<i>Gaia</i>FGK benchmark stars: Effective temperatures and surface gravities

Heiter, U.; Jofré, P.; Gustafsson, B.; Korn, A. J.; Soubiran, C.; Thévenin, F.

doi:10.1051/0004-6361/201526319

Cited by 287 publications

(464 citation statements)

References 265 publications

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“…7 (right panel) that the derived lithium values are once again consistent with the AMBRE/Li abundances. The atmospheric parameters that are derived by Heiter et al (2015) and Jofré et al (2014b) are very similar to the independent determinations by the AMBRE project. These comparisons again confirm that the lithium abundances of the AMBRE/Li catalogue are reliable for a scientific exploitation.…”

Section: Lithium Abundance Of the Gaia-benchmark Starssupporting

confidence: 81%

“…Indeed, when comparing the AMBRE/Li abundances with the lithium abundances derived using the atmospheric parameters from the literature (middle panel), the agreement becomes very satisfactory with no bias and a smaller dispersion σ = 0.14 dex. Finally, when adopting the effective temperature and surface gravity of Heiter et al (2015) and metallicity of Jofré et al (2014b), we see in Fig. 7 (right panel) that the derived lithium values are once again consistent with the AMBRE/Li abundances.…”

Section: Lithium Abundance Of the Gaia-benchmark Starssupporting

confidence: 76%

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The AMBRE project: Constraining the lithium evolution in the Milky Way

Guiglion

Laverny

Recio–Blanco

et al. 2016

A&A

140

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Context. The chemical evolution of lithium in the Milky Way represents a major problem in modern astrophysics. Indeed, lithium is, on the one hand, easily destroyed in stellar interiors, and, on the other hand, produced at some specific stellar evolutionary stages that are still not well constrained. Aims. The goal of this paper is to investigate the lithium stellar content of Milky Way stars in order to put constraints on the lithium chemical enrichment in our Galaxy, in particular in both the thin and thick discs. Methods. Thanks to high-resolution spectra from the ESO archive and high quality atmospheric parameters, we were able to build a massive and homogeneous catalogue of lithium abundances for 7 300 stars derived with an automatic method coupling, a synthetic spectra grid, and a Gauss-Newton algorithm. We validated these lithium abundances with literature values, including those of the Gaia benchmark stars. Results. In terms of lithium galactic evolution, we show that the interstellar lithium abundance increases with metallicity by 1 dex from [M/H] = −1 dex to +0.0 dex. Moreover, we find that this lithium ISM abundance decreases by about 0.5 dex at super-solar metalllicity. Based on a chemical separation, we also observed that the stellar lithium content in the thick disc increases rather slightly with metallicity, while the thin disc shows a steeper increase. The lithium abundance distribution of α-rich, metal-rich stars has a peak at ALi ∼ 3 dex. Conclusions. We conclude that the thick disc stars suffered of a low lithium chemical enrichment, showing lithium abundances rather close to the Spite plateau while the thin disc stars clearly show an increasing lithium chemical enrichment with the metallicity, probably thanks to the contribution of low-mass stars.

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Section: Lithium Abundance Of the Gaia-benchmark Starssupporting

confidence: 81%

Section: Lithium Abundance Of the Gaia-benchmark Starssupporting

confidence: 76%

The AMBRE project: Constraining the lithium evolution in the Milky Way

Guiglion

Laverny

Recio–Blanco

et al. 2016

A&A

140

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“…For the RVS, a compilation of radial-velocity standards was undertaken (Crifo et al 2010;Soubiran et al 2013), while for the solar system object processing, data on solar analogues had to be compiled to calibrate the interpretation of the Gaia photometry. A set of ∼30 Gaia FGK benchmark stars have been extensively studied to provide a reference for the astrophysical parameter inference system Blanco-Cuaresma et al 2014;Heiter et al 2015;Jofré et al 2015;Hawkins et al 2016). One of the largest auxiliary observation programmes is the GBOT effort already mentioned in Sect.…”

