The VIMOS VLT deep survey - The evolution of galaxy clustering to z 2 from first epoch observations
The VIMOS VLT deep survey - The evolution of galaxy clustering to z 2 from first epoch observations
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VIMOS VLT 深度巡天 - 从第一纪观测到星系团到 z 2 的演化
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发表时间：
2004
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通讯作者：
D. Rizzo
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作者：
O. Fèvre;L. Guzzo;B. Meneux;A. Pollo;A. Cappi;S. Colombi;A. Iovino;C. Marinoni;C. Marinoni;H. McCracken;R. Scaramella;D. Bottini;B. Garilli;V. Brun;D. Maccagni;J. Picat;M. Scodeggio;L. Tresse;G. Vettolani;A. Zanichelli;C. Adami;M. Arnaboldi;S. Arnouts;S. Bardelli;J. Blaizot;M. Bolzonella;S. Charlot;S. Charlot;P. Ciliegi;T. Contini;S. Foucaud;P. Franzetti;I. Gavignaud;O. Ilbert;O. Ilbert;B. Marano;G. Mathez;A. Mazure;R. Merighi;S. Paltani;R. Pelló;L. Pozzetti;M. Radovich;G. Zamorani;E. Zucca;M. Bondi;A. Bongiorno;G. Busarello;F. Lamareille;Y. Mellier;P. Merluzzi;V. Ripepi;D. Rizzo
本文给出了第一历元VIMOS VLT深巡天（VVDS）的星系主星族从z=2.1到z=0.2的成团演化。我们计算了VVDS-02 h和VVDS-CDFS场的相关函数\xi（r_p，\pi）和w_p（r_p），以及相关长度r_0（z），这些数据来自于0.61 ° ^2区域内的7155个星系。我们发现，对于光度与本地2dFGRS和SDSS样本相当的星系，该样本中的相关长度在z=0.5到z=1.1之间大致保持不变，r_0（z）=2.5-2.8 h^{-1} Mpc（共动），这表明相关函数的振幅在z~1处比本地观测到的低约2.5倍。在我们的最低红移仓z=[0.2，0.5]中的相关长度是r_0=2.4 h^{-1} Mpc，比相同红移下的任何其他群体都要低，这表明非常低光度星系的低聚类，比2dFGRS或SDSS中的暗1.5等。在更高的红移z=[1.3，2.1]时，相关长度增加到r_0~3.0 h^{-1} Mpc，因为我们观测到的星系越来越亮，与局部MB_AB=-20.5的星系相当。我们将我们的测量结果与在z=[0.7，1.35] \citep{coil}范围内的DEEP 2测量结果进行了比较，并选择了与调查中相同的幅度和颜色选择标准，并找到了可比较的结果。随着红移的增加，VVDS星系缓慢变化的聚集与暗物质聚集的预测演化明显不同，表明明亮的星系已经在追踪90亿至100亿年前暗物质分布中出现的大尺度结构，这是星系与暗物质偏差强烈演化的支持证据。
This paper presents the evolution of the clustering of the main population of galaxies from z=2.1 to z=0.2, from the first epoch VIMOS VLT Deep Survey (VVDS), a magnitude limited sample with 17.5<=I_{AB}<=24. We have computed the correlation functions \xi(r_p,\pi) and w_p(r_p), and the correlation length r_0(z), for the VVDS-02h and VVDS-CDFS fields, for a total of 7155 galaxies in a 0.61deg^2 area. We find that the correlation length in this sample stays roughly constant from z=0.5 to z=1.1, with r_0(z)=2.5-2.8 h^{-1} Mpc (comoving), for galaxies comparable in luminosity to the local 2dFGRS and SDSS samples, indicating that the amplitude of the correlation function was ~2.5x lower at z~1 than observed locally. The correlation length in our lowest redshift bin z=[0.2,0.5] is r_0=2.4 h^{-1} Mpc, lower than for any other population at the same redshift, indicating the low clustering of very low luminosity galaxies, 1.5 magnitudes fainter than in the 2dFGRS or SDSS. The correlation length is increasing to r_0~3.0 h^{-1} Mpc at higher redshifts z=[1.3,2.1], as we are observing increasingly brighter galaxies, comparable to galaxies with MB_AB=-20.5 locally. We compare our measurement to the DEEP2 measurements in the range z=[0.7,1.35] \citep{coil} on the population selected applying the same magnitude and color selection criteria as in their survey, and find comparable results. The slowly varying clustering of VVDS galaxies as redshift increases is markedly different from the predicted evolution of the clustering of dark matter, indicating that bright galaxies are already tracing the large scale structures emerging from the dark matter distribution 9-10 billion years ago, a supporting evidence for a strong evolution of the galaxy vs. dark matter bias.