14787( 10) - 26-May-2017 18:58:06 - [ 1] HUBBLE SPACE TELESCOPE OBSERVING PROGRAM 14787 Version: 10 Check-in Time: 26-May-2017 18:58:06 STScI Edit Number: 2 Title Imaging the Ejecta in Classical Novae ------------------------------------------------------------------------------------ Type Cycle GO 24 ------------------------------------------------------------------------------------ Investigators Contact? PI: Dr. Justin D. Linford George Washington University Y CoI: Dr. Laura Chomiuk Michigan State University N CoI: Dr. Jennifer L Sokoloski Columbia University in the City of New N York CoI: Dr. Michael Rupen Dominion Astrophysical Observatory N CoI: Dr. Thomas Nelson University of Pittsburgh N CoI: Dr. Koji Mukai NASA Goddard Space Flight Center N CoI: Dr. Amy Mioduszewski Associated Universities, Inc. N CoI: Mr. Thomas Finzell Michigan State University N CoI: Ms. Jennifer Helen Seng Weston Columbia University in the City of New N York CoI: Dr. Stephen S. Lawrence Hofstra University Y ------------------------------------------------------------------------------------ Abstract A nova outburst results when sufficient mass accretes from a companion star onto the surface of a white dwarf, triggering a thermonuclear explosion. In classical novae the bulk of the emission comes from the warm, expanding ejecta. The prevailing theories assume that the explosion occurs as a single, spherically symmetric ejection event and predict a simple relationship between the white dwarf mass, the accretion rate, and the mass loss and energetics of the explosion. However, observations with modern instruments indicate that nova eruptions are far from simple. There is now evidence for multiple ejection events, common envelopes, non-spherical geometry, and even jet-like structures in the ejecta. Our ENova collaboration combines radio, mm, optical, and X-ray observations and detailed theoretical modelling to study the most common major explosions in the universe. Among our results so far are the direct demonstration of the importance of shocks in novae, including the detection of gamma-ray producing shocks in several sources, and the realization that multiple, long-lived outflows are much more common than previously assumed. Here we propose to continue these highly successful observations with coordinated detailed VLA radio interferometry and HST optical imaging and spectroscropy of several recent novae with substantial VLA monitoring already in progress. ------------------------------------------------------------------------------------ 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. We have been awarded 37.5 hours of VLA A-configuration time for a campaign to image the expanding thermal ejecta of five recent classical novae. The high angular resolution during VLA A-configuration is essential to the interpretation of the radio light curves 14787( 10) - 26-May-2017 18:58:06 - [ 2] and learning how the nova morphologies have evolved since the previous A-configuration in 2014. We will combine these radio data with 6 orbits of contemporaneous HST observations described herein to image optically-thin line emission in the two recent Fermi-detected novae V339 Del and V5668 Sgr and also to obtain spatially-resolved optical spectroscopic data on V339 Del. These HST images and spectra will provide information about diffuse material in the ejecta that is not detectable by VLA and provide more details on the kinematics of the explosions at angular resolutions comparable to the VLA in A-configuration, tying together the extensive radio and optical data sets on these sources. The WFC3 imaging of the younger Nova V5668 Sgr will be done in a single, one-orbit visit (01), split evenly between the F502N and F657N filters. The WFC3 imaging of the older Nova V339 Del will be done in a single, two-orbit visit (02), also split evenly between the the F502N and F657N filters. The