Exoclimes_Conference_booklet1

instrument "MagAO" in December 2012, simultaneously with our visible-light and infrared
cameras. I will present my MagAO imaging data of Beta Pic b at 5 passbands, providing a
fuller picture of the planet's spectral energy distribution. This broad wavelength coverage
will be crucial to determining the energy balance of new exoplanets as improved AO
technology allows direct imaging to probe closer separations and lower masses. MagAO is
unique in achieving diffraction-limited imaging from 0.6-5 microns, and will be vital to
characterizing these planetary systems.
The Mid-Infrared Properties of Directly-Imaged Exoplanets
Andrew Skemer — University of Arizona!
Self-luminous exoplanets emit the majority of their photons in the mid-infrared (>3 micron).
However, the difficulty of working in the thermal infrared from the ground has precluded the
detailed studies of exoplanets at these longer wavelengths.
Using the low-emissivity adaptive optics systems at the LBT and Magellan, we present 6
new photometric points on the HR 8799 planets and 1 new photometric point on 2M1207
b. These data probe the 3-4 micron region where previous studies have found a 1-2
magnitude discrepancy between their atmospheres and field brown dwarfs. For the HR
8799 planets, we find a shallow 3-4 micron slope with only a hint of possible absorption in
the methane 3.3 micron fundamental absorption band (possibly indicating the presence of
patchy clouds). For 2M1207 b we find a similar if more extreme behavior, with no sign of
methane absorption.
The study has implications for understanding the broad properties of extrasolar giant
planets, and suggests that future mid-infrared direct-imaging searches (particularly JWST)
may need to reconsider their search strategy.
A large near-IR photometric monitoring survey of 69 ultracool L &T brown dwarfs
Paul Anthony!Wilson — University of Exeter
As the brown dwarf atmosphere cools through the L-T spectral sequence a rapid shift from
the red to the blue colours are observed across the L-T type transition. This shift in colour
happens across a narrow effective temperature range, which is hard for 1-D atmosphere
models to currently reproduce. Patchy clouds might be the explanation of the rapid change
in colour observed over a narrow temperature range. The consequence of patchy clouds
would be variations in the observed flux due to the rotation and evolution of the clouds.
I will present the results from our large near-IR photometric monitoring campaign which
covers 69 ultracool L & T type brown dwarfs. In particular I will discuss the frequency and
amplitude of variability across the different spectral types highlighting that our survey finds
new large amplitude variables across the L - T spectral range showing no preference for
the transition. I will also talk about observing variability at the much cooler T-Y transition.
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