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The Asteroseismic Target List for Solar-like Oscillators Observed in 2 minute Cadence with the Transiting Exoplanet Survey Satellite

  • Authors: Mathew Schofield, William J. Chaplin, Daniel Huber, Tiago L. Campante, Guy R. Davies, Andrea Miglio, Warrick H. Ball, Thierry Appourchaux, Sarbani Basu, Timothy R. Bedding, Jørgen Christensen-Dalsgaard, Orlagh Creevey, Rafael A. García, Rasmus Handberg, Steven D. Kawaler, Hans Kjeldsen, David W. Latham, Mikkel N. Lund, Travis S. Metcalfe, George R. Ricker, Aldo Serenelli, Victor Silva Aguirre, Dennis Stello, and Roland Vanderspek

2019 The Astrophysical Journal Supplement Series 241 12.

  • Provider: AAS Journals

Caption: Figure 9.

H–R diagram of all ATL stars with detection probabilities greater than 50% with (left panel) and without (right panel) including the β factor, which accounts for the attenuation of oscillation amplitudes toward the red edge of the instability strip (dashed line). Solid lines show solar metallicity evolutionary tracks with masses from 0.8 M to 2.0 M in steps of 0.2 M. Note that the sharp edges are due to cuts at the red edge of the instability strip (Equation (3)) and stars oscillating with frequencies accessible with TESS FFI data (Equation (4)).

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