A Search for "Dwarf" Seyfert Nuclei. V. Demographics of Nuclear Activity in Nearby Galaxies

Abstract

We use the sample of emission-line nuclei derived from a recently completed optical spectroscopic survey of nearby galaxies to quantify the incidence of local (z = 0) nuclear activity. Consistent with previous studies, we find detectable amounts of ionized gas in the central few hundred parsecs of most (86%) galaxies. Half of the objects can be classified as H II or star-forming nuclei and the other half as some form of AGN, of which we distinguish three classes --- Seyfert nuclei, LINERs, and transition objects. The population of AGNs consequently is very large; approximately 43% of the galaxies in our survey can be regarded as "active." Most of the objects have much lower luminosities than AGNs commonly studied; the median luminosity of the narrow H-alpha line, after correcting for extinction, is only 2 x 10^39 erg/s. Our sample therefore occupies the extreme faint end of the AGN luminosity function. We detect signatures of a broad-line region, as revealed by visible broad H-alpha emission, in $\sim$ 20% of the AGN sample. Seyfert nuclei, both type 1 and type 2, reside in $\sim$ 10% of all galaxies. LINERs make up the bulk (1/2--3/4) of the AGN population and a significant fraction (1/5--1/3) of all galaxies. A nonnegligible subset of LINERs emit broad H-alpha emission, furnishing direct evidence that at least some LINERs are indeed related physically to the AGN phenomenon. The dominant ionization mechanism of the nuclear emission depends strongly on the morphological type and luminosity of the host galaxy. AGNs are found predominantly in luminous, early-type (E to Sbc) galaxies, while H II nuclei prefer less luminous, late-type (Sbc and later) systems. The various AGN subclasses have broadly similar host galaxies.

To appear in the Astrophysical Journal. LaTex, 16 pages, plus an additional 10 figures and 2 tables. Uses AASTex macro aaspp4.sty

References in corpus (2)

• The Influence of Bars on Nuclear Activity
• Properties of H II Regions in the Centers of Nearby Galaxies

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