Super Hot Cores in NGC 253: witnessing the formation and early evolution of super star clusters

Using 0.2 arcsec (similar to 3 pc) ALMA images of vibrationally excited HC3N emission (HC3N*) we reveal the presence of eight unresolved Super Hot Cores (SHCs) in the inner 160 pc of NGC253. Our LTE and non-LTE modelling of the HC3N* emission indicate that SHCs have dust temperatures of 200-375 K, r...

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Detalles Bibliográficos
Autores: Rico Villas, F., Martín Pintado, J., González Alfonso, Eduardo|||0000-0001-5285-8517, Martín, S., Rivilla, V.M.
Tipo de recurso: artículo
Fecha de publicación:2019
País:España
Institución:Universidad de Alcalá (UAH)
Repositorio:e_Buah Biblioteca Digital Universidad de Alcalá
Idioma:inglés
OAI Identifier:oai:ebuah.uah.es:10017/67588
Acceso en línea:http://hdl.handle.net/10017/67588
https://dx.doi.org/10.1093/mnras/stz3347
Access Level:acceso abierto
Palabra clave:Galaxies: individual: NGC253
Galaxies: ISM
Galaxies: nuclei
Galaxies: star clusters: general
Galaxies: star formation
Astronomía
Astronomy
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spelling Super Hot Cores in NGC 253: witnessing the formation and early evolution of super star clustersRico Villas, F.Martín Pintado, J.González Alfonso, Eduardo|||0000-0001-5285-8517Martín, S.Rivilla, V.M.Galaxies: individual: NGC253Galaxies: ISMGalaxies: nucleiGalaxies: star clusters: generalGalaxies: star formationAstronomíaAstronomyUsing 0.2 arcsec (similar to 3 pc) ALMA images of vibrationally excited HC3N emission (HC3N*) we reveal the presence of eight unresolved Super Hot Cores (SHCs) in the inner 160 pc of NGC253. Our LTE and non-LTE modelling of the HC3N* emission indicate that SHCs have dust temperatures of 200-375 K, relatively high H-2 densities of (1-6) x 10(6) cm(-3) and high IR luminosities of (0.1-1) x 10(8) L-circle dot. As expected from their short-lived phase (similar to 10(4) yr), all SHCs are associated with young super star clusters (SSCs). We use the ratio of luminosities from the SHCs (protostar phase) and from the free-free emission (ZAMS star phase), to establish the evolutionary stage of the SSCs. The youngest SSCs, with the larges ratios, have ages of a few 10(4) yr (proto-SSCs) and the more evolved SSCs are likely between 105 and 10(6) yr (ZAMS-SSCs). The different evolutionary stages of the SSCs are also supported by the radiative feedback from the UV radiation as traced by the HNCO/CS ratio, with this ratio being systematically higher in the young proto-SSCs than in the older ZAMS-SSCs. We also estimate the SFR and the SFE of the SSCs. The trend found in the estimated SFE (similar to 40 per cent for proto-SSCs and > 85 per cent for ZAMS-SSCs) and in the gas mass reservoir available for star formation, one order of magnitude higher for proto-SSCs, suggests that star formation is still going on in proto-SSCs. We also find that the most evolved SSCs are located, in projection, closer to the centre of the galaxy than the younger proto-SSCs, indicating an inside-out SSC formation scenario.Oxford Academic20192019-12-02journal articlehttp://purl.org/coar/resource_type/c_6501NAhttp://purl.org/coar/version/c_be7fb7dd8ff6fe43info:eu-repo/semantics/articleapplication/pdfhttp://hdl.handle.net/10017/67588https://dx.doi.org/10.1093/mnras/stz3347reponame:e_Buah Biblioteca Digital Universidad de Alcaláinstname:Universidad de Alcalá (UAH)Inglésengopen accesshttp://purl.org/coar/access_right/c_abf2Attribution-NonCommercial-NoDerivatives 4.0 Internationalhttp://creativecommons.org/licenses/by-nc-nd/4.0/info:eu-repo/semantics/openAccessoai:ebuah.uah.es:10017/675882026-06-18T11:13:07Z
dc.title.none.fl_str_mv Super Hot Cores in NGC 253: witnessing the formation and early evolution of super star clusters
title Super Hot Cores in NGC 253: witnessing the formation and early evolution of super star clusters
spellingShingle Super Hot Cores in NGC 253: witnessing the formation and early evolution of super star clusters
Rico Villas, F.
Galaxies: individual: NGC253
Galaxies: ISM
Galaxies: nuclei
Galaxies: star clusters: general
Galaxies: star formation
Astronomía
Astronomy
title_short Super Hot Cores in NGC 253: witnessing the formation and early evolution of super star clusters
