Contents of: VI/111/./abstract/LSPINOGL_SAM12N_1.abs

The following document lists the file abstract/LSPINOGL_SAM12N_1.abs from catalogue VI/111.
A plain copy of the file (without headers/trailers) may be downloaded.

==> In this proposal, more time is being requested for LSPINOGL.S12AGN_*
==> This proposal requests an upgrade from Priority 3 for LSPINOGL.S12AGN_*
This proposal was approved by the OTAC, part of the observations have been and
are beeing collected, we request here the time needed to collect the necessary
data to derive more reliable and solid conclusions. Progress on the fundamental
issues of galactic and nuclear activity and of the physical connections
between the various classes of active galactic nuclei (AGN) towards a unified
scheme requires the analysis of a complete, large, unbiased and representative
sample and, most importantly, complete down to a certain bolometric flux limit.
It is also required to obtain, for such a sample, complete multifrequency data,
from X-rays to radio, to reveal the different continuum and line emission
components across the e.m spectrum. Both these requirements are met with the
12um Active Galaxy Sample, which has been shown to be bolometric flux limited
and for which extensive multi-frequency data have already been collected. The
observations are needed to understand the connections between high IR luminosity
starburst galaxies and AGN, to address the question if Seyfert 2 are dusty
Seyfert 1 whose broad line regions are obscured. We will use analytical methods
to reveal the dominant correlations underlying the observed properties of AGN
and define a new classification system, more physically based than the emission-
line scheme. Specifically, we propose to observe the 12um AGN Sample with 60-200
um PHT photometry and CAM imaging and to collect PHT-S spectrophotometry for a
subsample. The FIR photometry will uniquely detect and measure the occurrence
and shape of the far-IR turnover, giving the best test of nonthermal models.
The mid-IR imaging will separate nuclear and galaxy luminosities and measure
the distribution of hot dust. PHT-S will measure the emission-line spectrum,
with high-ionization forbidden lines, H and He recombination lines, molecular
transitions, and the continuum energy distribution. It is especially important
to determine how the broadband near/mid-IR magnitudes are affected by dust
features, both in absorption (silicates) and in emission (e.g., PAH's).

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