X-ray emission from the microquasar S26 observed by XMM-Newton

Autores
Rizzo, F. N.; Sotomayor Checa, Pablo Omar; Romero, Gustavo Esteban
Año de publicación
2021
Idioma
inglés
Tipo de recurso
documento de conferencia
Estado
versión publicada
Descripción
S26 is the microquasar with the most powerful jets observed in accreting stellar sources. The estimatedkinetic power for its jets is of the order of the bolometric luminosity of some ultraluminous X-ray sources. If thispower is coupled to the matter accretion onto the compact object, then S26 must be a super-accreting binary,similar to the galactic microquasar SS433. Nevertheless, data from Chandra X-ray Observatory seems to implythat the central X-ray luminosity is four orders of magnitude lower than the kinetic power of the jets, and belowthe Eddington limit for a stellar-mass black hole. Motivated to understand the origin of this discrepancy, weanalyze X-ray observations of S26 using data collected by the XMM-Newton space telescope. In this work wepresent an image and the spectrum of the source. Our results are consistent with those previously reported withChandra satellite observations regarding length of the source, orientation, spectral index, plasma temperature,and the X-ray flux in the 0.4-4 keV range, confirming the puzzling nature of the object.
Fil: Rizzo, F. N.. Universidad Nacional de la Plata. Facultad de Cs.astronómicas y Geofísicas. Departamento de Ciencias Exactas; Argentina
Fil: Sotomayor Checa, Pablo Omar. Provincia de Buenos Aires. Gobernación. Comisión de Investigaciones Científicas. Instituto Argentino de Radioastronomía. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto Argentino de Radioastronomía; Argentina. Universidad Nacional de la Plata. Facultad de Cs.astronómicas y Geofísicas. Departamento de Ciencias Exactas; Argentina
Fil: Romero, Gustavo Esteban. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas; Argentina. Provincia de Buenos Aires. Gobernación. Comisión de Investigaciones Científicas. Instituto Argentino de Radioastronomía. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto Argentino de Radioastronomía; Argentina
Reunion Anual de la Asociación Argentina de Astronomía
Córdoba
Argentina
Universidad Nacional de Córdoba
Materia
ISM: jets and outflows
X-rays: binaries
galaxies: individual (NGC 7793)
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:11336/218296
Acceder
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network_acronym_str CONICETDig
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network_name_str CONICET Digital (CONICET)
spelling X-ray emission from the microquasar S26 observed by XMM-NewtonRizzo, F. N.Sotomayor Checa, Pablo OmarRomero, Gustavo EstebanISM: jets and outflowsX-rays: binariesgalaxies: individual (NGC 7793)https://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1S26 is the microquasar with the most powerful jets observed in accreting stellar sources. The estimatedkinetic power for its jets is of the order of the bolometric luminosity of some ultraluminous X-ray sources. If thispower is coupled to the matter accretion onto the compact object, then S26 must be a super-accreting binary,similar to the galactic microquasar SS433. Nevertheless, data from Chandra X-ray Observatory seems to implythat the central X-ray luminosity is four orders of magnitude lower than the kinetic power of the jets, and belowthe Eddington limit for a stellar-mass black hole. Motivated to understand the origin of this discrepancy, weanalyze X-ray observations of S26 using data collected by the XMM-Newton space telescope. In this work wepresent an image and the spectrum of the source. Our results are consistent with those previously reported withChandra satellite observations regarding length of the source, orientation, spectral index, plasma temperature,and the X-ray flux in the 0.4-4 keV range, confirming the puzzling nature of the object.Fil: Rizzo, F. N.. Universidad Nacional de la Plata. Facultad de Cs.astronómicas y Geofísicas. Departamento de Ciencias Exactas; ArgentinaFil: Sotomayor Checa, Pablo Omar. Provincia de Buenos Aires. Gobernación. Comisión de Investigaciones Científicas. Instituto Argentino de Radioastronomía. