collaborators

6 papers

astro-ph.EP2026

Super-Earth masses and stellar abundances from NIRPS reveal tentative evidence for water-rich formation around M dwarfs

Drew Weisserman, Nicole Gromek, Ryan Cloutier +98

Tracing the compositional link between terrestrial super-Earths and their host stars provides clues to their dominant formation pathway. By constraining the stellar abundances of r…

astro-ph.EP2026

NIRPS tightens the mass estimate of GJ 3090 b and detects a planet near the stellar rotation period

Pierrot Lamontagne, Drew Weisserman, Charles Cadieux +148

We present an updated characterization of the planetary system orbiting the nearby M2 dwarf GJ 3090 (TOI-177; pc), based on new high-precision radial velocity (RV) observa…

astro-ph.EP2025

NIRPS and TESS reveal a peculiar system around the M dwarf TOI-756: A transiting sub-Neptune and a cold eccentric giant

Léna Parc, François Bouchy, Neil J. Cook +148

The Near InfraRed Planet Searcher (NIRPS) joined HARPS on the 3.6-m ESO telescope at La Silla Observatory in April 2023, dedicating part of its Guaranteed Time Observations (GTO) p…

astro-ph.IM2025

NIRPS joining HARPS at ESO 3.6 m. On-sky performance and science objectives

Francois Bouchy, Rene Doyon, Francesco Pepe +131

The Near-InfraRed Planet Searcher (NIRPS) is a high-resolution, high-stability near-infrared (NIR) spectrograph equipped with an AO system. Installed on the ESO 3.6-m telescope, it…

astro-ph.EP2025

Diving into the planetary system of Proxima with NIRPS -- Breaking the metre per second barrier in the infrared

Alejandro Suárez Mascareño, Étienne Artigau, Lucile Mignon +138

We obtained 420 high-resolution spectra of Proxima, over 159 nights, using the Near Infra Red Planet Searcher (NIRPS). We derived 149 nightly binned radial velocity measurements wi…

astro-ph.EP2025

Blind search for activity-sensitive lines in the near-infrared using HARPS and NIRPS observations of Proxima and Gl 581

João Gomes da Silva, Elisa Delgado-Mena, Nuno C. Santos +145

Stellar activity variability is one of the main obstacles to the detection of Earth-like planets using the RV method. The aim of this work is to measure the effect of activity in t…