Characterizing the Mid-infrared Extragalactic Sky with WISE and SDSS

Autores
Yan, L.; Donoso, Emilio; Tsai, Chao Wei; Stern, D.; Assef, R. J.; Eisenhardt, P.; Blain, A. W.; Cutri, R.; Jarrett, T. H.; Stanford, S. A.; Wright, E.; Bridge, C.; Riechers, D. A.
Año de publicación
2013
Idioma
inglés
Tipo de recurso
artículo
Estado
versión publicada
Descripción
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.
Fil: Yan, L.. California Institute of Technology. Infrared Processing and Analysis Center; Estados Unidos;
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
Fil: Tsai, Chao Wei. California Institute of Technology. Infrared Processing and Analysis Center; Estados Unidos;
Fil: Stern, D.. California Institute of Technology. Jet Propulsion Laboratory; Estados Unidos;
Fil: Assef, R. J.. California Institute of Technology. Jet Propulsion Laboratory; Estados Unidos;
Fil: Eisenhardt, P.. California Institute of Technology. Jet Propulsion Laboratory; Estados Unidos;
Fil: Blain, A. W.. University of Leicester. Department of Physics & Astronomy; Reino Unido;
Fil: Cutri, R.. California Institute of Technology. Infrared Processing and Analysis Center; Estados Unidos;
Fil: Jarrett, T. H.. California Institute of Technology. Infrared Processing and Analysis Center; Estados Unidos;
Fil: Stanford, S. A.. University of California. Department of Physics; Estados Unidos;
Fil: Wright, E.. University of California. Astronomy Department; Estados Unidos;
Fil: Bridge, C.. California Institute of Technology. Astronomy Department; Estados Unidos;
Fil: Riechers, D. A.. California Institute of Technology. Astronomy Department; Estados Unidos; . Cornell University. Astronomy Department; Estados Unidos;
Materia
Galaxies Evolution
Galaxies High-Redshift
Galaxies Starburst
Infrared Galaxies
Nivel de accesibilidad
acceso abierto
Condiciones de uso
https://creativecommons.org/licenses/by-nc-sa/2.5/ar/
Repositorio
CONICET Digital (CONICET)
Institución
Consejo Nacional de Investigaciones Científicas y Técnicas
OAI Identificador
oai:ri.conicet.gov.ar:11336/1643

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oai_identifier_str oai:ri.conicet.gov.ar:11336/1643
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repository_id_str 3498
network_name_str CONICET Digital (CONICET)
spelling Characterizing the Mid-infrared Extragalactic Sky with WISE and SDSSYan, L.Donoso, EmilioTsai, Chao WeiStern, D.Assef, R. J.Eisenhardt, P.Blain, A. W.Cutri, R.Jarrett, T. H.Stanford, S. A.Wright, E.Bridge, C.Riechers, D. A.Galaxies EvolutionGalaxies High-RedshiftGalaxies StarburstInfrared Galaxieshttps://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1The 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.Fil: Yan, L.. California Institute of Technology. Infrared Processing and Analysis Center; Estados Unidos;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; ArgentinaFil: Tsai, Chao Wei. California Institute of Technology. Infrared Processing and Analysis Center; Estados Unidos;Fil: Stern, D.. California Institute of Technology. Jet Propulsion Laboratory; Estados Unidos;Fil: Assef, R. J.. California Institute of Technology. Jet Propulsion Laboratory; Estados Unidos;Fil: Eisenhardt, P.. California Institute of Technology. Jet Propulsion Laboratory; Estados Unidos;Fil: Blain, A. W.. University of Leicester. Department of Physics & Astronomy; Reino Unido;Fil: Cutri, R.. California Institute of Technology. Infrared Processing and Analysis Center; Estados Unidos;Fil: Jarrett, T. H.. California Institute of Technology. Infrared Processing and Analysis Center; Estados Unidos;Fil: Stanford, S. A.. University of California. Department of Physics; Estados Unidos;Fil: Wright, E.. University of California. Astronomy Department; Estados Unidos;Fil: Bridge, C.. California Institute of Technology. Astronomy Department; Estados Unidos;Fil: Riechers, D. A.. California Institute of Technology. Astronomy Department; Estados Unidos; . Cornell University. Astronomy Department; Estados Unidos;American Astronomical Society2013-03-18info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/1643Yan, 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; 1-160004-6256enginfo:eu-repo/semantics/altIdentifier/url/http://iopscience.iop.org/1538-3881/145/3/55/pdf/1538-3881_145_3_55.pdfinfo:eu-repo/semantics/altIdentifier/doi/10.1088/0004-6256/145/3/55info:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by-nc-sa/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2025-09-29T09:42:56Zoai:ri.conicet.gov.ar:11336/1643instacron:CONICETInstitucionalhttp://ri.conicet.gov.ar/Organismo científico-tecnológicoNo correspondehttp://ri.conicet.gov.ar/oai/requestdasensio@conicet.gov.ar; lcarlino@conicet.gov.arArgentinaNo correspondeNo correspondeNo correspondeopendoar:34982025-09-29 09:42:56.31CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse
dc.title.none.fl_str_mv Characterizing the Mid-infrared Extragalactic Sky with WISE and SDSS
title Characterizing the Mid-infrared Extragalactic Sky with WISE and SDSS
spellingShingle Characterizing the Mid-infrared Extragalactic Sky with WISE and SDSS
Yan, L.
