0Assigned ID: 628
----- Attempting Submission 1 (Fri Apr 08 17:43:22 GMT 2016) -----The number of orbits used exceeds the number allocatedFollowing approval by the TTRB, I have added visit 14, labeled "SN 2015F (06A)". This is one orbit in F625W, to account for not splitting visit 06 between F555W and F625W.
To allow for a longer schedubility window, I don't pack the orbit completely. This leaves ~12 days, June 26 - July 08, during which this extra visit can be scheduled.
As visit 06 will now be devoted to F555W, it would be best to devote all of the extra visit 06A to F625W, as the supernova may be too faint to catch with just a 1/2 orbit in the filter.-1715059945----- Attempting Submission 1 (Wed Jul 20 14:42:32 GMT 2016) -----
----- Attempting Submission 4 (Thu Oct 06 18:30:26 GMT 2016) -----
----- Attempting Submission 5 (Wed Nov 16 16:30:41 GMT 2016) -----
----- Attempting Submission 6 (Tue Jan 03 21:18:54 GMT 2017) -----
----- Attempting Submission 7 (Mon Feb 27 17:12:43 GMT 2017) -----
----- Attempting Submission 8 (Mon Apr 10 18:20:25 GMT 2017) -----
----- Attempting Submission 9 (Tue Apr 25 15:17:15 GMT 2017) -----
----- Attempting Submission 11 (Wed Jun 14 15:44:51 GMT 2017) -----
----- Attempting Submission 12 (Thu Jun 15 21:52:43 GMT 2017) -----Following approval by the TTRB, I have added one more orbit (in the new visit 14).Going gently into the night: constraining Type Ia supernova nucleosynthesis using late-time photometryWe propose to use WFC3 photometry to construct the optical light curves of the nearby Type Ia supernovae SN 2015F and ASASSN-14lp at late times (>500 days after maximum light). These light curves will allow us to conduct a fundamental test of the theoretically predicted behavior of Type Ia supernova light curves at late times. We will observationally determine whether the nuclear physics of Type Ia supernova ejecta are solely determined by the radioactive decay of 56Co to 56Fe, or whether (and by how much) other nuclear heating mechanisms (such as the leptonic decays of 57Co) become discernible, as predicted. The spatial resolution of HST+WFC3 is crucial to the success of this experiment. At these late times, the fading supernovae are as bright as other surrounding objects (bright stars, star clusters), which would dominate the point-spread functions of ground-based observatories. Due to the rarity of nearby Type Ia supernovae, this experiment will double the sample of supernovae for which this experiment has been conducted and cut the uncertainty on the results by half. Moreover, if this experiment is not conducted in Cycle 24, it is highly unlikely that we would be able to perform it again during the remaining lifetime of HST.We propose to observe the late-time light curves of two Type Ia supernovae (SNe Ia) with WFC3. Due to HST's visibility constraints, we will observe SN 2015F eight times (visits 01-08 in this proposal) and ASASSN-14lp five times (visits 09-13). To minimize the number of orbits used, the visits to each SN will alternate between one single orbit with F555W, and two orbits split between F555W, F438W, F625W, and F814W. This setup will allow us to construct the quasi-bolometric light curves of the SNe, with the added insurance of a high S/N F555W light curve, in case the S/N in any of the other filters is too low to construct the quasi-bolometric light curve. These two options will be sufficient for us to detect the anticipated change in the light curves predicted from the decay of 57Co. The colors we measure here will also allow us to determine whether either of the two target SNe become contaminated by light echoes.
Unfortunately, there are no previous HST observations of the locations of these SNe (GO-13646 imaged the host-galaxy of SN 2015F, but the pointing did not include the location of the SN). Thus, our first visit to each SN will act as a test to determine the effect of the galaxy's diffuse background light on the observations and the S/N of the SN in each filter. We may have to adjust the exposure time we request for each filter for the following visits accordingly.
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