Evidence for He I 10830 \AA~ absorption during the transit of a warm Neptune around the M-dwarf GJ 3470 with the Habitable-zone Planet Finder

TL;DR

This study presents the first evidence of Helium I 10830 Å absorption in the atmosphere of a warm Neptune orbiting an M-dwarf, using ground-based spectroscopy, revealing atmospheric outflow characteristics.

Contribution

It reports the detection of Helium I 10830 Å absorption in an M-dwarf exoplanet's atmosphere and models the exosphere based on UV and X-ray flux assumptions.

Findings

Detected broad He I 10830 Å absorption with a blueshifted wing to -36 km/sec

Measured the column density of metastable Helium as 2.4 x 10^{10} cm^{-2}

First evidence of this absorption feature in an M-dwarf exoplanet atmosphere.

Abstract

Understanding the dynamics and kinematics of out-flowing atmospheres of hot and warm exoplanets is crucial to understanding the origins and evolutionary history of the exoplanets near the evaporation desert. Recently, ground based measurements of the meta-stable Helium atom's resonant absorption at 10830 \AA~has become a powerful probe of the base environment which is driving the outflow of exoplanet atmospheres. We report evidence for the He I 10830 \AA~in absorption (equivalent width $\sim$ $0.012 \pm 0.002$ \AA) in the exosphere of a warm Neptune orbiting the M-dwarf GJ 3470, during three transits using the Habitable Zone Planet Finder (HPF) near infrared spectrograph. This marks the first reported evidence for He I 10830 \AA\, atmospheric absorption for a planet orbiting an M-dwarf. Our detected absorption is broad and its blueshifted wing extends to -36 km/sec, the largest reported in the literature to date. We modelled the state of Helium atoms in the exosphere of GJ3470b based on assumptions on the UV and X-ray flux of GJ 3470, and found our measurement of flux-weighted column density of meta-stable state Helium $(N_{He^2_3S} = 2.4 \times 10^{10} \mathrm{cm^{-2}})$, derived from our transit observations, to be consistent with model, within its uncertainties. The methodology developed here will be useful to study and constrain the atmospheric outflow models of other exoplanets like GJ 3470b which are near the edge of the evaporation desert.