15192( 5) - 07-Mar-2018 22:18:14 - [ 1] HUBBLE SPACE TELESCOPE OBSERVING PROGRAM 15192 Version: 5 Check-in Time: 07-Mar-2018 22:18:14 STScI Edit Number: 2 Title Whimper of a Bang: Documenting the Final Days of the Nearby Type Ia Supernova 2011fe ------------------------------------------------------------------------------------ Type Cycle GO 25 ------------------------------------------------------------------------------------ Investigators Contact? PI: Prof. Benjamin John Shappee University of Hawaii Y CoI: Dr. Krzysztof Z. Stanek The Ohio State University N CoI: Dr. Chris S. Kochanek The Ohio State University N CoI: Dr. Peter M. Garnavich University of Notre Dame N ------------------------------------------------------------------------------------ Abstract Even though SNe Ia are crucial to cosmological studies as distance indicators, the exact nature of these systems remains theoreltically ambiguous and observationally elusive. However, there is a new hope. The very late-time light curves of SNe Ia harbor important clues to the natures of their progenitor systems. First, the ejecta from the SN will shock heat a non-degenerate companion, leaving it luminous and visible at very late times after the SN has faded . Second, due to nucleosynthetic effects during the explosion, single and double degenerate SNe Ia models are predicted to produce vastly differing amounts of 57Co and 55Fe. 57Co and 55Fe dominate the power of the very late time light curves of SNe Ia after >1050 days after the initial explosion. Broadband observations of the bolometric luminosity at these epochs have the ability to measure the ratio of these two isotopes and thus discriminate between progenitor models. As the brightest SN Ia in nearly 40 years, SN 2011fe offers a prime opportunity to follow a SN Ia to such late epochs. Here we propose HST WFC3 optical and IR photometry of SN 2011fe to observe the transition from a 57Co to a 55Fe powered lightcurve and to constrain a possible shock-heated companion. These observations will place unique constraints on progenitor systems of SNe Ia. SN 2011fe, having been already observed for more than 1600 days and a factor of four million in flux. The observations proposed here would follow SN 2011fe to an epoch 2.5 times later than any other SNe Ia. SN 2011fe is likely to remain the best studied normal SN Ia of our generation and if these observations are not made now, they will likely never be done with Hubble. ------------------------------------------------------------------------------------ Observations Description ------------------------ The observations proposed here continue a project from Cycles 22 and 23 with the goal of constructing a quasi-bolometric light curve to monitor the late-time evolution of SN 2011fe. We have already obtained four epochs and a fifth epoch is scheduled for September 2016. We propose obtaining two additional epochs during Cycles 24 and 25 at ~ 2100 and ~ 2500 days after tBmax to well-sample the transition to a dominantly 55Fe powered light curve and to constrain the existence of a shock-heated companion. The very late-time spectra of SNe Ia predominantly consists of line emission over a very broad range of wavelengths longwards of the UV (where there is little emission). We selected the F438W (B), F555W (V ) and F600LP (R+I) 15192( 5) - 07-Mar-2018 22:18:14 - [ 2] filters for WFC3/UVIS and F110W (Y J) and F160W (H) for WFC3/IR. There are a number of reasons this filter combination is ideal for this project: 1) These filters cover 4000 to 17000 A with no gaps and relatively uniform throughput. Our ground-based spectroscopy and photometry show there is little flux blueward of 4000 A so we forgo the F336W (U) and UV filters. 