<=== observer ===>
"RTUFFS",\
"Tuffs, R.J.",\
"",\
"Max-Planck-Institut fuer Kernphysik",\
"Saupfercheckweg 1",\
"103980",\
"D-69029",\
"Heidelberg",\
"Germany",\
" 496221 516295",\
" 496221 516324",\
"rjt@taurus.mpi-hd.mpg.de"
<=== proposal ===>
"SNR",1,2,\
{"supernova remnants","dust properties"},\
{"Tuffs, R.J.","Pearce, G.","Russell, S.","Rasmussen, I."\
"Schnopper, H.","Skaley, D.","Voelk, H.J.","Wells, M.","Drury, L."}
<=== title ===>
Observations of Dust and Gas in Supernova Remnants
<=== abstract ===>
SCIENTIFIC ABSTRACT
We propose a spectrophotometric and spectropolarimetric investigation of the
prototype young galactic supernova remnants Cas A and the Crab Nebula,
respectively. This investigation addresses the possible formation, composition
and destruction of grains in these objects, the properties of dust and gas in
the pre-existing circum-progenitor media (CPM), and the chemical composition and
dynamics of the ejecta. We further propose to study the early stages in the
evolution of the remnant of SN1987A, which could be a brightening infrared
source during the lifetime of ISO. In the event of an autumn launch the Crab
Nebula will be not visible to ISO, and we intead propose an investigation of the
shock processing of interstellar grains at the blast wave of the Cygnus Loop.
OBSERVATION SUMMARY
Using PHT-C we propose to measure several positions within the Crab Nebula in
it's polarised synchrotron emission at 12, 25, 60 and 100 micron. This addresses
the question of the origin of the ``bump'' in the FIR spectrum detected by IRAS.
The positions for polarimetry are chosen to be at positions of different
magnetic field orientations as revealed from maps of the radio synchrotron
emission. Oversampled absolute photometric mapping in total power at 60, 100,
and 200 micron will be achieved by concatenating linear scans taken in the
absolute photometry mode to two dimensional mapping observations. This will
establish the integrated spectrum of the nebula in the FIR, and will measure the
spatial distribution of mass column densities and temperatures of the grains in
the nebula. Spectrophotometric mapping of the entire nebula using PHT-S will
probe the chemical composition of the grains, and provide a survey of line
emission from more highly ionised species in the photoionised gas than can be
seen in the UV and visible. These measurements are complemented by the ISOCAM
mapping of the nebula by Lagage et al.
PHT-C diffraction-limited mapping of Cas A at 200, 160, 100 and 60 micron should
provide a definitive measurement of the mass of any grains present in unshocked,
cold dense regions of the metal rich ejecta, which should be mainly interior to
the hot component of emission collisionally heated by shocked gas in the shell
of the remnant. PHT-S mapping will probe the location and compositions of the
ejecta and circumprogenitor medium, both in the gas and solid state components.
A particular aim is to investigate the possible presence of gas components with
densities and temperatures intermediate between those found in the dense fast
optical filaments and the diffuse X-ray emitting plasma. The spectral resolution
of approximately 3000 kms**-1 should provide information on the pattern of
velocities of ejected species emitting infared fine structure line emission.
A map with a finer raster will be made with PHT-S towards the complex of fast
optical filaments outside the shell to the North-East. A deeper single pointing
will be made with PHT-S towards the expansion centre of the remnant. These
observations are complementary to the ISOCAM mapping observations of Cas A
proposed by Lagage et al.
The remnant of SN1987A will be observed with the PHT-C100 and PHT-C200 arrays in
the C60, C90, C160 and C180 filters to measure any dust from the ejecta/
circumprogenitor medium in the 10 - 30 K temperature range. To lower the
FIR confusion limit from interstellar dust emission from the LMC, spatially
oversampled scans will be taken through the source. Warmer dust associated with
the blast wave/shocked gas will be searched for using the PHT-P2 detector with
the 25 micron filter at a fixed spacecraft raster position with the focal plane
chopper in it's triangular mode. Optimum sensitivity and angular resolution for
broad-band emission from the supernova/cpm in 12-18 micron range will be
provided by ISOCAM using it's smallest pixel size and longest readout interval.
