15438( 4) - 17-May-2018 19:45:07 - [ 1] HUBBLE SPACE TELESCOPE OBSERVING PROGRAM 15438 Version: 4 Check-in Time: 17-May-2018 19:45:07 STScI Edit Number: 0 Title Gamma-ray Quiet Novae: What Sets the Gamma-Ray Luminosity of Novae? ------------------------------------------------------------------------------------ Type Cycle GO 25 ------------------------------------------------------------------------------------ Investigators Contact? PI: Dr. Jennifer L Sokoloski Columbia University in the City of New Y York CoI: Dr. Laura Chomiuk Michigan State University N CoI: Dr. Thomas Nelson University of Pittsburgh N CoI: Dr. Koji Mukai NASA Goddard Space Flight Center N CoI: Dr. Justin D. Linford George Washington University N CoI: Dr. Michael Rupen Dominion Astrophysical Observatory N CoI: Dr. Amy Mioduszewski Associated Universities, Inc. N CoI: Dr. Jennifer Helen Seng Weston AAAS Fellowship Programs, Inc. N CoI: Dr. Stephen S. Lawrence Hofstra University N ------------------------------------------------------------------------------------ Abstract One of the most astounding discoveries in nova research has been the recent finding that many classical novae emit detectable levels of GeV gamma-rays. How do they do it? The correct answer to this question must also explain why some novae are intrinsically gamma-ray quiet. The goal of this proposal is to identify the differences between gamma-ray quiet and gamma-ray bright novae that explain their discrepant gamma-ray luminosities. We request 12.5 hours of JVLA time to spatially resolve and briefly monitor two carefully selected gamma-quiet classical novae--- V5667 Sgr and V2659 Cyg. We also request 3 orbits of HST imaging and spectroscopy to capture the full remnantand kinematics of V5667 Sgr. These observations will test the hypothesis that gamma-ray production in novae requires collisions between: 1) a slow, dense equatorial flow; and 2) a powerful, isotropic fast wind. This research is timely, requires the JVLA, and has implications for the physics of a wide variety of eruptive transients. ------------------------------------------------------------------------------------ Observations Description ------------------------ This project is a coordinated campaign to use the highest-resolutions in both VLA interferometry and HST direct and spectral imaging to study the expanding thermal ejecta of recent classical novae that were NOT detected in gamma-ray emission. The goal of this proposal is to identify the differences between gamma-ray quiet and gamma-ray bright novae that explain their discrepant gamma-ray luminosities. We have been awarded 12.5 hours of JVLA A-configuration time to spatially resolve and monitor two carefully selected gamma-quiet classical novae--- V5667 Sgr and V2659 Cyg. We have also been awarded 3 orbits of HST time to observe V5667 Sgr. We will use WFC3 to obtain narrow-band [OIII] and Halpha+[NII] images, with the F502N and F657N filters respectively, of the young remnant around gamma-ray faint nova V5667 Sgr. The WFC3-UVIS-DITHER-BOX patter will be used to take dithered images in each filter so that we can remove cosmic-ray and CCD 15438( 4) - 17-May-2018 19:45:07 - [ 2] artifacts as well as drizzle the images to improved spatial resolution of at least 0.03"/pixel. We will also use STIS, with the G430L grating, to obtain a spatially resolved spectrum. For the STIS observation, we will use a 4-point STIS-ALONG-SLIT dither pattern with CR-SPLIT=2 readouts at each dither point. Including one such exposure pattern in each spectroscopic orbit allows us to build up a total of approximately 3600 seconds of spectral exposure in approximately 400 second