Contents of: VI/111/./abstract/FMIRABEL_HEATDUST.abs

The following document lists the file abstract/FMIRABEL_HEATDUST.abs from catalogue VI/111.
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We propose to use ISOCAM and ISOPHOT to study phenomena at  the interface
between the High Energy Astrophysics and the Physics of Cold Interstellar Gas. 
If an X-ray binary is inside or near a molecular cloud most of the energy from 
the relativistic particles streaming out from the compact source must be 
dissipated by heating of the interstellar material and thermal emission from 
dust is expected. The Galactic Center region is appropriate to study these 
phenomena since in there massive stellar remnants and molecular gas are more 
abundant than anywhere else in the Galaxy. In that region of the sky we wish 
to study the emission from dust heated by the compact source of annihilation 
of positrons 1E1740.7-2942 ("Great  Annihilator") and by the large scale 
electric current known under the name of "Snake". Another sources of study 
for the autumn launch are the radio "ears" in W50  which are brightened by 
particles streaming out from the classic microquasar SS433, and the runaway 
binary Circinus X-1 which is moving through the interstellar medium at a speed 
of several hundred km/s. We point out that our proposed observations of 
SS433/W50 are of different nature to those proposed by Salama with PHT who 
aims to determine the spectral shape of the central source. 
In the event of a spring launch we will observe the black hole candidates 
NPersei92, NMon75, NMuscae, Cyg X-1, and the peculiar IR bright binary Cyg X-3. 

In order to obtain some spectral information all sources will be observed 
using CAM01 with the filters LW2 (5-8.5 microns) and LW3 (12-18 microns) in the 
microscanning mode and PHOT C100 at 90 microns. For all sources we will use a 
p.f.o.v. of 6", for maximum sensitivity.Typically, for CAM, we aim at detecting
fluxes in the range of 0.002 to 0.003 mJy/arcsec2 with a S/N ratio of order 3. 
For the Great Annihilator, we will cover a field of (2.5'x2.5'),with a raster
of (4x4) steps. The same field will be covered with PHOT in one exposure.
For  the Snake, we will perform a 6x3 position raster , with a displacement of
16 pixels. The area covered for the latter source will be roughly 500x200 
arcsec with the highest S/N ratio; the total area covered is of the order of 
700x400 arcsec. The PHT concatenated observation will be performed in the 
raster mode as well, using a linear raster with 4 images displaced by 0.5'.
For SS433/W50, we will observe the center of the lobes, over an area of 16'x10',
again with steps of 16 pixels. With PHOT, we will survey the same area with a
raster of (5x3) positions,with displacements of 1.5'.
For Circinus X-1, we will use a raster of (6x6) steps to cover an area in
excess of an ISO field of view. This will be followed by a raster with PHOT
with 4 positions, with displacements by 1.5' in both directions.
For the sources visible in the spring, we plan to use a strategy similar to
that used for the Great Annihilator.

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