ASteCA: Automated Stellar Cluster Analysis

Perren, G. I.; Vazquez, R. A.; Piatti, Andrés E.

doi:10.1051/0004-6361/201424946

Cited by 112 publications

(135 citation statements)

References 141 publications

(113 reference statements)

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“…It provides input for population synthesis models to study resolved and unresolved star clusters and galaxies (e.g. Perren, Vázquez & Piatti 2015;Gutkin, Charlot & Bruzual 2016;Chevallard & Charlot 2016), and offers reliable models for many other field of studies, such as to derive black hole mass when observing gravitational waves (e.g. Spera, Mapelli & Bressan 2015;Belczynski et al 2016), to get host star parameters for exoplanets (Santos et al 2013;Maldonado et al 2015, etc.…”

Section: Introductionmentioning

confidence: 99%

New parsec data base of α-enhanced stellar evolutionary tracks and isochrones – I. Calibration with 47 Tuc (NGC 104) and the improvement on RGB bump

Bressan

Marigo

et al. 2018

Monthly Notices of the Royal Astronomical Society

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Precise studies on the Galactic bulge, globular cluster, Galactic halo and Galactic thick disk require stellar models with α enhancement and various values of helium content. These models are also important for extra-Galactic population synthesis studies. For this purpose we complement the existing PARSEC models, which are based on the solar partition of heavy elements, with α-enhanced partitions. We collect detailed measurements on the metal mixture and helium abundance for the two populations of 47 Tuc (NGC 104) from the literature, and calculate stellar tracks and isochrones with these α-enhanced compositions. By fitting the precise color-magnitude diagram with HST ACS/WFC data, from low main sequence till horizontal branch, we calibrate some free parameters that are important for the evolution of low mass stars like the mixing at the bottom of the convective envelope. This new calibration significantly improves the prediction of the RGB bump brightness. Comparison with the observed RGB and HB luminosity functions also shows that the evolutionary lifetimes are correctly predicted. As a further result of this calibration process, we derive the age, distance modulus, reddening, and the red giant branch mass loss for 47 Tuc. We apply the new calibration and α-enhanced mixtures of the two 47 Tuc populations ( [α/Fe] ∼0.4 and 0.2) to other metallicities. The new models reproduce the RGB bump observations much better than previous models. This new PARSEC database, with the newly updated α-enhanced stellar evolutionary tracks and isochrones, will also be part of the new stellar products for Gaia .

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Section: Introductionmentioning

confidence: 99%

New parsec data base of α-enhanced stellar evolutionary tracks and isochrones – I. Calibration with 47 Tuc (NGC 104) and the improvement on RGB bump

Bressan

Marigo

et al. 2018

Monthly Notices of the Royal Astronomical Society

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“…We give in Sect. 2.9 of Perren et al (2015, hereafter Paper I) a non-exhaustive list of articles in which these methods were employed. Still, by-eye studies continue to be used.…”

Section: Introductionmentioning

confidence: 99%

Astrophysical properties of star clusters in the Magellanic Clouds homogeneously estimated by ASteCA

Perren

Piatti

Vazquez

2017

A&A

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Aims. We seek to produce a homogeneous catalog of astrophysical parameters of 239 resolved star clusters, located in the Small and Large Magellanic Clouds, observed in the Washington photometric system. Methods. The cluster sample was processed with the recently introduced Automated Stellar Cluster Analysis (ASteCA) package, which ensures both an automatized and a fully reproducible treatment, together with a statistically based analysis of their fundamental parameters and associated uncertainties. The fundamental parameters determined for each cluster with this tool, via a color-magnitude diagram (CMD) analysis, are metallicity, age, reddening, distance modulus, and total mass. Results. We generated a homogeneous catalog of structural and fundamental parameters for the studied cluster sample and performed a detailed internal error analysis along with a thorough comparison with values taken from 26 published articles. We studied the distribution of cluster fundamental parameters in both Clouds and obtained their age-metallicity relationships. Conclusions. The ASteCA package can be applied to an unsupervised determination of fundamental cluster parameters, which is a task of increasing relevance as more data becomes available through upcoming surveys.

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“…The code includes functions to perform cluster structure analysis, luminosity function curves, integrated colour estimates statistically cleaned from field star contamination, a Bayesian membership assignment algorithm, and a synthetic clusterbased best isochrone matching method to simultaneously estimate clusters' properties (age, metallicity, distance, reddening, mass and binarity). Perren, Vázquez & Piatti (2015) showed that it does not introduce any biases or new correlations between the various derived cluster parameter values.…”

Section: Synthetic Colour-magnitude Diagramsmentioning

confidence: 95%

New age–metallicity diagnostic diagram for the Washington photometric system

Piatti

Perren

2015

Monthly Notices of the Royal Astronomical Society

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The age calibration of the Washington δT 1 index is mainly used to estimate ages of star clusters older than 1 Gyr, no age-metallicity degeneracy effect is considered. We have profusely exploited synthetic T 1 versus C − T 1 colour magnitude diagrams aiming at exploring the intrinsic behaviour of the δT 1 index. The analysis shows that δT 1 varies with age and metal content as well. In general, the dependence on age weakens for ages greater than ∼ 6 Gyr, and results even less sensitive to age as the metallicity decreases. For ages younger than ∼ 5 Gyr δT 1 shows a strong correlation with both age and metallicity. The δC index -defined as δT 1 for the C passband-is also a combined measurement of age and metallicity. We introduce a new age-metallicity diagnostic diagram, δT 1 versus δC -δT 1 , which has shown the ability of unambiguously providing age and metallicity estimates, simultaneously. The new procedure allows to derive ages from 1 up to 13 Gyr and metallicities [Fe/H] from -2.0 up to +0.5 dex, and is independent of the cluster reddening and distance modulus. It does solve the constraints found in the δT 1 index and surpasses the performance of the standard giant branch metallicity method. All these features make the diagnostic diagram a powerful tool for estimating accurate ages as well as metallicities.

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ASteCA: Automated Stellar Cluster Analysis

Cited by 112 publications

References 141 publications

New parsec data base of α-enhanced stellar evolutionary tracks and isochrones – I. Calibration with 47 Tuc (NGC 104) and the improvement on RGB bump

New parsec data base of α-enhanced stellar evolutionary tracks and isochrones – I. Calibration with 47 Tuc (NGC 104) and the improvement on RGB bump

Astrophysical properties of star clusters in the Magellanic Clouds homogeneously estimated by ASteCA

New age–metallicity diagnostic diagram for the Washington photometric system

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