The ISOCAM image will also be sensitive to echo emission structures from the
interstellar medium around the supernova. The limiting rms flux densities to
point sources reached in the 12-18/25/60/90/160/180 micron filters is predicted
to be approximately 0.01/8/3/1/3/4 mJy respectively.
Continuued in scientific justification section...
<=== scientific_justification ===>
For an autumn launch a field in the north eastern shell of the Cygnus loop will
be mapped with full oversampling in the FIR to provide diffraction-limited
images of the dust emission. This remnant is the prototype of a middle-aged SNR
expanding into a diffuse interstellar medium. It's proximity (770pc) and high
galactic latitude make it an ideal testing ground for the processing of grains
by shocks and the effect of grain emission on shock structure. The field chosen
contains the most prominent optical filaments seen on the palomar sky survey,
as well as the brightest ridge of 60 micron emission seen by IRAS. In addition
to the 2D maps, which will be obtained using PHT-C in the 60, 100, 160 and 200
micron filters and with ISOCAM in the 12-18 micron filter, oversampled scans at
25 microns will be obtained through the field perpendicular to the optical
filamentary emission using PHT-P in a 10 arcsec aperture. Images of spectral
features from grains and from the carriers of the unidentified infrared emission
features (if they survive the passage of the shock), and of fine structure lines
from ions will be provided in the 2.5-5 and 6-12 micron spectral ranges by
a raster map using PHT-S. These data from ISO will be compared with structures
in the cooling gas downstream of the blastwave and embedded overtaken clouds,
deduced from x-ray, visible, near infrared and submm. images. This should help
elucidate the location, heating mechanisms and luminosities of dust components
having the various temperature and size distributions envisaged to be present.
To provide information on low surface brightness collisionally heated dust
emission embedded in the tenuous unity filling factor plasma well downstream of
the optical filaments, 32 arcmin length scans perpendicular to the blast wave
will also be performed with PHT-C in the 60, 100 and 160 micron filters.
Fine structure line emission from highly ionized species in the hot plasma
will be investigated using PHT-S scans along the same scan line.
A summary of the major astronomical observation template parameters is given
in the tables below:
Table of main astronomical observation template parameters for Crab Nebula:
--------------------------------------------------------------------------------
