The Structure of The Emission Line Regions of Compact Steep Spectrum Radio Sources.

Details The Structure of The Emission Line Regions of Compact Steep Spectrum Radio Sources. The Structure of The Emission Line Regions of Compact Steep Spectrum Radio Sources.

Jul 1995

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995hst..prop.5923a&link_type=abstract

HST Proposal ID #5923

Computer Science

Hst Proposal Id #5923 Agn

Scientific paper

Extended emission line regions {EELR} aligned with the radio structure have been found in AGN of all radio powers and redshifts. This alignment implies that the nuclear radiation is collimated. Generally the EELR of Seyfert galaxies stretch many Kpc beyond their radio structure and their ionization structure is dominated by the form of the nuclear radiation. In contrast the EELR in powerful radio sources are co-spatial with the radio structure. There, interactions with the radio ejecta are an important source of excitation. This contribution severly limits our ability to use the EELR as an aspect independent method of determining the role of beaming at high luminosity. The Compact Steep Spectrum sources have quasi-linear radio structure confined to small angular {<= 0.2 -1.5 ''} and spatial scales {<= 10 Kpc}. We believe that anisotropic radiation will excite EELR beyond the CSS radio emission, providing a high radio luminosity sample in which these effects are decoupled. This will allow a direct study of beaming in gas which is not interacting with the radio ejecta for a sample of sources with a wind range of intrinsic powers. In contrast on scales Co-spatial with the radio structure we expect to see the strong interactions manifested as NLR. We have already developed a true dynamical model for the formation of the NLR in Seyferts which explains both their velocity field and morphology. Resolving the emission structure of CSS and comparing this with the radio structure is essential in extending this modeling to the regime of more powerful ionizing radiation field and very large shock velocities. In principal finding and measuring displacemnts between the gas and radio emission in this region gives cooling times and hence shock velocities. Here we propose WFPC/2 emission line imagery of the CSS in CIV or OIII5007 to establish their emission line structure and its relationship to the radio structure.

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