies we find a lower value of M 200 /L 200 = 17 ± 9. Our measurements also show that early-and late-type galaxies have comparable halo masses for stellar masses M * < 10 11 M , whereas the virial masses of early-type galaxies are higher for higher stellar masses. To compare the efficiency with which baryons have been converted into stars, we determine the total stellar mass within r 200 . Our results for early-type galaxies suggest a variation in efficiency with a minimum of ∼10% for a stellar mass M * ,200 = 10 12 M . The results for the late-type galaxies are not well constrained, but do suggest a larger value.

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Intrinsic Alignment of Cluster Galaxies: The Redshift Evolution

Cited by 59 publications

References 49 publications

Intrinsic alignments of group and cluster galaxies in photometric surveys

Intrinsic alignments of group and cluster galaxies in photometric surveys

Weak-lensing-inferred scaling relations of galaxy clusters in the RCS2: mass-richness, mass-concentration, mass-bias, and more

Galaxy-galaxy lensing constraints on the relation between baryons and dark matter in galaxies in the Red Sequence Cluster Survey 2

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