Adaptive optics Now: Soon: High angular resolution High contrast imaging Soon: Spectroscopy application Smaller instruments N E 1” 1” Credits: James R. Graham (UCB); ESO, T. Stolker et al.; Zurlo et al.

An Earth-like exoplanet in the Habitable Zone The Holy Grail: An Earth-like exoplanet in the Habitable Zone Exoplanets around low mass stars requirements: RV in the near IR Long term stability: 1m/s High spectral resolution HZ distances from Kopparapu et al. 2013

NIRPS: the red arm of HARPS AO injection module (Conod et al. 2016, SPIE): 0.4” fiber 50% encircled energy up to I=13 in best (25%) seeing condition (0.7”) Hardware available in april 2017 Validation and tests in prep. Spectrograph: 0.98-1.8 µm 100000 resolution Pressure / thermal control Sampling: 3-elements/LSF Very compact design HARPS Front-end HARPS Guiding Camera Wavefront Sensor: Shack-Hartmann 14x14 subapertures 15 pixels/subap readout noise < 0.3e- up to 2kHz 0.7-095 µm Atmospheric Dispersion Corrector Telescope light Deformable Mirror: ALPAO DM241 custom 15x15 actuators 10 µm stroke Settling time 800 µs Dichroic mirror NIRPS YJH Fiber Head Parabola R4 custom grating: 13 gr/mm Detector: Hawaii 4RG 4kx4k Prisms Camera lenses Mirror 1 m

NIRPS AO-fiber coupling Simulation of the coupling efficiency of the NIRPS AO PSF into the fibers: AO residual wavefront simulations: Analytical model of the fiber: NIRPS is one of the first application where we have to coupled an AO corrected PSF into small fibers. We performed some simulation of this coupling, using AO residual wavefront coupled with an analytical model of the fiber modes. The results are for a median seeing condition and I=10. We studied this due to the modal noise. Modal noise is a limitation fro the RV performances of the Spectrograph. Photo center moves and can induce fake radial velocities. Animation Nois is propto fiber size and lambda to the square, HARPS: 700nm NIRPS: 1550nm MODAL NOISE: # modes: NIRPS Fibers: 29 µm Wavelength: 0.98-1.8 µm