Shock Energy in Merging Systems: The Elephant in the Room.

Assigned ID: 301 ----- Attempting Submission 1 (Fri Feb 25 07:30:03 GMT 2011) ----- HST Phase I Proposal 301 (Cycle19_revised.apt) successfully submitted. ----- Attempting Submission 2 (Fri Feb 25 19:11:55 GMT 2011) ----- HST Phase I Proposal 301 (Cycle19_revised.apt) successfully submitted. ----- Attempting Submission 3 (Fri Feb 25 19:20:59 GMT 2011) ----- HST Phase I Proposal 301 (Cycle19_revised.apt) successfully submitted. ----- Attempting Submission 4 (Fri Feb 25 23:40:05 GMT 2011) ----- ----- Attempting Submission 1 (Fri Jul 08 12:28:53 GMT 2011) ----- The warnings refer to the use of patterns with the quad filters. This is understood and may be ignored. Shock Energy in Merging Systems: The Elephant in the Room. The relationship between shocks, star formation and the evolution of merging galaxies is not well understood. We are now poised to gain major insight in this area, thanks to the high resolution narrow-band imaging capabilities of WFC3 and recent major advances in theoretical shock and and photoionization models. Shocks and star formation in merging galaxies are regulated by fundamental physical properties of the ISM such as dust, gas density, ionized gas structure, and the presence of galactic winds and outflows. We aim to uncover the relationship between shocks, galactic winds, and the fundamental ISM properties in two famous mergers NGC 6240 and Arp 220. These two galaxies are currently transitioning from disk galaxies into spheroids and they are close enough to achieve the spatial scales required to resolve individual supernova remnants with WFC3 imaging. We propose to image NGC 6240 and Arp 220 in key shock and photoionization sensitive diagnostic lines [OII], [OIII], H-beta, [NII]+H-alpha, [SII], and (where possible) [OI] to (1) resolve the source of the ionizing radiation field (shocks versus photoionization by hot stars) at spatial scales of 25-35 pc, and (2) map the distribution of the star formation and ionized gas to search for links with merger-driven shocks and large-scale gas flows.

Our total exposure time estimates to reach a S/N = 5 per 0.07” resolution element are given in the following Table, as calculated with the WFC3 UVIS imaging Exposure Time Calculator. We used the H images of Heckman (1987) plus the HST image of NGC 6240 by Gerssen et al. (2004) to measure the limiting fluxes of prominent emission-line structures. We then used ground-based long-slit data (Kim et al. 1995, Kewley et al. 2000, Rupke et al. 2005, Moustakas & Kennicutt 2006) to scale these H fluxes and estimate the expected fluxes of other emission lines. Overhead estimates shown in the Table below include setup, readout, dithering, and filter change overheads, plus 2-3 exposures per filter (3 exposures for total exposure times > 1000, and 2 exposures for total exposure times < 1000) to ensure robust cosmic-ray removal. Due to the short exposures in the red and narrow-band filters, we expect there to be at least 2, and at most 4 buffer dumps. We will try to minimize the effect of these dumps by placing the short exposures at the beginning or end of orbits. Our total overhead includes the time required for 4 buffer dumps as shown in the table. Including overheads, we request 7 orbits for Arp 220, and 8 orbits for NGC 6240, for a total of 15 orbits. n/a n/a None. ISM IN EXTERNAL GALAXIES 12 false 0.0 0.0 false false false false SUPPORTED GALAXY INTERACTING GALAXY SHOCK FRONT STARBURST J2000 J2000 GALAXY INTERACTING GALAXY SHOCK FRONT STARBURST J2000 J2000 WFC3/UVIS Imaging No No FQ492N WFC3/UVIS Imaging No No FQ508N WFC3/UVIS Imaging No No F645N WFC3/UVIS Imaging No No F673N WFC3/UVIS Imaging No No F680N WFC3/UVIS Imaging No No F467M WFC3/UVIS Imaging No No F621M WFC3/UVIS Imaging No No FQ492N WFC3/UVIS Imaging No No FQ508N WFC3/UVIS Imaging No No F665N WFC3/UVIS Imaging No No F680N WFC3/UVIS Imaging No No F467M WFC3/UVIS Imaging No No F621M POS-TARG DITHER DITHER 4 2.414 WFC3-UVIS-DITHER-BOX false 81.785 true 0.112 0.173 2 85.759 POS-TARG WFC3-UVIS-GAP-LINE 23.884 1

false

POS-TARG MOSAIC DITHER 3 2.414 WFC3-UVIS-DITHER-LINE-3PT false true 0.135 2 85.759 POS-TARG WFC3-UVIS-GAP-LINE 46.84 2

true

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