Please let me know if you have any problems opening the file. Thanks very much for your help.1012140534Assigned ID: 1987
----- Attempting Submission 1 (Sat Mar 02 00:05:19 GMT 2013) -----I think this is it! I have attempted to image the supernova remnant efficiently using all requested filters. I have dithered
using large offsets to cover the chip gap when using the regular filters. For quad filters I have employed small recommend
offsets. I have used the FLASH option for all filters to help with CTE.
I'd like to thank everyone for tremendous support preparing Phase II.
Please let me know if there are any problems with the program as submitted.
Regards, Dan1881700828----- Attempting Submission 1 (Wed Jun 26 19:22:43 GMT 2013) -----I am aware of the errors:
>>Warning (Form): Be very careful mixing POS TARG and Center_Pattern = Yes
This comes up because I am dithering across the chip gap by centering in a region of the remnant where
there is least emission. The offset is about 5 arcsec to the west.
>>Warning (Form): POS TARG & PATTERN should be used carefully with ACS ramp or WFC3 quad filters as central wavelengths & transmission efficiencies vary within the apertures.
For ramp filters I use a very small offset (<0.15arcsec) to dither a fifth image with respect to a dither box pattern of four images.Toward A Comprehensive Kinematic and Chemical Survey of the Young O-rich SNR 1E 0102-7219 in the SMCWe propose the first comprehensive UV and optical imaging survey of the young, oxygen-rich, SMC supernova remnant 1E 0102-7219 (E0102). These data will be coordinated with an optical spectroscopic survey of E0102 already in progress that has uncovered previously unknown high velocity S-rich ejecta and an elaborate bubble-like, large-scale ejecta structure having a velocity distribution that spans more than twice the currently accepted mean value.
Combining the proposed WFC3 UV and optical imaging with our recent spectroscopic survey will allow: (1) the first complete mapping of E0102's high and low velocity metal-rich ejecta, (2) a first-of-its-kind map of UV emission in [Ne IV] 2425 and Mg II 2800 of an O-rich SNR, (3) identification of remnant regions exhibiting sulfur emission associated with the inner Si,S,Ca,Ar layer of the progenitor star, (4) investigation of an expected population of exceptionally high velocity, outer knots like those seen in Cas A, (5) calculation of an accurate mean expansion velocity and age via proper motions using archival HST data, and (6) creation of a high-resolution 3D kinematic and chemical reconstruction of E0102's UV and optically emitting ejecta.
This data set will reveal E0102's full structure in extraordinary detail, and provide powerful insights on the dynamics and nucleosynthesis yields of high-mass progenitor core-collapse supernova explosion models. It will also set the stage for more expansive multi-wavelength studies that can incorporate the already rich data available in Chandra X-ray and Spitzer infrared observations.We request a suite of UV and optical WFC3/UVIS images of E0102 taken over a total of 10 orbits. E0102 is a faint SNR and we have chosen narrow filters because our experience imaging Cas A has shown dramatic differences in sensitivity between broad- and narrow-band filters. Some of the observations will use the quad filters, which we are aware have 1/6 the field of view (FOV) of the WFC3/UVIS and will necessitate a two tile mosaic to image the entire remnant that is some 30'' in diameter. This will introduce additional overhead that has been incorporated into our requested number of orbits.
We have used archival FOS spectra of E0102 (Figure 5) and the WFC3 ETC employing a 5x5 extraction region to estimate exposure lengths. Most images will have total exposure lengths between 1500-2400 s, broken up into three- or four-point dithered images to achieve the best S/N and high resolutions we desire. The UV images will require additional time. The breakdown of the orbits follow below.
Two orbits will be used for UV images. The FQ243N and F280N filters will map the [Ne IV] and Mg II 2800 emission. The ETC calculates that the F280N and FQ243N images with total exposure lengths of 2400-3000 s will yield images of S/N>10. Five orbits are allocated for the [O III] and [O II] maps. The combination of the FQ492N, F502N, and FQ508N filters will maximize sensitivity for the [O III] 4959, 5007 lines and probe the entire extent of the ejecta velocities revealed in our survey while minimizing background light. These filters will divide the remnant up into the blueshifted, low velocity, and redshifted regions, and will go deeper than previous ACS/WFC images. Anticipated proper motions between our data and an archival 2003 F475W image will be 0.07''.
Two orbits are allocated for [S II] 6716, 6731 imaging. Both the F665N and F673N filters will sample the full velocity range of the S-rich ejecta. We note that the standard F673N filter alone would entirely miss the high-velocity [S II] emission uncovered in our
spectroscopic survey (Figure 3).
One orbit is allocated for [N II]+Halpha imaging. A large population of outer, exceptionally high velocity ejecta knots in Cas A have recently been uncovered that show strong [N II]+Halpha emissions. Our proposed F657N image can be compared with an archival WFC/ACS F658N image obtained in 2003 to determine whether a similar population exists around E0102. A comparable population with velocities > 10,000 km s would show a total proper motion shift of > 0.3'', or approximately 7 pixels over the ten years separating the images. A F645N contains no significant emission lines and will be used for continuum and star subtraction
for the F657N, F665N, and F673N filters.ISM AND CIRCUMSTELLAR MATTERDefaultfalsetruefalsefalsefalseSUPPORTEDEXT-MEDIUMSNRThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000WFC3/UVISImagingNoNoF280NWFC3/UVISImagingNoNoFQ243NWFC3/UVISImagingNoNoF373NWFC3/UVISImagingNoNoF467MWFC3/UVISImagingNoNoFQ492NWFC3/UVISImagingNoNoF502NWFC3/UVISImagingNoNoFQ508NWFC3/UVISImagingNoNoF665NWFC3/UVISImagingNoNoF673NWFC3/UVISImagingNoNoF657NWFC3/UVISImagingNoNoF645NPOS-TARGDITHER4.5LINE3.5falsefalse81.785423.884WFC3-UVIS-DITHER-BOX4falsePOS-TARGDITHER0.173LINE0.112falsefalse81.785423.884WFC3-UVIS-DITHER-BOX6falsePOS-TARGMOSAICDITHER42.414WFC3-UVIS-DITHER-BOXfalse81.785true0.1120.173285.759POS-TARGWFC3-UVIS-GAP-LINE23.8847falsePOS-TARGMOSAICDITHER42.414WFC3-UVIS-DITHER-BOXfalse81.785true0.1120.173385.759POS-TARGWFC3-UVIS-GAP-LINE23.8848falsePOS-TARGDITHER0.145LINEfalsefalse246.84WFC3-UVIS-DITHER-LINE9false/pool/casanova0/data/hst/cycle21/OP-cache/e0102-cycle21_v4-v01.xmlHst Same orient constraint links visits (01 02 03)The scheduling data was generated by CASM 21.2.CASM was run in Phase II mode.(Tic-Visit
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