In this resubmission we implemented dithering for the first two narrowband filter exposures
in Visits 01-02. We also use the full array for the long exposures at the end of every visit.
Also for these long exposures, we insert a SAME-POS command to point to the same
position as the shorter exposures which are using the M512C subarray.----- Attempting Submission 2 (Wed Aug 04 15:37:12 GMT 2010) -----We use the SAME POS command to put the science targets at the same CCD locatin
when switching from short exposure sub-array to long exposures on the full
UVIS array.Imaging accretion sources and circumbinary disks in young brown dwarfsWe propose to obtain deep WFC3/UVIS imaging observations of two accreting, nearby, young brown dwarf binaries. The first, 2M1207, is a brown dwarf with a planetary mass companion that became a benchmark in low-mass star formation and low-mass evolutionary models. The second, 2M0041, is a nearby young brown dwarf with clear evidence for accretion, but its space motion suggests a slightly higher age than the canonical accretion lifetime of 5-10 Myr. It has recently been discovered to be a binary and is likely to become a second benchmark object in this field. With narrow band images centered on the Halpha line that is indicative of accretion, we aim to determine the accretion ratio between the two components in each system. Halpha was observed in both systems but so far not spatially resolved. In particular, we want to search for accretion in the planetary mass companion of 2M1207. The evidence for accretion in 2M0041 and the possibility that it is in fact older than 10Myr suggests that the accretion lifetime is longer in brown dwarfs than in stars, and in particular that it is longer in brown dwarf binaries. Accretion could be sustained for a longer time if the accreting material is replenished by a circumbinary disk that might exist in both systems. We propose deep WFC/UVIS observations in the optical to search for circumbinary disks, similar to the famous disk around the binary TTauri system GG Tau.This program aims to detect H-alpha from young, low mass objects and produce a high-contrast imageof the environment to detect circumstellar disks. To minimize buffer overheads, the H-alpha portion of the experiment uses a 512x512 subarray. The longer exposures for circumstellar material in optical scattered light utilize the F606W filter with a 2Kx2K subarray. For PSF subtraction, we use several rolls for each of the two sources (2M0041 and 2M1207).For optimal PSF subtraction, the orbits (for each of the two sources) should be consecutive orbits. We specify GROUP WITHIN and ORIENT FROM commands. The ORIENT FROM should be the maximum allowable (typically 30 degrees).STAR FORMATION12false0.00.0falsefalsefalsefalsefalsefalseSUPPORTEDSTARBROWN DWARFThis object was generated by the targetselector and retrieved from the SIMBAD database.J200012 07 33.4700-39 32 54.00J2000STARBROWN DWARFThis object was generated by the targetselector and retrieved from the SIMBAD database.J200000 41 35.3900-56 21 12.77J2000WFC3/UVISImagingNoNoF606WWFC3/UVISImagingNoNoF656NWFC3/UVISImagingNoNoF606WWFC3/UVISImagingNoNoF656NPOS-TARGDITHER0.135LINEfalsefalse346.84LINE1falseTiming link suitability includes constraints ([Group (01 02) Within 0.1 days])The scheduling data was generated by CASM 18.3.1.CASM was run in Phase II mode./private/var/folders/ve/vewOJg+6FJaP0Vbvh0dD0k+++TI/-Tmp-/OPVisit4964587597622447816.xml(Tic-Visit
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