0 Assigned ID: 724 ----- Attempting Submission 1 (Fri Apr 10 19:44:05 GMT 2015) ----- HST Phase I Proposal 724 (HST_LHS6343_loic.pdf.apt) successfully submitted. Receipt: # 724-1 ----- Attempting Submission 2 (Fri Apr 10 19:56:41 GMT 2015) ----- HST Phase I Proposal 724 (HST_LHS6343_loic.pdf.apt) successfully submitted. Receipt: # 724-2 ----- Attempting Submission 3 (Fri Apr 10 20:09:42 GMT 2015) ----- Minor comments or questions: 1) Could I narrow my starting phase even more (to +/-10 minutes) without loss of scheduling ability? 2) Is it a problem if I itemized the forward and reverse scans rather than use the "round trip"? 3) I am cutting it too tight, leaving ~15 seconds or less before occultation starts? 4) Peter McCullough works, even at his vacation cottage :-) -1632415341 ----- Attempting Submission 1 (Thu Jul 23 20:46:13 GMT 2015) ----- As the number of field Brown Dwarfs counts in the thousands, interpreting their physical parameters (mass, temperature, radius, luminosity, age, metallicity) relies as heavily as ever on atmosphere and evolutionary models. Fortunately, models are largely successful in explaining observations (colors, spectral types, luminosity), so they appear well calibrated in a relative sense. However, an absolute model-independent calibration is still lacking. Eclipsing BDs systems are a unique laboratory in this respect but until recently only one such system was known, 2M0535-05 -- a very young (<3 Myr) binary Brown Dwarfs showing a peculiar temperature reversal (Stassun et al. 2006). Due to its young age, 2M0535-05 is an ill-suited test for Gyr-old field Brown Dwarfs whose population is by far the most common in the solar neighborhood. Recently, a second system -- an evolved BD (>1 Gyr) -- was identified (62.1+/-1.2 MJup, 0.783+/-0.011 RJup) transiting LHS6343 with a 12.7-day period. We propose to use WFC3 in drift scan mode and 5 HST orbits to determine the spectral type (a proxy for temperature) as well as the near-infrared luminosity of this brown dwarf. We conducted simulations that predict a signal-to-noise ratio ranging between 10 and 30 per resolution element in the peaks of the spectrum. These measurements, coupled with existing luminosity measurements with Spitzer at 3.6 and 4.5 microns, will allow us to trace the spectral energy distribution of the Brown Dwarf and directly calculate its blackbody temperature. It will be the first field Brown Dwarfs with simultaneous measurements of its radius, mass, luminosity and temperature all measured independently of models. I want to use WFC3 in scan mode to measure the secondary eclipse of a brown dwarf (LHS6343 C) around LHS6343 A. There is a nearby (0.55") binary (LHS6343 B) that I want to position along the spectral dispersion axis so that A and B spectra overlap from the start of the scan. Also, to establish the respective individual spectra of A and B, I want to take staring spectra of each individual component. Finally, I also want to obtain a direct image at the start of every orbit to establish the wavelength solution zero-point. COOL STARS 12 false false false false SUPPORTED STAR BROWN DWARF M V-IV This object was generated by the targetselector and retrieved from the SIMBAD database. LHS6343 A is an M3 dwarf around which a Brown Dwarf (LHS 6343 C) orbits on a 12.7 day period. It is an eclipsing brown dwarf. At 0.6 arcsec is a second M3 dwarf (LHS 6343 B), bound to the system. The B component has a position angle of 118 degrees (east of north, CCW) relative to the A component. J2000 J2000 J=9.57 H=8.97 K=8.70 WFC3/IR Spectroscopic No No G141 POS-TARG DITHER 0.572 LINE 0.365 false false 74.653 4 18.528 WFC3-IR-DITHER-BOX-MIN 1 false 1437684345080 /private/var/folders/zm/vg6r39lx1972d1zlfn24_hqh0000gn/T/OPVisit2069000618715019059.xml The scheduling data was generated by CASM 23.2. CASM was run in Phase II mode. I want to observe the secondary eclipse of a BD (component C) orbiting an M3 dwarf (component A). A second M3 (component B) star is found ~0.6 arcsec at a position angle of 118 degrees (East of North CCW) with respect to component A. The scanning spectroscopy will have all components blended. But I will want to obtain crude resolved spectroscopy and photometry of both stars. At the begining of orbit 1, I obtain a direct image (F130N) and a staring grism spectrum, at each of 4 dither positions. That builds up to 48 sub-array (256x256) reads (the max that can then be dumped in parallel during the scanning exposure). At the very end of orbit 1, I insert a short direct imaging F130N at the same X,Y position as where my scans start (X=0.0",Y=-1.5"). My scanning exposures use 16 reads (NSAMP=15) and I itemize each forward then reverse scans. They are dumped every 3 scans (i.e. every time a cumulative 48 reads have been performed). My scans starts at X=0.0", Y=-1.5" to follow what Bean (13021) did on GJ1214b. For the 4 other orbits, I obtain a direct image in one filter then proceed with the scans, always at X=0.0",Y=-1.5" and finish with another direct image. I cycle through the available narrow-band filters (F126,F128,F130,F132,F164,F167). The start phase is very important. Needs to happen between 0.9840 and 0.9865 (***preference for 0.9845***). Phase=0.0 is corresponds to the middle of the secondary eclipse. Remember the period is large (12.7 days) so the apparent narrow range translates into a range of 45 minutes. The period is very precise (from Montet et al . 2014). The HJD given here is that of the secondary eclipse best fitted by Montet from Spitzer observations. It is equivalent to 0.186 days (4.46h) past the 0.5 phase between transits. The HJD was corrected from JD to heliocentric JD so it went from 2456947.112 to 2456947.114, a 183 seconds correction, well within the uncertainty. I constrained the visit orient such that the two stars in the system are within 30 degrees from being parallel to the detector X axis. 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