final submission? 1910512329 Assigned ID: 683 ----- Attempting Submission 1 (Fri Apr 11 18:55:26 GMT 2014) ----- HST Phase I Proposal 683 (TWHya.apt) successfully submitted. ----- Attempting Submission 2 (Fri Apr 11 22:01:48 GMT 2014) ----- HST Phase I Proposal 683 (TWHya.apt) successfully submitted. ORBITAL VISIBILITY OVERRUN ORBITAL VISIBILITY OVERRUN ORBITAL VISIBILITY OVERRUN First draft of submission Available mode not formally approved, but request is into STIS user support lead Submission 1: PSF star has changed from Phase I (request approved by Nolan Walborn), and will trigger Duplication flags because it was used previously for program 8624. Since it is a PSF reference, it should not conflict with current duplication policies. I do want to verify that Visits 6 and Visits 7 will be reasonably close by in relative orientation to each other once scheduling has begun. Submission 2: fixed typos per suggestion of Charles Proffitt Submission 3: Increased BAR5 exposure times by roughly factor of 5 to get to 50% full well in Visits 1-4. Changed CR-SPLITs to account for this. -1646376009 ----- Attempting Submission 1 (Thu Jul 24 20:01:14 GMT 2014) ----- ----- Attempting Submission 2 (Thu Sep 04 17:57:26 GMT 2014) ----- ----- Attempting Submission 3 (Thu Jan 07 19:28:02 GMT 2016) ----- Warnings/Errors on previously observed visits. We propose to use eight orbits of HST/STIS coronagraphy with the new bent finger occulter (BAR5) to probe, for the first time in visible scattered light, the protoplanetary disk of TW Hya down to as close as 8-13 AU (0.15-0.24"; roughly Saturn's orbit). That distance is a factor of three improvement compared to previous STIS images of this disk taken in 2000. HST/STIS provides a unique window through visible wavelengths at inner working angles on Solar System scales and at a spatial resolution comparable to the highest resolution modes of ALMA in Cycle 2. Previous scattered light observations show that the surface brightness of the disk abruptly changes its character interior to 50 AU, which could be indicative of a gap opened by a forming planet, a large opacity change, or shadowing from the inner disk. We will probe the inner disk at high fidelity, with the goal of discriminating between these three possibilities. A secondary goal will be to look for brightness variations and Keplerian motion of structures in the outer disk during the 15 year baseline between images. These legacy observations of TW Hya's small dust grain population will provide an anchor for future JWST, ALMA, Gemini Planet Imager (GPI), SPHERE, and polarimetric observations of this disk. This proposal is designed to blend the techniques of GO 12228 (a sub-array coroangraphic wedge observation of the target at two wedge positions at multiple orientations) using the newly available but unsupported BAR5 postion on the 50CORON aperture. We will execute a total of 8 visits of one orbit each grouped into two sets of four linked visits. The strategy will be to perform 3 visits of TW Hya interspersed with a single PSF reference observation at each wedge position. For each 4 visit block, we will first perform a target acquisition at the BAR10 position, then POS-TARG to the BAR5 position via parameters determined by the calibration program 12923. We will dither at that position to guard against the slit non-repeatability of the STIS slit mechanism, then switch to the WEDGEA1.0 position to take deeper observations of the outer region of the disk. We attempt to keep the count levels of both TW Hya and its PSF reference as close as possible to avoid CTE effects between the PSF and target. We set exposure times such that 50% of full well is reached at the wedge/bar edges. Since TW Hya is variable we wish to guard against unintended saturation at our innermost working angles. This may also avoid saturation of the PSF in our BAR5 dither positions. DEBRIS DISKS 12 false false false false AVAILABLE STAR M V-IV PRE-MAIN SEQUENCE STAR PROTOPLANETARY DISK REGULAR VARIABLE position from 2MASS, proper motion from UCAC4 J2000 J2000 STAR K V-IV Coordinates taken from 2MASS, proper motion taken from UCAC4 HD-85512 J2000 J2000 STIS/CCD Imaging Yes No BAR10 STIS/CCD Imaging Yes No WEDGEA1.0 STIS/CCD Imaging Yes No BAR10 STIS/CCD Imaging Yes No WEDGEA1.0 STIS/CCD Imaging Yes No BAR10 STIS/CCD Imaging Yes No WEDGEA1.0 STIS/CCD Imaging Yes No BAR10 STIS/CCD Imaging Yes No WEDGEA1.0 Timing link suitability includes constraints ([02 After 01 by 0.0 to 0.1 days]) The scheduling data was generated by CASM 23.2. CASM was run in Phase II mode. 1452189506203 /private/var/folders/9d/jk8g77fd2jx3sxdb33rhwx48000300/T/OPVisit6816745580212233891.xml TW Hya First of two sets of visits, each containing three visits of TW Hya at different relative orientations with one PSF calibration observation interleaved. This is the first TW Hya visit in the first set. The four visits within each set must be executed sequentally in contiguous orbits interrupted only for Earth occultation. Orientation: We wish to schedule this visit (1) at -30 deg from Visit 2, with the absolute orientation of Visit 2 unconstrained. We allow a relative orientation tolerence from -15 deg to -30 deg to assist in guide star selection and scheduling. NOTE to PC: Schedule as close to -30 deg from Visit 2 as possible. Relative Timing: This visit (1) should immediately preceed visit (2). I.e., They should be executed sequentially in "back-to-back" orbits. (Tic-Visit :proposal-id 13753 :visit-id "01" :proposal-version -1 :trans-version "20150609" :date "07-Jan-2016 12:58:26.