Transmission spectroscopy of the ultra-hot Jupiter MASCARA-4 b: Disentangling the hydrostatic and exospheric regimes of ultra-hot Jupiters

TL;DR

This study uses high-resolution spectroscopy to analyze the atmosphere of the ultra-hot Jupiter MASCARA-4 b, distinguishing between its hydrostatic and exospheric regimes through detection of various atomic and ionic species.

Contribution

It provides the first detailed transmission spectrum of MASCARA-4 b, revealing the presence of multiple species and differentiating atmospheric regimes in ultra-hot Jupiters.

Findings

Detected excess absorption by Hα, Hβ, Na D, Ca+ H&K, Mg, Fe lines

Observed Fe+ absorption exceeds hydrostatic model predictions, indicating exosphere presence

Disentangled hydrostatic and exospheric regimes in ultra-hot Jupiter atmospheres

Abstract

Ultra-hot Jupiters (UHJs), rendering the hottest planetary atmospheres, offer great opportunities of detailed characterisation with high-resolution spectroscopy. MASCARA-4 b is a recently discovered close-in gas giant belonging to this category. In order to refine system and planet parameters, we carried out radial velocity measurements and transit photometry with the CORALIE spectrograph and EulerCam at the Swiss 1.2m Euler telescope. We observed two transits of MASCARA-4 b with the high-resolution spectrograph ESPRESSO at ESO's Very Large Telescope. We searched for atomic, ionic, and molecular species via individual absorption lines and cross-correlation techniques. These results are compared to literature studies on UHJs characterised to date. With CORALIE and EulerCam observations, we updated the mass of MASCARA-4 b (1.675 +/- 0.241 Jupiter masses) as well as other system and planet parameters. In the transmission spectrum derived from ESPRESSO observations, we resolve excess absorption by H$\alpha$, H$\beta$, Na D1 & D2, Ca+ H & K, and a few strong individual lines of Mg, Fe and Fe+. We also present the cross-correlation detection of Mg, Ca, Cr, Fe and Fe+. The absorption strength of Fe+ significantly exceeds the prediction from a hydrostatic atmospheric model, as commonly observed in other UHJs. We attribute this to the presence of Fe+ in the exosphere due to hydrodynamic outflows. This is further supported by the positive correlation of absorption strengths of Fe+ with the H$\alpha$ line. Comparing transmission signatures of various species in the UHJ population allows us to disentangle the hydrostatic regime (as traced via the absorption by Mg and Fe) from the exospheres (as probed by H$\alpha$ and Fe+) of the strongly irradiated atmospheres.