2) A single long pass filter would not be sufficient because the shape of the SN spectral energy distribution is known to be changing with ionization (McClelland et al. 2013; Graham et al 2015; Taubenberger et al. 2015, Shappee et al. in prep.). Computing the bolometric luminosity with a single F350LP observation would lead to large systematic uncertainties. However, using individual broad band filters retains some spectral information without the impossible expense of taking a spectrum. Without this information, we could mistake a change in ionization state for a change in the bolometric luminosity or interpret a light echo as a flattening of the bolometric light curve. 3) Finally, the optical filter combination also attempts to evenly partition the optical energy. In the spectrum obtained 850 days after tBmax, the wavelength ranges covered by B, V , R, and I, contained 48%, 37%, 21%, 19% of the optical energy. Thus we have kept B and V as separate filters but F600LP covers both the R and I wavelength ranges. We estimated the number of orbits and exposures needed for our program using the estimated magnitudes shown in Figure 1 and the recommendations in the HST Primer. We require a SNR of 7 and 5 for the 3 optical filters during Cycle 24 and 25, respectively. These SNRs will allow us to construct a quasi-bolometric light curve of SN 2011fe and distinguish between the Ropke et al. (2012) models by ~ 3 sigma at each epoch. Conveniently, these SNRs will also allow us to constrain the light from a possible 1Msun shock-heated companion at the 2 and 3-sigma level during each epoch in the F 555W and F 600LP filters, respectively. The NIR, however, is not as simple because it appears that SN 2011fe is blended in the Cycle 22 and 23 F110W and F160W observations with nearby, faint, very-red stars. There is also the concern that crowding and confusion may inhibit our measurement in the optical. Luckily, SN 2011fe exploded in a sparse region of the outer disk of M101 where archival pre-explosion HST images existed. Li et al. (2011) use these images and Keck AO observations of SN 2011fe to constrain the progenitor system. They detect no counter part at the location of the SN and place upper limits of F435W < 27.87, F555W < 27.49, and F814W < 26.81 at its position. These limits are fainter than SN 2011fe is expected to be during all of Cycle 24. We then used the exposure time calculator to estimate the length of our required ob- servations. The exposure time calculations for all of the observations include both their dates and coordinates to ensure that our estimated times are accurate and that the correct contribution of zodiacal light is accounted for. The estimates are also based on the observed optical spectrum of SN 2011fe taken 850 days after tBmax which is calibrated to the expected broad-band magnitudes for each epoch. Finally, because no SN Ia has ever been observed at these epochs, changes in the ionization state of SN 2011fe are possible and can not be predicted. This could conceivably significantly change which filters receive the largest portion of the SN flux. 15192( 5) - 07-Mar-2018 22:18:14 - [ 3] Thus, we will use the Cycle 23/24 photometry to determine if the exposure time distribution needs to be adjusted for Cycle 24/25, respectively. It is important to note that both of the proposed observations in Cycle 24 and Cycle 25 are critical to understanding the late-time evolution of SN 2011fe. Cycle 24 could unveil the existence of a shock-heated companion. But decisively determining if a flattening in the F600LP lightcurve is due to a companion (evolves on a time scale of ~ 1000 years), 55Fe becoming the dominate heating source (half-life of ~ 3 years), or a change in ionization state will be difficult without a latter epoch. If a shock-heated companion is not seen, then the observations in Cycle 25 will represent the first time we observe a SNe Ia light curve powered by 55Fe. Additionally, difference imaging with the later, deeper epoch will allow us to better deal with crowding, especially in the NIR filters. All of these reasons make late-time observations key. Finally, because there is still a large and ongoing interest in SN 2011fe, we will waive our 1 year proprietary period and make the data immediately public. Parallel Observations: As the closest face-on Milky Way analogue, M101 is an