The Maser-emitting Structure and Time Variability of the SiS Lines J = 14-13 and 15-14 in IRC+10216

Autores
Fonfra, J. P.; Fernandez Lopez, Manuel; Pardo, J. R.; Agúndez, M.; Sánchez Contreras, C.; Velilla Prieto, L.; Cernicharo, J.; Santander García, M.; Quintana Lacaci, G.; Castro Carrizo, A.; Curiel, S.
Año de publicación
2018
Idioma
inglés
Tipo de recurso
artículo
Estado
versión publicada
Descripción
We present new high angular resolution interferometer observations of the v = 0 J = 14-13 and 15-14 SiS lines toward IRC+10216, carried out with the Combined Array for Research in Millimeter-wave Astronomy and the Atacama Large Millimeter Array. The maps, with angular resolutions of ≃0.″25 and 0.″55, reveal (1) an extended, roughly uniform, and weak emission with a size of ≃0.″5; (2) a component elongated approximately along the east-west direction peaking at ≃0.″13 and 0.″17 at both sides of the central star; and (3) two blue- and redshifted compact components peaking around 0.″07 to the NW of the star. We have modeled the emission with a 3D radiation transfer code, finding that the observations cannot be explained only by thermal emission. Several maser clumps and one arc-shaped maser feature arranged from 5 to 20 from the central star, in addition to a thin shell-like maser structure at ≃13 , are required to explain the observations. This maser-emitting set of structures accounts for 75% of the total emission, while the other 25% is produced by thermally excited molecules. About 60% of the maser emission comes from the extended emission, and the rest comes from the set of clumps and the arc. The analysis of a time monitoring of these and other SiS and 29SiS lines carried out with the IRAM 30 m telescope from 2015 to present suggests that the intensity of some spectral components of the maser emission strongly depends on the stellar pulsation, while other components show a mild variability. This monitoring evidences a significant phase lag of ≃0.2 between the maser and near-IR light curves.
Fil: Fonfra, J. P.. Consejo Superior de Investigaciones Científicas; España
Fil: Fernandez Lopez, Manuel. 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
Fil: Pardo, J. R.. Consejo Superior de Investigaciones Científicas; España
Fil: Agúndez, M.. Consejo Superior de Investigaciones Científicas; España
Fil: Sánchez Contreras, C.. Consejo Superior de Investigaciones Científicas; España
Fil: Velilla Prieto, L.. Consejo Superior de Investigaciones Científicas; España
Fil: Cernicharo, J.. Consejo Superior de Investigaciones Científicas; España
Fil: Santander García, M.. Observatorio Astronomico Nacional; España
Fil: Quintana Lacaci, G.. Consejo Superior de Investigaciones Científicas; España
Fil: Castro Carrizo, A.. Institut de Radioastronomie Millimétrique; Francia
Fil: Curiel, S.. Universidad Nacional Autónoma de México; México
Materia
Circumstellar Matter
Masers
Stars: Agb And Post-Agb
Stars: Individual (Irc+10216)
Stars: Oscillations
Techniques: Interferometric
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:11336/82399
Acceder
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oai_identifier_str oai:ri.conicet.gov.ar:11336/82399
network_acronym_str CONICETDig
repository_id_str 3498
network_name_str CONICET Digital (CONICET)
spelling The Maser-emitting Structure and Time Variability of the SiS Lines J = 14-13 and 15-14 in IRC+10216Fonfra, J. P.Fernandez Lopez, ManuelPardo, J. R.Agúndez, M.Sánchez Contreras, C.Velilla Prieto, L.Cernicharo, J.Santander García, M.Quintana Lacaci, G.Castro Carrizo, A.Curiel, S.Circumstellar MatterMasersStars: Agb And Post-AgbStars: Individual (Irc+10216)Stars: OscillationsTechniques: Interferometrichttps://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1We present new high angular resolution interferometer observations of the v = 0 J = 14-13 and 15-14 SiS lines toward IRC+10216, carried out with the Combined Array for Research in Millimeter-wave Astronomy and the Atacama Large Millimeter Array. The maps, with angular resolutions of ≃0.″25 and 0.″55, reveal (1) an extended, roughly uniform, and weak emission with a size of ≃0.″5; (2) a component elongated approximately along the east-west direction peaking at ≃0.″13 and 0.″17 at both sides of the central star; and (3) two blue- and redshifted compact components peaking around 0.