Cloud Structure of the Nearest Brown Dwarfs II: High-amplitude variability for Luhman 16 A and B in and out of the 0.99 micron FeH feature

TL;DR

This study presents the first spectroscopic variability observations of the nearby brown dwarf binary Luhman 16AB, revealing significant variability and providing insights into cloud structures and their impact on observed features.

Contribution

It reports the first detection of variability in Luhman 16A and analyzes the spectral behavior of both components, advancing understanding of brown dwarf cloud dynamics.

Findings

Significant variability detected in both Luhman 16A and B.

Variability amplitudes of 9.3% and 4.5% respectively.

No variability observed across the 0.99 μm FeH feature.

Abstract

The re-emergence of the 0.99 $\mu$m FeH feature in brown dwarfs of early- to mid-T spectral type has been suggested as evidence for cloud disruption where flux from deep, hot regions below the Fe cloud deck can emerge. The same mechanism could account for color changes at the L/T transition and photometric variability. We present the first observations of spectroscopic variability of brown dwarfs covering the 0.99 $\mu$m FeH feature. We observed the spatially resolved very nearby brown dwarf binary WISE J104915.57-531906.1 (Luhman 16AB), a late-L and early-T dwarf, with HST/WFC3 in the G102 grism at 0.8-1.15 $\mu$m. We find significant variability at all wavelengths for both brown dwarfs, with peak-to-valley amplitudes of 9.3% for Luhman 16B and 4.5% for Luhman 16A. This represents the first unambiguous detection of variability in Luhman 16A. We estimate a rotational period between 4.5 and 5.5 h, very similar to Luhman 16B. Variability in both components complicates the interpretation of spatially unresolved observations. The probability for finding large amplitude variability in any two brown dwarfs is less than 10%. Our finding may suggest that a common but yet unknown feature of the binary is important for the occurrence of variability. For both objects, the amplitude is nearly constant at all wavelengths except in the deep K I feature below 0.84 $\mu$m. No variations are seen across the 0.99 $\mu$m FeH feature. The observations lend strong further support to cloud height variations rather than holes in the silicate clouds, but cannot fully rule out holes in the iron clouds. We re-evaluate the diagnostic potential of the FeH feature as a tracer of cloud patchiness.