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Tracing the evolution of dust obscured star-formation and accretion back to the reionisation epoch with SPICA

hal.structure.identifierINAF - Osservatorio Astronomico di Bologna [OABO]
dc.contributor.authorGRUPPIONI, C.
hal.structure.identifierAstrophysique Interprétation Modélisation [AIM (UMR7158 / UMR_E_9005 / UM_112)]
dc.contributor.authorCIESLA, L.
hal.structure.identifierAUTRES
dc.contributor.authorHATZIMINAOGLOU, E.
hal.structure.identifierIstituto Nazionale di Astrofisica [INAF]
dc.contributor.authorPOZZI, F.
hal.structure.identifierDipartimento di Fisica e Astronomia "Galileo Galilei"
dc.contributor.authorRODIGHIERO, G.
hal.structure.identifierINAF - Osservatorio Astronomico di Roma [OAR]
dc.contributor.authorSANTINI, P.
dc.contributor.authorARMUS, L.
hal.structure.identifierUniversiteit Gent = Ghent University = Université de Gand [UGENT]
dc.contributor.authorBAES, M.
hal.structure.identifierFORMATION STELLAIRE 2017
dc.contributor.authorBRAINE, J.
hal.structure.identifierLaboratoire d'Etude du Rayonnement et de la Matière en Astrophysique [LERMA]
dc.contributor.authorCHARMANDARIS, V.
hal.structure.identifierAstrophysics Group
dc.contributor.authorCLEMENTS, D. L.
dc.contributor.authorCHRISTOPHER, N.
hal.structure.identifierAstrophysique Interprétation Modélisation [AIM (UMR7158 / UMR_E_9005 / UM_112)]
dc.contributor.authorDANNERBAUER, H.
dc.contributor.authorEFSTATHIOU, A.
hal.structure.identifierSteward Observatory
dc.contributor.authorEGAMI, E.
hal.structure.identifierIstituto di Astrofisica e Planetologia Spaziali - INAF [IAPS]
dc.contributor.authorFERNÁNDEZ-ONTIVEROS, J. A.
dc.contributor.authorFONTANOT, F.
hal.structure.identifierDipartimento di Fisica e Astronomia "Galileo Galilei"
dc.contributor.authorFRANCESCHINI, A.
dc.contributor.authorGONZALEZ-ALFONSO, E.
hal.structure.identifierSchool of Physics and Astronomy [Cardiff]
dc.contributor.authorGRIFFIN, M.
dc.contributor.authorKANEDA, H.
dc.contributor.authorMARCHETTI, L.
hal.structure.identifierINAF - Osservatorio Astronomico di Trieste [OAT]
dc.contributor.authorMONACO, P.
dc.contributor.authorNAKAGAWA, T.
dc.contributor.authorONAKA, T.
hal.structure.identifierinconnu
dc.contributor.authorPAPADOPOULOS, A.
dc.contributor.authorPEARSON, C.
hal.structure.identifierAUTRES
dc.contributor.authorPÉREZ-FOURNON, I.
dc.contributor.authorPEREZ-GONZALEZ, P.
dc.contributor.authorROELFSEMA, P.
dc.contributor.authorSCOTT, D.
hal.structure.identifierDepartment of Physics and Astronomy [Milton Keynes]
dc.contributor.authorSERJEANT, S.
hal.structure.identifierAntarctic Research a European Network for Astrophysics [ARENA]
dc.contributor.authorSPINOGLIO, L.
hal.structure.identifierDipartimento di Astronomia [Padova]
hal.structure.identifierDepartment of Physics and Astronomy [South Africa]
dc.contributor.authorVACCARI, M.
hal.structure.identifierSRON Netherlands Institute for Space Research [SRON]
dc.contributor.authorVAN DER TAK, F.
hal.structure.identifierAlma Mater Studiorum Università di Bologna = University of Bologna [UNIBO]
dc.contributor.authorVIGNALI, C.
dc.contributor.authorWANG, L.
dc.contributor.authorWADA, T.
dc.date.issued2017
dc.identifier.issn1323-3580
dc.description.abstractEnOur current knowledge of star formation and accretion luminosity at high-redshift (z>3-4), as well as the possible connections between them, relies mostly on observations in the rest-frame ultraviolet (UV), which are strongly affected by dust obscuration. Due to the lack of sensitivity of past and current infrared (IR) instrumentation, so far it has not been possible to get a glimpse into the early phases of the dust-obscured Universe. Among the next generation of IR observatories, SPICA, observing in the 12-350 micron range, will be the only facility that can enable us to make the required leap forward in understanding the obscured star-formation rate and black-hole accretion rate densities (SFRD and BHARD, respectively) with respect to what Spitzer and Herschel achieved in the mid- and far-IR at z<3. In particular, SPICA will have the unique ability to trace the evolution of the obscured SFRD and BHARD over cosmic time, from the peak of their activity back to the reionisation epoch (i.e., 3 < z < 6 - 7), where its predecessors had severe limitations. Here we discuss the potential of both deep and shallow photometric surveys performed with the SPICA mid-IR instrument (SMI), enabled by the very low level of impact of dust obscuration in a band centred at 34 micron. These unique unbiased photometric surveys that SPICA will perform will be followed up by observations both with the SPICA spectrometers and with other facilities at shorter and longer wavelengths, with the aim to fully characterise the evolution of AGNs and star-forming galaxies after re-ionisation.
dc.language.isoen
dc.publisherCambridge University Press (CUP)
dc.title.enTracing the evolution of dust obscured star-formation and accretion back to the reionisation epoch with SPICA
dc.typeArticle de revue
dc.identifier.doi10.1017/pasa.2017.49
dc.subject.halPlanète et Univers [physics]/Astrophysique [astro-ph]/Astrophysique galactique [astro-ph.GA]
dc.identifier.arxiv1710.02353
bordeaux.journalPublications of the Astronomical Society of Australia
bordeaux.pageid.e055
bordeaux.volume34
bordeaux.peerReviewedoui
hal.identifierhal-01612984
hal.version1
hal.popularnon
hal.audienceInternationale
hal.origin.linkhttps://hal.archives-ouvertes.fr//hal-01612984v1
bordeaux.COinSctx_ver=Z39.88-2004&amp;rft_val_fmt=info:ofi/fmt:kev:mtx:journal&amp;rft.jtitle=Publications%20of%20the%20Astronomical%20Society%20of%20Australia&amp;rft.date=2017&amp;rft.volume=34&amp;rft.spage=id.e055&amp;rft.epage=id.e055&amp;rft.eissn=1323-3580&amp;rft.issn=1323-3580&amp;rft.au=GRUPPIONI,%20C.&amp;CIESLA,%20L.&amp;HATZIMINAOGLOU,%20E.&amp;POZZI,%20F.&amp;RODIGHIERO,%20G.&amp;rft.genre=article


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