″07 to the NW of the star. We have modeled the emission with a 3D radiation transfer code, finding that the observations cannot be explained only by thermal emission. Several maser clumps and one arc-shaped maser feature arranged from 5 to 20 from the central star, in addition to a thin shell-like maser structure at ≃13 , are required to explain the observations. This maser-emitting set of structures accounts for 75% of the total emission, while the other 25% is produced by thermally excited molecules. About 60% of the maser emission comes from the extended emission, and the rest comes from the set of clumps and the arc. The analysis of a time monitoring of these and other SiS and 29SiS lines carried out with the IRAM 30 m telescope from 2015 to present suggests that the intensity of some spectral components of the maser emission strongly depends on the stellar pulsation, while other components show a mild variability. This monitoring evidences a significant phase lag of ≃0.2 between the maser and near-IR light curves.Fil: Fonfra, J. P.. Consejo Superior de Investigaciones Científicas; EspañaFil: Fernandez Lopez, Manuel. 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; ArgentinaFil: Pardo, J. R.. Consejo Superior de Investigaciones Científicas; EspañaFil: Agúndez, M.. Consejo Superior de Investigaciones Científicas; EspañaFil: Sánchez Contreras, C.. Consejo Superior de Investigaciones Científicas; EspañaFil: Velilla Prieto, L.. Consejo Superior de Investigaciones Científicas; EspañaFil: Cernicharo, J.. Consejo Superior de Investigaciones Científicas; EspañaFil: Santander García, M.. Observatorio Astronomico Nacional; EspañaFil: Quintana Lacaci, G.. Consejo Superior de Investigaciones Científicas; EspañaFil: Castro Carrizo, A.. Institut de Radioastronomie Millimétrique; FranciaFil: Curiel, S.. Universidad Nacional Autónoma de México; MéxicoIOP Publishing2018-06info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/82399Fonfra, J. P.; Fernandez Lopez, Manuel; Pardo, J. R.; Agúndez, M.; Sánchez Contreras, C.; et al.; The Maser-emitting Structure and Time Variability of the SiS Lines J = 14-13 and 15-14 in IRC+10216; IOP Publishing; Astrophysical Journal; 860; 2; 6-2018; 1-180004-637XCONICET DigitalCONICETenginfo:eu-repo/semantics/altIdentifier/doi/10.3847/1538-4357/aac5e3info:eu-repo/semantics/altIdentifier/url/https://iopscience.iop.org/article/10.3847/1538-4357/aac5e3info:eu-repo/semantics/altIdentifier/url/https://www.ncbi.nlm.nih.gov/pmc/articles/PMC6029660/info:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by-nc-sa/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2025-10-22T11:16:51Zoai:ri.conicet.gov.ar:11336/82399instacron: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 11:16:52.108CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse
dc.title.none.fl_str_mv The Maser-emitting Structure and Time Variability of the SiS Lines J = 14-13 and 15-14 in IRC+10216
title The Maser-emitting Structure and Time Variability of the SiS Lines J = 14-13 and 15-14 in IRC+10216
spellingShingle The Maser-emitting Structure and Time Variability of the SiS Lines J = 14-13 and 15-14 in IRC+10216
Fonfra, J. P.
Circumstellar Matter
Masers
Stars: Agb And Post-Agb
Stars: Individual (Irc+10216)
Stars: Oscillations
Techniques: Interferometric
title_short The Maser-emitting Structure and Time Variability of the SiS Lines J = 14-13 and 15-14 in IRC+10216
title_full The Maser-emitting Structure and Time Variability of the SiS Lines J = 14-13 and 15-14 in IRC+10216
title_fullStr The Maser-emitting Structure and Time Variability of the SiS Lines J = 14-13 and 15-14 in IRC+10216
title_full_unstemmed The Maser-emitting Structure and Time Variability of the SiS Lines J = 14-13 and 15-14 in IRC+10216
title_sort The Maser-emitting Structure and Time Variability of the SiS Lines J = 14-13 and 15-14 in IRC+10216
dc.creator.none.fl_str_mv Fonfra, J. P.
Fernandez Lopez, Manuel
Pardo, J. R.
Agúndez, M.
Sánchez Contreras, C.
Velilla Prieto, L.
Cernicharo, J.
Santander García, M.
Quintana Lacaci, G.
Castro Carrizo, A.
Curiel, S.
author Fonfra, J. P.
author_facet Fonfra, J. P.
Fernandez Lopez, Manuel
Pardo, J. R.
Agúndez, M.
Sánchez Contreras, C.
Velilla Prieto, L.
Cernicharo, J.
Santander García, M.
Quintana Lacaci, G.
Castro Carrizo, A.
Curiel, S.
author_role author
author2 Fernandez Lopez, Manuel
Pardo, J. R.
Agúndez, M.
Sánchez Contreras, C.
Velilla Prieto, L.
Cernicharo, J.
Santander García, M.
Quintana Lacaci, G.
Castro Carrizo, A.
