V. Silva Aguirre, D. Stello, A. Stokholm, J. L. Rørsted, W. H. Ball, S. Basu, D. Bossini, L. Bugnet, D. L. Buzasi, T. L. Campante, L. Carboneau, W. J. Chaplin, E. Corsaro, G. R. Davies, Y. Elsworth, R. García, P. Gaulme, O. J. Hall, R. Handberg, M. Hon, T. Kallinger, L. Kang, M. N. Lund, S. Mathur, A. Mints, B. Mosser, Z. Çelik Orhan, T. S. Rodrigues, M. Vrard, M. Yildiz, M. Yıldız, J. C. Zinn, S. Örtel, P. G. Beck, K. J. Bell, Z. Guo, C. Jiang, J. S. Kuszlewicz, C. A. Kuehn, T. Li, M. Lundkvist, M. H. Pinsonneault, J. Tayar, M. S. Cunha, S. Hekker, D. Huber, A. Miglio, M. J. P. F. G. Monteiro, D. Slumstrup, M. L. Winther, G. Angelou, O. Benomar, A. Bódi, B. L. De Moura, S. Deheuvels, A. Derekas, M. P. Di Mauro, M.-A. Dupret, A. Jiménez, Y. Lebreton, Matthews J. M., N. Nardetto, J. D. do Nascimento Jr., L. F. Pereira, L. F. Rodríguez Díaz, A. M. Serenelli, E. Spitoni, E. Stonkutè, J.-C. Suárez, R. Szabó, V. Van Eylen, R. Ventura, K. Verma, A. Weiss, T. Wu, T. Barclay, J. Christensen-Dalsgaard, J. M. Jenkins, H. Kjeldsen, G. R. Ricker, S. Seager, R. K. Vanderspek
Since the onset of the "space revolution" of high-precision high-cadence photometry, asteroseismology has been demonstrated as a powerful tool for informing Galactic archeology investigations. The launch of the NASA Transiting Exoplanet Survey Satellite (TESS) mission has enabled seismic-based inferences to go full sky—providing a clear advantage for large ensemble studies of the different Milky Way components. Here we demonstrate its potential for investigating the Galaxy by carrying out the first asteroseismic ensemble study of red giant stars observed by TESS. We use a sample of 25 stars for which we measure their global asteroseimic observables and estimate their fundamental stellar properties, such as radius, mass, and age. Significant improvements are seen in the uncertainties of our estimates when combining seismic observables from TESS with astrometric measurements from the Gaia mission compared to when the seismology and astrometry are applied separately. Specifically, when combined we show that stellar radii can be determined to a precision of a few percent, masses to 5%–10%, and ages to the 20% level. This is comparable to the precision typically obtained using end-of-mission Kepler data.
Astrophysics - Solar and Stellar Astrophysics; Astrophysics - Astrophysics of Galaxies
The Astrophysical Journal Letters
Volume 889, Number 2