3/2/14: Based on the first orbit we have made minor modifications to the the dither pattern and orbit packing. 3/3/14: Updated exposures to enable schedulability. 560468515 Submission failed due to an error: java.lang.NullPointerException ----- Attempting Submission 2 (Mon Mar 03 00:50:41 GMT 2014) ----- ----- Attempting Submission 3 (Mon Mar 03 18:48:26 GMT 2014) ----- Confirmation and characterization of young planetary companions hidden in the HST NICMOS archive We propose to conduct WFC3 high contrast observations of six faint planetary candidates orbiting young (1 to 100 Myrs) stars identified in archival HST NICMOS coronagraphic data as part of our team's program AR-12652. Such rare objects are of the utmost importance to comparative exo-planetology as their physical properties reflect the initial conditions of still poorly constrained planetary formation mechanisms. Moreover directly imaged systems are precious artifacts in the expanding exo-planetary treasure trove as they are readily available for spectroscopic characterization. Our statistical analysis, which combines population synthesis models and empirical inspections of the entire NICMOS field of view for all sources observed in coronaraphic mode, almost guarantees that one of these six faint candidates is associated with its putative host star. We will conduct our observation in four near infrared filter, F125W, F160W to establish the baseline luminosity of our candidates and in F127M and F139M in order to probe the depth their water absorption features, characteristic of substellar /exo-planetary like atmospheres. Because of the youth of our targets, this program, which only requires a modest 12 HST orbits, will almost certainly identify and image a young or adolescent exo-planet. General observing strategy: Our goal is to identify with WFC3 six sub-stellar companions candidates detected via re-processing of the HST NICMOS archive. Our targets were selected based on their faint V magnitude, which makes them difficult to observe with the depth of contrast required to detect our candidates using ground based adaptive optics. Our observing rationale can be described as follows: - we will dedicate two orbits to each putative host star. This will allow us to observe each source with two distinct HST roll angles, a method that has been proven very useful in order to discriminate astrophysical point sources from telescope and/or instrumental speckles. - we will observe each candidate companion in four filters. We will use two wide band filters (F125W and F160W) which will provide a photometric baseline to put in perspective the properties of the sub-stellar companions detected by this program with the ensemble of sub-stellar companions already detected from the ground. We will use two narrow band filters (F127M and F139M, not accessible from the ground) in order to further characterize the bulk physical properties and the atmospheric chemistry of the companions we will detect. - we will reduce our data using the Karhunen-Loeve Image Processing (KLIP) algorithm described in Soummer, Pueyo and Larking 2012, that is at the algorithm underlying our NICMOS detections. This algorithm uses a library of reference PSF in order to build a set of eigen-mnodes representative of the statistical properties of the telescope+instrument quasi-static response. - the KLIP algorithm works optimally on Nyquist samples PSFs, which will not be the case for the raw WFC3 data. We will thus use dithers in order to obtain a set of PSFs realizations for which the stellar location varies within a WFC3 pixel. We will recombine there dither using an optimized Fourier based image recombination algorithm which will yield a Nyquist sampled dataset at half the WFC3 plate scale. - the KLIP algorithm only works on images that are not saturated and whose quasi-static PSF structures exhibit roughly the same level of photon noise statistics. Because of the absence of a coronagraph on WFC3 we will need to saturate the inner 0.5'' of the WFC3 PSF in order to obtain sufficient exposure depth to detect our six candidates (all located at least 1'' beyond their star). We predict that the F127M and F139M PSFs of this present program added to F127M and F139M PSFs from GO-12511 will be sufficient to detect and confirm/rule out common proper motion for all of our candidates. The characterization in the wide band filters will the require us to optimize the number of dithered images used to generate in each "super-sample" Nyquist PSF. Since our the observing sequence in the wide band filters will yield in average 8 wide band PSFs and since each Nyquist