A Comparison of Stellar Elemental Abundance Techniques and Measurements

Hinkel, Natalie R.; Young, Patrick; Pagano, Michael; Desch, S. J.; Anbar, Ariel D.; Adibekyan, V.; Blanco-Cuaresma, S.; Carlberg, Joleen K.; Delgado-Mena, E.; Liu, F.; Nordlander, Thomas; Sousa, S. G.; Korn, A. J.; Gruyters, Pieter; Heiter, U.; Jofré, P.; Santos, N. C.; Soubiran, C.

doi:10.3847/0067-0049/226/1/4

Cited by 92 publications

(103 citation statements)

References 144 publications

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“…Since the last update published in Hinkel et al (2016), we have included 55 additional catalogs from the literature as well as 11 new elements and species (namely: Si II, Nb II, Pr II, Gd II, Tb II, Dy II, Er II, Tm II, Yb II, Hf II, Th II), as shown in Fig. 2.…”

Section: The Hypatia Catalog 21mentioning

confidence: 99%

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A Catalog of Stellar Unified Properties (CATSUP) for 951 FGK-Stars within 30 pc

Hinkel

Mamajek

Turnbull³

et al. 2017

ApJ

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Almost every star in our Galaxy is likely to harbor a terrestrial planet, but accurate measurements of an exoplanet's mass and radius demands accurate knowledge of the properties of its host star. The imminent TESS and CHEOPS missions are slated to discover thousands of new exoplanets. Along with WFIRST, which will directly image nearby planets, these surveys make urgent the need to better characterize stars in the nearby solar neighborhood (< 30 pc). We have compiled the CATalog of Stellar Unified Properties (CATSUP) for 951 stars, including such data as: Gaia astrometry; multiplicity within stellar systems; stellar elemental abundance measurements; standardized spectral types; Ca II H and K stellar activity indices; GALEX NUV and FUV photometry; and X-ray fluxes and luminosities from ROSAT, XMM, and Chandra. We use this data-rich catalog to find correlations, especially between stellar emission indices, colors, and galactic velocity. Additionally, we demonstrate that thick-disk stars in the sample are generally older, have lower activity, and have higher velocities normal to the galactic plane. We anticipate CATSUP will be useful in discerning other trends among stars within the nearby solar neighborhood, for comparing thin-disk vs. thick-disk stars, for comparing stars with and without planets, and for finding correlations between chemical and kinematic properties.

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Section: The Hypatia Catalog 21mentioning

confidence: 99%

“…Please see Hinkel et al (2014Hinkel et al ( , 2016 for more details. In the header, "S/N" is signal-to-noise report by the literature source, "λ Range" is the wavelength coverage, "Stellar Atmo" is the stellar atmospheric model, "Eq.…”

Section: Atlas9mentioning

confidence: 99%

A Catalog of Stellar Unified Properties (CATSUP) for 951 FGK-Stars within 30 pc

Hinkel

Mamajek

Turnbull³

et al. 2017

ApJ

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“…Multiple surveys studied the distribution of the stellar population C/O ratios (Teske et al 2014;Nissen et al 2014;Hinkel et al 2016;Brewer & Fischer 2016). These works concluded that planets hosting stars C/O ratios cluster around the solar (0.55) value, and very few stars (if any) have C/O larger than 0.8.…”

Section: Case: High Stellar C/o Ratiomentioning

confidence: 99%

Disentangling hot Jupiters formation location from their chemical composition

Ali-Dib

2017

Monthly Notices of the Royal Astronomical Society

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We use a population synthesis model that includes pebbles and gas accretion, planetary migration, and a simplified chemistry scheme to study the formation of hot-Jupiters. Models have been proposed that these planets can either originate beyond the snowline and then move inward via disk migration, or form "in-situ" inside the snowline. The goal of this work is to verify which of these two scenarios is more compatible with pebble accretion, and whether we can distinguish observationally between them via the resulting planetary C/O ratios and core masses. Our results show that, for solar system composition, the C/O ratios will vary but moderately between the two populations, since a significant amount of carbon and oxygen are locked up in refractories. In this case, we find a strong correlation between the carbon and oxygen abundances and core mass. The C/O ratio variations are more pronounced in the case where we assume that all carbon and oxygen are in volatiles. On average, Hot-Jupiters forming "in-situ" inside the snowline will have higher C/O ratios because they accrete less water ice. However, only Hot-Jupiters forming in-situ around stars with C/O=0.8 can have a C/O ratio higher than unity. We finally find that, even with fast pebble accretion, it is significantly easier to form Hot-Jupiters outside of the snowline, even if forming these "in-situ" is not impossible in the limit of the simplifying assumptions made.

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“…It would thus be expected that each ion of each element would also be affected to different degrees. For a broader view of uncertainties in spectroscopic abundance determination we refer the interested reader to the detailed empirical study of Hinkel et al (2016).…”

Section: Summary Of Uncertaintiesmentioning

confidence: 99%

NGC 6752 AGB stars revisited

Campbell

MacLean

D’Orazi

et al. 2017

A&A

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Context.A recent study reported a strong apparent depression of Fe i, relative to Fe ii, in the AGB stars of NGC 6752. This depression is much greater than that expected from the neglect of non-local thermodynamic equilibrium effects, in particular the dominant effect of overionisation. The iron abundances derived from Fe i were then used to scale all other neutral species in the study. Aims. Here we attempt to reproduce the apparent Fe discrepancy, and investigate differences in reported sodium abundances. Methods. We compare in detail the methods and results of the recent study with those of an earlier study of NGC 6752 AGB stars. Iron and sodium abundances are derived using Fe i, Fe ii, and Na i lines. We explore various uncertainties to test the robustness of our abundance determinations. Results. We reproduce the large Fe i depression found by the recent study, using different observational data and computational tools. Further investigation shows that the degree of the apparent Fe i depression is strongly dependent on the adopted stellar effective temperature. To minimise uncertainties in Fe i we derive temperatures for each star individually using the infrared flux method (IRFM). We find that the T eff scales used by both the previous studies are cooler, by up to 100 K; such underestimated temperatures amplify the apparent Fe i depression. Our IRFM temperatures result in negligible apparent depression, consistent with theory. We also re-derived sodium abundances and, remarkably, found them to be unaffected by the new temperature scale. [Na/H] in the AGB stars is consistent between all studies. Since Fe is constant, it follows that [Na/Fe] is also consistent between studies, apart from any systematic offsets in Fe. Conclusions. We recommend the use of (V − K) relations for AGB stars, based on comparisons with our individually-derived IRFM temperatures, and their inherently low uncertainties. We plan to investigate the effect of the improved temperature scale on other elements, and re-evaluate the subpopulation distributions on the AGB, in the next paper of this series.

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A Comparison of Stellar Elemental Abundance Techniques and Measurements

Cited by 92 publications

References 144 publications

A Catalog of Stellar Unified Properties (CATSUP) for 951 FGK-Stars within 30 pc

A Catalog of Stellar Unified Properties (CATSUP) for 951 FGK-Stars within 30 pc

Disentangling hot Jupiters formation location from their chemical composition

NGC 6752 AGB stars revisited

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