0Assigned ID: 943
----- Attempting Submission 1 (Fri Apr 05 23:23:21 GMT 2019) -----The observations were changed to use subarrays so that it is possible to obtain unsaturated data on the star in the field-of-view and only mildly saturated data from which the companion spectrum can be extracted from Visits 9-20.3995353----- Attempting Submission 1 (Thu Jul 25 01:24:46 GMT 2019) -----
----- Attempting Submission 2 (Fri Sep 27 18:44:13 GMT 2019) -----
----- Attempting Submission 3 (Sun Sep 29 01:41:37 GMT 2019) -----
HST Phase II Proposal 15819 (28SepAPT.apt) successfully submitted.
Receipt: # 15819-3
----- Attempting Submission 4 (Mon Oct 07 01:49:42 GMT 2019) -----
----- Attempting Submission 5 (Tue Oct 08 02:26:58 GMT 2019) -----
HST Phase II Proposal 15819 (7OctEdits2.apt) successfully submitted.
Receipt: # 15819-5
----- Attempting Submission 6 (Tue Oct 08 02:42:31 GMT 2019) -----
----- Attempting Submission 7 (Mon Oct 14 01:29:04 GMT 2019) -----
HST Phase II Proposal 15819 (13OctAPTfile.apt) successfully submitted.
Receipt: # 15819-7
----- Attempting Submission 8 (Mon Oct 14 02:08:36 GMT 2019) -----
HST Phase II Proposal 15819 (13OctAPTfile.apt) successfully submitted.
Receipt: # 15819-8
----- Attempting Submission 9 (Mon Oct 14 02:14:29 GMT 2019) -----
HST Phase II Proposal 15819 (13OctAPTfile.apt) successfully submitted.
Receipt: # 15819-9
----- Attempting Submission 10 (Mon Dec 16 03:15:45 GMT 2019) -----Determining Benchmark Precision Abundances for Ultracool CompanionsWith sensitive HST spectroscopy coupled with advanced atmospheric retrieval techniques, we propose to measure the 0.8-1.7um spectra of four planetary temperature T/Y companions and to determine abundances, metallicities, C/O ratios, effective temperatures, surface gravities, and temperature-pressure profiles. Models of star and planet formation suggest that the compositions of the atmospheres of companions relative to their primaries represent an important pathway to understanding the formation mechanism. This program will establish the first high precision atmospheric composition measurements for a set of three benchmark substellar systems with mass ratios comparable to binary systems and test the hypothesis that the C/O ratios are the same for each component, distinct from the prediction for star-planet pairs. The results will provide an important comparison to imaged or transiting exoplanet companions, and we will compare the the benchmark systems to the fourth target, GJ 504 b, the coolest directly imaged companion that may be planetary. The target mass ratios extend from high values comparable to binary stars down to low ratios analogous to exoplanet systems. Covering this broad continuum of mass ratios is essential to test the models in different regimes. Only space-based observations will provide the high sensitivity required to perform the retrieval analysis and robustly determine the atmospheric properties. Another core project goal is developing a comprehensive, high sensitivity spectral library of the coolest companions with legacy value for advancing theoretical atmosphere/evolution models and complementing future JWST observations.Using the WFC3 G102 and G141grisms, we will obtain R~100-200 spectra over the 0.8-1.7um wavelength range. The combination of projected separation (<1 arcsec vs. >1 arcsec) and delta magnitudes, (<3 vs. >10) determines which of observational approaches is used for each target.
A+B on array: For the two T-T pair targets in the list, the close-in and similar brightness sources WISE1217+16 and WISE1711+3500, we will obtain spectra of both the primary and the secondary on the WFC3 detector, choosing the orientation of the spacecraft in order for the direction of the dispersion to be at an angle near to the orthogonal direction of the binary at the epoch of observation. We will carry out a series of short ~500-1000s exposures such as were utilized in the HST survey of isolated T/Y dwarfs (Schneider+ 2015). The WFC3 ETC confirms that the primaries will not be saturated. We will minimize the flux contamination between the two components by taking advantage or the spatial symmetry of the telescope diffractive response and use the companion-free half of the dispersed image as a reference to minimize blending between the spectra of the two components. This technique is now routine for similar ground based observations (LSS mode of SPHERE, see Hinkley+ 2015, Mesa+ 2016 and reference therein) that are much less stable than with HST (i.e. the technique should be more effective with HST data). These targets will require two orbits per grism setting to build up high quality spectra on the companions to use as input for the atmospheric retrieval code.
Primary off array: For the companions to stars with separations of several arcseconds, a different observational approach is required. Specifically, we will place the primary off the detector and disperse in the direction orthogonal to the line joining primary and secondary. Based on our Exposure Time Calculations, two orbits per grism are necessary to obtain sufficient SNR on GJ504b and GJ 758 B. Because the diffractive halo due to the primary will still bright at the locations of the companions in this regime, we will carry a series of moderately short (~360s) exposures in order to avoid saturation of any remaining halo at the location of the secondaries. We also request an additional orbit per setting, using the same exposure parameters, to obtain a symmetric image of this halo, this time with both primary the companion off the detector. For the background subtraction, we will use the same algorithm as for the T+T/Y pairs, but with the background data from a second position.The members of our team have the required combination of expertise in both observational and theoretical work to complete the proposed program. For the observational and data analysis work, PI Patience and Co-I Pueyo are experts in the planning, execution, and analysis of high contrast imaging and spectral extraction of directly imaged companions. Patience and Pueyo have experience working on the discovery and/or analysis of the photometric and spectroscopic observations of many of the imaged planets shown in Figure 3 (e.g. HR 8799, 51 Eri, Beta Pic, 2M1207, HD 95086) and will work with the observational student and postdocs on the data aspects of the project and the broader scientific context of the program. Patience supervises PhD student Hom who would analyze parts of the data as a core thesis component, and Hom performed the data analysis of an archive spectrum in Figure 4. Postdoc Schneider has considerable experience with HST spectra of cool objects, including previous WFC3 grism programs that produced the spectrum shown in Figure 5. For the theoretical work, Co-PI Line is an expert in exoplanet atmospheric retrieval modeling on brown dwarfs and exoplanets, and will oversee/assist with the modeling implementation of the cool object spectra; an example of a model spectrum from this approach is shown in Figure 5 of the proposal, along with a summary of a range of model fits in Figure 4. Line supervises PhD students Zalesky and Iyer who will work on different aspects of the project. Zalesky will run the atmospheric retrievals on the final data products, in an analogous approach as used to fit spectra of isolated T/Y-dwarfs, as shown in Figure 2 of the proposal (a student-led paper with 4 members of our proposal team). The results of the project would lead to several student- and postdoc-led papers reporting on the systems in different mass ratio/separation regimes and also a final summary paper of the full population of T/Y-companions.Stellar PhysicsPlanets and Planet Formation6falsefalsefalsefalsefalsefalsefalseSUPPORTEDSTARBROWN DWARFLOW MASS COMPANIONTNOThis coordinates have been updated to GAIA DR2 measurements and are currently centered on the star. The proper motion includes the multiplication by cos(Dec) -- is this the HST convention?