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 1 :saa-model "24" :si-bright-earth-limb-angle 20.0 :data-volume 33696 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 13753 :visit-id "01" :obset-id "01" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 13753 :visit-id "01" :orbit-number 1 :pcs-time 333 :si-vis-utilization 2750 :al-overhead-at-end 0 :internal-dur-at-end 337 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3092 :pcs-gap 0 ) true 1 0 V = 5.78, sp = A0V, Exptime rounded to nearest 0.1 second ETC Request ID: STIS.ta.625567 NOTE TO PC/CS: Here we use the BAR5 occulter (Aperture) that we comissioned in GO program 12923. This aperture is not available in APT Phase 2, *AND* the SIAF locations of the aperture fiducial we determined in GO 12923 is yet to be populated in SIAF.dat and flowed down to the ground system. We therefore call out BAR10 and use POS TARGs to move the target to the desired positions behind the BAR5 occulter. He we attempt to place the target on the mid-line of BAR5. We then use a subarray readout of CENTYERAXIS2 = 700 appopriate for BAR5 with a SIZEAXIS2 = 137 (the same ass we use elsewhere for Wedge0.6A). SCALABLE BENCHMARK: We expect full-well at r=0.15" with BAR10 from wings of stellar PSF in 1 second for V=5.0 (A0V) {**to be re-verified**}. HR 4796 is V = 5.78 so saturation in 2.09s. So 90% full well in appx 1.85s. Use this for the BAR5 exposures, repeated (8x) with multiple CR Splits. NOTE TO PC/CS: Here we use the BAR5 occulter (Aperture) that we comissioned in GO program 12923. This aperture is not available in APT Phase 2, *AND* the SIAF locations of the aperture fiducial we determined in GO 12923 is yet to be populated in SIAF.dat and flowed down to the ground system. We therefore call out BAR10 and use POS TARGs to move the target to the desired positions behind the BAR5 occulter. He we attempt to place the target 1/4 pixel above the mid-line of BAR5. We then use a subarray readout of CENTYERAXIS2 = 700 appopriate for BAR5 with a SIZEAXIS2 = 137 (the same ass we use elsewhere for Wedge0.6A). SCALABLE BENCHMARK: We expect full-well at r=0.15" with BAR10 from wings of stellar PSF in 1 second for V=5.0 (A0V) {**to be re-verified**}. HR 4796 is V = 5.78 so saturation in 2.09s. So 90% full well in appx 1.85s. Use this for the BAR5 exposures, repeated (8x) with multiple CR Splits. NOTE TO PC/CS: Here we use the BAR5 occulter (Aperture) that we comissioned in GO program 12923. This aperture is not available in APT Phase 2, *AND* the SIAF locations of the aperture fiducial we determined in GO 12923 is yet to be populated in SIAF.dat and flowed down to the ground system. We therefore call out BAR10 and use POS TARGs to move the target to the desired positions behind the BAR5 occulter. He we attempt to place the target 1/4 pixel below the mid-line of BAR5. We then use a subarray readout of CENTYERAXIS2 = 700 appopriate for BAR5 with a SIZEAXIS2 = 137 (the same as we use elsewhere for Wedge0.6A). SCALABLE BENCHMARK: We expect full-well at r=0.15" with BAR10 from wings of stellar PSF in 1 second for V=5.0 (A0V) {**to be re-verified**}. HR 4796 is V = 5.78 so saturation in 2.09s. So 90% full well in appx 1.85s. Use this for the BAR5 exposures, repeated (8x) with multiple CR Splits. SCALABLE BENCHMARK: We expect full-well at r=0.3" from wings of stellar PSF in 1 second for V=3.55 (A0V). HR 4796 is V =5.78 so saturation in 7.80s. So 90% full well in appx 7.02s. Use this for the "short" exposures, repeated (8x) with multiple CR Splits. For long exposures at WedgeA1.0 go (up to) 20x deeper in each that will fit into remainer of visibility period CR-SPLIT at least 3 times - and trim exposure time to fit in visibility window. SCALABLE PARAMETER FOR SUB-ARRAY Readout: SIZEAXIS2 = 20 is 1" in full extent (r = 0.5") For these "long" exposures we will image perpendicular to the wedge (symmetrically) centered on the target to the maximum extent permitted by the limits of the FOV (edge of the detector) on the "small" side of the Wedge A taper. Thus, for these short exposures we use SIZEAXIS12 = 427, appropriate for the WedgeA1.0 position. Timing link suitability includes constraints ([02 After 01 by 0.0 to 0.1 days] [03 After 02 by 0.0 to 0.1 days]) The scheduling data was generated by CASM 23.2. CASM was run in Phase II mode. 1452194438507 /private/var/folders/9d/jk8g77fd2jx3sxdb33rhwx48000300/T/OPVisit6485119183232735602.xml TW Hya First of two sets of visits, each containing three visits of TW HYA at different relative orientations with one PSF calibration observation interleaved. This is the second TW Hya visit in the first set. The four visits within each set must be executed sequentally in contiguous orbits interrupted only for Earth occultation. Orientation: There are no orientation constraints on this visit (2). This visit at nominal roll as scheduled by STScI. Visits 1, 4, 5, 6 and 8 carry relative orientation constraints w.r.t. this visit. Relative Timing: This visit (2) should immediately follow Visit 1 and immediately preceed Visit 3 in back-to-back orbits. (Tic-Visit :proposal-id 13753 :visit-id "02" :proposal-version -1 :trans-version "20150609" :date "07-Jan-2016 14:20:38.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 1 :saa-model "24" :si-bright-earth-limb-angle 20.0 :data-volume 33696 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 13753 :visit-id "02" :obset-id "02" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 13753 :visit-id "02" :orbit-number 1 :pcs-time 333 :si-vis-utilization 2750 :al-overhead-at-end 0 :internal-dur-at-end 337 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3092 :pcs-gap 0 ) true 1 0 V = 5.78, sp = A0V, Exptime rounded to nearest 0.1 second ETC Request ID: STIS.ta.618243 NOTE TO PC/CS: Here we use the BAR5 occulter (Aperture) that we comissioned in GO program 12923. This aperture is not available in APT Phase 2, *AND* the SIAF locations of the aperture fiducial we determined in GO 12923 is yet to be populated in SIAF.dat and flowed down to the ground system. We therefore call out BAR10 and use POS TARGs to move the target to the desired positions behind the BAR5 occulter. He we attempt to place the target on the mid-line of BAR5. We then use a subarray readout of CENTYERAXIS2 = 700 appopriate for BAR5 with a SIZEAXIS2 = 137 (the same ass we use elsewhere for Wedge0.6A). SCALABLE BENCHMARK: We expect full-well at r=0.15" with BAR10 from wings of stellar PSF in 1 second for V=5.0 (A0V) {**to be re-verified**}. HR 4796 is V = 5.78 so saturation in 2.09s. So 90% full well in appx 1.85s. Use this for the BAR5 exposures, repeated (8x) with multiple CR Splits. NOTE TO PC/CS: Here we use the BAR5 occulter (Aperture) that we comissioned in GO program 12923. This aperture is not available in APT Phase 2, *AND* the SIAF locations of the aperture fiducial we determined in GO 12923 is yet to be populated in SIAF.dat and flowed down to the ground system. We therefore call out BAR10 and use POS TARGs to move the target to the desired positions behind the BAR5 