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, Frederick 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

Research output: Contribution to journalArticle

46 Citations (Scopus)

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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stars
metal
metals
asteroseismology
scaling
halos
metallicity
astrophysics
cool stars
radii
catalogs
power spectra
envelopes
oscillation
telescopes
oscillations
shift
estimates
parameter

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., ... 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
Epstein, Courtney R. ; Elsworth, Yvonne P. ; Johnson, Jennifer A. ; Shetrone, Matthew ; Mosser, Benoît ; Hekker, Saskia ; Tayar, Jamie ; Harding, Paul ; Pinsonneault, Marc ; Silva Aguirre, Víctor ; Basu, Sarbani ; Beers, Timothy C. ; Bizyaev, Dmitry ; Bedding, Timothy R. ; Chaplin, William J. ; Frinchaboy, Peter M. ; García, Rafael A. ; Pérez, Ana E.García ; Hearty, Frederick R. ; Huber, Daniel ; Ivans, Inese I. ; Majewski, Steven R. ; Mathur, Savita ; Nidever, David ; Serenelli, Aldo ; Schiavon, Ricardo P. ; Schneider, Donald P. ; Schönrich, Ralph ; Sobeck, Jennifer S. ; Stassun, Keivan G. ; Stello, Dennis ; Zasowski, Gail. / Testing the asteroseismic mass scale using metal-poor stars characterized with APOGEE and Kepler. In: Astrophysical Journal Letters. 2014 ; Vol. 785, No. 2.
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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.",
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Epstein, CR, Elsworth, YP, Johnson, JA, Shetrone, M, Mosser, B, Hekker, S, Tayar, J, Harding, P, Pinsonneault, M, Silva Aguirre, V, Basu, S, Beers, TC, Bizyaev, D, Bedding, TR, Chaplin, WJ, Frinchaboy, PM, García, RA, Pérez, AEG, Hearty, FR, Huber, D, Ivans, II, Majewski, SR, Mathur, S, Nidever, D, Serenelli, A, Schiavon, RP, Schneider, DP, Schönrich, R, Sobeck, JS, Stassun, KG, Stello, D & Zasowski, G 2014, 'Testing the asteroseismic mass scale using metal-poor stars characterized with APOGEE and Kepler', Astrophysical Journal Letters, vol. 785, no. 2, L28. https://doi.org/10.1088/2041-8205/785/2/L28

Testing the asteroseismic mass scale using metal-poor stars characterized with APOGEE and Kepler. / Epstein, Courtney R.; Elsworth, Yvonne P.; Johnson, Jennifer A.; Shetrone, Matthew; Mosser, Benoît; Hekker, Saskia; Tayar, Jamie; Harding, Paul; Pinsonneault, Marc; Silva Aguirre, Víctor; Basu, Sarbani; Beers, Timothy C.; Bizyaev, Dmitry; Bedding, Timothy R.; Chaplin, William J.; Frinchaboy, Peter M.; García, Rafael A.; Pérez, Ana E.García; Hearty, Frederick R.; Huber, Daniel; Ivans, Inese I.; Majewski, Steven R.; Mathur, Savita; Nidever, David; Serenelli, Aldo; Schiavon, Ricardo P.; Schneider, Donald P.; Schönrich, Ralph; Sobeck, Jennifer S.; Stassun, Keivan G.; Stello, Dennis; Zasowski, Gail.

In: Astrophysical Journal Letters, Vol. 785, No. 2, L28, 20.04.2014.

Research output: Contribution to journalArticle

TY - JOUR

T1 - Testing the asteroseismic mass scale using metal-poor stars characterized with APOGEE and Kepler

AU - Epstein, Courtney R.

AU - Elsworth, Yvonne P.

AU - Johnson, Jennifer A.

AU - Shetrone, Matthew

AU - Mosser, Benoît

AU - Hekker, Saskia

AU - Tayar, Jamie

AU - Harding, Paul

AU - Pinsonneault, Marc

AU - Silva Aguirre, Víctor

AU - Basu, Sarbani

AU - Beers, Timothy C.

AU - Bizyaev, Dmitry

AU - Bedding, Timothy R.

AU - Chaplin, William J.

AU - Frinchaboy, Peter M.

AU - García, Rafael A.

AU - Pérez, Ana E.García

AU - Hearty, Frederick R.

AU - Huber, Daniel

AU - Ivans, Inese I.

AU - Majewski, Steven R.

AU - Mathur, Savita

AU - Nidever, David

AU - Serenelli, Aldo

AU - Schiavon, Ricardo P.

AU - Schneider, Donald P.

AU - Schönrich, Ralph

AU - Sobeck, Jennifer S.

AU - Stassun, Keivan G.

AU - Stello, Dennis

AU - Zasowski, Gail

PY - 2014/4/20

Y1 - 2014/4/20

N2 - 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.

AB - 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.

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