sampled image can be generated using four raw PSFs we will have ~22 reference PSFs to analyze each wide band images. We believe that given the stability of WFC3 this number of references is sufficient to characterize the sub stellar companions we will detect. Orbit packing: Requirements Each orbit will consist of a single roll. For each orbit we designed observing sequences under the following hard requirements: - HR1: the inner ~0.5'' (pm 0.1'') of each exposure is saturated. - HR2: the exposure time of each single dither is sufficient for a "raw detector" SNR of at least 5 for each of our candidates in each filter. - HR3: the total number of images in the program is large enough to yield at least 20 Nyquist "super sampled" PSFs after dither recombination for each source in each filter. Moreover in order to facilitate astrometric calibration for common proper motion we added the following soft requirement: -SR1 the first read of at least one exposure in one filter ought to yield an unsaturated stellar PSF. Note that in principle stellar location can be derived using the unsaturated diffraction spikes associated with secondary support structures, albeit at a precision level inferior to the case of having an unsaturated stellar PSF. This requirement is only important for the sources that exhibit less than 0.5'' proper motion since the NICMOS epoch. Orbit packing Based on the characteristics of our target stars and of the candidates detect with NICMOS these requirements flow down to three types of orbit packing - "bright sources", J ~ 7.5 mag: RE0723+20 and HD160934, For all filters three WFC3-IR-DITHER-BOX-Min dither patterns of 4 exposures each. A total of 12 exposures per source, per orbit, per filter. A total of 3 Nyquist sampled images per source, per orbit, per filter. - "medium sources", J ~ 8.5 mag: HD146516 and V1121 Oph, For all filters one 1 SPIRAL dither patterns of 9 exposures each. A total of 9 exposures per source, per orbit, per filter. A conservative total of 2 Nyquist sampled images per source, per orbit, per filter. - "faint sources", J ~ 9.8 mag: GJ3631 and RXJ18521730-3700119. For all filters one 2 SPIRAL dither patterns of 6 exposures each. A total of 6 exposures per source, per orbit, per filter. A conservative total of 1 Nyquist sampled images per source, per orbit, per filter. These observations meet almost all the requirements (see below). The orbits were finally packed with extra exposures (without the dither patterns) in order to reach deeper exposures. Verification of requirements - HR1 was verified using our custom PSF saturation modeling tool developed as part of GO-12511. Preliminary dat from GO-12511 shows that our modeling tool is well calibrated and we expect the saturation region in the final images to be adequate. - HR2: using the WFC3 ETC we checked that all candidates in all filter will exhibit a "raw SNR" (without speckles) of more than 5 in every single exposure except for the candidate around RE0723+20 in F139M. Given that this filter probes a water absorption band for which sub-stellar companions are faint and usually not detected from the ground we decided that t was acceptable to take the risk of only obtain an upper limit in this particular on this source instead of increasing the exposure time (e.g the saturation radius) which would in turn comprise the uniformity of our PSF library for this filter. - HR3: based on the numbers derive above the number of Nyquist sampled references will be for each type of sources: "bright sources": 21 reference PSFs "medium sources": 22 reference PSFs "faint sources": 23 reference PSFs -SR1: see below for the saturation of the first read in F127M. All wide band filters are saturated RE0723+20 Saturated pm ~1.6'' --> No need for precise astrometry HD160934 Saturated pm ~0.5''--> No need for precise astrometry HD146516 Saturated pm~0.1'' --> We added a short exposure in 128 sub-array for astrometric calibration V1121 Oph Saturated pm~0.2'' -> We added a short exposure in 128 sub-array for astrometric calibration GJ3631 Not saturated pm~10'' RXJ18521730-3700119 Not saturated pm~0.15'' We additionally packed the orbits with extra exposures (outside dither patterns) in the medium band filters in order to maximize efficency. Roll angles In order to simplify our data-reduction we are asking for a range of the telescope orients that prevents our candidates from being hidden behind the spiders. These were derived based on the PA of the candidates on the NICMOS detector, rotated back to the sky. We set exclusion zones of ~45 degrees at the first visit around each spiders so that the candidates lies