important nearby galaxy for many reasons. For example, Shara et al. (2013) have compiled a catalog of 10, 000 Wolf- Rayet stars using extensive HST WFC3 He II optical narrow-band imaging. There are also F435W/F555W/F814W/F658N(Halpha) mosaics covering most of the galaxy (GO 9490, 9492, 9720). We have performed a study of Cepheids using archival ACS data that provides the distance which is commonly used for SN 2011fe (Shappee & Stanek 2011). M101 is an important galaxy for the recent 2.4% determination of the Hubble Constant (Riess et al. 2016). We are surveying the entire galaxy for new Cepheids with the LBT. We include ACS in parallel mode to broaden the archival data base. We have used APT and Aladin to confirm it is possible to place the ACS detector (given the roll restrictions created by the timing of the observations) on both of the two Cepheid fields used for published HST Cepheid distance measurements. Our parallel fields could add another, even deeper, epoch for each field and help to better constrain down Cepheid periods, magnitudes, and reddening in those fields. However, because M101 is such and interesting and large galaxy, an ACS parallel observation at any roll angle would be valuable. ------------------------------------------------------------------------------------ 15192( 5) - 07-Mar-2018 22:18:14 - [ 4] TARGET LIST Fixed Targets ------------------------------------------------------------------------------------------------------------------------------------ Tar| Target | Target | Target |Coord | Radial | Flux data No | Name | Description | Position |Eqnx | Vel. | ------------------------------------------------------------------------------------------------------------------------------------ 1 SN-2011FE-UV EXT-STAR, SUPERNOVA RA=14H03M14.3269S, J2000 V = 27.5 +/- 1.0 IS TYPE IA DEC=+54D16'22.93" Reference Frame: Other: SIMBAD Comments: This object was generated by the targetselector and retrieved from the SIMBAD database. ------------------------------------------------------------------------------------------------------------------------------------ 2 SN-2011FE-IR EXT-STAR, SUPERNOVA RA=14H03M6.0919S, J2000 V = 27.5 +/- 1.0 TYPE IA DEC=+54D16'26.53" Reference Frame: Other: SIMBAD Comments: This object was generated by the targetselector and retrieved from the SIMBAD database. ------------------------------------------------------------------------------------------------------------------------------------ 15192( 5) - 07-Mar-2018 22:18:14 - [ 5] Patterns ------------------------------------------------------------------------------------------------------------------------------------ Pattern_Number: 1 Primary_Pattern Secondary_Pattern Pattern_Type WFC3-UVIS-DITHER-BOX Pattern_Purpose DITHER Number_Of_Points 4 Point_Spacing 0.173 Line_Spacing 0.112 Coordinate_Frame POS-TARG Pattern_Orient 23.884 Angle_Between_Sides 81.785 Center_Pattern NO ------------------------------------------------------------------------------------------------------------------------------------ Pattern_Number: 2 Primary_Pattern Secondary_Pattern Pattern_Type WFC3-IR-DITHER-BOX-MIN Pattern_Purpose DITHER Number_Of_Points 4 Point_Spacing 0.572 Line_Spacing 0.365 Coordinate_Frame POS-TARG Pattern_Orient 18.528 Angle_Between_Sides 74.653 Center_Pattern NO ------------------------------------------------------------------------------------------------------------------------------------ Pattern_Number: 3 Primary_Pattern Secondary_Pattern Pattern_Type LINE LINE Pattern_Purpose DITHER DITHER Number_Of_Points 3 2 Point_Spacing 0.605 0.06775 Line_Spacing Coordinate_Frame POS-TARG POS-TARG Pattern_Orient 41.788 0 Angle_Between_Sides Center_Pattern NO NO Pattern_Comments: This is an attempt at a 6 point pattern described: http://www.stsci.edu/itt/review/DrizzlePac/HTML/AppendixC3.html "Forming a six-point dither3, however, is less clear; a calculation suggests that crossing the linear three point dither, described above, with a (1/2, 0) two-point dither is the optimal strategy. For square