An L' and M-band AO Imaging Survey for Extrasolar Giant Planets: Progress and Preliminary Results

Details An L' and M-band AO Imaging Survey for Extrasolar Giant Planets: Progress and Preliminary Results An L' and M-band AO Imaging Survey for Extrasolar Giant Planets: Progress and Preliminary Results

Dec 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006aas...20922603h&link_type=abstract

2007 AAS/AAPT Joint Meeting, American Astronomical Society Meeting 209, #226.03; Bulletin of the American Astronomical Society,

Physics

Optics

1

Scientific paper

Self luminous extrasolar giant planets can in principle be imaged by ground based telescopes equipped with adaptive optics (AO) systems at a variety of infrared wavelengths. The H band (1.6 microns) has been most widely used in surveys for such planets. However, interesting complementary results can be obtained with observations at longer wavelength, in particular the L' band (3.8 microns). We summarize our technique, and describe preliminary results. Our survey is complementary to other work in that we observe nearby, older stars, while H band surveys target younger stars that tend to be more distant. This division of targets comes about because the H band planet/star brightness ratio falls quickly as planets age and cool, while the same ratio in L' remains more favorable for older stars. Because our target sample is comprised of stars closer to the sun, we are sensitive to planets in orbits as close-in as our own Jupiter and Saturn. We have chosen F through early M stars as our survey targets to match (roughly) the samples of radial velocity surveys. This should allow us to constrain the observed distributions of planets as a function of planetary mass and orbital radius and compare with results for closer-in planets from radial velocity surveys. Our sample consists of about 50 stars within 25pc, with ages from 0.1 to about 2 Gyr, chosen so that our predicted sensitivity limit for each target corresponds to less than 10 Jupiter masses. To date, we have completed about half of our survey, and have developed careful strategies to maximize sensitivity and detect and characterize any real sources. We report on these, and on the sensitivity we have obtained.

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