[Mg/Fe] ratios in the solar neighbourhood: Stellar yields and chemical evolution scenarios

Palla, Marco; Santos-Peral, P.; Recio–Blanco, A.; Matteuccí, F.

doi:10.1051/0004-6361/202142645

Cited by 19 publications

(7 citation statements)

References 121 publications

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“…The stars (∼ 55% are giants) cover a metallicity domain from ∼ -2.5 dex to +0.4 dex and seem to reproduce a flat trend in the metal-poor regime ([Fe/H] ≲ -1.0 dex) followed by a decrease in [Mg/Fe] even at supersolar metallicities ([Fe/H] > 0.0 dex). This behaviour is in perfect agreement with Galactic chemical evolution models (Chiappini et al 1997;Kobayashi et al 2006;Romano et al 2010;Spitoni et al 2020;Palla et al 2022). The sample seems to be dominated by Galactic disc stars, although metal-poor stars ([Fe/H] < -1.0 dex) are mostly halo stars.…”

Section: Magnesiumsupporting

confidence: 84%

Chemical characterisation of the X-shooter Spectral Library (XSL): [Mg/Fe] and [Ca/Fe] abundances

Santos-Peral

Sánchez-Blázquez

Vazdekis

et al. 2023

A&A

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Context. The X-shooter Spectral Library (XSL) is a large empirical stellar library used as a benchmark for the development of stellar population models. The inclusion of α-element abundances is crucial to disentangling the chemical evolution of any stellar system. Aims. The aim of this paper is to provide a catalogue of high-precision, accurate magnesium and calcium abundances from a wide variety of stars that are well distributed in the Hertzsprung-Russell (HR) diagram. Methods. We originally performed an analysis of the derived Mg and Ca abundances for medium-resolution spectra of 611 stars from the XSL Data Release 2. For this purpose, we used the GAUGUIN automated abundance estimation code to fit the ultravioletblue (UVB) and visible (VIS) spectra. We tested the consistency of the atmospheric parameters and chemical abundances with the Gaia DR3 and the AMBRE Project datasets. Results. We finally obtained precise [Mg/Fe] and [Ca/Fe] abundances for 192 and 217 stars, respectively, from which 174 stars have measurements in both elements. The stars cover a broad effective temperature range of 4000 < T eff < 6500 K, surface gravity of 0.3 < log(g) < 4.8 cm s −2 , and metallicity of -2.5 < [Fe/H] < +0.4 dex. We find an excellent agreement with the abundance estimates from the AMBRE:HARPS and the Gaia-RVS (Radial Velocity Spectrometer) analysis. Moreover, the resulting abundances reproduce a plateau in the metal-poor regime followed by a decreasing trend even at supersolar metallicities, as predicted by Galactic chemical evolution models. Conclusions. This catalogue is suitable for improving the modelling of evolutionary stellar population models with empirical α enhancements, which could significantly contribute to the analysis of external galaxies' abundances in the near future.

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Section: Magnesiumsupporting

confidence: 84%

Chemical characterisation of the X-shooter Spectral Library (XSL): [Mg/Fe] and [Ca/Fe] abundances

Santos-Peral

Sánchez-Blázquez

Vazdekis

et al. 2023

A&A

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“…Several previous OCs catalogues also suggested the possibility of a change in the slope between inner and outer disk (e.g., Yong et al 2012;Magrini et al 2023), however, uncertainties affecting individual distances, the limited number of objects located in the outermost regions, and the possibility that the change in the slope was driven by an age effect hampered firm conclusions. In passing, we also notice that the different scenario in the modeling of radial gradients have, within the two-infall paradigm, a marginal impact on the fit of the observed α-bimodality (e.g., Spitoni et al 2019Spitoni et al , 2021Palla et al 2022). The stellar data adopted for such analyses have Galactocentric distances smaller than 12-14 kpc, as those from outer regions are significant severely limited in number (see, e.g., Spitoni et al 2021).…”

