The following document lists the file abstract/FMIRABEL_HEATDUST.abs
from catalogue VI/111.
A plain copy of the file
(without headers/trailers) may be downloaded.
SCIENTIFIC ABSTRACT:
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.
OBSERVATION SUMMARY:
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.