Science Keywords: Select from 2 to 5 items. This request is not easily categorizable by the supported keywords. It is a mission support proposal to observe stars to enable solar system science. -2019836758 Assigned ID: 28 ----- Attempting Submission 1 (Sun Mar 26 21:37:48 GMT 2017) ----- HST Phase I Proposal 28 (kemocc.apt) successfully submitted. Receipt: # 28-1 see submission comments, there (still) are not enough solar system science keywords to provide the required 2 keywords. Use of BLADE special requirement was added at the suggestion of CS Linda Driscoll. Filter for visit 3 changed due to recommendation from CS Linda Driscoll. 428972705 ----- Attempting Submission 1 (Sat Apr 08 02:16:43 GMT 2017) ----- ----- Attempting Submission 2 (Tue Apr 11 14:10:27 GMT 2017) ----- Astrometry of occultation stars for 2014MU69, New Horizons extended mission target We propose observations of three stars predicted to be occulted by Classical TNO (486958) 2014MU69 in 2017. These imaging observations will be used to improve the determination of the stellar proper motions. Without these observations, the uncertainty in the ground-track prediction is dominated by the uncertainty on the proper motions. With these observations, the prediction will be limited by the uncertainty in the orbit determination for 2014MU69 and good enough to enable observational campaigns. This represents a reduction in the prediction uncertainty by roughly a factor of 4. This improvement makes a ground-based observing campaign and a SOFIA observation possible. These observations contribute to the pre-encounter investigation of the New Horizons extended mission target whose flyby will take place on 2019 Jan 1. Plan A: This visit sequence is for the June 3 and July 10 stars, both at about R=15. The strategy combines short-exposure sub-frame images with full-field longer exposure images. The short exposures are set to expose on the target stars without saturation. Using sub-frames allows getting more images in an orbit. The full-frame images will saturate the target star but will provide much higher SNR data on fainter field stars and allow us to calibrate all stars in the sub-frame to get them onto the Gaia astrometric reference frame. There are eight short exposures, 5 seconds each, with the F350LP filter using a 1K sub-array and a 4-point box dither pattern (repeated twice). There are four long exposures, 90 seconds each, with the F350LP filter, a 4-point box dither and full frame (UVIS1+UVIS2) FOV. The pointing will be set up so that the target star does not move in absolute pixel coordinates between long and short exposures. The long exposure time is not critical and can be adjusted downward to ensure the pattern fits in a single visibility window when scheduled. The signal-to-noise ratio on the short exposures is high enough that we will be dominated by GAIA DR1 catalog errors. The choice of filter in this case is somewhat arbitrary but in using the same filter as for our 2014 MU69 astrometry we will be able to use these new images to improve our PSF modeling on those data. Plan B: This visit sequence is for the July 17 star, at R=12.5. Due to the source brightness, we will use the F475W (g') filter. The basic observing pattern is same as for Plan A but the short exposure time is 1.5 seconds and the long exposure time is 27 seconds. Solar System 0 AVAILABLE STAR BULGE g' = 15.15, G5 apparent J2000 J2000 STAR BULGE g' = 15.43, G0 apparent J2000 J2000 STAR BULGE g' = 12.60, K3 apparent J2000 J2000 WFC3/UVIS Imaging No No F350LP WFC3/UVIS Imaging No No F350LP WFC3/UVIS Imaging No No F475W POS-TARG DITHER 0.173 LINE 0.112 false false 81.785 4 23.884 WFC3-UVIS-DITHER-BOX 2 false The scheduling data was generated by CASM 25.0. CASM was run in Phase II mode. Observations consist of a set of exposures that just avoid saturation on the target star using a 1k sub-array and then a longer exposure set to get nearby fainter field stars and thus the target will be satuarted on these. All observations should be done within a single visiblility window. Observations need to be scheduled as soon as possible without being a distruptive TOO. The event is on 2017-06-03 so these observations need to schedule in early May to give sufficient time to provide preediction updates needed for deployment of ground-based assets for the occultation. (Tic-Visit :proposal-id 14926 :visit-id "01" :proposal-version -1 :trans-version "20170109" :date "07-Apr-2017 19:03:26.0" :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 1297584 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 14926 :visit-id "01" :obset-id "01" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 14926 :visit-id "01" :orbit-number 1 :pcs-time 333 :si-vis-utilization 2785 :al-overhead-at-end 123 :internal-dur-at-end 352 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3222 :pcs-gap 0 ) true 1 0 The intention of this visit is to get more of the fainter field stars around the target star but across a wider field. Ignoring the edither pattern, the target star should be in the same location on the detector as the short exposure set. The scheduling data was generated by CASM 25.0. CASM was run in Phase II mode. Observations consist of a set of exposures that just avoid saturation on the target star using a 1k sub-array and then a longer exposure set to get nearby fainter field stars and thus the target will be satuarted on these. All observations should be done within a single visiblility window. Observations need to be scheduled as soon as possible without being a distruptive TOO. These observations should be done no later than mid-June but earlier is better. (Tic-Visit :proposal-id 14926 :visit-id "02" :proposal-version -1 :trans-version "20170109" :date "07-Apr-2017 19:03:27.0" :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 1297584 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 14926 :visit-id "02" :obset-id "02" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 14926 :visit-id "02" :orbit-number 1 :pcs-time 333 :si-vis-utilization 2785 :al-overhead-at-end 123 :internal-dur-at-end 352 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3222 :pcs-gap 0 ) true 1 0 The intention of this visit is to get more of the fainter field stars around the target star but across a wider field. Ignoring the edither pattern, the target star should be in the same location on the detector as the short exposure set. /tmp/OPVisit3223437515456083927.xml The scheduling data was generated by CASM 25.0. CASM was run in Phase II mode. Observations consist of a set of exposures that just avoid saturation on the target star using a 1k sub-array and then a longer exposure set to get nearby fainter field stars and thus the target will be satuarted on these. All observations should be done within a single visiblility window. Observations need to be scheduled as soon as possible without being a distruptive TOO. These observations should be done no later than mid-June but earlier is better. (Tic-Visit :proposal-id 14926 :visit-id "03" :proposal-version -1 :trans-version "20170109" :date "11-Apr-2017 11:08:21.0" :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 1297584 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 14926 :visit-id "03" :obset-id "03" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 14926 :visit-id "03" :orbit-number 1 :pcs-time 333 :si-vis-utilization 2791 :al-overhead-at-end 125 :internal-dur-at-end 352 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3222 :pcs-gap 0 ) true 1 0 The intention of this visit is to get more of the fainter field stars around the target star but across a wider field. Ignoring the edither pattern, the target star should be in the same location on the detector as the short exposure set.