occulter. He we attempt to place the target 1/4 pixel above the mid-line of BAR5. We then use a subarray readout of CENTYERAXIS2 = 700 appopriate for BAR5 with a SIZEAXIS2 = 137 (the same ass we use elsewhere for Wedge0.6A). SCALABLE BENCHMARK: We expect full-well at r=0.15" with BAR10 from wings of stellar PSF in 1 second for V=5.0 (A0V) {**to be re-verified**}. HR 4796 is V = 5.78 so saturation in 2.09s. So 90% full well in appx 1.85s. Use this for the BAR5 exposures, repeated (8x) with multiple CR Splits. NOTE TO PC/CS: Here we use the BAR5 occulter (Aperture) that we comissioned in GO program 12923. This aperture is not available in APT Phase 2, *AND* the SIAF locations of the aperture fiducial we determined in GO 12923 is yet to be populated in SIAF.dat and flowed down to the ground system. We therefore call out BAR10 and use POS TARGs to move the target to the desired positions behind the BAR5 occulter. He we attempt to place the target 1/4 pixel below the mid-line of BAR5. We then use a subarray readout of CENTYERAXIS2 = 700 appopriate for BAR5 with a SIZEAXIS2 = 137 (the same ass we use elsewhere for Wedge0.6A). SCALABLE BENCHMARK: We expect full-well at r=0.15" with BAR10 from wings of stellar PSF in 1 second for V=5.0 (A0V) {**to be re-verified**}. HR 4796 is V = 5.78 so saturation in 2.09s. So 90% full well in appx 1.85s. Use this for the BAR5 exposures, repeated (8x) with multiple CR Splits. SCALABLE BENCHMARK: We expect full-well at r=0.3" from wings of stellar PSF in 1 second for V=3.55 (A0V). HR 4796 is V =5.78 so saturation in 7.80s. So 90% full well in appx 7.02s. Use this for the "short" exposures, repeated (8x) with multiple CR Splits. For long exposures at WedgeA1.0 go (up to) 20x deeper in each that will fit into remainer of visibility period CR-SPLIT at least 3 times - and trim exposure time to fit in visibility window. SCALABLE PARAMETER FOR SUB-ARRAY Readout: SIZEAXIS2 = 20 is 1" in full extent (r = 0.5") For these "long" exposures we will image perpendicular to the wedge (symmetrically) centered on the target to the maximum extent permitted by the limits of the FOV (edge of the detector) on the "small" side of the Wedge A taper. Thus, for these short exposures we use SIZEAXIS12 = 427, appropriate for the WedgeA1.0 position. Timing link suitability includes constraints ([03 After 02 by 0.0 to 0.1 days] [04 After 03 by 0.0 to 0.1 days]) The scheduling data was generated by CASM 23.2. CASM was run in Phase II mode. 1452194780233 /private/var/folders/9d/jk8g77fd2jx3sxdb33rhwx48000300/T/OPVisit985388946953026197.xml PSF (HD 85512). PSF calibration target for TW Hya. V = 7.636. B - V = +1.15. Spex. K6Vk This is the PSF star calibrator for the flanking visits (1-4). We levy no orientation constraints on this visit (3). However, we choose this target since it has been used in the past for TW Hya. So as Visits 2 and 3 must be scheduled in sequential contiguous orbits, if scheduled at nominal roll (as we expect also Visit 2 will be) then we expect absolute orientations of Visits 2 and 3 to be very similar (within a few degrees). This is important so we maintain similar Sun and Beta angles for the science target and its PSF calibrator, Relative Timing: This visit (3) should immediately follow visit 2 and immediately precede visit 4. I.e., they should be executed sequentially in "back-to-back" orbits. (Tic-Visit :proposal-id 13753 :visit-id "03" :proposal-version -1 :trans-version "20150609" :date "07-Jan-2016 14:26:20.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 1 :saa-model "24" :si-bright-earth-limb-angle 20.0 :data-volume 218624 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 13753 :visit-id "03" :obset-id "03" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 13753 :visit-id "03" :orbit-number 1 :pcs-time 333 :si-vis-utilization 2706 :al-overhead-at-end 0 :internal-dur-at-end 349 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3114 :pcs-gap 0 ) true 1 0 V = 5.57, sp = B9V, Exptime rounded to nearest 0.1 second ETC Request ID: STIS.ta.618247 NOTE TO PC/CS: Here we use the BAR5 occulter (Aperture) that we comissioned in GO program 12923. This aperture is not available in APT Phase 2, *AND* the SIAF locations of the aperture fiducial we determined in GO 12923 is yet to be populated in SIAF.dat and flowed down to the ground system. We therefore call out BAR10 and use POS TARGs to move the target to the desired positions behind the BAR5 occulter. He we attempt to place the target on the mid-line of BAR5. We then use a subarray readout of CENTYERAXIS2 = 700 appopriate for BAR5 with a SIZEAXIS2 = 137 (the same ass we use elsewhere for Wedge0.6A). SCALABLE BENCHMARK: We expect full-well at r=0.15" with BAR10 from wings of stellar PSF in 1 second for V=5.0 (A0V) {**to be re-verified**}. HR 4735 is V = 5.57 so saturation in 1.69Ss. So 90% full well in appx 1.52s. Use this for the BAR5 exposures, repeated (8x) with multiple CR Splits. NOTE TO PC/CS: Here we use the BAR5 occulter (Aperture) that we comissioned in GO program 12923. This aperture is not available in APT Phase 2, *AND* the SIAF locations of the aperture fiducial we determined in GO 12923 is yet to be populated in SIAF.dat and flowed down to the ground system. We therefore call out BAR10 and use POS TARGs to move the target to the desired positions behind the BAR5 occulter. He we attempt to place the target on 1/4 PIXEL ABOVE the mid-line of BAR5. We then use a subarray readout of CENTYERAXIS2 = 700 appopriate for BAR5 with a SIZEAXIS2 = 137 (the same ass we use elsewhere for Wedge0.6A). SCALABLE BENCHMARK: We expect full-well at r=0.15" with BAR10 from wings of stellar PSF in 1 second for V=5.0 (A0V) {**to be re-verified**}. HR 4735 is V = 5.57 so saturation in 1.69Ss. So 90% full well in appx 1.52s. Use this for the BAR5 exposures, repeated (8x) with multiple CR Splits. NOTE TO PC/CS: Here we use the BAR5 occulter (Aperture) that we comissioned in GO program 12923. This aperture is not available in APT Phase 2, *AND* the SIAF locations of the aperture fiducial we determined in GO 12923 is yet to be populated in SIAF.dat and flowed down to the ground system. We therefore call out BAR10 and use POS TARGs to move the target to the desired positions behind the BAR5 occulter. He we attempt to place the target on 1/4 pixel below the