The 3-5 micron Spectrum of NGC 1068 at High Angular Resolution: Distribution of Emission and Absorption Features across the Nuclear Continuum Source

Details The 3-5 micron Spectrum of NGC 1068 at High Angular Resolution: Distribution of Emission and Absorption Features across the Nuclear Continuum Source The 3-5 micron Spectrum of NGC 1068 at High Angular Resolution: Distribution of Emission and Absorption Features across the Nuclear Continuum Source

2009-06-26

arxiv.org/abs/0906.4885v2

Astrophys.J.701:1710-1720,2009

Astronomy and Astrophysics

Astrophysics

Cosmology and Extragalactic Astrophysics

42 pages, incl. 2 tables and 5 figures. Accepted by ApJ on 22 June 2009. Typos fixed, references changed/removed

Scientific paper

10.1088/0004-637X/701/2/1710

We report moderate resolution 3-5 micron spectroscopy of the nucleus of NGC 1068 obtained at 0.3 arcsec (20 pc) resolution with the spectrograph slit aligned approximately along the ionization cones of the AGN. The deconvolved FWHM of the nuclear continuum source in this direction is 0.3 arcsec. Four coronal lines of widely different excitations were detected; the intensity of each peaks near radio knot C, approximately 0.3 arcsec north of the infrared continuum peak, where the radio jet changes direction. Together with the broadened line profiles observed near that location, this suggests that shock-ionization is the dominant excitation mechanism of the coronal lines. The depth of the 3.4 micron hydrocarbon absorption is maximum at and just south of the continuum peak, similar to the 10 micron silicate absorption. That and the similar and rapid variations of the optical depths of both features across the nucleus suggest that substantial portions of both arise in a dusty environment just in front of the continuum source(s). A new and tighter limit is set on the column density of CO. Although clumpy models of the dust screen might explain the shallowness of the silicate feature, the presence of the 3.4 micron feature and the absence of CO are strongly reminiscent of Galactic diffuse cloud environments and a consistent explanation for them and the observed silicate feature is found if all three phenomena occur in such an environment, existing as close as 10 pc from the central engine.

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