Crotts et al. SN2014J resubmission: GO/DD => GO1362229080Assigned ID: 776
----- Attempting Submission 1 (Fri Apr 10 20:28:29 GMT 2015) -----FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browserThis is the Phase 2 submission for program 14146 to image the light echoes from SN 2014J, consisting of 3 visits. The first visit (Visit 5) shoud be executed as soon as possible, most preferably before the end of July 2015. A program change request has been submitted to support this.
RESUBMISSION UPDATE 12 MAY 2016: Based on the strength of the light echoes, SN and diffuse background
detected in Visits 01 and 02, and the fading rate of the supernova, the patterns and exposure times for Visit 03
were rebalanced to increase the total exposure times in F438W and F555W, without significantly decreasing the
total times in F502N and F658N. The error warning regarding the FLASH level for the F438W exposures (03.002)
is not relevant, due to the diffuse background of M 82 in the vicinity of SN 2014J.-1811627382----- Attempting Submission 1 (Tue Jul 07 21:13:34 GMT 2015) -----
----- Attempting Submission 3 (Thu May 12 21:02:40 GMT 2016) -----RESUBMISSION UPDATE 12 MAY 2016: Based on the strength of the light echoes, SN and diffuse background
detected in Visits 01 and 02, and the fading rate of the supernova, the patterns and exposure times for Visit 03
were rebalanced to increase the total exposure times in F438W and F555W, without significantly decreasing the
total times in F502N and F658N. The error warning regarding the FLASH level for the F438W exposures (03.002)
is not relevant, due to the diffuse background of M 82 in the vicinity of SN 2014J.Light Echoes and Environment of SN 2014J in M82Type Ia SN 2014J exploded in the nearby M82 = NGC 3032, reaching V maximum light around 2014 February 5, the closest SN since 1987 and likely the closest SN Ia since 1885. Recent HST/WFC3 imaging (2014 September 5 and 2015 February 2) of M82 in the vicinity of SN 2014J reveals a light echo at radius 0.6 arcsec from SN 2014J (or 13 pc in M82), meaning a z distance of 330 pc closer t0 Earth than the SN. Additional echoes reside at a smaller radii of about 0.3-0.4 arcsec (or z = 80-160 pc). HST observations of SN 2014J's echoes over the next few years will allow us to map and explore further star formaion in M82, and rhe 3-D structure of gas and dust. Echoes in the near future might also reveal circumstellar structure around SN 2014J's progenitor star. 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. M82 is a special 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, with SN 2014J providing the most useful Ia 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 GALAXIES12falsefalsefalsefalsefalsefalseSUPPORTEDSTARSUPERNOVA TYPE IAJ2000J2000WFC3/UVISImagingNoNoF438WWFC3/UVISImagingNoNoF555WWFC3/UVISImagingNoNoF658NWFC3/UVISImagingNoNoF502NWFC3/UVISImagingNoNoF438WWFC3/UVISImagingNoNoF555WWFC3/UVISImagingNoNoF658NWFC3/UVISImagingNoNoF502NPOS-TARGDITHER0.173LINE0.112falsefalse81.785423.884WFC3-UVIS-DITHER-BOX3falseThe scheduling data was generated by CASM 24.0.CASM was run in Phase II mode./Users/physsl/Research/Data/SN2014J/HST_Cyc23_2015/OP-cache/14146-v01.xmlThis Visit 01 defines the data for the fifth epoch of observations of the light echoes of SN2014J in M82. Epochs 1--4 were taken during GO 13626.143735568400034.0(Tic-Visit
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UPDATE (added 12 May 2016): Based on the strength of the light echoes detected in Visits 01 and 02, and the fading rate of the supernova, the patterns and exposure times for this Visit were rebalanced to increase the total exposure times in F438W and F555W without significantly decreasing the total times in F502N and F658N. The error warning regarding the FLASH level for the F438W exposures (03.002) is not relevant, due to the diffuse background of M 82 in the vicinity of SN 2014J.(Tic-Visit
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