scientific abstract we propose a detailed study of the ir spectrum of 3 broad line radio galaxies from 2-200 microns using pht-s,pht-p and pht-c in order to determine the origin of the 25 micron emission peak seen in iras data and search for other possible emission. such a program will; - determine the relative contributions of thermal and non-thermal emission components to the ir and bolometric luminosities, and thus search for the ir signature of the .naked central engine.; - probe the physical conditions in the central engine via studies of the spectrum of any ir synchrotron continuum component(s) observation summary the continuum flux distribution of 3c390.3 will be measured between 2.5 and 200 microns using pht-s-s,pht-s-l, pht-p (20,25 microns), pht-c (60,100,120,135,160 microns). same measurements to be made for 3c120. for 3c279, the continuum flux distrubution will be measured with pht-p in seven filters (3.5,4.85,7.3,12.8, 16,20,25 microns) and pht-c (60,100,120,135,160 microns). for each source all observations will be concatenated to avoid intrinsic continuum variability perturbing the results. times were calculated as follows; 3c390.3, 1jy source in pht-c, 250mjy in pht-s,pht-p; for 3c120,1jy source in pht-c, 250mjy in pht-s,pht-p; for 3c279, 1jy in pht-c and 50mjy in pht-p. times include rectangular chopping and aim for s/n of 10.
Instrument
CAM01 , PHT03 , PHT22 , PHT40
Temporal Coverage
1996-02-05T04:38:11Z/1996-12-10T11:36:22Z
Version
1.0
Mission Description
The Infrared Space Observatory (ISO) was the worlds first true orbiting infrared observatory. Equipped with four highly-sophisticated and versatile scientific instruments, it was launched by Ariane in November 1995 and provided astronomers world-wide with a facility of unprecedented sensitivity and capabilities for a detailed exploration of the Universe at infrared wavelengths.
European Space Agency, Barr et al., 1999, 'The infrared flux distribution of Broad Line radio Galaxies and the 25mu bump in 3C390.3', 1.0, European Space Agency, https://doi.org/10.5270/esa-fxt4t0g
