# Simulating Radial Velocity Observations of Trappist-1 with SPIRou

## TL;DR

This study simulates radial velocity observations of the TRAPPIST-1 system with SPIRou, highlighting challenges posed by stellar activity signals and proposing bi-site observations to improve planet mass estimations.

## Contribution

It demonstrates the impact of stellar activity on RV measurements of TRAPPIST-1 and suggests observational strategies to mitigate these effects for better planet characterization.

## Key findings

- Stellar activity signals can overshadow planetary signals in RV data.
- White noise impacts mass estimates for some planets.
- Bi-site observations improve filtering of stellar activity signals.

## Abstract

We simulate a radial velocity (RV) follow-up of the TRAPPIST-1 system, a faithful representative of M dwarfs hosting transiting Earth-sized exoplanets to be observed with SPIRou in the months to come. We generate a RV curve containing the signature of the 7 transiting TRAPPIST-1 planets and a realistic stellar activity curve statistically compatible with the light curve obtained with the K2 mission. We find a +/-5 m/s stellar activity signal comparable in amplitude with the planet signal. Using various sampling schemes and white noise levels, we create time-series from which we estimate the masses of the 7 planets. We find that the precision on the mass estimates is dominated by (i) the white noise level for planets c, f and e and (ii) the stellar actvitity signal for planets b, d and h. In particular, the activity signal completely outshines the RV signatures of planets d and h that remain undetected regardless of the RV curve sampling and level of white noise in the dataset. We find that a RV follow-up of TRAPPIST-1 using SPIRou alone would likely result in an insufficient coverage of the rapidly evolving activity signal of the star, especially with bright-time observations only, making statistical methods such as Gaussian Process Regression hardly capable of firmly detecting planet f and accurately recovering the mass of planet g. In contrast, we show that using bi-site observations with good longitudinal complementary would allow for a more accurate filtering of the stellar activity RV signal.