ISOCAM mid-infrared spectroscopy and NIR photometry of the HII complex N4 in the Large Magellanic Cloud

Autores
Contursi, A; Rubio, M.; Sauvage, M.; Cesarsky, R.; Barba, Rodolfo Hector; Boulanger, F
Año de publicación
2007
Idioma
inglés
Tipo de recurso
artículo
Estado
versión publicada
Descripción
Context: We present the analysis of ISOCAM-CVF and the J, H, and Ks photometry data for the HII region complex N4 in the Large Magellanic Cloud (LMC). Aims: The aim is twofold: 1) to study the connection between the interstellar medium and the star content of this region; 2) to investigate the effects of the lower-than-Galactic metallicity on dust properties. Methods: A dust-features - gas lines - continuum fitting technique on the whole ISOCAM-CVF data cube allows the production of images in each single emission and detailed analysis of dust (both continuum and bands), and ionized gas. The near infrared (NIR) photometry provides, for the first time, information on the stellar content of N4. Results: The mid-infrared (MIR) spectral characteristics of N4 are those expected for an HII region complex, i.e. very similar to those observed in galactic HII regions. The images in single dust feature bands and gas lines clearly show that the HII region core is completely devoid of the carriers responsible for the aromatic features (AFs). On the other hand, the ionized gas arises almost completely in this dust cavity, where the two main exciting stars of N4 are also located. The HII region models from Stasińska (1982, A&AS, 48, 2999) predict an HII region size that corresponds to the observed size of the dust cavity. We find evidence that the effect of lower-than-Galactic metallicity (although not as extreme as in the case of LMC) on the carriers responsible for the AFs is not to prevent their formation or to modify their chemical properties, but to enhance their destruction by the high and hard interstellar radiation field. We argue that this is the dominant process responsible for the absence of AFs in the HII region core. We show that this mechanism is more efficient on smaller dust particles/molecules thus affecting the dust-size distribution. We argue that effects on dust-size distribution, rather than the different dust properties due to a lower metallicity, should be taken into account when analyzing more distant, relatively low-metallicity galaxies. Finally, the analysis of the stellar content of N4 reveals 7 stars: 4 reddened O MS stars and three stars with envelopes. In particular, one of these seems to be an ultra compact HII region containing an embedded young stellar object.
Fil: Contursi, A. Institut Max Planck fuer Gesellschaft. Max Planck Institute for Extraterrestrial Physics; Alemania
Fil: Rubio, M.. Universidad de Chile; Chile
Fil: Sauvage, M.. Service D'astrophysique Du Cea; Francia
Fil: Cesarsky, R.. Universidad de La Serena; Chile
Fil: Barba, Rodolfo Hector. Institut Max Planck fuer Gesellschaft. Max Planck Institute for Extraterrestrial Physics; Alemania. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - San Juan. Instituto de Ciencias Astronómicas, de la Tierra y del Espacio. Universidad Nacional de San Juan. Instituto de Ciencias Astronómicas, de la Tierra y del Espacio; Argentina
Fil: Boulanger, F. Institut d'Astrophysique Spatiale; Francia
Materia
ISOCAM
Large Magellanic Cloud
HII complex N4
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:11336/214799

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network_name_str CONICET Digital (CONICET)
spelling ISOCAM mid-infrared spectroscopy and NIR photometry of the HII complex N4 in the Large Magellanic CloudContursi, ARubio, M.Sauvage, M.Cesarsky, R.Barba, Rodolfo HectorBoulanger, FISOCAMLarge Magellanic CloudHII complex N4https://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1Context: We present the analysis of ISOCAM-CVF and the J, H, and Ks photometry data for the HII region complex N4 in the Large Magellanic Cloud (LMC). Aims: The aim is twofold: 1) to study the connection between the interstellar medium and the star content of this region; 2) to investigate the effects of the lower-than-Galactic metallicity on dust properties. Methods: A dust-features - gas lines - continuum fitting technique on the whole ISOCAM-CVF data cube allows the production of images in each single emission and detailed analysis of dust (both continuum and bands), and ionized gas. The near infrared (NIR) photometry provides, for the first time, information on the stellar content of N4. Results: The mid-infrared (MIR) spectral characteristics of N4 are those expected for an HII region complex, i.e. very similar to those observed in galactic HII regions. The images in single dust feature bands and gas lines clearly show that the HII region core is completely devoid of the carriers responsible for the aromatic features (AFs). On the other hand, the ionized gas arises almost completely in this dust cavity, where the two main exciting stars of N4 are also located. The HII region models from Stasińska (1982, A&AS, 48, 2999) predict an HII region size that corresponds to the observed size of the dust cavity. We find evidence that the effect of lower-than-Galactic metallicity (although not as extreme as in the case of LMC) on the carriers responsible for the AFs is not to prevent their formation or to modify their chemical properties, but to enhance their destruction by the high and hard interstellar radiation field. We argue that this is the dominant process responsible for the absence of AFs in the HII region core. We show that this mechanism is more efficient on smaller dust particles/molecules thus affecting the dust-size distribution. We argue that effects on dust-size distribution, rather than the different dust properties due to a lower metallicity, should be taken into account when analyzing more distant, relatively low-metallicity galaxies. Finally, the analysis of the stellar content of N4 reveals 7 stars: 4 reddened O MS stars and three stars with envelopes. In particular, one of these seems to be an ultra compact HII region containing an embedded young stellar object.Fil: Contursi, A. Institut Max Planck fuer Gesellschaft. Max Planck Institute for Extraterrestrial Physics; AlemaniaFil: Rubio, M.. Universidad de Chile; ChileFil: Sauvage, M.. Service D'astrophysique Du Cea; FranciaFil: Cesarsky, R.. Universidad de La Serena; ChileFil: Barba, Rodolfo Hector. Institut Max Planck fuer Gesellschaft. Max Planck Institute for Extraterrestrial Physics; Alemania. