JWST unveils a high mean molecular weight atmosphere for mini-Neptune TOI-1130b: Evidence for formation beyond the water ice line

Abstract

We present the combined JWST/NIRSpec G395H and NIRISS SOSS transmission spectrum of a warm mini-Neptune, TOI-1130b (3.66 R${}_{\oplus }$, 19.8 M${}_{\oplus }$, $T_{eq}\sim 825$ K). It is part of a rare and unique multi-planet system TOI-1130, which hosts an inner mini-Neptune and an outer hot Jupiter locked in a 2:1 mean motion resonance. From the transmission spectrum of TOI-1130b we detect multiple molecules -- H${}_2$O (7.5$\ddot{I}ƒ$), CO${}_2$ (3.3$\ddot{I}ƒ$), and SO${}_2$ (3.6$\ddot{I}ƒ$), as well as a tentative detection of CH${}_4$ ($\sim$2$\ddot{I}ƒ$). We find a strong optical slope in the NIRISS/SOSS spectrum, which is consistent with TESS and CHEOPS transit depth measurements. From equilibrium chemistry retrievals we measure the atmospheric metallicity ($\log Z/Z_{\odot }=1.8_{-0.3}^{+0.4}$) and C/O ratio ($<$0.75 at 3$\ddot{I}ƒ$ level confidence) and constrain the atmospheric mean molecular weight, $\hat{I}¼$ = 5.5${}_{-0.8}^{+1.3}$ amu. These constraints are consistent with self-consistent forward model grids. We detect no significant He I 1.083$\hat{I}¼$m absorption signal and put a mass-loss rate upper limit of $10^{11}$g\s${}^{-1}$. The volatile-rich high mean molecular weight atmosphere of TOI-1130b along with the `pebble-filtering' effect of the outer hot Jupiter supports the ex-situ formation scenario beyond the water ice line and subsequent migration, coherent with its present orbital architecture. A volatile-rich formation scenario could also potentially explain the location of TOI-1130b at the edge of the `radius cliff'. This result hints that the mini-Neptune population may not a homogeneous formation history; rather, volatile-rich ex-situ formation also contributes to its population.

Accepted ApJ Letters