osn aot RA DEC Tint (s) per filter PFOV Chop ISO Raster
(spr./ (1950) per ISO pointing (") throw raster Incr.
aut.) S/12/25/60/100/200 Mode/" ny nz dy dz "
--------------------------------------------------------------------------------
1/- PHT51 05 31 31.1 +21 59 22 - - - 64 - - - R/210 - - - -
2/- PHT51 05 31 31.1 +21 59 22 - - - - 32 - - R/210 - - - -
3/- PHT51 05 31 35.1 +21 58 57 - - - 64 - - - R/210 - - - -
4/- PHT51 05 31 35.1 +21 58 57 - - - - 32 - - R/210 - - - -
5/- PHT51 05 31 25.9 +21 59 20 - - - 64 - - - R/210 - - - -
6/- PHT51 05 31 25.9 +21 59 20 - - - - 32 - - R/210 - - - -
7/- PHT51 05 31 30.3 +21 58 25 - - - 64 - - - R/210 - - - -
8/- PHT51 05 31 30.3 +21 58 25 - - - - 32 - - R/210 - - - -
9/- PHT51 05 31 23.9 +22 00 30 - - - 64 - - - R/210 - - - -
10/- PHT51 05 31 23.9 +22 00 30 - - - - 32 - - R/210 - - - -
11/- PHT51 05 31 23.3 +22 00 00 - - - 64 - - - R/210 - - - -
12/- PHT51 05 31 23.3 +22 00 00 - - - - 32 - - R/210 - - - -
13/- PHT32 05 31 31.2 +21 58 51 - - - 8 8 - - - 5 7 90 69
14/- PHT25 05 31 31.2 +21 58 51 - - - 8 - - - - 1 4 - 138
15/- PHT25 05 31 31.2 +21 58 51 - - - - 8 - - - 1 4 - 138
16/- PHT32 05 31 31.2 +21 58 51 - - - - - 8 - - 5 11 90 46
17/- PHT25 05 31 31.2 +21 58 51 - - - - - 8 - - 1 4 - 180
18/- PHT50 05 31 31.2 +21 58 51 - - 64 - - - 127x127 R/210 - - - -
19/- PHT05 05 31 31.2 +21 58 51 - - 8 - - - 127x127 - 5 1 180 -
20/- PHT50 05 31 31.2 +21 58 51 - 64 - - - - 127x127 R/210 - - - -
21/- PHT05 05 31 31.2 +21 58 51 - 8 - - - - 127x127 - 5 1 180 -
22/- PHT50 05 31 23.9 +22 00 30 - - 64 - - - 127x127 R/210 - - - -
23/- PHT05 05 31 23.9 +22 00 30 - - 8 - - - 127x127 - 5 1 180 -
24/- PHT50 05 31 23.9 +22 00 30 - 64 - - - - 127x127 R/210 - - - -
25/- PHT05 05 31 23.9 +22 00 30 - 8 - - - - 127x127 - 5 1 180 -
26/- PHT50 05 31 23.3 +22 00 00 - - 64 - - - 127x127 R/210 - - - -
27/- PHT05 05 31 23.3 +22 00 00 - - 8 - - - 127x127 - 5 1 180 -
28/- PHT50 05 31 23.3 +22 00 00 - 64 - - - - 127x127 R/210 - - - -
29/- PHT05 05 31 23.3 +22 00 00 - 8 - - - - 127x127 - 5 1 180 -
30/- PHT40 05 31 31.2 +21 58 51 16 - - - - - - - 15 15 24 24
--------------------------------------------------------------------------------
Table of main astronomical observation template parameters for Cas A:
--------------------------------------------------------------------------------
osn aot RA DEC Tint (s) per filter ISO Chopper Raster
(spr./ (1950) per ISO pointing raster Mode/throw Incr.
aut.) S/60/100/160/200 ny nz /(") dy dz(")
--------------------------------------------------------------------------------
31/1 PHT32 23 21 13.0 +58 32 35 - 8 8 - - 6 6 - - 90 69