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto Argentino de Radioastronomía; Argentina. Universidad Nacional de la Plata. Facultad de Cs.astronómicas y Geofísicas. Departamento de Ciencias Exactas; ArgentinaFil: Romero, Gustavo Esteban. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas; Argentina. Provincia de Buenos Aires. Gobernación. Comisión de Investigaciones Científicas. Instituto Argentino de Radioastronomía. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto Argentino de Radioastronomía; ArgentinaReunion Anual de la Asociación Argentina de AstronomíaCórdobaArgentinaUniversidad Nacional de CórdobaAsociación Argentina de Astronomía.Rohrmann, Rene DanielGomez, Mercedes NievesBoeris, Claudia EvelinaSgró, Mario Agustín2021info:eu-repo/semantics/publishedVersioninfo:eu-repo/semantics/conferenceObjectCongresoJournalhttp://purl.org/coar/resource_type/c_5794info:ar-repo/semantics/documentoDeConferenciaapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/218296X-ray emission from the microquasar S26 observed by XMM-Newton; Reunion Anual de la Asociación Argentina de Astronomía; Córdoba; Argentina; 2021; 283-2860571-32851669-9521CONICET DigitalCONICETenghttp://astronomiaargentina.fcaglp.unlp.edu.ar/uploads/docs/baaa63.pdfinfo:eu-repo/semantics/altIdentifier/url/http://www.astronomiaargentina.org.ar/b63/2022BAAA...63..283R.pdfinfo:eu-repo/semantics/altIdentifier/url/https://ui.adsabs.harvard.edu/abs/2022BAAA...63..283R/abstractNacionalinfo:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by-nc-sa/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2025-09-29T09:55:03Zoai:ri.conicet.gov.ar:11336/218296instacron: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 09:55:04.222CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse
dc.title.none.fl_str_mv X-ray emission from the microquasar S26 observed by XMM-Newton
title X-ray emission from the microquasar S26 observed by XMM-Newton
spellingShingle X-ray emission from the microquasar S26 observed by XMM-Newton
Rizzo, F. N.
ISM: jets and outflows
X-rays: binaries
galaxies: individual (NGC 7793)
title_short X-ray emission from the microquasar S26 observed by XMM-Newton
title_full X-ray emission from the microquasar S26 observed by XMM-Newton
title_fullStr X-ray emission from the microquasar S26 observed by XMM-Newton
title_full_unstemmed X-ray emission from the microquasar S26 observed by XMM-Newton
title_sort X-ray emission from the microquasar S26 observed by XMM-Newton
dc.creator.none.fl_str_mv Rizzo, F. N.
Sotomayor Checa, Pablo Omar
Romero, Gustavo Esteban
author Rizzo, F. N.
author_facet Rizzo, F. N.
Sotomayor Checa, Pablo Omar
Romero, Gustavo Esteban
author_role author
author2 Sotomayor Checa, Pablo Omar
Romero, Gustavo Esteban
author2_role author
author
dc.contributor.none.fl_str_mv Rohrmann, Rene Daniel
Gomez, Mercedes Nieves
Boeris, Claudia Evelina
Sgró, Mario Agustín
dc.subject.none.fl_str_mv ISM: jets and outflows
X-rays: binaries
galaxies: individual (NGC 7793)
topic ISM: jets and outflows
X-rays: binaries
galaxies: individual (NGC 7793)
purl_subject.fl_str_mv https://purl.org/becyt/ford/1.3
https://purl.org/becyt/ford/1
dc.description.none.fl_txt_mv S26 is the microquasar with the most powerful jets observed in accreting stellar sources. The estimatedkinetic power for its jets is of the order of the bolometric luminosity of some ultraluminous X-ray sources. If thispower is coupled to the matter accretion onto the compact object, then S26 must be a super-accreting binary,similar to the galactic microquasar SS433. Nevertheless, data from Chandra X-ray Observatory seems to implythat the central X-ray luminosity is four orders of magnitude lower than the kinetic power of the jets, and belowthe Eddington limit for a stellar-mass black hole. Motivated to understand the origin of this discrepancy, weanalyze X-ray observations of S26 using data collected by the XMM-Newton space telescope. In this work wepresent an image and the spectrum of the source. Our results are consistent with those previously reported withChandra satellite observations regarding length of the source, orientation, spectral index, plasma temperature,and the X-ray flux in the 0.4-4 keV range, confirming the puzzling nature of the object.