V-magnitude is for stellar primary.
The offset needed is being investigated.J2000J2000J_B=19.8STARBROWN DWARFLOW MASS COMPANIONTNOThis coordinates have been updated to GAIA DR2 measurements and are currently centered on the star. The proper motion includes the multiplication by cos(Dec) -- is this the HST convention?
V-magnitude is for stellar primary.
The offset needed is being investigated.J2000J2000J=19.8STARBROWN DWARFLOW MASS COMPANIONTNOThe coordinates and proper motion are from the reference Kirkpatrick+ 2019J2000J2000J_A=17.886STARBROWN DWARFLOW MASS COMPANIONTNOThe coordinates, proper motion and parallax are from Kirkpatrick+ 2019J2000J2000J_A=17.83, H_A=18.18WFC3/IRSpectroscopicNoNoG102WFC3/IRSpectroscopicNoNoG102WFC3/IRSpectroscopicNoNoG102WFC3/IRSpectroscopicNoNoG102WFC3/IRSpectroscopicNoNoG141WFC3/IRSpectroscopicNoNoG141WFC3/IRSpectroscopicNoNoG141WFC3/IRSpectroscopicNoNoG141POS-TARGDITHER5Pattern is designed to make a 5arcsecond dither in -Y direction on array.
Is the direction down vertically with these settings? Is Pattern Orientation = 86.788 correct for dither in Y direction on array?LINEfalsefalse286.788WFC3-IR-DITHER-LINE1falsePOS-TARGDITHEROTHER310.0LINEfalsefalse1.0286.788POS-TARGLINE86.7883trueTiming link suitability includes constraints ([01 After 02 by 1.0 to 500.0 days])The scheduling data was generated by CASM 27.2.CASM was run in Phase II mode.These comments apply to all observations of this target, and are copied in Visits 1 to 4.
This target is a binary pair of brown dwarfs with a separation of ~0".8 or 6 pixels. The position angle of B is -31.6deg E of N (that it, B is at about 1 o'clock relative to A). This was measured in 2012, and I have contacted the authors of the imaging discovery paper, and they are not monitoring the system and do not have a more recent measurement. It would be ideal to make an early observation of this system to make any adjustments for a more optimal ORIENT range, if needed due to orbital motion. Due to this consideration, Visits 1, 3, and 4 are tagged with a timing requirement of -- after Visit 2 -- so that the orientation of Visit 2 can be checked.
The aim of the observation is to have the binary pair vertical on the detector so that the spectra are as separate as possible, either with B above A or B below A, so the ORIENT ranges have been set up to be +/-33degrees of vertical such that the vertical separation is 5-6 pixels.
The central value of ORIENT was set to 103.4deg (or 103.4+180deg) based on the manual, from 135deg-31.6deg=103.4deg. The 135deg is used for the Y-axis of WFC3/IR.
This target has conflicting values of proper motion in two papers by the same group, and the most recent published value is used.1594741196000134.02999999999997(Tic-Visit
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)true10Timing link suitability includes constraints ([01 After 02 by 1.0 to 500.0 days] [03 After 02 by 1.0 to 500.0 days] [04 After 02 by 1.0 to 500.0 days])The scheduling data was generated by CASM 27.2.CASM was run in Phase II mode.These comments apply to all observations of this target, and are copied in Visits 1 to 4.
This target is a binary pair of brown dwarfs with a separation of ~0".8 or 6 pixels. The position angle of B is -31.6deg E of N (that it, B is at about 1 o'clock relative to A). This was measured in 2012, and I have contacted the authors of the imaging discovery paper, and they are not monitoring the system and do not have a more recent measurement. It would be ideal to make an early observation of this system to make any adjustments for a more optimal ORIENT range, if needed due to orbital motion. Due to this consideration, Visits 1, 3, and 4 are tagged with a timing requirement of -- after Visit 2 -- so that the orientation of Visit 2 can be checked.
The aim of the observation is to have the binary pair vertical on the detector so that the spectra are as separate as possible, either with B above A or B below A, so the ORIENT ranges have been set up to be +/-33degrees of vertical such that the vertical separation is 5-6 pixels.
The central value of ORIENT was set to 103.4deg (or 103.4+180deg) based on the manual, from 135deg-31.6deg=103.4deg. The 135deg is used for the Y-axis of WFC3/IR.
This target has conflicting values of proper motion in two papers by the same group, and the most recent published value is used.1594632547000136.39999999999998(Tic-Visit
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)true10Timing link suitability includes constraints ([03 After 02 by 1.0 to 500.0 days])The scheduling data was generated by CASM 27.2.CASM was run in Phase II mode.These comments apply to all observations of this target, and are copied in Visits 1 to 4.
This target is a binary pair of brown dwarfs with a separation of ~0".8 or 6 pixels. The position angle of B is -31.6deg E of N (that it, B is at about 1 o'clock relative to A). This was measured in 2012, and I have contacted the authors of the imaging discovery paper, and they are not monitoring the system and do not have a more recent measurement. It would be ideal to make an early observation of this system to make any adjustments for a more optimal ORIENT range, if needed due to orbital motion. Due to this consideration, Visits 1, 3, and 4 are tagged with a timing requirement of -- after Visit 2 -- so that the orientation of Visit 2 can be checked.