32/2 PHT32 23 21 13.0 +58 32 35 - - - 8 8 6 11 - - 90 31
33/3 PHT40 23 21 13.0 +58 32 35 32 - - - - 13 13 - - 24 24
34/4 PHT40 23 21 12.0 +58 32 20 256 - - - - 1 1 T 30 - -
35/5 PHT40 23 21 36.0 +58 33 34 32 - - - - 7 7 - - 12 12
--------------------------------------------------------------------------------
Table of main astronomical observation template parameters for SN1987A:
--------------------------------------------------------------------------------
osn aot RA DEC Tint (s) per filter PFOV Chopper ISO
(spr./ (1950) per ISO pointing (") mode/throw raster
aut.) 12-18/25/60/90/160/180 /(") ny nz
--------------------------------------------------------------------------------
36/6 PHT03 05 35 50.0 -69 17 58 - 256 - - - - 10 T/15 1 1
37/7 PHT32 05 35 50.0 -69 17 58 - - 32 32 - - - - 3 2
38/8 PHT32 05 35 50.0 -69 17 58 - - - - 32 32 - - 3 2
39/9 CAM01 05 35 50.0 -69 17 58 4x20 - - - - - 1.5 - 2 2
--------------------------------------------------------------------------------
Table of main astronomical observation template parameters for Cygnus Loop:
--------------------------------------------------------------------------------
osn aot RA DEC Tint (s) per filter PFOV ISO Raster
(spr./ (1950) per ISO pointing (") raster Increment
aut.) S/12-18/25/60/100/160/200 ny nz dy dz (")
--------------------------------------------------------------------------------
-/10 PHT32 20 54 16.3 +31 33 31 - - - - - 8 8 - 21 1 90 -
-/11 PHT32 20 54 16.3 +31 33 31 - - - 8 8 - - - 21 1 90 -
-/12 PHT40 20 54 16.3 +31 33 31 64 - - - - - - - 32 1 60 -
-/13 PHT32 20 54 16.3 +31 33 31 - - - - - 8 8 - 6 9 90 46
-/14 PHT32 20 54 16.3 +31 33 31 - - - 8 8 - - - 6 7 90 69
-/15 CAM01 20 54 16.3 +31 33 31 - 4x5 - - - - - 6 5 3 96 96
-/16 PHT40 20 54 16.3 +31 33 31 16 - - - - - - - 14 14 24 24
-/17 PHT03 20 54 24.8 +31 31 36 - - 8 - - - - 10 31 1 10 -
-/18 PHT03 20 54 24.8 +31 31 36 - - 8 - - - - 10 30 1 10 -
-/19 PHT03 20 54 21.4 +31 32 22 - - 8 - - - - 10 31 1 10 -
-/20 PHT03 20 54 21.4 +31 32 22 - - 8 - - - - 10 30 1 10 -
-/21 PHT03 20 54 18.0 +31 33 08 - - 8 - - - - 10 31 1 10 -
-/22 PHT03 20 54 18.0 +31 33 08 - - 8 - - - - 10 30 1 10 -
-/23 PHT03 20 54 14.6 +31 33 54 - - 8 - - - - 10 31 1 10 -
-/24 PHT03 20 54 14.6 +31 33 54 - - 8 - - - - 10 30 1 10 -
-/25 PHT03 20 54 11.2 +31 34 40 - - 8 - - - - 10 31 1 10 -
-/26 PHT03 20 54 11.2 +31 34 40 - - 8 - - - - 10 30 1 10 -
-/27 PHT03 20 54 07.8 +31 35 26 - - 8 - - - - 10 31 1 10 -
-/28 PHT03 20 54 07.8 +31 35 26 - - 8 - - - - 10 30 1 10 -
--------------------------------------------------------------------------------
Time distribution for autumn launch targets:
