Evidence of Cross-Fueling in Active Galaxies

We discuss four interacting pairs of galaxies with emission from tidally stripped ionized gas. Three of the pairs (Kar 29, Arp 194, and ESO 253-IG026) host a collisional ring galaxy, and a head-on collision cannot be ruled out even in the fourth case (NGC 7592). Emitting regions are revealed outside the disk of the ring galaxies, either in the form of a bright filament or of blobs. Long-slit spectroscopic data reveal gas kinematics dominated by non-rotational motions. We are able to show that ionized gas in the vicinity (from a few kpc down to our resolution limit, several hundred pc) of one member galaxy in each of these systems is most probably falling toward the nucleus. Extended LINER-like emission with relatively broad lines---indicative of shock heating, probably due to collision of tidally stripped molecular clouds---is observed in two objects (ESO 253-IG026 and Kar 29). The nuclear spectra of the remaining two systems show dominant H ii emission associated with star formation, with some evidence suggesting a low-luminosity, obscured active nucleus. None of the four galaxy pairs hosts a luminous Seyfert 1 nucleus. The observed phenomenology---including the notable LINER-like emission---has apparently been produced within ~108 yr from the pair's closest approach. We may not be able to observe clear evidence of infall from ionized gas in Seyfert 1 galaxies if the inception of luminous, unobscured, type 1 activity requires a much longer timescale

Multiwavelength observations of short-timescale variability in NGC 4151 .4. Analysis of multiwavelength continuum variability

This paper combines data from the three preceding papers in order to analyze the multi-wave-band variability and spectral energy distribution of the Seyfert 1 galaxy NGC 4151 during the 1993 December monitoring campaign. The source, which was near its peak historical brightness, showed strong, correlated variability at X-ray, ultraviolet, and optical wavelengths. The strongest variations were seen in medium-energy (similar to 1.5 keV) X-rays, with a normalized variability amplitude (NVA) of 24%. Weaker (NVA = 6%) variations (uncorrelated with those at lower energies) were seen at soft gamma-ray energies of similar to 100 keV. No significant variability was seen in softer (0.1-1 keV) X-ray bands. In the ultraviolet/optical regime, the NVA decreased from 9% to 1% as the wavelength increased from 1275 to 6900 Angstrom These data do not probe extreme ultraviolet (1200 Angstrom to 0.1 keV) or hard X-ray (2-50 keV) variability. The phase differences between variations in different bands were consistent with zero lag, with upper limits of less than or similar to 0.15 day between 1275 Angstrom and the other ultraviolet bands, less than or similar to 0,3 day between 1275 Angstrom and 1.5 keV, and less than or similar to 1 day between 1275 and 5125 Angstrom These tight limits represent more than an order of magnitude improvement over those determined in previous multi-wave-band AGN monitoring campaigns. The ultraviolet fluctuation power spectra showed no evidence for periodicity, but were instead well fitted with a very steep, red power law (a less than or equal to -2.5). If photons emitted at a ''primary'' wave band are absorbed by nearby material and ''reprocessed'' to produce emission at a secondary wave band, causality arguments require that variations in the secondary band follow those in the primary band. The tight interband correlation and limits on the ultraviolet and medium-energy X-ray lags indicate that the reprocessing region is smaller than similar to 0.15 it-day in size. After correcting for strong (a factor of greater than or similar to 15) line-of-sight absorption, the medium-energy X-ray luminosity variations appear adequate to drive the ultraviolet/optical variations. However, the medium-energy X-ray NVA is 2-4 times that in the ultraviolet, and the single-epoch, absorption-corrected X-ray/gamma-ray luminosity is only about one-third of that of the ultraviolet/optical/infrared, suggesting that at most about a third of the total low-energy flux could be reprocessed high-energy emission. The strong wavelength dependence of the ultraviolet NVAs is consistent with an origin in an accretion disk, with the variable emission coming from the hotter inner regions and nonvariable emission from the cooler outer regions. These data, when combined with the results of disk fits, indicate a boundary between these regions near a radius of order R approximate to 0.07 1t-day. No interband lag would be expected, as reprocessing (and thus propagation between regions) need not occur, and the orbital timescale of similar to 1 day is consistent with the observed variability timescale. However, such a model does not immediately explain the good correlation between ultraviolet and X-ray variations