RV measurements of directly imaged brown dwarf GQ Lup B to search for exo-satellites

Katelyn Horstman; Jean-Baptiste Ruffio; Konstantin Batygin; Dimitri Mawet; Ashley Baker; Chih-Chun Hsu; Jason J. Wang; Ji Wang; Sarah Blunt; Jerry W. Xuan; Yinzi Xin; Joshua Liberman; Shubh Agrawal; Quinn M. Konopacky; Geoffrey A. Blake; Clarissa R. Do O; Randall Bartos; Charlotte Z. Bond; Benjamin Calvin; Sylvain Cetre; Jacques-Robert Delorme; Greg Doppmann; Daniel Echeverri; Luke Finnerty; Michael P. Fitzgerald; Nemanja Jovanovic; Ronald Lopez; Emily C. Martin; Evan Morris; Jacklyn Pezzato; Garreth Ruane; Ben Sappey; Tobias Schofield; Andrew Skemer; Taylor Venenciano; J. Kent Wallace; Nicole L. Wallack; Peter Wizinowich

arXiv · 2408.10299

RV measurements of directly imaged brown dwarf GQ Lup B to search for exo-satellites

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Abstract

GQ Lup B is one of the few substellar companions with a detected cicumplanetary disk, or CPD. Observations of the CPD suggest the presence of a cavity, possibly formed by an exo-satellite. Using the Keck Planet Imager and Characterizer (KPIC), a high contrast imaging suite that feeds a high resolution spectrograph (1.9-2.5 microns, R$\sim$35,000), we present the first dedicated radial velocity (RV) observations around a high-contrast, directly imaged substellar companion, GQ Lup B, to search for exo-satellites. Over 11 epochs, we find a best and median RV error of 400-1000 m/s, most likely limited by systematic fringing in the spectra due to transmissive optics within KPIC. With this RV precision, KPIC is sensitive to exomoons 0.6-2.8% the mass of GQ Lup B ($\sim 30 M_{\text{Jup}}$) at separations between the Roche limit and $65 R_{\text{Jup}}$, or the extent of the cavity inferred within the CPD detected around GQ Lup B. Using simulations of HISPEC, a high resolution infrared spectrograph planned to debut at W.M. Keck Observatory in 2026, we estimate future exomoon sensitivity to increase by over an order of magnitude, providing sensitivity to less massive satellites potentially formed within the CPD itself. Additionally, we run simulations to estimate the amount of material that different masses of satellites could clear in a CPD to create the observed cavity. We find satellite-to-planet mass ratios of $q > 2 \times 10^{-4}$ can create observable cavities and report a maximum cavity size of $\sim 51 \, R_{\text{Jup}}$ carved from a satellite.

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Katelyn Horstman, Jean-Baptiste Ruffio, Konstantin Batygin, Dimitri Mawet, Ashley Baker, Chih-Chun Hsu, Jason J. Wang, Ji Wang, Sarah Blunt, Jerry W. Xuan, Yinzi Xin, Joshua Liberman, Shubh Agrawal, Quinn M. Konopacky, Geoffrey A. Blake, Clarissa R. Do O, Randall Bartos, Charlotte Z. Bond, Benjamin Calvin, Sylvain Cetre, Jacques-Robert Delorme, Greg Doppmann, Daniel Echeverri, Luke Finnerty, Michael P. Fitzgerald, Nemanja Jovanovic, Ronald Lopez, Emily C. Martin, Evan Morris, Jacklyn Pezzato, Garreth Ruane, Ben Sappey, Tobias Schofield, Andrew Skemer, Taylor Venenciano, J. Kent Wallace, Nicole L. Wallack, Peter Wizinowich. 2024-08-19. RV measurements of directly imaged brown dwarf GQ Lup B to search for exo-satellites. https://arxiv.org/abs/2408.10299

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