mid-line of BAR5. We then use a subarray readout of CENTYERAXIS2 = 700 appropriate for BAR5 with a SIZEAXIS2 = 137 (the same ass we use elsewhere for Wedge0.6A). SCALABLE BENCHMARK: We expect full-well at r=0.15" with BAR10 from wings of stellar PSF in 1 second for V=5.0 (A0V) {**to be re-verified**}. HR 4735 is V = 5.57 so saturation in 1.69Ss. So 90% full well in appx 1.52s. Use this for the BAR5 exposures, repeated (8x) with multiple CR Splits. SCALABLE BENCHMARK: We expect full-well at r=0.3" from wings of stellar PSF in 1 second for V=3.55 (A0V). HR 4725 is V =5.57 so saturation in 6.43s. So 90% full well in appx 5.78s. Use this for the "short" exposures, repeated (8x) with multiple CR Splits. For long exposures at WedgeA1.0 go (up to) 20x deeper in each that will fit into remainer of visibility period CR-SPLIT at least 3 times - and trim exposure time to fit in visibility window. SCALABLE PARAMETER FOR SUB-ARRAY Readout: SIZEAXIS2 = 20 is 1" in full extent (r = 0.5") For these "long" exposures we will image perpendicular to the wedge (symmetrically) centered on the target to the maximum extent permitted by the limits of the FOV (edge of the detector) on the "small" side of the Wedge A taper. Thus, for these short exposures we use SIZEAXIS12 = 427, appropriate for the WedgeA1.0 position. SCALABLE BENCHMARK: We expect full-well at r=0.3" from wings of stellar PSF in 1 second for V=3.55 (A0V). HR 4725 is V =5.57 so saturation in 6.43s. So 90% full well in appx 5.78s. Use this for the "short" exposures, repeated (8x) with multiple CR Splits. For long exposures at WedgeA1.0 go (up to) 20x deeper in each that will fit into remainer of visibility period CR-SPLIT at least 3 times - and trim exposure time to fit in visibility window. SCALABLE PARAMETER FOR SUB-ARRAY Readout: SIZEAXIS2 = 20 is 1" in full extent (r = 0.5") For these "long" exposures we will image perpendicular to the wedge (symmetrically) centered on the target to the maximum extent permitted by the limits of the FOV (edge of the detector) on the "small" side of the Wedge A taper. Thus, for these short exposures we use SIZEAXIS12 = 427, appropriate for the WedgeA1.0 position. SCALABLE BENCHMARK: We expect full-well at r=0.3" from wings of stellar PSF in 1 second for V=3.55 (A0V). HR 4725 is V =5.57 so saturation in 6.43s. So 90% full well in appx 5.78s. Use this for the "short" exposures, repeated (8x) with multiple CR Splits. For long exposures at WedgeA1.0 go (up to) 20x deeper in each that will fit into remainer of visibility period CR-SPLIT at least 3 times - and trim exposure time to fit in visibility window. SCALABLE PARAMETER FOR SUB-ARRAY Readout: SIZEAXIS2 = 20 is 1" in full extent (r = 0.5") For these "long" exposures we will image perpendicular to the wedge (symmetrically) centered on the target to the maximum extent permitted by the limits of the FOV (edge of the detector) on the "small" side of the Wedge A taper. Thus, for these short exposures we use SIZEAXIS12 = 427, appropriate for the WedgeA1.0 position. Timing link suitability includes constraints ([04 After 03 by 0.0 to 0.1 days]) The scheduling data was generated by CASM 23.2. CASM was run in Phase II mode. 1452194418602 /private/var/folders/9d/jk8g77fd2jx3sxdb33rhwx48000300/T/OPVisit1838085479894363322.xml TW Hya (V=10.8, B-V=1.15) First of two sets of visits, each containing three visits of HR 4796 at different relative orientations with one PSF calibration observation interleaved. This is the third HD 4796 visit in the first set. The four visits within each set must be executed sequentally in contiguous orbits interrupted only for Earth occultation. Orientation: We wish to schedule this visit (4) at +30 deg from Visit 2, with the absolute orientation of Visit 2 unconstrained. We allow a relative orientation tolerence from +15 deg to +30 deg to assist in guide star selection and scheduling. NOTE to PC: Schedule as close to +30 deg from Visit 2 as possible. Relative Timing: This visit (4) should immediately follow Visit 3. I.e., They should be executed sequentially in "back-to-back" orbits. (Tic-Visit :proposal-id 13753 :visit-id "04" :proposal-version -1 :trans-version "20150609" :date "07-Jan-2016 14:20:18.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 1 :saa-model "24" :si-bright-earth-limb-angle 20.0 :data-volume 33696 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 13753 :visit-id "04" :obset-id "04" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 13753 :visit-id "04" :orbit-number 1 :pcs-time 333 :si-vis-utilization 2750 :al-overhead-at-end 0 :internal-dur-at-end 337 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3092 :pcs-gap 0 ) true 1 0 V = 5.78, sp = A0V, Exptime rounded to nearest 0.1 second Taken from Program 8624, where TWHYa had NOTE TO PC/CS: Here we use the BAR5 occulter (Aperture) that we comissioned in GO program 12923. This aperture is not available in APT Phase 2, *AND* the SIAF locations of the aperture fiducial we determined in GO 12923 is yet to be populated in SIAF.dat and flowed down to the ground system. We therefore call out BAR10 and use POS TARGs to move the target to the desired positions behind the BAR5 occulter. He we attempt to place the target on the mid-line of BAR5. We then use a subarray readout of CENTYERAXIS2 = 700 appopriate for BAR5 with a SIZEAXIS2 = 137 (the same ass we use elsewhere for Wedge0.6A). SCALABLE BENCHMARK: We expect full-well at r=0.15" with BAR10 from wings of stellar PSF in 1 second for V=5.0 (A0V) {**to be re-verified**}. HR 4796 is V = 5.78 so saturation in 2.09s. So 90% full well in appx 1.85s. Use this for the BAR5 exposures, repeated (8x) with multiple CR Splits. NOTE TO PC/CS: Here we use the BAR5 occulter (Aperture) that we comissioned in GO program 12923. This aperture is not available in APT Phase 2, *AND* the SIAF locations of the aperture fiducial we determined in GO 12923 is yet to be populated in SIAF.dat and flowed down to the ground system. We therefore call out BAR10 and use POS TARGs to move the target to the desired positions behind the BAR5 occulter. He we attempt to place the target 1/4 pixel above the mid-line of BAR5. We then use a subarray readout of CENTYERAXIS2 = 700 appopriate for BAR5 with a SIZEAXIS2 = 137 (the same ass we use elsewhere for Wedge0.6A). SCALABLE BENCHMARK: We