Intrinsic Ellipticity Correlation of SDSS Luminous Red Galaxies and Misalignment With Their Host Dark Matter Halos

Okumura, Teppei; Jing, Y. P.; Li, Cheng

doi:10.1088/0004-637x/694/1/214

Cited by 150 publications

(198 citation statements)

References 76 publications

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“…5), which is expected if the galaxies are virialised within an elliptic halo. In addition, E0454 is elongated along the same direction, and Okumura et al (2009) show that the central luminous red galaxies in clusters are preferentially aligned within ∼35 degrees with their host dark matter haloes. The separations between E0454 and the halo centre should therefore be regarded as lower limits.…”

Section: E0454 Is Not At the Centre Of The Dark Matter Potentialmentioning

confidence: 83%

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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Section: E0454 Is Not At the Centre Of The Dark Matter Potentialmentioning

confidence: 83%

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

Schirmer¹,

Suyu²,

Schrabback

et al. 2010

A&A

View full text Add to dashboard Cite

show abstract

“…It is instructive to compare these 2D misalignment angle distributions to the commonly assumed single-Gaussian distribution (see e.g. Okumura et al 2009). None of the distributions found in this study resembles a single-Gaussian and we therefore caution interested practitioners against adopting this assumption.…”

Section: A P P E N D I X B : a Na Ly T I C F I T S F O R T H E M I S mentioning

confidence: 99%

“…However, different studies have reached somewhat conflicting conclusions about the typical values of this misalignment angle (see e.g. Heymans et al 2004;Kang et al 2007;Wang et al 2008;Okumura, Jing & Li 2009). …”

mentioning

confidence: 99%

The alignment and shape of dark matter, stellar, and hot gas distributions in the EAGLE and cosmo-OWLS simulations

Velliscig

Cacciato

Schaye

et al. 2015

Mon. Not. R. Astron. Soc.

139

158

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(2015) 'The alignment and shape of dark matter, stellar, and hot gas distributions in the EAGLE and cosmo-OWLS simulations.', Monthly notices of the Royal Astronomical Society., 453 (1). pp. 721-738. Additional information: Use policyThe full-text may be used and/or reproduced, and given to third parties in any format or medium, without prior permission or charge, for personal research or study, educational, or not-for-pro t purposes provided that:• a full bibliographic reference is made to the original source • a link is made to the metadata record in DRO • the full-text is not changed in any way The full-text must not be sold in any format or medium without the formal permission of the copyright holders.Please consult the full DRO policy for further details.

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“…Here M0.3 g is the g-band absolute magnitude K-and E-corrected to redshift z = 0.3 (see Eisenstein et al 2001 for references). We further select those LRGs that are expected to be the central galaxy of their host dark matter halos, using a method similar to that adopted in Reid & Spergel (2009) and Okumura et al (2009). We use linking lengths of 0.8 h −1 Mpc and 20 h −1 Mpc for separations perpendicular and parallel to the line of sight when linking galaxies into groups.…”

Section: The Lrg Sample At Intermediate Redshiftmentioning

confidence: 99%

Galaxy Clustering and Projected Density Profiles as Traced by Satellites in Photometric Surveys: Methodology and Luminosity Dependence

Wang¹,

Jing²,

Li³

et al. 2011

ApJ

Self Cite

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We develop a new method which measures the projected density distribution w p (r p )n of photometric galaxies surrounding a set of spectroscopically-identified galaxies, and simultaneously the projected cross-correlation function w p (r p ) between the two populations. In this method we are able to divide the photometric galaxies into subsamples in luminosity intervals even when redshift information is unavailable, enabling us to measure w p (r p )n and w p (r p ) as a function of not only the luminosity of the spectroscopic galaxy, but also that of the photometric galaxy. Extensive tests show that our method can measure w p (r p ) in a statistically unbiased way. The accuracy of the measurement depends on the validity of the assumption inherent to the method that the foreground/background galaxies are randomly distributed and are thus uncorrelated with those galaxies of interest. Therefore, our method can be applied to the cases where foreground/background galaxies are distributed in large volumes, which is usually valid in real observations.We have applied our method to data from the Sloan Digital Sky Survey (SDSS) including a sample of 10 5 luminous red galaxies (LRGs) at z ∼ 0.4 and a sample of about half a million galaxies at z ∼ 0.1, both of which are cross-correlated with a deep photometric sample drawn from the SDSS. On large scales, the relative bias factor of galaxies measured from w p (r p ) at z ∼ 0.4 depends on luminosity in a manner similar to what is found for those at z ∼ 0.1, which are usually probed by autocorrelations of spectroscopic samples in previous studies. On scales smaller than a few Mpc and at both z ∼ 0.4 and z ∼ 0.1, the photometric galaxies of different luminosities exhibit similar density profiles around spectroscopic galaxies at fixed luminosity and redshift. This provides clear observational support for the assumption commonly-adopted in halo occupation distribution (HOD) models that satellite galaxies of different luminosities are distributed in a similar way, following the dark matter distribution within their host halos.

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Intrinsic Ellipticity Correlation of SDSS Luminous Red Galaxies and Misalignment With Their Host Dark Matter Halos

Cited by 150 publications

References 76 publications

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

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

The alignment and shape of dark matter, stellar, and hot gas distributions in the EAGLE and cosmo-OWLS simulations

Galaxy Clustering and Projected Density Profiles as Traced by Satellites in Photometric Surveys: Methodology and Luminosity Dependence

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