FOS Observations of Liner Galaxy Nuclei: Ultraviolet Clues to the Nature of the Liner Phenomenon - CYCLE3HIGH

Details FOS Observations of Liner Galaxy Nuclei: Ultraviolet Clues to the Nature of the Liner Phenomenon - CYCLE3HIGH FOS Observations of Liner Galaxy Nuclei: Ultraviolet Clues to the Nature of the Liner Phenomenon - CYCLE3HIGH

Jul 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993hst..prop.4350r&link_type=abstract

HST Proposal ID #4350

Physics

Hst Proposal Id #4350

Scientific paper

LINER galaxies potentially form a class of "dwarf" AGN, dominating the number densities of low luminosity AGN and their contribution to the diffuse X-ray background. LINERs also provide clues as to how star formation in galaxies might be triggered, and the relationship between star formation and nonthermal activity. Progress has been made at optical and radio wavelengths towards explaining the low-excitation, line-emitting gas observed in LINERs. However, the nature of this ubiquitous class of galaxies remains elusive primarily because the nuclear emission is swamped by galactic light at these wavelengths. Several models have been proposed -- shock heating, cooling flows, photoion- ization by "dwarf" AGN, and photoionization by hot stars or "Warmers". The direct spectral "signatures" of the nuclear emission can only be effectively studied in the UV where contamination from normal stars is much reduced. To understand the fundamental energetics of LINER galaxies, it is essential to characterize their UV continuum and determine the fluxes and profiles of the diagnostically important UV emission lines. The unique capabilities of HST offer us an unprecedented opportunity to isolate and study the nuclei of LINERs in the UV. We therefore propose FOS observations of a sample of LINERs, to 1) measure their UV continua accurately, 2) search for nonthermal (or stellar) photoionizing continua and also for UV absorption lines from hot young stars, and 3) measure the strengths and profiles of the UV emission lines.

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