Fil: Rizzo, F. N.. Universidad Nacional de la Plata. Facultad de Cs.astronómicas y Geofísicas. Departamento de Ciencias Exactas; Argentina
Fil: Sotomayor Checa, Pablo Omar. Provincia de Buenos Aires. Gobernación. Comisión de Investigaciones Científicas. Instituto Argentino de Radioastronomía. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto Argentino de Radioastronomía; Argentina. Universidad Nacional de la Plata. Facultad de Cs.astronómicas y Geofísicas. Departamento de Ciencias Exactas; Argentina
Fil: Romero, Gustavo Esteban. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas; Argentina. Provincia de Buenos Aires. Gobernación. Comisión de Investigaciones Científicas. Instituto Argentino de Radioastronomía. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto Argentino de Radioastronomía; Argentina
Reunion Anual de la Asociación Argentina de Astronomía
Córdoba
Argentina
Universidad Nacional de Córdoba
description S26 is the microquasar with the most powerful jets observed in accreting stellar sources. The estimatedkinetic power for its jets is of the order of the bolometric luminosity of some ultraluminous X-ray sources. If thispower is coupled to the matter accretion onto the compact object, then S26 must be a super-accreting binary,similar to the galactic microquasar SS433. Nevertheless, data from Chandra X-ray Observatory seems to implythat the central X-ray luminosity is four orders of magnitude lower than the kinetic power of the jets, and belowthe Eddington limit for a stellar-mass black hole. Motivated to understand the origin of this discrepancy, weanalyze X-ray observations of S26 using data collected by the XMM-Newton space telescope. In this work wepresent an image and the spectrum of the source. Our results are consistent with those previously reported withChandra satellite observations regarding length of the source, orientation, spectral index, plasma temperature,and the X-ray flux in the 0.4-4 keV range, confirming the puzzling nature of the object.
publishDate 2021
dc.date.none.fl_str_mv 2021
dc.type.none.fl_str_mv info:eu-repo/semantics/publishedVersion
info:eu-repo/semantics/conferenceObject
Congreso
Journal
http://purl.org/coar/resource_type/c_5794
info:ar-repo/semantics/documentoDeConferencia
status_str publishedVersion
format conferenceObject
dc.identifier.none.fl_str_mv http://hdl.handle.net/11336/218296
X-ray emission from the microquasar S26 observed by XMM-Newton; Reunion Anual de la Asociación Argentina de Astronomía; Córdoba; Argentina; 2021; 283-286
0571-3285
1669-9521
CONICET Digital
CONICET
url http://hdl.handle.net/11336/218296
identifier_str_mv X-ray emission from the microquasar S26 observed by XMM-Newton; Reunion Anual de la Asociación Argentina de Astronomía; Córdoba; Argentina; 2021; 283-286
0571-3285
1669-9521
CONICET Digital
CONICET
dc.language.none.fl_str_mv eng
language eng
dc.relation.none.fl_str_mv http://astronomiaargentina.fcaglp.unlp.edu.ar/uploads/docs/baaa63.pdf
info:eu-repo/semantics/altIdentifier/url/http://www.astronomiaargentina.org.ar/b63/2022BAAA...63..283R.pdf
info:eu-repo/semantics/altIdentifier/url/https://ui.adsabs.harvard.edu/abs/2022BAAA...63..283R/abstract
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.coverage.none.fl_str_mv Nacional
dc.publisher.none.fl_str_mv Asociación Argentina de Astronomía.
publisher.none.fl_str_mv Asociación Argentina de Astronomía.
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 13.070432

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