The aim of the observation is to have the binary pair vertical on the detector so that the spectra are as separate as possible, either with B above A or B below A, so the ORIENT ranges have been set up to be +/-33degrees of vertical such that the vertical separation is 5-6 pixels.
The central value of ORIENT was set to 103.4deg (or 103.4+180deg) based on the manual, from 135deg-31.6deg=103.4deg. The 135deg is used for the Y-axis of WFC3/IR.
This target has conflicting values of proper motion in two papers by the same group, and the most recent published value is used.1594889872000136.39999999999998(Tic-Visit
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:dark-offset NIL
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:pcs-gap 0
)true10Timing link suitability includes constraints ([04 After 02 by 1.0 to 500.0 days])The scheduling data was generated by CASM 27.2.CASM was run in Phase II mode.These comments apply to all observations of this target, and are copied in Visits 1 to 4.
This target is a binary pair of brown dwarfs with a separation of ~0".8 or 6 pixels. The position angle of B is -31.6deg E of N (that it, B is at about 1 o'clock relative to A). This was measured in 2012, and I have contacted the authors of the imaging discovery paper, and they are not monitoring the system and do not have a more recent measurement. It would be ideal to make an early observation of this system to make any adjustments for a more optimal ORIENT range, if needed due to orbital motion. Due to this consideration, Visits 1, 3, and 4 are tagged with a timing requirement of -- after Visit 2 -- so that the orientation of Visit 2 can be checked.
The aim of the observation is to have the binary pair vertical on the detector so that the spectra are as separate as possible, either with B above A or B below A, so the ORIENT ranges have been set up to be +/-33degrees of vertical such that the vertical separation is 5-6 pixels.
The central value of ORIENT was set to 103.4deg (or 103.4+180deg) based on the manual, from 135deg-31.6deg=103.4deg. The 135deg is used for the Y-axis of WFC3/IR.
This target has conflicting values of proper motion in two papers by the same group, and the most recent published value is used.1594895591000136.39999999999998(Tic-Visit
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:si-bright-earth-limb-angle 20.0
:data-volume 661536
:tdrss-contact-duration 0
:coron NIL
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(Tic-Obset
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:pcs-gap 0
)true10Timing link suitability includes constraints ([05 After 06 by 1.0 to 500.0 days])The scheduling data was generated by CASM 27.2.CASM was run in Phase II mode.These comments apply to all observations of this target, and are copied in Visits 5 to 8.
This target is a binary pair of brown dwarfs with a separation of ~0".78 or 5.6 pixels. The position angle of B is 14.5deg E of N (that it, B is between 11 and 12 o'clock relative to A). This was measured in 2012, and I have contacted the authors of the imaging discovery paper, and they are not monitoring the system and do not have a more recent measurement. It would be ideal to make an early observation of this system to make any adjustments for a more optimal ORIENT range, if needed due to orbital motion. Due to this consideration, Visits 5, 7, and 8 are tagged with a timing requirement of -- after Visit 6 -- so that the orientation of Visit 6 can be checked.
The aim of the observation is to have the binary pair vertical on the detector so that the spectra are as separate as possible, either with B above A or B below A, so the ORIENT ranges have been set up to be +/-27degrees of vertical such that the vertical separation is 5-5.6 pixels.
The central value of ORIENT was set to 149.5deg (or 149.5+180deg) based on the manual, from 135deg+14.5deg=149.5deg. The 135deg is used for the Y-axis of WFC3/IR.1605452900000305.5134284419703(Tic-Visit
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:number-of-orbits 1
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:si-bright-earth-limb-angle 20.0
:data-volume 591888
:tdrss-contact-duration 0
:coron NIL
)
(Tic-Obset
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)true10Timing link suitability includes constraints ([05 After 06 by 1.0 to 500.0 days] [07 After 06 by 1.0 to 500.0 days] [08 After 06 by 1.0 to 500.0 days])The scheduling data was generated by CASM 27.2.CASM was run in Phase II mode.These comments apply to all observations of this target, and are copied in Visits 5 to 8.
This target is a binary pair of brown dwarfs with a separation of ~0".78 or 5.6 pixels. The position angle of B is 14.5deg E of N (that it, B is between 11 and 12 o'clock relative to A). This was measured in 2012, and I have contacted the authors of the imaging discovery paper, and they are not monitoring the system and do not have a more recent measurement. It would be ideal to make an early observation of this system to make any adjustments for a more optimal ORIENT range, if needed due to orbital motion. Due to this consideration, Visits 5, 7, and 8 are tagged with a timing requirement of -- after Visit 6 -- so that the orientation of Visit 6 can be checked.
The aim of the observation is to have the binary pair vertical on the detector so that the spectra are as separate as possible, either with B above A or B below A, so the ORIENT ranges have been set up to be +/-27degrees of vertical such that the vertical separation is 5-5.6 pixels.
The central value of ORIENT was set to 149.5deg (or 149.5+180deg) based on the manual, from 135deg+14.5deg=149.5deg. The 135deg is used for the Y-axis of WFC3/IR.1605305179000306.2252038925277(Tic-Visit
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:coron NIL
)
(Tic-Obset
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)true10Timing link suitability includes constraints ([07 After 06 by 1.0 to 500.0 days])The scheduling data was generated by CASM 27.2.CASM was run in Phase II mode.These comments apply to all observations of this target, and are copied in Visits 5 to 8.
This target is a binary pair of brown dwarfs with a separation of ~0".78 or 5.6 pixels. The position angle of B is 14.5deg E of N (that it, B is between 11 and 12 o'clock relative to A). This was measured in 2012, and I have contacted the authors of the imaging discovery paper, and they are not monitoring the system and do not have a more recent measurement. It would be ideal to make an early observation of this system to make any adjustments for a more optimal ORIENT range, if needed due to orbital motion. Due to this consideration, Visits 5, 7, and 8 are tagged with a timing requirement of -- after Visit 6 -- so that the orientation of Visit 6 can be checked.
