High angular resolution K-band spectroscopy of the nucleus of NGC 1068 with PUEO-GRIF (CFHT)

Details High angular resolution K-band spectroscopy of the nucleus of NGC 1068 with PUEO-GRIF (CFHT) High angular resolution K-band spectroscopy of the nucleus of NGC 1068 with PUEO-GRIF (CFHT)

Dec 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003a%26a...411..335g&link_type=abstract

Astronomy and Astrophysics, v.411, p.335-342 (2003)

Astronomy and Astrophysics

Astrophysics

16

Galaxies: Seyfert, Galaxies: Individual: Ngc 1068

Scientific paper

We provide new high angular resolution K-band spectroscopic observations of the nucleus of NGC 1068 obtained with the new 3-D spectrograph GriF coupled to PUEO, the CFHT adaptive optics system. Results match well with the general framework of the unified model of active galactic nuclei (AGN) and bring more precise evaluation of the size and structure of the close AGN environment. The K-band emission is dominated by the thermal continuum of the compact central source (albeit resolved: FWHM ~ 0.12\arcsec) with a color temperature around 950 K (reddened sublimation temperature of the dust, corresponding to 1200 K when deredenned), interpreted as the border of a sublimation cavity within the dust torus, surrounding the central core. Coronal emission lines ([Si Vi], [Si Vii] and [Ca Viii]) are detected from a few tenths of arcseconds around this compact source and a new [Si Vi] emission spot is found at 0.7\arcsec north of the central source. The Brackett gamma emission features a very broad component (FWHM=2500 km s-1) in the central 200 mas and we claim that it correponds to the broad line region seen through the dust. A narrower component (FWHM=1600 km s-1) is seen at larger angular distance and is likely the trace of the narrow line region. Molecular hydrogen emission lines are detected beyond 0.6\arcsec of the central source. We interpret the lack of emission in the center as a lack of excited molecular H_2 along the line of sight, because of the putitative dust torus shading gas from UV photons. No evidence of stellar activity in a 1\arcsec radius around the central source can be found. We also compare these observations to the results of a numerical model of a torus harboring an active galactic nucleus. The main characteristics of the observed spectra (slope, flux) match well with the unified scheme of AGN, in the case of a dense (tau_V =40) obscuring torus containing silicate grains with an inclination angle of around 22° with regards to the line of sight.

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