The Gaia FGK Benchmark Stars Version 2.1*

Jofré, P.; Heiter, U.; Maia, M. Tucci; Soubiran, C.; Worley, C. C.; Hawkins, Keith; Blanco-Cuaresma, S.; Rodrigo, C.

doi:10.3847/2515-5172/aadc61

Cited by 55 publications

(87 citation statements)

References 13 publications

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“…We made a comprehensive comparison of our T eff , log g, and [Fe/H] values with those of virtually all relevant determinations of stellar atmospheric parameters of FGK-type stars. Our parameter determinations are in good agreement with the literature values in general, particularly with the region of the parameter space covered by the YaPSI isochrones (Spada et al 2017) and the Gaia benchmark stars (Jofré et al 2014(Jofré et al , 2018. The scarcity of Fe ii lines in the NIR wavelength range covered by CARMENES prevented us from performing the stellar parameter determinations using this spectral region alone.…”

Section: Discussionsupporting

confidence: 88%

“…10 but restricting the analysis to the Fe i and Fe ii lines found in the optical wavelength region covered by the VIS channel of CARMENES. Jofré et al (2018), can be found in Fig. 14. We find good agreement between our derived values and the fundamental T eff and log g, i.e.…”

Section: Resultsmentioning

confidence: 92%

“…In Figs. 10 and 11 we compare the stellar atmospheric parameters computed with StePar with values from the literature (McWilliam 1990;Heiter & Luck 2003;Allende Prieto et al 2004;Valenti & Fischer 2005;Hekker & Meléndez 2007;Liu et al 2007;Sousa et al 2008;Takeda et al 2008;Lyubimkov et al 2010;Wu et al 2011;Thygesen et al 2012;Santos et al 2013;Morel et al 2014;Luck 2014;Jofré et al 2014Jofré et al , 2015da Silva et al 2015;Jofré et al 2018), taking into account the VIS and NIR channels simultaneously, and only the VIS channel, respectively. To explore possible sources of potential systematic trends or offsets, we followed the Monte Carlo method implemented in Tabernero et al (2018).…”

Section: Resultsmentioning

confidence: 99%

“…Reference for spectral type, SpT: Caballero et al (in prep.). f Gaia benchmark star (Jofré et al 2014(Jofré et al , 2018.…”

Section: Appendix A: Appendixmentioning

confidence: 99%

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Stellar atmospheric parameters of FGK-type stars from high-resolution optical and near-infrared CARMENES spectra

Marfil

Tabernero

Montes

et al. 2020

Monthly Notices of the Royal Astronomical Society

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With the purpose of assessing classic spectroscopic methods on high-resolution and high signal-to-noise ratio spectra in the near-infrared wavelength region, we selected a sample of 65 F-, G-, and K-type stars observed with CARMENES, the new, ultrastable, double-channel spectrograph at the 3.5 m Calar Alto telescope. We computed their stellar atmospheric parameters (T eff , log g, ξ, and [Fe/H]) by means of the StePar code, a Python implementation of the equivalent width method that employs the 2017 version of the MOOG code and a grid of MARCS model atmospheres. We compiled four Fe i and Fe ii line lists suited to metal-rich dwarfs, metal-poor dwarfs, metal-rich giants, and metal-poor giants that cover the wavelength range from 5 300 to 17 100Å, thus substantially increasing the number of identified Fe i and Fe ii lines up to 653 and 23, respectively. We examined the impact of the near-infrared Fe i and Fe ii lines upon our parameter determinations after an exhaustive literature search, placing special emphasis on the 14 Gaia benchmark stars contained in our sample. Even though our parameter determinations remain in good agreement with the literature values, the increase in the number of Fe i and Fe ii lines when the near-infrared region is taken into account reveals a deeper T eff scale that might stem from a higher sensitivity of the near-infrared lines to T eff .

