K_(s) number counts in the Groth and Coppi fields
We have used William Herschel Telescope/INGRID K_(s) images on two high-latitude fields, the Coppi and Groth strips, to obtain galaxy number counts over similar to 180 arcmin^(2), to a depth of K_(s) similar to 21.0. Detection efficiency corrections as a function of object size have been calculated...
| Autores: | , , , , , , , |
|---|---|
| Tipo de recurso: | artículo |
| Fecha de publicación: | 2003 |
| País: | España |
| Institución: | Universidad Complutense de Madrid (UCM) |
| Repositorio: | Docta Complutense |
| Idioma: | inglés |
| OAI Identifier: | oai:docta.ucm.es:20.500.14352/51339 |
| Acceso en línea: | https://hdl.handle.net/20.500.14352/51339 |
| Access Level: | acceso abierto |
| Palabra clave: | 52 Hubble deep field Band galaxy counts Faint galaxies Compact galaxies Evolution Luminosity Colors Telescope Redshift Star Astrofísica Astronomía (Física) Física atmosférica 2501 Ciencias de la Atmósfera |
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K_(s) number counts in the Groth and Coppi fieldsCristobal Hornillos, DavidBalcells, MarcPrieto, MercedesGuzmán, RafaelGallego Maestro, JesúsCardiel López, NicolásSerrano Laguna, ÁngelPello, Roser52Hubble deep fieldBand galaxy countsFaint galaxiesCompact galaxiesEvolutionLuminosityColorsTelescopeRedshiftStarAstrofísicaAstronomía (Física)Física atmosférica2501 Ciencias de la AtmósferaWe have used William Herschel Telescope/INGRID K_(s) images on two high-latitude fields, the Coppi and Groth strips, to obtain galaxy number counts over similar to 180 arcmin^(2), to a depth of K_(s) similar to 21.0. Detection efficiency corrections as a function of object size have been calculated on each pointing. We have used a signal-to-noise threshold in two complementary half-exposure images to remove spurious detections. Our data cover the range from K_(s) = 14.5 to K_(s) = 21.0, so they are useful for investigating a previously reported change in the number count slope (d log N/dm) at K similar to 17. We find a slope gamma(b) = 0.54 0.63 for K < 17.5 and a slope γ(f) = 0.25 0.29 for K > 17.5. A total contribution from galaxies to the extragalactic background light (EBL) in the K band of nuI(nu) = 10.5 nW m^(-2) sr^(-1) has been calculated. This K-band EBL coming from galaxies accounts for only similar to 50% of the recent measurements of the diffuse EBL. Standard number count models fail to reproduce the observed slope change at K similar to 17.5 unless elliptical and spiral formation is pushed to z less than or similar to 2.IOP PublishingUniversidad Complutense de Madrid20032003-09-2020032003-09-20journal articlehttp://purl.org/coar/resource_type/c_6501info:eu-repo/semantics/articleapplication/pdfhttps://hdl.handle.net/20.500.14352/51339reponame:Docta Complutenseinstname:Universidad Complutense de Madrid (UCM)Inglésengopen accesshttp://purl.org/coar/access_right/c_abf2info:eu-repo/semantics/openAccessoai:docta.ucm.es:20.500.14352/513392026-06-02T12:44:21Z |
| dc.title.none.fl_str_mv |
K_(s) number counts in the Groth and Coppi fields |
| title |
K_(s) number counts in the Groth and Coppi fields |
| spellingShingle |
K_(s) number counts in the Groth and Coppi fields Cristobal Hornillos, David 52 Hubble deep field Band galaxy counts Faint galaxies Compact galaxies Evolution Luminosity Colors Telescope Redshift Star Astrofísica Astronomía (Física) Física atmosférica 2501 Ciencias de la Atmósfera |
| title_short |
K_(s) number counts in the Groth and Coppi fields |
| title_full |
K_(s) number counts in the Groth and Coppi fields |
| title_fullStr |
K_(s) number counts in the Groth and Coppi fields |
| title_full_unstemmed |
K_(s) number counts in the Groth and Coppi fields |
| title_sort |
