0Assigned ID: 312
----- Attempting Submission 1 (Thu Apr 06 21:48:09 GMT 2017) -----
HST Phase I Proposal 312 (APT_N6946_cy25.apt) successfully submitted.
Receipt: # 312-1
----- Attempting Submission 7 (Fri Apr 07 15:38:27 GMT 2017) -----
HST Phase I Proposal 312 (APT_N6946_cy25.apt) successfully submitted.
Receipt: # 312-70----- Attempting Submission 1 (Wed Jul 19 17:38:15 GMT 2017) -----Characterizing the Supernova Remnant Population of the Fireworks Galaxy, NGC 6946Characterizing large uniform samples of supernova remnants (SNRs) in spiral galaxies can lead to fundamental insights about the stellar cycle of life, death, and rebirth. We have underway a comprehensive multiwavelength (optical, near-IR, radio, X-ray) campaign using both imaging and spectroscopy to identify and characterize the rich SNR population in NGC 6946, which has produced more historical SNe than any other galaxy. Our catalog of ~200 candidates from ground-based imaging is missing key information about their size and morphology, since at the 5.9 Mpc distance, where 1" = 33 pc, all the smaller (younger) SNRs are unresolved. We request HST (WFC3 UVIS) imaging in H-alpha and [S II] 6716, 6731 of seven fields in NGC 6946, which will allow us to (a) measure sizes and morphologies of the ground-based SNR candidates, (b) identify small-diameter SNR candidates missed in the ground-based survey or located in confused regions, (c) search for optical traces from any of the 7 (out of 9) historical SNe within our survey region, and (d) search for any exceptional objects such as very young SNRs or micro-quasars that may be masquerading as normal SNR candidates. We also propose to use deep photometry and CMD-fitting on archival HST-ACS two-color broadband imagery of three fields, plus one additional ACS field proposed here, to determine the age of the stellar population surrounding many of the SNRs, and thus constrain the masses of their progenitor SNe. Finally, we will compare NGC 6946 with a similarly comprehensive analysis we have done for M83 to understand what characteristics might be galaxy dependent versus more universal.We request seven WFC3 UVIS fields in F657N (Halpha) and F673N ([S II]) to approximately cover the bright optical disk of NGC 6946 and also roughly duplicate the 9-field region observed previously with the WFC3 IR in Paschen beta (Prog. 14156, Leroy, PI) and in [Fe II] 1.64 um (Prog. 14638, Long, PI). We also request continuum imaging in a single filter, F547M, which avoids emission lines and will be used to scale and subtract from the narrow band emission images to remove galaxy background light and enhance the emission-line analysis. The continuum imagery requested here only needs to go deep enough for this purpose, and can be kept reasonably short.
Our previous experience with HST observations of M83 and other galaxies allows us to have significant confidence in what will be seen for NGC 6946. Using our ground-based flux-calibrated imagery of both galaxies, the brightest SNRs in both galaxies have comparable fluxes of about 1E-14 ergs/cm^2/s, but the bulk of the SNR population identified so far in NGC 6946 is ~ 2x fainter than for M83 (~5E-16 instead of about 1E-15). This is to be expected due to the greater distance and somewhat higher foreground extinction for NGC6946. Thus, we scale up the exposure times used for M83, and have determined a 3 orbit per field strategy (basically, one orbit in F657N, ~1.5 orbits in F673N, and ~0.5 orbit in F547M for continuum subtraction, assuming dithering by 3 exposures.
Existing data in NGC 6946 informs what we need for the additional field of ACS continuum imaging. Two orbits (each) of broadband B and R will match the existing data and provide the needed depth for the CMD fitting.
Parallels: NGC 6946 has an extended stellar halo beyond the bright disk. With a separation of ~6 arcmin between the WFC3 and ACS footprints in the HST focal plane, this makes the idea of parallel observing favorable. We therefore have included parallel imaging in R (F606W) and I (F814W) broadband filters (more appropriate than B and R for the outer halo) in our program. THis includes ACS R and I parallels on the prime WFC3 exposures AND WFC3 R and I in parallel on the ACS prime observations. Depending on the specific orientation of the observations, some of these parallel fields may overlap existing parallel fields from earlier programs, thus driving the detection limits even fainter in those regions.Stellar PhysicsGalaxies and the IGM6falsefalsefalsefalsefalsefalseSUPPORTEDGALAXYSPIRALSTARBURSTJ2000J2000GALAXYSPIRALSTARBURSTJ2000J2000GALAXYSPIRALSTARBURSTJ2000J2000GALAXYSPIRALSTARBURSTJ2000J2000GALAXYSPIRALSTARBURSTJ2000J2000GALAXYSPIRALSTARBURSTJ2000J2000GALAXYSPIRALSTARBURSTJ2000J2000GALAXYSPIRALSTARBURSTJ2000J2000WFC3/UVISImagingNoNoF657NWFC3/UVISImagingNoNoF673NWFC3/UVISImagingNoNoF547MWFC3/UVISImagingNoNoF657NWFC3/UVISImagingNoNoF673NWFC3/UVISImagingNoNoF547MWFC3/UVISImagingNoNoF657NWFC3/UVISImagingNoNoF673NWFC3/UVISImagingNoNoF547MWFC3/UVISImagingNoNoF657NWFC3/UVISImagingNoNoF673NWFC3/UVISImagingNoNoF547MWFC3/UVISImagingNoNoF657NWFC3/UVISImagingNoNoF673NWFC3/UVISImagingNoNoF547MWFC3/UVISImagingNoNoF657NWFC3/UVISImagingNoNoF673NWFC3/UVISImagingNoNoF547MWFC3/UVISImagingNoNoF657NWFC3/UVISImagingNoNoF673NWFC3/UVISImagingNoNoF547MACS/WFCImagingNoNoF435WACS/WFCImagingNoNoF606WACS/WFCImagingNoNoF606WACS/WFCImagingNoNoF814WACS/WFCImagingNoNoF606WACS/WFCImagingNoNoF814WACS/WFCImagingNoNoF606WACS/WFCImagingNoNoF814WACS/WFCImagingNoNoF606WACS/WFCImagingNoNoF814WACS/WFCImagingNoNoF606WACS/WFCImagingNoNoF814WACS/WFCImagingNoNoF606WACS/WFCImagingNoNoF814WACS/WFCImagingNoNoF606WACS/WFCImagingNoNoF814WWFC3/UVISImagingNoNoF606WWFC3/UVISImagingNoNoF814WPOS-TARGDITHER1.605LINEfalsefalse386.7WFC3-UVIS-DITHER-LINE-3PT1falsePOS-TARGDITHER3.034LINEfalsefalse385.29ACS-WFC-DITHER-LINE2falsePOS-TARGDITHER1.605LINE0.112falsefalse81.6486.7WFC3-UVIS-DITHER-BOX3false/private/var/folders/th/7gqts1jd1d5631_1msrthvz0000403/T/OPVisit7670328301649839362.xmlHst Same orient constraint links visits (01 02 03 04 05 06 07)The scheduling data was generated by CASM 25.2.CASM was run in Phase II mode.(Tic-Visit
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