Slowly Cooling White Dwarfs in NGC 6752

Autores
Chen, Jianxing; Ferraro, Francesco R.; Cadelano, Mario; Salaris, Maurizio; Lanzoni, Barbara; Pallanca, Cristina; Althaus, Leandro Gabriel; Cassisi, Santi; Dalessandro, Emanuele
Año de publicación
2022
Idioma
inglés
Tipo de recurso
artículo
Estado
versión publicada
Descripción
Recently, a new class of white dwarfs (“slowly cooling WDs”) has been identified in the globular cluster M13. The cooling time of these stars is increased by stable thermonuclear hydrogen burning in their residual envelope. These WDs are thought to be originated by horizontal branch (HB) stars populating the HB blue tail that skipped the asymptotic giant branch phase. To further explore this phenomenon, we took advantage of deep photometric data acquired with the Hubble Space Telescope in the near-ultraviolet and investigate the bright portion of the WD cooling sequence in NGC 6752, another Galactic globular cluster with a metallicity, age, and HB morphology similar to M13. The normalized WD luminosity function derived in NGC 6752 turns out to be impressively similar to that observed in M13, in agreement with the fact that the stellar mass distribution along the HB of these two systems is almost identical. As in the case of M13, the comparison with theoretical predictions is consistent with ∼70% of the investigated WDs evolving at slower rates than standard, purely cooling WDs. Thanks to its relatively short distance from Earth, NGC 6752 photometry reaches a luminosity 1 order of a magnitude fainter than the case of M13, allowing us to sample a regime where the cooling time delay, with respect to standard WD models, reaches ∼300 Myr. The results presented in this paper provide new evidence for the existence of slowly cooling WDs and further support to the scenario proposing a direct causal connection between this phenomenon and the HB morphology of the host stellar cluster.
Fil: Chen, Jianxing. Universidad de Bologna; Italia
Fil: Ferraro, Francesco R.. Universidad de Bologna; Italia
Fil: Cadelano, Mario. Universidad de Bologna; Italia
Fil: Salaris, Maurizio. Istituto Nazionale di Astrofisica; Italia
Fil: Lanzoni, Barbara. Universidad de Bologna; Italia
Fil: Pallanca, Cristina. Universidad de Bologna; Italia
Fil: Althaus, Leandro Gabriel. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto de Astrofísica La Plata. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas. Instituto de Astrofísica La Plata; Argentina
Fil: Cassisi, Santi. Istituto Nazionale di Astrofisica; Italia
Fil: Dalessandro, Emanuele. Osservatorio di Astrofisica e Scienza dello Spazio di Bologna; Italia
Materia
white dwarfs
stellar populations
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:11336/210881
Acceder
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oai_identifier_str oai:ri.conicet.gov.ar:11336/210881
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repository_id_str 3498
network_name_str CONICET Digital (CONICET)
spelling Slowly Cooling White Dwarfs in NGC 6752Chen, JianxingFerraro, Francesco R.Cadelano, MarioSalaris, MaurizioLanzoni, BarbaraPallanca, CristinaAlthaus, Leandro GabrielCassisi, SantiDalessandro, Emanuelewhite dwarfsstellar populationshttps://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1Recently, a new class of white dwarfs (“slowly cooling WDs”) has been identified in the globular cluster M13. The cooling time of these stars is increased by stable thermonuclear hydrogen burning in their residual envelope. These WDs are thought to be originated by horizontal branch (HB) stars populating the HB blue tail