Curiel, S.
author2_role author
author
author
author
author
author
author
author
author
author
dc.subject.none.fl_str_mv Circumstellar Matter
Masers
Stars: Agb And Post-Agb
Stars: Individual (Irc+10216)
Stars: Oscillations
Techniques: Interferometric
topic Circumstellar Matter
Masers
Stars: Agb And Post-Agb
Stars: Individual (Irc+10216)
Stars: Oscillations
Techniques: Interferometric
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 present new high angular resolution interferometer observations of the v = 0 J = 14-13 and 15-14 SiS lines toward IRC+10216, carried out with the Combined Array for Research in Millimeter-wave Astronomy and the Atacama Large Millimeter Array. The maps, with angular resolutions of ≃0.″25 and 0.″55, reveal (1) an extended, roughly uniform, and weak emission with a size of ≃0.″5; (2) a component elongated approximately along the east-west direction peaking at ≃0.″13 and 0.″17 at both sides of the central star; and (3) two blue- and redshifted compact components peaking around 0.″07 to the NW of the star. We have modeled the emission with a 3D radiation transfer code, finding that the observations cannot be explained only by thermal emission. Several maser clumps and one arc-shaped maser feature arranged from 5 to 20 from the central star, in addition to a thin shell-like maser structure at ≃13 , are required to explain the observations. This maser-emitting set of structures accounts for 75% of the total emission, while the other 25% is produced by thermally excited molecules. About 60% of the maser emission comes from the extended emission, and the rest comes from the set of clumps and the arc. The analysis of a time monitoring of these and other SiS and 29SiS lines carried out with the IRAM 30 m telescope from 2015 to present suggests that the intensity of some spectral components of the maser emission strongly depends on the stellar pulsation, while other components show a mild variability. This monitoring evidences a significant phase lag of ≃0.2 between the maser and near-IR light curves.
Fil: Fonfra, J. P.. Consejo Superior de Investigaciones Científicas; España
Fil: Fernandez Lopez, Manuel. 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
Fil: Pardo, J. R.. Consejo Superior de Investigaciones Científicas; España
Fil: Agúndez, M.. Consejo Superior de Investigaciones Científicas; España
Fil: Sánchez Contreras, C.. Consejo Superior de Investigaciones Científicas; España
Fil: Velilla Prieto, L.. Consejo Superior de Investigaciones Científicas; España
Fil: Cernicharo, J.. Consejo Superior de Investigaciones Científicas; España
Fil: Santander García, M.. Observatorio Astronomico Nacional; España
Fil: Quintana Lacaci, G.. Consejo Superior de Investigaciones Científicas; España
Fil: Castro Carrizo, A.. Institut de Radioastronomie Millimétrique; Francia
Fil: Curiel, S.. Universidad Nacional Autónoma de México; México
description We present new high angular resolution interferometer observations of the v = 0 J = 14-13 and 15-14 SiS lines toward IRC+10216, carried out with the Combined Array for Research in Millimeter-wave Astronomy and the Atacama Large Millimeter Array. The maps, with angular resolutions of ≃0.″25 and 0.″55, reveal (1) an extended, roughly uniform, and weak emission with a size of ≃0.″5; (2) a component elongated approximately along the east-west direction peaking at ≃0.″13 and 0.″17 at both sides of the central star; and (3) two blue- and redshifted compact components peaking around 0.″07 to the NW of the star. We have modeled the emission with a 3D radiation transfer code, finding that the observations cannot be explained only by thermal emission. Several maser clumps and one arc-shaped maser feature arranged from 5 to 20 from the central star, in addition to a thin shell-like maser structure at ≃13 , are required to explain the observations. This maser-emitting set of structures accounts for 75% of the total emission, while the other 25% is produced by thermally excited molecules. About 60% of the maser emission comes from the extended emission, and the rest comes from the set of clumps and the arc. The analysis of a time monitoring of these and other SiS and 29SiS lines carried out with the IRAM 30 m telescope from 2015 to present suggests that the intensity of some spectral components of the maser emission strongly depends on the stellar pulsation, while other components show a mild variability. This monitoring evidences a significant phase lag of ≃0.2 between the maser and near-IR light curves.
publishDate 2018
dc.date.none.fl_str_mv 2018-06
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/11336/82399
Fonfra, J. P.; Fernandez Lopez, Manuel; Pardo, J. R.; Agúndez, M.; Sánchez Contreras, C.; et al.; The Maser-emitting Structure and Time Variability of the SiS Lines J = 14-13 and 15-14 in IRC+10216; IOP Publishing; Astrophysical Journal; 860; 2; 6-2018; 1-18
0004-637X
CONICET Digital
CONICET
url http://hdl.handle.net/11336/82399
identifier_str_mv Fonfra, J. P.; Fernandez Lopez, Manuel; Pardo, J. R.; Agúndez, M.; Sánchez Contreras, C.; et al.; The Maser-emitting Structure and Time Variability of the SiS Lines J = 14-13 and 15-14 in IRC+10216; IOP Publishing; Astrophysical Journal; 860; 2; 6-2018; 1-18
0004-637X
CONICET Digital
CONICET
dc.language.none.fl_str_mv eng
language eng
dc.relation.none.fl_str_mv info:eu-repo/semantics/altIdentifier/doi/10.3847/1538-4357/aac5e3
info:eu-repo/semantics/altIdentifier/url/https://iopscience.iop.org/article/10.3847/1538-4357/aac5e3
info:eu-repo/semantics/altIdentifier/url/https://www.ncbi.nlm.nih.gov/pmc/articles/PMC6029660/
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 IOP Publishing
publisher.none.fl_str_mv IOP Publishing
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 12.982451

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