The bright Seyfert 1 galaxy H1419+480 ( z \sim 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 fit by a power-law with photon index \Gamma = 1.84 \pm 0.01 and an Fe K \alpha line of equivalent width \sim 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 OVII absorption at the emission redshift , plus a 2 \sigma detection of OVIII absorption .
A photoionised gas model fit yields \log \xi \sim 1.15 - 1.30 ( \xi in { erg } { cm } { s } ^ { -1 } ) with N _ { H } \sim 5 \times 10 ^ { 21 } { cm } ^ { -2 } for solar abundances .
We find that the ionized absorber was weaker or absent in an earlier ROSAT observation .
An IUE spectrum of this source obtained two decades before shows a variable ( within a year ) CIV absorber outflowing with a velocity \sim 1800 { km } { s } ^ { -1 } .
We show that both X-ray and UV absorptions are consistent with arising in the same gas , with varying ionisation .