The aim of the observation is to have the binary pair vertical on the detector so that the spectra are as separate as possible, either with B above A or B below A, so the ORIENT ranges have been set up to be +/-27degrees of vertical such that the vertical separation is 5-5.6 pixels.
The central value of ORIENT was set to 149.5deg (or 149.5+180deg) based on the manual, from 135deg+14.5deg=149.5deg. The 135deg is used for the Y-axis of WFC3/IR.1605464396000305.4590933499409(Tic-Visit
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:data-volume 591888
:tdrss-contact-duration 0
:coron NIL
)
(Tic-Obset
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)true10Timing link suitability includes constraints ([08 After 06 by 1.0 to 500.0 days])The scheduling data was generated by CASM 27.2.CASM was run in Phase II mode.These comments apply to all observations of this target, and are copied in Visits 5 to 8.
This target is a binary pair of brown dwarfs with a separation of ~0".78 or 5.6 pixels. The position angle of B is 14.5deg E of N (that it, B is between 11 and 12 o'clock relative to A). This was measured in 2012, and I have contacted the authors of the imaging discovery paper, and they are not monitoring the system and do not have a more recent measurement. It would be ideal to make an early observation of this system to make any adjustments for a more optimal ORIENT range, if needed due to orbital motion. Due to this consideration, Visits 5, 7, and 8 are tagged with a timing requirement of -- after Visit 6 -- so that the orientation of Visit 6 can be checked.
The aim of the observation is to have the binary pair vertical on the detector so that the spectra are as separate as possible, either with B above A or B below A, so the ORIENT ranges have been set up to be +/-27degrees of vertical such that the vertical separation is 5-5.6 pixels.
The central value of ORIENT was set to 149.5deg (or 149.5+180deg) based on the manual, from 135deg+14.5deg=149.5deg. The 135deg is used for the Y-axis of WFC3/IR.1606236992000302.5(Tic-Visit
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:trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0
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:si-bright-earth-limb-angle 20.0
:data-volume 591888
:tdrss-contact-duration 0
:coron NIL
)
(Tic-Obset
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(Tic-Orbit
:proposal-id 15819
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:pcs-gap 0
)true10Timing link suitability includes constraints ([12 After 09 by 1.0 to 500.0 days] [09 After 11 by 1.0 to 500.0 days])The scheduling data was generated by CASM 27.2.CASM was run in Phase II mode.These comments apply to all observations of this target, and are copied in Visits 9-14.
This target is a brown dwarf/planet companion to a bright star with a separation of ~2.5arcseconds or 19 pixels. The position angle of B is ~319deg E of N (that it, B is between 10 and 11 o'clock relative to A). This target is being monitored for orbital motion, and the group following the orbit provided these relations to estimate the separation and position angle at a given time t expressed in fractional years, such as 2020.5:
Sep (mas) = -2894.9367 + 2.6746 x t
P.A. (deg) = 2354.0681 - 1.0075 x t
For a date of 2020.0, the separation is 2.507arcseconds and the P.A. is 319.9deg E of N.
To check the orientation, the Visits are set to occur after Visit 11 which will be used to confirm that the ORIENT is the best possible value.
The aim of the observation is to have the binary pair arranged such that they are vertical and their dispersed spectra do not overlap. The smallest subarray is used to enable exposure times that have a series of reads that include unsaturated spectra of the primary and exposures that should saturate out to a radius of 5 pixels based on radial profile information provided by STScI.
For the best PSF stability, the ORIENT for Visits 12 and 13 are set to match Visit 11; these are all using the same grism.
To subtract the stellar background, an observation at an orientation different by 175-180degrees is taken in each grism. Visits 10 and 14 are the background observations and have an orientation requirement based on Visit 9 or Visit 11.(Tic-Visit
:proposal-id 15819
:visit-id "09"
:proposal-version -1
:trans-version "20190514"
:date "13-Dec-2019 20:54:03.0"
: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 588032
:tdrss-contact-duration 0
:coron NIL
)
(Tic-Obset
:proposal-id 15819
:visit-id "09"
:obset-id "09"
:pcs-mode "FGS"
)
(Tic-Orbit
:proposal-id 15819
:visit-id "09"
:orbit-number 1
:pcs-time 333
:si-vis-utilization 2671
:al-overhead-at-end 0
:internal-dur-at-end 396
:dark-offset NIL
:dark-utilization 0
:max-dark-utilization 1920
:low-sky "N"
:pcs-visibility 3145
:pcs-gap 0
)false10Timing link suitability includes constraints ([10 After 11 by 1.0 to 500.0 days])The scheduling data was generated by CASM 27.2.CASM was run in Phase II mode.These comments apply to all observations of this target, and are copied in Visits 9-14.
This target is a brown dwarf/planet companion to a bright star with a separation of ~2.5arcseconds or 19 pixels. The position angle of B is ~319deg E of N (that it, B is between 10 and 11 o'clock relative to A). This target is being monitored for orbital motion, and the group following the orbit provided these relations to estimate the separation and position angle at a given time t expressed in fractional years, such as 2020.5:
Sep (mas) = -2894.9367 + 2.6746 x t
P.A. (deg) = 2354.0681 - 1.0075 x t
For a date of 2020.0, the separation is 2.507arcseconds and the P.A. is 319.9deg E of N.
To check the orientation, the Visits are set to occur after Visit 11 which will be used to confirm that the ORIENT is the best possible value.
The aim of the observation is to have the binary pair arranged such that they are vertical and their dispersed spectra do not overlap. The smallest subarray is used to enable exposure times that have a series of reads that include unsaturated spectra of the primary and exposures that should saturate out to a radius of 5 pixels based on radial profile information provided by STScI.
For the best PSF stability, the ORIENT for Visits 12 and 13 are set to match Visit 11; these are all using the same grism.
