profiles, with a broadening up to 300 km s$^{-1}$, which suggests that both the neutral and ionised gas are coming from several components with different velocities. However, with spectral resolution $>$100 km s$^{-1}$, the lines are well fitted by a single Gaussian and we cannot separate the different velocity components in the spectra. This suggested complex velocity structure is corroborated by studies of optical lines that show broad profiles as well [@kunth-1998; @ostlin-1999], and where the neutral gas is shifted compared to the ionised gas, expanding over few kpcs [@kunth-2003]. FUSE spectra in [@grimes-2007] show absorption lines of the ISM with FWHM 300 km s$^{-1}$ and blueshifted by 80 km s$^{-1}$. The higher ionisation lines can be stronger in galactic outflows [@contursi-2012].

![image](19818f05){width="18cm"}

The \[C [ii]{}\] line shows a marginally extended emission at 157 $\mu$m, peaking at a signal-to-noise ratio of 50 in the center and dropping below detection at the edge of the map. The emission of the other lines is rather compact. The shape of the PACS spectrometer beam is not known well enough to measure an accurate source size if the source were slightly extended. Hence we cannot recover spatial information. To derive total line intensities, we 