Team top 40% second 30% last 30%
PHT : 0 12801 22533
Time distribution for spring launch targets:
Team top 40% second 30% last 30%
PHT : 15526 10209 5045
<=== autumn_launch_targets ===>
1, "PHT32", 2.0, "N", "CASMAP", 23.35361, 58.54306, 1950, 0., 0., 1455, 2
2, "PHT32", 2.0, "N", "CASMAP", 23.35361, 58.54306, 1950, 0., 0., 2242, 0
3, "PHT40", 2.0, "N", "CASMAP", 23.35361, 58.54306, 1950, 0., 0., 6512, 0
4, "PHT40", 2.0, "N", "CASCEN", 23.35333, 58.53897, 1950, 0., 0., 520, 0
5, "PHT40", 2.0, "N", "CASFOF1", 23.36000, 58.55944, 1950, 0., 0., 2072, 0
6, "PHT03", 3.0, "N", "SN1987A", 5.59722, -69.29947, 1950, 0., 0., 601, 7
7, "PHT32", 3.0, "N", "SN1987A", 5.59722, -69.29947, 1950, 0., 0., 616, 8
8, "PHT32", 3.0, "N", "SN1987A", 5.59722, -69.29947, 1950, 0., 0., 516, 9
9, "CAM01", 3.0, "N", "SN1987A", 5.59722, -69.29947, 1950, 0., 0., 670, 0
10, "PHT32", 3.0, "N", "CYGSTRIP", 20.90454, 31.55861, 1950, 0., 0., 589, 11
11, "PHT32", 3.0, "N", "CYGSTRIP", 20.90454, 31.55861, 1950, 0., 0., 903, 12
12, "PHT40", 3.0, "N", "CYGSTRIP", 20.90454, 31.55861, 1950, 0., 0., 2369, 0
13, "PHT32", 3.0, "N", "CYGMAP", 20.90454, 31.55861, 1950, 0., 0., 1921, 14
14, "PHT32", 3.0, "N", "CYGMAP", 20.90454, 31.55861, 1950, 0., 0., 1601, 15
15, "CAM01", 3.0, "N", "CYGMAP", 20.90454, 31.55861, 1950, 0., 0., 520, 0
16, "PHT40", 3.0, "N", "CYGMAP", 20.90454, 31.55861, 1950, 0., 0., 4375, 0
17, "PHT03", 3.0, "N", "CYGMS0", 20.90690, 31.52666, 1950, 0., 0., 808, 18
18, "PHT03", 3.0, "N", "CYGMS0", 20.90690, 31.52666, 1950, 0., 0., 634, 19
19, "PHT03", 3.0, "N", "CYGMS1", 20.90596, 31.53944, 1950, 0., 0., 648, 20
20, "PHT03", 3.0, "N", "CYGMS1", 20.90596, 31.53944, 1950, 0., 0., 634, 21
21, "PHT03", 3.0, "N", "CYGMS2", 20.90501, 31.55222, 1950, 0., 0., 648, 22
22, "PHT03", 3.0, "N", "CYGMS2", 20.90501, 31.55222, 1950, 0., 0., 634, 23
23, "PHT03", 3.0, "N", "CYGMS3", 20.90406, 31.56500, 1950, 0., 0., 648, 24
24, "PHT03", 3.0, "N", "CYGMS3", 20.90406, 31.56500, 1950, 0., 0., 634, 25
25, "PHT03", 3.0, "N", "CYGMS4", 20.90312, 31.57778, 1950, 0., 0., 648, 26
26, "PHT03", 3.0, "N", "CYGMS4", 20.90312, 31.57778, 1950, 0., 0., 634, 27
27, "PHT03", 3.0, "N", "CYGMS5", 20.90218, 31.59056, 1950, 0., 0., 648, 28
28, "PHT03", 3.0, "N", "CYGMS5", 20.90218, 31.59056, 1950, 0., 0., 634, 0
<=== spring_launch_targets ===>
1, "PHT51", 1.0, "N", "CRABPOL1", 5.52530, 21.98944, 1950, 0., 0., 596, 2
2, "PHT51", 1.0, "N", "CRABPOL1", 5.52530, 21.98944, 1950, 0., 0., 304, 3
3, "PHT51", 1.0, "N", "CRABPOL2", 5.52641, 21.98264, 1950, 0., 0., 436, 4
4, "PHT51", 1.0, "N", "CRABPOL2", 5.52641, 21.98264, 1950, 0., 0., 304, 5
