This is the third paper in a series devoted to the WIde-field Nearby Galaxy-cluster Survey (WINGS). WINGS is a long-term project aimed at gathering wide-field, multiband imaging and spectroscopy of galaxies in a complete sample of 77 X-ray selected, nearby clusters (0.04<z<0.07) located far from the galactic plane (|b|>=20{deg}). The main goal of this project is to establish a local reference sample for evolutionary studies of galaxies and galaxy clusters. This paper presents the near-infrared (J,K) photometric catalogs of 28 clusters of the WINGS sample and describes the procedures followed to construct them.
This catalog contains the surface brightness measurements of ~71700 galaxies detected in the K images of the WINGS cluster survey for a subsample of 26 clusters observed with the UKIRT WFCAM. For each galaxy K magnitude, mean surface brightness, effective radius, Sersic index and axial ratio are given, together with their erros. These global parameters were obtained by simultaneously fitting the major and minor axis light growth curves of galaxies with a 2D flattened Sersic-law, convolved by the appropriate, space-varying PSF, which was previously evaluated by the tool itself. (http://adsabs.harvard.edu/abs/2006A%26A...446..373P)
For each WINGS galaxy with V absolute magnitude brighter than -16, the local density calculated as the Log (decimal) of the number of galaxies with M_V <= -19.5 per Mpc**2 is given. It is computed from the circular area enclosing the first 10 closest galaxies, plus the background counts expected from Berta et al. (2006). The Local Densities are also corrected for border effects.
The Coverage field fraction are also given, both at CCDX, i.e. the fraction of the circular area of radius CCDX and centered in the X-ray center, which is included in the field of the CCD mosaics, and at CCDB (centered in the BCG).
For clusters without velocity dispersion the distances are given in pixels and NOT in R200.
These clusters are A311, A2665, A3164, and Z1261.
The catalogue contains a total number of ~39 900 galaxies, for which we provide the automated estimates of the morphological type, applying
the purposely devised tool MORPHOT to the V-band WINGS imaging. The used tool is non-parametric and fully empirical. In particular, MORPHOT exploits 21 morphological diagnostics, directly and easily computable from the galaxy image, to provide two independent classifications: one based on a maximum likelihood (ML), semi- analytical technique and the other one on a neural network (NN) machine. A suitably selected sample of ∼1000 visually classified WINGS galaxies is used to calibrate the diagnostics for theML estimator and as a training set in the NN machine. The final morphological estimator combines the two techniques. (http://adsabs.harvard.edu/abs/2012MNRAS.420..926F)
Using V band photometry of the WINGS survey, we derive galaxy luminosity functions (LF) in nearby clusters. This sample is complete down to M_V_=-15.15, and it is homogeneous, thus facilitating the study of an unbiased sample of clusters with different characteristics. We constructed the photometric LF for 72 out of the original 76 WINGS clusters, excluding only those without a velocity dispersion estimate. For each cluster we obtained the LF for galaxies in a region of radius=0.5xr_200_, and fitted them with single and double Schechter's functions. We also derive the composite LF for the entire sample, and those pertaining to different morphological classes. Finally, we derive the spectroscopic cumulative LF for 2009 galaxies that are cluster members. The double Schechter fit parameters are correlated neither with the cluster velocity dispersion nor with the X-ray luminosity. Our median values of the Schechter's fit slope are, on average, in agreement with measurements of nearby clusters, but are less steep that those derived from large surveys, such as the SDSS. Early-type galaxies out number late-types at all magnitudes, but both early and late types contribute equally to the faint end of the LF. Finally, the spectroscopic LF is in excellent agreement with the one derived for A2199, A85 and Virgo, and with the photometric LF at the bright magnitudes (where both are available). There is a large spread in the LF of different clusters, however, this spread is not caused by correlation of the LF shape with cluster characteristics such as X-ray luminosity or velocity dispersions. The faint end is flatter than previously derived ({alpha}_f_=-1.7), which is at odds with that predicted from numerical simulations.
Optical (V, B) photometric catalog of WINGS detections (galaxies, stars, unclassified objects) in the 76 wide--fields of the WINGS survey of local clusters of galaxies. (http://adsabs.harvard.edu/abs/2009A%26A...497..667V)
WINGS (WIde-field Nearby Galaxy-cluster Survey) is an all-sky (|b|>20) survey of a complete, X-ray selected sample of galaxy clusters in the redshift range 0.04-0.07. The core of the WINGS project is the optical (B,V) imaging survey. It provides photometric data for huge samples of galaxies (~550,000) and stars (~190,000) in the inner field (34'x34') of 77 nearby galaxy clusters. (http://adsabs.harvard.edu/abs/2006A%26A...445..805F)
The catalog gives the redshifts for ~6000 galaxies of the WINGS survey. The given membership has been derived using as cluster velocity dispersion the new determination that takes into account literature as well as this dataset.(http://adsabs.harvard.edu/abs/2009A%26A...495..707C)
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