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dc.contributor.authorKirkpatrick, A.
dc.contributor.authorAlberts, Stacey
dc.contributor.authorPope, Alexandra
dc.contributor.authorBarro, Guillermo
dc.contributor.authorBonato, Matteo
dc.contributor.authorKocevski, Dale D.
dc.contributor.authorPérez-González, Pablo
dc.contributor.authorRieke, George H.
dc.contributor.authorRodríguez-Muñoz, Lucia
dc.contributor.authorSajina, Anna
dc.contributor.authorGrogin, Norman A.
dc.contributor.authorMantha, Kameswara Bharadwaj
dc.contributor.authorPandya, Viraj
dc.contributor.authorPforr, Janine
dc.contributor.authorSalvato, Mara
dc.contributor.authorSantini, Paola
dc.date.accessioned2017-12-04T22:59:28Z
dc.date.available2017-12-04T22:59:28Z
dc.date.issued2017-11-07
dc.identifier.citationThe AGN–Star Formation Connection: Future Prospects with JWST 2017, 849 (2):111 The Astrophysical Journalen
dc.identifier.issn1538-4357
dc.identifier.doi10.3847/1538-4357/aa911d
dc.identifier.urihttp://hdl.handle.net/10150/626176
dc.description.abstractThe bulk of the stellar growth over cosmic time is dominated by IR-luminous galaxies at cosmic noon (z = 1-2), many of which harbor a hidden active galactic nucleus (AGN). We use state-of-the-art infrared color diagnostics, combining Spitzer and Herschel observations, to separate dust-obscured AGNs from dusty star-forming galaxies (SFGs) in the CANDELS and COSMOS surveys. We calculate 24 mu m counts of SFGs, AGN/star-forming "Composites," and AGNs. AGNs and Composites dominate the counts above 0.8 mJy at 24 mu m, and Composites form at least 25% of an IR sample even to faint detection limits. We develop methods to use the Mid-Infrared Instrument (MIRI) on JWST to identify dust-obscured AGNs and Composite galaxies from z similar to 1-2. With the sensitivity and spacing of MIRI filters, we will detect >4 times as many AGN hosts as with Spitzer/IRAC criteria. Any star formation rates based on the 7.7 mu m PAH feature (likely to be applied to MIRI photometry) must be corrected for the contribution of the AGN, or the star formation rate will be overestimated by similar to 35% for cases where the AGN provides half the IR luminosity and similar to 50% when the AGN accounts for 90% of the luminosity. Finally, we demonstrate that our MIRI color technique can select AGNs with an Eddington ratio of lambda(Edd) similar to 0.01 and will identify AGN hosts with a higher specific star formation rate than X-ray techniques alone. JWST/MIRI will enable critical steps forward in identifying and understanding dust-obscured AGNs and the link to their host galaxies.
dc.description.sponsorshipYCAA; NASA [ADAP13-0054]; NSF AAG [AST-1312418, AST-1313206]en
dc.language.isoenen
dc.publisherIOP PUBLISHING LTDen
dc.relation.urlhttp://stacks.iop.org/0004-637X/849/i=2/a=111?key=crossref.0f7b52760cbebba780f7ac3b199f7da7en
dc.rights© 2017. The American Astronomical Society. All rights reserved.en
dc.subjectgalaxies: activeen
dc.subjectgalaxies: photometryen
dc.subjectgalaxies: star formationen
dc.titleThe AGN–Star Formation Connection: Future Prospects with JWSTen
dc.typeArticleen
dc.contributor.departmentUniv Arizona, Steward Observen
dc.identifier.journalThe Astrophysical Journalen
dc.description.collectioninformationThis item from the UA Faculty Publications collection is made available by the University of Arizona with support from the University of Arizona Libraries. If you have questions, please contact us at repository@u.library.arizona.edu.en
dc.eprint.versionFinal published versionen
refterms.dateFOA2018-08-14T21:43:05Z
html.description.abstractThe bulk of the stellar growth over cosmic time is dominated by IR-luminous galaxies at cosmic noon (z = 1-2), many of which harbor a hidden active galactic nucleus (AGN). We use state-of-the-art infrared color diagnostics, combining Spitzer and Herschel observations, to separate dust-obscured AGNs from dusty star-forming galaxies (SFGs) in the CANDELS and COSMOS surveys. We calculate 24 mu m counts of SFGs, AGN/star-forming "Composites," and AGNs. AGNs and Composites dominate the counts above 0.8 mJy at 24 mu m, and Composites form at least 25% of an IR sample even to faint detection limits. We develop methods to use the Mid-Infrared Instrument (MIRI) on JWST to identify dust-obscured AGNs and Composite galaxies from z similar to 1-2. With the sensitivity and spacing of MIRI filters, we will detect >4 times as many AGN hosts as with Spitzer/IRAC criteria. Any star formation rates based on the 7.7 mu m PAH feature (likely to be applied to MIRI photometry) must be corrected for the contribution of the AGN, or the star formation rate will be overestimated by similar to 35% for cases where the AGN provides half the IR luminosity and similar to 50% when the AGN accounts for 90% of the luminosity. Finally, we demonstrate that our MIRI color technique can select AGNs with an Eddington ratio of lambda(Edd) similar to 0.01 and will identify AGN hosts with a higher specific star formation rate than X-ray techniques alone. JWST/MIRI will enable critical steps forward in identifying and understanding dust-obscured AGNs and the link to their host galaxies.


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