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Near-Infrared galaxy counts and evolution from the wide-field Alhambra survey

AutorHornillos, Cristóbal; Moles, Mariano ; Perea, Jaime ; Castander, Francisco J. ; Alfaro, Emilio J. ; Benítez, Narciso ; Cerviño, Miguel ; Fernández-Soto, Alberto ; González Delgado, Rosa M. ; Husillos, César ; Márquez, Isabel ; Masegosa, Josefa ; Olmo, Ascensión del ; Prada, Francisco ; Quintana, José María ; Sánchez, Sebastián F.
Palabras claveCosmology: observations
Galaxies: evolution
Galaxies: high-redshift
Galaxies: photometry
Infrared: galaxies
Surveys
Fecha de publicación2009
EditorAmerican Astronomical Society
Institute of Physics Publishing
CitaciónAstrophysical Journal 696(2): 1554 (2009)
ResumenThe ALHAMBRA survey aims to cover 4 deg2 using a system of 20 contiguous, equal width, medium-band filters spanning the range 3500 Å-9700 Å plus the standard JHKs filters. Here we analyze deep near-IR number counts of one of our fields (ALH08) for which we have a relatively large area (0.5 deg2) and faint photometry (J = 22.4, H = 21.3, and K = 20.0 at the 50% of recovery efficiency for point-like sources). We find that the logarithmic gradient of the galaxy counts undergoes a distinct change to a flatter slope in each band: from 0.44 at [17.0, 18.5] to 0.34 at [19.5, 22.0] for the J band; for the H band 0.46 at [15.5, 18.0] to 0.36 at [19.0, 21.0], and in Ks the change is from 0.53 in the range [15.0, 17.0] to 0.33 in the interval [18.0, 20.0]. These observations together with faint optical counts are used to constrain models that include density and luminosity evolution of the local type-dependent luminosity functions. Our models imply a decline in the space density of evolved early-type galaxies with increasing redshift, such that only 30%-50% of the bulk of the present day red ellipticals was already in place at z~1.
Descripciónarxiv:0902.2403v1
Hornillos, Cristóbal et al.
Versión del editorhttp://dx.doi.org/10.1088/0004-637X/696/2/1554
URIhttp://hdl.handle.net/10261/42448
DOI10.1088/0004-637X/696/2/1554
ISSN0004-637X
E-ISSN1538-4357
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