are between the spiders. For each source we defined roll angles for the second visits with respect to the first visits which a) is sufficently large, b) ensures that the candidates are still between spiders, c) provides scheduelable observations. Time constraint We are asking for observations of our three candidates with the least proper motion as late as scheduelable in the cycle (e.g after June 14 after checking schedulability). EXTRA-SOLAR PLANETS Default false false false false false SUPPORTED STAR K V-IV This object was generated by the targetselector and retrieved from the SIMBAD database. V-V429-GEM J2000 J2000 J = 7.643 STAR K V-IV This object was generated by the targetselector and retrieved from the SIMBAD database. HD-160934 J2000 J = 7.618 STAR G V-IV This object was generated by the targetselector and retrieved from the SIMBAD database. HD-146516 J2000 J = 8.51 STAR K V-IV This object was generated by the targetselector and retrieved from the SIMBAD database. V-V1121-OPH J2000 J = 8.302 STAR M V-IV This object was generated by the targetselector and retrieved from the SIMBAD database. GJ-3631 J2000 J = 9.834 STAR K V-IV This object was generated by the targetselector and retrieved from the SIMBAD database. 2MASS-J18521730-3700119 J2000 J = 9.772 WFC3/IR Imaging No No F160W WFC3/IR Imaging No No F125W WFC3/IR Imaging No No F139M WFC3/IR Imaging No No F127M WFC3/IR Imaging No No F160W WFC3/IR Imaging No No F125W WFC3/IR Imaging No No F139M WFC3/IR Imaging No No F127M WFC3/IR Imaging No No F160W WFC3/IR Imaging No No F125W WFC3/IR Imaging No No F139M WFC3/IR Imaging No No F127M WFC3/IR Imaging No No F160W WFC3/IR Imaging No No F125W WFC3/IR Imaging No No F139M WFC3/IR Imaging No No F127M WFC3/IR Imaging No No F160W WFC3/IR Imaging No No F125W WFC3/IR Imaging No No F139M WFC3/IR Imaging No No F127M WFC3/IR Imaging No No F160W WFC3/IR Imaging No No F125W WFC3/IR Imaging No No F139M WFC3/IR Imaging No No F127M POS-TARG DITHER 0.065 LINE 0.065 false false 74.653 4 18.528 WFC3-IR-DITHER-BOX-MIN 3 false POS-TARG DITHER 0.065 LINE 0.065 false false 0 4 0 WFC3-IR-DITHER-BOX-MIN 4 false The scheduling data was generated by CASM 21.2. CASM was run in Phase II mode. The PA of the the candidate is ~21.5 degrees East of North. We define the orient ranges accordingly so that the candiate is not located on the PSF spiders. We used a 135 degrees rotation between the WFC3 frame and the telescope frame. 1392647710000 97.0 (Tic-Visit :proposal-id 13331 :visit-id "01" :proposal-version -1 :trans-version "20130502" :date "03-Mar-2014 11:40:26.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 1 :saa-model "30" :si-bright-earth-limb-angle 20.0 :data-volume 1573248 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 13331 :visit-id "01" :obset-id "01" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 13331 :visit-id "01" :orbit-number 1 :pcs-time 333 :si-vis-utilization 2900 :al-overhead-at-end 0 :internal-dur-at-end 708 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3244 :pcs-gap 0 ) true 1 0 The scheduling data was generated by CASM 21.2. CASM was run in Phase II mode. An orient of 180 degrees pm 10 with respect to visit 01 will ensure that the candidate still does not lie under ths spider. We checked that this orient can be schedueled. (Tic-Visit :proposal-id 13331 :visit-id "02" :proposal-version -1 :trans-version "20130502" :date "03-Mar-2014 11:40:32.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 1 :saa-model "30" :si-bright-earth-limb-angle 20.0 :data-volume 1573248 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 13331 :visit-id "02" :obset-id "02" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 13331 :visit-id "02" :orbit-number 1 :pcs-time 333 :si-vis-utilization 2900 :al-overhead-at-end 0 :internal-dur-at-end 708 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3244 :pcs-gap 0 ) true 1 0 The scheduling data was generated by CASM 21.2. CASM was run in Phase II mode. The PA of the the candidate is ~347 degrees East of North. We define the orient ranges accordingly so that the candiate is not located on the PSF spiders. We used a 135 degrees rotation between the WFC3 frame and the telescope frame. (Tic-Visit :proposal-id 13331 :visit-id "03" :proposal-version -1 :trans-version "20130502" :date "03-Mar-2014 11:40:39.