sub-exposures. We have found that the large number of STIS sub-exposures are necessary and minimally sufficient to reliably filter the large number of bad pixels found on the STIS detector. The goal of the WFC3 imaging is to detect, or place meaningful contraints on, emission from substracture within the remnant, for comparison with radio and HST images of gamma-ray-bright novae. The goal of the STIS specroscopy is to provide 3-D kinematics of the V5667 Sgr remnant in [O III] and H-beta, as well as evidence for resolved structure in high-ionization-state lines such as [NeV] and [FeVII] that tend to trace shocks. We will use both imaging and spectroscopy to obtain expansion parallax distance estimates to V5667 Sgr. ------------------------------------------------------------------------------------ 15438( 4) - 17-May-2018 19:45:07 - [ 3] TARGET LIST Fixed Targets ------------------------------------------------------------------------------------------------------------------------------------ Tar| Target | Target | Target |Coord | Radial | Flux data No | Name | Description | Position |Eqnx | Vel. | ------------------------------------------------------------------------------------------------------------------------------------ 1 NOVA-SGR-201 EXT-STAR, CLASSICAL RA=18H14M25.1590S +/- 0.001", J2000 V = 14.0 +/- 0.5 5-A NOVA, EJECTA, EMISSION DEC=-25D54'34.58" +/- 0.001" LINE NEBULA, SHELL Reference Frame: ICRS Extended: YES Comments: V-band flux from an AAVSO CCD measurement on 2017/06/25. At average, fairly linear fading rate in V from October 2015 to June 2017, it should fade by roughly 0.5 magnitudes more in the coming year, through June 2018. Epoch of Position RA proper motion (seconds of time/yr) DEC Proper Motion (arcsec/yr) Annual Parallax (arcsec) 2016.93 0.0 0.0 0.0 ------------------------------------------------------------------------------------------------------------------------------------ 15438( 4) - 17-May-2018 19:45:07 - [ 4] Patterns ------------------------------------------------------------------------------------------------------------------------------------ Pattern_Number: 1 Primary_Pattern Secondary_Pattern Pattern_Type WFC3-UVIS-DITHER-BOX Pattern_Purpose DITHER Number_Of_Points 4 Point_Spacing 0.519 Line_Spacing 0.336 Coordinate_Frame POS-TARG Pattern_Orient 23.884 Angle_Between_Sides 81.785 Center_Pattern NO Pattern_Comments: Standard WFC3-UVIS-DITHER-BOX pattern scaled up 3.0x in size to dither short exposures for cosmic ray & bad pixels, and to move potentially saturated/bled central pixels with larger column separations ------------------------------------------------------------------------------------------------------------------------------------ Pattern_Number: 3 Primary_Pattern Secondary_Pattern Pattern_Type STIS-ALONG-SLIT Pattern_Purpose DITHER Number_Of_Points 4 Point_Spacing 0.5332 Line_Spacing Coordinate_Frame POS-TARG Pattern_Orient 90.0 Angle_Between_Sides Center_Pattern YES Pattern_Comments: STIS spectroscopic dither pattern of four pointings spaced 10.5 pixels apart (with CRSPLIT=2 at each pointing) to provide 8 exposures with which to remove cosmic rays and CCD artifacts, and to be drizzled to improve spatial resolution. ------------------------------------------------------------------------------------------------------------------------------------ Pattern_Number: 5 Primary_Pattern Secondary_Pattern Pattern_Type WFC3-UVIS-DITHER-LINE-3PT Pattern_Purpose DITHER Number_Of_Points 3 Point_Spacing 0.135 Line_Spacing Coordinate_Frame POS-TARG Pattern_Orient 46.84 Angle_Between_Sides Center_Pattern NO Pattern_Comments: Standard WFC3-UVIS-DITHER-LINE-3PT pattern to