A new study led by the GAPS (Global Architecture of Planetary Systems) collaboration has provided unprecedented observational constraints on the atmosphere of WASP-13b, an extremely low-density and inflated hot Jupiter orbiting a G1-type star every 4.35 days. Using the GIARPS observing mode at the Telescopio Nazionale Galileo (TNG), the team performed high-resolution transmission spectroscopy across multiple transits to search for atomic and molecular signatures in both the optical and near-infrared domains.

The available time offered in this call at TNG via INAF-TAC is 39 nights, 14 of which are reserved to exo-planetary research programs (see special notices below) and 25 are for other science programs. We encourage applicants to submit proposals asking a row of consecutive nights to be done in visitor mode. The budget can increase if not all the nights offered in other calls will be effectively allocated by the respective TACs. The foreseen schedule breakdown is reported at the bottom. All proposals will be judged strictly on their scientific merit.

Long-term observations with the HARPS-N spectrograph at the Telescopio Nazionale Galileo are helping astronomers investigate a compact system of four young planets, but the strong activity of their host star makes their masses difficult to measure. Physical and architectural properties of young planetary systems can look very different from those of the mature population. Studying them offers a rare opportunity to investigate how planets form and evolve before their architecture settles into its final configuration. One particularly interesting example is V1298 Tau, a star approximately 20 million years old that hosts four confirmed transiting planets.

An international collaboration among researchers from France, Chile, Germany, Poland, and Italy has compared the cross-correlated radial velocity (RV) curves of five Cepheids, obtained simultaneously in the V band (with HARPS-N) and the H band (with GIANO-B). They found that, for all stars, the V-band RV curve amplitude is approximately 5% larger than that of the H band. This amplitude difference can be explained to first order by the wavelength dependence of the geometric projection factor (i.e., the ratio between the true pulsation velocity and the observed radial velocity), which is directly linked to the expected limb darkening in the V and H bands.