We present an investigation of the clustering of the faint (i(AB)' < 24.5) field galaxy population in the redshift range 0.2 < z < 1.2. Using 100 000 precise photometric redshifts extracted from galaxies in the four ultra-deep fields of the Canada-France Legacy Survey, we construct a set of volume-limited galaxy samples. We use these catalogues to study in detail the dependence of the amplitude A(w) and slope delta of the galaxy correlation function w on absolute M-B rest-frame luminosity, redshift, and best-fitting spectral type (or, equivalently, rest-frame colour). Our derived comoving correlation lengths for magnitude-limited samples are in excellent agreement with measurements made in spectroscopic surveys. Our main conclusions are as follows: 1. the comoving correlation length for all galaxies with -19 < M-B-5 log h < -22 declines steadily from z similar to 0.3 to z similar to 1; 2. at all redshifts and luminosity ranges, galaxies with redder rest-frame colours have clustering amplitudes from two and three times higher than bluer ones; 3. for both the red and blue galaxy populations, the clustering amplitude is invariant with redshift for bright galaxies (-19 < MB -5 log h < -22); 4. at z similar to 0.5 for less luminous galaxies with M-B -5 log h similar to -19 we find higher clustering amplitudes of similar to 6 h(-1) Mpc; 5. the relative bias between redder and bluer rest-frame populations increases gradually towards fainter magnitudes. Among the most important implications of these results is that although the full galaxy population traces the underlying dark matter distribution quite well (and is therefore quite weakly biased), redder, older galaxies have clustering lengths that are almost invariant with redshift are quite strongly biased by z similar to 1.

Clustering properties of a type-selected volume-limited sample of galaxies in the CFHTLS / H.J. Mccracken, O. Ilbert, Y. Mellier, E. Bertin, L. Guzzo, S. Arnouts, O. Le Fèvre, G. Zamorani. - In: ASTRONOMY & ASTROPHYSICS. - ISSN 0004-6361. - 479:2(2008), pp. 321-334.

Clustering properties of a type-selected volume-limited sample of galaxies in the CFHTLS

E. Bertin;L. Guzzo;
2008

Abstract

We present an investigation of the clustering of the faint (i(AB)' < 24.5) field galaxy population in the redshift range 0.2 < z < 1.2. Using 100 000 precise photometric redshifts extracted from galaxies in the four ultra-deep fields of the Canada-France Legacy Survey, we construct a set of volume-limited galaxy samples. We use these catalogues to study in detail the dependence of the amplitude A(w) and slope delta of the galaxy correlation function w on absolute M-B rest-frame luminosity, redshift, and best-fitting spectral type (or, equivalently, rest-frame colour). Our derived comoving correlation lengths for magnitude-limited samples are in excellent agreement with measurements made in spectroscopic surveys. Our main conclusions are as follows: 1. the comoving correlation length for all galaxies with -19 < M-B-5 log h < -22 declines steadily from z similar to 0.3 to z similar to 1; 2. at all redshifts and luminosity ranges, galaxies with redder rest-frame colours have clustering amplitudes from two and three times higher than bluer ones; 3. for both the red and blue galaxy populations, the clustering amplitude is invariant with redshift for bright galaxies (-19 < MB -5 log h < -22); 4. at z similar to 0.5 for less luminous galaxies with M-B -5 log h similar to -19 we find higher clustering amplitudes of similar to 6 h(-1) Mpc; 5. the relative bias between redder and bluer rest-frame populations increases gradually towards fainter magnitudes. Among the most important implications of these results is that although the full galaxy population traces the underlying dark matter distribution quite well (and is therefore quite weakly biased), redder, older galaxies have clustering lengths that are almost invariant with redshift are quite strongly biased by z similar to 1.
cosmology : large-scale structure of Universe; galaxies : photometry; cosmology : observations
Settore FIS/05 - Astronomia e Astrofisica
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Utilizza questo identificativo per citare o creare un link a questo documento: http://hdl.handle.net/2434/590046
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