Dear Shelly Meyett: This is a revised Phase II observing plan. The target positions have been modified for Visits 2 and 3. Since the HST observations need to be done via a CVZ, this means they must be done in Hubble's late May 2008 CVZ window for Cas A. Any questions about this Phase II submission should be sent to D. Patnaude (dpatnaude@cfa.harvard.edu) and R. Fesen (fesen@snr.dartmouth.edu). Thanks, -Dan Patnaude and Rob Fesen ----- Attempting Submission 1 (Fri Oct 12 18:55:12 GMT 2007) ----- Phase II Proposal 11337 (Prop_11337_v7.apt) successfully submitted. ----- Attempting Submission 2 (Thu Dec 27 18:54:34 GMT 2007) ----- Phase II Proposal 11337 (Prop_11337_v91.apt) successfully submitted. ----- Attempting Submission 3 (Sat Apr 26 22:33:36 GMT 2008) ----- Investigating the X-ray Variability of Cassiopeia A We propose a 50 ksec ACIS-S observation of Cas A to follow X-ray flux changes associated with ejecta recently encountered by the reverse shock. This will allow us to investigate Cas A's near-term X-ray evolution and the fine-scale structure of its SN debris. We also request the Chandra observation be followed by HST NICMOS & WFPC2 images of four identified X-ray variable features in the high ionization NIR lines of [Si VI] and [Si X] and low ionization optical lines of [S II] and [O III]. The proposed X-ray/optical/NIR observations will yield a multi-wavelength study of the remnant's advancing reverse shock in an inhomogeneous multi-phase ejecta medium at resolutions down to a fraction of an arcsecond, providing a hi-resolution broad temperature study of reverse shock heated SN ejecta.
This project involves WFPC2 imaging and NICMOS imaging of three (3) regions in the Cas A supernova remnant that have been identified as likely reverse shock front regions. Although we currently (Oct 2007) don't know exactly what specific regions in the remnant will show significant X-ray emission changes - that information will come from a scheduled 12 Dec 2007 Chandra observation - we have selected three place-holding targets regions, namely, CAS-A-SOUTH, CAS-A_WEST, and CAS-A_NW for the HST planning of Phase II observations. The WFPC2 images will consist of red (F675W) and blue/green (F450W, mainly sensitive to [O III] 5007,4959 line emission). Since the regions of interest are small, we will center them in the WFC3 chip and perform a four point dither. CTE should not be too much of a problem since the features of interest will likely not be very faint. The NICMOS observations will involve both NIC1 and NIC3 due to the need of different NIR filters. For NIC3, we wish to use the F196N filter, while for NIC1 we want to use the F145M filter. Because more than one reverse shokc feature may be present within the FOV of both the WFC3 and NIC3 but not the NIC1 due to its much smaller FOV, we have designed a program consisting of two NIC1 pointings within each of the three NIC3 and WFPC2 pointings. These are called regions ...-NIC1-A and ...NIC1-B. 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