Crotts DD proposal on SN 2014J light echoes - addressed GO/DD 136211968254573Assigned ID: 2226
----- Attempting Submission 1 (Wed Jan 29 22:04:05 GMT 2014) -----
HST Phase I Proposal 2226 (sn2014jechoesDD.apt) successfully submitted.
----- Attempting Submission 3 (Thu Jan 30 03:41:37 GMT 2014) -----
HST Phase I Proposal 2226 (sn2014jechoesDD.apt) successfully submitted.
----- Attempting Submission 4 (Fri Jan 31 19:43:33 GMT 2014) -----
HST Phase I Proposal 2226 (sn2014jechoesDD.apt) successfully submitted.ORBITAL VISIBILITY OVERRUN
ORBITAL VISIBILITY OVERRUN
ORBITAL VISIBILITY OVERRUN
ORBITAL VISIBILITY OVERRUNThis is submitted solely for the purposes of executing Visit 5.-83932795----- Attempting Submission 1 (Sat Feb 15 01:44:56 GMT 2014) -----
----- Attempting Submission 2 (Tue Feb 18 01:37:55 GMT 2014) -----
----- Attempting Submission 3 (Wed Mar 12 22:53:35 GMT 2014) -----
----- Attempting Submission 4 (Mon Nov 03 18:18:00 GMT 2014) -----Orbit and Visit Planners have been run. Also, there is a small visibility overrun that does not affect schedulability.Light Echoes and Environment of SN 2014J in M82Supernova 2014J is likely the closest Type Ia SN since 1885. This offers us a unique opportunity to study the environment of SNe Ia, here at a level of detail several times better than any other, farther SN Ia observed by HST. Prime tools for probing this environment, supernova light echoes, are likely to succeed given what we know about where this SN resides in its host galaxy, M82. M82 is a spacial galaxy in terms of star formation activity, and SN 2014J offers a special probe of this galaxy since it is a Ia, not core collapse SN, so more likely to sample the structure of M82 more typically, rather than centered on a region recently producing massive stars, such as a core-collapse progenitor. We describe how the light echo mapping that will be provided by the proposed observations will produce a high-resolution, three-dimensional view of a large part of M82, and how this can be directly compared to models of the interstellar medium to learn how star formation feeds back into the gaseous structure of galaxies. This comparison is arguably only possible with SN light echoes, of which SN 2014J is likely to provide the most useful example.The prime purpose of these observations is to obtain unsaturated or only mildly saturated images primarily in broad bands in which the field containing SN 2014J was imaged prior to the SN outburst. These bands are F438W, F555W and F814W. Exposure times will need to be adjust to provide these, given the somewhat unpredictable variable nature of the source. In addition there are several narrow bands observed before outburst that can be compared to look at new extended sources in atomic line transitions (F487N, F502N, F658N, F673N). For these we need if possible to acheive satisfactory S/N ratio in the background galaxy surface brightness. Finally, we will use some small fraction of exposure time to extended the UV light curve past maximum light and look for extended UV reflection for this uique object (F218W, F225W, F275W, F336W).ISM IN EXTERNAL GALAXIES0SUPPORTEDSTARSUPERNOVA TYPE IAJ2000J2000WFC3/UVISImagingNoNoF438WWFC3/UVISImagingNoNoF555WWFC3/UVISImagingNoNoF658NWFC3/UVISImagingNoNoF502NWFC3/UVISImagingNoNoF438WWFC3/UVISImagingNoNoF555WWFC3/UVISImagingNoNoF658NWFC3/UVISImagingNoNoF502NPOS-TARGDITHER0.135LINEfalsefalse346.84WFC3-UVIS-DITHER-LINE-3PT2falsePOS-TARGDITHER0.173LINE0.112falsefalse81.785423.884WFC3-UVIS-DITHER-BOX3falseThe scheduling data was generated by CASM 21.2.CASM was run in Phase II mode.The purpose of this visit is to obtain immediately post-maximum imaging of SN 2014J in M82 in such a way as not grossly oversaturate the SN point source but still detect the galaxy's surface brightness at good efficiency. This one-orbit visit uses some of the same filters that will be employed on Visit 2, but will verify that we are using the proper selection of exposure times and apertures most effectively.1394580575000155.1963711128858(Tic-Visit
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)false11The scheduling data was generated by CASM 21.2.CASM was run in Phase II mode.This Visit 2 defines most of the data for the first epoch of the project, and will be adjusted according to the results of Visit 1. Since SN 2014J is a highly variable and not well-predicted source, we may need to adjust the exposure times in Visit 2 according to Visit 1.1395764694000132.9381012439826(Tic-Visit
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)true11The scheduling data was generated by CASM 21.2.CASM was run in Phase II mode.This Visit 4 defines the data for the third epoch of the project, and will be adjusted according to the results of Visits 1 through 3. Since SN 2014J is a highly variable and not well-predicted source, we may need to adjust the exposure times in Visit 4 according to Visits 1 through 3. Visit 4 needs to occur about three months after Visit 3.1409943929000342.95564594817597(Tic-Visit
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)true21The scheduling data was generated by CASM 22.2.CASM was run in Phase II mode.This Visit 5 defines the data for the fourth epoch of the project.1422853111000196.34074564746356(Tic-Visit
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