FLASH level may be too high for this exposure or a long subexposure. See extended explanation in the diagnostic browser FLASH level may be too high for this exposure or a long subexposure. See extended explanation in the diagnostic browser FLASH level may be too high for this exposure or a long subexposure. See extended explanation in the diagnostic browser FLASH level may be too high for this exposure or a long subexposure. See extended explanation in the diagnostic browser FLASH level may be too high for this exposure or a long subexposure. See extended explanation in the diagnostic browser FLASH level may be too high for this exposure or a long subexposure. See extended explanation in the diagnostic browser FLASH level may be too high for this exposure or a long subexposure. See extended explanation in the diagnostic browser FLASH level may be too high for this exposure or a long subexposure. See extended explanation in the diagnostic browser FLASH level may be too high for this exposure or a long subexposure. See extended explanation in the diagnostic browser FLASH level may be too high for this exposure or a long subexposure. See extended explanation in the diagnostic browser 0 ----- Attempting Submission 2 (Tue Jul 03 08:53:37 GMT 2018) ----- it is all ok Located at 2.0 pc, the L8+T1 dwarfs system Luhman16AB is the third closest system known to Earth, making it a key benchmark for detailed investigation of brown dwarf atmospheric properties, thermal evolution, multiplicity and planet-hosting frequency. Indeed, a recent ground-based astrometric campaign suggested this system to host a 5-30 Jupiter masses exoplanet. We propose to use HST in spatial-scanning mode to obtain the most accurate annual parallax of any brown dwarf to date, achieving an unprecedented accuracy of 1 part in 10000 (50 micro-arcsecond) for each of the two components of Luh16, and to constrain their absolute space motions with similar accuracy. Most importantly, we will be able to confirm the giant planet candidate and to search for faint companions co-moving with the targets, either resolved or through astrometric perturbations of the A-B orbital motion, the latter probing down to few Earth-masses. Present-day ground-based direct imaging and AO facilities have fundamental limitations (field of view, PSF stability, differential chromatic effects, visibility) which introduce systematic and seasonal errors that are hard to quantify, and which have already resulted many times in clamorous false alarm in the recent past. This is particularly true for faint and red objects. Luhman 16A and B will be problematic for GAIA (faint, color, crowding, visibility), and the here proposed HST spatial-scanning mode observations will actually be an important complementary validation of the final GAIA catalog itself (expected 2020). Similarly, JWST is not expected to provide any better astrometry than HST because of its broader and irregular PSFs. Each visit is scheduled in a 4-10 days window, centered at a well defined epoch. These epochs are choose as to better constraints the maxima elongation along the major and minor axis of the annual parallax of Luh16AB, its proper motions, the cusp and curve of the resulting cycloid combined motions, and to sample presence of possible extrasolar planets with periods between ~15 days and ~6months. Three epochs are taken at the maxima elongation along the annual parallax semi-major axis. Five epochs at the maxima elongations along the semi-minor axis of the annual parallax. Three epochs are taken at the cycloid (pms+annaual annual parallax) curles of the Luh16AB proper motions (visits labeled "ricciolo"), and two epochs at the bottom of the cycloid motion (visits labeled "pancia"). For total of 3+5+3+2 = 13 epochs. Eleven of these epochs should be taken within Cycle 22, and the last two within Cycle 23. The first epoch should be taken as early as possible (this should be in this August 29th, 2014). Each epoch contains three images in point source imaging mode, and four in spatial-scanning mode with WFC3/UVIS. In addition to the images taken in spatial scan mode and to the short two point-source images at the beginning and at the end of the single orbit-visits --- as requested at the phase I stage --- it turned out possible to fit in the orbit one extra point source images of 348s in F606W. The color information will be a precious to discriminate the nature (and so the distance) of the reference sources in the field (for example to separate slow close by red dwarf from far away giants). EXTRA-SOLAR PLANETS 6 false false false false false false false SUPPORTED STAR BROWN DWARF We have mapped the relative path of Luhman 16AB between 2014 and 2016 J2000 J2000 Sloan-i = 15 +/- .5 STAR BROWN DWARF We have mapped the relative path of Luhman 16AB between 2014 and 2016 J2000 J2000 Sloan-i = 15 +/- .5 WFC3/UVIS Imaging No No F814W 1435336579556 The scheduling data was generated by CASM 23.2. CASM was run in Phase II mode. Epoch 2016-10-05. This is the epoch is taken at the minimum NE-elongation in the minor axis of the annual parallax (AP). The epococh must be around 2016-10-05 +/- 25 days Then we want to scan perpendicularly to the minor axis. ORIENTATION = ~ 90d or ~270d +/- 35d main SCAN along Y, where CTE are worse, so SCAN ORIENT. secondary SCAN along X. A suitalbe window seems to be between 28 September 2015 and 15 Oct 2016. The closer to the Oct 5th 2016, the better. 1475546500000 220.0 (Tic-Visit :proposal-id 14330 :visit-id "06" :proposal-version -1 :trans-version "20150609" :date "26-Jun-2015 18:36:19.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 1 :saa-model "29" :si-bright-earth-limb-angle 20.0 :data-volume 2021248 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 14330 :visit-id "06" :obset-id "06" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 14330 :visit-id "06" :orbit-number 1 :pcs-time 333 :si-vis-utilization 2819 :al-overhead-at-end 125 :internal-dur-at-end 668 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3403 :pcs-gap 0 ) false 1 0 1530607902015 The scheduling data was generated by CASM 26.0. CASM was run in Phase II mode. /tmp/OPVisit2485374570134281659.xml Epoch 2016-08-29. This is the epoch is taken at the ricciolo of the cycloid apparent motion. The epoch must be around 2016-08-29 +/- 15 days main SCAN along Y, where CTE are worse, so SCAN ORIENT. secondary SCAN along X. (Tic-Visit :proposal-id 14330 :visit-id "11" :proposal-version -1 :trans-version "20180409" :date "03-Jul-2018 10:51:41.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 1 :saa-model "29" :si-bright-earth-limb-angle 20.0 :data-volume 2021248 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 14330 :visit-id "11" :obset-id "11" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 14330 :visit-id "11" :orbit-number 1 :pcs-time 333 :si-vis-utilization 2951 :al-overhead-at-end 125 :internal-dur-at-end 668 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3393 :pcs-gap 0 ) true 1 0