Integrated spectroscopic study of 7 star clusters in the Small Magellanic Cloud

Talavera, M. L.; Ahumada, A. V.; Santos, J. F. C.; Clariá, J. J.; Bica, E.; Parisi, M. C.; Torres, M. C.

doi:10.1002/asna.200911299

Cited by 11 publications

(11 citation statements)

References 35 publications

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“…The age differences larger than 0.4 (black filled squares) represent ∼ 55 per cent of the cluster sample. This result suggests that the integrated spectroscopy matching technique should be used with caution, since it particularly might misguide when applying it in studies of stellar population synthesis in galaxies (Ahumada, Clariá & Bica 2007;Palma et al 2008b;Talavera et al 2010;Minniti et al 2014).…”

Section: Scope Of the Integrated Spectroscopymentioning

confidence: 99%

Bruck 88: a young star cluster with an old age resemblance in the outskirts of the Small Magellanic Cloud

Piatti

2014

Monthly Notices of the Royal Astronomical Society

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We present spectroscopic and photometric results for the Small Magellanic Cloud (SMC) cluster Bruck 88. From the comparison of the cluster integrated spectrum with template cluster spectra we found that the Milky Way globular cluster template spectra are the ones which best resemble it. However, the extracted cluster colour magnitude diagram reveals that Bruck 88 is a young cluster (log(t) = 8.1 ± 0.1). The derived cluster age is compatible with the presence of a Bright Red Giant (BRG) star located ∼ 2.6 arcsec in the sky from the cluster centre. We serendipitously observed HW 33, a star cluster located ≈ 3 arcmin to the south-east from Bruck 88. We obtained for the cluster the same age than Bruck 88 and surprisingly, a BRG star located within the cluster radius also appears to be compatible with the cluster age. We estimated the MK type of the BRG star in the Bruck 88 field to be in the range G9 II/Ib K1 III. By combining the spectrum of a star within this MK type range with a 100-150 Myr template cluster integrated spectrum, we found that a proportion 85/15 in the sense BRG/template results in a spectrum which best resembles that of Bruck 88. This result confirms that a BRG star dominates the cluster integrated spectrum, so that it causes the globular cluster appearance of its integrated light.

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Section: Scope Of the Integrated Spectroscopymentioning

confidence: 99%

Bruck 88: a young star cluster with an old age resemblance in the outskirts of the Small Magellanic Cloud

Piatti

2014

Monthly Notices of the Royal Astronomical Society

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“…Following the procedure described by Clariá (2008), reddenings and ages of more than 50 small angular diameter Galactic OCs have been estimated (Ahumada et al 2000(Ahumada et al , 2001(Ahumada et al , 2007(Ahumada et al , 2010Palma et al 2008a). Although metallicity has an impact on the spectra of OCs older than ∼ 0.5 Gyr, the metallicity features in the spectra of these clusters in the 3600 Å < λ < 7400 Å spectral range are relatively weak (see, e.g., Bica & Alloin 1986), so they do not significantly affect the determination of the two derived parameters.…”

Section: Library Of Template Spectramentioning

confidence: 99%

Fast Integrated Spectra Analyzer: A New Computational Tool for Age and Reddening Determination of Small Angular Diameter Open Clusters

Benítez-Llambay¹,

Clariá²,

Piatti³

2012

Publications of the Astronomical Society of the Pacific

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We present a new algorithm called 'Fast Integrated Spectra Analyzer" (FISA) that permits fast and reasonably accurate age and reddening determinations for small angular diameter open clusters by using their integrated spectra in the (3600-7400)Å range and currently available template spectrum libraries. This algorithm and its implementation help to achieve astrophysical results in shorter times than from other methods. A brief review is given of the integrated spectroscopic technique applied to the study of open clusters as well as the basic assumptions that justify its use. We describe the numerical algorithm employed in detail, show examples of its application, and provide a link to the code. Our method has successfully been applied to integrated spectroscopy of open clusters, both in the Galaxy and in the Magellanic Clouds, to determine ages and reddenings.

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“…Integrated-light spectra of star clusters have proven to be accurate tools for studying extragalactic clusters for which spatially resolved data is not available (Ahumada et al 2002;Puzia et al 2005Puzia et al , 2006Santos et al 2006;Palma et al 2008;Talavera et al 2010;Cid Fernandes & Gonzalez Delgado 2010;Asa'd et al 2013;Asa'd 2014;Chilingarian & Asa'd 2018). In this work we aim to address the question: To what extent can integrated-light spectra be used to identify age spreads at different ages?…”

Section: Introductionmentioning

confidence: 99%

On the Precision of Full-spectrum Fitting of Stellar Populations. III. Identifying Age Spreads

Asa'd,

Goudfrooij,

As'ad

et al. 2021

Preprint

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In this third paper of a series on the precision of obtaining ages of stellar populations using the full spectrum fitting technique, we examine the precision of this technique in deriving possible age spreads within a star cluster. We test how well an internal age spread can be resolved as a function of cluster age, population mass fraction, and signal-to-noise (S/N) ratio. For this test, the two ages (Age (SSP 1 ) and Age (SSP 2 )) are free parameters along with the mass fraction of SSP 1 . We perform the analysis on 118,800 mock star clusters covering all ages in the range 6.8 < log (age/yr) < 10.2, with mass fractions from 10% to 90% for two age gaps (0.2 dex and 0.5 dex). Random noise is added to the model spectra to achieve S/N ratios between 50 to 100 per wavelength pixel. We find that the mean of the derived Age (SSP 1 ) generally matches the real Age (SSP 1 ) to within 0.1 dex up to ages around log (age/yr) = 9.5. The precision decreases for log (age/yr) > 9.6 for any mass fraction or S/N, due to the similarity of SED shapes for those ages. In terms of the recovery of age spreads, we find that the derived age spreads are often larger than the real ones, especially for log(age/yr) < ∼ 8.0 and high mass fractions of SSP 1 . Increasing the age gap in the mock clusters improves the derived parameters, but Age (SSP 2 ) is still overestimated for the younger ages.

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Integrated spectroscopic study of 7 star clusters in the Small Magellanic Cloud

Cited by 11 publications

References 35 publications

Bruck 88: a young star cluster with an old age resemblance in the outskirts of the Small Magellanic Cloud

Bruck 88: a young star cluster with an old age resemblance in the outskirts of the Small Magellanic Cloud

Fast Integrated Spectra Analyzer: A New Computational Tool for Age and Reddening Determination of Small Angular Diameter Open Clusters

On the Precision of Full-spectrum Fitting of Stellar Populations. III. Identifying Age Spreads

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