On the derivation of dynamical masses of the stellar clusters in the circumnuclear region of NGC 2903

Autores
Hägele, Guillermo Federico; Díaz Beltrán, Ángeles Isabel; Cardaci, Mónica Viviana; Terlevich, Elena; Terlevich, Roberto
Año de publicación
2009
Idioma
inglés
Tipo de recurso
artículo
Estado
versión publicada
Descripción
Gas and star velocity dispersions have been derived for four circumnuclear star-forming regions (CNSFRs) and the nucleus of the spiral galaxy NGC 2903 using high-resolution spectroscopy in the blue and far red. Stellar velocity dispersions have been obtained from the Ca ii triplet lines at λλ 8494, 8542, 8662 Å, using cross-correlation techniques, while gas velocity dispersions have been measured by Gaussian fits to the Hβ λ 4861 Å line. The CNSFRs, with sizes of about 100 to 150 pc in diameter, show a complex structure at the Hubble Space Telescope (HST) resolution, with a good number of subclusters with linear diameters between 3 and 8 pc. Their stellar velocity dispersions range from 39 to 67 km s-1. These values, together with the sizes measured on archival HST images, yield upper limits to the dynamical masses for the individual star clusters between 1.8 and 8.7 × 106 M⊙ and upper limits to the masses for the whole CNSFR between 4.9 × 106 and 4.3 × 107 M⊙. The masses of the ionizing stellar population responsible for the H ii region gaseous emission have been derived from their published Hα luminosities and are found to be between 1.9 and 2.5 × 10 6 M⊙ for the star-forming regions, and 2.1 × 105 M⊙ for the galaxy nucleus, therefore constituting between 1 and 4 per cent of the total dynamical mass. In the CNSFR, star and gas velocity dispersions are found to differ by about 20 km s-1 with the Hβ lines being narrower than both the stellar lines and the [O iii] λ 5007 Å lines. The ionized gas kinematics are complex; two different kinematical components seem to be present as evidenced by different widths and Doppler shifts. The line profiles in the spectra of the galaxy nucleus, however, are consistent with the presence of a single component with radial velocity and velocity dispersion close to those measured for the stellar absorption lines. The presence and reach of two distinct components in the emission lines in ionized regions and the influence that this fact could have on the observed line ratios are of major interest for several reasons, among others, the classification of the activity in the central regions of galaxies, the inferences about the nature of the source of ionization for the two components and the derivation of the gaseous chemical abundances.
Facultad de Ciencias Astronómicas y Geofísicas
Materia
Ciencias Astronómicas
Galaxies: individual: NGC 2903
Galaxies: kinematics and dynamics
Galaxies: star clusters
Galaxies: starburst
H ii regions
Nivel de accesibilidad
acceso abierto
Condiciones de uso
http://creativecommons.org/licenses/by-nc-sa/4.0/
Repositorio
SEDICI (UNLP)
Institución
Universidad Nacional de La Plata
OAI Identificador
oai:sedici.unlp.edu.ar:10915/82671

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oai_identifier_str oai:sedici.unlp.edu.ar:10915/82671
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network_name_str SEDICI (UNLP)
spelling On the derivation of dynamical masses of the stellar clusters in the circumnuclear region of NGC 2903Hägele, Guillermo FedericoDíaz Beltrán, Ángeles IsabelCardaci, Mónica VivianaTerlevich, ElenaTerlevich, RobertoCiencias AstronómicasGalaxies: individual: NGC 2903Galaxies: kinematics and dynamicsGalaxies: star clustersGalaxies: starburstH ii regionsGas and star velocity dispersions have been derived for four circumnuclear star-forming regions (CNSFRs) and the nucleus of the spiral galaxy NGC 2903 using high-resolution spectroscopy in the blue and far red. Stellar velocity dispersions have been obtained from the Ca ii triplet lines at λλ 8494, 8542, 8662 Å, using cross-correlation techniques, while gas velocity dispersions have been measured by Gaussian fits to the Hβ λ 4861 Å line. The CNSFRs, with sizes of about 100 to 150 pc in diameter, show a complex structure at the Hubble Space Telescope (HST) resolution, with a good number of subclusters with linear diameters between 3 and 8 pc. Their stellar velocity dispersions range from 39 to 67 km s-1. These values, together with the sizes measured on archival HST images, yield upper limits to the dynamical masses for the individual star clusters between 1.8 and 8.7 × 106 M⊙ and upper limits to the masses for the whole CNSFR between 4.9 × 106 and 4.3 × 107 M⊙. The masses of the ionizing stellar population responsible for the H ii region gaseous emission have been derived from their published Hα luminosities and are found to be between 1.9 and 2.5 × 10 6 M⊙ for the star-forming regions, and 2.1 × 105 M⊙ for the galaxy nucleus, therefore constituting between 1 and 4 per cent of the total dynamical mass. In the CNSFR, star and gas velocity dispersions are found to differ by about 20 km s-1 with the Hβ lines being narrower than both the stellar lines and the [O iii] λ 5007 Å lines. The ionized gas kinematics are complex; two different kinematical components seem to be present as evidenced by different widths and Doppler shifts. The line profiles in the spectra of the galaxy nucleus, however, are consistent with the presence of a single component with radial velocity and velocity dispersion close to those measured for the stellar absorption lines. The presence and reach of two distinct