2003MNRAS.346..897B

The bright type 1 Seyfert galaxy H1419+480 (z ∼ 0.072), whose X-ray colours from earlier HEAO-1 and ROSAT missions suggested a complex X-ray spectrum, has been observed with XMM-Newton. The EPIC spectrum above 2 keV is well fitted by a power law with photon index Γ 1.84±0.01 and an Fe Kα line of equivalent width ∼250 eV. At softer energies, a decrement with respect to this model extending from 0.5 to 1 keV is clearly detected. After trying a number of models, we find that the best fit corresponds to O VII absorption at the emission redshift, plus a 2σ detection of O VIII absorption. A photoionized gas model fit yields logξ∼ 1.15-1.30 (ξ in erg.cm/s) with N_H∼ 5x10²¹/cm2 for solar abundances. We find that the ionized absorber was weaker or absent in an earlier ROSAT observation. An International Ultraviolet Explorer spectrum of this source obtained two decades before shows a variable (within a year) C iv absorber outflowing with a velocity ∼1800 km/s. We show that both X-ray and ultraviolet absorptions are consistent with arising in the same gas, with varying ionization.