STIS spectral imaging of Nova V339 Del will be done in a single, three-orbit visit (03), using the G430L grating to probe the structure and kinematics of the newborn remnant in permitted and forbidden transitions spanning a large range of ionization states. As these HST visits are coordinated observations with the VLA A-configuration radio campaign, there are moderately strong timing constraints. The VLA will only be in its A-configuration for four months from 2016/09/23 through 2017/01/23, so the observations of V339 Del will be executed in that same general window. V5668 Sgr is fading more slowly than anticipated, so we are delaying that visit until the second half of Cycle 24. ------------------------------------------------------------------------------------ 14787( 10) - 26-May-2017 18:58:06 - [ 3] TARGET LIST Fixed Targets ------------------------------------------------------------------------------------------------------------------------------------ Tar| Target | Target | Target |Coord | Radial | Flux data No | Name | Description | Position |Eqnx | Vel. | ------------------------------------------------------------------------------------------------------------------------------------ 1 NOVA-DEL-201 EXT-STAR, CLASSICAL RA=20H23M30.6800S +/- 0.05", J2000 V = 14.2 +/- 0.2 B = 15.2 +/-0.2; R = 3 NOVA, EJECTA, EMISSION DEC=+20D46'3.80" +/- 0.05" 14.0 +/-0.2 LINE NEBULA, SHELL Reference Frame: ICRS Extended: YES Comments: This object was generated by the targetselector and retrieved from the SIMBAD database, coordinates confirmed with those reported in most recent literature and in the Target Confirmation tool. Photometry reported here is taken from the most recent CCD measurements (early July 2016) in the AAVSO database. The nova is fading, although fairly slowly at this late stage in its evolution. Based on the last few months of the AAVSO light curve, we predict it will fade to V ~ 14.5 and R ~ 14.2 by the early portion of Cycle 24 in late 2016. ------------------------------------------------------------------------------------------------------------------------------------ 2 NOVA-SGR-201 EXT-STAR, CLASSICAL RA=18H36M56.8400S +/- 0.1", J2000 V = 10.31 +/- 0.2 B = 11.25 +/-0.2, R = 5-B NOVA, EJECTA, EMISSION DEC=-28D55'39.80" +/- 0.1" 10.97 +/-0.2 LINE NEBULA, SHELL Reference Frame: ICRS Extended: YES Comments: This object was generated by the targetselector and retrieved from the SIMBAD database, coordinates confirmed with those reported in most recent literature and in the Target Confirmation tool. Photometry reported here is taken from the most recent CCD measurements (early July 2016) in the AAVSO database. The nova is fading, although surprisingly slowly for a novae at this relatively young age. Based on the last few months of the AAVSO light curve, we predict it will fade to V ~ 12.0 and R ~ 13.6 by the June 2017. ------------------------------------------------------------------------------------------------------------------------------------ 14787( 10) - 26-May-2017 18:58:06 - [ 4] Patterns ------------------------------------------------------------------------------------------------------------------------------------ Pattern_Number: 3 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 WRC3-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: 4 Primary_Pattern Secondary_Pattern Pattern_Type WFC3-UVIS-DITHER-LINE-3PT Pattern_Purpose DITHER Number_Of_Points 3 Point_Spacing 0.405 Line_Spacing Coordinate_Frame POS-TARG Pattern_Orient 46.84 Angle_Between_Sides Center_Pattern NO Pattern_Comments: Standard WRC3-UVIS-DITHER-LINE-3PT pattern scaled up 3.0x in size to dither short exposures for cosmic ray & bad pixels, and move potentially saturated/bled central pixels with larger column separations ------------------------------------------------------------------------------------------------------------------------------------ Pattern_Number: 