Galaxies Evolution
Galaxies High-Redshift
Galaxies Starburst
Infrared Galaxies
title_short Characterizing the Mid-infrared Extragalactic Sky with WISE and SDSS
title_full Characterizing the Mid-infrared Extragalactic Sky with WISE and SDSS
title_fullStr Characterizing the Mid-infrared Extragalactic Sky with WISE and SDSS
title_full_unstemmed Characterizing the Mid-infrared Extragalactic Sky with WISE and SDSS
title_sort Characterizing the Mid-infrared Extragalactic Sky with WISE and SDSS
dc.creator.none.fl_str_mv Yan, L.
Donoso, Emilio
Tsai, Chao Wei
Stern, D.
Assef, R. J.
Eisenhardt, P.
Blain, A. W.
Cutri, R.
Jarrett, T. H.
Stanford, S. A.
Wright, E.
Bridge, C.
Riechers, D. A.
author Yan, L.
author_facet Yan, L.
Donoso, Emilio
Tsai, Chao Wei
Stern, D.
Assef, R. J.
Eisenhardt, P.
Blain, A. W.
Cutri, R.
Jarrett, T. H.
Stanford, S. A.
Wright, E.
Bridge, C.
Riechers, D. A.
author_role author
author2 Donoso, Emilio
Tsai, Chao Wei
Stern, D.
Assef, R. J.
Eisenhardt, P.
Blain, A. W.
Cutri, R.
Jarrett, T. H.
Stanford, S. A.
Wright, E.
Bridge, C.
Riechers, D. A.
author2_role author
author
author
author
author
author
author
author
author
author
author
author
dc.subject.none.fl_str_mv Galaxies Evolution
Galaxies High-Redshift
Galaxies Starburst
Infrared Galaxies
topic Galaxies Evolution
Galaxies High-Redshift
Galaxies Starburst
Infrared Galaxies
purl_subject.fl_str_mv https://purl.org/becyt/ford/1.3
https://purl.org/becyt/ford/1
dc.description.none.fl_txt_mv 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.
Fil: Yan, L.. California Institute of Technology. Infrared Processing and Analysis Center; Estados Unidos;
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
Fil: Tsai, Chao Wei. California Institute of Technology. Infrared Processing and Analysis Center; Estados Unidos;
Fil: Stern, D.. California Institute of Technology. Jet Propulsion Laboratory; Estados Unidos;
Fil: Assef, R. J.. California Institute of Technology. Jet Propulsion Laboratory; Estados Unidos;
Fil: Eisenhardt, P.. California Institute of Technology. Jet Propulsion Laboratory; Estados Unidos;
Fil: Blain, A. W.. University of Leicester. Department of Physics & Astronomy; Reino Unido;
Fil: Cutri, R.. California Institute of Technology. Infrared Processing and Analysis Center; Estados Unidos;
Fil: Jarrett, T. H.. California Institute of Technology. Infrared Processing and Analysis Center; Estados Unidos;
Fil: Stanford, S. A.. University of California. Department of Physics; Estados Unidos;
Fil: Wright, E.. University of California. Astronomy Department; Estados Unidos;
Fil: Bridge, C.. California Institute of Technology. Astronomy Department; Estados Unidos;
Fil: Riechers, D. A.. California Institute of Technology. Astronomy Department; Estados Unidos; . Cornell University. Astronomy Department; Estados Unidos;
description 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.
publishDate 2013
dc.date.none.fl_str_mv 2013-03-18
dc.type.none.fl_str_mv info:eu-repo/semantics/article
info:eu-repo/semantics/publishedVersion
http://purl.org/coar/resource_type/c_6501
info:ar-repo/semantics/articulo
format article
status_str publishedVersion
dc.identifier.none.fl_str_mv http://hdl.handle.net/11336/1643
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
0004-6256
url http://hdl.handle.net/11336/1643
identifier_str_mv 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
0004-6256
dc.language.none.fl_str_mv eng
language eng
dc.relation.none.fl_str_mv info:eu-repo/semantics/altIdentifier/url/http://iopscience.iop.org/1538-3881/145/3/55/pdf/1538-3881_145_3_55.pdf
info:eu-repo/semantics/altIdentifier/doi/10.1088/0004-6256/145/3/55
dc.rights.none.fl_str_mv info:eu-repo/semantics/openAccess
https://creativecommons.org/licenses/by-nc-sa/2.5/ar/
eu_rights_str_mv openAccess
rights_invalid_str_mv https://creativecommons.org/licenses/by-nc-sa/2.5/ar/
dc.format.none.fl_str_mv application/pdf
application/pdf
dc.publisher.none.fl_str_mv American Astronomical Society
publisher.none.fl_str_mv American Astronomical Society
dc.source.none.fl_str_mv reponame:CONICET Digital (CONICET)
instname:Consejo Nacional de Investigaciones Científicas y Técnicas
reponame_str CONICET Digital (CONICET)
collection CONICET Digital (CONICET)
instname_str Consejo Nacional de Investigaciones Científicas y Técnicas
repository.name.fl_str_mv CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicas
repository.mail.fl_str_mv dasensio@conicet.gov.ar; lcarlino@conicet.gov.ar
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