To subtract the stellar background, an observation at an orientation different by 175-180degrees is taken in each grism. Visits 10 and 14 are the background observations and have an orientation requirement based on Visit 9 or Visit 11.(Tic-Visit
:proposal-id 15819
:visit-id "10"
:proposal-version -1
:trans-version "20190514"
:date "13-Dec-2019 20:54:11.0"
: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 588032
:tdrss-contact-duration 0
:coron NIL
)
(Tic-Obset
:proposal-id 15819
:visit-id "10"
:obset-id "10"
:pcs-mode "FGS"
)
(Tic-Orbit
:proposal-id 15819
:visit-id "10"
:orbit-number 1
:pcs-time 333
:si-vis-utilization 2671
:al-overhead-at-end 0
:internal-dur-at-end 396
:dark-offset NIL
:dark-utilization 0
:max-dark-utilization 1920
:low-sky "N"
:pcs-visibility 3145
:pcs-gap 0
)false10Timing link suitability includes constraints ([09 After 11 by 1.0 to 500.0 days] [10 After 11 by 1.0 to 500.0 days])The scheduling data was generated by CASM 27.2.CASM was run in Phase II mode.These comments apply to all observations of this target, and are copied in Visits 9-14.
This target is a brown dwarf/planet companion to a bright star with a separation of ~2.5arcseconds or 19 pixels. The position angle of B is ~319deg E of N (that it, B is between 10 and 11 o'clock relative to A). This target is being monitored for orbital motion, and the group following the orbit provided these relations to estimate the separation and position angle at a given time t expressed in fractional years, such as 2020.5:
Sep (mas) = -2894.9367 + 2.6746 x t
P.A. (deg) = 2354.0681 - 1.0075 x t
For a date of 2020.0, the separation is 2.507arcseconds and the P.A. is 319.9deg E of N.
To check the orientation, the Visits are set to occur after Visit 11 which will be used to confirm that the ORIENT is the best possible value.
The aim of the observation is to have the binary pair arranged such that they are vertical and their dispersed spectra do not overlap. The smallest subarray is used to enable exposure times that have a series of reads that include unsaturated spectra of the primary and exposures that should saturate out to a radius of 5 pixels based on radial profile information provided by STScI.
For the best PSF stability, the ORIENT for Visits 12 and 13 are set to match Visit 11; these are all using the same grism.
To subtract the stellar background, an observation at an orientation different by 175-180degrees is taken in each grism. Visits 10 and 14 are the background observations and have an orientation requirement based on Visit 9 or Visit 11.(Tic-Visit
:proposal-id 15819
:visit-id "11"
:proposal-version -1
:trans-version "20190514"
:date "13-Dec-2019 11:38:44.0"
: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 588032
:tdrss-contact-duration 0
:coron NIL
)
(Tic-Obset
:proposal-id 15819
:visit-id "11"
:obset-id "11"
:pcs-mode "FGS"
)
(Tic-Orbit
:proposal-id 15819
:visit-id "11"
:orbit-number 1
:pcs-time 333
:si-vis-utilization 2669
:al-overhead-at-end 0
:internal-dur-at-end 396
:dark-offset NIL
:dark-utilization 0
:max-dark-utilization 1920
:low-sky "N"
:pcs-visibility 3145
:pcs-gap 0
)false10Timing link suitability includes constraints ([12 After 09 by 1.0 to 500.0 days])The scheduling data was generated by CASM 27.2.CASM was run in Phase II mode.These comments apply to all observations of this target, and are copied in Visits 9-14.
This target is a brown dwarf/planet companion to a bright star with a separation of ~2.5arcseconds or 19 pixels. The position angle of B is ~319deg E of N (that it, B is between 10 and 11 o'clock relative to A). This target is being monitored for orbital motion, and the group following the orbit provided these relations to estimate the separation and position angle at a given time t expressed in fractional years, such as 2020.5:
Sep (mas) = -2894.9367 + 2.6746 x t
P.A. (deg) = 2354.0681 - 1.0075 x t
For a date of 2020.0, the separation is 2.507arcseconds and the P.A. is 319.9deg E of N.
To check the orientation, the Visits are set to occur after Visit 11 which will be used to confirm that the ORIENT is the best possible value.
The aim of the observation is to have the binary pair arranged such that they are vertical and their dispersed spectra do not overlap. The smallest subarray is used to enable exposure times that have a series of reads that include unsaturated spectra of the primary and exposures that should saturate out to a radius of 5 pixels based on radial profile information provided by STScI.
For the best PSF stability, the ORIENT for Visits 12 and 13 are set to match Visit 11; these are all using the same grism.
To subtract the stellar background, an observation at an orientation different by 175-180degrees is taken in each grism. Visits 10 and 14 are the background observations and have an orientation requirement based on Visit 9 or Visit 11.(Tic-Visit
:proposal-id 15819
:visit-id "12"
:proposal-version -1
:trans-version "20190514"
:date "13-Dec-2019 11:38:55.0"
: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 588032
:tdrss-contact-duration 0
:coron NIL
)
(Tic-Obset
:proposal-id 15819
:visit-id "12"
:obset-id "12"
:pcs-mode "FGS"
)
(Tic-Orbit
:proposal-id 15819
:visit-id "12"
:orbit-number 1
:pcs-time 333
:si-vis-utilization 2669
:al-overhead-at-end 0
:internal-dur-at-end 396
:dark-offset NIL
:dark-utilization 0
:max-dark-utilization 1920
:low-sky "N"
:pcs-visibility 3145
:pcs-gap 0
)false10The scheduling data was generated by CASM 27.2.CASM was run in Phase II mode.These comments apply to all observations of this target, and are copied in Visits 9-14.
This target is a brown dwarf/planet companion to a bright star with a separation of ~2.5arcseconds or 19 pixels. The position angle of B is ~319deg E of N (that it, B is between 10 and 11 o'clock relative to A). This target is being monitored for orbital motion, and the group following the orbit provided these relations to estimate the separation and position angle at a given time t expressed in fractional years, such as 2020.5:
Sep (mas) = -2894.9367 + 2.6746 x t
P.A. (deg) = 2354.0681 - 1.0075 x t
For a date of 2020.0, the separation is 2.507arcseconds and the P.A. is 319.9deg E of N.