expect full-well at r=0.15" with BAR10 from wings of stellar PSF in 1 second for V=5.0 (A0V) {**to be re-verified**}. HR 4796 is V = 5.78 so saturation in 2.09s. So 90% full well in appx 1.85s. Use this for the BAR5 exposures, repeated (8x) with multiple CR Splits. NOTE TO PC/CS: Here we use the BAR5 occulter (Aperture) that we comissioned in GO program 12923. This aperture is not available in APT Phase 2, *AND* the SIAF locations of the aperture fiducial we determined in GO 12923 is yet to be populated in SIAF.dat and flowed down to the ground system. We therefore call out BAR10 and use POS TARGs to move the target to the desired positions behind the BAR5 occulter. He we attempt to place the target 1/4 pixel below the mid-line of BAR5. We then use a subarray readout of CENTYERAXIS2 = 700 appopriate for BAR5 with a SIZEAXIS2 = 137 (the same ass we use elsewhere for Wedge0.6A). SCALABLE BENCHMARK: We expect full-well at r=0.15" with BAR10 from wings of stellar PSF in 1 second for V=5.0 (A0V) {**to be re-verified**}. HR 4796 is V = 5.78 so saturation in 2.09s. So 90% full well in appx 1.85s. Use this for the BAR5 exposures, repeated (8x) with multiple CR Splits. SCALABLE BENCHMARK: We expect full-well at r=0.3" from wings of stellar PSF in 1 second for V=3.55 (A0V). HR 4796 is V =5.78 so saturation in 7.80s. So 90% full well in appx 7.02s. Use this for the "short" exposures, repeated (8x) with multiple CR Splits. For long exposures at WedgeA1.0 go (up to) 20x deeper in each that will fit into remainer of visibility period CR-SPLIT at least 3 times - and trim exposure time to fit in visibility window. SCALABLE PARAMETER FOR SUB-ARRAY Readout: SIZEAXIS2 = 20 is 1" in full extent (r = 0.5") For these "long" exposures we will image perpendicular to the wedge (symmetrically) centered on the target to the maximum extent permitted by the limits of the FOV (edge of the detector) on the "small" side of the Wedge A taper. Thus, for these short exposures we use SIZEAXIS12 = 427, appropriate for the WedgeA1.0 position. Timing link suitability includes constraints ([06 After 05 by 0.0 to 0.1 days]) The scheduling data was generated by CASM 23.2. CASM was run in Phase II mode. 1452194491158 /private/var/folders/9d/jk8g77fd2jx3sxdb33rhwx48000300/T/OPVisit1709696074882894020.xml TW Hya (V=10.8, B-V=1.15) Second of two sets of visits, each containing three visits of TW Hya at different relative orientations with one PSF calibration observation interleaved. This is the first TW Hya visit in the first set. The four visits within each set must be executed sequentally in contiguous orbits interrupted only for Earth occultation. Orientation: We wish to schedule this visit (5) at -30 deg from Visit 6. We allow a relative orientation tolerence from -15 deg to -30 deg to assist in guide star selection and scheduling. NOTE to PC: Schedule as close to -30 deg from Visit 6 as possible. Relative Timing: This visit (5) should immediately precede visit 6. 1432455575000 94.0 (Tic-Visit :proposal-id 13753 :visit-id "05" :proposal-version -1 :trans-version "20150609" :date "07-Jan-2016 14:21:30.0" :trans-errors '(:WARNINGS 1 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 1 :saa-model "24" :si-bright-earth-limb-angle 20.0 :data-volume 55008 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 13753 :visit-id "05" :obset-id "05" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 13753 :visit-id "05" :orbit-number 1 :pcs-time 333 :si-vis-utilization 2762 :al-overhead-at-end 0 :internal-dur-at-end 359 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3092 :pcs-gap 0 ) true 1 1 V = 5.78, sp = A0V, Exptime rounded to nearest 0.1 second ETC Request ID: STIS.ta.618243 NOTE TO PC/CS: Here we use the BAR5 occulter (Aperture) that we comissioned in GO program 12923. This aperture is not available in APT Phase 2, *AND* the SIAF locations of the aperture fiducial we determined in GO 12923 is yet to be populated in SIAF.dat and flowed down to the ground system. We therefore call out BAR10 and use POS TARGs to move the target to the desired positions behind the BAR5 occulter. He we attempt to place the target on the mid-line of BAR5. We then use a subarray readout of CENTYERAXIS2 = 700 appopriate for BAR5 with a SIZEAXIS2 = 137 (the same ass we use elsewhere for Wedge0.6A). SCALABLE BENCHMARK: We expect full-well at r=0.15" with BAR10 from wings of stellar PSF in 1 second for V=5.0 (A0V) {**to be re-verified**}. HR 4796 is V = 5.78 so saturation in 2.09s. So 90% full well in appx 1.85s. Use this for the BAR5 exposures, repeated (8x) with multiple CR Splits. NOTE TO PC/CS: Here we use the BAR5 occulter (Aperture) that we comissioned in GO program 12923. This aperture is not available in APT Phase 2, *AND* the SIAF locations of the aperture fiducial we determined in GO 12923 is yet to be populated in SIAF.dat and flowed down to the ground system. We therefore call out BAR10 and use POS TARGs to move the target to the desired positions behind the BAR5 occulter. He we attempt to place the target 1/4 pixel above the mid-line of BAR5. We then use a subarray readout of CENTYERAXIS2 = 700 appopriate for BAR5 with a SIZEAXIS2 = 137 (the same ass we use elsewhere for Wedge0.6A). SCALABLE BENCHMARK: We expect full-well at r=0.15" with BAR10 from wings of stellar PSF in 1 second for V=5.0 (A0V) {**to be re-verified**}. HR 4796 is V = 5.78 so saturation in 2.09s. So 90% full well in appx 1.85s. Use this for the BAR5 exposures, repeated (8x) with multiple CR Splits. NOTE TO PC/CS: Here we use the BAR5 occulter (Aperture) that we comissioned in GO program 12923. This aperture is not available in APT Phase 2, *AND* the SIAF locations of the aperture fiducial we determined in GO 12923 is yet to be populated in SIAF.dat and flowed down to the ground system. We therefore call out BAR10 and use POS TARGs to move the target to the desired positions behind the BAR5 occulter. He we attempt to place the target 1/4 pixel below the mid-line of BAR5. We then use a subarray readout of CENTYERAXIS2 = 700 appopriate for BAR5 with a SIZEAXIS2 = 137 (the same ass we use elsewhere for Wedge0.6A). SCALABLE BENCHMARK: We expect full-well at r=0.15" with BAR10 from wings of stellar PSF in 1 second for V=5.0 (A0V) {**to be re-verified**}. HR 4796 is V = 5.78 so saturation in 2.09s. So 