5 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. ------------------------------------------------------------------------------------------------------------------------------------ 14787( 10) - 26-May-2017 18:58:06 - [ 5] Patterns ------------------------------------------------------------------------------------------------------------------------------------ Pattern_Number: 6 Primary_Pattern Secondary_Pattern Pattern_Type LINE WFC3-UVIS-DITHER-BOX Pattern_Purpose DITHER DITHER Number_Of_Points 3 4 Point_Spacing 0.135 0.519 Line_Spacing 0.336 Coordinate_Frame POS-TARG POS-TARG Pattern_Orient 46.84 23.884 Angle_Between_Sides 81.785 Center_Pattern NO NO Pattern_Comments: Pattern for longer WFC3 exposures, to allow for three repetitions of the 4-point WFC3-UVIS-DITHER-BOX pattern, each with slightly offset pointings to maximize recovery of spatial information. This pattern was suggested as a modification to Visit 02 by Sylvia Baggett in late Sept. 2016. ------------------------------------------------------------------------------------------------------------------------------------ Pattern_Number: 7 Primary_Pattern Secondary_Pattern Pattern_Type LINE WFC3-UVIS-DITHER-BOX Pattern_Purpose DITHER DITHER Number_Of_Points 2 4 Point_Spacing 0.135 0.519 Line_Spacing 0.336 Coordinate_Frame POS-TARG POS-TARG Pattern_Orient 46.84 23.884 Angle_Between_Sides 81.785 Center_Pattern NO NO Pattern_Comments: Pattern for longer WFC3 exposures, to allow for three repetitions of the 4-point WFC3-UVIS-DITHER-BOX pattern, each with slightly offset pointings to maximize recovery of spatial information. This pattern was suggested as a modification to Visit 02 by Sylvia Baggett in late Sept. 2016. ------------------------------------------------------------------------------------------------------------------------------------ 14787( 10) - 26-May-2017 18:58:06 - [ 6] Visit: 01 (Visit 01 new: 1 orbit of WFC3 imaging on V5668 Sgr) Visit Requirements: BETWEEN 01-MAY-2017:00:00:00 AND 31-AUG-2017:00:00:00 On Hold Comments: Additional Comments: NOTE: This orbit was re-structured in May 2017 based on updated brightnesses and line strengths from recetn AAVSO photometry and ground-based spectra. The purpose of Visit 01 is to take WFC3 images of the expanding remnant of Nova Sgr 2015b = V5668 Sgr. This imaging visit is for one orbit, for a total of 244 seconds in F502N ( [O III] ) and 324 seconds in F657N ( Halpha+[N II] ). V5668 Sgr has faded much more slowly than expected, and hence is significantly brighter than was expected. We request that these exposures be taken late in Cycle 24, between 2017-05-01 and 2017-08-31, to allow the nova to fade below V~12.0 magnitude, but still stay within ~6 months of the VLA A-configuration radio imaging. We split the exposures in each filter into two sets, with the first set short enough to avoid saturating the brightest pixels of the central stellar point source. The second sets will most likely saturate the central point source, but we want to search for faint extended nebular shells 0.5--1.0" out from the core. Exposure times estimated from the ETC using recent AAVSO V-band photometry and SMARTS spectra of V5668 Sgr. Note that use of the "auto-expand" function to maximally pack the orbit severely restricts the scheduling windows, so the requested exposure times are about as large as we can practically make them. Flash levels 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 1.0 S (4 PATTERN 3 1 15-B S 1C-SUB S) Comments: Post-flash = 12 e- based on ETC WFC3UVIS.im.827956 We use two iterations of the 4-point of a 3x expanded WFC3-UVIS-DITHER-BOX with 230 second subexposures: if the nova fades to V=14.5 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 and on scaling our previous images of V959 Mon and T Pyx. ------------------------------------------------------------------------------------------------------------------------------------ 