This is the revised program with the pointings and orient values negotiated with Tony Roman. WFC3-UVIS-DITHER-LINE-3PT has been added for all the quadrant filter exposures per the recommendation of Knox Long. ----- Attempting Submission 3 (Wed Oct 05 16:39:53 GMT 2011) ----- Knowledge of chemical abundances is fundamental to understanding the processes of nucleosynthesis and galactic chemical evolution. There are two major problems in nebular astrophysics that seriously affect the ability to derive reliable elemental abundances from emission lines. Attempts to solve these long-standing problems [the "abundance" & "temperature problems"-see text] have focused on electron temperature (Te) fluctuations within nebulae. The problems remain, and there is now a substantial faction who argue that Te variations alone are insufficient. We propose to build upon the previous observations of the benchmark Orion Nebula to measure not only Te variations but also the cospatial electron density (Ne) and ionization variations. With the new capability enabled by WFC3 and its unique set of narrow-band filters, we will obtain images with a scale as fine as 0.04". Through these filters, we will isolate emission lines including OIII 4363 & 5007, NII 5755 & 6584, SII 6716 & 6731, and SIII 9532 A. These observations will allow us to study in unprecedented detail variations (as well as their interdependence) in the fine-scale structure of Ne[SII], temperature (Te[OIII] for the high-ionization regions, Te[NII] for the low-ionization ones), and the degree of ionization via S+/S++. As a coordinated parallel program with no added time, we will image with ACS/F658N to provide a second epoch dataset with at least a seven year time-base. The goal is to obtain greater accuracy for the motions of jets and shocks arising from Young Stellar Objects and thus to better determine the time-dependent-characteristics of the episodic collimated outflows from these objects.

WFC3/UVIS imaging will be made of M42 (the Orion Nebula). A set of full field images will be made centered on a region SW of the Trapezium and a set of quadrant filter images will be made in a portion of the full field images that is centered to the NE from the center for the full field filters. We choose these targets for several important reasons, including that they include the brightest part of the nebula, they include some shocked outflow sources, and for which Co-I O'Dell has Keck HIRES spectra. Coordinated parallel images will be made using the ACS. The position combinations of the ORION-INNER and ORION-QUADS WFC3 targets are: ORION-INNER Target 5:35:09.57 -5:24:22.82 ORION-QUADS Target 5:35:12.89 -5:24:00.83 This is for an ORIENT = 70 Degrees exactly, our preferred ORIENT. This specific value permits a scheduling window in 2012 from 16 or 17 Jan - 13 Mar, ~56 days. If we cannot get this specific ORIENT value, then a range from 60 - 80 Degrees would also work. However we would need to know the expected value in order to make small changes to our target positions (order a few arcsec). The reason for this is to avoid the bright stars in the Trapezium. Note that the APT submission has the ORIENT range from 60 - 80 Degrees which opens the scheduling window a few more days, from 8 Jan - 13 Mar 2012. ISM AND CIRCUMSTELLAR MATTER 12 true 0.0 0.0 false false false false SUPPORTED ISM EMISSION LINE NEBULA PLANETARY NEBULA RING NEBULA FULLFIELDFILTERS J2000 J2000 V-magnitude estimate is for a field star, which is not important for this emission-line object. ISM EMISSION LINE NEBULA PLANETARY NEBULA RING NEBULA QUAD-FILTERS J2000 J2000 V-magnitude is for a field star, which is not important for this emission-line object. WFC3/UVIS Imaging No No FQ436N WFC3/UVIS Imaging No No FQ437N WFC3/UVIS Imaging No No FQ575N WFC3/UVIS Imaging No No FQ672N WFC3/UVIS Imaging No No FQ674N WFC3/UVIS Imaging No No FQ750N WFC3/UVIS Imaging No No F469N WFC3/UVIS Imaging No No F487N WFC3/UVIS Imaging No No F502N WFC3/UVIS Imaging No No F547M WFC3/UVIS Imaging No No F645N WFC3/UVIS Imaging No No F656N WFC3/UVIS Imaging No No F658N WFC3/UVIS Imaging No No F673N WFC3/UVIS Imaging No No F953N ACS/WFC Imaging No No F502N ACS/WFC Imaging No No F658N ACS/WFC Imaging No No F660N ACS/WFC Imaging No No F550M POS-TARG MOSAIC DITHER 4 3.264 WFC3-UVIS-DITHER-BOX false 81.785 false 0.112 0.173 2 63.697 POS-TARG WFC3-UVIS-MOSAIC-LINE 23.884 1 false POS-TARG DITHER 0.135 LINE false false 3 46.84 WFC3-UVIS-DITHER-LINE-3PT 2 false The scheduling data was generated by CASM 19.3. 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