A Search for Giant Planet Companions to T Tauri Stars

TL;DR

This study uses multiwavelength radial velocity measurements to distinguish between stellar activity and potential planetary signals in young T Tauri stars, aiming to identify early giant planet companions.

Contribution

It introduces a multiwavelength RV survey approach to differentiate stellar activity from planetary signals in very young stars, addressing challenges of magnetic activity.

Findings

RV amplitude decreases at longer wavelengths by a factor of 2-3.

Three targets show different periodicities in optical and infrared, indicating different variability mechanisms.

Demonstrated capability to detect hot Jupiters and trends from distant companions using infrared RV measurements.

Abstract

We present results from an ongoing multiwavelength radial velocity (RV) survey of the Taurus-Auriga star forming region as part of our effort to identify pre--main sequence giant planet hosts. These 1-3 Myr old T Tauri stars present significant challenges to traditional RV surveys. The presence of strong magnetic fields gives rise to large, cool star spots. These spots introduce significant RV jitter which can mimic the velocity modulation from a planet-mass companion. To distinguish between spot-induced and planet-induced RV modulation, we conduct observations at ~6700 Angstroms and ~2.3 microns and measure the wavelength dependence (if any) in the RV amplitude. CSHELL observations of the known exoplanet host Gl 86 demonstrate our ability to detect not only hot Jupiters in the near infrared but also secular trends from more distant companions. Observations of nine very young stars reveal a typical reduction in RV amplitude at the longer wavelengths by a factor of ~2-3. While we can not confirm the presence of planets in this sample, three targets show different periodicities in the two wavelength regions. This suggests different physical mechanisms underlying the optical and K band variability.