Removed link between visits 01 and 02 due to closely spaced observing opportunities. -2053754590 ----- Attempting Submission 4 (Fri May 17 20:21:59 GMT 2013) ----- ----- Attempting Submission 5 (Mon Jul 22 20:20:17 GMT 2013) ----- In house processing Extrasolar Storms: The Physics and Chemistry of Evolving Cloud Structures in Brown Dwarf Atmospheres Condensate clouds pose the most significant challenge to the understanding of ultracool atmospheres of brown dwarfs and giant exoplanets. In three ongoing Spitzer programs we have taken advantage of Spitzer's ability to obtain high-cadence uninterrupted observations to pioneer a new technique, rotational phase mapping, and successfully explored the properties of cloud covers in ~50 brown dwarfs. Among other exciting results we found that most brown dwarfs possess heterogeneous cloud cover, often with complex surface structures. Perhaps the most perplexing behavior seen in our surveys is light curve evolution on timescales as short as 5 hours and as long as a year. This unexpected behavior offers a unique opportunity to explore the dynamics of cloud layers, but requires multi-epoch data sets. We propose here to follow up a representative set of varying brown dwarfs via multi-epoch Spitzer and HST phase mapping to carry out the first quantitative exploration of cloud cover evolution. The proposed study will establish the first time-resolved multi-wavelength light curve library for brown dwarfs. Spitzer uniquely offers precise 3-5 micron photometry and continuous coverage that allow us to detect cloud structures a fraction of the size of the Great Red Spot on Jupiter in our targets. Combined with HST grism spectroscopy during a subset of the Spitzer observations, the Spitzer phase maps will allow us to disentangle the effects of cloud formation, differential rotation, large-scale rainout and dispersal of clouds. As different wavelengths probe different pressures and different rotational phases probe different latitudes we will be able to explore the two or even three-dimensional structure of the atmospheres. We will also constrain the dynamical and radiative timescales for brown dwarfs and compare these to theoretical predictions to identify the underlying atmospheric dynamics. This program will leave a unique legacy that will propel studies of ultracool atmosphere studies into a new era. This proposal will obtain time-resolved WFC3 grism spectra of brown dwarfs. Each target will be observed in two visits, with 3 or 4 orbits per visit depending on the target's rotational period. Because the observations aim to cover entire rotation periods of the sources it is critical that the observations in a given visit are scheduled back-to-back. All targets are also observed with Spitzer in eight separate visits, and the HST scheduling must be coordinated in such a way that the HST visits take place during the longer Spitzer visits. For each target there are 8 long Spitzer visits and two shorter HST visits and the HST visits can take place during any two of the Spitzer visits. Please, coordinate with the PI and the SSC regarding the optimal windows. Our team has prepared a detailed analysis of the Spitzer windows and possible scheduling opportunities to help the HST-Spitzer coordination. Thank you, Daniel Apai EXTRA-SOLAR PLANETS 12 false false 0.0 0.0 false false false SUPPORTED STAR BROWN DWARF J2000 J2000 J=13.45 STAR BROWN DWARF Sp Type=T6.5 Proper Motion: 0.31"/yr (175degree) Burgasser et al. 2003 Current Position from WISE J2000 J2000 J=15.6 STAR BROWN DWARF Proper motion from Kirkpatrick et al. 2010, ApJS 190 100 Current position from WISE J2000 J2000 J=13.43 H=12.39 K=11.65 STAR BROWN DWARF Current position from WISE J2000 J2000 J=12.83, K=11.31 WFC3/IR Spectroscopic No No G141 WFC3/IR Spectroscopic No No G141 WFC3/IR Spectroscopic No No G141 WFC3/IR Spectroscopic No No G141 WFC3/IR Spectroscopic No No G141 WFC3/IR Spectroscopic No No G141 WFC3/IR Spectroscopic No No G141 WFC3/IR Spectroscopic No No G141 Timing link suitability includes constraints ([02 After 01 by 4.0 to 3650.0 days]) The scheduling data was generated by CASM 21.2. CASM was run in Phase II mode. 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Must be coordinated with Spitzer IRAC observations Direct Image in F132N to help wavelength calibration. Must be coordinated with Spitzer IRAC observations Direct Image in F132N to help wavelength calibration. Must be coordinated with Spitzer IRAC observations Timing link suitability includes constraints ([02 After 01 by 4.0 to 3650.0 days]) The scheduling data was generated by CASM 21.2. 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Must be coordinated with Spitzer IRAC observations Direct Image in F132N to help wavelength calibration. Using the same POS TARG as for the G141 observations Must be coordinated with Spitzer IRAC observations Direct Image in F132N to help wavelength calibration. Must be coordinated with Spitzer IRAC observations Timing link suitability includes constraints ([04 After 03 by 15.0 to 3650.0 days]) The scheduling data was generated by CASM 21.0. 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Must be coordinated with Spitzer IRAC observations Direct Image in F132N to help wavelength calibration. Must be coordinated with Spitzer IRAC observations Direct Image in F132N to help wavelength calibration. Must be coordinated with Spitzer IRAC observations Direct Image in F132N to help wavelength calibration. Must be coordinated with Spitzer IRAC observations Timing link suitability includes constraints ([06 After 05 by 15.0 to 3650.0 days]) The scheduling data was generated by CASM 21.0. CASM was run in Phase II mode. 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Must be coordinated with Spitzer IRAC observations Direct Image in F132N to help wavelength calibration. Must be coordinated with Spitzer IRAC observations Direct Image in F132N to help wavelength calibration. Must be coordinated with Spitzer IRAC observations Timing link suitability includes constraints ([06 After 05 by 15.0 to 3650.0 days]) The scheduling data was generated by CASM 21.0. CASM was run in Phase II mode. 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Must be coordinated with Spitzer IRAC observations Direct Image in F132N to help wavelength calibration. Must be coordinated with Spitzer IRAC observations Direct Image in F132N to help wavelength calibration. Must be coordinated with Spitzer IRAC observations Direct Image in F132N to help wavelength calibration. Must be coordinated with Spitzer IRAC observations Timing link suitability includes constraints ([08 After 07 by 15.0 to 3650.0 days]) The scheduling data was generated by CASM 21.0. 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Using the same POS TARG as for the G141 observations Must be coordinated with Spitzer IRAC observations Direct Image in F132N to help wavelength calibration. Must be coordinated with Spitzer IRAC observations Direct Image in F132N to help wavelength calibration. Must be coordinated with Spitzer IRAC observations Direct Image in F132N to help wavelength calibration. Must be coordinated with Spitzer IRAC observations