Testing the Nature of ''Type 2'' LINERs Using UV Spectroscopy

Details Testing the Nature of ''Type 2'' LINERs Using UV Spectroscopy Testing the Nature of ''Type 2'' LINERs Using UV Spectroscopy

Dec 1997

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1997hst..prop.7357h&link_type=abstract

HST Proposal ID #7357

Physics

Hst Proposal Id #7357 Agn/Quasars

Scientific paper

LINERs, like Seyferts, come in two varieties: ``type 1'' have broad permitted lines and ``type 2'' only have narrow lines. While LINER 1s undoubtedly are genuine AGNs, the true nature of LINER 2s remains unknown. Since LINER 2s make up most of the LINER population, determining their ionization mechanism has become the key problem in understanding the origin of LINERs and their place in the AGN paradigm. The leading candidates for the energy source are photoionization {by an AGN-like continuum or by hot stars} and fast shocks. We propose to discriminate between these two mechanisms by means of UV and optical spectroscopy, since ionization by fast shocks predicts much stronger high-excitation UV lines such as C IV 1549, C III] 1909, and [Ne IV] 3426. In the cases where the UV continuum is strong enough, photoionization by hot stars can be further discerned through characteristic stellar absorption and/or P Cygni emission lines. We have selected two LINER 2 nuclei from our ground-based spectroscopic survey {NGC 3507 and NGC 4486 [M87]} for which we wish to acquire low-resolution { 500 km/s} STIS spectra covering the region 1150 to 10270 Angstrom.

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