We measure the real-space galaxy power spectrum on large scales at redshifts 0.5-1.2 using optical colour selected samples from the Canada-France-Hawaii Telescope Legacy Survey. With the redshift distributions measured with a preliminary ~14000 spectroscopic redshifts from the VIMOS Public Extragalactic Redshift Survey (VIPERS), we deproject the angular distribution and directly estimate the three-dimensional power spectrum. We use a maximum likelihood estimator that is optimal for a Gaussian random field giving well-defined window functions and error estimates. This measurement presents an initial look at the large-scale structure field probed by the VIPERS. We measure the galaxy bias of the VIPERS-like sample to be b g= 1.38 ± 0.05 (σ 8= 0.8) on scales k < 0.2hMpc -1 averaged over 0.5 < z < 1.2. We further investigate three photometric redshift slices, and marginalizing over the bias factors while keeping other Λ cold dark matter parameters fixed, we find the matter density Ω m= 0.30 ± 0.06.

The power spectrum from the angular distribution of galaxies in the CFHTLS-Wide fields at redshift ∼0.7

CUCCIATI, OLGA;MARULLI, FEDERICO;
2012

Abstract

We measure the real-space galaxy power spectrum on large scales at redshifts 0.5-1.2 using optical colour selected samples from the Canada-France-Hawaii Telescope Legacy Survey. With the redshift distributions measured with a preliminary ~14000 spectroscopic redshifts from the VIMOS Public Extragalactic Redshift Survey (VIPERS), we deproject the angular distribution and directly estimate the three-dimensional power spectrum. We use a maximum likelihood estimator that is optimal for a Gaussian random field giving well-defined window functions and error estimates. This measurement presents an initial look at the large-scale structure field probed by the VIPERS. We measure the galaxy bias of the VIPERS-like sample to be b g= 1.38 ± 0.05 (σ 8= 0.8) on scales k < 0.2hMpc -1 averaged over 0.5 < z < 1.2. We further investigate three photometric redshift slices, and marginalizing over the bias factors while keeping other Λ cold dark matter parameters fixed, we find the matter density Ω m= 0.30 ± 0.06.
2012
B. R. Granett;L. Guzzo;J. Coupon;S. Arnouts;P. Hudelot;O. Ilbert;H. J. McCracken;Y. Mellier;C. Adami;J. Bel;M. Bolzonella;D. Bottini;A. Cappi;O. Cucciati;S. de la Torre;P. Franzetti;A. Fritz;B. Garilli;A. Iovino;J. Krywult;V. Le Brun;O. Le Fevre;D. Maccagni;K. Malek;F. Marulli;B. Meneux;L. Paioro;M. Polletta;A. Pollo;M. Scodeggio;H. Schlagenhaufer;L. Tasca;R. Tojeiro;D. Vergani;A. Zanichelli
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Utilizza questo identificativo per citare o creare un link a questo documento: https://hdl.handle.net/11585/143249
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