Detalles de publicación
PP 025024
The Complete Spitzer Survey of Stellar Structure in Galaxies (CS4G)
(1) Instituto de Astrofísica de Canarias, c/ Vía Láctea s/n, E-38205, La Laguna, Tenerife, Spain
(2) Departamento de Astrofísica, Universidad de La Laguna, E-38206, La Laguna, Tenerife, Spain
(3) Space Physics and Astronomy Research Unit, University of Oulu, Pentti Kaiteran katu 1, FI-90014 Oulu, Finland
(4) Departamento de Física de la Tierra y Astrofísica, Universidad Complutense de Madrid, E-28040 Madrid, Spain
(5) Centre of Astrophysics Research, School of Physics, Astronomy and Mathematics, University of Hertfordshire, Hatfield, UK
(6) Department of Physics and Astronomy, University of Alabama, Box 870324, Tuscaloosa, AL 35487, USA
(7) IPAC, Mail Code 314-6, Caltech, 1200 E. California Blvd., Pasadena, CA 91125, USA
(8) Max-Planck-Institut für Extraterrestriche Physik, Giessenbach-Str. 1, D-85748 Garching, Germany
(9) Aix Marseille Univ, CNRS, CNES, LAM, Marseille, France
(10) Centre for Extragalactic Astronomy, Department of Physics, Durham University, South Road, Durham DH1 3LE, UK
(11) MMT Observatory, University of Arizona, 933 N Cherry Ave, Tucson AZ 85721
(12) Kavli Institute for Astronomy and Astrophysics, Peking University, 12 Beijing 100871, P. R. China
(13) Department of Astronomy, School of Physics, Peking University, Beijing 100871, P. (14) University of Louisville, Department of Physics and Astronomy, 102 Natural Science Building, 40292, KY Louisville, USA
(15) Finnish Centre of Astronomy with ESO (FINCA), Vesilinnantie 5, FI-20014 University of Turku, Finland
(16) Specim, Spectral Imaging Ltd., Elektroniikkatie 13, FI-90590 Oulu, Finland
(17) Department of Astronomy and Atmospheric Sciences, Kyungpook National University, Daegu 702-701, Republic of Korea
(18) Department of Physics and Astronomy, Stony Brook University, Stony Brook, NY 11794-3800, USA
(19) Normet Oy, Elektroniikkatie 8, FI-90590 Oulu, Finland
(20) The Observatories, Carnegie Institution for Science, 813 Santa Barbara Street, Pasadena, CA 91101, USA
(21) Department of Astronomy \& Astrophysics, University of Chicago, 5640 South Ellis Avenue, Chicago, IL 60637, USA
(22) Observatório do Valongo, Universidade Federal do Rio de Janeiro, Rio de Janeiro, Brazil
(23) Kapteyn Astronomical Institute, University of Groningen, PO Box 800, NL-9700 AV Groningen, the Netherlands
(24) Observatorio Astronómico Nacional (IGN), C/Alfonso XII, 3, E28014 Madrid, Spain
(25) NASA Headquarters Mary W. Jackson Building, 300 E Street SW, Washington, DC 20546, USA
(26) Steward Observatory and Department of Astronomy, University of Arizona, 933 N. Cherry Ave., Tucson, AZ 85721, USA
The \textit{Spitzer} Survey of Stellar Structure in Galaxies (S$^4$G), together with its Early Type Galaxy (ETG) extension, stand as the most extensive dataset of deep, uniform mid-infrared (mid-IR; 3.6 and 4.5$\,\mu$m) imaging for a sample of $2817$ nearby ($d<40 \,$Mpc) galaxies. However, the velocity criterion used to select the original sample results in an additional 422 galaxies without H\,{\sc i} detection that ought to have been included in the S$^4$G on the basis of their optical recession velocities.
In order to create a complete magnitude-, size- and volume-limited sample of nearby galaxies we collect $3.6\,\mu$m and $i$-band images using archival data from different surveys and complement it with new observations for the missing galaxies. Since most, but not all, of these galaxies have a Hubble type in Hyperleda $T_\mathrm{HL}>0$, we denote the sample of these additional galaxies as Disc Galaxy (DG) extension. We present the Complete \textit{Spitzer} Survey of Stellar Structure in Galaxies (CS$^4$G), encompassing a sample of $3239$ galaxies (S$^4$G$+$ETG$+$DG) with consistent imaging, surface brightness profiles, photometric parameters, and revised morphological classification.
