Detection of solar-like oscillations in the bright red giant stars $\gamma$ Psc and ${\theta }^1$ Tau from a 190-day high-precision spectroscopic multisite campaign

Abstract

Red giants are evolved stars which exhibit solar-like oscillations. Although a multitude of stars have been observed with space telescopes, only a handful of red-giant stars were targets of spectroscopic asteroseismic observing projects. We search for solar-like oscillations in the two bright red-giant stars $\gamma$ Psc and ${\theta }^1$ Tau from time series of ground-based spectroscopy and determine the frequency of the excess of oscillation power ${\nu }_{max}$ and the mean large frequency separation $\Delta \nu$ for both stars. The radial velocities of $\gamma$ Psc and ${\theta }^1$ Tau were monitored for 120 and 190 days, respectively. Nearly 9000 spectra were obtained. To reach the accurate radial velocities, we used simultaneous thorium-argon and iodine-cell calibration of our optical spectra. In addition to the spectroscopy, we acquired VLTI observations of $\gamma$ Psc for an independent estimate of the radius. Also 22 days of observations of ${\theta }^1$ Tau with the MOST-satellite were analysed. The frequency analysis of the radial velocity data of $\gamma$ Psc revealed an excess of oscillation power around 32 $\mu$Hz and a large frequency separation of 4.1$\pm$0.1$\mu$Hz. ${\theta }^1$ Tau exhibits oscillation power around 90 $\mu$Hz, with a large frequency separation of 6.9$\pm$0.2$\mu$Hz. Scaling relations indicate that $\gamma$ Psc is a star of about $\sim$1 M${}_{\odot }$ and $\sim$10 R${}_{\odot }$. ${\theta }^1$ Tau appears to be a massive star of about $\sim$2.7 M${}_{\odot }$ and $\sim$11 R${}_{\odot }$. The radial velocities of both stars were found to be modulated on time scales much longer than the oscillation periods. While the mass of ${\theta }^1$ Tau is in agreement with results from dynamical parallaxes, we find a lower mass for $\gamma$ Psc than what is given in the literature. The long periodic variability agrees with the expected time scales of rotational modulation.

15 pages, 15 figures; accepted for publication in A&A

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