components in the emission lines in ionized regions and the influence that this fact could have on the observed line ratios are of major interest for several reasons, among others, the classification of the activity in the central regions of galaxies, the inferences about the nature of the source of ionization for the two components and the derivation of the gaseous chemical abundances.Facultad de Ciencias Astronómicas y Geofísicas2009info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionArticulohttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdf2295-2312http://sedici.unlp.edu.ar/handle/10915/82671enginfo:eu-repo/semantics/altIdentifier/issn/0035-8711info:eu-repo/semantics/altIdentifier/doi/10.1111/j.1365-2966.2009.14898.xinfo:eu-repo/semantics/openAccesshttp://creativecommons.org/licenses/by-nc-sa/4.0/Creative Commons Attribution-NonCommercial-ShareAlike 4.0 International (CC BY-NC-SA 4.0)reponame:SEDICI (UNLP)instname:Universidad Nacional de La Platainstacron:UNLP2025-10-22T16:56:23Zoai:sedici.unlp.edu.ar:10915/82671Institucionalhttp://sedici.unlp.edu.ar/Universidad públicaNo correspondehttp://sedici.unlp.edu.ar/oai/snrdalira@sedici.unlp.edu.arArgentinaNo correspondeNo correspondeNo correspondeopendoar:13292025-10-22 16:56:23.565SEDICI (UNLP) - Universidad Nacional de La Platafalse
dc.title.none.fl_str_mv On the derivation of dynamical masses of the stellar clusters in the circumnuclear region of NGC 2903
title On the derivation of dynamical masses of the stellar clusters in the circumnuclear region of NGC 2903
spellingShingle On the derivation of dynamical masses of the stellar clusters in the circumnuclear region of NGC 2903
Hägele, Guillermo Federico
Ciencias Astronómicas
Galaxies: individual: NGC 2903
Galaxies: kinematics and dynamics
Galaxies: star clusters
Galaxies: starburst
H ii regions
title_short On the derivation of dynamical masses of the stellar clusters in the circumnuclear region of NGC 2903
title_full On the derivation of dynamical masses of the stellar clusters in the circumnuclear region of NGC 2903
title_fullStr On the derivation of dynamical masses of the stellar clusters in the circumnuclear region of NGC 2903
title_full_unstemmed On the derivation of dynamical masses of the stellar clusters in the circumnuclear region of NGC 2903
title_sort On the derivation of dynamical masses of the stellar clusters in the circumnuclear region of NGC 2903
dc.creator.none.fl_str_mv Hägele, Guillermo Federico
Díaz Beltrán, Ángeles Isabel
Cardaci, Mónica Viviana
Terlevich, Elena
Terlevich, Roberto
author Hägele, Guillermo Federico
author_facet Hägele, Guillermo Federico
Díaz Beltrán, Ángeles Isabel
Cardaci, Mónica Viviana
Terlevich, Elena
Terlevich, Roberto
author_role author
author2 Díaz Beltrán, Ángeles Isabel
Cardaci, Mónica Viviana
Terlevich, Elena
Terlevich, Roberto
author2_role author
author
author
author
dc.subject.none.fl_str_mv Ciencias Astronómicas
Galaxies: individual: NGC 2903
Galaxies: kinematics and dynamics
Galaxies: star clusters
Galaxies: starburst
H ii regions
topic Ciencias Astronómicas
Galaxies: individual: NGC 2903
Galaxies: kinematics and dynamics
Galaxies: star clusters
Galaxies: starburst
H ii regions
dc.description.none.fl_txt_mv Gas and star velocity dispersions have been derived for four circumnuclear star-forming regions (CNSFRs) and the nucleus of the spiral galaxy NGC 2903 using high-resolution spectroscopy in the blue and far red. Stellar velocity dispersions have been obtained from the Ca ii triplet lines at λλ 8494, 8542, 8662 Å, using cross-correlation techniques, while gas velocity dispersions have been measured by Gaussian fits to the Hβ λ 4861 Å line. The CNSFRs, with sizes of about 100 to 150 pc in diameter, show a complex structure at the Hubble Space Telescope (HST) resolution, with a good number of subclusters with linear diameters between 3 and 8 pc. Their stellar velocity dispersions range from 39 to 67 km s-1. These values, together with the sizes measured on archival HST images, yield upper limits to the dynamical masses for the individual star clusters between 1.8 and 8.7 × 106 M⊙ and upper limits to the masses for the whole CNSFR between 4.9 × 106 and 4.3 × 107 M⊙. The masses of the ionizing stellar population responsible for the H ii region gaseous emission have been derived from their published Hα luminosities and are found to be between 1.9 and 2.5 × 10 6 M⊙ for the star-forming regions, and 2.1 × 105 M⊙ for the galaxy nucleus, therefore constituting between 1 and 4 per cent of the total dynamical mass. In the CNSFR, star and gas velocity dispersions are found to differ by about 20 km s-1 with the Hβ lines being narrower than both the stellar lines and the [O iii] λ 5007 Å lines. The ionized gas kinematics are complex; two different kinematical components seem to be present as evidenced by different widths and Doppler shifts. The line profiles in the spectra of the galaxy nucleus, however, are consistent with the presence of a single component with radial velocity and velocity dispersion close to those measured for the stellar absorption lines. The presence and reach of two distinct components in the emission lines in ionized regions and the influence that this fact could have on the observed line ratios are of major interest for several reasons, among others, the classification of the activity in the central regions of galaxies, the inferences about the nature of the source of ionization for the two components and the derivation of the gaseous chemical abundances.
