A Portrait of the Rotation of Ultra-cool Dwarfs Revealed by TESS

Abstract

This study presents the results of a search for rotation signatures in 250 Gaia Data Release 3 ultra-cool dwarfs (UCDs) with TESS light curves (LCs). We identified 71 targets with unambiguous periodicities, of which 61 present rotation signatures and a single-source behavior, with periods between 0.133 and 5.81 days. Five UCDs show double-dip features, namely variations with two periods, one approximately double or half the other. The remaining 10 UCDs with unambiguous variability present a likely nonsingle behavior. We also found 20 UCDs showing complex behavior in their LCs, with noticeable fluctuations and irregular structure, with a few exhibiting apparent changes in their temporal structure. The remaining 159 targets show noisy LCs corresponding to low-amplitude signals, whose temporal variation cannot be easily identified. The distribution of the UCDs with rotation signature in a color–magnitude diagram points to a lack of rotating objects within about 11.5 < M _G < 12.5 and G – G _RP < 1.5, separating them into two regimes, one mainly composed of less massive late-M stars with P _rot ≥ 1.0 day, and another mainly composed of more massive early-M stars with P _rot < 1.0 day. It is important to emphasize that by separating stars into age intervals, one observes that UCDs with P _rot ≥ 1.0 day tend to be located in regions of younger objects, and, in contrast, those with P _rot < 1.0 day are mainly concentrated in regions of older objects. Whether this trend of stars contrasting the sample separation is physical or produced by observational biases is a question to be verified in future studies.

Keywords

• Low mass stars
• Stellar rotation
• Brown dwarfs
• Stellar photometry
• Space observatories
• Stellar astronomy