pixels, the half-pixel dither could be taken in either direction. But WFC3 IR pixels are slightly longer in the x-direction, so the dither should be performed along the x-axis." ------------------------------------------------------------------------------------------------------------------------------------ 15192( 5) - 07-Mar-2018 22:18:14 - [ 6] Patterns ------------------------------------------------------------------------------------------------------------------------------------ Pattern_Number: 4 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_Number: 5 Primary_Pattern Secondary_Pattern Pattern_Type LINE LINE Pattern_Purpose DITHER DITHER Number_Of_Points 3 2 Point_Spacing 0.135 0.0198 Line_Spacing Coordinate_Frame POS-TARG POS-TARG Pattern_Orient 46.84 0.0 Angle_Between_Sides Center_Pattern NO NO Pattern_Comments: This is supposed to be a 6 point dither as described in: http://documents.stsci.edu/hst/HST_overview/documents/DrizzlePac/AppendixC3.html This is for UVIS. ------------------------------------------------------------------------------------------------------------------------------------ 15192( 5) - 07-Mar-2018 22:18:14 - [ 7] Visit: 01 (Seventh Epoch (1st Visit)) Visit Requirements: ORIENT 205D TO 230 D; BETWEEN 01-MAR-2018:00:00:00 AND 31-MAR-2018:00:00:00; ON HOLD On Hold Comments: Because of earth glow, orbits will need to be adjusted shortly before execution when sky brightness plots can be made. Additional Comments: 13 orbits were not schedulable together, so we had to split the epoch into at least two visits. However, only up to 6 orbits are schedulable together, so we had to schedule three visits. 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 SN-2011FE-U WFC3/UVI ACCUM UVIS F555W 1 1050 S GS ACQ SCENARIO BASE1B3; VIS S (6300 S) PATTERN 5 1-4; PAR 2 WITH 1 ------------------------------------------------------------------------------------------------------------------------------------ 2 ANY ACS/WFC ACCUM WFC F814W 2 410 S see below (5262 S) ------------------------------------------------------------------------------------------------------------------------------------ 3 SN-2011FE-U WFC3/UVI ACCUM UVIS F600LP 1 1800 S PAR 4 WITH 3 VIS S see below (11496 S) ------------------------------------------------------------------------------------------------------------------------------------ 4 ANY ACS/WFC ACCUM WFC F814W 3 400 S see below (8904 S) ------------------------------------------------------------------------------------------------------------------------------------ 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 | ------------------------------------------------------------------------------------------------------------------------------------ SN-2011FE-UVIS 1 WFC3/UVI ACCUM UVIS F555W 1 1 none none 1 N/A S SN-2011FE-UVIS 1 WFC3/UVI ACCUM UVIS F555W 1 2 none none 2 N/A S SN-2011FE-UVIS 1 WFC3/UVI ACCUM UVIS F555W 2 1 none none 3 N/A S SN-2011FE-UVIS 1 WFC3/UVI ACCUM UVIS F555W 2 2 none none 4 N/A S SN-2011FE-UVIS 1 WFC3/UVI ACCUM UVIS F555W 3 1 none none 5 N/A S SN-2011FE-UVIS 1 WFC3/UVI ACCUM UVIS F555W 3 2 none none 6 N/A S ANY 2 ACS/WFC ACCUM WFC F814W 1 1 1 none 1 426.0 S ANY 2 ACS/WFC ACCUM WFC F814W 1 1 2 none 1 426.0 S ANY 2 ACS/WFC ACCUM WFC F814W 1 2 1 none 2 441.0 S ANY 2 ACS/WFC ACCUM WFC F814W 1 2 2 none 2 441.0 S ANY 2 ACS/WFC ACCUM WFC F814W 2 1 1 none 3 441.0 S 15192( 5) - 07-Mar-2018 22:18:14 - [ 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 | ------------------------------------------------------------------------------------------------------------------------------------ ANY 2 ACS/WFC ACCUM WFC F814W 2 1 2 none 3 441.0 S ANY 2 ACS/WFC ACCUM WFC F814W 2 2 1 none 4 441.0 S ANY 2 ACS/WFC ACCUM WFC F814W 2 2 2 none 4 441.0 S ANY 2 ACS/WFC ACCUM WFC F814W 3 1 1 none 5 441.0 S ANY 2 ACS/WFC ACCUM WFC F814W 3 1 2 none 5 441.0 S ANY 2 ACS/WFC ACCUM WFC F814W 3 2 1 none 6 441.0 S ANY 2 ACS/WFC ACCUM WFC F814W 3 2 2 none 6 441.0 S SN-2011FE-UVIS 3 WFC3/UVI ACCUM UVIS F600LP 1 1 none none 1 1821.0 S S