dither shortest WFC3 exposures for cosmic ray & bad pixels, and to move potentially saturated/bled central pixels to new colums. ------------------------------------------------------------------------------------------------------------------------------------ 15438( 4) - 17-May-2018 19:45:07 - [ 5] Visit: 01 (Visit 01: 1 orbit of WFC3 imaging on V5668 Sgr) Visit Requirements: SCHED 100% On Hold Comments: Additional Comments: The purpose of Visit 01 is to take WFC3 images of the expanding remnant of Nova Sgr 2105-A = V5667 Sgr, to pair with our awarded VLA A-configuration radio interfermetry (March through June 2018). The inherent schedulability of targets in Sagittarius naturally restricts Visit 01 to be relatively contemporaneous with the JVLA A-configuration observations. This visit should be scheduled before the STIS spectroscopic Visit 02, in order to provide contemporaneous spatial intensity mapping with the spectra, yet also to provide preview imaging to select a major axis for optimal slit orientation for the STIS spectra in Visit 02 to follow. This imaging visit is for one orbit, for a total of ~640 seconds in F502N ( [O III] ) and ~640 seconds in F657N ( Halpha+[N II] ). One science goal is to use WFC3 image expansion proper motion and STIS spectra to determine an expansion parallax distance to V5667 Sgr. There is a slight chance it will still be an unresolved point source in the WFC3 imaging. Hence the series of very short, yet well-dithered exposures to insure against saturation and yet provide a good test of a partially-resolved PSF. The longer exposures are to search for faint nebulosity out to 0.5 arcsec (at the expected size/surface brightness). Exposure times estimated from the ETC and by scaling our past F502N and F657N images of V339 Del and V959 Mon up to the anticipated maximum brightness of V5667 Sgr in early-2018. If newer ground-based photometry or spectra indicate dramatic or unexpected changes, we may request an adjustment of exposure times within this orbit. Flash levels are set using the minimum ETC recommendation that did not trigger a warning flag. Exposures ------------------------------------------------------------------------------------------------------------------------------------ Exp | Target | Instr | Oper. | Aper |Spectral|Central| Optional |Num| Time | Special Num | Name | Config | Mode | or FOV |Element |Waveln.| Parameters |Exp| (Total) | Requirements ------------------------------------------------------------------------------------------------------------------------------------ 1 NOVA-SGR-20 WFC3/UVI ACCUM UVIS2-C1K F502N FLASH=12, BLADE=A 1 5.0 S (15 PATTERN 5 1 15-A S 1C-SUB S) Comments: Post-flash = 12 e- based on ETC WFC3UVIS.im.1038861 We use a single iteration of the 3-point WFC3-UVIS-DITHER-LINE-3PT with short 5.0 sec integrations at each point to provide insurance against saturation. Conservatively, 1) if the nova is an unresolved point source, and 2) if the V=14.0 flux levels detected by AASVSO observers is entirely [O III] 4959, 5007 line emission, then 5 second exposures should not saturate, based on calculations using on ETC WFC3UVIS.im.1038856, WFC3UVIS.im.1038858 & WFC3UVIS.im.1038861. ------------------------------------------------------------------------------------------------------------------------------------ 15438( 4) - 17-May-2018 19:45:07 - [ 6] Exposures ------------------------------------------------------------------------------------------------------------------------------------ Exp | Target | Instr | Oper. | Aper |Spectral|Central| Optional |Num| Time | Special Num | Name | Config | Mode | or FOV |Element |Waveln.