90% full well in appx 1.85s. Use this for the BAR5 exposures, repeated (8x) with multiple CR Splits. SCALABLE BENCHMARK: We expect full-well at r=0.3" from wings of stellar PSF in 1 second for V=3.55 (A0V). HR 4796 is V =5.78 so saturation in 7.80s. So 90% full well in appx 7.02s. Use this for the "short" exposures, repeated (8x) with multiple CR Splits. For long exposures at WedgeA1.0 go (up to) 20x deeper in each that will fit into remainer of visibility period CR-SPLIT at least 3 times - and trim exposure time to fit in visibility window. SCALABLE PARAMETER FOR SUB-ARRAY Readout: SIZEAXIS2 = 20 is 1" in full extent (r = 0.5") For these "long" exposures we will image perpendicular to the wedge (symmetrically) centered on the target to the maximum extent permitted by the limits of the FOV (edge of the detector) on the "small" side of the Wedge A taper. Thus, for these short exposures we use SIZEAXIS12 = 427, appropriate for the WedgeA1.0 position. Timing link suitability includes constraints ([06 After 05 by 0.0 to 0.1 days] [07 After 06 by 0.0 to 0.1 days]) The scheduling data was generated by CASM 23.2. CASM was run in Phase II mode. 1452189416862 /private/var/folders/9d/jk8g77fd2jx3sxdb33rhwx48000300/T/OPVisit4655687415735706637.xml TW Hya (V=10.8, B-V=1.15) Second of two sets of visits, each containing three visits of TW Hya at different relative orientations with one PSF calibration observation interleaved. This is the second TW Hya visit in the second set. The four visits within each set must be executed sequentally in contiguous orbits interrupted only for Earth occultation. Relative Orientation: We wish to schedule this visit (6) at EITHER -90 deg OR +90 deg from Visit 2. Either (+ or -) is equally acceptable, but there is no way to specificy this via APT 22.2. Here we specify a range of positive relative orientations of +75 deg to +105 deg to assist in guide star selection and scheduling. NOTE to PC: Schedule as close to +90 deg from Visit 2 as possible. Note to PC: You may freely change the parity of the relative orientation to negative if needed for guide star selection and scheduling. Relative Timing: Schedule in orbit immediately after visit 5 and before visit 7, i.e. they should be back-to-back. 1432461301000 109.0 (Tic-Visit :proposal-id 13753 :visit-id "06" :proposal-version -1 :trans-version "20150609" :date "07-Jan-2016 12:56:56.0" :trans-errors '(:WARNINGS 1 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 1 :saa-model "24" :si-bright-earth-limb-angle 20.0 :data-volume 55008 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 13753 :visit-id "06" :obset-id "06" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 13753 :visit-id "06" :orbit-number 1 :pcs-time 333 :si-vis-utilization 2762 :al-overhead-at-end 0 :internal-dur-at-end 359 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3092 :pcs-gap 0 ) true 1 1 V = 5.78, sp = A0V, Exptime rounded to nearest 0.1 second ETC Request ID: STIS.ta.618243 NOTE TO PC/CS: Here we use the BAR5 occulter (Aperture) that we comissioned in GO program 12923. This aperture is not available in APT Phase 2, *AND* the SIAF locations of the aperture fiducial we determined in GO 12923 is yet to be populated in SIAF.dat and flowed down to the ground system. We therefore call out BAR10 and use POS TARGs to move the target to the desired positions behind the BAR5 occulter. He we attempt to place the target on the mid-line of BAR5. We then use a subarray readout of CENTYERAXIS2 = 700 appopriate for BAR5 with a SIZEAXIS2 = 137 (the same ass we use elsewhere for Wedge0.6A). SCALABLE BENCHMARK: We expect full-well at r=0.15" with BAR10 from wings of stellar PSF in 1 second for V=5.0 (A0V) {**to be re-verified**}. HR 4796 is V = 5.78 so saturation in 2.09s. So 90% full well in appx 1.85s. Use this for the BAR5 exposures, repeated (8x) with multiple CR Splits. NOTE TO PC/CS: Here we use the BAR5 occulter (Aperture) that we comissioned in GO program 12923. This aperture is not available in APT Phase 2, *AND* the SIAF locations of the aperture fiducial we determined in GO 12923 is yet to be populated in SIAF.dat and flowed down to the ground system. We therefore call out BAR10 and use POS TARGs to move the target to the desired positions behind the BAR5 occulter. He we attempt to place the target 1/4 pixel above the mid-line of BAR5. We then use a subarray readout of CENTYERAXIS2 = 700 appopriate for BAR5 with a SIZEAXIS2 = 137 (the same ass we use elsewhere for Wedge0.6A). SCALABLE BENCHMARK: We expect full-well at r=0.15" with BAR10 from wings of stellar PSF in 1 second for V=5.0 (A0V) {**to be re-verified**}. HR 4796 is V = 5.78 so saturation in 2.09s. So 90% full well in appx 1.85s. Use this for the BAR5 exposures, repeated (8x) with multiple CR Splits. NOTE TO PC/CS: Here we use the BAR5 occulter (Aperture) that we comissioned in GO program 12923. This aperture is not available in APT Phase 2, *AND* the SIAF locations of the aperture fiducial we determined in GO 12923 is yet to be populated in SIAF.dat and flowed down to the ground system. We therefore call out BAR10 and use POS TARGs to move the target to the desired positions behind the BAR5 occulter. He we attempt to place the target 1/4 pixel below the mid-line of BAR5. We then use a subarray readout of CENTYERAXIS2 = 700 appopriate for BAR5 with a SIZEAXIS2 = 137 (the same ass we use elsewhere for Wedge0.6A). SCALABLE BENCHMARK: We expect full-well at r=0.15" with BAR10 from wings of stellar PSF in 1 second for V=5.0 (A0V) {**to be re-verified**}. HR 4796 is V = 5.78 so saturation in 2.09s. So 90% full well in appx 1.85s. Use this for the BAR5 exposures, repeated (8x) with multiple CR Splits. SCALABLE BENCHMARK: We expect full-well at r=0.3" from wings of stellar PSF in 1 second for V=3.55 (A0V). HR 4796 is V =5.78 so saturation in 7.80s. So 90% full well in appx 7.02s. Use this for the "short" exposures, repeated (8x) with multiple CR Splits. For long exposures at WedgeA1.0 go (up to) 20x deeper in each that will fit into remainer of visibility period CR-SPLIT at least 3 times - and trim exposure time to fit in visibility window. SCALABLE PARAMETER FOR SUB-ARRAY Readout: SIZEAXIS2 = 20 is 1" in full extent (r = 0.5") For these "long" exposures we will image perpendicular to the wedge (symmetrically) centered on