0 Assigned ID: 729 ----- Attempting Submission 1 (Fri Apr 11 19:45:36 GMT 2014) ----- HST Phase I Proposal 729 (sn2011fe.apt) successfully submitted. ----- Attempting Submission 2 (Fri Apr 11 20:55:30 GMT 2014) ----- HST Phase I Proposal 729 (sn2011fe.apt) successfully submitted. ----- Attempting Submission 3 (Fri Apr 11 22:25:56 GMT 2014) ----- HST Phase I Proposal 729 (sn2011fe.apt) successfully submitted. ----- Attempting Submission 4 (Fri Apr 11 22:47:08 GMT 2014) ----- HST Phase I Proposal 729 (sn2011fe.apt) successfully submitted. ----- Attempting Submission 5 (Sat Apr 12 14:18:42 GMT 2014) ----- David Golimowski added internal visits to obtain WFC1-1K subarray bias frames for calibration of ACS science exposures. GROUP-WITHIN constraints were added to the science visits to ensure that the bias frames are obtained within 14 days of the science exposures. The 4 internal calibration orbits are charged to the Cycle 22 ACS Calibration Program. (WEK) added a postflash of 9 e- as well as changed the BETWEEN to 1st of Jan to 31st of Jan 1378803295 ----- Attempting Submission 1 (Sun Jul 20 20:16:36 GMT 2014) ----- ----- Attempting Submission 2 (Fri Oct 03 18:06:00 GMT 2014) ----- ----- Attempting Submission 3 (Tue Oct 21 04:41:01 GMT 2014) ----- ----- Attempting Submission 4 (Tue Jun 16 14:29:30 GMT 2015) ----- New warnings are associated with 4 internal orbits added to obtained ACS subarray bias frames to calibrate the supported ACS science exposures. These warnings should be ignored. SN 2011fe - tackling the Type Ia progenitor puzzle through extremely late time photometry We propose to obtain extremely late-time photometry for the nearby SN Ia 2011fe. Located nearby in M101 and along a line of sight with negligible extincition, SN 2011fe provides us with the once-in-a-lifetime chance to probe SN Ia physics by measuring the very late time luminosity decline. Such extremely late photometric measurements are only accessible to HST. Despite the importance of SNe Ia in astrophysics and cosmology, and a large concerted effort to understand these objects, it is still unclear whether SNe Ia result from the explosion of an accreting white dwarf (single-degenerate scenario) or from the merger-explosion of two white dwarfs (double-degenerate scenario). However, theoretical models predict clear differences in the very late time light-curves of the two scenarios. The UBVRI photometry which we propose to obtain will extend a current Gemini imaging campaign enabling us to test whether SN 2011fe originated from a single-degenerate or from a double-degenerate progenitor. As SN 2011fe is a typical SN Ia, the result - together with the results from complementary tests - will have a significant impact on the interpretation of SNe Ia and on future developments in SN Ia theory. We are aiming to determine the decline rate of bolometric luminosity of the very nearby supernova SN 2011fe - a way to distinguish between two different explosion models for this Type Ia supernova. Thus, we have designed our observations to measure the flux over the whole UVOIR range using a filter set that has very little overlap at two epochs (~1200 and ~1450 days). As we expect very little flux shifting into and out of the UVOIR range (some shifting within the UVOIR range is definitely expected) we can determine a true bolometric decline rate despite only measuring pseudo-bolometric flux. In addition, we have included U filter observations in the first epoch to see if the surprising flux excess in g-band from our 930 day Gemini observation continues into the UV. For the optical bands we employ the ACS instrument and have grouped them (using a three point dither pattern) into one orbit in the first epoch and two orbits in the second epoch (using a four point dither pattern). As we are only interested in measuring the brightness of the supernova we have opted for the smaller aperture WFC1-1K, which is a good compromise between avoiding overheads due to buffer dumps and having some calibration stars to tie our observations to our previous Gemini data. The infrared observations will be performed using WFC3 and are similarly arranged as the optical. They are also grouped in a three-point dither pattern and use a smaller Aperture (IR512) to avoid unnecessary overheads. In addition, all of our IR sequences have at least 12 Reads, to achieve good readnoise performance. Furthermore, the F105W filter is subject to variable higher background than APT predicts due to the existence of He I 10830 emission in the upper atmosphere (see Brammer et al. 2014). We have put the IR observations in a non-interruptable sequence and have aranged our pattern in such a way that all z-band photometry is taken in the middle of the orbit to avoid unneccesary contamination. CALIBRATION ORBITS: As per STScI policy, 4 internal orbits have been added to this proposal for the purpose of obtaining subarray bias frames that are contemporaneous with the science observations. These internal orbits will be charged to STScI's Cycle 22 ACS Calibration Program. The ACS Instrument Team at STScI is responsible for producing superbias reference files from the bias frames obtained in this GO proposal. RESOLVED STELLAR POPULATIONS 12 Regular false false false false false SUPPORTED STAR SUPERNOVA TYPE IA This object was generated by the targetselector and retrieved from the SIMBAD database. J2000 J2000 WFC3/IR Imaging No No F125W WFC3/IR Imaging No No F160W WFC3/IR Imaging No No F105W WFC3/UVIS Imaging No No F336W ACS/WFC Imaging No No F475W ACS/WFC Imaging No No F625W ACS/WFC Imaging No No F775W WFC3/IR Imaging No No F125W WFC3/IR Imaging No No F160W WFC3/IR Imaging No No F105W ACS/WFC Imaging No No F475W ACS/WFC Imaging No No F625W ACS/WFC Imaging No No F775W POS-TARG DITHER 0.605 LINE false false 3 41.788 WFC3-IR-DITHER-LINE-3PT 1 false POS-TARG DITHER 3.011 LINE false false 3 85.28 ACS-WFC-DITHER-LINE 2 false POS-TARG DITHER 0.135 LINE false false 3 46.84 WFC3-UVIS-DITHER-LINE-3PT 3 false POS-TARG DITHER 0.265 LINE 0.187 false false 69.05 4 20.67 ACS-WFC-DITHER-BOX 5 false Timing link suitability includes constraints ([Group (01 A1 A2) Within 14.0 days]) The scheduling data was generated by CASM 22.2. 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