CXO J004318.8+412016*A steady supersoft X-ray source in M 31

Autores
Orio, Marina; Luna, Gerardo Juan Manuel; Kotulla, R.; Gallager, J. S.; Zampieri, L.; Mikolajewska, J.; Harbeck, D.; Bianchini, A.; Chiosi, E.; Della Valle, M.; de Martino, D.; Kaur, A.; Mapelli, M.; Munari, U.; Odendaal, A.; Trinchieri, G.; Wade, J.; Zemko, P.
Año de publicación
2017
Idioma
inglés
Tipo de recurso
artículo
Estado
versión publicada
Descripción
We obtained an optical spectrum of a star we identify as the optical counterpart of the M31 Chandra source CXO J004318.8+412016, because of prominent emission lines of the Balmer series, of neutral helium, and a He II line at 4686 Å. The continuum energy distribution and the spectral characteristics demonstrate the presence of a red giant of K or earlier spectral type, so we concluded that the binary is likely to be a symbiotic system. CXO J004318.8+412016 has been observed in X-rays as a luminous supersoft source (SSS) since 1979, with effective temperature exceeding 40 eV and variable X-ray luminosity, oscillating between a few times 1035 erg s-1 and a few times 1037 erg s-1 in the space of a few weeks. The optical, infrared and ultraviolet colours of the optical object are consistent with an an accretion disc around a compact object companion, which may be either a white dwarf or a black hole, depending on the system parameters. If the origin of the luminous supersoft X-rays is the atmosphere of a white dwarf that is burning hydrogen in shell, it is as hot and luminous as post-thermonuclear flash novae, yet no major optical outburst has ever been observed, suggesting that the white dwarf is very massive (m ≥ 1.2 M⊙) and it is accreting and burning at the high rate m > 10-8 M⊙ yr-1 expected for Type Ia supernovae progenitors. In this case, the X-ray variability may be due to a very short recurrence time of only mildly degenerate thermonuclear flashes.
Fil: Orio, Marina. Osservatorio Astronomico Di Padova; Italia. University of Wisconsin; Estados Unidos
Fil: Luna, Gerardo Juan Manuel. 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. Universidad de Buenos Aires; Argentina
Fil: Kotulla, R.. University of Wisconsin; Estados Unidos
Fil: Gallager, J. S.. University of Wisconsin; Estados Unidos
Fil: Zampieri, L.. Osservatorio Astronomico Di Padova; Italia
Fil: Mikolajewska, J.. Nicolaus Copernicus Astronomical Center Of The Polish Academy Of Sciences; Polonia
Fil: Harbeck, D.. Wiyn Observatory; Estados Unidos
Fil: Bianchini, A.. Università di Padova; Italia
Fil: Chiosi, E.. Università di Padova; Italia
Fil: Della Valle, M.. Osservatorio Astronomico Di Capodimonte; Italia
Fil: de Martino, D.. Osservatorio Astronomico Di Capodimonte; Italia
Fil: Kaur, A.. Clemson University; Estados Unidos
Fil: Mapelli, M.. Osservatorio di Padova; Italia
Fil: Munari, U.. Osservatorio di Padova; Italia
Fil: Odendaal, A.. University of the Free State; Sudáfrica
Fil: Trinchieri, G.. Osservatorio Astronomico di Brera; Italia
Fil: Wade, J.. University of Wisconsin; Estados Unidos
Fil: Zemko, P.. Università di Padova; Italia
Materia
BINARIES: SYMBIOTIC
GALAXIES: INDIVIDUAL: M31
WHITE DWARFS
X-RAYS: BINARIES
X-RAYS: INDIVIDUAL: CXO J004318.8+412016
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:11336/24574
Acceder
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oai_identifier_str oai:ri.conicet.gov.ar:11336/24574
network_acronym_str CONICETDig
repository_id_str 3498
network_name_str CONICET Digital (CONICET)
spelling CXO J004318.8+412016*A steady supersoft X-ray source in M 31Orio, MarinaLuna, Gerardo Juan ManuelKotulla, R.Gallager, J. S.Zampieri, L.Mikolajewska, J.Harbeck, D.Bianchini, A.Chiosi, E.Della Valle, M.de Martino, D.Kaur, A.Mapelli, M.Munari, U.Odendaal, A.Trinchieri, G.Wade, J.Zemko, P.BINARIES: SYMBIOTICGALAXIES: INDIVIDUAL: M31WHITE DWARFSX-RAYS: BINARIESX-RAYS: INDIVIDUAL: CXO J004318.8+412016https://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1We obtained an optical spectrum of a star we identify as the optical counterpart of the M31 Chandra source CXO J004318.8+412016, because of prominent emission lines of the Balmer series, of neutral helium, and a He II line