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|Title:||Galaxy luminosity functions in WINGS clusters||Authors:||MORETTI, ALESSIA
POGGIANTI, Bianca Maria
Couch, W. J.
|Issue Date:||2015||Journal:||ASTRONOMY & ASTROPHYSICS||Number:||581||First Page:||A11||Abstract:||<BR /> Aims: Using V band photometry of the WINGS survey, we derive galaxy luminosity functions (LF) in nearby clusters. This sample is complete down to M<SUB>V</SUB> = -15.15, and it is homogeneous, thus facilitating the study of an unbiased sample of clusters with different characteristics. <BR /> Methods: 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 = 0.5 × r<SUB>200</SUB>, 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. <BR /> Results: 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). <BR /> Conclusions: 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 (α<SUB>f</SUB> = -1.7), which is at odds with that predicted from numerical simulations. <P />Based on observations collected at the European Organisation for Astronomical Research in the Southern Hemisphere, Chile. Progs. ID 67.A-0030, 68.A-0139, and 69.A-0119.Table 1 and full Fig. 1 (Fig. A.1) are available in electronic form at <A href="http://www.aanda.org/10.1051/0004-6361/201526080/olm">http://www.aanda.org</A>||Acknowledgments:||We acknowledge the financial contribution from PRIN/INAF2014 “Galaxy evolution from cluster cores to filaments”. B.V. acknowledges the World Premier International Research Center Initiative (WPI), MEXT, Japan and the Kakenhi Grant-in-Aid for Young Scientists (B)(26870140) from the Japan Society for the Promotion of Science (JSPS). We thank the anonymous referee whose comments greatly improved the paper.||URI:||http://hdl.handle.net/20.500.12386/23163||URL:||https://www.aanda.org/articles/aa/abs/2015/09/aa26080-15/aa26080-15.html
|Appears in Collections:||1.01 Articoli in rivista|
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