2024-03-28T13:52:26Zhttp://digital.csic.es/dspace-oai/requestoai:digital.csic.es:10261/1341092021-10-28T15:40:39Zcom_10261_97com_10261_4com_10261_45com_10261_49com_10261_37col_10261_350col_10261_298col_10261_175col_10261_290
00925njm 22002777a 4500
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Hurtado-Gil, L.
author
Arnalte-Mur, P.
author
Martínez, Vicente J.
author
Fernández-Soto, Alberto
author
Stefanon, Mauro
author
Ascaso, Begoña
author
López-Sanjuan, C.
author
Márquez, Isabel
author
Pović, Mirjana
author
Viironen, Kerttu
author
Aguerri, J.A.L.
author
Alfaro, Emilio J.
author
Aparicio Villegas, Teresa
author
Benítez, Narciso
author
Broadhurst, T.
author
Cabrera-Caño, Jesús
author
Castander, Francisco J.
author
Cepa, Jordi
author
Cerviño, Miguel
author
Cristóbal-Hornillos, David
author
González Delgado, Rosa M.
author
Husillos, César
author
Infante, Leopoldo
author
Masegosa, Josefa
author
Moles, Mariano
author
Molino, Alberto
author
Olmo, Ascensión del
author
Paredes, Silvestre
author
Prada, Francisco
author
Quintana, José María
author
2016
We study the clustering of galaxies as a function of spectral type and redshift in the range 0.35 <z <1.1 using data from the Advanced Large Homogeneous Area Medium Band Redshift Astronomical (ALHAMBRA) survey. The data cover 2.381 deg in 7 fields, after applying a detailed angular selection mask, with accurate photometric redshifts down to I <24. From this catalog we draw five fixed number density redshift-limited bins. We estimate the clustering evolution for two different spectral populations selected using the ALHAMBRA-based photometric templates: quiescent and star-forming galaxies. For each sample we measure the real-space clustering using the projected correlation function. Our calculations are performed over the range [0.03, 10.0] h Mpc, allowing us to find a steeper trend for Mpc, which is especially clear for star-forming galaxies. Our analysis also shows a clear early differentiation in the clustering properties of both populations: star-forming galaxies show weaker clustering with evolution in the correlation length over the analyzed redshift range, while quiescent galaxies show stronger clustering already at high redshifts and no appreciable evolution. We also perform the bias calculation where similar segregation is found, but now it is among the quiescent galaxies where a growing evolution with redshift is clearer (abrigatted). These findings clearly corroborate the well-known color-density relation, confirming that quiescent galaxies are mainly located in dark matter halos that are more massive than those typically populated by star-forming galaxies.
Astrophysical Journal 818(2): 174 (2016)
http://hdl.handle.net/10261/134109
10.3847/0004-637X/818/2/174
http://dx.doi.org/10.13039/501100000780
http://dx.doi.org/10.13039/501100003329
http://dx.doi.org/10.13039/501100003359
http://dx.doi.org/10.13039/501100002809
http://dx.doi.org/10.13039/501100011011
Cosmology: observations
Galaxies: distances and redshifts
Large-scale structure of universe
Methods: data analysis
Methods: statistical
The Alhambra survey: evolution of galaxy spectral segregation