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
- Institución
- Consejo Nacional de Investigaciones Científicas y Técnicas
- OAI Identificador
- oai:ri.conicet.gov.ar:11336/1643
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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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1844613351100907520 |
score |
13.070432 |