SN-2011FE-UVIS 3 WFC3/UVI ACCUM UVIS F600LP 1 2 none none 2 1935.0 S S SN-2011FE-UVIS 3 WFC3/UVI ACCUM UVIS F600LP 2 1 none none 3 1935.0 S S SN-2011FE-UVIS 3 WFC3/UVI ACCUM UVIS F600LP 2 2 none none 4 1935.0 S S SN-2011FE-UVIS 3 WFC3/UVI ACCUM UVIS F600LP 3 1 none none 5 1935.0 S S SN-2011FE-UVIS 3 WFC3/UVI ACCUM UVIS F600LP 3 2 none none 6 1935.0 S S ANY 4 ACS/WFC ACCUM WFC F814W 1 1 1 none 1 463.0 S ANY 4 ACS/WFC ACCUM WFC F814W 1 1 2 none 1 463.0 S ANY 4 ACS/WFC ACCUM WFC F814W 1 1 3 none 1 463.0 S ANY 4 ACS/WFC ACCUM WFC F814W 1 2 1 none 2 501.0 S ANY 4 ACS/WFC ACCUM WFC F814W 1 2 2 none 2 501.0 S ANY 4 ACS/WFC ACCUM WFC F814W 1 2 3 none 2 501.0 S ANY 4 ACS/WFC ACCUM WFC F814W 2 1 1 none 3 501.0 S ANY 4 ACS/WFC ACCUM WFC F814W 2 1 2 none 3 501.0 S ANY 4 ACS/WFC ACCUM WFC F814W 2 1 3 none 3 501.0 S ANY 4 ACS/WFC ACCUM WFC F814W 2 2 1 none 4 501.0 S ANY 4 ACS/WFC ACCUM WFC F814W 2 2 2 none 4 501.0 S ANY 4 ACS/WFC ACCUM WFC F814W 2 2 3 none 4 501.0 S ANY 4 ACS/WFC ACCUM WFC F814W 3 1 1 none 5 501.0 S ANY 4 ACS/WFC ACCUM WFC F814W 3 1 2 none 5 501.0 S ANY 4 ACS/WFC ACCUM WFC F814W 3 1 3 none 5 501.0 S ANY 4 ACS/WFC ACCUM WFC F814W 3 2 1 none 6 501.0 S ANY 4 ACS/WFC ACCUM WFC F814W 3 2 2 none 6 501.0 S ANY 4 ACS/WFC ACCUM WFC F814W 3 2 3 none 6 501.0 S 15192( 5) - 07-Mar-2018 22:18:14 - [ 9] Visit: 02 (Seventh Epoch (3rd Visit)) Visit Requirements: ORIENT 205D TO 230 D; BETWEEN 01-MAR-2018:00:00:00 AND 31-MAR-2018:00:00:00; ON HOLD ; VISIBILITY INTERVAL 65.58 M On Hold Comments: Because of earth glow, orbits will need to be adjusted shortly before execution when sky brightness plots can be made. Additional Comments: 13 orbits were not schedulable together, so we had to split the epoch into at least two visits. However, only up to 6 orbits are schedulable together, so we had to schedule three visits. 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 SN-2011FE-I WFC3/IR MULTIAC IR F110W SAMP-SEQ=SPARS200, NSAMP=8 1 DEF GS ACQ SCENARIO BASE1B3; R CUM (5611.731 PATTERN 2 1-4; PAR 2 S) WITH 1 ------------------------------------------------------------------------------------------------------------------------------------ 2 ANY ACS/WFC ACCUM WFC F658N 1 1490 S see below (5770 S) ------------------------------------------------------------------------------------------------------------------------------------ 3 SN-2011FE-I WFC3/IR MULTIAC IR F160W SAMP-SEQ=SPARS200, NSAMP=11 1 DEF PAR 4 WITH 3 R CUM (8011.732 S) ------------------------------------------------------------------------------------------------------------------------------------ 4 ANY ACS/WFC ACCUM WFC F435W 1 1000 S see below (7423 S) ------------------------------------------------------------------------------------------------------------------------------------ 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 | ------------------------------------------------------------------------------------------------------------------------------------ SN-2011FE-IR 1 WFC3/IR MULTIAC IR F110W 1 none none none 1 N/A CUM SN-2011FE-IR 1 WFC3/IR MULTIAC IR F110W 2 none none none 2 N/A CUM SN-2011FE-IR 1 WFC3/IR MULTIAC IR F110W 3 none none none 3 N/A CUM SN-2011FE-IR 1 WFC3/IR MULTIAC IR F110W 4 none none none 4 N/A CUM ANY 2 ACS/WFC ACCUM WFC F658N 1 none none none 1 1336.0 S ANY 2 ACS/WFC ACCUM WFC F658N 2 none none none 2 1478.0 S ANY 2 ACS/WFC ACCUM WFC F658N 3 none none none 3 1478.0 S ANY 2 ACS/WFC ACCUM WFC F658N 4 none none none 4 1478.0 S SN-2011FE-IR 3 WFC3/IR MULTIAC IR F160W 1 none none none 1 N/A CUM SN-2011FE-IR 3 WFC3/IR MULTIAC IR F160W 2 none none none 2 N/A CUM 15192( 5) - 07-Mar-2018 22:18:14 - [ 10] 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 | ------------------------------------------------------------------------------------------------------------------------------------ SN-2011FE-IR 3 WFC3/IR MULTIAC IR F160W 3 none none none 3 N/A CUM SN-2011FE-IR 3 WFC3/IR MULTIAC IR F160W 4 none none none 4 N/A CUM ANY 4 ACS/WFC ACCUM WFC F435W 1 none none none 1 1855.0 S ANY 4 ACS/WFC ACCUM WFC F435W 2 none