| Parameters |Exp| (Total) | Requirements ------------------------------------------------------------------------------------------------------------------------------------ 2 NOVA-SGR-20 WFC3/UVI ACCUM UVIS2-C1K F502N FLASH=12 1 160.0 S PATTERN 1 2 15-A S 1C-SUB (640 S) Comments: Post-flash = 12 e- based on WFC3UVIS.im.1040153 We use a single iteration of the 4-point WFC3-UVIS-DITHER-BOX with 3x expanded throws with 160 second subexposures: at V=14.0 these should not saturate the brightest few pixels of central point source in F502N; but if it does the larger dither pattern will help keep saturated and bloomed pixels/columns separated. Estimates based on the ETC WFC3UVIS.im.1040153 and on scaling our previous images of V959 Mon and T Pyx. ------------------------------------------------------------------------------------------------------------------------------------ 3 NOVA-SGR-20 WFC3/UVI ACCUM UVIS2-C1K F657N FLASH=12, BLADE=A 1 5.0 S (15 PATTERN 5 3 15-A S 1C-SUB S) Comments: Post-flash = 12 e- based on WFC3UVIS.im.1040161 We use a single iteration of the 3-point WFC3-UVIS-DITHER-LINE-3PT with short 5.0 sec integrations at each point to provide insurance against saturation. Scaling from [O III] to H-alpha using previous HST spectra of young nova remanants, these 5 second exposures should not saturate, based on calculations using on ETC WFC3UVIS.im.1040161 and exposures used on V339 Del and V5668 Sgr. ------------------------------------------------------------------------------------------------------------------------------------ 4 NOVA-SGR-20 WFC3/UVI ACCUM UVIS2-C1K F657N FLASH=12 1 160.0 S PATTERN 1 4 15-A S 1C-SUB (640 S) Comments: Post-flash = 12 e- based on WFC3UVIS.im.1040156 We use a single iteration of the 4-point WFC3-UVIS-DITHER-BOX with 3x expanded throws with 160 second subexposures. Scaling from [O III] to H-alpha using previous HST spectra of young nova remanants, these exposures are unlikely to saturate at the central point source in F657N; but if it does the larger dither pattern will help keep saturated and bloomed pixels/columns separated. Estimates based on the ETC WFC3UVIS.im.1040156 and on scaling our previous images of V339 Del and V5668 Sgr. ------------------------------------------------------------------------------------------------------------------------------------ 15438( 4) - 17-May-2018 19:45:07 - [ 7] Sub Exposures ------------------------------------------------------------------------------------------------------------------------------------ Target | Exp |Instr | Oper. | Aper |Spectral|Cent.|Primary |Secondary |Iteration |CR-SPLIT |Orbit |Duration Name | Num |Config | Mode | or FOV |Element |Wave.|Pattern Pos |Pattern Pos |Num |Num |Number | ------------------------------------------------------------------------------------------------------------------------------------ Sub Exposures ------------------------------------------------------------------------------------------------------------------------------------ Target | Exp |Instr | Oper. | Aper |Spectral|Cent.|Primary |Secondary |Iteration |CR-SPLIT |Orbit |Duration Name | Num |Config | Mode | or FOV |Element |Wave.