Two-dimensional multi-component photometric decomposition of CALIFA galaxies

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We present a two-dimensional multi-component photometric decomposition of 404 galaxies from the Calar Alto Legacy Integral Field Area data release 3 (CALIFA-DR3). They represent all possible galaxies with no clear signs of interaction and not strongly inclined in the final CALIFA data release. Galaxies are modelled in the g, r, and i Sloan Digital Sky Survey (SDSS) images including, when appropriate, a nuclear point source, bulge, bar, and an exponential or broken disc component. We use a human-supervised approach to determine the optimal number of structures to be included in the fit. The dataset, including the photometric parameters of the CALIFA sample, is released together with statistical errors and a visual analysis of the quality of each fit. The analysis of the photometric components reveals a clear segregation of the structural composition of galaxies with stellar mass. At high masses (log (M-*/M-circle dot) > 11), the galaxy population is dominated by galaxies modelled with a single Sersic or a bulge+disc with a bulge-to-total (B/T) luminosity ratio B/T > 0.2. At intermediate masses (9.5 < log (M-*/M-circle dot) < 11), galaxies described with bulge+disc but B/T < 0.2 are preponderant, whereas, at the low mass end (log (M-*/M-circle dot) < 9.5), the prevailing population is constituted by galaxies modelled with either pure discs or nuclear point sources+discs (i.e., no discernible bulge). We obtain that 57% of the volume corrected sample of disc galaxies in the CALIFA sample host a bar. This bar fraction shows a significant drop with increasing galaxy mass in the range 9.5 < log (M-*/M-circle dot) < 11.5. The analyses of the extended multi-component radial profile result in a volume-corrected distribution of 62%, 28%, and 10% for the so-called Type I (pure exponential), Type II (down-bending), and Type III (up-bending) disc profiles, respectively. These fractions are in discordance with previous findings. We argue that the different methodologies used to detect the breaks are the main cause for these differences.
© ESO, 2017. Artículo firmado por 23 autores. J.M.A. and V.W. acknowledges support from the European Research Council Starting Grant (SEDmorph; P.I. V. Wild). L.S.M acknowledges financial support from the Spanish Ministerio de Economía y Competitividad (MINECO) via grant AYA2012-31935. A.d.L.C. acknowledges support from the UK Science and Technology Facilities Council (STFC) grant ST/J001651/1 and from the Spanish Ministry of Economy and Competitiveness (MINECO) grant AYA2011-24728. C.C.-T. thanks the support of the Spanish Ministerio de Educación, Cultura y Deporte by means of the FPU fellowship program and the support from the Plan Nacional de Investigación y Desarrollo funding programs, AYA2012-30717 and AyA2013-46724P, of Spanish Ministerio de Economía y Competitividad (MINECO)'. E.F. acknowledges support by the MINECO grant AYA2014-53506-P and the Junta de Andalucía grant FQM108. J.L.A. acknowledges financial support from the MINECO grant AYA2013-43188-P. E.M.C. and L.C. are supported by Padua University through grants 60A02-5857/13, 60A025833/14, and 60A02-4434/15. L.C. acknowledges the University of St. Andrews for the hospitality while this paper was in progress. L.G. was supported in part by FONDECYT through grant 3140566 and the US National Science Foundation under Grant AST-1311862. I.M. acknowledges financial support from the MINECO grant AYA-42227-P. RAOM acknowledges support from CAPES (Brazil) through a PDJ fellowship from project 88881.030413/2013-01, program CSF-PVE. P.P. is supported by FCT through the Investigador FCT Contract No. IF/01220/2013 and POPH/FSE (EC) by FEDER funding through the program COMPETE. P.S.B. acknowledge financial support from the: CONICYT-Chile Basal-CATA PFB-06/2007 and the AYA2013-48226-C3-1-P by the Ministerio de Ciencia e Innovación. This paper is based on data from the Calar Alto Legacy Integral Field Area Survey, CALIFA (, funded by the Spanish Ministery of Science under grant ICTS-2009-10, and the Centro Astronómico Hispano-Alemán. Based on observations collected at the Centro Astronómico Hispano Alemán (CAHA) at Calar Alto, operated jointly by the Max-Planck Institut fur Astronomie and the Instituto de Astrofísica de Andalucía (CSIC). We acknowledge the use of SDSS data (
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