The ALHAMBRA survey: evolution of galaxy clustering since $z \sim 1$

Autor: Arnalte-Mur, P., Martínez, V. J., Norberg, P., Fernández-Soto, A., Ascaso, B., Merson, A. I., Aguerri, J. A. L., Castander, F. J., Hurtado-Gil, L., López-Sanjuan, C., Molino, A., Montero-Dorta, A. D., Stefanon, M., Alfaro, E., Aparicio-Villegas, T., Benítez, N., Broadhurst, T., Cabrera-Caño, J., Cepa, J., Cerviño, M., Cristóbal-Hornillos, D., del Olmo, A., Delgado, R. M. González, Husillos, C., Infante, L., Márquez, I., Masegosa, J., Moles, M., Perea, J., Pović, M., Prada, F., Quintana, J. M.
Rok vydání: 2013
Předmět:
Zdroj: MNRAS, Volume 441, pp. 1783-1801 (2014)
Druh dokumentu: Working Paper
DOI: 10.1093/mnras/stu681
Popis: We study the clustering of galaxies as function of luminosity and redshift in the range $0.35 < z < 1.25$ using data from the Advanced Large Homogeneous Area Medium Band Redshift Astronomical (ALHAMBRA) survey. The ALHAMBRA data used in this work cover $2.38 \mathrm{deg}^2$ in 7 independent fields, after applying a detailed angular selection mask, with accurate photometric redshifts, $\sigma_z \lesssim 0.014 (1+z)$, down to $I_{\rm AB} < 24$. Given the depth of the survey, we select samples in $B$-band luminosity down to $L^{\rm th} \simeq 0.16 L^{*}$ at $z = 0.9$. We measure the real-space clustering using the projected correlation function, accounting for photometric redshifts uncertainties. We infer the galaxy bias, and study its evolution with luminosity. We study the effect of sample variance, and confirm earlier results that the COSMOS and ELAIS-N1 fields are dominated by the presence of large structures. For the intermediate and bright samples, $L^{\rm med} \gtrsim 0.6L^{*}$, we obtain a strong dependence of bias on luminosity, in agreement with previous results at similar redshift. We are able to extend this study to fainter luminosities, where we obtain an almost flat relation, similar to that observed at low redshift. Regarding the evolution of bias with redshift, our results suggest that the different galaxy populations studied reside in haloes covering a range in mass between $\log_{10}[M_{\rm h}/(h^{-1}\mathrm{M}_{\odot})] \gtrsim 11.5$ for samples with $L^{\rm med} \simeq 0.3 L^{*}$ and $\log_{10}[M_{\rm h}/(h^{-1}\mathrm{M}_{\odot})] \gtrsim 13.0$ for samples with $L^{\rm med} \simeq 2 L^{*}$, with typical occupation numbers in the range of $\sim 1 - 3$ galaxies per halo.
Comment: 21 pages, 16 figures, 3 tables. Accepted for publication in MNRAS. v2: matches accepted version. Small changes following referee comments, including addition of new fig. 11 and discussion on halo occupation numbers. Main results remain unchanged
Databáze: arXiv
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