The Hubble/STIS near-ultraviolet transmission spectrum of HD 189733 b

¹ Space Research Institute, Austrian Academy of Sciences, Schmiedlstrasse 6, 8042, Graz, Austria
e-mail: patricio.cubillos@oeaw.ac.at
² INAF – Osservatorio Astrofisico di Torino, Via Osservatorio 20, 10025 Pino Torinese, Italy
³ Lunar and Planetary Laboratory, University of Arizona, 1629 E. University Blvd., Tucson, AZ 85721, USA
⁴ Laboratory for Atmospheric and Space Physics, University of Colorado, 600 UCB, Boulder, CO 80309, USA
⁵ School of Physical Sciences, The Open University, Walton Hall, Milton Keynes MK7 6AA, UK

Received: 26 September 2022
Accepted: 30 January 2023

Abstract

The benchmark hot Jupiter HD 189733 b has been a key target, used to lay out the foundations of comparative planetology for giant exo-planets. As such, HD 189733 b has been extensively studied across the electromagnetic spectrum. Here we report the observation and analysis of three transit light curves of HD 189733 b obtained with Hubble/STIS in the near-ultraviolet (NUV), the last remaining unexplored spectral window to be probed with present-day instrumentation for this planet. The NUV is a unique window for atmospheric mass-loss studies owing to the strong resonance lines and large photospheric flux. Overall, from a low-resolution analysis (R = 50) we found that the planet’s NUV spectrum is well characterized by a relatively flat baseline, consistent with the optical-infrared transmission, plus two regions at ~2350 and ~2600 Å that exhibit a broad and significant excess absorption above the continuum. From an analysis at a higher resolution (R = 4700), we found that the transit depths at the core of the magnesium resonance lines are consistent with the surrounding continuum. We discarded the presence of Mg II absorption in the upper atmosphere at a ~2–4σ confidence level, whereas we could place no significant constraint for Mg I absorption. These broad absorption features coincide with the expected location of Fe II bands; however, solar-abundance hydrodynamic models of the upper atmosphere are not able to reproduce the amplitude of these features with iron absorption. This scenario would require a combination of little to no iron condensation in the lower atmosphere super-solar metallicities and a mechanism to enhance the absorption features (such as zonal wind broadening). The true nature of this feature remains to be confirmed.