# An emission spectrum for WASP-121b measured across the 0.8-1.1 micron wavelength range using the Hubble Space Telescope

## TL;DR

This study presents Hubble Space Telescope observations of WASP-121b's emission spectrum from 0.8 to 1.1 microns, revealing atmospheric properties, thermal inversion, and chemical composition through spectral retrieval analysis.

## Contribution

It extends the wavelength coverage of WASP-121b's emission spectrum and provides detailed atmospheric retrieval including thermal dissociation and ionization effects.

## Key findings

- Emission due to H- shortward of 1.1 micron
- No evidence for the previously reported 1.25 micron VO feature
- Estimated atmospheric metallicity and C/O ratio consistent with solar values

## Abstract

WASP-121b is a transiting gas giant exoplanet orbiting close to its Roche limit, with an inflated radius nearly double that of Jupiter and a dayside temperature comparable to a late M dwarf photosphere. Secondary eclipse observations covering the 1.1-1.6 micron wavelength range have revealed an atmospheric thermal inversion on the dayside hemisphere, likely caused by high altitude absorption at optical wavelengths. Here we present secondary eclipse observations made with the Hubble Space Telescope Wide Field Camera 3 spectrograph that extend the wavelength coverage from 1.1 micron down to 0.8 micron. To determine the atmospheric properties from the measured eclipse spectrum, we performed a retrieval analysis assuming chemical equilibrium, with the effects of thermal dissociation and ionization included. Our best-fit model provides a good fit to the data with reduced chi^2=1.04. The data diverge from a blackbody spectrum and instead exhibit emission due to H- shortward of 1.1 micron. The best-fit model does not reproduce a previously reported bump in the spectrum at 1.25 micron, possibly indicating this feature is a statistical fluctuation in the data rather than a VO emission band as had been tentatively suggested. We estimate an atmospheric metallicity of [M/H]=1.09(-0.69,+0.57), and fit for the carbon and oxygen abundances separately, obtaining [C/H]=-0.29(-0.48,+0.61) and [O/H]=0.18(-0.60,+0.64). The corresponding carbon-to-oxygen ratio is C/O=0.49(-0.37,+0.65), which encompasses the solar value of 0.54, but has a large uncertainty.