OUTFLOWING DIFFUSE GAS IN THE ACTIVE GALACTIC NUCLEUS OF NGC 1068

Spectra of the archetypal Type II Seyfert galaxy NGC 1068 in a narrow wavelength interval near 3.7 mu m have revealed a weak absorption feature due to two lines of the molecular ion H-3(+). The observed wavelength of the feature corresponds to a velocity of -70 km s(-1) relative to the systemic velocity of the galaxy, implying an outward flow from the nucleus along the line of sight. The absorption by H-3(+) along with the previously known broad hydrocarbon absorption at 3.4 mu m are probably formed in diffuse gas that is in close proximity to the continuum source, i.e., within a few tens of parsecs of the central engine. Based on that conclusion and the measured H-3(+) absorption velocity and with the assumption of a spherically symmetric wind we estimate a rate of mass outflow from the active galactic nucleus of similar to 1 M(circle dot)yr(-1).