Reddening and age for 13 southern Galactic open clusters determined
from integrated spectra

Ahumada, A. V.; Clariá, J. J.; Bica, E.; Dutra, Carlos Maximiliano; Torres, M. C.

doi:10.1051/0004-6361:20011133

Cited by 18 publications

(39 citation statements)

References 28 publications

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“…Star cluster templates are also useful to derive parameters of unstudied clusters, e.g. Galactic open clusters (Santos & Bica 1993;Piatti et al 1999;Ahumada et al 2000Ahumada et al , 2001.…”

Section: Introductionmentioning

confidence: 99%

Dating star clusters in the Small Magellanic Cloud by means of integrated spectra

Ahumada

Clariá

Bica

et al. 2002

A&A

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Abstract. In this study flux-calibrated integrated spectra in the range (3600-6800) Å are presented for 16 concentrated star clusters in the Small Magellanic Cloud (SMC), approximately half of which constitute unstudied objects. We have estimated ages and foreground interstellar reddening values from the comparison of the line strengths and continuum distribution of the cluster spectra with those of template cluster spectra with known parameters. Most of the sample clusters are young blue clusters (6-50 Myr), while L 28, NGC 643 and L 114 are found to be intermediate-age clusters (1-6 Gyr). One well known SMC cluster (NGC 416) was observed for comparison purposes. The sample includes clusters in the surroundings and main body of the SMC, and the derived foreground reddening values are in the range 0.00 ≤ E(B − V) ≤ 0.15. The present data also make up a cluster spectral library at SMC metallicity.

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Section: Introductionmentioning

confidence: 99%

Dating star clusters in the Small Magellanic Cloud by means of integrated spectra

Ahumada

Clariá

Bica

et al. 2002

A&A

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“…In all cases, the ages and foreground interstellar reddening values were determined using equivalent widths of the Balmer absorption lines and comparing the observed spectra with template spectra. The present cluster sample complements previous ones (Ahumada et al 2000(Ahumada et al , 2001, in an effort to gather a spectral library with several clusters per age interval.…”

Section: Discussionmentioning

confidence: 99%

“…The present cluster sample, together with those previously analised using the same technique (Ahumada et al 2000(Ahumada et al , 2001, represents a statistically meaningful sample of 42 open clusters of the Galactic disc. We considered it interesting to compare the parameters determined via integrated spectroscopy for these 42 clusters with those of well-known clusters located in similar regions of the Galactic disc.…”

Section: Comparison With Known Open Clusters Located In the Same Galamentioning

confidence: 91%

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Integrated spectral properties of 22 small angular diameter galactic open clusters

Ahumada

Clariá

Bica

2007

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Aims. Flux-calibrated integrated spectra of a sample of 22 Galactic open clusters of small angular diameter are presented. With one exception (ESO 429-SC2), all objects have Galactic longitudes in the range 208• < l < 33• . The spectra cover the range ≈3600−6800 Å, with a resolution of ≈14 Å. The properties of the present cluster sample are compared with those of well-studied clusters located in two 90• sectors, centred at l = 257• and l = 347• . The dissolution rate of Galactic open clusters in these two sectors is examined. Methods. Using the equivalent widths of the Balmer lines and comparing line intensities and continuum distribution of the cluster spectra with those of template cluster spectra with known properties, we derive both foreground reddening values and ages. Thus, we provide information independent of that determined through colour-magnitude diagrams.

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“…The analysis method is the same as that used by Ahumada et al (2001). For the sake of illustrating the method, we show in Fig.…”

Section: Methods Of Analysismentioning

confidence: 99%

Near infrared photometric and optical spectroscopic study of 22 low mass star clusters embedded in nebulae

Soares¹,

Bica²,

Ahumada³

et al. 2007

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Aims. Among the star clusters in the Galaxy, those embedded in nebulae represent the youngest group, which has only recently been explored. The analysis of a sample of 22 candidate embedded stellar systems in reflection nebulae and/or HII environments is presented. Methods. We employed optical spectroscopic observations of stars in the directions of the clusters carried out at CASLEO (Argentina) together with near infrared photometry from the 2MASS catalogue. Our analysis is based on source surface density, colour−colour diagrams and on theoretical pre-main sequence isochrones. We take into account the field star contamination by carrying out a statistical subtraction. Results. The studied objects have the characteristics of low mass systems. We derive their fundamental parameters. Most of the cluster ages are younger than 2 Myr. The studied embedded stellar systems in reflection nebulae and/or HII region complexes do not have stars of spectral types earlier than B. The total stellar masses locked in the clusters are in the range 20−220 M . They are found to be gravitationally unstable and are expected to dissolve in a timescale of a few Myr.

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Reddening and age for 13 southern Galactic open clusters determined from integrated spectra

Cited by 18 publications

References 28 publications

Dating star clusters in the Small Magellanic Cloud by means of integrated spectra

Dating star clusters in the Small Magellanic Cloud by means of integrated spectra

Integrated spectral properties of 22 small angular diameter galactic open clusters

Near infrared photometric and optical spectroscopic study of 22 low mass star clusters embedded in nebulae

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