Observations of the Galactic Centre with ISO

scientific abstract we propose to survey selected extended regions within the inner 3 x 2 degrees of our galaxy in the 4 to 200 micron wavelength range. from smaller structures, such as the circumnuclear disk, the streamer, some cloud cores, m0.130.08, sgra east, the arc as well as previously catalogued discrete fir sources, we plan to take surface brightness spectra in the same wavelength range. through comparison with model calculations, with existing images from iras, and with images at 2.2 micron and submm wavelength, these observations will provide much detailed information of the morphology, the sources of heating, the intensity of the interstellar radiation field, and the location relative to the galactic centre of the various dust components. a particular goal is to distinguish between the possible star burst and monster nature of the inner few parsecs. observation summary isocam exposures centered on sgr a*: 1.5 arcsec pfov with the sw4,sw1, sw3, sw8, sw9, sw10, sw5. 3.0 arcsec pfov with the lw1, lw2, lw3, lw7, lw8. concatenated p05 and p25 1 dimensional rasters: each raster has 1x32 points with an interval of 3.; the central raster is centered on sgra*; its elongations are displaced by + 75. in l and b to cover in total +2 degs in l and b. 7 points are overlapping. p25 from l + 2 and b + 2 degrees towards sgr a* at 200 microns. p05 from l + 2 and b + 2 degrees towards sgr a* at 100, 60, 25, 4.85 and 3.6 microns. (raw iras data, which is highly nonlinear in the bright central region, will be compared with the p05 scans at 100, 60 and 25 microns to calibrate the iras survey of the central region at these wavelength s). large rasters: 1) raster strip scan with p25 (ny1, nz6 at 200 microns and ny1, nz7 at 100 and 60 microns, centered 72 east of sgr a*). these are concatinated to p32 raster maps at 200, 100 and 60 microns, centered on the same position. th truncated!, Please s [truncated!, Please see actual data for full text]