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2002MNRAS.332..617F - Mon. Not. R. Astron. Soc., 332, 617-646 (2002/May-3)
The Las Campanas Infrared Survey - II. Photometric redshifts, comparison with models and clustering evolution.
FIRTH A.E., SOMERVILLE R.S., McMAHON R.G., LAHAV O., ELLIS R.S., SABBEY C.N., McCARTHY P.J., CHEN H.-W., MARZKE R.O., WILSON J., ABRAHAM R.G., BECKETT M.G., CARLBERG R.G., LEWIS J.R., MacKAY C.D., MURPHY D.C., OEMLER A.E. and PERSSON S.E.
Abstract (from CDS):
We also determine the angular correlation function w (θ ) for magnitude, colour, spectral type and photometric redshift-selected subsamples of the data and use the photometric redshift distributions to derive the spatial clustering statistic ξ (r ) as a function of spectral type and redshift out to z ∼1.2. Parametrizing ξ (r ) by ξ (r c ,z )=[r c/r ∗(z )]–1.8 , where r c is in comoving coordinates, we find that r ∗(z ) increases by a factor of 1.5-2 from z =0 to z ∼1.2. We interpret this as a selection effect - the galaxies selected at z ∼1.2 are intrinsically very luminous, about 1-1.5mag brighter than L ∗. When galaxies are selected by absolute magnitude, we find no evidence for evolution in r ∗ over this redshift range. Extrapolated to z =0, we find r ∗(z =0)∼6.5h –1 Mpc for red galaxies and r ∗(z =0)∼2-4h –1 Mpc for blue galaxies. We also find that, while the angular clustering amplitude of EROs with R -H >4 or I -H >3 is up to four times that of the whole galaxy population, the spatial clustering length r ∗(z =1) is ∼7.5-10.5h –1 Mpc, which is only a factor of ∼1.7 times r ∗(z =1) for R -H <4 and I -H <3 galaxies lying in a similar redshift and luminosity range. This difference is similar to that observed between red and blue galaxies at low redshifts.
Abstract Copyright: 2002 Blackwell Science Ltd
Journal keyword(s): surveys - galaxies: distances and redshifts - galaxies: photometry - cosmology: observations - large-scale structure of Universe - infrared: galaxies
VizieR on-line data: <CDS Catalogue: VII/228>
Simbad objects: 2
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