0 Assigned ID: 379 ----- Attempting Submission 1 (Fri Apr 11 06:31:34 GMT 2014) ----- HST Phase I Proposal 379 (SN2011fe.apt) successfully submitted. ----- Attempting Submission 2 (Fri Apr 11 20:28:51 GMT 2014) ----- HST Phase I Proposal 379 (SN2011fe.apt) successfully submitted. ----- Attempting Submission 3 (Fri Apr 11 23:28:43 GMT 2014) ----- HST Phase I Proposal 379 (SN2011fe.apt) successfully submitted. 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 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 PATTERN AND COORDINATED PARALLEL MISMATCH PATTERN AND COORDINATED PARALLEL MISMATCH PATTERN AND COORDINATED PARALLEL MISMATCH There is a warning (which appears multiple times. I contacted my program coordinator (Crystal Mannfolk), and I was told that I could ignore them. Also, the exposure times for the second and third epochs of observations will depend on what the first epoch reveals. Thus, I put a hold on the later observations. ############ Resubmition Dec 23 2014 ############## I have changed the exposure times slightly based on the first epoch of observations. ############ Resubmition Mar 17 2015 ############## ############ Resubmition Mar 17 2015 (2nd) ############## When analyzing the first epoch further it was realized that CTE were negatively impactign the F438W exposure. Post-flash have been added to WFC3 F438W and ACS F435W, F555W, and F658N. ############ Resubmition Mar 17 2015 (2nd) ############## The ACS team caught an error when using the ACS ETC. ACS only needs post-flash on F658N (not F435W, F555W). ############ Resubmition May 6 2015 ############## The 3rd epochs exposure times have been adjusted, and only the parallel ACS F658N exposure need flashed now because the exposure times are longer exposures for this epoch. 1154922440 ----- Attempting Submission 1 (Fri Jul 25 19:01:29 GMT 2014) ----- ----- Attempting Submission 2 (Wed Dec 24 00:26:23 GMT 2014) ----- ----- Attempting Submission 3 (Tue Mar 17 17:45:28 GMT 2015) ----- HST Phase II Proposal 13737 (SN2011fe.apt) successfully submitted. Receipt: # 13737-3 ----- Attempting Submission 4 (Tue Mar 17 20:29:16 GMT 2015) ----- HST Phase II Proposal 13737 (SN2011fe.apt) successfully submitted. Receipt: # 13737-4 ----- Attempting Submission 5 (Wed May 06 23:47:33 GMT 2015) ----- There is a warning (which appears multiple times). I contacted my program coordinator (Crystal Mannfolk), and I was told that I could ignore them. 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. Due to nucleosynthetic effects during explosion, single and double degenerate SNe Ia models are predicted to produce vastly differing amounts 57Co and 55Fe. 57Co and 55Fe dominate the power of the very late time light curves of SNe Ia at ~1050 days and ~1500 after the initial explosion, respectively. Broad band 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 powered lightcurve to a 57Co powered one. These observations will place unique constraints on progenitor systems of SNe Ia. SN 2011fe 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 because this measurement will not be possible next cycle for SN 2011fe. 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 Regular 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. 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 F850LP 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 WFC3/UVIS Imaging No No F438W WFC3/UVIS Imaging No No F555W WFC3/UVIS Imaging No No F850LP 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 WFC3/UVIS Imaging No No F438W WFC3/UVIS Imaging No No F555W WFC3/UVIS Imaging No No F850LP 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 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 1430955986646 The scheduling data was generated by CASM 23.0. CASM was run in Phase II mode. /tmp/OPVisit7831962058255998781.xml 1412818283000 18.6844767751559 (Tic-Visit :proposal-id 13737 :visit-id "01" :proposal-version -1 :trans-version "20150128" :date "06-May-2015 16:46:24.0" :trans-errors '(:WARNINGS 5 :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 8169552 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 13737 :visit-id "01" :obset-id "01" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 13737 :visit-id "01" :orbit-number 1 :pcs-time 333 :si-vis-utilization 3076 :al-overhead-at-end 116 :internal-dur-at-end 668 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3409 :pcs-gap 0 ) (Tic-Orbit :proposal-id 13737 :visit-id "01" :orbit-number 2 :pcs-time 222 :si-vis-utilization 3187 :al-overhead-at-end 116 :internal-dur-at-end 668 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3409 :pcs-gap 0 ) (Tic-Orbit :proposal-id 13737 :visit-id "01" :orbit-number 3 :pcs-time 222 :si-vis-utilization 3187 :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 3409 :pcs-gap 0 ) (Tic-Orbit :proposal-id 13737 :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 3409 :pcs-gap 0 ) true 4 0 1430955994094 The scheduling data was generated by CASM 23.0. CASM was run in Phase II mode. /tmp/OPVisit8366033605471180794.xml Needed to reduce the last parallel exposure on the 4th orbit to make the 5th orbit not need a buffer dump. 1428300229000 178.0 (Tic-Visit :proposal-id 13737 :visit-id "02" :proposal-version -1 :trans-version "20150128" :date "06-May-2015 16:46:31.0" :trans-errors '(:WARNINGS 4 :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 9022240 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 13737 :visit-id "02" :obset-id "02" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 13737 :visit-id "02" :orbit-number 1 :pcs-time 333 :si-vis-utilization 3076 :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 3409 :pcs-gap 0 ) (Tic-Orbit :proposal-id 13737 :visit-id "02" :orbit-number 2 :pcs-time 222 :si-vis-utilization 3187 :al-overhead-at-end 110 :internal-dur-at-end 0 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3409 :pcs-gap 0 ) (Tic-Orbit :proposal-id 13737 :visit-id "02" :orbit-number 3 :pcs-time 222 :si-vis-utilization 3187 :al-overhead-at-end 116 :internal-dur-at-end 0 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3409 :pcs-gap 0 ) (Tic-Orbit :proposal-id 13737 :visit-id "02" :orbit-number 4 :pcs-time 222 :si-vis-utilization 3187 :al-overhead-at-end 116 :internal-dur-at-end 347 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3409 :pcs-gap 0 ) (Tic-Orbit :proposal-id 13737 :visit-id "02" :orbit-number 5 :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 3409 :pcs-gap 0 ) true 5 0 Added 5 e- flash to avoid CTE effects. ETC estimated an electron count of 7.6 e- given the filter, exp time, RA and Dec, and rough date of the exposures. Added 15 e- flash to avoid CTE effects. ETC estimated an electron count of 5.9 e- given the filter, exp time, RA and Dec, and rough date of the exposures. 1430948005349 The scheduling data was generated by CASM 23.0. CASM was run in Phase II mode. /home/shappee/Research/Proposals/HST/Cycle22/OP-cache/SN2011fe-v03.xml 7 orbits were not schedulable together, so we had to split the thrid epoch into two visits. (Tic-Visit :proposal-id 13737 :visit-id "03" :proposal-version -1 :trans-version "20150128" :date "06-May-2015 14:33:25.0" :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 4583760 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 13737 :visit-id "03" :obset-id "03" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 13737 :visit-id "03" :orbit-number 1 :pcs-time 333 :si-vis-utilization 3076 :al-overhead-at-end 115 :internal-dur-at-end 0 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3409 :pcs-gap 0 ) (Tic-Orbit :proposal-id 13737 :visit-id "03" :orbit-number 2 :pcs-time 222 :si-vis-utilization 3187 :al-overhead-at-end 115 :internal-dur-at-end 0 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3409 :pcs-gap 0 ) (Tic-Orbit :proposal-id 13737 :visit-id "03" :orbit-number 3 :pcs-time 222 :si-vis-utilization 3187 :al-overhead-at-end 115 :internal-dur-at-end 0 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3409 :pcs-gap 0 ) (Tic-Orbit :proposal-id 13737 :visit-id "03" :orbit-number 4 :pcs-time 222 :si-vis-utilization 3187 :al-overhead-at-end 115 :internal-dur-at-end 699 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3409 :pcs-gap 0 ) true 4 0 The exposure times for the third visit will be adjusted depending on the second visits observations. It is not possible to know the SED at these times because no SN Ia has been observed this late. 1430955241267 The scheduling data was generated by CASM 23.0. CASM was run in Phase II mode. /home/shappee/Research/Proposals/HST/Cycle22/OP-cache/SN2011fe-v04.xml 7 orbits were not schedulable together, so we had to split the thrid epoch into two visits. Needed to reduce the last parallel exposure on the 4th orbit to make the 5th orbit not need a buffer dump. (Tic-Visit :proposal-id 13737 :visit-id "04" :proposal-version -1 :trans-version "20150128" :date "06-May-2015 16:33:59.0" :trans-errors '(:WARNINGS 2 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 3 :saa-model "29" :si-bright-earth-limb-angle 20.0 :data-volume 4438480 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 13737 :visit-id "04" :obset-id "04" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 13737 :visit-id "04" :orbit-number 1 :pcs-time 333 :si-vis-utilization 3076 :al-overhead-at-end 71 :internal-dur-at-end 0 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3409 :pcs-gap 0 ) (Tic-Orbit :proposal-id 13737 :visit-id "04" :orbit-number 2 :pcs-time 222 :si-vis-utilization 3187 :al-overhead-at-end 116 :internal-dur-at-end 31 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3409 :pcs-gap 0 ) (Tic-Orbit :proposal-id 13737 :visit-id "04" :orbit-number 3 :pcs-time 222 :si-vis-utilization 3187 :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 3409 :pcs-gap 0 ) true 3 0 The exposure times for the third visit will be adjusted depending on the second visits observations. It is not possible to know the SED at these times because no SN Ia has been observed this late. Added 15 e- flash to avoid CTE effects. ETC estimated an electron count of 5.5 e- given the filter, adjusted exp time of each exposure, RA and Dec, and rough date of the exposures. Added 13 e- flash to avoid CTE effects. ETC estimated an electron count of 7 e- given the filter of each exposure, adjusted exp time, RA and Dec, and rough date of the exposures.