0 Assigned ID: 503 ----- Attempting Submission 1 (Fri Apr 08 14:47:21 GMT 2016) ----- HST Phase I Proposal 503 (Oph_followup_cycle24.apt) successfully submitted. Receipt: # 503-1 ----- Attempting Submission 2 (Fri Apr 08 16:32:25 GMT 2016) ----- HST Phase I Proposal 503 (Oph_followup_cycle24.apt) successfully submitted. Receipt: # 503-2 ----- Attempting Submission 3 (Fri Apr 08 17:00:37 GMT 2016) ----- HST Phase I Proposal 503 (Oph_followup_cycle24.apt) successfully submitted. Receipt: # 503-3 ----- Attempting Submission 4 (Fri Apr 08 20:52:55 GMT 2016) ----- 0 ----- Attempting Submission 1 (Thu Jul 21 16:21:42 GMT 2016) ----- ----- Attempting Submission 2 (Tue Sep 13 12:31:41 GMT 2016) ----- 0 We propose for follow-up observations to confirm common proper motion for two candidate planetary mass companions, identified as part of our GO 12944 (PI Allers) search for companions to the youngest (~0.5 Myr) brown dwarfs in the nearby Ophiuchus star-forming region. If confirmed to be co-moving, these would be among the lowest mass planetary mass companions imaged to date, with estimated masses <5 Jupiter Masses and would be vital benchmark objects for evolutionary models at these young ages. With our multi-band optical and IR photometric approach based on the SpT-Q relation seen for Ophiuchus brown dwarfs (Allers in prep.), we have already estimated the spectral type of our candidate companions. This approach distinguishes substellar objects from background interlopers based on the strength of the 1.4 um water feature robustly observed in MLTY objects but not in reddened background stars -- both our candidates show clear evidence of absorption at 1.4 um. If confirmed, these candidate companions would significantly increase the census of young planetary mass companions around extremely young brown dwarfs. These candidate companions are too faint to be observed with ground-based laser guide star adaptive optics (LGS AO) nor is the 1.4 um water feature observable from the ground for such faint objects due to telluric absorption, thus HST is the only telescope in the world suitable for these observations. In Cycle 20, we found two low mass candidate companions orbiting a brown dwarf and extremely low mass star respectively in the nearby Ophiuchus star-forming region. Both candidates show evidence of water absorption at 1.4 um, as expected for substellar or planetary mass objects (and would not be seen if they were background stellar contaminants). However, to confirm these objects as true low mass companions, we must measure common proper motion with their primary, requiring a second epoch of observations. 1) The primary goal of the program is to confirm or refute common proper motion for the two candidate companions. If background objects, with ~4 years between observations, we expect ~100 mas of motion relative to their primaries since the first epoch. Thus, followup UVIS F850LP observations with a 40 mas platescale will be critical. 2) the secondary goal is to get a measurement of the depth of water absorption for the candidate around Oph57, which dropped out entirely in this filter in the first epoch observation, but was clearly detected in F127M. Thus, to guarantee that we go deep enough for Oph57, we split the observing time solely between F139M and F850LP. Since the water absorption feature was already well measured in the first epoch GY92-3 observation, we will observe only in F850LP for this target. The first epoch UVIS observations suffered a bit (in terms of cosmic ray removal issues) from only having 2 dither positions per filter (due to avoiding WFC3 full frame serial buffer dumps), so we have primarily used subapertures with either 3 point dithers or box dithers throughout here. Our science is better served by very high quality imaging of the inner 30" than lower quality, less dithered observations of the full chip. The other thing is that the first epoch UVIS images suffered strongly from charge transfer efficiency issues. We've tried to mitigate this in a variety of ways in this observations: 1) For GY92-3, we've chosen the UVIS2_C2K2C_SUB subaperture to place the target as close as possible to the amplifier on the chip. Since we only care about the inner 30", this should be a sufficient field of view. While the UVIS2_C512C_CTE full chip aperture is available too, GY92-3 is bright enough to saturate in less than 349 s, preventing full-frame observations. For the fainter target Oph57 we use the UVIS2_C512C_CTE aperture and the IRSUB512. 2) We've tried to make the exposures reasonably long to increase the background and have also added a postflash of 10 e- for both targets. We've also set ORIENT ranges to avoid the candidate companions accidentally falling into the diffraction spikes. Extrasolar Planets and Planet Formation Stellar Physics 12 false false false false false false SUPPORTED STAR BROWN DWARF EXTRA-SOLAR PLANET This object was generated by the targetselector and retrieved from the SIMBAD database. J2000 J2000 SpT=M7.25, J=15.06, H=13.92, K=13.18 STAR BROWN DWARF EXTRA-SOLAR PLANET This object was generated by the targetselector and retrieved from the SIMBAD database. J2000 J2000 SpT=M6.5, I=15.62, J=12.3, H=11.5, K=10.9 WFC3/IR Imaging No No F127M WFC3/IR Imaging No No F139M WFC3/IR Imaging No No F127M WFC3/IR Imaging No No F139M WFC3/UVIS Imaging No No F850LP POS-TARG DITHER 0.173 LINE 0.112 false false 81.785 4 23.884 WFC3-UVIS-DITHER-BOX 2 false POS-TARG DITHER 0.572 LINE 0.365 false false 74.653 4 18.528 WFC3-IR-DITHER-BOX-MIN 3 false POS-TARG DITHER 0.135 LINE false false 3 46.84 WFC3-UVIS-DITHER-LINE-3PT 4 false 1473769463659 The scheduling data was generated by CASM 24.2. CASM was run in Phase II mode. (Tic-Visit :proposal-id 14686 :visit-id "01" :proposal-version -1 :trans-version "20160601" :date "13-Sep-2016 13:24:22.0" :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 1120720 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 14686 :visit-id "01" :obset-id "01" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 14686 :visit-id "01" :orbit-number 1 :pcs-time 333 :si-vis-utilization 2889 :al-overhead-at-end 122 :internal-dur-at-end 668 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3222 :pcs-gap 0 ) false 1 0 1473769471670 The scheduling data was generated by CASM 24.2. CASM was run in Phase II mode. (Tic-Visit :proposal-id 14686 :visit-id "02" :proposal-version -1 :trans-version "20160601" :date "13-Sep-2016 13:24:30.0" :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 492704 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 14686 :visit-id "02" :obset-id "02" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 14686 :visit-id "02" :orbit-number 1 :pcs-time 333 :si-vis-utilization 2884 :al-overhead-at-end 171 :internal-dur-at-end 575 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3222 :pcs-gap 0 ) true 1 0