Table 5: Emission lines from the shocked gas of the southern ER.
Emission Rest wavel. Relative fluxa $V_{\rm peak}^{{b}}$ $V_{\rm blue}^{{c}}$ $V_{\rm red}^{{c}}$ Extinction
  (Å)   (km s-1) (km s-1) (km s-1) correctiond
Ne V 3425.86 $6.0\pm1.7$ $9.8\pm28.6$ $-247.6\pm47.2$ $260.7\pm46.1$ 2.06
Ne III 3868.75 $29.5\pm1.5$ $31.7\pm 8.2$ $-173.2\pm 6.7$ $236.4\pm 6.7$ 1.94
S II 4068.60 $41.2\pm2.1$ $31.7\pm 8.2$ $-114.5\pm 6.6$ $192.6\pm 8.1$ 1.90
S II 4076.35 $12.6\pm0.9$ $32.8\pm 9.4$ $-168.2\pm 9.0$ $237.2\pm 9.0$ 1.90
H$\delta$ 4101.73 $26.5\pm1.9$ $18.8\pm 8.0$ $-118.6\pm 9.1$ $215.2\pm12.1$ 1.89
H$\gamma$ 4340.46 $57.4\pm2.0$ $28.7\pm 7.2$ $-147.5\pm 5.5$ $210.5\pm 5.9$ 1.84
O III 4363.21 $10.4\pm1.3$ $32.9\pm 8.6$ $-168.9\pm 7.8$ $222.7\pm 7.8$ 1.84
Fe III 4658.05 $3.1\pm0.6$ $12.8\pm18.7$ $-232.3\pm28.6$ $259.6\pm28.1$ 1.76
He II 4685.7 $10.1\pm1.2$ $39.5\pm15.6$ $-170.9\pm20.0$ $224.2\pm20.0$ 1.75
H$\beta $ 4861.32 $149.8\pm2.9$ $34.1\pm 3.7$ $-175.1\pm 3.5$ $218.5\pm 2.0$ 1.71
O III 4958.91 $18.3\pm0.8$ $14.3\pm 6.2$ $-226.3\pm12.9$ $204.0\pm 6.0$ 1.68
O III 5006.84 $55.3\pm1.5$ $16.4\pm 7.0$ $-214.4\pm 5.8$ $215.6\pm 5.0$ 1.67
O I 5577.34 $3.5\pm0.4$ $38.5\pm 9.3$ $-141.2\pm10.0$ $214.8\pm10.0$ 1.57
N II 5754.59 $63.5\pm1.4$ $40.7\pm 5.9$ $-188.0\pm 3.6$ $207.9\pm 3.0$ 1.54
He I 5875.63 $49.7\pm1.2$ $38.2\pm 5.4$ $-215.0\pm 3.0$ $231.6\pm 4.9$ 1.53
O I 6300.30 $69.1\pm1.3$ $32.5\pm 5.1$ $-162.4\pm 1.8$ $193.7\pm 3.8$ 1.47
S III 6312.06 $2.6\pm0.4$ $24.7\pm12.5$ $-158.5\pm16.8$ $213.0\pm16.8$ 1.47
O I 6363.78 $21.7\pm0.8$ $27.1\pm 9.2$ $-143.7\pm 5.4$ $175.1\pm 3.7$ 1.47
N II 6548.05 $24.3\pm0.8$ $31.5\pm 6.0$ $-190.8\pm 4.1$ $196.6\pm 6.6$ 1.45
H$\alpha $ 6562.80 $582.0\pm8.7$ $36.0\pm 2.5$ $-190.9\pm 1.2$ $223.2\pm 0.9$ 1.45
N II 6583.45 $76.1\pm1.4$ $28.8\pm 3.6$ $-184.2\pm 2.9$ $194.2\pm 1.6$ 1.45
He I 6678.15 $10.0\pm0.5$ $31.4\pm 8.1$ $-188.4\pm 6.3$ $252.8\pm 6.3$ 1.44
S II 6716.44 $1.3\pm 0.2$ $20.1\pm10.0$ $-124.3\pm13.7$ $167.1\pm13.7$ 1.43
S II 6730.82 $3.1\pm0.4$ $27.5\pm10.3$ $-146.0\pm12.4$ $202.4\pm12.4$ 1.43
Ar III 7135.79 $5.9\pm0.6$ $19.6\pm14.5$ $-196.2\pm20.1$ $217.6\pm15.7$ 1.39
Fe II 7155.16 $11.2\pm0.5$ $14.1\pm 6.3 $ $-184.2\pm 9.1$ $199.8\pm 8.4$ 1.39
S III 9068.6 $6.8\pm0.8$ $-0.1\pm17.5$ $-272.7\pm24.0$ $240.4\pm42.0$ 1.24
S III 9531.10 $16.5\pm1.4$ $23.4\pm 8.5$ $-275.5\pm25.7$ $216.7\pm12.5$ 1.22
a Fluxes are relative to the flux of H$\beta $ of the unshocked component in the Northern ER: ``100`` corresponds to $(31.3\pm 0.5) \times 10^{-16}\rm ~erg~s^{-1}~cm^{-2}$. Fluxes are not corrected for the extinction. The errors are only statistical, and do not include systematic uncertaities (see text).
b The velocities are relative to the unshocked, narrow component of the emission lines.
c The velocity where fluxes are 5% of the peak flux.
d $E(B-V)=0.16~{\rm mag}$, with $E(B-V)=0.10~{\rm mag}$ for LMC and $E(B-V)=0.06~{\rm mag}$ for the Milky Way.

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