1. 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.

2. 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

3. 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: µm
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 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

4. 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: µm