Origin of the Coronal Line Emission in NGC1068

Details Origin of the Coronal Line Emission in NGC1068 Origin of the Coronal Line Emission in NGC1068

Feb 1997

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1997ap%26ss.248..113m&link_type=abstract

Astrophysics and Space Science, Volume 248, Issue 1-2, pp. 113-120

Astronomy and Astrophysics

Astrophysics

2

Scientific paper

We present recent observations of several near infrared emission lines of highly ionized (IP ≱ 100eV) species in NGC1068 which appear to be emitted predominantly within the NE ionization cone; peak at ≱ 30pc from the nucleus and are blueshifted by ≃ 300 km s-1 relative to the systemic velocity. The blueshift is the same as that observed for the better known Fe coronal lines in the visible and the absence of red-shifted components in the less extincted infrared lines suggests that any emission in the counter-cone to the SW is intrinsically faint rather than heavily obscured. Following a review of the possible ionization mechanisms and comparison of the line ratios with recent models we conclude that the coronal emission arises predominantly in outflowing gas photoionized by the EUV continuum of the AGN.

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