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dc.contributor.author
Yan, L.
dc.contributor.author
Donoso, Emilio
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dc.contributor.author
Tsai, Chao Wei
dc.contributor.author
Stern, D.
dc.contributor.author
Assef, R. J.
dc.contributor.author
Eisenhardt, P.
dc.contributor.author
Blain, A. W.
dc.contributor.author
Cutri, R.
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Jarrett, T. H.
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Stanford, S. A.
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Wright, E.
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Bridge, C.
dc.contributor.author
Riechers, D. A.
dc.date.available
2015-08-12T15:32:59Z
dc.date.issued
2013-03-18
dc.identifier.citation
Yan, L.; Donoso, Emilio; Tsai, Chao Wei; Stern, D.; Assef, R. J.; et al.; Characterizing the Mid-infrared Extragalactic Sky with WISE and SDSS; American Astronomical Society; Astronomical Journal; 145; 5; 18-3-2013; 1-16
dc.identifier.issn
0004-6256
dc.identifier.uri
http://hdl.handle.net/11336/1643
dc.description.abstract
The Wide-field Infrared Survey Explorer (WISE) has completed its all-sky survey in four channels at 3.4–22um, detecting hundreds of millions of objects. We merge the WISE mid-infrared data with optical data from the Sloan Digital Sky Survey (SDSS) and provide a phenomenological characterization of WISE extragalactic sources. WISE is most sensitive at 3.4um (W1) and least sensitive at 22um (W4). The W1 band probes massive early-type galaxies out to z~1. This is more distant than SDSS identified early-type galaxies, consistent with the fact that 28% of 3.4um sources have faint or no r-band counterparts (r > 22.2). In contrast, 92%–95% of 12um and 22um sources have SDSS optical counterparts with r<22.2. WISE 3.4um detects 89.8% of the entire SDSS QSO catalog at S/N W1 >7σ, but only 18.9% at 22um with S/N W4 > 5 sigma. We show that WISE colors alone are effective in isolating stars (or local early-type galaxies), star-forming galaxies, and strong active galactic nuclei (AGNs)/QSOs at z~3. We highlight three major applications of WISE colors: (1) Selection of strong AGNs/QSOs at z~3 using W1−W2>0.8 and W2<15.2 criteria, producing a better census of this population. The surface density of these strong AGN/QSO candidates is 67.5$pm$0.14 deg^−2 . (2) Selection of dust-obscured, type-2 AGN/QSO candidates. We show that WISE W1−W2>0.8, W2 < 15.2 combined with r−W2>6 (Vega) colors can be used to identify type-2 AGN candidates. The fraction of these type-2 AGN candidates is one-third of all WISE color-selected AGNs. (3) Selection of ultraluminous infrared galaxies (ULIRGs) at z∼2 with extremely red colors, r − W4 > 14 or well-detected 22um sources lacking detections in the 3.4 and 4.6um bands. The surface density of z∼2 ULIRG candidates selected with r −W4 > 14 is 0.9$pm$0.07 deg−2 at S/N W4~5 (the corresponding, lowest flux density of 2.5 mJy), which is consistent with that inferred from smaller area Spitzer surveys. Optical spectroscopy of a small number of these high-redshift ULIRG candidates confirms our selection, and reveals a possible trend that optically fainter or r−W4 redder candidates are at higher redshifts.
dc.format
application/pdf
dc.language.iso
eng
dc.publisher
American Astronomical Society
dc.rights
info:eu-repo/semantics/openAccess
dc.rights.uri
https://creativecommons.org/licenses/by-nc-sa/2.5/ar/
dc.subject
Galaxies Evolution
dc.subject
Galaxies High-Redshift
dc.subject
Galaxies Starburst
dc.subject
Infrared Galaxies
dc.subject.classification
Astronomía
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dc.subject.classification
Ciencias Físicas
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dc.subject.classification
CIENCIAS NATURALES Y EXACTAS
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dc.title
Characterizing the Mid-infrared Extragalactic Sky with WISE and SDSS
dc.type
info:eu-repo/semantics/article
dc.type
info:ar-repo/semantics/artículo
dc.type
info:eu-repo/semantics/publishedVersion
dc.date.updated
2016-03-30 10:35:44.97925-03
dc.journal.volume
145
dc.journal.number
5
dc.journal.pagination
1-16
dc.journal.pais
Estados Unidos
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dc.journal.ciudad
Washington
dc.conicet.avisoEditorial
©2013. The American Astronomical Society. All rights reserved.
dc.description.fil
Fil: Yan, L.. California Institute of Technology. Infrared Processing and Analysis Center; Estados Unidos;
dc.description.fil
Fil: Donoso, Emilio. California Institute of Technology. Infrared Processing and Analysis Center; Estados Unidos; . Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Cientifico Tecnológico - CONICET - San Juan. Instituto de Ciencias Astronómicas de la Tierra y del Espacio; Argentina
dc.description.fil
Fil: Tsai, Chao Wei. California Institute of Technology. Infrared Processing and Analysis Center; Estados Unidos;
dc.description.fil
Fil: Stern, D.. California Institute of Technology. Jet Propulsion Laboratory; Estados Unidos;
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Fil: Assef, R. J.. California Institute of Technology. Jet Propulsion Laboratory; Estados Unidos;
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Fil: Eisenhardt, P.. California Institute of Technology. Jet Propulsion Laboratory; Estados Unidos;
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Fil: Blain, A. W.. University of Leicester. Department of Physics & Astronomy; Reino Unido;
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Fil: Cutri, R.. California Institute of Technology. Infrared Processing and Analysis Center; Estados Unidos;
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Fil: Jarrett, T. H.. California Institute of Technology. Infrared Processing and Analysis Center; Estados Unidos;
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Fil: Stanford, S. A.. University of California. Department of Physics; Estados Unidos;
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Fil: Wright, E.. University of California. Astronomy Department; Estados Unidos;
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Fil: Bridge, C.. California Institute of Technology. Astronomy Department; Estados Unidos;
dc.description.fil
Fil: Riechers, D. A.. California Institute of Technology. Astronomy Department; Estados Unidos; . Cornell University. Astronomy Department; Estados Unidos;
dc.journal.title
Astronomical Journal
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dc.relation.alternativeid
info:eu-repo/semantics/altIdentifier/url/http://iopscience.iop.org/1538-3881/145/3/55/pdf/1538-3881_145_3_55.pdf
dc.relation.alternativeid
info:eu-repo/semantics/altIdentifier/doi/http://dx.doi.org/10.1088/0004-6256/145/3/55
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