Transmission spectroscopy of the inflated exo-Saturn HAT-P-19b

TL;DR

This study refines the orbital and physical parameters of exo-Saturn HAT-P-19b, presents its transmission spectrum showing no significant features, and assesses stellar activity over a year to improve understanding of its atmosphere and host star.

Contribution

It provides the first transmission spectrum of HAT-P-19b and refines its orbital, physical, and stellar parameters using spectroscopic and photometric data.

Findings

Refined planet-to-star radius ratio of 0.1390 ± 0.0012

Orbital period refined to 4.0087844 ± 0.0000015 days

Transmission spectrum shows no significant absorption features

Abstract

We observed the Saturn-mass and Jupiter-sized exoplanet HAT-P-19b to refine its transit parameters and ephemeris as well as to shed first light on its transmission spectrum. We monitored the host star over one year to quantify its flux variability and to correct the transmission spectrum for a slope caused by starspots. A transit of HAT-P-19b was observed spectroscopically with OSIRIS at the Gran Telescopio Canarias in January 2012. The spectra of the target and the comparison star covered the wavelength range from 5600 to 7600 AA. One high-precision differential light curve was created by integrating the entire spectral flux. This white-light curve was used to derive absolute transit parameters. Furthermore, a set of light curves over wavelength was formed by a flux integration in 41 wavelength channels of 50 AA width. We analyzed these spectral light curves for chromatic variations of transit depth. The transit fit of the combined white-light curve yields a refined value of the planet-to-star radius ratio of 0.1390 pm 0.0012 and an inclination of 88.89 pm 0.32 degrees. After a re-analysis of published data, we refine the orbital period to 4.0087844 pm 0.0000015 days. We obtain a flat transmission spectrum without significant additional absorption at any wavelength or any slope. However, our accuracy is not sufficient to significantly rule out the presence of a pressure-broadened sodium feature. Our photometric monitoring campaign allowed for an estimate of the stellar rotation period of 35.5 pm 2.5 days and an improved age estimate of 5.5^+1.8_-1.3 Gyr by gyrochronology.