Testing the asteroseismic mass scale using metal-poor stars characterized with APOGEE and Kepler

Courtney R. Epstein, Yvonne P. Elsworth, Jennifer A. Johnson, Matthew Shetrone, Benoît Mosser, Saskia Hekker, Jamie Tayar, Paul Harding, Marc Pinsonneault, Víctor Silva Aguirre, Sarbani Basu, Timothy C. Beers, Dmitry Bizyaev, Timothy R. Bedding, William J. Chaplin, Peter M. Frinchaboy, Rafael A. García, Ana E.García Pérez, Fred R. Hearty, Daniel HuberInese I. Ivans, Steven R. Majewski, Savita Mathur, David Nidever, Aldo Serenelli, Ricardo P. Schiavon, Donald P. Schneider, Ralph Schönrich, Jennifer S. Sobeck, Keivan G. Stassun, Dennis Stello, Gail Zasowski

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Abstract

Fundamental stellar properties, such as mass, radius, and age, can be inferred using asteroseismology. Cool stars with convective envelopes have turbulent motions that can stochastically drive and damp pulsations. The properties of the oscillation frequency power spectrum can be tied to mass and radius through solar-scaled asteroseismic relations. Stellar properties derived using these scaling relations need verification over a range of metallicities. Because the age and mass of halo stars are well-constrained by astrophysical priors, they provide an independent, empirical check on asteroseismic mass estimates in the low-metallicity regime. We identify nine metal-poor red giants (including six stars that are kinematically associated with the halo) from a sample observed by both the Kepler space telescope and the Sloan Digital Sky Survey-III APOGEE spectroscopic survey. We compare masses inferred using asteroseismology to those expected for halo and thick-disk stars. Although our sample is small, standard scaling relations, combined with asteroseismic parameters from the APOKASC Catalog, produce masses that are systematically higher (<ΔM > =0.17 ± 0.05 M) than astrophysical expectations. The magnitude of the mass discrepancy is reduced by known theoretical corrections to the measured large frequency separation scaling relationship. Using alternative methods for measuring asteroseismic parameters induces systematic shifts at the 0.04 M level. We also compare published asteroseismic analyses with scaling relationship masses to examine the impact of using the frequency of maximum power as a constraint. Upcoming APOKASC observations will provide a larger sample of 100 metal-poor stars, important for detailed asteroseismic characterization of Galactic stellar populations.

Original languageEnglish (US)
Article numberL28
JournalAstrophysical Journal Letters
Volume785
Issue number2
DOIs
StatePublished - Apr 20 2014

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All Science Journal Classification (ASJC) codes

  • Astronomy and Astrophysics
  • Space and Planetary Science

Cite this

Epstein, C. R., Elsworth, Y. P., Johnson, J. A., Shetrone, M., Mosser, B., Hekker, S., Tayar, J., Harding, P., Pinsonneault, M., Silva Aguirre, V., Basu, S., Beers, T. C., Bizyaev, D., Bedding, T. R., Chaplin, W. J., Frinchaboy, P. M., García, R. A., Pérez, A. E. G., Hearty, F. R., ... Zasowski, G. (2014). Testing the asteroseismic mass scale using metal-poor stars characterized with APOGEE and Kepler. Astrophysical Journal Letters, 785(2), [L28]. https://doi.org/10.1088/2041-8205/785/2/L28