Context. Close-in, giant planets are expected to influence their host stars via tidal or magnetic interaction. But are these effects in X-rays strong enough in suitable targets known so far to be observed with today's instrumentation? Aims. The υ And system, an F8V star with a Hot Jupiter, was observed to undergo cyclic changes in chromospheric activity indicators with its innermost planet's period. We aim to investigate the stellar chromospheric and coronal activity over several months. Methods. We therefore monitored the star in X-rays as well as at optical wavelengths to test coronal and chromospheric activity indicators for planet-induced variability, making use of the Chandra X-ray Observatory as well as the echelle spectrographs FOCES and HRS at Calar Alto (Spain) and the Hobby-Eberly Telescope (Texas, US). Results. The stellar activity level is low, as seen both in X-rays as in Ca ii line fluxes; the chromospheric data show variability with the stellar rotation period. We do not find activity variations in X-rays or in the optical that can be traced back to the planet. Conclusions. Gaining observational evidence of star-planet interactions in X-rays remains challenging.

Close-in extrasolar giant planets are expected to cool their thermospheres by producing H + 3 emission in the near-infrared (NIR), but simulations predict H + 3 emission intensities that differ in the resulting intensity by several orders of magnitude. We want to test the observability of H + 3 emission with CRIRES at the Very Large Telescope (VLT), providing adequate spectral resolution for planetary atmospheric lines in NIR spectra. We search for signatures of planetary H + 3 emission in the L band, using spectra of HD 209458 obtained during and after secondary eclipse of its transiting planet HD 209458 b. We searched for H + 3 emission signatures in spectra containing the combined light of the star and, possibly, the planet. With the information on the ephemeris of the transiting planet, we derive the radial velocities at the time of observation and search for the emission at the expected line positions. We also apply a cross-correlation test to search for planetary signals and use a shift and add technique combining all observed spectra taken after secondary eclipse to calculate an upper emission limit. We do not find signatures of atmospheric H + 3 emission in the spectra containing the combined light of HD 209458 and its orbiting planet. We calculate the emission limit for the H + 3 line at 3953.0 nm [Q(1, 0)] to be 8.32 × 10 18 W and a limit of 5.34 × 10 18 W for the line at 3985.5 nm [Q(3, 0)]. Comparing our emission limits to the theoretical predictions suggests that we lack 1 to 3 magnitudes of sensitivity to measure H + 3 emission in our target object. We show that under more favorable weather conditions the data quality can be improved significantly, reaching 5 × 10 16 W for star-planet systems that are close to Earth. We estimate that pushing the detection limit down to 10 15 W will be possible with ground-based observations with future instrumentation, for example, the European Extremly Large Telescope.

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