This is a revised Phase II proposal based on Andy Fruchter's suggestions to
turn off CR-SPLIT and to use the UDF dither pattern (0,0), (3.0,1.5),(4.5,4.5)
and (1.5,3.0) pixels.
----- Submission 1 (Mon May 09 21:10:26 GMT 2005) -----
Phase II Proposal 10577 (sn1006_p2) successfully submitted.
----- Submission 2 (Tue Aug 02 20:28:02 GMT 2005) -----
Assigned ID: 76
----- Submission 1 (Thu Jan 20 17:25:41 GMT 2005) -----
Resolving the non-radiative shock in SN1006
An ACS image of the H alpha filament in the supernova remnant SN1006 will
resolve the thickness of the H alpha emission zone. This will permit us to
derive an accurate pre-shock density, which in turn can be used to model
the time-dependent X-ray spectrum of the bright X-ray ridge with no free
parameters, thus benchmarking these widely used models. We will also search
for evidence of a shock precursor, and we will use the scale of ripples in the
shock to estimate the level of density inhomogeneity in the pre-shock gas.
This is a deep WFC H alpha image of the NW filament in SN1006.
It uses the UDF dither pattern as suggested by Andy Fruchter;
(0,0), (3.0,1.5), (4.5,4.5), 1.5,3.0) pixels and CR-SPLIT=0.
ISM AND CIRCUMSTELLAR MATTER
12
false
0.0
false
false
false
false
false
SUPPORTED
ISM
EMISSION LINE NEBULA
FILAMENT
SHOCK FRONT
SNR
3.2E-16 erg/(cm2 s arcsec2) in H alpha emission
J2000
15 02 19.1700
-41 44 50.00
J2000
ACS/WFC
Imaging
No
No
F658N
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