# Mapping atmospheric features of the planetary-mass brown dwarf SIMP 0136 with JWST NIRISS

## TL;DR

This study uses JWST NIRISS data to map atmospheric features of the brown dwarf SIMP 0136, revealing complex variability, multiple atmospheric layers, and asymmetries, and introduces new analysis methods for atmospheric characterization.

## Contribution

It presents a detailed atmospheric mapping of SIMP 0136 using innovative spectral and brightness mapping techniques, advancing brown dwarf atmospheric studies.

## Key findings

- 81% of spectral variations explained by two components
- Time-averaged spectrum requires at least three atmospheric regions
- Brightness maps show North-South atmospheric asymmetry

## Abstract

In this paper, we analyze James Webb Space Telescope Near Infrared Imager and Slitless Spectrograph time-series spectroscopy data to characterize the atmosphere of the planetary-mass brown dwarf SIMP J01365662+093347. Principal component analysis reveals that 81\% of spectral variations can be described by two components, implying that variability within a single rotational phase is induced by at least three distinct spectral regions. By comparing our data to a grid of Sonora Diamondback atmospheric models, we confirm that the time-averaged spectrum cannot be explained by a single model but require a linear combination of at least three regions. Projecting these models onto the principal component plane shows that the overall variability is highly correlated with changes in temperature, cloud coverage, and possibly effective metallicity. We also extract brightness maps from the lightcurve and establish North-South asymmetry in the atmosphere. A combined multidimensional analysis of spectro-photometric variability links the three spectral regions to three atmospheric layers. Forsterite cloud and water abundance at each level form unique harmonics of atmospheric variability observed in different spectral bands. Atmospheric retrievals on the time-averaged spectrum are consistent with an optically thick iron cloud deck beneath a patchy forsterite cloud layer and with the overall adiabatic curve. We also demonstrate two new analysis methods: a regionally-resolved spectra retrieval that relies on multi-wavelength spherical harmonics maps, and a method to constrain brightness maps using Doppler information present in the spectra. Future observations of variable brown dwarfs of higher spectral resolution or spanning multiple rotations should help break mapping degeneracy.