Table 2.
Emission lines of Haro 14 in the MUSE observed range for which line maps have been generated.
| Line | Ion | IP |
 |
 |
 |
|---|---|---|---|---|---|
| (Å) | (eV) | (10−14 ) | (10−14 ) | (10−19 ) | |
| 4861 (Hβ) | H I | 13.60 | 11.0 | 15.9 | 27 |
| 5007 | [O III] | 35.12 | 23.5 | 33.5 | 12 |
| 6300 | [O I] | 13.62 | 1.6 | 2.1 | 11 |
| 6563 (Hα) | H I | 13.60 | 35.4 | 45.6 | 9 |
| 6583 | [N II] | 14.53 | 4.1 | 5.3 | 8 |
| 6716, 6731 | [S II] | 10.36 | 10.8 | 13.9 | 10 |
| 7135 | [Ar III] | 27.63 | 1.0 | 1.3 | 8 |
| 9069 | [S III] | 23.34 | 2.2 | 2.5 | 15 |
Notes. IP: ionization potential of the ionization stage of the line, for recombination (H I) and charge exchange (O I) dominated lines; of the previous (lower) ionization stage for the rest of the forbidden lines (in italics). 
and 
are the observed and interstellar-extinction-corrected fluxes as measured in the integrated spectrum (units are 10−14 erg s−1 cm−2). 
is the limit surface brightness in units of 10−19 erg s−1 cm−2 arcsec−2.
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