To check the orientation, the Visits are set to occur after Visit 11 which will be used to confirm that the ORIENT is the best possible value.
The aim of the observation is to have the binary pair arranged such that they are vertical and their dispersed spectra do not overlap. The smallest subarray is used to enable exposure times that have a series of reads that include unsaturated spectra of the primary and exposures that should saturate out to a radius of 5 pixels based on radial profile information provided by STScI.
For the best PSF stability, the ORIENT for Visits 12 and 13 are set to match Visit 11; these are all using the same grism.
To subtract the stellar background, an observation at an orientation different by 175-180degrees is taken in each grism. Visits 10 and 14 are the background observations and have an orientation requirement based on Visit 9 or Visit 11.(Tic-Visit
:proposal-id 15819
:visit-id "13"
:proposal-version -1
:trans-version "20190514"
:date "13-Dec-2019 11:39:05.0"
: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 588032
:tdrss-contact-duration 0
:coron NIL
)
(Tic-Obset
:proposal-id 15819
:visit-id "13"
:obset-id "13"
:pcs-mode "FGS"
)
(Tic-Orbit
:proposal-id 15819
:visit-id "13"
:orbit-number 1
:pcs-time 333
:si-vis-utilization 2669
:al-overhead-at-end 0
:internal-dur-at-end 396
:dark-offset NIL
:dark-utilization 0
:max-dark-utilization 1920
:low-sky "N"
:pcs-visibility 3145
:pcs-gap 0
)false10The scheduling data was generated by CASM 27.2.CASM was run in Phase II mode.These comments apply to all observations of this target, and are copied in Visits 9-14.
This target is a brown dwarf/planet companion to a bright star with a separation of ~2.5arcseconds or 19 pixels. The position angle of B is ~319deg E of N (that it, B is between 10 and 11 o'clock relative to A). This target is being monitored for orbital motion, and the group following the orbit provided these relations to estimate the separation and position angle at a given time t expressed in fractional years, such as 2020.5:
Sep (mas) = -2894.9367 + 2.6746 x t
P.A. (deg) = 2354.0681 - 1.0075 x t
For a date of 2020.0, the separation is 2.507arcseconds and the P.A. is 319.9deg E of N.
To check the orientation, the Visits are set to occur after Visit 11 which will be used to confirm that the ORIENT is the best possible value.
The aim of the observation is to have the binary pair arranged such that they are vertical and their dispersed spectra do not overlap. The smallest subarray is used to enable exposure times that have a series of reads that include unsaturated spectra of the primary and exposures that should saturate out to a radius of 5 pixels based on radial profile information provided by STScI.
For the best PSF stability, the ORIENT for Visits 12 and 13 are set to match Visit 11; these are all using the same grism.
To subtract the stellar background, an observation at an orientation different by 175-180degrees is taken in each grism. Visits 10 and 14 are the background observations and have an orientation requirement based on Visit 9 or Visit 11.(Tic-Visit
:proposal-id 15819
:visit-id "14"
:proposal-version -1
:trans-version "20190514"
:date "13-Dec-2019 11:39:15.0"
: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 588032
:tdrss-contact-duration 0
:coron NIL
)
(Tic-Obset
:proposal-id 15819
:visit-id "14"
:obset-id "14"
:pcs-mode "FGS"
)
(Tic-Orbit
:proposal-id 15819
:visit-id "14"
:orbit-number 1
:pcs-time 333
:si-vis-utilization 2669
:al-overhead-at-end 0
:internal-dur-at-end 396
:dark-offset NIL
:dark-utilization 0
:max-dark-utilization 1920
:low-sky "N"
:pcs-visibility 3145
:pcs-gap 0
)false10Timing link suitability includes constraints ([15 After 17 by 1.0 to 500.0 days])The scheduling data was generated by CASM 27.2.CASM was run in Phase II mode.These comments apply to all observations of this target, and are copied in each Visit for this target, Visits 15-20.
This target is a brown dwarf/planet companion to a bright star with a separation of ~1.5arcseconds or 11.5 pixels. The position angle of B is ~208deg E of N (that it, B is between 4 and 5 o'clock relative to A). This target is being monitored for orbital motion, and the group following the orbit provided estimates for changes from a time of 2014.7 into future dates:
Change in sep. (mas) = -34mas/yr
Change in P.A.(deg) = 1.86deg/yr
Sep. in 2014.7: 1697mas
P.A. in 2014.7: 207.8deg
For a date of 2020.0, the separation is 1.516arcseconds and the P.A. is 217.7deg E of N.
To check the orientation, the Visits are set to occur after Visit 17 which will be used to confirm that the ORIENT is the best possible value.
The aim of the observation is to have the binary pair arranged such that they are vertical and their dispersed spectra do not overlap. The smallest subarray is used to enable exposure times that have a series of reads that include unsaturated spectra of the primary and exposures that should saturate out to a radius of 5 pixels based on radial profile information provided by STScI.
For the best PSF stability, the ORIENT for Visits 18 and 19 are set to match Visit 17; these are all using the same grism.
To subtract the stellar background, an observation at an orientation different by 175-180degrees is taken in each grism. Visits 16 and 20 are the background observations and have an orientation requirement linked to Visit 15 or Visit 17.1592894426000192.0(Tic-Visit
:proposal-id 15819
:visit-id "15"
:proposal-version -1
:trans-version "20190514"
:date "12-Dec-2019 21:12:11.0"
: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 588032
:tdrss-contact-duration 0
:coron NIL
)
(Tic-Obset
:proposal-id 15819
:visit-id "15"
:obset-id "15"
:pcs-mode "FGS"
)
(Tic-Orbit
:proposal-id 15819
:visit-id "15"
:orbit-number 1
:pcs-time 333
:si-vis-utilization 2671
:al-overhead-at-end 0
:internal-dur-at-end 396
:dark-offset NIL
:dark-utilization 0
:max-dark-utilization 1920
:low-sky "N"
:pcs-visibility 3180
:pcs-gap 0
)true10Timing link suitability includes constraints ([16 After 17 by 1.0 to 500.0 days])The scheduling data was generated by CASM 27.2.CASM was run in Phase II mode.These comments apply to all observations of this target, and are copied in each Visit for this target, Visits 15-20.
