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Linking the X-ray and infrared properties of star-forming galaxies at z < 1.5

Symeonidis, M. and Georgakakis, A. and Page, M. J. and Bock, J. and Bonzini, M. and Buat, V. and Farrah, D. and Franceschini, A. and Ibar, E. and Lutz, D. and Magnelli, B. and Magdis, G. and Oliver, S. J. and Pannella, M. and Paolillo, M. and Rosario, D. and Roseboom, I. G. and Vaccari, M. and Villforth, C. (2014) Linking the X-ray and infrared properties of star-forming galaxies at z < 1.5. Monthly Notices of the Royal Astronomical Society, 443 (4). pp. 3728-3740. ISSN 0035-8711. http://resolver.caltech.edu/CaltechAUTHORS:20141107-142352785

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Abstract

We present the most complete study to date of the X-ray emission from star formation in high-redshift (median z = 0.7; z < 1.5), IR-luminous (L_(IR) = 10^(10)–10^(13) L_⊙) galaxies detected by Herschel's PACS and SPIRE instruments. For our purpose, we take advantage of the deepest X-ray data to date, the Chandra Deep Fields (North and South). Sources which host AGN are removed from our analysis by means of multiple AGN indicators. We find an AGN fraction of 18 ± 2 per cent amongst our sample and note that AGN entirely dominate at values of log [L_X/L_(IR)] > −3 in both hard and soft X-ray bands. From the sources which are star formation dominated, only a small fraction are individually X-ray detected and for the bulk of the sample we calculate average X-ray luminosities through stacking. We find an average soft X-ray to infrared ratio of log 〈L_(SX)/L_(IR)〉 = −4.3 and an average hard X-ray to infrared ratio of log 〈L_(HX)/L_(IR)〉 = −3.8. We report that the X-ray/IR correlation is approximately linear through the entire range of LIR and z probed and, although broadly consistent with the local (z < 0.1) one, it does display some discrepancies. We suggest that these discrepancies are unlikely to be physical, i.e. due to an intrinsic change in the X-ray properties of star-forming galaxies with cosmic time, as there is no significant evidence for evolution of the L_X/L_(IR) ratio with redshift. Instead, they are possibly due to selection effects and remaining AGN contamination. We also examine whether dust obscuration in the galaxy plays a role in attenuating X-rays from star formation, by investigating changes in the L_X/L_(IR) ratio as a function of the average dust temperature. We conclude that X-rays do not suffer any measurable attenuation in the host galaxy.


Item Type:Article
Related URLs:
URLURL TypeDescription
http://dx.doi.org/10.1093/mnras/stu1441DOIArticle
http://mnras.oxfordjournals.org/content/443/4/3728PublisherArticle
http://arxiv.org/abs/1407.4511arXivDiscussion Paper
ORCID:
AuthorORCID
Page, M. J.0000-0002-6689-6271
Bock, J.0000-0002-5710-5212
Farrah, D.0000-0003-1748-2010
Lutz, D.0000-0003-0291-9582
Magdis, G.0000-0002-4872-2294
Oliver, S. J.0000-0001-7862-1032
Vaccari, M.0000-0002-6748-0577
Additional Information:© 2014 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society. Accepted 2014 July 16. Received 2014 July 15; in original form 2014 June 13. This paper uses data from Herschel’s photometers SPIRE and PACS. SPIRE has been developed by a consortium of institutes led by Cardiff Univ. (UK) and including Univ. Lethbridge (Canada); NAOC (China); CEA, LAM (France); IFSI, Univ. Padua (Italy); IAC (Spain); Stockholm Observatory (Sweden); Imperial College London, RAL, UCL-MSSL, UKATC, Univ. Sussex (UK); and Caltech, JPL, NHSC, Univ. Colorado (USA). This development has been supported by national funding agencies: CSA (Canada); NAOC (China); CEA, CNES, CNRS (France); ASI (Italy); MCINN (Spain); SNSB (Sweden); STFC, UKSA (UK); and NASA (USA). PACS has been developed by a consortium of institutes led by MPE (Germany) and including UVIE (Austria); KU Leuven, CSL, IMEC (Belgium); CEA, LAM (France); MPIA (Germany); INAF-IFSI/OAA/OAP/OAT, LENS, SISSA (Italy); IAC (Spain). This development has been supported by the funding agencies BMVIT (Austria), ESA-PRODEX (Belgium), CEA/CNES (France), DLR (Germany), ASI/INAF (Italy) and CICYT/MCYT (Spain). The scientific results reported in this paper are based to a significant degree on observations made by the Chandra X-ray Observatory.
Funders:
Funding AgencyGrant Number
Canadian Space Agency (CSA)UNSPECIFIED
National Astronomical Observatories, Chinese Academy of Sciences (NAOC)UNSPECIFIED
Commissariat à l’Energie Atomique (CEA)UNSPECIFIED
Centre National d'Études Spatiales (CNES)UNSPECIFIED
Centre National de la Recherche Scientifique (CNRS)UNSPECIFIED
Agenzia Spaziale Italiana (ASI)UNSPECIFIED
Ministerio de Ciencia e Innovación (MCINN)UNSPECIFIED
Swedish National Space Board (SNSB)UNSPECIFIED
Science and Technology Facilities Council (STFC)UNSPECIFIED
United Kingdom Space Agency (UKSA)UNSPECIFIED
NASAUNSPECIFIED
Bundesministerium für Verkehr, Innovation und Technologie (BMVIT)UNSPECIFIED
ESA-PRODEX (Belgium)UNSPECIFIED
Deutsches Zentrum für Luft- und Raumfahrt (DLR)UNSPECIFIED
Istituto Nazionale di Astrofisica (INAF)UNSPECIFIED
Comisión Interministerial de Ciencia y Tecnología (CICYT)UNSPECIFIED
Ministerio de Ciencia Y Tecnologia (MCYT)UNSPECIFIED
Subject Keywords:galaxies: evolution; galaxies: general; galaxies: high-redshift; galaxies: starburst; submillimetre: general; X-rays: galaxies
Issue or Number:4
Record Number:CaltechAUTHORS:20141107-142352785
Persistent URL:http://resolver.caltech.edu/CaltechAUTHORS:20141107-142352785
Official Citation:Symeonidis, M., Georgakakis, A., Page, M. J., Bock, J., Bonzini, M., Buat, V., . . . Villforth, C. (2014). Linking the X-ray and infrared properties of star-forming galaxies at z < 1.5. Monthly Notices of the Royal Astronomical Society, 443(4), 3728-3740. doi: 10.1093/mnras/stu1441
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:51457
Collection:CaltechAUTHORS
Deposited By: Jason Perez
Deposited On:10 Nov 2014 19:02
Last Modified:09 Jul 2019 21:42

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