at 4686 Å. The continuum energy distribution and the spectral characteristics demonstrate the presence of a red giant of K or earlier spectral type, so we concluded that the binary is likely to be a symbiotic system. CXO J004318.8+412016 has been observed in X-rays as a luminous supersoft source (SSS) since 1979, with effective temperature exceeding 40 eV and variable X-ray luminosity, oscillating between a few times 1035 erg s-1 and a few times 1037 erg s-1 in the space of a few weeks. The optical, infrared and ultraviolet colours of the optical object are consistent with an an accretion disc around a compact object companion, which may be either a white dwarf or a black hole, depending on the system parameters. If the origin of the luminous supersoft X-rays is the atmosphere of a white dwarf that is burning hydrogen in shell, it is as hot and luminous as post-thermonuclear flash novae, yet no major optical outburst has ever been observed, suggesting that the white dwarf is very massive (m ≥ 1.2 M⊙) and it is accreting and burning at the high rate m > 10-8 M⊙ yr-1 expected for Type Ia supernovae progenitors. In this case, the X-ray variability may be due to a very short recurrence time of only mildly degenerate thermonuclear flashes.Fil: Orio, Marina. Osservatorio Astronomico Di Padova; Italia. University of Wisconsin; Estados UnidosFil: Luna, Gerardo Juan Manuel. 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. Universidad de Buenos Aires; ArgentinaFil: Kotulla, R.. University of Wisconsin; Estados UnidosFil: Gallager, J. S.. University of Wisconsin; Estados UnidosFil: Zampieri, L.. Osservatorio Astronomico Di Padova; ItaliaFil: Mikolajewska, J.. Nicolaus Copernicus Astronomical Center Of The Polish Academy Of Sciences; PoloniaFil: Harbeck, D.. Wiyn Observatory; Estados UnidosFil: Bianchini, A.. Università di Padova; ItaliaFil: Chiosi, E.. Università di Padova; ItaliaFil: Della Valle, M.. Osservatorio Astronomico Di Capodimonte; ItaliaFil: de Martino, D.. Osservatorio Astronomico Di Capodimonte; ItaliaFil: Kaur, A.. Clemson University; Estados UnidosFil: Mapelli, M.. Osservatorio di Padova; ItaliaFil: Munari, U.. Osservatorio di Padova; ItaliaFil: Odendaal, A.. University of the Free State; SudáfricaFil: Trinchieri, G.. Osservatorio Astronomico di Brera; ItaliaFil: Wade, J.. University of Wisconsin; Estados UnidosFil: Zemko, P.. Università di Padova; ItaliaWiley Blackwell Publishing, Inc2017-09info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/24574Orio, Marina; Luna, Gerardo Juan Manuel; Kotulla, R.; Gallager, J. S.; Zampieri, L.; et al.; CXO J004318.8+412016*A steady supersoft X-ray source in M 31; Wiley Blackwell Publishing, Inc; Monthly Notices of the Royal Astronomical Society; 470; 2; 9-2017; 2212-22240035-8711CONICET DigitalCONICETenginfo:eu-repo/semantics/altIdentifier/doi/10.1093/mnras/stx1355info:eu-repo/semantics/altIdentifier/url/https://academic.oup.com/mnras/article-abstract/470/2/2212/3861854/CXO-J004318-8-412016-a-steady-supersoft-X-ray?redirectedFrom=fulltextinfo:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by-nc-sa/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2025-10-22T12:17:32Zoai:ri.conicet.gov.ar:11336/24574instacron: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:34982025-10-22 12:17:32.504CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse
dc.title.none.fl_str_mv CXO J004318.8+412016*A steady supersoft X-ray source in M 31
title CXO J004318.8+412016*A steady supersoft X-ray source in M 31
spellingShingle CXO J004318.8+412016*A steady supersoft X-ray source in M 31
Orio, Marina
BINARIES: SYMBIOTIC
GALAXIES: INDIVIDUAL: M31
WHITE DWARFS
X-RAYS: BINARIES
X-RAYS: INDIVIDUAL: CXO J004318.8+412016
title_short CXO J004318.8+412016*A steady supersoft X-ray source in M 31
title_full CXO J004318.8+412016*A steady supersoft X-ray source in M 31
title_fullStr CXO J004318.8+412016*A steady supersoft X-ray source in M 31
title_full_unstemmed CXO J004318.8+412016*A steady supersoft X-ray source in M 31
title_sort CXO J004318.8+412016*A steady supersoft X-ray source in M 31
dc.creator.none.fl_str_mv Orio, Marina
Luna, Gerardo Juan Manuel
Kotulla, R.