This target is a brown dwarf/planet companion to a bright star with a separation of ~1.5arcseconds or 11.5 pixels. The position angle of B is ~208deg E of N (that it, B is between 4 and 5 o'clock relative to A). This target is being monitored for orbital motion, and the group following the orbit provided estimates for changes from a time of 2014.7 into future dates:
Change in sep. (mas) = -34mas/yr
Change in P.A.(deg) = 1.86deg/yr
Sep. in 2014.7: 1697mas
P.A. in 2014.7: 207.8deg
For a date of 2020.0, the separation is 1.516arcseconds and the P.A. is 217.7deg E of N.
To check the orientation, the Visits are set to occur after Visit 17 which will be used to confirm that the ORIENT is the best possible value.
The aim of the observation is to have the binary pair arranged such that they are vertical and their dispersed spectra do not overlap. The smallest subarray is used to enable exposure times that have a series of reads that include unsaturated spectra of the primary and exposures that should saturate out to a radius of 5 pixels based on radial profile information provided by STScI.
For the best PSF stability, the ORIENT for Visits 18 and 19 are set to match Visit 17; these are all using the same grism.
To subtract the stellar background, an observation at an orientation different by 175-180degrees is taken in each grism. Visits 16 and 20 are the background observations and have an orientation requirement linked to Visit 15 or Visit 17.16093776620007.0(Tic-Visit
:proposal-id 15819
:visit-id "16"
:proposal-version -1
:trans-version "20190514"
:date "13-Dec-2019 20:54:18.0"
: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 588032
:tdrss-contact-duration 0
:coron NIL
)
(Tic-Obset
:proposal-id 15819
:visit-id "16"
:obset-id "16"
:pcs-mode "FGS"
)
(Tic-Orbit
:proposal-id 15819
:visit-id "16"
:orbit-number 1
:pcs-time 333
:si-vis-utilization 2671
:al-overhead-at-end 0
:internal-dur-at-end 396
:dark-offset NIL
:dark-utilization 0
:max-dark-utilization 1920
:low-sky "N"
:pcs-visibility 3180
:pcs-gap 0
)true10Timing link suitability includes constraints ([15 After 17 by 1.0 to 500.0 days] [16 After 17 by 1.0 to 500.0 days] [18 After 17 by 1.0 to 500.0 days] [19 After 17 by 1.0 to 500.0 days] [20 After 17 by 1.0 to 500.0 days])Hst Same orient constraint links visits (17 18 19)The scheduling data was generated by CASM 27.2.CASM was run in Phase II mode.These comments apply to all observations of this target, and are copied in each Visit for this target, Visits 15-20.
This target is a brown dwarf/planet companion to a bright star with a separation of ~1.5arcseconds or 11.5 pixels. The position angle of B is ~208deg E of N (that it, B is between 4 and 5 o'clock relative to A). This target is being monitored for orbital motion, and the group following the orbit provided estimates for changes from a time of 2014.7 into future dates:
Change in sep. (mas) = -34mas/yr
Change in P.A.(deg) = 1.86deg/yr
Sep. in 2014.7: 1697mas
P.A. in 2014.7: 207.8deg
For a date of 2020.0, the separation is 1.516arcseconds and the P.A. is 217.7deg E of N.
To check the orientation, the Visits are set to occur after Visit 17 which will be used to confirm that the ORIENT is the best possible value.
The aim of the observation is to have the binary pair arranged such that they are vertical and their dispersed spectra do not overlap. The smallest subarray is used to enable exposure times that have a series of reads that include unsaturated spectra of the primary and exposures that should saturate out to a radius of 5 pixels based on radial profile information provided by STScI.
For the best PSF stability, the ORIENT for Visits 18 and 19 are set to match Visit 17; these are all using the same grism.
To subtract the stellar background, an observation at an orientation different by 175-180degrees is taken in each grism. Visits 16 and 20 are the background observations and have an orientation requirement linked to Visit 15 or Visit 17.1592425724000194.0(Tic-Visit
:proposal-id 15819
:visit-id "17"
:proposal-version -1
:trans-version "20190514"
:date "12-Dec-2019 20:48:18.0"
: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 588032
:tdrss-contact-duration 0
:coron NIL
)
(Tic-Obset
:proposal-id 15819
:visit-id "17"
:obset-id "17"
:pcs-mode "FGS"
)
(Tic-Orbit
:proposal-id 15819
:visit-id "17"
:orbit-number 1
:pcs-time 333
:si-vis-utilization 2669
:al-overhead-at-end 0
:internal-dur-at-end 396
:dark-offset NIL
:dark-utilization 0
:max-dark-utilization 1920
:low-sky "N"
:pcs-visibility 3180
:pcs-gap 0
)true10Timing link suitability includes constraints ([18 After 17 by 1.0 to 500.0 days])Hst Same orient constraint links visits (17 18 19)The scheduling data was generated by CASM 27.2.CASM was run in Phase II mode.These comments apply to all observations of this target, and are copied in each Visit for this target, Visits 15-20.
This target is a brown dwarf/planet companion to a bright star with a separation of ~1.5arcseconds or 11.5 pixels. The position angle of B is ~208deg E of N (that it, B is between 4 and 5 o'clock relative to A). This target is being monitored for orbital motion, and the group following the orbit provided estimates for changes from a time of 2014.7 into future dates:
Change in sep. (mas) = -34mas/yr
Change in P.A.(deg) = 1.86deg/yr
Sep. in 2014.7: 1697mas
P.A. in 2014.7: 207.8deg
For a date of 2020.0, the separation is 1.516arcseconds and the P.A. is 217.7deg E of N.
To check the orientation, the Visits are set to occur after Visit 17 which will be used to confirm that the ORIENT is the best possible value.