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 1 :saa-model "30" :si-bright-earth-limb-angle 20.0 :data-volume 1723200 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 13331 :visit-id "03" :obset-id "03" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 13331 :visit-id "03" :orbit-number 1 :pcs-time 333 :si-vis-utilization 3151 :al-overhead-at-end 0 :internal-dur-at-end 708 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3511 :pcs-gap 0 ) true 1 0 The scheduling data was generated by CASM 21.2. CASM was run in Phase II mode. An orient of 90 degrees pm 10 with respect to visit 03 will ensure that the candidate still does not lie under ths spider. We checked that this orient can be schedueled. 1394020413000 264.0 (Tic-Visit :proposal-id 13331 :visit-id "04" :proposal-version -1 :trans-version "20130502" :date "03-Mar-2014 11:40:44.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 1 :saa-model "30" :si-bright-earth-limb-angle 20.0 :data-volume 1723200 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 13331 :visit-id "04" :obset-id "04" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 13331 :visit-id "04" :orbit-number 1 :pcs-time 333 :si-vis-utilization 3151 :al-overhead-at-end 0 :internal-dur-at-end 708 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3511 :pcs-gap 0 ) true 1 0 Timing link suitability includes constraints ([06 After 05]) The scheduling data was generated by CASM 21.2. CASM was run in Phase II mode. The PA of the the candidate is ~228.4 degrees East of North. We define the orient ranges accordingly so that the candiate is not located on the PSF spiders. We used a 135 degrees rotation between the WFC3 frame and the telescope frame. The timing requirements are placed on a few targets to ensure sufficient separation from our first epoch to enable proper motion studies. (Tic-Visit :proposal-id 13331 :visit-id "05" :proposal-version -1 :trans-version "20130502" :date "03-Mar-2014 11:40:48.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 1 :saa-model "30" :si-bright-earth-limb-angle 20.0 :data-volume 1578432 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 13331 :visit-id "05" :obset-id "05" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 13331 :visit-id "05" :orbit-number 1 :pcs-time 333 :si-vis-utilization 2885 :al-overhead-at-end 0 :internal-dur-at-end 642 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3244 :pcs-gap 0 ) true 1 0 Timing link suitability includes constraints ([06 After 05]) The scheduling data was generated by CASM 21.2. CASM was run in Phase II mode. An orient of 180 degrees pm 10 with respect to visit 05 will ensure that the candidate still does not lie under ths spider. We checked that this orient can be schedueled. (Tic-Visit :proposal-id 13331 :visit-id "06" :proposal-version -1 :trans-version "20130502" :date "03-Mar-2014 11:40:52.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 1 :saa-model "30" :si-bright-earth-limb-angle 20.0 :data-volume 1578432 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 13331 :visit-id "06" :obset-id "06" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 13331 :visit-id "06" :orbit-number 1 :pcs-time 333 :si-vis-utilization 2885 :al-overhead-at-end 0 :internal-dur-at-end 642 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3244 :pcs-gap 0 ) true 1 0 Timing link suitability includes constraints ([08 After 07]) The scheduling data was generated by CASM 21.2. CASM was run in Phase II mode. The PA of the the candidate is ~212.4 degrees East of North. We define the orient ranges accordingly so that the candiate is not located on the PSF spiders. We used a 135 degrees rotation between the WFC3 frame and the telescope frame. The timing requirements are placed on a few targets to ensure sufficient separation from our first epoch to enable proper motion studies. (Tic-Visit :proposal-id 13331 :visit-id "07" :proposal-version -1 :trans-version "20130502" :date "03-Mar-2014 11:41:54.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 1 :saa-model "30" :si-bright-earth-limb-angle 20.0 :data-volume 1577312 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 13331 :visit-id "07" :obset-id "07" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 13331 :visit-id "07" :orbit-number 1 :pcs-time 333 :si-vis-utilization 2836 :al-overhead-at-end 0 :internal-dur-at-end 642 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3239 :pcs-gap 0 ) false 1 0 Timing link suitability includes constraints ([08 After 07]) The scheduling data was generated by CASM 21.2. CASM was run in Phase II mode. An orient of 180 degrees pm 10 with respect to visit 07 will ensure that the candidate still does not lie under ths spider. We checked that this orient can be schedueled. (Tic-Visit :proposal-id 13331 :visit-id "08" :proposal-version -1 :trans-version "20130502" :date "03-Mar-2014 11:42:13.