The X-ray spectrum of NGC 7213 is known to present no evidence for Compton reflection , a unique result among bright Seyfert 1s .
The observed neutral iron K \alpha line , therefore , can not be associated with a Compton-thick material , like the disc or the torus , but is due to Compton-thin gas , with the Broad Line Region ( BLR ) as the most likely candidate .
To check this hypothesis , a long Chandra HETG observation , together with a quasi-simultaneous optical spectroscopic observation at the ESO NTT EMMI were performed .
We found that the iron line is resolved with a FWHM= 2 400 ^ { +1 100 } _ { -600 } km s ^ { -1 } , in perfect agreement with the value measured for the broad component of the H \alpha , 2640 ^ { +110 } _ { -90 } km s ^ { -1 } .
Therefore , NGC 7213 is the only Seyfert 1 galaxy whose iron K \alpha line is unambiguously produced in the BLR .
We also confirmed the presence of two ionised iron lines and studied them in greater detail than before .
The resonant line is the dominant component in the Fe xxv triplet , therefore suggesting an origin in collisionally ionised gas .
If this is the case , the blueshift of around 1 000 km s ^ { -1 } of the two ionised iron lines could be the first measure of the velocity of a starburst wind from its X-ray emission .