Planets around solar-type stars: Methods for detection and constraints on their distribution from an L' and M band adaptive optics imaging survey

Details Planets around solar-type stars: Methods for detection and constraints on their distribution from an L' and M band adaptive optics imaging survey Planets around solar-type stars: Methods for detection and constraints on their distribution from an L' and M band adaptive optics imaging survey

Aug 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007phdt........17h&link_type=abstract

Proquest Dissertations And Theses 2007. Section 0009, Part 0606 672 pages; [Ph.D. dissertation].United States -- Arizona: The U

Physics

Optics

4

Planets, Solar-Type Stars, Adaptive Optics Imaging, Extrasolar Planets

Scientific paper

We have attempted adaptive optics (AO) imaging of planets around nearby stars in the L' and M bands, using the Clio instrument on the MMT. The MMT AO system, with its deformable secondary mirror, offers uniquely low background AO- corrected images in these bands. This allowed us to explore a wavelength regime that has not been well utilized in searches for extrasolar planets, but offers some advantages over the more commonly used shorter-wavelength H band regime.
We have taken deep L' and M band images of the interesting debris disk stars Vega and e Eri. Our observations of e Eri attain better sensitivity to low mass planets within 3 arcseconds of the star than any other AO observations to date. At 1.7 arcsec, the maximum separation of the known planet e Eri b, our M band sensitivity corresponds to objects only 9-16 times brighter than the predicted brightness of this planet. M is by far the most promising band for directly imaging this planet for the first time, though Clio would require a multi-night integration.
We have carried out a survey of 50 nearby stars, using mostly the L' band. The survey objective was to determine whether power law fits to the statistics of planet mass m and orbital semimajor axis a from radial velocity (RV) surveys apply when extrapolated to orbital radii beyond the outer limits of RV sensitivity. Given dN/dm a m -1.44 , our survey null result rules out dN/daa a -0.2 extending beyond 155 AU, or dN/da constant extending beyond 70 AU, at the 95% confidence level. We have not placed as tight constraints on the planet distributions as the best H band surveys. However, we have probed older planet populations and by using a different wavelength regime have helped diversify results against model uncertainties.
We have developed careful and well-tested observing, image processing, sensitivity analysis, and source detection methods, and helped advance L' and M band AO astronomy. These wavelengths will become increasingly important with the advent of new giant telescopes sensitive to interesting, low-temperature planets with red H-L' and H-M colors.

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