14787( 10) - 26-May-2017 18:58:06 - [ 7] 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 30.0 S PATTERN 7 2 15-B S 1C-SUB (240 S) Comments: Post-flash = 12 e- based on ETC WFC3UVIS.im.827956 We use two iterations of the 4-point of a 3x expanded WFC3-UVIS-DITHER-BOX with 230 second subexposures: if the nova fades to V=14.5 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 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 1.0 S (4 PATTERN 3 3 15-B S 1C-SUB S) Comments: Post-flash = 12 e- based on WFC3UVIS.im.827980 We use three iterations at each of the 4-points of a 3x expanded WFC3-UVIS-DITHER-BOX with 150 second subexposures: if the nova fades to R=14.2 these should not saturate the brightest few pixels of 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 and on scaling our previous images of V959 Mon and T Pyx. ------------------------------------------------------------------------------------------------------------------------------------ 4 NOVA-SGR-20 WFC3/UVI ACCUM UVIS2-C1K F657N FLASH=12 1 40.0 S PATTERN 7 4 15-B S 1C-SUB (320 S) Comments: Post-flash = 12 e- based on WFC3UVIS.im.827980 We use three iterations at each of the 4-points of a 3x expanded WFC3-UVIS-DITHER-BOX with 150 second subexposures: if the nova fades to R=14.2 these should not saturate the brightest few pixels of 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 and on scaling our previous images of V959 Mon and T Pyx. ------------------------------------------------------------------------------------------------------------------------------------ 14787( 10) - 26-May-2017 18:58:06 - [ 8] 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-B 1 WFC3/UVI ACCUM UVIS2-C1 F502N 1 none none none 1 N/A S K1C-SUB NOVA-SGR-2015-B 1 WFC3/UVI ACCUM UVIS2-C1 F502N 2 none none none 1 N/A S K1C-SUB NOVA-SGR-2015-B 1 WFC3/UVI ACCUM UVIS2-C1 F502N 3 none none none 1 N/A S K1C-SUB NOVA-SGR-2015-B 1 WFC3/UVI ACCUM UVIS2-C1 F502N 4 none none none 1 N/A S K1C-SUB NOVA-SGR-2015-B 2 WFC3/UVI ACCUM UVIS2-C1 F502N 1 1 none none 1 N/A S K1C-SUB NOVA-SGR-2015-B 2 WFC3/UVI ACCUM UVIS2-C1 F502N 1 2 none none 1 N/A S K1C-SUB NOVA-SGR-2015-B 2 WFC3/UVI ACCUM UVIS2-C1 F502N 1 3 none none 1 N/A S K1C-SUB NOVA-SGR-2015-B 2 WFC3/UVI ACCUM UVIS2-C1 F502N 1 4 none none 1 N/A S K1C-SUB NOVA-SGR-2015-B 2 WFC3/UVI ACCUM UVIS2-C1 F502N 2 1 none none 1 N/A S K1C-SUB NOVA-SGR-2015-B 2 WFC3/UVI ACCUM UVIS2-C1 F502N 2 2 none none 1 N/A S K1C-SUB NOVA-SGR-2015-B 2 WFC3/UVI ACCUM UVIS2-C1 F502N 2 3 none none 1 N/A S K1C-SUB NOVA-SGR-2015-B 2 WFC3/UVI ACCUM UVIS2-C1 F502N 2 4 none none 1 N/A S K1C-SUB NOVA-SGR-2015-B 3 WFC3/UVI ACCUM UVIS2-C1 F657N 1 none none none 1 N/A S K1C-SUB NOVA-SGR-2015-B 3 WFC3/UVI ACCUM UVIS2-C1 F657N 2 none none none 1 N/A S K1C-SUB NOVA-SGR-2015-B 3 WFC3/UVI ACCUM UVIS2-C1 F657N 3 none none none 1 N/A S K1C-SUB NOVA-SGR-2015-B 3 WFC3/UVI ACCUM UVIS2-C1 F657N 4 none none none 1 N/A S K1C-SUB NOVA-SGR-2015-B 4 WFC3/UVI ACCUM UVIS2-C1 F657N 1 1 none none 1 N/A S K1C-SUB NOVA-SGR-2015-B 4 WFC3/UVI ACCUM UVIS2-C1 F657N 1 2 none none 1 N/A S K1C-SUB NOVA-SGR-2015-B 4 WFC3/UVI ACCUM UVIS2-C1 F657N 1 3 none none 1 N/A S K1C-SUB NOVA-SGR-2015-B 4 WFC3/UVI ACCUM UVIS2-C1 F657N 1 4 none none 1 N/A S K1C-SUB NOVA-SGR-2015-B 4 WFC3/UVI ACCUM UVIS2-C1 F657N 2 1 none none 1 N/A S K1C-SUB 14787( 10) - 26-May-2017 18:58:06 - [ 9] 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-B 4 WFC3/UVI ACCUM UVIS2-C1 F657N 2 2 none none 1 N/A S K1C-SUB NOVA-SGR-2015-B 4 WFC3/UVI ACCUM UVIS2-C1 F657N 2 3 none none 1 N/A S K1C-SUB NOVA-SGR-2015-B 4 WFC3/UVI ACCUM UVIS2-C1 F657N 2 4 none none 1 N/A S K1C-SUB 14787( 10) - 26-May-2017 18:58:06 - [ 10] Visit: 02 (Visit 02: 2 orbits of WFC3 imaging on V339 Del) Visit Requirements: ORIENT 315D TO 140 D; BETWEEN 23-SEP-2016:00:00:00 AND 24-JAN-2017:00:00:00 On Hold Comments: Additional Comments: The