Gallager, J. S.
Zampieri, L.
Mikolajewska, J.
Harbeck, D.
Bianchini, A.
Chiosi, E.
Della Valle, M.
de Martino, D.
Kaur, A.
Mapelli, M.
Munari, U.
Odendaal, A.
Trinchieri, G.
Wade, J.
Zemko, P.
author Orio, Marina
author_facet Orio, Marina
Luna, Gerardo Juan Manuel
Kotulla, R.
Gallager, J. S.
Zampieri, L.
Mikolajewska, J.
Harbeck, D.
Bianchini, A.
Chiosi, E.
Della Valle, M.
de Martino, D.
Kaur, A.
Mapelli, M.
Munari, U.
Odendaal, A.
Trinchieri, G.
Wade, J.
Zemko, P.
author_role author
author2 Luna, Gerardo Juan Manuel
Kotulla, R.
Gallager, J. S.
Zampieri, L.
Mikolajewska, J.
Harbeck, D.
Bianchini, A.
Chiosi, E.
Della Valle, M.
de Martino, D.
Kaur, A.
Mapelli, M.
Munari, U.
Odendaal, A.
Trinchieri, G.
Wade, J.
Zemko, P.
author2_role author
author
author
author
author
author
author
author
author
author
author
author
author
author
author
author
author
dc.subject.none.fl_str_mv BINARIES: SYMBIOTIC
GALAXIES: INDIVIDUAL: M31
WHITE DWARFS
X-RAYS: BINARIES
X-RAYS: INDIVIDUAL: CXO J004318.8+412016
topic BINARIES: SYMBIOTIC
GALAXIES: INDIVIDUAL: M31
WHITE DWARFS
X-RAYS: BINARIES
X-RAYS: INDIVIDUAL: CXO J004318.8+412016
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 obtained an optical spectrum of a star we identify as the optical counterpart of the M31 Chandra source CXO J004318.8+412016, because of prominent emission lines of the Balmer series, of neutral helium, and a He II line at 4686 Å. The continuum energy distribution and the spectral characteristics demonstrate the presence of a red giant of K or earlier spectral type, so we concluded that the binary is likely to be a symbiotic system. CXO J004318.8+412016 has been observed in X-rays as a luminous supersoft source (SSS) since 1979, with effective temperature exceeding 40 eV and variable X-ray luminosity, oscillating between a few times 1035 erg s-1 and a few times 1037 erg s-1 in the space of a few weeks. The optical, infrared and ultraviolet colours of the optical object are consistent with an an accretion disc around a compact object companion, which may be either a white dwarf or a black hole, depending on the system parameters. If the origin of the luminous supersoft X-rays is the atmosphere of a white dwarf that is burning hydrogen in shell, it is as hot and luminous as post-thermonuclear flash novae, yet no major optical outburst has ever been observed, suggesting that the white dwarf is very massive (m ≥ 1.2 M⊙) and it is accreting and burning at the high rate m > 10-8 M⊙ yr-1 expected for Type Ia supernovae progenitors. In this case, the X-ray variability may be due to a very short recurrence time of only mildly degenerate thermonuclear flashes.
