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The Spitzer-IRAC/MIPS Extragalactic Survey (SIMES). II. Enhanced Nuclear Accretion Rate in Galaxy Groups at z ∼ 0.2

Baronchelli, I. and Rodighiero, G. and Teplitz, H. I. and Scarlata, C. M. and Franceschini, A. and Berta, S. and Barrufet, L. and Vaccari, M. and Bonato, M. and Ciesla, L. and Zanella, A. and Carraro, R. and Mancini, C. and Puglisi, A. and Malkan, M. and Mei, S. and Marchetti, L. and Colbert, J. and Sedgwick, C. and Serjeant, S. and Pearson, C. and Radovich, M. and Grado, A. and Limatola, L. and Covone, G. (2018) The Spitzer-IRAC/MIPS Extragalactic Survey (SIMES). II. Enhanced Nuclear Accretion Rate in Galaxy Groups at z ∼ 0.2. Astrophysical Journal, 857 (1). Art. No. 64. ISSN 1538-4357. https://resolver.caltech.edu/CaltechAUTHORS:20180416-144946143

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Abstract

For a sample of star-forming galaxies in the redshift interval 0.15 < z < 0.3, we study how both the relative strength of the active galactic nucleus (AGN) infrared emission, compared to that due to the star formation (SF), and the numerical fraction of AGNs change as a function of the total stellar mass of the hosting galaxy group (M*_(group)) between 10^(10.25) and 10^(11.9) M ⊙. Using a multicomponent spectral energy distribution SED fitting analysis, we separate the contribution of stars, AGN torus, and star formation to the total emission at different wavelengths. This technique is applied to a new multiwavelength data set in the SIMES field (23 not-redundant photometric bands), spanning the wavelength range from the UV (GALEX) to the far-IR (Herschel) and including crucial AKARI and WISE mid-IR observations (4.5 μm < λ < 24 μm), where the black hole thermal emission is stronger. This new photometric catalog, which includes our best photo-z estimates, is released through the NASA/IPAC Infrared Science Archive (IRSA). Groups are identified through a friends-of-friends algorithm (~62% purity, ~51% completeness). We identified a total of 45 galaxies requiring an AGN emission component, 35 of which are in groups and 10 in the field. We find the black hole accretion rate (BHAR) ∝ (M*_(group))^(1.21±0.27) and (BHAR/SFR) ∝ ((M*_(group))^(1.04±0.24), while, in the same range of M*_(group), we do not observe any sensible change in the numerical fraction of AGNs. Our results indicate that the nuclear activity (i.e., the BHAR and the BHAR/SFR ratio) is enhanced when galaxies are located in more massive and richer groups.


Item Type:Article
Related URLs:
URLURL TypeDescription
https://doi.org/10.3847/1538-4357/aab78bDOIArticle
http://iopscience.iop.org/article/10.3847/1538-4357/aab78b/metaPublisherArticle
https://arxiv.org/abs/1803.06356arXivDiscussion Paper
ORCID:
AuthorORCID
Baronchelli, I.0000-0003-0556-2929
Rodighiero, G.0000-0002-9415-2296
Teplitz, H. I.0000-0002-7064-5424
Scarlata, C. M.0000-0002-9136-8876
Berta, S.0000-0002-0320-1532
Vaccari, M.0000-0002-6748-0577
Zanella, A.0000-0001-8600-7008
Mancini, C.0000-0002-4297-0561
Puglisi, A.0000-0001-9369-1805
Malkan, M.0000-0001-6919-1237
Mei, S.0000-0002-2849-559X
Marchetti, L.0000-0003-3948-7621
Serjeant, S.0000-0002-0517-7943
Pearson, C.0000-0001-6139-649X
Grado, A.0000-0002-0501-8256
Limatola, L.0000-0002-1896-8605
Additional Information:© 2018 The American Astronomical Society. Received 2017 October 2; revised 2018 February 26; accepted 2018 March 15; published 2018 April 16. This work is based on observations obtained with AKARI, a JAXA project with the participation of ESA; data products from the Wide-field Infrared Survey Explorer, which is a joint project of the University of California, Los Angeles, and the Jet Propulsion Laboratory/California Institute of Technology, funded by the National Aeronautics and Space Administration; data from the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA; data from Herschel, an ESA space observatory with science instruments provided by European-led Principal Investigator consortia and with important participation from NASA; and observations made with the NASA Galaxy Evolution Explorer, operated for NASA by the California Institute of Technology under NASA contract NAS5-98034. Further fundamental observations were obtained with the ESO VST and VISTA and the CTIO observatories. We gratefully acknowledge Simon Lilly and Alvio Renzini for supplying us with the extended sample of spectroscopic redshifts measured in the COSMOS field. M.V. acknowledges support from the European Commission Research Executive Agency (FP7-SPACE-2013-1 GA 607254), the South African Department of Science and Technology (DST/CON 0134/2014), and the Italian Ministry for Foreign Affairs and International Cooperation (PGR GA ZA14GR02). R.C. acknowledges financial support from CONICYT Doctorado Nacional No. 21161487. I.B. thanks Stefano Rubele for the useful discussions concerning the technical details of the optical data reduction, Lee Armus for his comments on the AGN fraction reliability, and Gabriele Rodeghiero and Maurizio Pajola for their helpful comments about data representation.
Group:Infrared Processing and Analysis Center (IPAC)
Funders:
Funding AgencyGrant Number
NASA/JPL/CaltechUNSPECIFIED
NASANAS5-98034
European Commission Research Executive AgencyFP7-SPACE-2013-1 GA 607254
Department of Science and Technology (South Africa)DST/CON 0134/2014
Ministero Affari Esteri e della Cooperazione Internazionale (MAECI)PGR GA ZA14GR02
Comisión Nacional de Investigación Científica y Tecnológica (CONICYT)21161487
Subject Keywords:galaxies: evolution – galaxies: groups: general – galaxies: star formation – infrared: galaxies – quasars: supermassive black holes – submillimeter: galaxies
Issue or Number:1
Record Number:CaltechAUTHORS:20180416-144946143
Persistent URL:https://resolver.caltech.edu/CaltechAUTHORS:20180416-144946143
Official Citation:I. Baronchelli et al 2018 ApJ 857 64
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:85883
Collection:CaltechAUTHORS
Deposited By: Tony Diaz
Deposited On:16 Apr 2018 22:24
Last Modified:03 Oct 2019 19:36

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