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The Alhambra survey: evolution of galaxy spectral segregation

AutorHurtado-Gil, L.; Arnalte-Mur, P. ; Martínez, Vicente J.; Fernández-Soto, Alberto ; Stefanon, Mauro; Ascaso, Begoña ; López-Sanjuan, C.; Márquez, Isabel ; Pović, Mirjana; Viironen, Kerttu; Aguerri, J. A. L.; Alfaro, Emilio J. ; Aparicio Villegas, Teresa ; Benítez, Narciso ; Broadhurst, T.; Cabrera-Caño, Jesús; Castander, Francisco J. ; Cepa, Jordi; Cerviño, Miguel ; Cristóbal-Hornillos, David ; González Delgado, Rosa M. ; Husillos, César ; Infante, Leopoldo; Masegosa, Josefa ; Moles, Mariano ; Molino, Alberto ; Olmo, Ascensión del ; Paredes, Silvestre; Prada, Francisco ; Quintana, José María
Palabras claveCosmology: observations
Galaxies: distances and redshifts
Large-scale structure of universe
Methods: data analysis
Methods: statistical
Fecha de publicación2016
EditorInstitute of Physics Publishing
CitaciónAstrophysical Journal 818(2): 174 (2016)
ResumenWe 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.
Versión del editorhttp://doi.org/10.3847/0004-637X/818/2/174
Identificadoresissn: 1538-4357
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