Asteroseismic Properties of Solar-type Stars Observed with the NASA<i>K2</i>Mission: Results from Campaigns 1–3 and Prospects for Future Observations

Lund, Mikkel N.; Chaplin, W. J.; Casagrande, Luca; Aguirre, V. Silva; Basu, Sarbani; Bieryla, Allyson; Christensen‐Dalsgaard, J.; Latham, David W.; White, T. R.; Davies, G. R.; Huber, Daniel; Buchhave, Lars A.; Handberg, R.

doi:10.1088/1538-3873/128/970/124204

Cited by 29 publications

(19 citation statements)

References 119 publications

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“…[Fe/H] comes from spectroscopic observations from the APOGEE survey (Majewski et al 2017). Lund et al (2016) present an asteroseismic analysis of 33 solar-like stars observed by the K2 mission. The modeling of M, R, and ρ was done through grid-based modeling using the Bayesian Stellar Algorithm (BASTA; Silva Aguirre et al 2015) and GARSTEC.…”

Section: Data Samplementioning

confidence: 99%

Empirical Relations for the Accurate Estimation of Stellar Masses and Radii

Moya

Zuccarino

Chaplin

et al. 2018

ApJS

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In this work, we have taken advantage of the most recent accurate stellar characterizations carried out using asteroseismology, eclipsing binaries and interferometry to evaluate a comprehensive set of empirical relations for the estimation of stellar masses and radii. We have gathered a total of 934 stars-of which around two-thirds are on the main sequence-that are characterized with different levels of precision, most of them having estimates of M, R, T eff , L, g, ρ, and [Fe/H]. We have deliberately used a heterogeneous sample (in terms of characterizing techniques and spectroscopic types) to reduce the influence of possible biases coming from the observation, reduction, and analysis methods used to obtain the stellar parameters. We have studied a total of 576 linear combinations of T eff , L, g, ρ, and [Fe/H] (and their logarithms) to be used as independent variables to estimate M or R. We have used an error-in-variables linear regression algorithm to extract the relations and to ensure the fair treatment of the uncertainties. We present a total of 38 new or revised relations that have an adj-R 2 regression statistic higher than 0.85, and a relative accuracy and precision better than 10% for almost all the cases. The relations cover almost all the possible combinations of observables, ensuring that, whatever list of observables is available, there is at least one relation for estimating the stellar mass and radius.

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Section: Data Samplementioning

confidence: 99%

Empirical Relations for the Accurate Estimation of Stellar Masses and Radii

Moya

Zuccarino

Chaplin

et al. 2018

ApJS

Self Cite

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“…The noise model applied in the detection probability test follows that first proposed for Kepler in Chaplin et al (2011b), modified for the noise performance of K2 by Lund et al (2016). The procedure predicts the expected global signal-to-noise level in the detected oscillations against background from intrinsic stellar noise (granulation) and shot/instrumental noise.…”

Section: Selection Functionmentioning

confidence: 99%

The K2 Galactic Caps Project – going beyond the Kepler field and ageing the Galactic disc

Rendle

Miglio

Chiappini

et al. 2019

Monthly Notices of the Royal Astronomical Society

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Analyses of data from spectroscopic and astrometric surveys have led to conflicting results concerning the vertical characteristics of the Milky Way. Ages are often used to provide clarity, but typical uncertainties of > 40 % restrict the validity of the inferences made. Using the Kepler APOKASC sample for context, we explore the global population trends of two K2 campaign fields (3 and 6), which extend further vertically out of the Galactic plane than APOKASC. We analyse the properties of red giant stars utilising three asteroseismic data analysis methods to cross-check and validate detections. The Bayesian inference tool PARAM is used to determine the stellar masses, radii and ages. Evidence of a pronounced red giant branch bump and an [α/Fe] dependence on the position of the red clump is observed from the radii distribution of the K2 fields. Two peaks in the age distribution centred at ∼5 and and ∼12 Gyr are found using a sample with σ age < 35 %. In a comparison with Kepler, we find the older peak to be more prominent for K2. This age bimodality is also observed based on a chemical selection of low-(≤ 0.1) and high-(> 0.1) [α/Fe] stars. As a function of vertical distance from the Galactic mid-plane (|Z |), the age distribution shows a transition from a young to old stellar population with increasing |Z | for the K2 fields. Further coverage of campaign targets with high resolution spectroscopy is required to increase the yield of precise ages achievable with asteroseismology.

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“…[h] Table 2. Comparisons of our measurements with those from other works: the GALAH survey (Buder et al 2018a), the GALAH-TGAS survey (Buder et al 2018b), K2 asteroseismology parameters (Lund et al 2016) and the TESS Input Catalog (Stassun et al 2018). We for all but the asteroseismology comparison we divide our sample into evolved stars (where the comparison survey measures log g < 4) and dwarfs of different spectral classes.…”

Section: Acknowledgmentsmentioning

confidence: 98%

“…To further test our stellar parameter measurements we also compared our results with objects in the GALAH-TGAS survey (a separate stellar parameter calculation from the main GALAH survey using GALAH spectra and GAIA TGAS parallaxes Buder et al 2018b), K2 asteroseismology parameters (Lund et al 2016) and the aforementioned TESS Input Catalog (Stassun et al 2018). We note that the GALAH-TGAS survey includes some of the astrometric data that went into the Gaia parallaxes we use, hence it is not entirely independent.…”

Section: Comparison To Other Stellar Parameter Estimatesmentioning

confidence: 99%

Data-driven stellar parameters for southern TESS FGK targets

Deacon

Henning

Kossakowski

2019

Monthly Notices of the Royal Astronomical Society

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We present stellar parameter estimates for 939,457 southern FGK stars that are candidate targets for the TESS mission. Using a data-driven method similar to the CAN-NON, we build a model of stellar colours as a function of stellar parameters. We then use these in combination with stellar evolution models to estimate the effective temperature, gravity, metallicity, mass, radius and extinction for our selected targets. Our effective temperature estimates compare well with those from spectroscopic surveys and the addition of Gaia DR2 parallaxes allows us to identify subgiant interlopers into the TESS sample. We are able to estimate the radii of TESS targets with a typical uncertainty of 9.3%. This catalogue can be used to screen exoplanet candidates from TESS and provides a homogeneous set of stellar parameters for statistical studies.

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Asteroseismic Properties of Solar-type Stars Observed with the NASAK2Mission: Results from Campaigns 1–3 and Prospects for Future Observations

Cited by 29 publications

References 119 publications

Empirical Relations for the Accurate Estimation of Stellar Masses and Radii

Empirical Relations for the Accurate Estimation of Stellar Masses and Radii

The K2 Galactic Caps Project – going beyond the Kepler field and ageing the Galactic disc

Data-driven stellar parameters for southern TESS FGK targets

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