HST Continuum and Narrow-band Images of AGN

Details HST Continuum and Narrow-band Images of AGN HST Continuum and Narrow-band Images of AGN

May 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992aas...180.0201k&link_type=abstract

American Astronomical Society, 180th AAS Meeting, #02.01; Bulletin of the American Astronomical Society, Vol. 24, p.727

Astronomy and Astrophysics

Astronomy

4

Scientific paper

We present a gallery of narrow-band Hα , [O III], and [N II] and 547 nm continuum images of active galactic nuclei obtained by the FOS team using the Planetary Camera on the Hubble Space Telescope. For NGC 1068 we also show a UV continuum ``image'' in the 2460--2780 Angstroms band. In many cases, particularly for Seyfert 2 galaxies and LINERs, the narrow-line region is resolved into biconical or even jet-like structures, indicating collimation of the ionizing radiation. Discrete clouds are frequently associated with corresponding radio structures. In contrast, for most Seyfert 1 galaxies the narrow-line region is unresolved, although the striking double cone structure we observe in NGC 4151 is a notable exception. The lack of extended structure in Seyfert 1 galaxies may be the result of two factors: i) we may be viewing the central engine along the axis of symmetry, fore-shortening any collimated structure, and ii) the axis of the central engine in Seyfert 1 galaxies may be preferentially tipped out of the plane of the parent galaxy. The UV image of NGC 1068 is constructed from FOS peak-up acquisitions using grating G270H and the 0.3'' aperture, and it resolves the continuum scattering region. Approximately 60 image arises from a region ~ 0.5'' in extent lying wholly within the ionizing cone defined by the [O III] emission line clouds observed by Evans et al. The remaining 40\ location of the continuum peak in the Lynds et al. F547M PC image. In addition to NGC 1068 and NGC 4151, we will present images of M51, M81, Mrk 3, Mrk 463 and an example of a Seyfert 1 with little or no extended [O III]: NGC3783. This work is supported by NASA Grant NAG 5-1630 to the FOS team.

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