Evolution since<i>z</i>= 0.5 of the Morphology‐Density Relation for Clusters of Galaxies

Dressler, Alan; Oemler, Augustus; Couch, Warrick J.; Smail, Ian; Ellis, Richard S.; Barger, A. J.; Butcher, H. R.; Poggianti, Bianca M.; Sharples, R. M.

doi:10.1086/304890

Cited by 1,035 publications

(1,435 citation statements)

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“…of galaxies can be computed considering the projected distances D p, n to the nth nearest neighbour, and can be used to study the effect of the environment on the distribution of galactic types, as done by Dressler (Dressler 1980;Dressler et al 1997). Similarly, when spectroscopic redshifts are available, it is possible to compute the three-dimensional (non projected) distance D n to the nth nearest neighbour and derive a volume density…”

Section: (2+1)-dimensional Density From Photometric Redshiftsmentioning

confidence: 99%

A new (2+1)D cluster finding algorithm based on photometric redshifts: large scale structure in the Chandra deep field south

Trèvese

Castellano

Fontana

et al. 2006

A&A

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Aims. We study galaxy clustering and explore the dependence of galaxy properties on the the environment up to a redshift z ∼ 1, on the basis of a deep multi-band survey in the Chandra Deep Field South. Methods. We have developed a new method which combines galaxy angular positions and photometric redshifts to estimate the local galaxy number-density. This allows both the detection of overdensities in the galaxy distribution and the study of the properties of the galaxy population as a function of the environmental density. Results. We detect two moderate overdensities at z ∼ 0.7 and z ∼ 1 previously identified spectroscopically. We find that the fraction of red galaxies within each structure increases with volume density, extending to z ∼ 1 previous results. We measure "red sequence" slopes consistent with the values found in X-ray selected clusters, supporting the notion that the mass-metallicity relation hold constant up to z ∼ 1. Conclusions. Our method based on photometric redshifts allows to extend structure detection and density estimates up to the limits of photometric surveys, i.e. considerably deeper than spectroscopic surveys. Since X-ray cluster detection at high redshift is presently limited to massive relaxed structures, galaxy volume density based on photometric redshift appears as a valuable tool in the study of galaxy evolution.

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Section: (2+1)-dimensional Density From Photometric Redshiftsmentioning

confidence: 99%

A new (2+1)D cluster finding algorithm based on photometric redshifts: large scale structure in the Chandra deep field south

Trèvese

Castellano

Fontana

et al. 2006

A&A

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“…Most ellipticals look round or football-shaped, with modest ellipticities, or equivalently, large axis ratios. On the other hand, the ellipticity distribution of S0 galaxies is peaked at $ 0:5, while that of spirals is nearly flat at almost all ellipticities (Sandage, Freeman, & Stokes 1970;van den Bergh 1990;Fasano & Vio 1991;Franx, Illingworth, & de Zeeuw 1991;Lambas, Maddox, & Loveday 1992;Jørgensen & Franx 1994;Andreon et al 1996;Dressler et al 1997). Figure 18 presents the ellipticity distribution of the 145 GSS QS-E/S0's with 16:5 < I < 22 as the thick histogram (z phot sample included).…”

Section: Ellipticity Distributionmentioning

confidence: 99%

The DEEP Groth Strip Survey. X. Number Density and Luminosity Function of Field E/S0 Galaxies atz< 1

Simard

Faber

et al. 2002

ApJ

142

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We present the luminosity function and color-redshift relation of a magnitude-limited sample of 145 mostly red field E/S0 galaxies at zd1 from the DEEP Groth Strip Survey (GSS). Using nearby galaxy images as a training set, we develop a quantitative method to classify E/S0 galaxies based on smoothness, symmetry, and bulge-to-total light ratio. Using this method, we identify 145 E/S0's at 16:5 < I < 22 within the GSS, for which 44 spectroscopic redshifts (z spec ) are available. Most of the galaxies with spectroscopic redshifts (86%) form a '' red envelope '' in the redshift-color diagram, consistent with predictions of spectral synthesis models in which the dominant stellar population is formed at redshifts ze1:5. We use the tight correlation between VÀI and z spec for this red subset to estimate redshifts of the remaining E/S0's to an accuracy of $10%, with the exception of a small number (16%) of blue interlopers at low redshift that are quantitatively classified as E/S0's but are not contained within the red envelope. Constructing a luminosity function of the full sample of 145 E/S0's, we find that there is about 1.1-1.9 mag brightening in rest-frame B-band luminosity back to z ' 0:8 from z ¼ 0, consistent with other studies. Together with the red colors, this brightening is consistent with models in which the bulk of stars in red field E/S0's formed before z for e1:5 and have been evolving rather quiescently, with few large starbursts since then. Evolution in the number density of field E/ S0 galaxies is more difficult to measure, and uncertainties in the raw counts and their ratio to local samples might amount to as much as a factor of 2. Within that uncertainty, the number density of red E/S0's to z ' 0:8 seems relatively static, being comparable to or perhaps moderately less than that of local E/S0's, depending on the assumed cosmology. A doubling of E/S0 number density since z ¼ 1 can be ruled out with high confidence (97%) if m ¼ 1. Taken together, our results are consistent with the hypothesis that the majority of luminous field E/S0's were already in place by z $ 1, that the bulk of their stars were already fairly old, and that their number density has not changed by large amounts since then.

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“…To do that we simply assume that the fraction of S0 galaxies in clusters decreases by 12% every Gyr from z=0 up z=0.5 and remains constant afterwards. This assumption is based on results of Dressler et al (1997) indicating that the fraction of S0 in clusters at z=0.5 is 2 to 3 times lower than at z=0.…”

Section: Time Evolution Of Abundances and Energymentioning

confidence: 99%

SNe heating and the chemical evolution of the intra-cluster medium

et al. 2002

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Evolution sincez= 0.5 of the Morphology‐Density Relation for Clusters of Galaxies

Cited by 1,035 publications

References 32 publications

A new (2+1)D cluster finding algorithm based on photometric redshifts: large scale structure in the Chandra deep field south

A new (2+1)D cluster finding algorithm based on photometric redshifts: large scale structure in the Chandra deep field south

The DEEP Groth Strip Survey. X. Number Density and Luminosity Function of Field E/S0 Galaxies atz< 1

SNe heating and the chemical evolution of the intra-cluster medium

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