The aim of the observation is to have the binary pair arranged such that they are vertical and their dispersed spectra do not overlap. The smallest subarray is used to enable exposure times that have a series of reads that include unsaturated spectra of the primary and exposures that should saturate out to a radius of 5 pixels based on radial profile information provided by STScI.
For the best PSF stability, the ORIENT for Visits 18 and 19 are set to match Visit 17; these are all using the same grism.
To subtract the stellar background, an observation at an orientation different by 175-180degrees is taken in each grism. Visits 16 and 20 are the background observations and have an orientation requirement linked to Visit 15 or Visit 17.1592917300000194.0(Tic-Visit
:proposal-id 15819
:visit-id "18"
:proposal-version -1
:trans-version "20190514"
:date "12-Dec-2019 20:51:09.0"
: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 588032
:tdrss-contact-duration 0
:coron NIL
)
(Tic-Obset
:proposal-id 15819
:visit-id "18"
:obset-id "18"
:pcs-mode "FGS"
)
(Tic-Orbit
:proposal-id 15819
:visit-id "18"
:orbit-number 1
:pcs-time 333
:si-vis-utilization 2669
:al-overhead-at-end 0
:internal-dur-at-end 396
:dark-offset NIL
:dark-utilization 0
:max-dark-utilization 1920
:low-sky "N"
:pcs-visibility 3180
:pcs-gap 0
)true10Timing link suitability includes constraints ([19 After 17 by 1.0 to 500.0 days])Hst Same orient constraint links visits (17 18 19)The scheduling data was generated by CASM 27.2.CASM was run in Phase II mode.These comments apply to all observations of this target, and are copied in each Visit for this target, Visits 15-20.
This target is a brown dwarf/planet companion to a bright star with a separation of ~1.5arcseconds or 11.5 pixels. The position angle of B is ~208deg E of N (that it, B is between 4 and 5 o'clock relative to A). This target is being monitored for orbital motion, and the group following the orbit provided estimates for changes from a time of 2014.7 into future dates:
Change in sep. (mas) = -34mas/yr
Change in P.A.(deg) = 1.86deg/yr
Sep. in 2014.7: 1697mas
P.A. in 2014.7: 207.8deg
For a date of 2020.0, the separation is 1.516arcseconds and the P.A. is 217.7deg E of N.
To check the orientation, the Visits are set to occur after Visit 17 which will be used to confirm that the ORIENT is the best possible value.
The aim of the observation is to have the binary pair arranged such that they are vertical and their dispersed spectra do not overlap. The smallest subarray is used to enable exposure times that have a series of reads that include unsaturated spectra of the primary and exposures that should saturate out to a radius of 5 pixels based on radial profile information provided by STScI.
For the best PSF stability, the ORIENT for Visits 18 and 19 are set to match Visit 17; these are all using the same grism.
To subtract the stellar background, an observation at an orientation different by 175-180degrees is taken in each grism. Visits 16 and 20 are the background observations and have an orientation requirement linked to Visit 15 or Visit 17.1593014517000194.0(Tic-Visit
:proposal-id 15819
:visit-id "19"
:proposal-version -1
:trans-version "20190514"
:date "12-Dec-2019 20:58:40.0"
: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 588032
:tdrss-contact-duration 0
:coron NIL
)
(Tic-Obset
:proposal-id 15819
:visit-id "19"
:obset-id "19"
:pcs-mode "FGS"
)
(Tic-Orbit
:proposal-id 15819
:visit-id "19"
:orbit-number 1
:pcs-time 333
:si-vis-utilization 2669
:al-overhead-at-end 0
:internal-dur-at-end 396
:dark-offset NIL
:dark-utilization 0
:max-dark-utilization 1920
:low-sky "N"
:pcs-visibility 3180
:pcs-gap 0
)true10Timing link suitability includes constraints ([20 After 17 by 1.0 to 500.0 days])The scheduling data was generated by CASM 27.2.CASM was run in Phase II mode.These comments apply to all observations of this target, and are copied in each Visit for this target, Visits 15-20.
This target is a brown dwarf/planet companion to a bright star with a separation of ~1.5arcseconds or 11.5 pixels. The position angle of B is ~208deg E of N (that it, B is between 4 and 5 o'clock relative to A). This target is being monitored for orbital motion, and the group following the orbit provided estimates for changes from a time of 2014.7 into future dates:
Change in sep. (mas) = -34mas/yr
Change in P.A.(deg) = 1.86deg/yr
Sep. in 2014.7: 1697mas
P.A. in 2014.7: 207.8deg
For a date of 2020.0, the separation is 1.516arcseconds and the P.A. is 217.7deg E of N.
To check the orientation, the Visits are set to occur after Visit 17 which will be used to confirm that the ORIENT is the best possible value.
The aim of the observation is to have the binary pair arranged such that they are vertical and their dispersed spectra do not overlap. The smallest subarray is used to enable exposure times that have a series of reads that include unsaturated spectra of the primary and exposures that should saturate out to a radius of 5 pixels based on radial profile information provided by STScI.
For the best PSF stability, the ORIENT for Visits 18 and 19 are set to match Visit 17; these are all using the same grism.
To subtract the stellar background, an observation at an orientation different by 175-180degrees is taken in each grism. Visits 16 and 20 are the background observations and have an orientation requirement linked to Visit 15 or Visit 17.160902920200012.0(Tic-Visit
:proposal-id 15819
:visit-id "20"
:proposal-version -1
:trans-version "20190514"
:date "12-Dec-2019 21:05:18.0"
: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 588032
:tdrss-contact-duration 0
:coron NIL
)
(Tic-Obset
:proposal-id 15819
:visit-id "20"
:obset-id "20"
:pcs-mode "FGS"
)
(Tic-Orbit
:proposal-id 15819
:visit-id "20"
:orbit-number 1
:pcs-time 333
:si-vis-utilization 2669
:al-overhead-at-end 0
:internal-dur-at-end 396
:dark-offset NIL
:dark-utilization 0
:max-dark-utilization 1920
:low-sky "N"
:pcs-visibility 3180
:pcs-gap 0
)true10