the target to the maximum extent permitted by the limits of the FOV (edge of the detector) on the "small" side of the Wedge A taper. Thus, for these short exposures we use SIZEAXIS12 = 427, appropriate for the WedgeA1.0 position. Timing link suitability includes constraints ([07 After 06 by 0.0 to 0.1 days] [08 After 07 by 0.0 to 0.1 days]) The scheduling data was generated by CASM 23.2. CASM was run in Phase II mode. 1452194221226 /private/var/folders/9d/jk8g77fd2jx3sxdb33rhwx48000300/T/OPVisit2533018298010122713.xml PSF (HD 85512). PSF calibration target for TW Hya. V=7.636 B-V=1.15, Spex K6Vk. This is the PSF star calibrator for the flanking visits (5-8). We levy no orientation constraints on this visit (7). However, we choose this target close in the sky to its paired science target. So as Visits 6 and 7 must be scheduled in sequential contiguous orbits, if scheduled at nominal roll (as we expect also Visit 06 will be) then we expect absolute orientations of Visits 6 and 7 to be very similar (within a few degrees). This is important so we maintain similar Sun and Beta angles for the science target and its PSF calibrator, Relative Timing: This visit (7) should immediately follow visit 6 and immediately precede visit 8. I.e., they should be executed sequentially in "back-to-back" orbits. 1432466871000 108.07499999999999 (Tic-Visit :proposal-id 13753 :visit-id "07" :proposal-version -1 :trans-version "20150609" :date "07-Jan-2016 14:17:00.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 1 :saa-model "24" :si-bright-earth-limb-angle 20.0 :data-volume 223952 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 13753 :visit-id "07" :obset-id "07" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 13753 :visit-id "07" :orbit-number 1 :pcs-time 333 :si-vis-utilization 2694 :al-overhead-at-end 0 :internal-dur-at-end 349 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3114 :pcs-gap 0 ) true 1 0 V = 5.57, sp = B9V, Exptime rounded to nearest 0.1 second ETC Request ID: STIS.ta.618247 NOTE TO PC/CS: Here we use the BAR5 occulter (Aperture) that we comissioned in GO program 12923. This aperture is not available in APT Phase 2, *AND* the SIAF locations of the aperture fiducial we determined in GO 12923 is yet to be populated in SIAF.dat and flowed down to the ground system. We therefore call out BAR10 and use POS TARGs to move the target to the desired positions behind the BAR5 occulter. He we attempt to place the target on the mid-line of BAR5. We then use a subarray readout of CENTYERAXIS2 = 700 appopriate for BAR5 with a SIZEAXIS2 = 137 (the same ass we use elsewhere for Wedge0.6A). SCALABLE BENCHMARK: We expect full-well at r=0.15" with BAR10 from wings of stellar PSF in 1 second for V=5.0 (A0V) {**to be re-verified**}. HR 4735 is V = 5.57 so saturation in 1.69Ss. So 90% full well in appx 1.52s. Use this for the BAR5 exposures, repeated (8x) with multiple CR Splits. NOTE TO PC/CS: Here we use the BAR5 occulter (Aperture) that we comissioned in GO program 12923. This aperture is not available in APT Phase 2, *AND* the SIAF locations of the aperture fiducial we determined in GO 12923 is yet to be populated in SIAF.dat and flowed down to the ground system. We therefore call out BAR10 and use POS TARGs to move the target to the desired positions behind the BAR5 occulter. He we attempt to place the target on 1/4 PIXEL ABOVE the mid-line of BAR5. We then use a subarray readout of CENTYERAXIS2 = 700 appopriate for BAR5 with a SIZEAXIS2 = 137 (the same ass we use elsewhere for Wedge0.6A). SCALABLE BENCHMARK: We expect full-well at r=0.15" with BAR10 from wings of stellar PSF in 1 second for V=5.0 (A0V) {**to be re-verified**}. HR 4735 is V = 5.57 so saturation in 1.69Ss. So 90% full well in appx 1.52s. Use this for the BAR5 exposures, repeated (8x) with multiple CR Splits. NOTE TO PC/CS: Here we use the BAR5 occulter (Aperture) that we comissioned in GO program 12923. This aperture is not available in APT Phase 2, *AND* the SIAF locations of the aperture fiducial we determined in GO 12923 is yet to be populated in SIAF.dat and flowed down to the ground system. We therefore call out BAR10 and use POS TARGs to move the target to the desired positions behind the BAR5 occulter. He we attempt to place the target on 1/4 pixel below the mid-line of BAR5. We then use a subarray readout of CENTYERAXIS2 = 700 appropriate for BAR5 with a SIZEAXIS2 = 137 (the same ass we use elsewhere for Wedge0.6A). SCALABLE BENCHMARK: We expect full-well at r=0.15" with BAR10 from wings of stellar PSF in 1 second for V=5.0 (A0V) {**to be re-verified**}. HR 4735 is V = 5.57 so saturation in 1.69Ss. So 90% full well in appx 1.52s. Use this for the BAR5 exposures, repeated (8x) with multiple CR Splits. SCALABLE BENCHMARK: We expect full-well at r=0.3" from wings of stellar PSF in 1 second for V=3.55 (A0V). HR 4725 is V =5.57 so saturation in 6.43s. So 90% full well in appx 5.78s. Use this for the "short" exposures, repeated (8x) with multiple CR Splits. For long exposures at WedgeA1.0 go (up to) 20x deeper in each that will fit into remainer of visibility period CR-SPLIT at least 3 times - and trim exposure time to fit in visibility window. SCALABLE PARAMETER FOR SUB-ARRAY Readout: SIZEAXIS2 = 20 is 1" in full extent (r = 0.5") For these "long" exposures we will image perpendicular to the wedge (symmetrically) centered on the target to the maximum extent permitted by the limits of the FOV (edge of the detector) on the "small" side of the Wedge A taper. Thus, for these short exposures we use SIZEAXIS12 = 427, appropriate for the WedgeA1.0 position. SCALABLE BENCHMARK: We expect full-well at r=0.3" from wings of stellar PSF in 1 second for V=3.55 (A0V). HR 4725 is V =5.57 so saturation in 6.43s. So 90% full well in appx 5.78s. Use this for the "short" exposures, repeated (8x) with multiple CR Splits. For long exposures at WedgeA1.0 go (up to) 20x deeper in each that will fit into remainer of visibility period CR-SPLIT at least 3 times - and trim exposure time to fit in visibility window. SCALABLE PARAMETER FOR SUB-ARRAY Readout: SIZEAXIS2 = 20 is 1" in full extent (r = 0.5") For these "long" exposures we will image perpendicular to the wedge (symmetrically) centered on the target to the maximum extent permitted by the limits of the FOV (edge of the