purpose of Visit 02 is to take deep WFC3 images of the expanding remnant of Nova Del 2013 = V339 Del, fairly contemporaneous with VLA A-configuration radio interfermetry (late September 2016 to late January 2017). This visit should be scheduled 21-90 days before the STIS spectroscopic Visit 03, in order to provide contemporaneous intensity mapping with the spectra, yet also to provide optimal slit orientation information for the STIS spectra in Visit 03 to follow shortly thereafter. This imaging visit is for two orbits, for a total of ~2200 seconds in F502N ( [O III] ) and ~2320 seconds in F657N ( Halpha+[N II] ). Exposure times estimated from the ETC and by scaling our past F502N and F657N images of Nova Mon and T Pyx up to the anticipated brightness of V339 Del in late 2016. If new ground-based photometry or spectra indicate dramatic or unexpected changes, we may request an adjustment of exposure times within this orbit. Note that use of the "auto-expand" function to maximally pack the orbit severely restricts the scheduling windows, so the requested exposure times are about as large as we can practically make them. Flash levels set using the minimum ETC recommendation that did not trigger a warning flag. Comment added with re-submission on 9/19/16: Visit Orient Range Requirement of MinOrient=315 and MaxOrient=140 degrees added upon recommendation of S. Baggett to prevent two nearby, but off-CCD stars to SW from producing flares in the images. This appears to have no impact on schedulability. 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-DEL-20 WFC3/UVI ACCUM UVIS2-C1K F502N FLASH=12 1 10 S (40 PATTERN 3 1 13 S 1C-SUB S) Comments: Post-flash = 12 e- based on ETC WFC3UVIS.im.827956 We use two iterations of the 4-point of a 3x expanded WFC3-UVIS-DITHER-BOX with 230 second subexposures: if the nova fades to V=14.5 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 and on scaling our previous images of V959 Mon and T Pyx. ------------------------------------------------------------------------------------------------------------------------------------ 14787( 10) - 26-May-2017 18:58:06 - [ 11] 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-DEL-20 WFC3/UVI ACCUM UVIS2-C1K F502N FLASH=12 1 110 S PATTERN 6 2 13 S 1C-SUB (1320 S) Comments: Post-flash = 12 e- based on ETC WFC3UVIS.im.827956 We use two iterations of the 4-point of a 3x expanded WFC3-UVIS-DITHER-BOX with 230 second subexposures: if the nova fades to V=14.5 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 and on scaling our previous images of V959 Mon and T Pyx. ------------------------------------------------------------------------------------------------------------------------------------ 3 NOVA-DEL-20 WFC3/UVI ACCUM UVIS2-C1K F657N FLASH=12 1 120 S PATTERN 6 3 13 S 1C-SUB (1440 S) Comments: Post-flash = 12 e- based on WFC3UVIS.im.827980 We use three iterations at each of the 4-points of a 3x expanded WFC3-UVIS-DITHER-BOX with 150 second subexposures: if the nova fades to R=14.2 these should not saturate the brightest few pixels of 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 and on scaling our previous images of V959 Mon and T Pyx. ------------------------------------------------------------------------------------------------------------------------------------ 4 NOVA-DEL-20 WFC3/UVI ACCUM UVIS2-C1K F657N FLASH=12 1 10 S (40 PATTERN 3 4 13 S 1C-SUB S) Comments: Post-flash = 12 e- based on WFC3UVIS.im.827980 We use three iterations at each of the 4-points of a 3x expanded WFC3-UVIS-DITHER-BOX with 150 second subexposures: if the nova fades to R=14.2 these should not saturate the brightest few pixels of 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 and on scaling our previous images of V959 Mon and T Pyx. ------------------------------------------------------------------------------------------------------------------------------------ 14787( 