GIARPS@TNG: GIANO-B and HARPS-N together for a wider wavelength range spectroscopy

Abstract

Since 2012, thanks to the installation of the high resolution echelle spectrograph in the optical range HARPS-N, the Italian telescope TNG (La Palma) became one of the key facilities for the study of the extrasolar planets. In 2014 TNG also offered GIANO to the scientific community, providing a near-infrared (NIR) cross-dispersed echelle spectroscopy covering 0.97 − 2.45 µm at a resolution of 50,000. GIANO, although designed for direct light-feed from the telescope at the Nasmyth-B focus, was provisionally mounted on the rotating building and connected via fibers to only available interface at the Nasmyth-A focal plane. The synergy between these two instruments is particularly appealing for a wide range of science cases, especially for the search of exoplanets around young and active stars and the characterisation of their atmosphere. Through the funding scheme "WOW" (a Way to Others Worlds), the Italian National Institute for Astrophysics (INAF) proposed to position GIANO at the focal station for which it was originally designed and the simultaneous use of these spectrographs with the aim to achieve high-resolution spectroscopy in a wide wavelength range (0.383 − 2.45 µm) obtained in a single exposure, giving rise to the project called GIARPS (GIANO-B & HARPS-N). Because of its characteristics GIARPS can be considered the first and unique worldwide instrument providing not only high resolution in a large wavelength band, but also a high precision radial velocity measurement both in the visible and in the NIR arm, since in the next future GIANO-B will be equipped with gas absorption cells.

Mass–Radius Relationship for M Dwarf Exoplanets: Comparing Nonparametric and Parametric Methods

“…This would further unveil features and regions that were indistinguishable earlier. This will particularly hold true as the M dwarf M-R space starts to fill up with radii from TESS (Thibault et al 2012), IRD (Kotani et al 2018), ESPRESSO (Hernndez et al 2017), NIRPS (Wildi et al 2017), SPIRou (Artigau et al 2014), iSHELL (Cale et al 2018), GIANO (Claudi et al 2017) and EXPRES (Jurgenson et al 2016).…”

“…It has also been shown that the spot-induced RV jitter is reduced in the near infrared (NIR) (Marchwinski et al 2015), which is where the spectral energy distributions for these stars peak. For these reasons, many more M dwarf planets will have their masses measured in the near future by instruments such as the HPF (Mahadevan et al 2012), CARMENES (Quirrenbach et al 2016), NIRPS (Wildi et al 2017), IRD (Kotani et al 2018), SPIRou (Artigau et al 2014), iSHELL (Cale et al 2018), GIANO (Claudi et al 2017), and NEID (Schwab et al 2016). Here we set the stage for these future datasets by assessing the dependence of the M-R model choices on mass and radius predictions, especially as a function of stellar type.…”

The CARMENES search for exoplanets around M dwarfs

“…Instruments such as CARMENES (Quirrenbach et al 2016) and GIARPS (GIANO-B+HARPS-N, Claudi et al 2017) minimize the stellar activity problem by obtaining simultaneous optical (VIS) and near-infrared (NIR) data. The RV signal of planetary origin is independent of the observed wavelength, whereas the amplitude of the signal due to stellar activity may strongly depend on wavelength (typically larger at shorter wavelengths; e.g., Martín et al 2006;Huélamo et al 2008;Carleo et al 2018).…”

Simulated mass measurements of the young planet K2-33b

“…Observing PMS stars in the near infrared (nIR) rather than in the V band should make it easier to separate the E-mail: baptiste.klein@irap.omp.eu planet signature from the stellar activity signal as the latter is expected to be weaker in this domain (Mahmud et al 2011) and the stars are significantly reddened. Highprecision nIR velocimeters like SPIRou (Donati et al 2018), CARMENES (Quirrenbach et al 2014), GIARPS (Claudi et al 2017) or NIRPS (Wildi et al 2017) are thus the most promising instruments worldwide to carry out mass measurements of close-in transiting planets orbiting PMS stars. Magnetic fields are however expected to affect stellar RV activity signals (Reiners et al 2013;Hébrard et al 2014), making the problem non trivial and worth a detailed simulation study.…”