Photon Noise–limited Doppler Asteroseismology with a Fourier Transform Seismometer. I. Fundamental Performances

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Abstract
The photon noise–limited performances of a Fourier transform (FT) seismometer for ground‐based asteroseismological observations are computed. Simulations are conducted for a set of stars close to solar type, with V magnitude equal to 4 and vsin i from 0 to 40 km s -1, extended to 100 km s -1 and 8500 K in order to include δ Scuti stars. Two instrumental configurations are considered and compared: the simplest one matched to a narrowband, visible spectral range, and another one that implies a low‐resolution postdisperser, which covers a large portion of the visible domain. The final results are presented as the ratio of the expected uncertainties of the FT seismometer, in the version with a postdisperser, to the minimum radial velocities obtained with a grating spectrometer, on the same stellar targets. This ratio varies roughly between 1 and 2; it is close to 1 for fast rotators. It is concluded that the FT seismometer can be a challenging solution for a network dedicated to asteroseismology.

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