Integrated spectral analysis of 18 concentrated star clusters in the Small Magellanic Cloud

We present in this study flux-calibrated integrated spectra in the range (3600-6800) Å for 18 concentrated SMC clusters. Cluster reddening values were estimated by interpolation between the extinction maps of Burstein & Heiles (1982, AJ, 87, 1165) and Schlegel et al. (1998, ApJ, 500, 525). The c...

Descripción completa

Guardado en:
Detalles Bibliográficos
Publicado: 2005
Materias:
Galaxies: star clusters
Magellanic Clouds
Techniques: spectroscopic
Calibration
Clouds
Continuum mechanics
Estimation
Galaxies
Interpolation
Spectroscopic analysis
Cluster formation
Magellanic clouds
Astrophysics
Acceso en línea:https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_00046361_v440_n1_p111_Piatti
http://hdl.handle.net/20.500.12110/paper_00046361_v440_n1_p111_Piatti
Aporte de:
Biblioteca Digital - Facultad de Ciencias Exactas y Naturales (UBA) de Universidad de Buenos Aires
id paper:paper_00046361_v440_n1_p111_Piatti
record_format dspace
spelling paper:paper_00046361_v440_n1_p111_Piatti2023-06-08T14:27:38Z Integrated spectral analysis of 18 concentrated star clusters in the Small Magellanic Cloud Galaxies: star clusters Magellanic Clouds Techniques: spectroscopic Calibration Clouds Continuum mechanics Estimation Galaxies Interpolation Spectroscopic analysis Cluster formation Galaxies: star clusters Magellanic clouds Techniques: spectroscopic Astrophysics We present in this study flux-calibrated integrated spectra in the range (3600-6800) Å for 18 concentrated SMC clusters. Cluster reddening values were estimated by interpolation between the extinction maps of Burstein & Heiles (1982, AJ, 87, 1165) and Schlegel et al. (1998, ApJ, 500, 525). The cluster parameters were derived from the template matching procedure by comparing the line strengths and continuum distribution of the cluster spectra with those of template cluster spectra with known parameters and from the equivalent width (EW) method. In this case, new calibrations were used together with diagnostic diagrams involving the sum of EWs of selected spectral lines. A very good agreement between ages derived from both methods was found. The final cluster ages obtained from the weighted average of values taken from the literature and the present measured ones range from 15 Mr (e.g. L 51) to 7 Gyr (K 3). Metal abundances have been derived for only 5 clusters from the present sample, while metallicity values directly averaged from published values for other 4 clusters have been adopted. Combining the present cluster sample with 19 additional SMC clusters whose ages and metal abundances were put onto a homogeneous scale, we analyse the age and metallicity distributions in order to explore the SMC star formation history and its spatial extent. By considering the distances of the clusters from the SMC centre instead of their projections onto the right ascension and declination axes, the present age-position relation suggests that the SMC inner disk could have been related to a cluster formation episode which reached the peak ∼2.5 Gyr ago. Evidence for an age gradient in the inner SMC disk is also presented. © ESO 2005. 2005 https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_00046361_v440_n1_p111_Piatti http://hdl.handle.net/20.500.12110/paper_00046361_v440_n1_p111_Piatti
institution Universidad de Buenos Aires
institution_str I-28
repository_str R-134
collection Biblioteca Digital - Facultad de Ciencias Exactas y Naturales (UBA)
topic Galaxies: star clusters
Magellanic Clouds
Techniques: spectroscopic
Calibration
Clouds
Continuum mechanics
Estimation
Galaxies
Interpolation
Spectroscopic analysis
Cluster formation
Galaxies: star clusters
Magellanic clouds
Techniques: spectroscopic
Astrophysics
spellingShingle Galaxies: star clusters
Magellanic Clouds
Techniques: spectroscopic
Calibration
Clouds
Continuum mechanics
Estimation
Galaxies
Interpolation
Spectroscopic analysis
Cluster formation
Galaxies: star clusters
Magellanic clouds
Techniques: spectroscopic
Astrophysics
Integrated spectral analysis of 18 concentrated star clusters in the Small Magellanic Cloud
topic_facet Galaxies: star clusters
Magellanic Clouds
Techniques: spectroscopic
Calibration
Clouds
Continuum mechanics
Estimation
Galaxies
Interpolation
Spectroscopic analysis
Cluster formation
Galaxies: star clusters
Magellanic clouds
Techniques: spectroscopic
Astrophysics
description We present in this study flux-calibrated integrated spectra in the range (3600-6800) Å for 18 concentrated SMC clusters. Cluster reddening values were estimated by interpolation between the extinction maps of Burstein & Heiles (1982, AJ, 87, 1165) and Schlegel et al. (1998, ApJ, 500, 525). The cluster parameters were derived from the template matching procedure by comparing the line strengths and continuum distribution of the cluster spectra with those of template cluster spectra with known parameters and from the equivalent width (EW) method. In this case, new calibrations were used together with diagnostic diagrams involving the sum of EWs of selected spectral lines. A very good agreement between ages derived from both methods was found. The final cluster ages obtained from the weighted average of values taken from the literature and the present measured ones range from 15 Mr (e.g. L 51) to 7 Gyr (K 3). Metal abundances have been derived for only 5 clusters from the present sample, while metallicity values directly averaged from published values for other 4 clusters have been adopted. Combining the present cluster sample with 19 additional SMC clusters whose ages and metal abundances were put onto a homogeneous scale, we analyse the age and metallicity distributions in order to explore the SMC star formation history and its spatial extent. By considering the distances of the clusters from the SMC centre instead of their projections onto the right ascension and declination axes, the present age-position relation suggests that the SMC inner disk could have been related to a cluster formation episode which reached the peak ∼2.5 Gyr ago. Evidence for an age gradient in the inner SMC disk is also presented. © ESO 2005.
title Integrated spectral analysis of 18 concentrated star clusters in the Small Magellanic Cloud
title_short Integrated spectral analysis of 18 concentrated star clusters in the Small Magellanic Cloud
title_full Integrated spectral analysis of 18 concentrated star clusters in the Small Magellanic Cloud
title_fullStr Integrated spectral analysis of 18 concentrated star clusters in the Small Magellanic Cloud
title_full_unstemmed Integrated spectral analysis of 18 concentrated star clusters in the Small Magellanic Cloud
title_sort integrated spectral analysis of 18 concentrated star clusters in the small magellanic cloud
publishDate 2005
url https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_00046361_v440_n1_p111_Piatti
http://hdl.handle.net/20.500.12110/paper_00046361_v440_n1_p111_Piatti
_version_ 1768545029459017728

Ejemplares similares