Section: Comparison Between Theory and Observationsmentioning

confidence: 89%

A new and Homogeneous metallicity scale for Galactic classical Cepheids

Silva

Crestani

Bono

et al. 2022

A&A

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Context. Classical Cepheids are the most popular distance indicators and tracers of young stellar populations. The key advantage is that they are bright and they can be easily identified in Local Group and Local Volume galaxies. Their evolutionary and pulsation properties depend on their chemical abundances. Aims. The main aim of this investigation is to perform a new and accurate abundance analysis of 20 calibrating Galactic Cepheids. We used high spectral resolution (R ~ 40 000–115 000) and high S/N spectra (~400), covering the entire pulsation cycle. Methods. We focused our attention on plausible systematics that would affect the estimate of atmospheric parameters and elemental abundances along the pulsation cycle. We cleaned the line list by using atomic transition parameters based on laboratory measurements and by removing lines that are either blended or that display abundance variations along the pulsation cycle. Results. The spectroscopic approach we developed brings forward small dispersions in the variation of the atmospheric parameters (σ(Teff) ~ 50 K, σ(log g) ~ 0.2 dex, and σ(ξ) ~ 0.2 kms−1) as well as in the abundance of both iron (≲0.05 dex) and α elements (≲0.10 dex) over the entire pulsation cycle. We also provide new and accurate effective temperature templates by splitting the calibrating Cepheids into four different period bins, ranging from short to long periods. For each period bin, we performed an analytical fit with Fourier series providing θ = 5040/Teff as a function of the pulsation phase. Conclusions. The current findings are a good viaticum for tracing the chemical enrichment of the Galactic thin disk by using classical Cepheids as a fundamental stepping stone for further investigations into the more metal-poor regime that is typical of Magellanic Cepheids.

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“…François et al 2004;Romano et al 2010;Côté et al 2017;Prantzos et al 2018). This set of yields has been widely used in the literature (Cescutti et al 2007(Cescutti et al , 2022Spitoni et al 2014Spitoni et al , 2015Spitoni et al , 2017Spitoni et al , 2019bMott et al 2013;Vincenzo et al 2019;Palla et al 2022) and has been shown to be able to reproduce the main features of the solar neighbourhood.…”

Section: Fronçois Et Al Yields Collectionmentioning

confidence: 99%

“…The new AMBRE:HARPS data were reproduced by Palla et al (2022) with chemical evolution models characterised by peculiar histories of SF, such as the two-infall model with a significant delay. Xiang & Rix (2022), analysing subgiant stars in LAMOST, confirmed that the stellar age-metallicity distribution splits into two almost disjointed parts, separated at age 8 Gyr.…”

Section: Introductionmentioning

confidence: 95%

Beyond the two-infall model

Spitoni

Recio–Blanco

Laverny

et al. 2023

A&A

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Context. The recent Gaia Data Release 3 (DR3) represents an unparalleled revolution in Galactic archaeology, providing numerous radial velocities and chemical abundances for millions of stars as well as all-sky coverage. Aims We present a new chemical evolution model for the Galactic disc components (high- and low- α sequence stars) designed to reproduce the new abundance ratios provided by the General Stellar Parametriser-spectroscopy module for the Gaia DR3 and constrained by the detailed star formation (SF) histories for both the thick and thin disc stars inferred from previous Gaia releases. Methods. Sophisticated modelling based on previous Gaia releases have found evidence for narrow episodes of enhanced SF inferred in recent time. Additionally, Gaia DR3 indicated the presence of young (massive) low-α disc stars that show evidence of a recent chemical impoverishment in several elements. In order to reproduce these observables, we propose a new chemical evolution model in which the low-α sequence is generated by two distinct infall episodes. Hence, in this study we compare Gaia DR3 chemical abundances with the predictions of a three-infall chemical evolution model for the high- and low-α components. Results The proposed three-infall chemical evolution model nicely reproduces the main features of the abundance ratio [X/Fe] versus [M/H] (X=Mg, Si, Ca, Ti, α) of Gaia DR3 stars in different age bins for the considered α elements. Moreover, the most recent gas infall – which started ∼2.7 Gyr ago – allowed us to predict accurately predict the Gaia DR3 young population which has experienced a recent chemical impoverishment. Conclusions. We extended previous chemical evolution models designed to reproduce APOGEE and APOKASC data in order to predict new Gaia DR3 chemical abundances. To this aim, we proposed a three-infall chemical evolution model to better trace both (i) the young population in Gaia DR3 with evidence of chemical impoverishment and (ii) the SF history from previous Gaia releases.

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[Mg/Fe] ratios in the solar neighbourhood: Stellar yields and chemical evolution scenarios

Cited by 19 publications

References 121 publications

Chemical characterisation of the X-shooter Spectral Library (XSL): [Mg/Fe] and [Ca/Fe] abundances

Chemical characterisation of the X-shooter Spectral Library (XSL): [Mg/Fe] and [Ca/Fe] abundances

A new and Homogeneous metallicity scale for Galactic classical Cepheids

Beyond the two-infall model

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