Hot Rocks Survey IV: Emission from LTT 3780 b is consistent with a bare rock

TL;DR

This study presents MIRI observations of LTT 3780 b, indicating its emission is consistent with a bare rock surface and ruling out certain atmospheric compositions, thus informing theories on small planet atmospheres around M dwarfs.

Contribution

First direct emission measurement of LTT 3780 b showing it likely lacks a substantial atmosphere, advancing understanding of rocky exoplanet atmospheres around M dwarfs.

Findings

Eclipse depth of 312±38 ppm consistent with a bare rock surface.

Ruled out CO₂ atmospheres above 0.01 bar with >3σ confidence.

Detected thermal emission matching a dayside temperature of approximately 1143 K.

Abstract

It is an open question whether small planets around M dwarfs are able to maintain atmospheres. The Hot Rocks Survey aims to address this question by observing 9 rocky exoplanets orbiting M dwarfs with MIRI emission photometry to constrain the onset of atmospheres. In this paper, we present two MIRI F1500W (15$\mu$m) eclipses of LTT 3780 b, an ultra-short period super-Earth ($P=0.768$ d, $R=1.325 \,R_\oplus$, $M = 2.46\,M_\oplus$) that receives 111x Earth's instellation, the highest in the survey. We find a combined eclipse depth of $312\pm38$ ppm, which is consistent between different data reduction and analysis assumptions, bolstering our confidence in the eclipse detection. This eclipse depth is consistent with the thermal emission from a bare rock surface, with a dayside temperature of $T_d=1143^{+104}_{-99}$ K, $98\pm9$ % of the maximum temperature predicted for a zero albedo, zero heat redistribution blackbody. We are able to confidently rule out CO$_2$-based atmospheres down to 0.01 bar surface pressure to greater than 3$\sigma$ (ruling out an approximately Mars-like atmosphere). We are unable to rule out a pure H$_2$O 1 bar atmosphere, though we argue that this composition is unlikely on such a highly irradiated planet, nor O$_2$ atmospheres due to the lack of features in the bandpass, though we can put constraints on CO$_2$-mixture atmospheres. As a potential bare rock, we consider a variety of surface composition models, but are unable to distinguish between them. However, LTT 3780 b is an excellent target for follow-up JWST observations to determine its surface composition and rule out additional atmospheric compositions.