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - San Juan. Instituto de Ciencias Astronómicas, de la Tierra y del Espacio. Universidad Nacional de San Juan. Instituto de Ciencias Astronómicas, de la Tierra y del Espacio; ArgentinaFil: Boulanger, F. Institut d'Astrophysique Spatiale; FranciaEDP Sciences2007-12info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/214799Contursi, A; Rubio, M.; Sauvage, M.; Cesarsky, R.; Barba, Rodolfo Hector; et al.; ISOCAM mid-infrared spectroscopy and NIR photometry of the HII complex N4 in the Large Magellanic Cloud; EDP Sciences; Astronomy and Astrophysics; 469; 2; 12-2007; 539-5510004-6361CONICET DigitalCONICETenginfo:eu-repo/semantics/altIdentifier/doi/10.1051/0004-6361:20066587info:eu-repo/semantics/altIdentifier/url/https://www.aanda.org/articles/aa/abs/2007/26/aa6587-06/aa6587-06.htmlinfo:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by-nc-sa/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2025-09-29T10:14:25Zoai:ri.conicet.gov.ar:11336/214799instacron: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 10:14:25.904CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse
dc.title.none.fl_str_mv ISOCAM mid-infrared spectroscopy and NIR photometry of the HII complex N4 in the Large Magellanic Cloud
title ISOCAM mid-infrared spectroscopy and NIR photometry of the HII complex N4 in the Large Magellanic Cloud
spellingShingle ISOCAM mid-infrared spectroscopy and NIR photometry of the HII complex N4 in the Large Magellanic Cloud
Contursi, A
ISOCAM
Large Magellanic Cloud
HII complex N4
title_short ISOCAM mid-infrared spectroscopy and NIR photometry of the HII complex N4 in the Large Magellanic Cloud
title_full ISOCAM mid-infrared spectroscopy and NIR photometry of the HII complex N4 in the Large Magellanic Cloud
title_fullStr ISOCAM mid-infrared spectroscopy and NIR photometry of the HII complex N4 in the Large Magellanic Cloud
title_full_unstemmed ISOCAM mid-infrared spectroscopy and NIR photometry of the HII complex N4 in the Large Magellanic Cloud
title_sort ISOCAM mid-infrared spectroscopy and NIR photometry of the HII complex N4 in the Large Magellanic Cloud
dc.creator.none.fl_str_mv Contursi, A
Rubio, M.
Sauvage, M.
Cesarsky, R.
Barba, Rodolfo Hector
Boulanger, F
author Contursi, A
author_facet Contursi, A
Rubio, M.
Sauvage, M.
Cesarsky, R.
Barba, Rodolfo Hector
Boulanger, F
author_role author
author2 Rubio, M.
Sauvage, M.
Cesarsky, R.
Barba, Rodolfo Hector
Boulanger, F
author2_role author
author
author
author
author
dc.subject.none.fl_str_mv ISOCAM
Large Magellanic Cloud
HII complex N4
topic ISOCAM
Large Magellanic Cloud
HII complex N4
purl_subject.fl_str_mv https://purl.org/becyt/ford/1.3
https://purl.org/becyt/ford/1
dc.description.none.fl_txt_mv Context: We present the analysis of ISOCAM-CVF and the J, H, and Ks photometry data for the HII region complex N4 in the Large Magellanic Cloud (LMC). Aims: The aim is twofold: 1) to study the connection between the interstellar medium and the star content of this region; 2) to investigate the effects of the lower-than-Galactic metallicity on dust properties. Methods: A dust-features - gas lines - continuum fitting technique on the whole ISOCAM-CVF data cube allows the production of images in each single emission and detailed analysis of dust (both continuum and bands), and ionized gas. The near infrared (NIR) photometry provides, for the first time, information on the stellar content of N4. Results: The mid-infrared (MIR) spectral characteristics of N4 are those expected for an HII region complex, i.e. very similar to those observed in galactic HII regions. The images in single dust feature bands and gas lines clearly show that the HII region core is completely devoid of the carriers responsible for the aromatic features (AFs). On the other hand, the ionized gas arises almost completely in this dust cavity, where the two main exciting stars of N4 are also located. The HII region models from Stasińska (1982, A&AS, 48, 2999) predict an HII region size that corresponds to the observed size of the dust cavity. We find evidence that the effect of lower-than-Galactic metallicity (although not as extreme as in the case of LMC) on the carriers responsible for the AFs is not to prevent their formation or to modify their chemical properties, but to enhance their destruction by the high and hard interstellar radiation field. We argue that this is the dominant process responsible for the absence of AFs in the HII region core. We show that this mechanism is more efficient on smaller dust particles/molecules thus affecting the dust-size distribution. We argue that effects on dust-size distribution, rather than the different dust properties due to a lower metallicity, should be taken into account when analyzing more distant, relatively low-metallicity galaxies. Finally, the analysis of the stellar content of N4 reveals 7 stars: 4 reddened O MS stars and three stars with envelopes. In particular, one of these seems to be an ultra compact HII region containing an embedded young stellar object.