10) - 26-May-2017 18:58:06 - [ 12] 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-DEL-2013 1 WFC3/UVI ACCUM UVIS2-C1 F502N 1 none none none 1 N/A S K1C-SUB NOVA-DEL-2013 1 WFC3/UVI ACCUM UVIS2-C1 F502N 2 none none none 1 N/A S K1C-SUB NOVA-DEL-2013 1 WFC3/UVI ACCUM UVIS2-C1 F502N 3 none none none 1 N/A S K1C-SUB NOVA-DEL-2013 1 WFC3/UVI ACCUM UVIS2-C1 F502N 4 none none none 1 N/A S K1C-SUB NOVA-DEL-2013 2 WFC3/UVI ACCUM UVIS2-C1 F502N 1 1 none none 1 N/A S K1C-SUB NOVA-DEL-2013 2 WFC3/UVI ACCUM UVIS2-C1 F502N 1 2 none none 1 N/A S K1C-SUB NOVA-DEL-2013 2 WFC3/UVI ACCUM UVIS2-C1 F502N 1 3 none none 1 N/A S K1C-SUB NOVA-DEL-2013 2 WFC3/UVI ACCUM UVIS2-C1 F502N 1 4 none none 1 N/A S K1C-SUB NOVA-DEL-2013 2 WFC3/UVI ACCUM UVIS2-C1 F502N 2 1 none none 1 N/A S K1C-SUB NOVA-DEL-2013 2 WFC3/UVI ACCUM UVIS2-C1 F502N 2 2 none none 1 N/A S K1C-SUB NOVA-DEL-2013 2 WFC3/UVI ACCUM UVIS2-C1 F502N 2 3 none none 1 N/A S K1C-SUB NOVA-DEL-2013 2 WFC3/UVI ACCUM UVIS2-C1 F502N 2 4 none none 1 N/A S K1C-SUB NOVA-DEL-2013 2 WFC3/UVI ACCUM UVIS2-C1 F502N 3 1 none none 1 N/A S K1C-SUB NOVA-DEL-2013 2 WFC3/UVI ACCUM UVIS2-C1 F502N 3 2 none none 1 N/A S K1C-SUB NOVA-DEL-2013 2 WFC3/UVI ACCUM UVIS2-C1 F502N 3 3 none none 1 N/A S K1C-SUB NOVA-DEL-2013 2 WFC3/UVI ACCUM UVIS2-C1 F502N 3 4 none none 1 N/A S K1C-SUB NOVA-DEL-2013 3 WFC3/UVI ACCUM UVIS2-C1 F657N 1 1 none none 2 N/A S K1C-SUB NOVA-DEL-2013 3 WFC3/UVI ACCUM UVIS2-C1 F657N 1 2 none none 2 N/A S K1C-SUB NOVA-DEL-2013 3 WFC3/UVI ACCUM UVIS2-C1 F657N 1 3 none none 2 N/A S K1C-SUB NOVA-DEL-2013 3 WFC3/UVI ACCUM UVIS2-C1 F657N 1 4 none none 2 N/A S K1C-SUB NOVA-DEL-2013 3 WFC3/UVI ACCUM UVIS2-C1 F657N 2 1 none none 2 N/A S K1C-SUB 14787( 10) - 26-May-2017 18:58:06 - [ 13] 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-DEL-2013 3 WFC3/UVI ACCUM UVIS2-C1 F657N 2 2 none none 2 N/A S K1C-SUB NOVA-DEL-2013 3 WFC3/UVI ACCUM UVIS2-C1 F657N 2 3 none none 2 N/A S K1C-SUB NOVA-DEL-2013 3 WFC3/UVI ACCUM UVIS2-C1 F657N 2 4 none none 2 N/A S K1C-SUB NOVA-DEL-2013 3 WFC3/UVI ACCUM UVIS2-C1 F657N 3 1 none none 2 N/A S K1C-SUB NOVA-DEL-2013 3 WFC3/UVI ACCUM UVIS2-C1 F657N 3 2 none none 2 N/A S K1C-SUB NOVA-DEL-2013 3 WFC3/UVI ACCUM UVIS2-C1 F657N 3 3 none none 2 N/A S K1C-SUB NOVA-DEL-2013 3 WFC3/UVI ACCUM UVIS2-C1 F657N 3 4 none none 2 N/A S K1C-SUB NOVA-DEL-2013 4 WFC3/UVI ACCUM UVIS2-C1 F657N 1 none none none 2 N/A S K1C-SUB NOVA-DEL-2013 4 WFC3/UVI ACCUM UVIS2-C1 F657N 2 none none none 2 N/A S K1C-SUB NOVA-DEL-2013 4 WFC3/UVI ACCUM UVIS2-C1 F657N 3 none none none 2 N/A S K1C-SUB NOVA-DEL-2013 4 WFC3/UVI ACCUM UVIS2-C1 F657N 4 none none none 2 N/A S K1C-SUB 14787( 10) - 26-May-2017 18:58:06 - [ 14] Visit: 03 (Visit 03: 3 orbits of STIS CCD G430L spectra on V339 Del) Visit Requirements: ORIENT 85D TO 105 D; ORIENT 265D TO 285 D On Hold Comments: Additional Comments: The purpose of Visit 03 is to use 3 orbits to take STIS CCD G430L spectra along either the major or minor axis of the expanding and fading remnant of Nova Del 2103 = V339 Del, after the axis orientation has been revealed by the WFC3 imaging Visit 02. Both Visits 02 and 03 are constrained to be relatively contemporaneous with VLA A-configuration observations of V339 Del (to be taken late September 2016 to late January 2017). This visit will likely require a specific narrow range in roll angle to place the STIS slit at the optimum PA to match spatial structures seen in the WFC3 imaging of Visit 02. As such, determining this exact roll angle and the subsequent scheduling window will need to wait until the Visit 02 imaging is taken and quickly analyzed. Either a major axis or minor axis should be available within 4 months after the WFC3 imaging visit, thus we request for this Visit to follow Visit 02 by at least 21 days, but not more than 120 days. Including solar and timing restrictions, Visit 03 will thus likely need to be scheduled in a few week window