none none 2 1856.0 S ANY 4 ACS/WFC ACCUM WFC F435W 3 none none none 3 1856.0 S ANY 4 ACS/WFC ACCUM WFC F435W 4 none none none 4 1856.0 S 15192( 5) - 07-Mar-2018 22:18:14 - [ 11] Visit: 03 (Seventh Epoch (2nd Visit)) Visit Requirements: ORIENT 205D TO 230 D; BETWEEN 01-MAR-2018:00:00:00 AND 31-MAR-2018:00:00:00; ON HOLD On Hold Comments: Because of earth glow, orbits will need to be adjusted shortly before execution when sky brightness plots can be made. Additional Comments: 13 orbits were not schedulable together, so we had to split the epoch into at least two visits. However, only up to 6 orbits are schedulable together, so we had to schedule three visits. 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 SN-2011FE-U WFC3/UVI ACCUM UVIS F438W 1 1400 S GS ACQ SCENARIO BASE1B3; VIS S see below PATTERN 5 1-2; PAR 2 (8950 S) WITH 1 ------------------------------------------------------------------------------------------------------------------------------------ 2 ANY ACS/WFC ACCUM WFC F555W 2 410 S see below (7584 S) ------------------------------------------------------------------------------------------------------------------------------------ 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 | ------------------------------------------------------------------------------------------------------------------------------------ SN-2011FE-UVIS 1 WFC3/UVI ACCUM UVIS F438W 1 1 none none 1 1444.0 S S SN-2011FE-UVIS 1 WFC3/UVI ACCUM UVIS F438W 1 2 none none 1 1444.0 S S SN-2011FE-UVIS 1 WFC3/UVI ACCUM UVIS F438W 2 1 none none 2 1515.0 S S SN-2011FE-UVIS 1 WFC3/UVI ACCUM UVIS F438W 2 2 none none 2 1516.0 S S SN-2011FE-UVIS 1 WFC3/UVI ACCUM UVIS F438W 3 1 none none 3 1515.0 S S SN-2011FE-UVIS 1 WFC3/UVI ACCUM UVIS F438W 3 2 none none 3 1516.0 S S ANY 2 ACS/WFC ACCUM WFC F555W 1 1 1 none 1 610.0 S ANY 2 ACS/WFC ACCUM WFC F555W 1 1 2 none 1 610.0 S ANY 2 ACS/WFC ACCUM WFC F555W 1 2 1 none 1 590.0 S ANY 2 ACS/WFC ACCUM WFC F555W 1 2 2 none 1 590.0 S ANY 2 ACS/WFC ACCUM WFC F555W 2 1 1 none 2 670.0 S ANY 2 ACS/WFC ACCUM WFC F555W 2 1 2 none 2 670.0 S ANY 2 ACS/WFC ACCUM WFC F555W 2 2 1 none 2 626.0 S ANY 2 ACS/WFC ACCUM WFC F555W 2 2 2 none 2 626.0 S ANY 2 ACS/WFC ACCUM WFC F555W 3 1 1 none 3 670.0 S ANY 2 ACS/WFC ACCUM WFC F555W 3 1 2 none 3 670.0 S ANY 2 ACS/WFC ACCUM WFC F555W 3 2 1 none 3 626.0 S ANY 2 ACS/WFC ACCUM WFC F555W 3 2 2 none 3 626.0 S 15192( 5) - 07-Mar-2018 22:18:14 - [ 12] Summary Form for Proposal 15192 Item Used in this proposal ------------------------------------------------------------------------------------------------------------------------------------ Apertures IR, UVIS, WFC ------------------------------------------------------------------------------------------------------------------------------------ Configurations ACS/WFC, WFC3/IR, WFC3/UVIS ------------------------------------------------------------------------------------------------------------------------------------ Opmodes ACCUM, MULTIACCUM ------------------------------------------------------------------------------------------------------------------------------------ Optional Parameters NSAMP=11, NSAMP=8, SAMP-SEQ=SPARS200 ------------------------------------------------------------------------------------------------------------------------------------ Special Requirements BETWEEN 01-MAR-2018:00:00:00 AND 31-MAR-2018:00:00:00, GS ACQ SCENARIO BASE1B3, ON HOLD , ORIENT 205D TO 230 D, PAR 2 WITH 1, PAR 4 WITH 3, PATTERN 2 1-4, PATTERN 5 1-2, PATTERN 5 1-4, VISIBILITY INTERVAL 65.58 M ------------------------------------------------------------------------------------------------------------------------------------ Spectral Elements F110W, F160W, F435W, F438W, F555W, F600LP, F658N, F814W ------------------------------------------------------------------------------------------------------------------------------------ Target Names ANY, SN-2011FE-IR, SN-2011FE-UVIS ------------------------------------------------------------------------------------------------------------------------------------