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We present a detailed analysis of a highly ionized, multiphased and collimated outflowing gas detected through O  v , O  vi , Ne  viii  and Mg  x  absorption associated with the QSO HE 0238–1904 ( z  em ≃ 0.629). Based on the similarities in the absorption‐line profiles and estimated covering fractions, we find that the O  vi  and Ne  viii  absorption trace the same phase of the absorbing gas. Simple photoionization models can reproduce the observed ,  and  from a single phase whereas the low‐ionization species (e.g. N  iii , N  iv  and O  iv ) originate from a different phase. The measured  ratio is found to be remarkably similar (within a factor of ∼2) in several individual absorption components kinematically spread over ∼1800 km s −1 . Under photoionization this requires a fine‐tuning between hydrogen density ( n  H ) and the distance of the absorbing gas from the Quasi Stellar Object (QSO). Alternatively, this can also be explained by collisional ionization in hot gas with  T ≥ 10 5.7  K. Long‐term stability favours the absorbing gas being located outside the broad‐line region. We speculate that the collimated flow of such a hot gas could possibly be triggered by the radio jet interaction.

Highly ionized collimated outflow from HE 0238–1904