sometime within late October 2016 to late December 2016, or possibly March--April 2017. This spectroscopic visit is for a total of three orbits, for a total of 1580+2280+2260=6120 seconds in 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. Note that use of the "auto-expand" function to maximally pack the orbit seems to severely restrict the scheduling windows, so the requested exposure times are about as large as we can practically make them. Comment added with re-submission on 11/01/16: A preliminary review of the WFC3 imaging from Visit 02 obtained on 10/18/16 shows that the remnant is spatially-resolved relative to a stellar PSF. [V339 Del FWHM ~ 7 pixels ~ 0.3 arcseconds; all stars have FWHM < 2 pixels ~0.08 arcseconds.] Additionally, the central core of V339 Del is resolved into an asymmetric ring-like structure ~0.2 arcsec (4--5 pixels) in diameter, with minimum and maximum pixels on opposite sides along a symmetry axis that runs from PA 50 to 230 E of N relative to the center of V339 Del overall (with the brightest pixel at PA 230). As such, following the original submitted Phase II plan, in order to gain maximum spatial resolution and minimize spatial-spectral confusion, we would want to schedule Visit 03 to place the STIS slit along this 230--50 symmetry axis. Requiring the STIS slit to match the 230 or 50 PA to within +/-10 degrees needs spacecraft ORIENT ranges of 265--285 or 85--105, respectively. We have added these specific "Orient Range" restrictions with this update of the Phase II plan. Additionally, to clear various errors and warnings, we removed the "On Hold" and "Timing Requirements" linking this visit explicitly to Visit 02, which has now been executed. The newly-added STIS orient ranges requirements (specifically the PA 230 alignment) are schedulable in March--May 2017. Exposures ------------------------------------------------------------------------------------------------------------------------------------ Exp | Target | Instr | Oper. | Aper |Spectral|Central| Optional |Num| Time | Special Num | Name | Config | Mode | or FOV |Element |Waveln.| Parameters |Exp| (Total) | Requirements ------------------------------------------------------------------------------------------------------------------------------------ 14787( 10) - 26-May-2017 18:58:06 - [ 15] 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-DEL-20 STIS/CCD ACQ 50CCD MIRROR ACQTYPE=DIFFUSE, CHECKBOX=5, 1 3 S (3 S) 13 DIFFUSE-CENTER=FLUX-CENTROID Comments: Acquistion imaging for V339 Del, which we expect to be a point source potentially surrounded by small-scale (<0.5 arcsec) nebular structures of possibly similar intensity. We will use the WFC3 imaging from Visit 02 to determine whether a ACQ-PEAK will be suitable, or if an OFFSET from a nearby star will be needed. ------------------------------------------------------------------------------------------------------------------------------------ 2 NOVA-DEL-20 STIS/CCD ACQ/PEA 52X0.1E1 MIRROR 1 3 S (3 S) 13 K Comments: Peak-up imaging for V339 Del, which we expect to be a point source potentially surrounded by small-scale (<0.5 arcsec) nebular structures of possibly similar intensity. We will use the WFC3 imaging from Visit 02 to determine whether a ACQ-PEAK will be suitable, or if an OFFSET from a nearby star will be needed. ------------------------------------------------------------------------------------------------------------------------------------ 3 NOVA-DEL-20 STIS/CCD ACCUM 52X2E1 G430L 4300 CR-SPLIT=2 1 395 S PATTERN 5 3 13 (1580 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 395 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 potentially increase the spatial resolution. Exposure estimates based on the ETC and on scaling our previous spectra of V959 Mon and T Pyx. ------------------------------------------------------------------------------------------------------------------------------------ 