Following the original strategy of the S$^4$G survey, we produce masks, surface brightness profiles, and curves of growth using masked $3.6\,\mu$m and $i$-band images. From these profiles, we derive the integrated quantities: total magnitude, stellar mass, concentration parameter, and galaxy size, converting between optical \textit{i}-band and $3.6\,\mu$m. We re-measure these parameters also for the S$^4$G and ETG to create a homogenous sample. We present new morphological revised $T$-types and we showcase mid-IR scaling relations for the stellar mass, galaxy size, concentration index, and morphological type.
Our new masking procedure increases the number of pixels masked out by a factor of five, improving the masking of fainter regions over previous S$^4$G data. Our photometric parameters from \textit{i}-band imaging yield measurements consistent with the original sample (S$^4$G) and its ETG extension in the $3.6\,\mu $m band. The new DG extension consists of galaxies with a wide morphological range ($-5<T_{\rm HL}<10$) and a mass range of $6<\log(M_*/M_\odot)<11$. The galaxies in the DG sample have an average mass of $\log(M_*/M_\odot) = 9.21$, an average galaxy isophotal radius at $25.5\,$mag\,arcsec$^{-2}$ of $R_{25.5}=7.1\,$kpc, and an average concentration index of $C_{82} = 2.92$.
We complete the S$^4$G sample by incorporating 422 galaxies into the original dataset. The new galaxies constitute 15\% of the total previous sample (S$^4$G+ETG), but in the lower-mass range ($M_*<10^{9}M_\odot$), the disc galaxy extension increases the sample by 36\%. The CS$^4$G includes at least 99.94\% of the complete sample of nearby galaxies, meeting the original selection criteria based on a comparison with the NED database. We make the images and surface brightness profiles available to the community together with the conjunct catalogue of the whole CS$^4$G dataset with consistent photometric measurements for 3239 galaxies. The CS$^4$G will enable a wide set of investigations into galaxy structure and evolution, and complement optical, near-infrared and mid-IR imaging to be obtained in coming years with \textit{Euclid}, Rubin, \textit{Roman} and other research projects.
In order to create a complete magnitude-, size- and volume-limited sample of nearby galaxies we collect $3.6\,\mu$m and $i$-band images using archival data from different surveys and complement it with new observations for the missing galaxies. Since most, but not all, of these galaxies have a Hubble type in Hyperleda $T_\mathrm{HL}>0$, we denote the sample of these additional galaxies as Disc Galaxy (DG) extension. We present the Complete \textit{Spitzer} Survey of Stellar Structure in Galaxies (CS$^4$G), encompassing a sample of $3239$ galaxies (S$^4$G$+$ETG$+$DG) with consistent imaging, surface brightness profiles, photometric parameters, and revised morphological classification.
Following the original strategy of the S$^4$G survey, we produce masks, surface brightness profiles, and curves of growth using masked $3.6\,\mu$m and $i$-band images. From these profiles, we derive the integrated quantities: total magnitude, stellar mass, concentration parameter, and galaxy size, converting between optical \textit{i}-band and $3.6\,\mu$m. We re-measure these parameters also for the S$^4$G and ETG to create a homogenous sample. We present new morphological revised $T$-types and we showcase mid-IR scaling relations for the stellar mass, galaxy size, concentration index, and morphological type.
Our new masking procedure increases the number of pixels masked out by a factor of five, improving the masking of fainter regions over previous S$^4$G data. Our photometric parameters from \textit{i}-band imaging yield measurements consistent with the original sample (S$^4$G) and its ETG extension in the $3.6\,\mu $m band. The new DG extension consists of galaxies with a wide morphological range ($-5<T_{\rm HL}<10$) and a mass range of $6<\log(M_*/M_\odot)<11$. The galaxies in the DG sample have an average mass of $\log(M_*/M_\odot) = 9.21$, an average galaxy isophotal radius at $25.5\,$mag\,arcsec$^{-2}$ of $R_{25.5}=7.1\,$kpc, and an average concentration index of $C_{82} = 2.92$.
We complete the S$^4$G sample by incorporating 422 galaxies into the original dataset. The new galaxies constitute 15\% of the total previous sample (S$^4$G+ETG), but in the lower-mass range ($M_*<10^{9}M_\odot$), the disc galaxy extension increases the sample by 36\%. The CS$^4$G includes at least 99.94\% of the complete sample of nearby galaxies, meeting the original selection criteria based on a comparison with the NED database. We make the images and surface brightness profiles available to the community together with the conjunct catalogue of the whole CS$^4$G dataset with consistent photometric measurements for 3239 galaxies. The CS$^4$G will enable a wide set of investigations into galaxy structure and evolution, and complement optical, near-infrared and mid-IR imaging to be obtained in coming years with \textit{Euclid}, Rubin, \textit{Roman} and other research projects.