Fil: Orio, Marina. Osservatorio Astronomico Di Padova; Italia. University of Wisconsin; Estados Unidos
Fil: Luna, Gerardo Juan Manuel. 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. Universidad de Buenos Aires; Argentina
Fil: Kotulla, R.. University of Wisconsin; Estados Unidos
Fil: Gallager, J. S.. University of Wisconsin; Estados Unidos
Fil: Zampieri, L.. Osservatorio Astronomico Di Padova; Italia
Fil: Mikolajewska, J.. Nicolaus Copernicus Astronomical Center Of The Polish Academy Of Sciences; Polonia
Fil: Harbeck, D.. Wiyn Observatory; Estados Unidos
Fil: Bianchini, A.. Università di Padova; Italia
Fil: Chiosi, E.. Università di Padova; Italia
Fil: Della Valle, M.. Osservatorio Astronomico Di Capodimonte; Italia
Fil: de Martino, D.. Osservatorio Astronomico Di Capodimonte; Italia
Fil: Kaur, A.. Clemson University; Estados Unidos
Fil: Mapelli, M.. Osservatorio di Padova; Italia
Fil: Munari, U.. Osservatorio di Padova; Italia
Fil: Odendaal, A.. University of the Free State; Sudáfrica
Fil: Trinchieri, G.. Osservatorio Astronomico di Brera; Italia
Fil: Wade, J.. University of Wisconsin; Estados Unidos
Fil: Zemko, P.. Università di Padova; Italia
description We obtained an optical spectrum of a star we identify as the optical counterpart of the M31 Chandra source CXO J004318.8+412016, because of prominent emission lines of the Balmer series, of neutral helium, and a He II line at 4686 Å. The continuum energy distribution and the spectral characteristics demonstrate the presence of a red giant of K or earlier spectral type, so we concluded that the binary is likely to be a symbiotic system. CXO J004318.8+412016 has been observed in X-rays as a luminous supersoft source (SSS) since 1979, with effective temperature exceeding 40 eV and variable X-ray luminosity, oscillating between a few times 1035 erg s-1 and a few times 1037 erg s-1 in the space of a few weeks. The optical, infrared and ultraviolet colours of the optical object are consistent with an an accretion disc around a compact object companion, which may be either a white dwarf or a black hole, depending on the system parameters. If the origin of the luminous supersoft X-rays is the atmosphere of a white dwarf that is burning hydrogen in shell, it is as hot and luminous as post-thermonuclear flash novae, yet no major optical outburst has ever been observed, suggesting that the white dwarf is very massive (m ≥ 1.2 M⊙) and it is accreting and burning at the high rate m > 10-8 M⊙ yr-1 expected for Type Ia supernovae progenitors. In this case, the X-ray variability may be due to a very short recurrence time of only mildly degenerate thermonuclear flashes.
publishDate 2017
dc.date.none.fl_str_mv 2017-09
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/11336/24574
Orio, Marina; Luna, Gerardo Juan Manuel; Kotulla, R.; Gallager, J. S.; Zampieri, L.; et al.; CXO J004318.8+412016*A steady supersoft X-ray source in M 31; Wiley Blackwell Publishing, Inc; Monthly Notices of the Royal Astronomical Society; 470; 2; 9-2017; 2212-2224
0035-8711
CONICET Digital
CONICET
url http://hdl.handle.net/11336/24574
identifier_str_mv Orio, Marina; Luna, Gerardo Juan Manuel; Kotulla, R.; Gallager, J. S.; Zampieri, L.; et al.; CXO J004318.8+412016*A steady supersoft X-ray source in M 31; Wiley Blackwell Publishing, Inc; Monthly Notices of the Royal Astronomical Society; 470; 2; 9-2017; 2212-2224
0035-8711
CONICET Digital
CONICET
dc.language.none.fl_str_mv eng
language eng
dc.relation.none.fl_str_mv info:eu-repo/semantics/altIdentifier/doi/10.1093/mnras/stx1355
info:eu-repo/semantics/altIdentifier/url/https://academic.oup.com/mnras/article-abstract/470/2/2212/3861854/CXO-J004318-8-412016-a-steady-supersoft-X-ray?redirectedFrom=fulltext
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 Wiley Blackwell Publishing, Inc
publisher.none.fl_str_mv Wiley Blackwell Publishing, Inc
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 12.91661

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