that skipped the asymptotic giant branch phase. To further explore this phenomenon, we took advantage of deep photometric data acquired with the Hubble Space Telescope in the near-ultraviolet and investigate the bright portion of the WD cooling sequence in NGC 6752, another Galactic globular cluster with a metallicity, age, and HB morphology similar to M13. The normalized WD luminosity function derived in NGC 6752 turns out to be impressively similar to that observed in M13, in agreement with the fact that the stellar mass distribution along the HB of these two systems is almost identical. As in the case of M13, the comparison with theoretical predictions is consistent with ∼70% of the investigated WDs evolving at slower rates than standard, purely cooling WDs. Thanks to its relatively short distance from Earth, NGC 6752 photometry reaches a luminosity 1 order of a magnitude fainter than the case of M13, allowing us to sample a regime where the cooling time delay, with respect to standard WD models, reaches ∼300 Myr. The results presented in this paper provide new evidence for the existence of slowly cooling WDs and further support to the scenario proposing a direct causal connection between this phenomenon and the HB morphology of the host stellar cluster.Fil: Chen, Jianxing. Universidad de Bologna; ItaliaFil: Ferraro, Francesco R.. Universidad de Bologna; ItaliaFil: Cadelano, Mario. Universidad de Bologna; ItaliaFil: Salaris, Maurizio. Istituto Nazionale di Astrofisica; ItaliaFil: Lanzoni, Barbara. Universidad de Bologna; ItaliaFil: Pallanca, Cristina. Universidad de Bologna; ItaliaFil: Althaus, Leandro Gabriel. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto de Astrofísica La Plata. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas. Instituto de Astrofísica La Plata; ArgentinaFil: Cassisi, Santi. Istituto Nazionale di Astrofisica; ItaliaFil: Dalessandro, Emanuele. Osservatorio di Astrofisica e Scienza dello Spazio di Bologna; ItaliaIOP Publishing2022-08info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/210881Chen, Jianxing; Ferraro, Francesco R.; Cadelano, Mario; Salaris, Maurizio; Lanzoni, Barbara; et al.; Slowly Cooling White Dwarfs in NGC 6752; IOP Publishing; Astrophysical Journal; 934; 2; 8-2022; 1-90004-637XCONICET DigitalCONICETenginfo:eu-repo/semantics/altIdentifier/doi/10.3847/1538-4357/ac7a45info:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by-nc-sa/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2025-09-29T10:23:37Zoai:ri.conicet.gov.ar:11336/210881instacron: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 10:23:37.721CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse
dc.title.none.fl_str_mv Slowly Cooling White Dwarfs in NGC 6752
title Slowly Cooling White Dwarfs in NGC 6752
spellingShingle Slowly Cooling White Dwarfs in NGC 6752
Chen, Jianxing
white dwarfs
stellar populations
title_short Slowly Cooling White Dwarfs in NGC 6752
title_full Slowly Cooling White Dwarfs in NGC 6752
title_fullStr Slowly Cooling White Dwarfs in NGC 6752
title_full_unstemmed Slowly Cooling White Dwarfs in NGC 6752
title_sort Slowly Cooling White Dwarfs in NGC 6752
dc.creator.none.fl_str_mv Chen, Jianxing
Ferraro, Francesco R.
Cadelano, Mario
Salaris, Maurizio
Lanzoni, Barbara
Pallanca, Cristina
Althaus, Leandro Gabriel
Cassisi, Santi
Dalessandro, Emanuele
author Chen, Jianxing
author_facet Chen, Jianxing
Ferraro, Francesco R.
Cadelano, Mario
Salaris, Maurizio
Lanzoni, Barbara
Pallanca, Cristina
Althaus, Leandro Gabriel
Cassisi, Santi
Dalessandro, Emanuele
author_role author
author2 Ferraro, Francesco R.
