Cosmic Microwave background bispectrum from Active Models of Structure Formation

Autores
Gangui, Alejandro; Pogosian, Levon; Winitzki, Serge
Año de publicación
2001
Idioma
inglés
Tipo de recurso
artículo
Estado
versión publicada
Descripción
We propose a method for a numerical computation of the angular bispectrum of the cosmic microwave background (CMB) anisotropies arising from active models such as cosmic topological defects, using a modified Boltzmann code based on CMBFAST. The method does not use CMB sky maps and requires moderate computational power. As a first implementation, we apply our method to a recently proposed model of simulated cosmic strings and estimate the observability of the non-Gaussian bispectrum signal. A comparison with the cosmic variance of the bispectrum estimator shows that the bispectrum for the simulated string model we used is not observable.
Fil: Gangui, Alejandro. Consejo Nacional de Investigaciónes Científicas y Técnicas. Oficina de Coordinación Administrativa Ciudad Universitaria. Instituto de Astronomía y Física del Espacio. - Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales. Instituto de Astronomía y Física del Espacio; Argentina
Fil: Pogosian, Levon. Case Western Reserve University; Estados Unidos
Fil: Winitzki, Serge. Case Western Reserve University; Estados Unidos
Materia
Cosmic Microwave
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:11336/22483
Acceder
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network_name_str CONICET Digital (CONICET)
spelling Cosmic Microwave background bispectrum from Active Models of Structure FormationGangui, AlejandroPogosian, LevonWinitzki, SergeCosmic Microwavehttps://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1We propose a method for a numerical computation of the angular bispectrum of the cosmic microwave background (CMB) anisotropies arising from active models such as cosmic topological defects, using a modified Boltzmann code based on CMBFAST. The method does not use CMB sky maps and requires moderate computational power. As a first implementation, we apply our method to a recently proposed model of simulated cosmic strings and estimate the observability of the non-Gaussian bispectrum signal. A comparison with the cosmic variance of the bispectrum estimator shows that the bispectrum for the simulated string model we used is not observable.Fil: Gangui, Alejandro. Consejo Nacional de Investigaciónes Científicas y Técnicas. Oficina de Coordinación Administrativa Ciudad Universitaria. Instituto de Astronomía y Física del Espacio. - Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales. Instituto de Astronomía y Física del Espacio; ArgentinaFil: Pogosian, Levon. Case Western Reserve University; Estados UnidosFil: Winitzki, Serge. Case Western Reserve University; Estados UnidosAmerican Physical Society2001-12info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/22483Gangui, Alejandro; Pogosian, Levon; Winitzki, Serge; Cosmic Microwave background bispectrum from Active Models of Structure Formation; American Physical Society; Physical Review D; 64; 4; 12-2001; 1-7; 0430010556-2821CONICET DigitalCONICETenginfo:eu-repo/semantics/altIdentifier/doi/10.1103/PhysRevD.64.043001info:eu-repo/semantics/altIdentifier/url/https://journals.aps.org/prd/abstract/10.1103/PhysRevD.64.043001info:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by-nc-sa/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2025-09-03T10:03:49Zoai:ri.conicet.gov.ar:11336/22483instacron: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:34982025-09-03 10:03:50.203CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse
dc.title.none.fl_str_mv Cosmic Microwave background bispectrum from Active Models of Structure Formation
title Cosmic Microwave background bispectrum from Active Models of Structure Formation
spellingShingle Cosmic Microwave background bispectrum from Active Models of Structure Formation
Gangui, Alejandro
Cosmic Microwave
title_short Cosmic Microwave background bispectrum from Active Models of Structure Formation
title_full Cosmic Microwave background bispectrum from Active Models of Structure Formation
title_fullStr Cosmic Microwave background bispectrum from Active Models of Structure Formation
title_full_unstemmed Cosmic Microwave background bispectrum from Active Models of Structure Formation
title_sort Cosmic Microwave background bispectrum from Active Models of Structure Formation
dc.creator.none.fl_str_mv Gangui, Alejandro
Pogosian, Levon
Winitzki, Serge
author Gangui, Alejandro
author_facet Gangui, Alejandro
Pogosian, Levon
Winitzki, Serge
author_role author
author2 Pogosian, Levon
Winitzki, Serge
author2_role author
author
dc.subject.none.fl_str_mv Cosmic Microwave
topic Cosmic Microwave
purl_subject.fl_str_mv https://purl.org/becyt/ford/1.3
https://purl.org/becyt/ford/1
dc.description.none.fl_txt_mv We propose a method for a numerical computation of the angular bispectrum of the cosmic microwave background (CMB) anisotropies arising from active models such as cosmic topological defects, using a modified Boltzmann code based on CMBFAST. The method does not use CMB sky maps and requires moderate computational power. As a first implementation, we apply our method to a recently proposed model of simulated cosmic strings and estimate the observability of the non-Gaussian bispectrum signal. A comparison with the cosmic variance of the bispectrum estimator shows that the bispectrum for the simulated string model we used is not observable.
Fil: Gangui, Alejandro. Consejo Nacional de Investigaciónes Científicas y Técnicas. Oficina de Coordinación Administrativa Ciudad Universitaria. Instituto de Astronomía y Física del Espacio. - Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales. Instituto de Astronomía y Física del Espacio; Argentina
Fil: Pogosian, Levon. Case Western Reserve University; Estados Unidos
Fil: Winitzki, Serge. Case Western Reserve University; Estados Unidos
description We propose a method for a numerical computation of the angular bispectrum of the cosmic microwave background (CMB) anisotropies arising from active models such as cosmic topological defects, using a modified Boltzmann code based on CMBFAST. The method does not use CMB sky maps and requires moderate computational power. As a first implementation, we apply our method to a recently proposed model of simulated cosmic strings and estimate the observability of the non-Gaussian bispectrum signal. A comparison with the cosmic variance of the bispectrum estimator shows that the bispectrum for the simulated string model we used is not observable.
publishDate 2001
dc.date.none.fl_str_mv 2001-12
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/11336/22483
Gangui, Alejandro; Pogosian, Levon; Winitzki, Serge; Cosmic Microwave background bispectrum from Active Models of Structure Formation; American Physical Society; Physical Review D; 64; 4; 12-2001; 1-7; 043001
0556-2821
CONICET Digital
CONICET
url http://hdl.handle.net/11336/22483
identifier_str_mv Gangui, Alejandro; Pogosian, Levon; Winitzki, Serge; Cosmic Microwave background bispectrum from Active Models of Structure Formation; American Physical Society; Physical Review D; 64; 4; 12-2001; 1-7; 043001
0556-2821
CONICET Digital
CONICET
dc.language.none.fl_str_mv eng
language eng
dc.relation.none.fl_str_mv info:eu-repo/semantics/altIdentifier/doi/10.1103/PhysRevD.64.043001
info:eu-repo/semantics/altIdentifier/url/https://journals.aps.org/prd/abstract/10.1103/PhysRevD.64.043001
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 Physical Society
publisher.none.fl_str_mv American Physical 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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score 13.13397

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