|Pattern Pos |Pattern Pos |Num |Num |Number | ------------------------------------------------------------------------------------------------------------------------------------ NOVA-SGR-2015-A 1 WFC3/UVI ACCUM UVIS2-C1 F502N 1 none none none 1 N/A S K1C-SUB NOVA-SGR-2015-A 1 WFC3/UVI ACCUM UVIS2-C1 F502N 2 none none none 1 N/A S K1C-SUB NOVA-SGR-2015-A 1 WFC3/UVI ACCUM UVIS2-C1 F502N 3 none none none 1 N/A S K1C-SUB NOVA-SGR-2015-A 2 WFC3/UVI ACCUM UVIS2-C1 F502N 1 none none none 1 N/A S K1C-SUB NOVA-SGR-2015-A 2 WFC3/UVI ACCUM UVIS2-C1 F502N 2 none none none 1 N/A S K1C-SUB NOVA-SGR-2015-A 2 WFC3/UVI ACCUM UVIS2-C1 F502N 3 none none none 1 N/A S K1C-SUB NOVA-SGR-2015-A 2 WFC3/UVI ACCUM UVIS2-C1 F502N 4 none none none 1 N/A S K1C-SUB NOVA-SGR-2015-A 3 WFC3/UVI ACCUM UVIS2-C1 F657N 1 none none none 1 N/A S K1C-SUB NOVA-SGR-2015-A 3 WFC3/UVI ACCUM UVIS2-C1 F657N 2 none none none 1 N/A S K1C-SUB NOVA-SGR-2015-A 3 WFC3/UVI ACCUM UVIS2-C1 F657N 3 none none none 1 N/A S K1C-SUB NOVA-SGR-2015-A 4 WFC3/UVI ACCUM UVIS2-C1 F657N 1 none none none 1 N/A S K1C-SUB NOVA-SGR-2015-A 4 WFC3/UVI ACCUM UVIS2-C1 F657N 2 none none none 1 N/A S K1C-SUB NOVA-SGR-2015-A 4 WFC3/UVI ACCUM UVIS2-C1 F657N 3 none none none 1 N/A S K1C-SUB NOVA-SGR-2015-A 4 WFC3/UVI ACCUM UVIS2-C1 F657N 4 none none none 1 N/A S K1C-SUB 15438( 4) - 17-May-2018 19:45:07 - [ 8] Visit: 02 (Visit 02: 2 orbits of STIS CCD G430L spectra on V5667 Sgr) Visit Requirements: SCHED 100%; ORIENT 110D TO 130 D; ORIENT 290D TO 310 D; AFTER 01 BY 60.0 D TO 550.0 D On Hold Comments: Additional Comments: The purpose of Visit 02 is to use 2 orbits to take STIS CCD G430L spectra of the expanding and fading remnant of Nova Sgr 2015-A = V5667 Sgr, after the remnant has been imaged by the WFC3 imaging Visit 01. The inherent schedulability of targets in Sagittarius naturally restricts Visit 01 to be relatively contemporaneous with JVLA A-configuration observations of V5667 Sgr (to be taken March through June 2018). Ideally, we would like to use the WFC3 imaging from Visit 01 to identify a major axis in the remnant to use as an optimal slit PA for the STIS spectra in Visit 02. But we are also accutely aware of the tight scheduling constraints in Cycle 25. As the determination of this broad roll angle range and scheduling window will need to wait until the Visit 01 WFC3 imaging is taken and then quickly analyzed, our current request for this visit to follow Visit 01 by at least 30 days, but not more than 550 days (1.5 years). While a specific PA to match the major axis is preferrable, we will provide up to +/-20 degrees of slop in our follow up request. The 550 day window and 40-degree roll range of should give plenty of scheduling opportunities, but if it does not, we are certainly willing to drop the PA requirement and take spectra at any arbitrary angle. This spectroscopic visit is for a total of two orbits, for a total of ~1440+2160=3600 seconds in STIS CCD G430L. If new ground-based photometry or spectra indicate dramatic or unexpected changes in brightness, we may request an adjustment of exposure times within this orbit. Exposures ------------------------------------------------------------------------------------------------------------------------------------ Exp | Target | Instr | Oper. | Aper |Spectral|Central| Optional |Num| Time | Special Num | Name | Config | Mode | or FOV |Element |Waveln.| Parameters |Exp| (Total) | Requirements ------------------------------------------------------------------------------------------------------------------------------------ 1 NOVA-SGR-20 STIS/CCD ACQ 50CCD MIRROR ACQTYPE=DIFFUSE, CHECKBOX=5, 1 3 S (3 S) 15-A DIFFUSE-CENTER=FLUX-CENTROID Comments: Acquistion imaging for V5667 Sgr, which we expect to be a faint point source surrounded by small-scale (<0.5 arcsec) bright nebular structures of higher intensity. The most current AAVSO CCD photometry of V5667 Sgr has it at V=14.0, likely dominated by the [O III] 4959, 5007 lines. An exposure time of 3 seconds should be below saturation, even assuming the worst case scenario of all 14.0 magnitudes of flux being concentrated in an unresolved point source and due entirely to the [O III] line source. Even