0 Assigned ID: 439 ----- Attempting Submission 1 (Fri Apr 10 12:10:01 GMT 2015) ----- HST Phase I Proposal 439 (HST_exovar_cycle23.apt) successfully submitted. Receipt: # 439-1 ----- Attempting Submission 2 (Fri Apr 10 15:22:18 GMT 2015) ----- HST Phase I Proposal 439 (HST_exovar_cycle23.apt) successfully submitted. Receipt: # 439-2 ----- Attempting Submission 3 (Fri Apr 10 17:22:48 GMT 2015) ----- 5-orbit variability monitoring observation for PSO 318, to be scheduled simultaneously with Spitzer variability monitoring. Updated to use the full WFC3 IR FOV. 1529795309 ----- Attempting Submission 1 (Fri Jul 17 12:50:12 GMT 2015) ----- ----- Attempting Submission 2 (Fri Jul 29 18:45:55 GMT 2016) ----- Variability attributed to cloud structure is a persistent feature for L and T type field brown dwarfs. Directly imaged planets occupy the same temperature regime as L and T type brown dwarfs and are likely to be equally variable. As part of our ongoing NTT SOFI survey for variability in young free-floating planets and low mass brown dwarfs, we detect significant variability in a young, free-floating planetary mass object, likely due to rotational modulation of inhomogeneous cloud cover. This is the first such detection in a bonafide planetary mass object -- here we propose for HST and Spitzer followup to pinpoint the source of the observed variability and determine the rotational period of the object. Due to its low surface gravity, while this object has a late L spectral type, it has an ``early/mid T'' Teff<1200 K. We will directly test the effect of low surface gravity on observed variability. If variability matches that found in objects with similar spectral type but higher surface gravity -- i.e. high-level hazes observed in mid L dwarfs by Yang et al. 2015 -- we expect similar variability amplitudes in all bands. If variability is due to inhomogeneous clouds as found in higher gravity T dwarfs with similar Teff (Buenzli et al. 2015, Apai et al. 2013), we expect variability to be strongest in broadband J and H and have lower amplitudes within the 1.4 um water absorption feature (only observable from space). As ground-based searches for brown dwarf variability only have sensitivities to >2-3% variability, we require the proven photometric stability of HST and Spitzer (sensitivity down to <0.5% variability) to be sensitive to small differences between bands. We are observing a free-floating young planet with WFC3 IR slitless spectroscopy with grism G141 to confirm and characterize time variability found from the ground. With an expected period of 5-20 hours, this target should be observed for 5 consecutive orbits to maximize coverage of as much of a rotational period as possible. At the beginning of each orbit, a direct image is taken for wavelength calibration. This target will be observed simulateously with Spitzer and thus scheduling must be coordinated. Orient ranges have been set to avoid background stars at PA~45 degrees. PRM, July 29, 2016: I tried a full-frame version of the program instead of the 256x256 subarray. Because SPARS25 can be parallel dumped, we get good packing. Do to idiosyncracies of APT and pointing maneuvers for certain apertures, I used GRISM1024 for each of the exposures (both direct imaging and grism). I didn't bother to fill in partial (smaller NSAMP) version of the same exposures to fill the orbits, but the PI should do so in a version to be submitted. Note the total exposure time is longer for both the direct image and the spectra, and as intended, the field of view is much larger (16 times in area) which may be helpful for extracting comparison star photometry or using the 0th order or 2nd order spectra of the objects for photometry. EXTRA-SOLAR PLANETS 12 false false false false false 17.6 false SUPPORTED STAR BROWN DWARF EXTRA-SOLAR PLANET NO J2000 J2000 JHKs=16.7, 15.7, 14.7 WFC3/IR Spectroscopic No No G141 /Users/bbiller/Documents/proposals/HST_exovar/cycle23/OP-cache/HST_14188_fullframe_nsamp12-v01.xml 1469541445026 The scheduling data was generated by CASM 24.2. CASM was run in Phase II mode. This 5-orbit visit should be coordinated with simultaneous Spitzer observations (17.6 Spitzer hours awarded, so there is a fairly long range of overlap). 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