Cadelano, Mario
Salaris, Maurizio
Lanzoni, Barbara
Pallanca, Cristina
Althaus, Leandro Gabriel
Cassisi, Santi
Dalessandro, Emanuele
author2_role author
author
author
author
author
author
author
author
dc.subject.none.fl_str_mv white dwarfs
stellar populations
topic white dwarfs
stellar populations
purl_subject.fl_str_mv https://purl.org/becyt/ford/1.3
https://purl.org/becyt/ford/1
dc.description.none.fl_txt_mv Recently, a new class of white dwarfs (“slowly cooling WDs”) has been identified in the globular cluster M13. The cooling time of these stars is increased by stable thermonuclear hydrogen burning in their residual envelope. These WDs are thought to be originated by horizontal branch (HB) stars populating the HB blue tail that skipped the asymptotic giant branch phase. To further explore this phenomenon, we took advantage of deep photometric data acquired with the Hubble Space Telescope in the near-ultraviolet and investigate the bright portion of the WD cooling sequence in NGC 6752, another Galactic globular cluster with a metallicity, age, and HB morphology similar to M13. The normalized WD luminosity function derived in NGC 6752 turns out to be impressively similar to that observed in M13, in agreement with the fact that the stellar mass distribution along the HB of these two systems is almost identical. As in the case of M13, the comparison with theoretical predictions is consistent with ∼70% of the investigated WDs evolving at slower rates than standard, purely cooling WDs. Thanks to its relatively short distance from Earth, NGC 6752 photometry reaches a luminosity 1 order of a magnitude fainter than the case of M13, allowing us to sample a regime where the cooling time delay, with respect to standard WD models, reaches ∼300 Myr. The results presented in this paper provide new evidence for the existence of slowly cooling WDs and further support to the scenario proposing a direct causal connection between this phenomenon and the HB morphology of the host stellar cluster.
Fil: Chen, Jianxing. Universidad de Bologna; Italia
Fil: Ferraro, Francesco R.. Universidad de Bologna; Italia
Fil: Cadelano, Mario. Universidad de Bologna; Italia
Fil: Salaris, Maurizio. Istituto Nazionale di Astrofisica; Italia
Fil: Lanzoni, Barbara. Universidad de Bologna; Italia
Fil: Pallanca, Cristina. Universidad de Bologna; Italia
Fil: Althaus, Leandro Gabriel. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto de Astrofísica La Plata. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas. Instituto de Astrofísica La Plata; Argentina
Fil: Cassisi, Santi. Istituto Nazionale di Astrofisica; Italia
Fil: Dalessandro, Emanuele. Osservatorio di Astrofisica e Scienza dello Spazio di Bologna; Italia
description Recently, a new class of white dwarfs (“slowly cooling WDs”) has been identified in the globular cluster M13. The cooling time of these stars is increased by stable thermonuclear hydrogen burning in their residual envelope. These WDs are thought to be originated by horizontal branch (HB) stars populating the HB blue tail that skipped the asymptotic giant branch phase. To further explore this phenomenon, we took advantage of deep photometric data acquired with the Hubble Space Telescope in the near-ultraviolet and investigate the bright portion of the WD cooling sequence in NGC 6752, another Galactic globular cluster with a metallicity, age, and HB morphology similar to M13. The normalized WD luminosity function derived in NGC 6752 turns out to be impressively similar to that observed in M13, in agreement with the fact that the stellar mass distribution along the HB of these two systems is almost identical. As in the case of M13, the comparison with theoretical predictions is consistent with ∼70% of the investigated WDs evolving at slower rates than standard, purely cooling WDs. Thanks to its relatively short distance from Earth, NGC 6752 photometry reaches a luminosity 1 order of a magnitude fainter than the case of M13, allowing us to sample a regime where the cooling time delay, with respect to standard WD models, reaches ∼300 Myr. The results presented in this paper provide new evidence for the existence of slowly cooling WDs and further support to the scenario proposing a direct causal connection between this phenomenon and the HB morphology of the host stellar cluster.
publishDate 2022
dc.date.none.fl_str_mv 2022-08
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/11336/210881
Chen, Jianxing; Ferraro, Francesco R.; Cadelano, Mario; Salaris, Maurizio; Lanzoni, Barbara; et al.; Slowly Cooling White Dwarfs in NGC 6752; IOP Publishing; Astrophysical Journal; 934; 2; 8-2022; 1-9
0004-637X
CONICET Digital
CONICET
url http://hdl.handle.net/11336/210881
identifier_str_mv Chen, Jianxing; Ferraro, Francesco R.; Cadelano, Mario; Salaris, Maurizio; Lanzoni, Barbara; et al.; Slowly Cooling White Dwarfs in NGC 6752; IOP Publishing; Astrophysical Journal; 934; 2; 8-2022; 1-9
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/ac7a45
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 13.070432

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