detector) on the "small" side of the Wedge A taper. Thus, for these short exposures we use SIZEAXIS12 = 427, appropriate for the WedgeA1.0 position. SCALABLE BENCHMARK: We expect full-well at r=0.3" from wings of stellar PSF in 1 second for V=3.55 (A0V). HR 4725 is V =5.57 so saturation in 6.43s. So 90% full well in appx 5.78s. Use this for the "short" exposures, repeated (8x) with multiple CR Splits. For long exposures at WedgeA1.0 go (up to) 20x deeper in each that will fit into remainer of visibility period CR-SPLIT at least 3 times - and trim exposure time to fit in visibility window. SCALABLE PARAMETER FOR SUB-ARRAY Readout: SIZEAXIS2 = 20 is 1" in full extent (r = 0.5") For these "long" exposures we will image perpendicular to the wedge (symmetrically) centered on the target to the maximum extent permitted by the limits of the FOV (edge of the detector) on the "small" side of the Wedge A taper. Thus, for these short exposures we use SIZEAXIS12 = 427, appropriate for the WedgeA1.0 position. Timing link suitability includes constraints ([08 After 07 by 0.0 to 0.1 days]) The scheduling data was generated by CASM 23.2. CASM was run in Phase II mode. 1452194492980 /private/var/folders/9d/jk8g77fd2jx3sxdb33rhwx48000300/T/OPVisit1664470042322059269.xml TW Hya (V=10.8, B-v=1.15) FSecond of two sets of visits, each containing three visits of TW Hya at different relative orientations with one PSF calibration observation interleaved. This is the third TW Hya visit in the first set. The four visits within each set must be executed sequentally in contiguous orbits interrupted only for Earth occultation. Orientation: We wish to schedule this visit (8) at +30 deg from Visit 06. We allow a relative orientation tolerence from +15 deg to +30 deg to assist in guide star selection and scheduling. NOTE to PC: Schedule as close to +30 deg from Visit 6 as possible. Relative Timing: This visit (8) should immediately follow Visit 7. I.e., They should be executed sequentially in "back-to-back" orbits. 1432472753000 124.0 (Tic-Visit :proposal-id 13753 :visit-id "08" :proposal-version -1 :trans-version "20150609" :date "07-Jan-2016 14:21:32.0" :trans-errors '(:WARNINGS 1 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 1 :saa-model "24" :si-bright-earth-limb-angle 20.0 :data-volume 55008 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 13753 :visit-id "08" :obset-id "08" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 13753 :visit-id "08" :orbit-number 1 :pcs-time 333 :si-vis-utilization 2762 :al-overhead-at-end 0 :internal-dur-at-end 359 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3092 :pcs-gap 0 ) true 1 1 V = 5.78, sp = A0V, Exptime rounded to nearest 0.1 second ETC Request ID: STIS.ta.618243 NOTE TO PC/CS: Here we use the BAR5 occulter (Aperture) that we comissioned in GO program 12923. This aperture is not available in APT Phase 2, *AND* the SIAF locations of the aperture fiducial we determined in GO 12923 is yet to be populated in SIAF.dat and flowed down to the ground system. We therefore call out BAR10 and use POS TARGs to move the target to the desired positions behind the BAR5 occulter. He we attempt to place the target on the mid-line of BAR5. We then use a subarray readout of CENTYERAXIS2 = 700 appopriate for BAR5 with a SIZEAXIS2 = 137 (the same ass we use elsewhere for Wedge0.6A). SCALABLE BENCHMARK: We expect full-well at r=0.15" with BAR10 from wings of stellar PSF in 1 second for V=5.0 (A0V) {**to be re-verified**}. HR 4796 is V = 5.78 so saturation in 2.09s. So 90% full well in appx 1.85s. Use this for the BAR5 exposures, repeated (8x) with multiple CR Splits. NOTE TO PC/CS: Here we use the BAR5 occulter (Aperture) that we comissioned in GO program 12923. This aperture is not available in APT Phase 2, *AND* the SIAF locations of the aperture fiducial we determined in GO 12923 is yet to be populated in SIAF.dat and flowed down to the ground system. We therefore call out BAR10 and use POS TARGs to move the target to the desired positions behind the BAR5 occulter. He we attempt to place the target 1/4 pixel above the mid-line of BAR5. We then use a subarray readout of CENTYERAXIS2 = 700 appopriate for BAR5 with a SIZEAXIS2 = 137 (the same ass we use elsewhere for Wedge0.6A). SCALABLE BENCHMARK: We expect full-well at r=0.15" with BAR10 from wings of stellar PSF in 1 second for V=5.0 (A0V) {**to be re-verified**}. HR 4796 is V = 5.78 so saturation in 2.09s. So 90% full well in appx 1.85s. Use this for the BAR5 exposures, repeated (8x) with multiple CR Splits. NOTE TO PC/CS: Here we use the BAR5 occulter (Aperture) that we comissioned in GO program 12923. This aperture is not available in APT Phase 2, *AND* the SIAF locations of the aperture fiducial we determined in GO 12923 is yet to be populated in SIAF.dat and flowed down to the ground system. We therefore call out BAR10 and use POS TARGs to move the target to the desired positions behind the BAR5 occulter. He we attempt to place the target 1/4 pixel below the mid-line of BAR5. We then use a subarray readout of CENTYERAXIS2 = 700 appopriate for BAR5 with a SIZEAXIS2 = 137 (the same ass we use elsewhere for Wedge0.6A). SCALABLE BENCHMARK: We expect full-well at r=0.15" with BAR10 from wings of stellar PSF in 1 second for V=5.0 (A0V) {**to be re-verified**}. HR 4796 is V = 5.78 so saturation in 2.09s. So 90% full well in appx 1.85s. Use this for the BAR5 exposures, repeated (8x) with multiple CR Splits. SCALABLE BENCHMARK: We expect full-well at r=0.3" from wings of stellar PSF in 1 second for V=3.55 (A0V). HR 4796 is V =5.78 so saturation in 7.80s. So 90% full well in appx 7.02s. Use this for the "short" exposures, repeated (8x) with multiple CR Splits. For long exposures at WedgeA1.0 go (up to) 20x deeper in each that will fit into remainer of visibility period CR-SPLIT at least 3 times - and trim exposure time to fit in visibility window. SCALABLE PARAMETER FOR SUB-ARRAY Readout: SIZEAXIS2 = 20 is 1" in full extent (r = 0.5") For these "long" exposures we will image perpendicular to the wedge (symmetrically) centered on the target to the maximum extent permitted by the limits of the FOV (edge of the detector) on the "small" side of the Wedge A taper. Thus, for these short exposures we use SIZEAXIS12 = 427, appropriate for the WedgeA1.0 position.