if the ACQ exposure mildly saturates, we are using the 52x2 slit, so a small aperture centering error is not critical. Additionally, We will be able to use the WFC3 imaging from the preceding Visit 01 to determine whether the 3-second ACQ and ACQ-PEAK will be suitable, or if it needs to be shortened or lengthened, or if an OFFSET from a nearby star will be needed. ------------------------------------------------------------------------------------------------------------------------------------ 15438( 4) - 17-May-2018 19:45:07 - [ 9] Exposures ------------------------------------------------------------------------------------------------------------------------------------ Exp | Target | Instr | Oper. | Aper |Spectral|Central| Optional |Num| Time | Special Num | Name | Config | Mode | or FOV |Element |Waveln.| Parameters |Exp| (Total) | Requirements ------------------------------------------------------------------------------------------------------------------------------------ 2 NOVA-SGR-20 STIS/CCD ACQ/PEA 52X0.1E1 MIRROR 1 3 S (3 S) 15-A K Comments: Peak-up imaging for V5667 Sgr, which we expect to be a faint point source surrounded by small-scale (<0.5 arcsec) bright nebular structures of higher intensity. The most current AAVSO CCD photometry of V5667 Sgr has it at V=14.0, likely dominated by the [O III] 4959, 5007 lines. An exposure time of 3 seconds should be below saturation, even assuming the worst case scenario of all 14.0 magnitudes of flux being concentrated in an unresolved point source and due entirely to the [O III] line source. Even if the ACQ-PEAK exposure mildly saturates, we are using the 52x2 slit, so a small aperture centering error is not critical. Additionally, we will be able to use the WFC3 imaging from the preceding Visit 01 to determine whether this 3-second ACQ and ACQ-PEAK will be suitable, or if it needs to be shortened or lengthened, or if an OFFSET from a nearby star will be needed. ------------------------------------------------------------------------------------------------------------------------------------ 3 NOVA-SGR-20 STIS/CCD ACCUM 52X2E1 G430L 4300 CR-SPLIT=2 1 360 S PATTERN 3 3 15-A (1440 S) Comments: We use a CR-SPLIT=2 at each of the 4-points of a centered STIS-ALONG-SLIT dither pattern with 0.5332 arcsec = 10.5 pixel steps, here with 300 second subexposures. In combination with the multiple orbits, the half-integer pixel step size will allow us to flag and remove cosmic rays, bad pixels and likely increase the STIS spatial resolution. Exposure estimates based on the ETC and on scaling our previous spectra of V339 Del and V959 Mon. ------------------------------------------------------------------------------------------------------------------------------------ 15438( 4) - 17-May-2018 19:45:07 - [ 10] Exposures ------------------------------------------------------------------------------------------------------------------------------------ Exp | Target | Instr | Oper. | Aper |Spectral|Central| Optional |Num| Time | Special Num | Name | Config | Mode | or FOV |Element |Waveln.| Parameters |Exp| (Total) | Requirements ------------------------------------------------------------------------------------------------------------------------------------ 4 NOVA-SGR-20 STIS/CCD ACCUM 52X2E1 G430L 4300 CR-SPLIT=2 1 540 S PATTERN 3 4 15-A (2160 S) Comments: We use a CR-SPLIT=2 at each of the 4-points of a centered STIS-ALONG-SLIT dither pattern with 0.5332 arcsec = 10.5 pixel steps, here with 500 second subexposures. In combination with the multiple orbits, the half-integer pixel step size will allow us to flag and remove cosmic rays, bad pixels and likely increase the STIS spatial resolution. Exposure estimates based on the ETC and on scaling our previous spectra of V339 Del and V959 Mon. ------------------------------------------------------------------------------------------------------------------------------------ Sub Exposures ------------------------------------------------------------------------------------------------------------------------------------ Target | Exp |Instr | Oper. | Aper |Spectral|Cent.