Facultad de Ciencias Astronómicas y Geofísicas
description Gas and star velocity dispersions have been derived for four circumnuclear star-forming regions (CNSFRs) and the nucleus of the spiral galaxy NGC 2903 using high-resolution spectroscopy in the blue and far red. Stellar velocity dispersions have been obtained from the Ca ii triplet lines at λλ 8494, 8542, 8662 Å, using cross-correlation techniques, while gas velocity dispersions have been measured by Gaussian fits to the Hβ λ 4861 Å line. The CNSFRs, with sizes of about 100 to 150 pc in diameter, show a complex structure at the Hubble Space Telescope (HST) resolution, with a good number of subclusters with linear diameters between 3 and 8 pc. Their stellar velocity dispersions range from 39 to 67 km s-1. These values, together with the sizes measured on archival HST images, yield upper limits to the dynamical masses for the individual star clusters between 1.8 and 8.7 × 106 M⊙ and upper limits to the masses for the whole CNSFR between 4.9 × 106 and 4.3 × 107 M⊙. The masses of the ionizing stellar population responsible for the H ii region gaseous emission have been derived from their published Hα luminosities and are found to be between 1.9 and 2.5 × 10 6 M⊙ for the star-forming regions, and 2.1 × 105 M⊙ for the galaxy nucleus, therefore constituting between 1 and 4 per cent of the total dynamical mass. In the CNSFR, star and gas velocity dispersions are found to differ by about 20 km s-1 with the Hβ lines being narrower than both the stellar lines and the [O iii] λ 5007 Å lines. The ionized gas kinematics are complex; two different kinematical components seem to be present as evidenced by different widths and Doppler shifts. The line profiles in the spectra of the galaxy nucleus, however, are consistent with the presence of a single component with radial velocity and velocity dispersion close to those measured for the stellar absorption lines. The presence and reach of two distinct components in the emission lines in ionized regions and the influence that this fact could have on the observed line ratios are of major interest for several reasons, among others, the classification of the activity in the central regions of galaxies, the inferences about the nature of the source of ionization for the two components and the derivation of the gaseous chemical abundances.
publishDate 2009
dc.date.none.fl_str_mv 2009
dc.type.none.fl_str_mv info:eu-repo/semantics/article
info:eu-repo/semantics/publishedVersion
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format article
status_str publishedVersion
dc.identifier.none.fl_str_mv http://sedici.unlp.edu.ar/handle/10915/82671
url http://sedici.unlp.edu.ar/handle/10915/82671
dc.language.none.fl_str_mv eng
language eng
dc.relation.none.fl_str_mv info:eu-repo/semantics/altIdentifier/issn/0035-8711
info:eu-repo/semantics/altIdentifier/doi/10.1111/j.1365-2966.2009.14898.x
dc.rights.none.fl_str_mv info:eu-repo/semantics/openAccess
http://creativecommons.org/licenses/by-nc-sa/4.0/
Creative Commons Attribution-NonCommercial-ShareAlike 4.0 International (CC BY-NC-SA 4.0)
eu_rights_str_mv openAccess
rights_invalid_str_mv http://creativecommons.org/licenses/by-nc-sa/4.0/
Creative Commons Attribution-NonCommercial-ShareAlike 4.0 International (CC BY-NC-SA 4.0)
dc.format.none.fl_str_mv application/pdf
2295-2312
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instname:Universidad Nacional de La Plata
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