0 Assigned ID: 423 ----- Attempting Submission 1 (Fri Apr 10 10:32:31 GMT 2015) ----- HST Phase I Proposal 423 (SN2011fe_Cycle23.apt) successfully submitted. Receipt: # 423-1 ----- Attempting Submission 2 (Fri Apr 10 22:21:17 GMT 2015) ----- HST Phase I Proposal 423 (SN2011fe_Cycle23.apt) successfully submitted. Receipt: # 423-2 ----- Attempting Submission 3 (Fri Apr 10 23:45:09 GMT 2015) ----- HST Phase I Proposal 423 (SN2011fe_Cycle23.apt) successfully submitted. Receipt: # 423-3 This target is not used in this proposal. This pattern is not used in this proposal. This pattern is not used in this proposal. This pattern is not used in this proposal. PATTERN AND COORDINATED PARALLEL MISMATCH PATTERN AND COORDINATED PARALLEL MISMATCH PATTERN AND COORDINATED PARALLEL MISMATCH PATTERN AND COORDINATED PARALLEL MISMATCH PATTERN AND COORDINATED PARALLEL MISMATCH Resubmission Aug 25, 2016 I have expanded the NIR visit visibility time to fill orbits on Sept. 27. This was done to be able to specify when in the orbit F110W would be observed. I have also put the F110W observations at the end of each orbit when HeI would not contaminate that filter's observations. This has required not using a pattern, so I have (attempted) to use POS TARG to construct a 6 pointed dither. Each orbit has two points of the dither. To put F110W completely at the end of each orbit, the dithers in each orbit follow an ABBA pattern so that only two repointings need to be made per orbit. -------------------- Resubmission July 15, 2016 I have adjusted the exposure times based on the 4th epoch's photometry. The only thing left is to worry about the Time-varying Excess Earth-glow again for the F110W photometry. ------------------------------------------- Resubmission Jan 4, 2016 I have corrected the POS-TARG (I had the offsets in pixel units not arcsec) as suggested by Crystal Mannfolk. -------- Resubmission Jan 1, 2016 I have rearrnged the last orbit of Visit 1 (Fourth Epoch) so that the two F110W exposures are during the middle of the orbit so they are in the darkest portion of the orbit as recommended by Crystal Mannfolk. I have also cut done the timing requirements so that the two F110W exposures would not cut into the bright time of those orbits. -------- Resubmission Oct 29, 2015 I have crsplit=2 the full orbit F435W exposures as recommended by the Susana Deustua. -------- Resubmission Jul 28, 2015 1) Fixed the overrun by increasing visiability interval by 3 seconds on the 01 and 03 visits. I used the visit planner to make sure the observations are still schedulable. I then adjusted other exposure times to use this 3 seconds. This is needed because cutting down the IR observations to not have that 3 second overrun caused a realitively large amount of unused time. 2) Changed orients to 261-271 for the 01 visit as recommended by Crystal. ________________ I have 2 orbits with a 3 second overrun. I have had the same orbit plan for this object last cycle before without problem. Do I need to correct this? I have been advised to ignore the "pattern and coordinated parralel mismatch" before, I assume this is still not a problem. 02 and 03 are on hold for the results of 01 since it is unknown what the SED of a supernova at these late times should be and I will adjust the exposure times accordingly. -1293510283 ----- Attempting Submission 1 (Thu Jul 23 23:50:35 GMT 2015) ----- HST Phase II Proposal 14166 (SN2011fe_Cycle23.apt) successfully submitted. Receipt: # 14166-1 ----- Attempting Submission 2 (Tue Jul 28 17:04:37 GMT 2015) ----- HST Phase II Proposal 14166 (SN2011fe_Cycle23.apt) successfully submitted. Receipt: # 14166-2 ----- Attempting Submission 3 (Thu Oct 29 23:52:21 GMT 2015) ----- HST Phase II Proposal 14166 (SN2011fe_Cycle23.apt) successfully submitted. Receipt: # 14166-3 ----- Attempting Submission 4 (Sat Jan 02 06:35:52 GMT 2016) ----- HST Phase II Proposal 14166 (SN2011fe_Cycle23.apt) successfully submitted. Receipt: # 14166-4 ----- Attempting Submission 5 (Mon Jan 04 17:44:46 GMT 2016) ----- ----- Attempting Submission 7 (Tue Jul 19 19:53:23 GMT 2016) ----- ----- Attempting Submission 8 (Fri Aug 26 03:56:53 GMT 2016) ----- I have been advised to ignore the "pattern and coordinated parralel mismatch" before, I assume this is still not a problem. Even though SNe Ia are crucial to cosmological studies as distance indicators, the exact nature of these systems remains theoretically ambiguous and observationally elusive. However, there is a new hope. The very late-time lightcurves 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 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 56Co to a 57Co 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 1300 days and a factor of a million in flux, is likely to remain the best studied