Searching Exoplanets around Vast M Dwarfs with InfraRed Exoplanets-Tracker

Details Searching Exoplanets around Vast M Dwarfs with InfraRed Exoplanets-Tracker Searching Exoplanets around Vast M Dwarfs with InfraRed Exoplanets-Tracker

Jan 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010aas...21547207w&link_type=abstract

American Astronomical Society, AAS Meeting #215, #472.07; Bulletin of the American Astronomical Society, Vol. 42, p.519

Astronomy and Astrophysics

Astronomy

Scientific paper

Exoplanets search programs using RV (radial velocity) technique have largely concentrated on main sequence stars with spectral types ranging from F to K. M dwarfs, which accounts for the largest population in local universe, are very faint to observe in optical band. However, there are several advantages in conducting exoplants survey around M dwarfs. First, they are less massive and have larger radial velocity induced by reflex motion. Second, HZ (habitable zone) is close in due to its low luminosity, which increases the chance of detecting planets in HZ. IR ET (Infrared Exoplanet Tracker) works in wavelength range from 0.8 to 1.35 micron, at which radiation from M dwarfs peak. In our simulation, it achieves 2.9 and 18.0 m/s RV precision for J band magnitude of 6 and 10 respectively assuming 16% instrument throughput. We have finished the work of interferometer for IR ET including manufacturing and testing. It is field compensated with more than 15 degree field of view and thermal stable which can achieve 0.5 m/s RV stability if temperature control reaches 1 mK precision. The group delay is precisely measured so that the barycentric RV correction error is down to less than 1 m/s. IR ET will be installed at APO 3.5m telescope in fall 2010. With its high precision and detection efficiency, we will be able to address the following fundamental questions: 1, what are the precise orbital solution, such as period, minimum mass and eccentricity. 2, what is the correlation between orbital elements and stellar properties such as stellar mass, spectral type and metallicity. 3, how does the correlation put constrains on planetary formation theory. The work is supported by W.M. Keck Foundation, NSF, UCF-UF SRI program and UF.

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