The VIMOS Public Extragalactic Redshift Survey (VIPERS): Measuring non-linear galaxy bias at z ∼ 0.8

Di Porto, C.; Branchini, ENZO FRANCO; Bel, J.; Marulli, F.; Bolzonella, M.; Cucciati, O.; De La Torre, S.; Granett, B. R.; Guzzo, L.; Marinoni, C.; Moscardini, L.; Abbas, U.; Adami, C.; Arnouts, S.; Bottini, D.; Cappi, A.; Coupon, J.; Davidzon, I.; De Lucia, G.; Fritz, A.; Franzetti, P.; Fumana, M.; Garilli, B.; Ilbert, O.; Iovino, A.; Krywult, J.; Le Brun, V.; Le Fèvre, O.; Maccagni, D.; Małek, K.; Mccracken, H. J.; Paioro, L.; Polletta, M.; Pollo, A.; Scodeggio, M.; Tasca, L. A. M.; Tojeiro, R.; Vergani, D.; Zanichelli, A.; Burden, A.; Marchetti, A.; Martizzi, D.; Mellier, Y.; Nichol, R. C.; Peacock, J. A.; Percival, W. J.; Viel, M.; Wolk, M.; Zamorani, G.

doi:10.1051/0004-6361/201424448

Aims. We use the first release of the VImos Public Extragalactic Redshift Survey of galaxies (VIPERS) of ∼50 000 objects to measure the biasing relation between galaxies and mass in the redshift range z = [0.5,1.1]. Methods. We estimate the 1-point distribution function [PDF] of VIPERS galaxies from counts in cells and, assuming a model for the mass PDF, we infer their mean bias relation. The reconstruction of the bias relation is performed through a novel method that accounts for Poisson noise, redshift distortions, inhomogeneous sky coverage. and other selection effects. With this procedure we constrain galaxy bias and its deviations from linearity down to scales as small as 4 h-1 Mpc and out to z = 1.1. Results. We detect small (up to 2%) but statistically significant (up to 3σ) deviations from linear bias. The mean biasing function is close to linear in regions above the mean density. The mean slope of the biasing relation is a proxy to the linear bias parameter. This slope increases with luminosity, which is in agreement with results of previous analyses. We detect a strong bias evolution only for z> 0.9, which is in agreement with some, but not all, previous studies. We also detect a significant increase of the bias with the scale, from 4 to 8 h-1 Mpc, now seen for the first time out to z = 1. The amplitude of non-linearity depends on redshift, luminosity, and scale, but no clear trend is detected. Owing to the large cosmic volume probed by VIPERS, we find that the mismatch between the previous estimates of bias at z ∼ 1 from zCOSMOS and VVDS-Deep galaxy samples is fully accounted for by cosmic variance. Conclusions. The results of our work confirm the importance of going beyond the over-simplistic linear bias hypothesis showing that non-linearities can be accurately measured through the applications of the appropriate statistical tools to existing datasets like VIPERS.

The VIMOS Public Extragalactic Redshift Survey (VIPERS): Measuring non-linear galaxy bias at z ∼ 0.8

Di Porto, C.;BRANCHINI, ENZO FRANCO;Bel, J.;Marulli, F.;Bolzonella, M.;Cucciati, O.;De La Torre, S.;Granett, B. R.;Guzzo, L.;Marinoni, C.;Moscardini, L.;Abbas, U.;Adami, C.;Arnouts, S.;Bottini, D.;Cappi, A.;Coupon, J.;Davidzon, I.;De Lucia, G.;Fritz, A.;Franzetti, P.;Fumana, M.;Garilli, B.;Ilbert, O.;Iovino, A.;Krywult, J.;Le Brun, V.;Le Fèvre, O.;Maccagni, D.;Małek, K.;Mccracken, H. J.;Paioro, L.;Polletta, M.;Pollo, A.;Scodeggio, M.;Tasca, L. A. M.;Tojeiro, R.;Vergani, D.;Zanichelli, A.;Burden, A.;Marchetti, A.;Martizzi, D.;Mellier, Y.;Nichol, R. C.;Peacock, J. A.;Percival, W. J.;Viel, M.;Wolk, M.;Zamorani, G.

2016-01-01

Abstract

Aims. We use the first release of the VImos Public Extragalactic Redshift Survey of galaxies (VIPERS) of ∼50 000 objects to measure the biasing relation between galaxies and mass in the redshift range z = [0.5,1.1]. Methods. We estimate the 1-point distribution function [PDF] of VIPERS galaxies from counts in cells and, assuming a model for the mass PDF, we infer their mean bias relation. The reconstruction of the bias relation is performed through a novel method that accounts for Poisson noise, redshift distortions, inhomogeneous sky coverage. and other selection effects. With this procedure we constrain galaxy bias and its deviations from linearity down to scales as small as 4 h-1 Mpc and out to z = 1.1. Results. We detect small (up to 2%) but statistically significant (up to 3σ) deviations from linear bias. The mean biasing function is close to linear in regions above the mean density. The mean slope of the biasing relation is a proxy to the linear bias parameter. This slope increases with luminosity, which is in agreement with results of previous analyses. We detect a strong bias evolution only for z> 0.9, which is in agreement with some, but not all, previous studies. We also detect a significant increase of the bias with the scale, from 4 to 8 h-1 Mpc, now seen for the first time out to z = 1. The amplitude of non-linearity depends on redshift, luminosity, and scale, but no clear trend is detected. Owing to the large cosmic volume probed by VIPERS, we find that the mismatch between the previous estimates of bias at z ∼ 1 from zCOSMOS and VVDS-Deep galaxy samples is fully accounted for by cosmic variance. Conclusions. The results of our work confirm the importance of going beyond the over-simplistic linear bias hypothesis showing that non-linearities can be accurately measured through the applications of the appropriate statistical tools to existing datasets like VIPERS.