title_full Super Hot Cores in NGC 253: witnessing the formation and early evolution of super star clusters
title_fullStr Super Hot Cores in NGC 253: witnessing the formation and early evolution of super star clusters
title_full_unstemmed Super Hot Cores in NGC 253: witnessing the formation and early evolution of super star clusters
title_sort Super Hot Cores in NGC 253: witnessing the formation and early evolution of super star clusters
dc.creator.none.fl_str_mv Rico Villas, F.
Martín Pintado, J.
González Alfonso, Eduardo|||0000-0001-5285-8517
Martín, S.
Rivilla, V.M.
author Rico Villas, F.
author_facet Rico Villas, F.
Martín Pintado, J.
González Alfonso, Eduardo|||0000-0001-5285-8517
Martín, S.
Rivilla, V.M.
author_role author
author2 Martín Pintado, J.
González Alfonso, Eduardo|||0000-0001-5285-8517
Martín, S.
Rivilla, V.M.
author2_role author
author
author
author
dc.subject.none.fl_str_mv Galaxies: individual: NGC253
Galaxies: ISM
Galaxies: nuclei
Galaxies: star clusters: general
Galaxies: star formation
Astronomía
Astronomy
topic Galaxies: individual: NGC253
Galaxies: ISM
Galaxies: nuclei
Galaxies: star clusters: general
Galaxies: star formation
Astronomía
Astronomy
description Using 0.2 arcsec (similar to 3 pc) ALMA images of vibrationally excited HC3N emission (HC3N*) we reveal the presence of eight unresolved Super Hot Cores (SHCs) in the inner 160 pc of NGC253. Our LTE and non-LTE modelling of the HC3N* emission indicate that SHCs have dust temperatures of 200-375 K, relatively high H-2 densities of (1-6) x 10(6) cm(-3) and high IR luminosities of (0.1-1) x 10(8) L-circle dot. As expected from their short-lived phase (similar to 10(4) yr), all SHCs are associated with young super star clusters (SSCs). We use the ratio of luminosities from the SHCs (protostar phase) and from the free-free emission (ZAMS star phase), to establish the evolutionary stage of the SSCs. The youngest SSCs, with the larges ratios, have ages of a few 10(4) yr (proto-SSCs) and the more evolved SSCs are likely between 105 and 10(6) yr (ZAMS-SSCs). The different evolutionary stages of the SSCs are also supported by the radiative feedback from the UV radiation as traced by the HNCO/CS ratio, with this ratio being systematically higher in the young proto-SSCs than in the older ZAMS-SSCs. We also estimate the SFR and the SFE of the SSCs. The trend found in the estimated SFE (similar to 40 per cent for proto-SSCs and > 85 per cent for ZAMS-SSCs) and in the gas mass reservoir available for star formation, one order of magnitude higher for proto-SSCs, suggests that star formation is still going on in proto-SSCs. We also find that the most evolved SSCs are located, in projection, closer to the centre of the galaxy than the younger proto-SSCs, indicating an inside-out SSC formation scenario.
publishDate 2019
dc.date.none.fl_str_mv 2019
2019-12-02
dc.type.none.fl_str_mv journal article
http://purl.org/coar/resource_type/c_6501
NA
http://purl.org/coar/version/c_be7fb7dd8ff6fe43
dc.type.openaire.fl_str_mv info:eu-repo/semantics/article
format article
dc.identifier.none.fl_str_mv http://hdl.handle.net/10017/67588
https://dx.doi.org/10.1093/mnras/stz3347
url http://hdl.handle.net/10017/67588
https://dx.doi.org/10.1093/mnras/stz3347
dc.language.none.fl_str_mv Inglés
eng
language_invalid_str_mv Inglés
language eng
dc.rights.none.fl_str_mv open access
http://purl.org/coar/access_right/c_abf2
Attribution-NonCommercial-NoDerivatives 4.0 International
http://creativecommons.org/licenses/by-nc-nd/4.0/
dc.rights.openaire.fl_str_mv info:eu-repo/semantics/openAccess
rights_invalid_str_mv open access
http://purl.org/coar/access_right/c_abf2
Attribution-NonCommercial-NoDerivatives 4.0 International
http://creativecommons.org/licenses/by-nc-nd/4.0/
eu_rights_str_mv openAccess
dc.format.none.fl_str_mv application/pdf
dc.publisher.none.fl_str_mv Oxford Academic
publisher.none.fl_str_mv Oxford Academic
dc.source.none.fl_str_mv reponame:e_Buah Biblioteca Digital Universidad de Alcalá
instname:Universidad de Alcalá (UAH)
instname_str Universidad de Alcalá (UAH)
reponame_str e_Buah Biblioteca Digital Universidad de Alcalá
collection e_Buah Biblioteca Digital Universidad de Alcalá
repository.name.fl_str_mv
repository.mail.fl_str_mv
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score 15.228081

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