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 1 :saa-model "30" :si-bright-earth-limb-angle 20.0 :data-volume 1577312 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 13331 :visit-id "08" :obset-id "08" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 13331 :visit-id "08" :orbit-number 1 :pcs-time 333 :si-vis-utilization 2836 :al-overhead-at-end 0 :internal-dur-at-end 642 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3239 :pcs-gap 0 ) false 1 0 The scheduling data was generated by CASM 21.2. CASM was run in Phase II mode. The PA of the the candidate is ~126.3 degrees East of North. We define the orient ranges accordingly so thatthe candiate is not located on the PSF spiders. We used a 135 degrees rotation between the WFC3 frame and the telescope frame. We've limited the Orientation requirements based on secheduling constraints (75-95), which appears to be the only overlapping region of orient range AND target visibility. 1395496512000 85.0 (Tic-Visit :proposal-id 13331 :visit-id "09" :proposal-version -1 :trans-version "20130502" :date "03-Mar-2014 11:43:32.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 1 :saa-model "30" :si-bright-earth-limb-angle 20.0 :data-volume 1292320 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 13331 :visit-id "09" :obset-id "09" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 13331 :visit-id "09" :orbit-number 1 :pcs-time 333 :si-vis-utilization 2827 :al-overhead-at-end 0 :internal-dur-at-end 677 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3233 :pcs-gap 0 ) true 1 0 The scheduling data was generated by CASM 21.2. CASM was run in Phase II mode. An orient of 30 degrees pm 5 with respect to visit 09 will ensure that the candidate still does not lie under ths spider. We checked that this orient can be schedueled. We've limited the Orientation requirements of the previous orbit based on secheduling constraints, which appears to be the only overlapping region of orient range AND target visibility. Please maximize the orient angle separation from the previous orbit (visit09) which enables smaller inner working angles. 1396773258000 112.0 (Tic-Visit :proposal-id 13331 :visit-id "10" :proposal-version -1 :trans-version "20130502" :date "03-Mar-2014 11:43:42.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 1 :saa-model "30" :si-bright-earth-limb-angle 20.0 :data-volume 1292320 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 13331 :visit-id "10" :obset-id "10" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 13331 :visit-id "10" :orbit-number 1 :pcs-time 333 :si-vis-utilization 2827 :al-overhead-at-end 0 :internal-dur-at-end 677 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3233 :pcs-gap 0 ) true 1 0 Timing link suitability includes constraints ([12 After 11]) The scheduling data was generated by CASM 21.2. CASM was run in Phase II mode. The PA of the the candidate is ~303.8 degrees East of North. We define the orient ranges accordingly so that the candiate is not located on the PSF spiders. We used a 135 degrees rotation between the WFC3 frame and the telescope frame. The timing requirements are placed on a few targets to ensure sufficient separation from our first epoch to enable proper motion studies. (Tic-Visit :proposal-id 13331 :visit-id "11" :proposal-version -1 :trans-version "20130502" :date "03-Mar-2014 11:41:14.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 1 :saa-model "30" :si-bright-earth-limb-angle 20.0 :data-volume 1301920 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 13331 :visit-id "11" :obset-id "11" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 13331 :visit-id "11" :orbit-number 1 :pcs-time 333 :si-vis-utilization 2891 :al-overhead-at-end 0 :internal-dur-at-end 677 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3287 :pcs-gap 0 ) true 1 0 Timing link suitability includes constraints ([12 After 11]) The scheduling data was generated by CASM 21.2. CASM was run in Phase II mode. An orient of 90 degrees pm 10 with respect to visit 11 will ensure that the candidate still does not lie under ths spider. We checked that this orient can be schedueled. (Tic-Visit :proposal-id 13331 :visit-id "12" :proposal-version -1 :trans-version "20130502" :date "03-Mar-2014 11:41:19.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 1 :saa-model "30" :si-bright-earth-limb-angle 20.0 :data-volume 1301920 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 13331 :visit-id "12" :obset-id "12" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 13331 :visit-id "12" :orbit-number 1 :pcs-time 333 :si-vis-utilization 2891 :al-overhead-at-end 0 :internal-dur-at-end 677 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3287 :pcs-gap 0 ) true 1 0