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Section: Discussionsupporting

confidence: 88%

Section: Resultsmentioning

confidence: 92%

Section: Resultsmentioning

confidence: 99%

“…Reference for spectral type, SpT: Caballero et al (in prep.). f Gaia benchmark star (Jofré et al 2014(Jofré et al , 2018.…”

Section: Appendix A: Appendixmentioning

confidence: 99%

See 2 more Smart Citations

Stellar atmospheric parameters of FGK-type stars from high-resolution optical and near-infrared CARMENES spectra

Marfil

Tabernero

Montes

et al. 2020

Monthly Notices of the Royal Astronomical Society

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“…We plot in Fig. 5 the obtained T eff and log g compared with the reference (Heiter et al 2015a;Jofré et al 2018) for each spectrum. We obtain a good agreement, with differences below 100 K and 0.1 dex in T eff and log g respectively, with however larger differences for the giants HD 107328, Vir and ξHya, especially for the surface gravity.…”

Section: Gaia Fgk Benchmark Starsmentioning

confidence: 99%

Differential abundances of open clusters and their tidal tails: Chemical tagging and chemical homogeneity

Casamiquela

Tarricq

Soubiran

et al. 2020

A&A

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Context. Well studied Open Clusters (OCs) of the Solar neighbourhood are frequently used as reference objects to test galactic and stellar theories. For that purpose their chemical composition needs to be known with a high level of confidence. It is also important to clarify if each OC is chemically homogeneous and if it has a unique chemical signature. Aims. The aims of this work are (1) to determine accurate and precise abundances of 22 chemical species (from Na to Eu) in the Hyades, Praesepe and Rupecht 147 using a large number of stars at different evolutionary states, (2) to evaluate the level of chemical homogeneity of these OCs, (3) to compare their chemical signatures. Methods. We gathered ∼800 high resolution and high signal-to-noise spectra of ∼100 members in the three clusters, obtained with the latest memberships based on Gaia DR2 data. We build a pipeline which computes atmospheric parameters and strictly line-by-line differential abundances among twin stars in our sample. With this method we are able to reach a very high precision in the abundances (0.01-0.02 dex in most of the elements). Results. We find large differences in the absolute abundances in some elements, which can be attributed to diffusion, NLTE effects or systematics in the analysis. For the three OCs, we find strong correlations in the differential abundances between different pairs of elements. According to our experiment with synthetic data, this can be explained by some level of chemical inhomogeneity. We compare differential abundances of several stars from the Hyades and Praesepe tails: the stars that differ more in chemical abundances also have distinct kinematics, even though they have been identified as members of the tail. Conclusions. It is possible to obtain high precision abundances using a differential analysis even when mixing spectra from different instruments. With this technique we find that the Hyades and Preasepe have the same chemical signature when G dwarfs and K giants are considered. Despite a certain level of inhomogeneity in each cluster, it is still possible to clearly distinguish the chemical signature of the older cluster Ruprecht 147 when compared to the Hyades and Praesepe.

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Sun‐like stars unlike the Sun: Clues for chemical anomaliesof cool stars

et al. 2017

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We present a summary of the splinter session "Sun-like stars unlike the Sun" that was held on June 9, 2016, as part of the Cool Stars 19 conference (Uppsala, Sweden), in which the main limitations (in the theory and observations) in the derivation of very precise stellar parameters and chemical abundances of Sun-like stars were discussed. The most important and most debated processes that can produce chemical peculiarities in solar-type stars were outlined and discussed. Finally, in an open discussion between all the participants, we tried to identify new pathways and prospects toward future solutions of the currently open questions.

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The Gaia FGK Benchmark Stars Version 2.1*

Cited by 55 publications

References 13 publications

Stellar atmospheric parameters of FGK-type stars from high-resolution optical and near-infrared CARMENES spectra

Stellar atmospheric parameters of FGK-type stars from high-resolution optical and near-infrared CARMENES spectra

Differential abundances of open clusters and their tidal tails: Chemical tagging and chemical homogeneity

Sun‐like stars unlike the Sun: Clues for chemical anomaliesof cool stars

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