5, "PHT51", 1.0, "N", "CRABPOL3", 5.52387, 21.98889, 1950, 0., 0., 436, 6
6, "PHT51", 1.0, "N", "CRABPOL3", 5.52387, 21.98889, 1950, 0., 0., 304, 7
7, "PHT51", 1.0, "N", "CRABPOL4", 5.52509, 21.97356, 1950, 0., 0., 436, 8
8, "PHT51", 1.0, "N", "CRABPOL4", 5.52509, 21.97356, 1950, 0., 0., 304, 9
9, "PHT51", 1.0, "N", "CRABPOL5", 5.52332, 21.00833, 1950, 0., 0., 436, 10
10, "PHT51", 1.0, "N", "CRABPOL5", 5.52332, 21.00833, 1950, 0., 0., 304, 11
11, "PHT51", 1.0, "N", "CRABPOL6", 5.52314, 22.00000, 1950, 0., 0., 436, 12
12,"PHT51", 1.0, "N", "CRABPOL6", 5.52314, 22.00000, 1950, 0., 0., 304, 13
13,"PHT32", 1.0, "N", "CRABMAP", 5.52532, 21.98072, 1950, 0., 0., 1255, 14
14,"PHT25", 1.0, "N", "CRABMAP", 5.52532, 21.98072, 1950, 0., 0., 205, 15
15,"PHT25", 1.0, "N", "CRABMAP", 5.52532, 21.98072, 1950, 0., 0., 209, 16
16,"PHT32", 1.0, "N", "CRABMAP", 5.52532, 21.98072, 1950, 0., 0., 1093, 17
17,"PHT25", 1.0, "N", "CRABMAP", 5.52532, 21.98072, 1950, 0., 0., 109, 0
18,"PHT50", 1.0, "N", "CRABMAP", 5.52532, 21.98072, 1950, 0., 0., 607, 19
19,"PHT05", 1.0, "N", "CRABMAP", 5.52532, 21.98072, 1950, 0., 0., 254, 20
20,"PHT50", 1.0, "N", "CRABMAP", 5.52532, 21.98072, 1950, 0., 0., 347, 21
21,"PHT05", 1.0, "N", "CRABMAP", 5.52532, 21.98072, 1950, 0., 0., 155, 22
22,"PHT50", 1.0, "N", "CRABPOL5", 5.52332, 21.00833, 1950, 0., 0., 447, 23
23,"PHT05", 1.0, "N", "CRABPOL5", 5.52332, 21.00833, 1950, 0., 0., 254, 24
24,"PHT50", 1.0, "N", "CRABPOL5", 5.52332, 21.00833, 1950, 0., 0., 347, 25
25,"PHT05", 1.0, "N", "CRABPOL5", 5.52332, 21.00833, 1950, 0., 0., 155, 26
26,"PHT50", 1.0, "N", "CRABPOL6", 5.52314, 22.00000, 1950, 0., 0., 447, 27
27,"PHT05", 1.0, "N", "CRABPOL6", 5.52314, 22.00000, 1950, 0., 0., 254, 28
28,"PHT50", 1.0, "N", "CRABPOL6", 5.52314, 22.00000, 1950, 0., 0., 347, 29
29,"PHT05", 1.0, "N", "CRABPOL6", 5.52314, 22.00000, 1950, 0., 0., 155, 0
30, "PHT40", 1.0, "N", "CRABMAP", 5.52532, 21.98072, 1950, 0., 0., 4286, 0
31, "PHT32", 2.0, "N", "CASMAP", 23.35361, 58.54306, 1950, 0., 0., 1455, 32
32, "PHT32", 2.0, "N", "CASMAP", 23.35361, 58.54306, 1950, 0., 0., 2242, 0
33, "PHT40", 2.0, "N", "CASMAP", 23.35361, 58.54306, 1950, 0., 0., 6512, 0
34, "PHT40", 3.0, "N", "CASCEN", 23.35333, 58.53897, 1950, 0., 0., 520, 0
35, "PHT40", 3.0, "N", "CASFOF1", 23.36000, 58.55944, 1950, 0., 0., 2072, 0
36, "PHT03", 3.0, "N", "SN1987A", 5.59722, -69.29947, 1950, 0., 0., 601, 37
37, "PHT32", 3.0, "N", "SN1987A", 5.59722, -69.29947, 1950, 0., 0., 616, 38
38, "PHT32", 3.0, "N", "SN1987A", 5.59722, -69.29947, 1950, 0., 0., 516, 39
39, "CAM01", 3.0, "N", "SN1987A", 5.59722, -69.29947, 1950, 0., 0., 670, 0