|Primary |Secondary |Iteration |CR-SPLIT |Orbit |Duration Name | Num |Config | Mode | or FOV |Element |Wave.|Pattern Pos |Pattern Pos |Num |Num |Number | ------------------------------------------------------------------------------------------------------------------------------------ NOVA-SGR-2015-A 1 STIS/CCD ACQ 50CCD MIRROR none none none none 1 N/A NOVA-SGR-2015-A 2 STIS/CCD ACQ/PEA 52X0.1E1 MIRROR none none none none 1 N/A K NOVA-SGR-2015-A 3 STIS/CCD ACCUM 52X2E1 G430L 4300 1 none none 1 1 N/A NOVA-SGR-2015-A 3 STIS/CCD ACCUM 52X2E1 G430L 4300 1 none none 2 1 N/A NOVA-SGR-2015-A 3 STIS/CCD ACCUM 52X2E1 G430L 4300 2 none none 1 1 N/A NOVA-SGR-2015-A 3 STIS/CCD ACCUM 52X2E1 G430L 4300 2 none none 2 1 N/A NOVA-SGR-2015-A 3 STIS/CCD ACCUM 52X2E1 G430L 4300 3 none none 1 1 N/A NOVA-SGR-2015-A 3 STIS/CCD ACCUM 52X2E1 G430L 4300 3 none none 2 1 N/A NOVA-SGR-2015-A 3 STIS/CCD ACCUM 52X2E1 G430L 4300 4 none none 1 1 N/A NOVA-SGR-2015-A 3 STIS/CCD ACCUM 52X2E1 G430L 4300 4 none none 2 1 N/A NOVA-SGR-2015-A 4 STIS/CCD ACCUM 52X2E1 G430L 4300 1 none none 1 2 N/A NOVA-SGR-2015-A 4 STIS/CCD ACCUM 52X2E1 G430L 4300 1 none none 2 2 N/A NOVA-SGR-2015-A 4 STIS/CCD ACCUM 52X2E1 G430L 4300 2 none none 1 2 N/A NOVA-SGR-2015-A 4 STIS/CCD ACCUM 52X2E1 G430L 4300 2 none none 2 2 N/A NOVA-SGR-2015-A 4 STIS/CCD ACCUM 52X2E1 G430L 4300 3 none none 1 2 N/A NOVA-SGR-2015-A 4 STIS/CCD ACCUM 52X2E1 G430L 4300 3 none none 2 2 N/A NOVA-SGR-2015-A 4 STIS/CCD ACCUM 52X2E1 G430L 4300 4 none none 1 2 N/A NOVA-SGR-2015-A 4 STIS/CCD ACCUM 52X2E1 G430L 4300 4 none none 2 2 N/A 15438( 4) - 17-May-2018 19:45:07 - [ 11] Summary Form for Proposal 15438 Item Used in this proposal ------------------------------------------------------------------------------------------------------------------------------------ Apertures 50CCD, 52X0.1E1, 52X2E1, UVIS2-C1K1C-SUB ------------------------------------------------------------------------------------------------------------------------------------ Configurations STIS/CCD, WFC3/UVIS ------------------------------------------------------------------------------------------------------------------------------------ Opmodes ACCUM, ACQ, ACQ/PEAK ------------------------------------------------------------------------------------------------------------------------------------ Optional Parameters ACQTYPE=DIFFUSE, BLADE=A, CHECKBOX=5, CR-SPLIT=2, DIFFUSE-CENTER=FLUX-CENTROID, FLASH=12 ------------------------------------------------------------------------------------------------------------------------------------ Special Requirements AFTER 01 BY 60.0 D TO 550.0 D, ORIENT 110D TO 130 D, ORIENT 290D TO 310 D, PATTERN 1 2, PATTERN 1 4, PATTERN 3 3, PATTERN 3 4, PATTERN 5 1, PATTERN 5 3, SCHED 100% ------------------------------------------------------------------------------------------------------------------------------------ Spectral Elements F502N, F657N, G430L, MIRROR ------------------------------------------------------------------------------------------------------------------------------------ Target Names NOVA-SGR-2015-A ------------------------------------------------------------------------------------------------------------------------------------