normal SN Ia of our generation and if these observations are not made this cycle, they will likely never be done with Hubble. The goal of this proposal is to construct a quasi-bolometric light curve for the evolving transient, where the spectrum consists of (predominantly) line emission over a very broad range of wavelengths other than the UV (where there is little emission). We selected the F438W ($B$), F555W ($V$) and F600LP ($R + I$) filters for WFC3/UVIS and F110W ($YJ$) 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\AA\ with no gaps and relatively uniform throughput. Our ground-based spectroscopy and photometry show there is little flux blueward of 4000 \AA{} so we forgo the F336W ($U$) and UV filters. 2) A single long pass filter would not be sufficient. Since the shape of the SN spectral energy distribution is known to be changing with ionization (\citealp{mcclelland13}, Shappee et al. in prep.), computing the bolometric luminosity with a single F350LP observation would be prone to a large uncertainties. Instead, we decided to use individual broad band filters to retain some spectral information without the added expense of taking a spectrum. Without this information, we could mistake a change in ionization state for a change in the bolometric luminosity. 3) Finally, the optical filter combination also attempts to evenly partition the optical energy. In the spectrum obtained $850$ days after $t_{B {\rm max}}$, the wave-length ranges covered by $B$, $V$, $R$, and $I$, contained 48\%, 37\%, 21\%, 19\% of the optical energy.\footnote{The wave-length ranges covered by the Bessel filters have overlap, so the sum is greater than one.} Thus we have kept $B$ and $V$ as separate filters but F600LP covers both the $R$ and $I$ wave-length ranges. Finally, we considered also asking for Spitzer observations, but SN~2011fe will be much too faint for mid-IR observations. We estimated the number of orbits and exposures needed for our program using the depth requirements needed to distinguish between the models shown and Figure \ref{fig:lightcurve} and recommendations in the HST Primer. We propose obtaining 3 epochs separated by approximately 160 days to well-sample the transition in powering isotopes. The required exposure times in the optical are determined by first fitting the \citet{roepke12} models to the ground-based LBT data. To be conservative, we then take the fainter model as our fiducial model. The NIR, however, is not as simple because SN~2011fe has become too faint for ground-based observations. Here we base our exposure time calculations as if the NIR ($1.0$--$1.7 \mu$m) had $10\%$ the flux as the optical ($4000$--$10000$ \AA). If we detect nothing, we will know that the NIR is unimportant, otherwise we will have a measure of its contribution as well. It is also important to note that because our measurement is the difference between points on the bolometric light curve, both the earlier and later observations with contribute to the statistical uncertainty in our measurement. Thus, it does not make sense to require the same signal-to-noise ratio (SNR) for the early observations, where it is inexpensive to increase the obtained SNR, and the later observations, where it is significantly more expensive to do so. Thus, we lower our required SNR as the SN fades. We require a SNR of 15, 12, and 10 for the optical filters and 10, 5, and 3 for the NIR upper limits for the 1st, 2nd, and 3rd epochs, respectively. There is also the concern that crowding and confusion may inhibit our measurement. Luckily, SN~2011fe exploded in a sparse region of the outer disk of M101 where archival pre-explosion HST images existed. \citet{li11} 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 $2 \sigma$ upper limits of F435W $<27.87$, F555W $< 27.49$, and F814W $< 26.81$ at its position. These limits are more than a magnitude fainter than SN~2011fe is expected during our last epoch.\footnote{It is important to note that these limits were placed with F435W, F555W, and F814W exposure times of 900, 720, and 720 seconds, respectively. This raises the question:~~why are the proposed exposure times so much longer? The reason is these limits are simply for a detection (SNR $\sim 1$), whereas our SNR requirements are much more stringent.