Brown dwarf atmosphere intensity grid produced by PICASO radiative transfer code and based on Sonora model atmospheres

Specific intensity in erg s^−1 Hz^−1 sr^−1 cm^−2 on a grid of the cosine of the viewing angle 𝜇 = cos 𝜙, wavelength 𝜆, surface effective temperature, and surface gravitational acceleration that was computed from the Sonora pressure-temperature and abundance profiles, using version 2.3 of the open source code PICASO (Batalha et al. 2019; Batalha et al. 2022), which has previously been used to compute the thermal emission spectra of brown dwarfs (e.g. Mang et al. 2022) and exoplanets (e.g. Robbins-Blanch et al. 2022).

This grid served as input to software PARS (Paint the Atmospheres of Rotating Stars; Lipatov and Brandt 2020) in an article that predicts the observational effects of rotation in brown dwarfs (Lipatov, Brandt, and Batalha 2022).