Abstract
AbstractCARMENES (Calar Alto high-Resolution search for M dwarfs with Exo-earths with Near-infrared and optical Echelle Spectrographs) will conduct a radial-velocity survey of ~ 300 M dwarfs with the 3.5m telescope at the Calar Alto Observatory. The CARMENES instrument is currently under construction; it consists of two independent échelle spectrographs, which together cover the wavelength range 0.55 – 1.7μm at a spectral resolution of R = 82,000. The spectrographs and the fiber input are designed with a goal of 1m/s radial velocity precision using simultaneous calibration with emission-line lamps.
Highlights
M-type stars span the mass range of 0.1 – 0.6 M, and obtaining statistics of planetary system occurrence and architecture for these stars is of great importance for understanding the physics of planet formation and evolution, and its dependence on stellar host mass
Each spectrograph will be coupled to the 3.5 m telescope with its own optical fiber
The near-IR vacuum tank is equipped with a temperature stabilization system; the thermal design of both spectrographs provides the capability of keeping the temperature of the optical bench constant to within ±0.01 K over 24 h
Summary
M-type stars span the mass range of 0.1 – 0.6 M , and obtaining statistics of planetary system occurrence and architecture for these stars is of great importance for understanding the physics of planet formation and evolution, and its dependence on stellar host mass. Radial-velocity searches for planets around M dwarfs benefit from a large signal and a short orbital period of planets in the habitable zone, which provides an opportunity for finding habitable planets in the Solar neighborhood. The current number of planet detections with M-star hosts is still low, due to the faintness of the targets in the visible wavelength range and the intrinsic stellar jitter. Project (see Quirrenbach et al 2010, 2012) is aimed at filling this gap, by constructing a radial-velocity instrument optimized for planet searches of mid- to late-type M dwarfs
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