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Table E.1

Broadening of the FIR lines (in km s-1).

Broadening Rotation


[N iii] 57 [O i] 63 [O iii] 88 [N ii] 122 [O i] 145 [C ii] 157 Axis Vrotation

PACS FWHM 105 85 125 290 260 240

Haro 2 n.a. 90 140 n.a. n.a.
Haro 3 100 90 110 NEE–SWW ±30 km s-1
Haro 11 160 130 200 200 100 160 N–S ±50 km s-1
He 2-10 160 100 170 NE–SW ±20 km s-1
HS 1330+3651 n.a. 150 n.a. n.a.
II Zw 40 n.a. 80 110 N–S ±30 km s-1
Mrk 1089 n.a. 80 130 NNE–SSW ±80 km s-1
Mrk 153 n.a. 80 120 n.a. n.a. NE–SW ±30 km s-1
Mrk 930 n.a. 120 120 N–S ±30 km s-1
NGC 1140 n.a. 100 100 NE–SW ±40 km s-1
NGC 1569 n.a. 80 100 n.a. n.a.
NGC 1705 n.a. 100 n.a. n.a.
NGC 2366 n.a. 80 70 n.a. n.a. -
NGC 4214 n.a. 80 80 -
SBS 1533+574 n.a. 80 n.a. n.a.
UM 448 n.a. 150 150 80 150 NNE–SSW ±60 km s-1
IC 10 n.a. 90 70 -
LMC 150 150 150 100 100
SMC n.a. 150 150 n.a. n.a.
NGC 4449 n.a. 90 90
NGC 5253 n.a. 60 90 NE–SW ±30 km s-1
NGC 6822 n.a. 100 80

Notes. The broadening (or intrinsic line width) is given as the observed FWHM subtracted by the instrumental FWHM. Uncertainties are on the order of 20%. We indicate the broadening of the spaxel where the emission peaks. This value can be higher elsewhere because of rotation or instrumental effects (uncentered point-source).

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