The GALAH survey: effective temperature calibration from the InfraRed Flux Method in the <i>Gaia</i> system

Casagrande, Luca; Lin, Jane; Rains, Adam D.; Liu, F.; Buder, Sven; Horner, Jonathan; Asplund, Martin; Lewis, Geraint F.; Martell, Sarah L.; Nordlander, Thomas; Stello, Dennis; Ting, Yuan-Sen; Wittenmyer, Robert A.; Bland‐Hawthorn, J.; Casey, Andrew R.; Silva, Gayandhi M. De; D’Orazi, V.; Freeman, K. C.; Hayden, Michael R.; Kos, Janez; Lind, Karin; Schlesinger, Katharine J.; Sharma, Sanjib; Simpson, Jeffrey D.; Zucker, D. B.; Zwitter, T.

doi:10.1093/mnras/stab2304

Cited by 66 publications

(46 citation statements)

References 57 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…The fitting residuals, as a function of (BP − RP ) and E(B − V ), are shown in the middle and bottom panels of Figure 1, respectively. The trends of our coefficients with color are consistent with the color-dependent coefficients of Casagrande et al (2021). Note that, in the above reddening coefficients, (BP − RP ) refers to intrinsic colors; iterations are needed when using the coefficients.…”

Section: Reddening Correctionssupporting

confidence: 74%

Stellar Loci V: Photometric Metallicities of 27 Million FGK Stars based on Gaia Early Data Release 3

Xu,

Yuan,

Niu

et al. 2021

Preprint

View full text Add to dashboard Cite

We combine LAMOST DR7 spectroscopic data and Gaia EDR3 photometric data to construct highquality giant (0.7 < (BP − RP ) < 1.4) and dwarf (0.5 < (BP − RP ) < 1.5) samples in the high Galactic latitude region, with precise corrections for magnitude-dependent systematic errors in the Gaia photometry and careful reddening corrections using empirically determined color-and reddeningdependent coefficients. We use the two samples to build metallicity-dependent stellar loci of Gaia colors for giants and dwarfs, respectively. For a given (BP − RP ) color, a one dex change in [Fe/H] results in about a 5 mmag change in (BP − G) color for solar-type stars. These relations are used to determine metallicity estimates from EDR3 colors. Despite the weak sensitivity, the exquisite data quality of these colors enables a typical precision of about δ [Fe/H] = 0.2 dex. Our method is valid for FGK stars with G ≤ 16, [Fe/H] ≥ −2.5, and E(B −V ) ≤ 0.5. Stars with fainter G magnitudes, lower metallicities, or larger reddening suffer from higher metallicity uncertainties. With the enormous data volume of Gaia, we have measured metallicity estimates for about 27 million stars with 10 < G ≤ 16 across almost the entire sky, including over 6 million giants and 20 million dwarfs, which can be used for a number of studies. These include investigations of Galactic formation and evolution, the identification of candidate stars for subsequent high-resolution spectroscopic follow-up, the identification of wide binaries, and to obtain metallicity estimates of stars for asteroseismology and exoplanet research.

show abstract

Section: Reddening Correctionssupporting

confidence: 74%

Stellar Loci V: Photometric Metallicities of 27 Million FGK Stars based on Gaia Early Data Release 3

Xu,

Yuan,

Niu

et al. 2021

Preprint

View full text Add to dashboard Cite

show abstract

“…As an additional check we inferred T eff for WASP-77 A using the colte code 9 (Casagrande et al 2021) that estimates T eff using a combination of color-T eff relations obtained by implementing the InfraRed Flux Method for Gaia and 2MASS photometry. As required by colte, we used Gaia EDR3 G, G BP , and G RP plus 2MASS J, H, and K s photometry as input.…”

Section: (2021)mentioning

confidence: 99%

“…Facilities: ARC, CDS, Exoplanet Archive, Gaia, IRSA, Skymapper, Sloan, TESS Software: astropy (Astropy Collaboration et al 2013Collaboration et al , 2018, CERES (Brahm et al 2017), colte (Casagrande et al 2021), eleanor (Feinstein et al 2019), IRAF (Tody 1986(Tody , 1993, isochrones (Morton 2015), iSpec (Blanco-Cuaresma et al 2014;Blanco-Cuaresma 2019), lightkurve (Lightkurve Collaboration et al 2018), MOOG (Sneden 1973), MultiNest (Feroz & Hobson 2008;Feroz et al 2009Feroz et al , 2019, numpy (Harris et al 2020), pandas (McKinney 2010; pandas Development Team 2020), PyMultinest (Buchner et al 2014), q 2 (Ramírez et al 2014), RadVel (Fulton et al 2017(Fulton et al , 2018, scipy (Virtanen et al 2020)…”

mentioning

confidence: 99%

Evidence that the Hot Jupiter WASP-77 A b Formed Beyond Its Parent Protoplanetary Disk's H2O Ice Line