Section: Simulations Supplementary Data and Observations Data Publimentioning

confidence: 99%

TheGaiamission

Prusti¹,

Bruijne²,

Brown³

et al. 2016

A&A

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5,534

1,139

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Gaia is a cornerstone mission in the science programme of the European Space Agency (ESA). The spacecraft construction was approved in 2006, following a study in which the original interferometric concept was changed to a direct-imaging approach. Both the spacecraft and the payload were built by European industry. The involvement of the scientific community focusses on data processing for which the international Gaia Data Processing and Analysis Consortium (DPAC) was selected in 2007. Gaia was launched on 19 December 2013 and arrived at its operating point, the second Lagrange point of the Sun-Earth-Moon system, a few weeks later. The commissioning of the spacecraft and payload was completed on 19 July 2014. The nominal five-year mission started with four weeks of special, ecliptic-pole scanning and subsequently transferred into full-sky scanning mode. We recall the scientific goals of Gaia and give a description of the as-built spacecraft that is currently (mid-2016) being operated to achieve these goals. We pay special attention to the payload module, the performance of which is closely related to the scientific performance of the mission. We provide a summary of the commissioning activities and findings, followed by a description of the routine operational mode. We summarise scientific performance estimates on the basis of in-orbit operations. Several intermediate Gaia data releases are planned and the data can be retrieved from the Gaia Archive, which is available through the Gaia home page.

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“…For example, the T eff has been determined through both photometric (e.g. Alonso et al 1996a;Nissen et al 2002;Ramírez & Meléndez 2005;Jonsell et al 2005;Masana et al 2006;Reddy et al 2006;González Hernández & Bonifacio 2009;Casagrande et al 2010Casagrande et al , 2011Ishigaki et al 2012) and spectroscopic (e.g. Gratton et al 1996Gratton et al , 2000Gratton et al , 2003Nissen & Schuster 1997;Mishenina et al 2000;Fulbright 2000;Sousa et al 2011) means.…”

Section: Samplementioning

confidence: 99%

“…Gratton et al 2000;Gehren et al 2004;Jonsell et al 2005). However, in some cases the Fe ionisation balance Fulbright 2000;Sousa et al 2011;Ishigaki et al 2012) or Mg-triplet wing fitting (e.g. Mashonkina & Gehren 2000) has been used.…”

Section: Samplementioning

confidence: 99%

GaiaFGK benchmark stars: new candidates at low metallicities

Hawkins

Jofré

Heiter

et al. 2016

A&A

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Context. We have entered an era of large spectroscopic surveys in which we can measure, through automated pipelines, the atmospheric parameters and chemical abundances for large numbers of stars. Calibrating these survey pipelines using a set of "benchmark stars" in order to evaluate the accuracy and precision of the provided parameters and abundances is of utmost importance. The recent proposed set of Gaia FGK benchmark stars has up to five metal-poor stars but no recommended stars within −2.0 < [Fe/H] < −1.0 dex. However, this metallicity regime is critical to calibrate properly. Aims. In this paper, we aim to add candidate Gaia benchmark stars inside of this metal-poor gap. We began with a sample of 21 metalpoor stars which was reduced to 10 stars by requiring accurate photometry and parallaxes, and high-resolution archival spectra. Methods. The procedure used to determine the stellar parameters was similar to the previous works in this series for consistency. The difference was to homogeneously determine the angular diameter and effective temperature (T eff ) of all of our stars using the Infrared Flux Method utilizing multi-band photometry. The surface gravity (log g) was determined through fitting stellar evolutionary tracks. The [Fe/H] was determined using four different spectroscopic methods fixing the T eff and log g from the values determined independent of spectroscopy. Results. We discuss, star-by-star, the quality of each parameter including how it compares to literature, how it compares to a spectroscopic run where all parameters are free, and whether Fe i ionisation-excitation balance is achieved.Conclusions. From the 10 stars, we recommend a sample of five new metal-poor benchmark candidate stars which have consistent T eff , log g, and [Fe/H] determined through several means. These stars, which are within −1.3 < [Fe/H] < −1.0, can be used for calibration and validation purpose of stellar parameter and abundance pipelines and should be of highest priority for future interferometric studies.

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GaiaFGK benchmark stars: Effective temperatures and surface gravities

Cited by 287 publications

References 265 publications

The AMBRE project: Constraining the lithium evolution in the Milky Way

The AMBRE project: Constraining the lithium evolution in the Milky Way

TheGaiamission

GaiaFGK benchmark stars: new candidates at low metallicities

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