14787( 10) - 26-May-2017 18:58:06 - [ 16] 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-DEL-20 STIS/CCD ACCUM 52X2E1 G430L 4300 CR-SPLIT=2 1 570 S PATTERN 5 4 13 (2280 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 570 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 potentially increase the spatial resolution. Exposure estimates based on the ETC and on scaling our previous spectra of V959 Mon and T Pyx. ------------------------------------------------------------------------------------------------------------------------------------ 5 NOVA-DEL-20 STIS/CCD ACCUM 52X2E1 G430L 4300 CR-SPLIT=2 1 565 S PATTERN 5 5 13 (2260 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 565 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 potentially increase the spatial resolution. Exposure estimates based on the ETC and on scaling our previous spectra of V959 Mon and T Pyx. ------------------------------------------------------------------------------------------------------------------------------------ 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-DEL-2013 1 STIS/CCD ACQ 50CCD MIRROR none none none none 1 N/A NOVA-DEL-2013 2 STIS/CCD ACQ/PEA 52X0.1E1 MIRROR none none none none 1 N/A K NOVA-DEL-2013 3 STIS/CCD ACCUM 52X2E1 G430L 4300 1 none none 1 1 N/A NOVA-DEL-2013 3 STIS/CCD ACCUM 52X2E1 G430L 4300 1 none none 2 1 N/A NOVA-DEL-2013 3 STIS/CCD ACCUM 52X2E1 G430L 4300 2 none none 1 1 N/A NOVA-DEL-2013 3 STIS/CCD ACCUM 52X2E1 G430L 4300 2 none none 2 1 N/A NOVA-DEL-2013 3 STIS/CCD ACCUM 52X2E1 G430L 4300 3 none none 1 1 N/A NOVA-DEL-2013 3 STIS/CCD ACCUM 52X2E1 G430L 4300 3 none none 2 1 N/A NOVA-DEL-2013 3 STIS/CCD ACCUM 52X2E1 G430L 4300 4 none none 1 1 N/A NOVA-DEL-2013 3 STIS/CCD ACCUM 52X2E1 G430L 4300 4 none none 2 1 N/A NOVA-DEL-2013 4 STIS/CCD ACCUM 52X2E1 G430L 4300 1 none none 1 2 N/A NOVA-DEL-2013 4 STIS/CCD ACCUM 52X2E1 G430L 4300 1 none none 2 2 N/A 14787( 10) - 26-May-2017 18:58:06 - [ 17] 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-DEL-2013 4 STIS/CCD ACCUM 52X2E1 G430L 4300 2 none none 1 2 N/A NOVA-DEL-2013 4 STIS/CCD ACCUM 52X2E1 G430L 4300 2 none none 2 2 N/A NOVA-DEL-2013 4 STIS/CCD ACCUM 52X2E1 G430L 4300 3 none none 1 2 N/A NOVA-DEL-2013 4 STIS/CCD ACCUM 52X2E1 G430L 4300 3 none none 2 2 N/A NOVA-DEL-2013 4 STIS/CCD ACCUM 52X2E1 G430L 4300 4 none none 1 2 N/A NOVA-DEL-2013 4 STIS/CCD ACCUM 52X2E1 G430L 4300 4 none none 2 2 N/A NOVA-DEL-2013 5 STIS/CCD ACCUM 52X2E1 G430L 4300 1 none none 1 3 N/A NOVA-DEL-2013 5 STIS/CCD ACCUM 52X2E1 G430L 4300 1 none none 2 3 N/A NOVA-DEL-2013 5 STIS/CCD ACCUM 52X2E1 G430L 4300 2 none none 1 3 N/A NOVA-DEL-2013 5 STIS/CCD ACCUM 52X2E1 G430L 4300 2 none none 2 3 N/A NOVA-DEL-2013 5 STIS/CCD ACCUM 52X2E1 G430L 4300 3 none none 1 3 N/A NOVA-DEL-2013 5 STIS/CCD ACCUM 52X2E1 G430L 4300 3 none none 2 3 N/A NOVA-DEL-2013 5 STIS/CCD ACCUM 52X2E1 G430L 4300 4 none none 1 3 N/A NOVA-DEL-2013 5 STIS/CCD ACCUM 52X2E1 G430L 4300 4 none none 2 3 N/A 14787( 10) - 26-May-2017 18:58:06 - [ 18] Summary Form for Proposal 14787 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 BETWEEN 01-MAY-2017:00:00:00 AND 31-AUG-2017:00:00:00, BETWEEN 23-SEP-2016:00:00:00 AND 24-JAN-2017:00:00:00, ORIENT 265D TO 285 D, ORIENT 315D TO 140 D, ORIENT 85D TO 105 D, PATTERN 3 1, PATTERN 3 3, PATTERN 3 4, PATTERN 5 3, PATTERN 5 4, PATTERN 5 5, PATTERN 6 2, PATTERN 6 3, PATTERN 7 2, PATTERN 7 4 ------------------------------------------------------------------------------------------------------------------------------------ Spectral Elements F502N, F657N, G430L, MIRROR ------------------------------------------------------------------------------------------------------------------------------------ Target Names NOVA-DEL-2013, NOVA-SGR-2015-B ------------------------------------------------------------------------------------------------------------------------------------