Reggiani,

Schlaufman,

Healy

et al. 2022

Preprint

View full text Add to dashboard Cite

Idealized protoplanetary disk and giant planet formation models have been interpreted to suggest that a giant planet's atmospheric abundances can be used to infer its formation location in its parent protoplanetary disk. It has recently been reported that the hot Jupiter WASP-77 A b has sub-solar atmospheric carbon and oxygen abundances with a solar C/O abundance ratio. Assuming solar carbon and oxygen abundances for its host star WASP-77 A, WASP-77 A b's atmospheric carbon and oxygen abundances possibly indicate that it accreted its envelope interior to its parent protoplanetary disk's H 2 O ice line from carbon-depleted gas with little subsequent planetesimal accretion or core erosion. We comprehensively model WASP-77 A and use our results to better characterize WASP-77 A b. We show that the photospheric abundances of carbon and oxygen in WASP-77 A are super-solar with a sub-solar C/O abundance ratio, implying that WASP-77 A b's atmosphere has significantly sub-stellar carbon and oxygen abundances with a super-stellar C/O ratio. Our result possibly indicates that WASP-77 A b's envelope was accreted by the planet beyond its parent protoplanetary disk's H 2 O ice line. While numerous theoretical complications to these idealized models have now been identified, the possibility of non-solar protoplanetary disk abundance ratios confound even the most sophisticated protoplanetary disk and giant planet formation models. We therefore argue that giant planet atmospheric abundance ratios can only be meaningfully interpreted relative to the possibly non-solar mean compositions of their parent protoplanetary disks as recorded in the photospheric abundances of their solar-type dwarf host stars.

show abstract

“…For the Gaia EDR3 dataset, the A G value can be given, however it is not always available. In this case, (G Bp -G Rp ) colordependent extinction coefficients presented in Casagrande et al (2021) are used for G, G Bp and G Rp . For the magnitudes, we separate the PDFs entirely (G, G Bp , G Rp ) and (H, J, Ks, B, V).…”

Section: Synthetic Photometrymentioning

confidence: 99%

The SAPP pipeline for the determination of stellar abundances and atmospheric parameters of stars in the core program of the PLATO mission

Gent,

Bergemann,

Serenelli

et al. 2021

Preprint

Self Cite

View full text Add to dashboard Cite

We introduce the SAPP (Stellar Abundances and atmospheric Parameters Pipeline), the prototype of the code that will be used to determine parameters of stars observed within the core program of the PLATO space mission. The pipeline is based on the Bayesian inference and provides effective temperature, surface gravity, metallicity, chemical abundances, and luminosity. The code in its more general version can have a much wider range of applications. It can also provide masses, ages, and radii of stars and can be used for stars of stellar types not targeted by the PLATO core program, such as red giants. We validate the code on a set of 27 benchmark stars that includes 19 FGK-type dwarfs, 6 GK-type sub-giants, and 2 red giants. Our results suggest that combining various observables is the optimal approach, as it allows to break degeneracies between different parameters and yields more accurate values of stellar parameters and more realistic uncertainties. For the PLATO core sample, we obtain a typical uncertainty of 27(syst.) ± 37 (stat.) K for T eff , 0.00 ± 0.01 dex for log g, 0.02 ± 0.02 dex for metallicity [Fe/H], −0.01 ± 0.03 R for radii, −0.01 ± 0.05 M for stellar masses, and −0.14 ± 0.63 Gyrs for ages. We also show that the best results are obtained by combining the ν max scaling relation and stellar spectra. This resolves the notorious problem of degeneracies, which is particularly important for F-type stars.

show abstract

The GALAH survey: effective temperature calibration from the InfraRed Flux Method in the Gaia system

Cited by 66 publications

References 57 publications

Stellar Loci V: Photometric Metallicities of 27 Million FGK Stars based on Gaia Early Data Release 3

Stellar Loci V: Photometric Metallicities of 27 Million FGK Stars based on Gaia Early Data Release 3

Evidence that the Hot Jupiter WASP-77 A b Formed Beyond Its Parent Protoplanetary Disk's H2O Ice Line

The SAPP pipeline for the determination of stellar abundances and atmospheric parameters of stars in the core program of the PLATO mission

Contact Info

Product

Resources

About