High-resolution X-ray and ultraviolet spectroscopy of the complex intrinsic absorption in NGC 4051 with Chandra and the Hubble Space Telescope

We present the results from simultaneous observations of the narrow-line Se yfert 1 galaxy NGC 4051 with the Chandra High Energy Transmission Grating S pectrometer and the Hubble Space Telescope Space Telescope Imaging Spectrog raph. The X-ray grating spectrum reveals absorption and emission lines from hydrogen-like and helium-like ions of O, Ne, Mg, and Si. We resolve two di stinct X-ray absorption systems: a high-velocity blueshifted system at -234 0 +/- 130 km s(-1) and a low-velocity blue-shifted system at -600 +/- 130 k m s(-1). In the UV spectrum we detect strong absorption, mainly from C IV, N V, and Si IV, that is resolved into as many as nine different intrinsic a bsorption systems with velocities between -650 and 30 km s(-1). Although th e low-velocity X-ray absorption is consistent in velocity with many of the UV absorption systems, the high-velocity X-ray absorption seems to have no UV counterpart. In addition to the absorption and emission lines, we also o bserve rapid X-ray variability and a state of low X-ray flux during the las t approximate to 15 ks of the observation. NGC 4051 has a soft X-ray excess that we fit in both the high and low X-ray flux states. The high-resolutio n X-ray spectrum directly reveals that the soft excess is not composed of n arrow emission lines and that it has significant spectral curvature. A powe r-law model fails to fit it, while a blackbody produces a nearly acceptable fit. We compare the observed spectral variability with the results of prev ious studies of NGC 4051.