A Large Stellar Evolution Database for Population Synthesis Studies. Iv. Integrated Properties and Spectra

Percival, S. M.; Salaris, Maurizio; Cassisi, S.; Pietrinferni, A.

doi:10.1088/0004-637x/690/1/427

Cited by 99 publications

(102 citation statements)

References 63 publications

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“…In support of our approach we also highlight that the use of [α/Fe] as a single parameter involving a set of elements is also justified by the findings of Johansson et al (2012), who find that the correlations of [O/Fe], [Mg/Fe], [C/Fe] with velocity dispersion are identical for ETGs. In general, models capable of predicting the effects of α-elements on the full optical spectrum of stellar populations are starting to become less rare, see Coelho et al (2007), Koleva et al (2008b), Walcher et al (2009), Percival et al (2009, Vazdekis et al (2011), Conroy & van Dokkum (2012, Prugniel & Koleva (2012), Vazdekis et al (2015).…”

Section: Stellar Population Models and Fitting Proceduresmentioning

confidence: 99%

Abundance patterns in early-type galaxies: is there a “knee” in the [Fe/H] vs. [α/Fe] relation?

Walcher

Coelho

Gallazzi

et al. 2015

A&A

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Early-type galaxies (ETGs) are known to be enhanced in α elements, in accordance with their old ages and short formation timescales. In this contribution we aim to resolve the enrichment histories of ETGs. This means we study the abundance of Fe ([Fe/H] We then analyze a spectroscopic sample of 2286 early-type galaxies from the SDSS selected to be ETGs. We separate out those galaxies for which the abundance of iron in stars grows throughout the lifetime of the galaxy, i.e. in which [Fe/H] o < [Fe/H] i . We call those consistent with self-enrichment, while the others must have experienced some mergers or significant gas accretion. We confirm earlier work where the [Fe/H] and [α/Fe] parameters are correlated with the mass and velocity dispersion of ETGs. We emphasize that the strongest relation is between [α/Fe] and age. This relation falls into two regimes, one with a steep slope for old galaxies and one with a shallow slope for younger ETGs. The vast majority of ETGs in our sample do not show the "knee" in the plot of [Fe/H] vs. [α/Fe] commonly observed in local group galaxies. This implies that for the vast majority of ETGs, the stars younger than 9.5 Gyr are likely to have been accreted or formed from accreted gas. The properties of the intermediate-age stars in accretion-dominated ETGs indicate that mass growth through late (minor) mergers in ETGs is dominated by galaxies with low [Fe/H] and low [α/Fe]. The method of reconstructing the stellar enrichment histories of ETGs introduced in this paper promises to constrain the star formation and mass assembly histories of large samples of galaxies in a unique way.

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Section: Stellar Population Models and Fitting Proceduresmentioning

confidence: 99%

Abundance patterns in early-type galaxies: is there a “knee” in the [Fe/H] vs. [α/Fe] relation?

Walcher

Coelho

Gallazzi

et al. 2015

A&A

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“…These libraries contain a large number of stars (usually above 1000) and they differ from each other in terms of resolution and wavelength coverage. They are frequently used for stellar population synthesis models and galactic studies (e.g., Vazdekis et al 2012;Percival et al 2009;Zhang et al 2005, and references therein) and for calibration or validation of methods that determine stellar parameters from stellar spectra (e.g. Allende Prieto et al 2008b;Koleva et al 2009;Wu et al 2011).…”

Section: Introductionmentioning

confidence: 99%

TheGaiaFGK benchmark stars

Blanco-Cuaresma¹,

Soubiran²,

Jofré³

et al. 2014

A&A

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174

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Context. An increasing number of high-resolution stellar spectra is available today thanks to many past and ongoing spectroscopic surveys. Consequently, numerous methods have been developed to perform an automatic spectral analysis on a massive amount of data. When reviewing published results, biases arise and they need to be addressed and minimized. Aims. We are providing a homogeneous library with a common set of calibration stars (known as the Gaia FGK benchmark stars) that will allow us to assess stellar analysis methods and calibrate spectroscopic surveys. Methods. High-resolution and signal-to-noise spectra were compiled from different instruments. We developed an automatic process to homogenize the observed data and assess the quality of the resulting library. Results. We built a high-quality library that will facilitate the assessment of spectral analyses and the calibration of present and future spectroscopic surveys. The automation of the process minimizes the human subjectivity and ensures reproducibility. Additionally, it allows us to quickly adapt the library to specific needs that can arise from future spectroscopic analyses.

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“…Brodie & Huchra 1990) to those which perform the simultaneous χ 2 -minimisation of a large number of spectral indices (see, e.g., Proctor et al 2004). Nevertheless, both photometric and spectroscopic methods are dependent on the accurate modelling of simple stellar populations (SSPs, see, Table 4 is available in electronic form at http://www.aanda.org e.g., Bruzual & Charlot 2003;Le Borgne et al 2004;Delgado et al 2005;Maraston 2005;Coelho et al 2007;Percival et al 2009;Lee et al 2009;Conroy & Gunn 2010;Vazdekis et al 2010).…”

Section: Introductionmentioning

confidence: 99%

Full spectral fitting of Milky Way and M 31 globular clusters: ages and metallicities

Cezario

Coelho

Alves-Brito

et al. 2012

A&A

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Context. The formation and evolution of disk galaxies are long standing questions in astronomy. Understanding the properties of globular cluster systems can lead to important insights on the evolution of its host galaxy. Aims. We aim to obtain the stellar population parameters -age and metallicity -of a sample of M 31 and Galactic globular clusters. Studying their globular cluster systems is an important step towards understanding their formation and evolution in a complete way. Methods. Our analysis employs a modern pixel-to-pixel spectral fitting technique to fit observed integrated spectra to updated stellar population models. By comparing observations to models we obtain the ages and metallicities of their stellar populations. We apply this technique to a sample of 38 globular clusters in M 31 and to 41 Galactic globular clusters, used as a control sample. Results. Our sample of M 31 globular clusters spans ages from 150 Myr to the age of the Universe. Metallicities [Fe/H] range from -2.2 dex to the solar value. The age-metallicity relation obtained can be described as having two components: an old population with a flat age-[Fe/H] relation, possibly associated with the halo and/or bulge, and a second one with a roughly linear relation between age and metallicity, higher metallicities corresponding to younger ages, possibly associated with the M 31 disk. While we recover the very well known Galactic GC metallicity bimodality, our own analysis of M 31's metallicity distribution function (MDF) suggests that both GC systems cover basically the same [Fe/H] range yet M 31's MDF is not clearly bimodal. These results suggest that both galaxies experienced different star formation and accretion histories.

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A Large Stellar Evolution Database for Population Synthesis Studies. Iv. Integrated Properties and Spectra

Cited by 99 publications

References 63 publications

Abundance patterns in early-type galaxies: is there a “knee” in the [Fe/H] vs. [α/Fe] relation?

Abundance patterns in early-type galaxies: is there a “knee” in the [Fe/H] vs. [α/Fe] relation?

TheGaiaFGK benchmark stars

Full spectral fitting of Milky Way and M 31 globular clusters: ages and metallicities

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