K_(s) number counts in the Groth and Coppi fields |
| dc.creator.none.fl_str_mv |
Cristobal Hornillos, David Balcells, Marc Prieto, Mercedes Guzmán, Rafael Gallego Maestro, Jesús Cardiel López, Nicolás Serrano Laguna, Ángel Pello, Roser |
| author |
Cristobal Hornillos, David |
| author_facet |
Cristobal Hornillos, David Balcells, Marc Prieto, Mercedes Guzmán, Rafael Gallego Maestro, Jesús Cardiel López, Nicolás Serrano Laguna, Ángel Pello, Roser |
| author_role |
author |
| author2 |
Balcells, Marc Prieto, Mercedes Guzmán, Rafael Gallego Maestro, Jesús Cardiel López, Nicolás Serrano Laguna, Ángel Pello, Roser |
| author2_role |
author author author author author author author |
| dc.contributor.none.fl_str_mv |
Universidad Complutense de Madrid |
| dc.subject.none.fl_str_mv |
52 Hubble deep field Band galaxy counts Faint galaxies Compact galaxies Evolution Luminosity Colors Telescope Redshift Star Astrofísica Astronomía (Física) Física atmosférica 2501 Ciencias de la Atmósfera |
| topic |
52 Hubble deep field Band galaxy counts Faint galaxies Compact galaxies Evolution Luminosity Colors Telescope Redshift Star Astrofísica Astronomía (Física) Física atmosférica 2501 Ciencias de la Atmósfera |
| description |
We have used William Herschel Telescope/INGRID K_(s) images on two high-latitude fields, the Coppi and Groth strips, to obtain galaxy number counts over similar to 180 arcmin^(2), to a depth of K_(s) similar to 21.0. Detection efficiency corrections as a function of object size have been calculated on each pointing. We have used a signal-to-noise threshold in two complementary half-exposure images to remove spurious detections. Our data cover the range from K_(s) = 14.5 to K_(s) = 21.0, so they are useful for investigating a previously reported change in the number count slope (d log N/dm) at K similar to 17. We find a slope gamma(b) = 0.54 0.63 for K < 17.5 and a slope γ(f) = 0.25 0.29 for K > 17.5. A total contribution from galaxies to the extragalactic background light (EBL) in the K band of nuI(nu) = 10.5 nW m^(-2) sr^(-1) has been calculated. This K-band EBL coming from galaxies accounts for only similar to 50% of the recent measurements of the diffuse EBL. Standard number count models fail to reproduce the observed slope change at K similar to 17.5 unless elliptical and spiral formation is pushed to z less than or similar to 2. |
| publishDate |
2003 |
| dc.date.none.fl_str_mv |
2003 2003-09-20 2003 2003-09-20 |
| dc.type.none.fl_str_mv |
journal article http://purl.org/coar/resource_type/c_6501 |
| dc.type.openaire.fl_str_mv |
info:eu-repo/semantics/article |
| format |
article |
| dc.identifier.none.fl_str_mv |
https://hdl.handle.net/20.500.14352/51339 |
| url |
https://hdl.handle.net/20.500.14352/51339 |
| dc.language.none.fl_str_mv |
Inglés eng |
| language_invalid_str_mv |
Inglés |
| language |
eng |
| dc.rights.none.fl_str_mv |
open access http://purl.org/coar/access_right/c_abf2 |
| dc.rights.openaire.fl_str_mv |
info:eu-repo/semantics/openAccess |
| rights_invalid_str_mv |
open access http://purl.org/coar/access_right/c_abf2 |
| eu_rights_str_mv |
openAccess |
| dc.format.none.fl_str_mv |
application/pdf |
| dc.publisher.none.fl_str_mv |
IOP Publishing |
| publisher.none.fl_str_mv |
IOP Publishing |
| dc.source.none.fl_str_mv |
reponame:Docta Complutense instname:Universidad Complutense de Madrid (UCM) |
| instname_str |
Universidad Complutense de Madrid (UCM) |
| reponame_str |
Docta Complutense |
| collection |
Docta Complutense |
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|
| repository.mail.fl_str_mv |
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1869408941166821376 |
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15,300719 |