} We then used the exposure time calculator to estimate the length of our required observations. Since zodiacal light is a significant background for the last epoch of observations we have slightly altered our requested date to take advantage of minimum of zodiacal light in the direction of M~101. The exposure time calculations for all of the observations include both their dates and coordinates to ensure that our estimated times are accurate. The estimates are also based on the observed optical spectra of SN~2011fe taken $850$ days after $t_{B {\rm max}}$ which is calibrated to the expected broad-band magnitudes for each epoch. Given the above constraints, the approximate exposure times we request for the first epoch in each filter are $3\times500$ sec in F438W, $3\times400$ sec in F555W, $3\times1500$ sec in F600LPW, $2\times1000$ sec in F110W, and $2\times950$ sec in F160W. The approximate exposure times we request for the second epoch in each filter are $3\times850$ sec in F438W, $3\times700$ sec in F555W, $3\times1900$ sec in F600LPW, $2\times1000$ sec in F110W, and $2\times950$ sec in F160W. Finally, the approximate exposure times we request for the third epoch in each filter are $3\times1200$ sec in F438W, $3\times1200$ sec in F555W, $3\times3025$ sec in F600LPW, $2\times1075$ sec in F110W, and $2\times1075$ sec in F160W. Because of the charge transfer effects of WFC3 when there are few background photons, we will probably use the pre-flash mode for the first two epochs with 438 and 555. This can, however, be settled in Phase 2 and does not affect our current exposure time requirements. No SN Ia has ever been observed at these epochs, so changes in the ionization state of SN~2011fe are possible and can not be predicted. This could conceivably significantly change what filters receive the largest portion of the SN flux. Thus, we plan to measure the light-curve of SN~2011fe soon after each observation is completed and use these measurements to inform how we distribute the next epoch's orbits among the filters. 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, M~101 is an important nearby galaxy for many reasons. For example, \citet{shara13} have compiled a catalog of 10,000 Wolf-Rayet stars using extensive HST He II optical narrow-band imaging. There are also F435W/F555W/F814W mosaics covering most of the galaxy (GO 9490). We even have a study of Cepheids using archival ACS data that provides the distance which is currently popular for SN~2011fe (Shappee \& Stanek 2011) and 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 the Cepheid fields as well as on lower metallicity regions missed by the F435W/F555W/F814W mosaics. However, because M101 is such and interesting and large galaxy, a ACS parallel observation at any roll angle would be interesting. COSMOLOGY 0 false false false false false false SUPPORTED EXT-STAR SUPERNOVA TYPE IA This object was generated by the targetselector and retrieved from the SIMBAD database. J2000 J2000 EXT-STAR SUPERNOVA TYPE IA This object was generated by the targetselector and retrieved from the SIMBAD database. A is for F438W and F555W where CTE is more imporant so I put SN 2011fe closer to the edge. J2000 J2000 EXT-STAR SUPERNOVA TYPE IA This object was generated by the targetselector and retrieved from the SIMBAD database. J2000 J2000 EXT-STAR SUPERNOVA TYPE IA This object was generated by the targetselector and retrieved from the SIMBAD database. J2000 J2000 WFC3/UVIS Imaging No No F438W WFC3/UVIS Imaging No No F555W WFC3/UVIS Imaging No No F600LP WFC3/IR Imaging No No F110W WFC3/IR Imaging No No F160W ACS/WFC Imaging No No F555W ACS/WFC Imaging No No F814W ACS/WFC Imaging No No F435W ACS/WFC Imaging No No F658N WFC3/UVIS Imaging No No F438W WFC3/UVIS Imaging No No F555W WFC3/UVIS Imaging No No F600LP WFC3/IR Imaging No No F110W WFC3/IR Imaging No No F160W ACS/WFC Imaging No No F555W ACS/WFC Imaging No No F814W ACS/WFC Imaging No No F435W ACS/WFC Imaging No No F658N POS-TARG DITHER 0.135 LINE false false 3 46.84 WFC3-UVIS-DITHER-LINE-3PT 1 false POS-TARG DITHER 0.636 LINE false false 2 41.788 WFC3-IR-DITHER-LINE 2 false POS-TARG DITHER 0.173 LINE 0.112 false false 81.785 4 23.884 WFC3-UVIS-DITHER-BOX 3 false POS-TARG DITHER 0.572 LINE 0.365 false false 74.653 4 18.528 WFC3-IR-DITHER-BOX-MIN 4 false POS-TARG DITHER DITHER 2 0.605 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." LINE false false 0.06775 3 41.788 POS-TARG LINE 0 5 true POS-TARG DITHER DITHER 2 0.135 This is an attempt at a 6 point pattern for UVIS as 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. (I am choosing the x-direction.) LINE false false 0.021625 3 46.84 POS-TARG LINE 0 7 true 1472177668905 The scheduling data was generated by CASM 24.2. CASM was run in Phase II mode. 3406 /data1/teton/bshappee/Research/Proposals/HST/Cycle23/OP-cache/SN2011fe_Cycle23_long-v01.xml 1455874067000 261.0 (Tic-Visit :proposal-id 14166 :visit-id "01" :proposal-version -1 :trans-version "20160601" :date "25-Aug-2016 19:14:27.0" :trans-errors '(:WARNINGS 3 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 4 :saa-model "29" :si-bright-earth-limb-angle 20.0 :data-volume 7303344 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 14166 :visit-id "01" :obset-id "01" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 14166 :visit-id "01" :orbit-number 1 :pcs-time 333 :si-vis-utilization 3073 :al-overhead-at-end 120 :internal-dur-at-end 0 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3406.0 :pcs-gap 0 ) (Tic-Orbit :proposal-id 14166 :visit-id "01" :orbit-number 2 :pcs-time 222 :si-vis-utilization 3184 :al-overhead-at-end 120 :internal-dur-at-end 0 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3406.0 :pcs-gap 0 ) (Tic-Orbit :proposal-id 14166 :visit-id "01" :orbit-number 3 :pcs-time 222 :si-vis-utilization 3184 :al-overhead-at-end 120 :internal-dur-at-end 699 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3406.0 :pcs-gap 0 ) (Tic-Orbit :proposal-id 14166 :visit-id "01" :orbit-number 4 :pcs-time 222 :si-vis-utilization 3184 :al-overhead-at-end 0 :internal-dur-at-end 1056 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3406.0 :pcs-gap 0 ) true 4 0 Add post flash as was recommended. Add post flash as was recommended. 1472180409937 The scheduling data was generated by CASM 24.2. CASM was run in Phase II mode. /data1/teton/bshappee/Research/Proposals/HST/Cycle23/OP-cache/SN2011fe_Cycle23_long-v02.xml 9 orbits were not schedulable together, so we had to split the thrid epoch into two visits. (Tic-Visit :proposal-id 14166 :visit-id "02" :proposal-version -1 :trans-version "20160601" :date "25-Aug-2016 20:00:07.0" :trans-errors '(:WARNINGS 2 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 4 :saa-model "29" :si-bright-earth-limb-angle 20.0 :data-volume 6875648 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 14166 :visit-id "02" :obset-id "02" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 14166 :visit-id "02" :orbit-number 1 :pcs-time 333 :si-vis-utilization 3070 :al-overhead-at-end 116 :internal-dur-at-end 352 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3403 :pcs-gap 0 ) (Tic-Orbit :proposal-id 14166 :visit-id "02" :orbit-number 2 :pcs-time 222 :si-vis-utilization 3181 :al-overhead-at-end 116 :internal-dur-at-end 352 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3403 :pcs-gap 0 ) (Tic-Orbit :proposal-id 14166 :visit-id "02" :orbit-number 3 :pcs-time 222 :si-vis-utilization 3181 :al-overhead-at-end 116 :internal-dur-at-end 352 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3403 :pcs-gap 0 ) (Tic-Orbit :proposal-id 14166 :visit-id "02" :orbit-number 4 :pcs-time 222 :si-vis-utilization 3181 :al-overhead-at-end 116 :internal-dur-at-end 699 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3403 :pcs-gap 0 ) true 4 0 The exposure times for the third visit will be adjusted depending on the 1st visit's observations. It is not possible to know the SED at these times because no SN Ia has been observed this late. 1472183081534 The scheduling data was generated by CASM 24.2. CASM was run in Phase II mode. /tmp/OPVisit2974548560825632383.xml 86 9 orbits were not schedulable together, so we had to split the thrid epoch into two visits. I have extended the visibility window so that the F110W observations can be made at a specific portion of an orbit where there eath is not brightening the backgrounds. (Tic-Visit :proposal-id 14166 :visit-id "03" :proposal-version -1 :trans-version "20160601" :date "25-Aug-2016 20:44:38.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 5 :saa-model "29" :si-bright-earth-limb-angle 20.0 :data-volume 11819024 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 14166 :visit-id "03" :obset-id "03" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 14166 :visit-id "03" :orbit-number 1 :pcs-time 333 :si-vis-utilization 4827 :al-overhead-at-end 0 :internal-dur-at-end 0 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 5160.0 :pcs-gap 0 ) (Tic-Orbit :proposal-id 14166 :visit-id "03" :orbit-number 2 :pcs-time 222 :si-vis-utilization 4938 :al-overhead-at-end 0 :internal-dur-at-end 0 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 5160.0 :pcs-gap 0 ) (Tic-Orbit :proposal-id 14166 :visit-id "03" :orbit-number 3 :pcs-time 222 :si-vis-utilization 4938 :al-overhead-at-end 0 :internal-dur-at-end 65 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 5160.0 :pcs-gap 0 ) (Tic-Orbit :proposal-id 14166 :visit-id "03" :orbit-number 4 :pcs-time 222 :si-vis-utilization 4938 :al-overhead-at-end 116 :internal-dur-at-end 352 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 5160.0 :pcs-gap 0 ) (Tic-Orbit :proposal-id 14166 :visit-id "03" :orbit-number 5 :pcs-time 222 :si-vis-utilization 4490 :al-overhead-at-end 116 :internal-dur-at-end 699 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 5160.0 :pcs-gap 0 ) true 5 0 The exposure times for the third visit will be adjusted depending on the 1st visit's observations. It is not possible to know the SED at these times because no SN Ia has been observed this late.