Fil: Contursi, A. Institut Max Planck fuer Gesellschaft. Max Planck Institute for Extraterrestrial Physics; Alemania
Fil: Rubio, M.. Universidad de Chile; Chile
Fil: Sauvage, M.. Service D'astrophysique Du Cea; Francia
Fil: Cesarsky, R.. Universidad de La Serena; Chile
Fil: Barba, Rodolfo Hector. Institut Max Planck fuer Gesellschaft. Max Planck Institute for Extraterrestrial Physics; Alemania. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - San Juan. Instituto de Ciencias Astronómicas, de la Tierra y del Espacio. Universidad Nacional de San Juan. Instituto de Ciencias Astronómicas, de la Tierra y del Espacio; Argentina
Fil: Boulanger, F. Institut d'Astrophysique Spatiale; Francia
description Context: We present the analysis of ISOCAM-CVF and the J, H, and Ks photometry data for the HII region complex N4 in the Large Magellanic Cloud (LMC). Aims: The aim is twofold: 1) to study the connection between the interstellar medium and the star content of this region; 2) to investigate the effects of the lower-than-Galactic metallicity on dust properties. Methods: A dust-features - gas lines - continuum fitting technique on the whole ISOCAM-CVF data cube allows the production of images in each single emission and detailed analysis of dust (both continuum and bands), and ionized gas. The near infrared (NIR) photometry provides, for the first time, information on the stellar content of N4. Results: The mid-infrared (MIR) spectral characteristics of N4 are those expected for an HII region complex, i.e. very similar to those observed in galactic HII regions. The images in single dust feature bands and gas lines clearly show that the HII region core is completely devoid of the carriers responsible for the aromatic features (AFs). On the other hand, the ionized gas arises almost completely in this dust cavity, where the two main exciting stars of N4 are also located. The HII region models from Stasińska (1982, A&AS, 48, 2999) predict an HII region size that corresponds to the observed size of the dust cavity. We find evidence that the effect of lower-than-Galactic metallicity (although not as extreme as in the case of LMC) on the carriers responsible for the AFs is not to prevent their formation or to modify their chemical properties, but to enhance their destruction by the high and hard interstellar radiation field. We argue that this is the dominant process responsible for the absence of AFs in the HII region core. We show that this mechanism is more efficient on smaller dust particles/molecules thus affecting the dust-size distribution. We argue that effects on dust-size distribution, rather than the different dust properties due to a lower metallicity, should be taken into account when analyzing more distant, relatively low-metallicity galaxies. Finally, the analysis of the stellar content of N4 reveals 7 stars: 4 reddened O MS stars and three stars with envelopes. In particular, one of these seems to be an ultra compact HII region containing an embedded young stellar object.
publishDate 2007
dc.date.none.fl_str_mv 2007-12
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/11336/214799
Contursi, A; Rubio, M.; Sauvage, M.; Cesarsky, R.; Barba, Rodolfo Hector; et al.; ISOCAM mid-infrared spectroscopy and NIR photometry of the HII complex N4 in the Large Magellanic Cloud; EDP Sciences; Astronomy and Astrophysics; 469; 2; 12-2007; 539-551
0004-6361
CONICET Digital
CONICET
url http://hdl.handle.net/11336/214799
identifier_str_mv Contursi, A; Rubio, M.; Sauvage, M.; Cesarsky, R.; Barba, Rodolfo Hector; et al.; ISOCAM mid-infrared spectroscopy and NIR photometry of the HII complex N4 in the Large Magellanic Cloud; EDP Sciences; Astronomy and Astrophysics; 469; 2; 12-2007; 539-551
0004-6361
CONICET Digital
CONICET
dc.language.none.fl_str_mv eng
language eng
dc.relation.none.fl_str_mv info:eu-repo/semantics/altIdentifier/doi/10.1051/0004-6361:20066587
info:eu-repo/semantics/altIdentifier/url/https://www.aanda.org/articles/aa/abs/2007/26/aa6587-06/aa6587-06.html
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 EDP Sciences
publisher.none.fl_str_mv EDP Sciences
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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