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Up: Nebular abundances of nearby

   
4 Measurements and analysis

Emission-line strengths were measured using locally-developed software. Flux ratios were corrected for underlying Balmer absorption with an equivalent width 2 Å (McCall et al. 1985). Corrections and analyses were performed with SNAP (Spreadsheet Nebular Analysis Package, Krawchuk et al. 1997). In the absence of [O III] $\lambda 4363$, the electron temperature was assumed to be Te = 104 K for computations. Where the density-dependent line ratio, I([S II] $\lambda 6716$)/I([S II] $\lambda 6731$), could not be formed, a value of ne = 100 cm-3 was adopted. Values of the reddening are derived using H$\alpha $ and H$\beta $ fluxes with the method described in Lee et al. (2003a). Errors in the reddening are computed from the maximum and minimum values of the reddening based upon $2\sigma$ errors in fits to emission lines.

Observed flux (F) and corrected intensity (I) ratios are listed in Tables 4 to 7 inclusive. The listed errors for the observed flux ratios at each wavelength $\lambda $ account for the errors in the fits to the line profiles, their surrounding continua, and the relative error in the sensitivity function stated in Table 3. Errors for observed ratios do not include the error in the flux at the H$\beta $ reference line. The uncertainty in the correction for underlying Balmer absorption was assumed to be zero. Errors in the corrected intensity ratios account for maximum and minimum errors in the flux of the specified line and of the H$\beta $ reference line; errors in the reddening are not included.

 

 
Table 4: Observed and corrected line ratios for Centaurus A group dwarf galaxies. Wavelengths are listed in Å. For a given galaxy whose H II regions have not been previously identified (see Table 3), the number of the H II region aperture extraction increases to the east. F is the observed flux ratio with respect to H$\beta $. I is the corrected intensity ratio, corrected for underlying Balmer absorption and the adopted reddening listed in Table 8. The errors in the observed line ratios account for the errors in the fits to the line profiles, the surrounding continua, and the relative error in the sensitivity function listed in Table 3; flux errors in the H$\beta $ reference line are not included. Errors in the corrected line ratios account for errors in the specified line and in the H$\beta $ reference line.
  A1243-335 H II#A A1324-412 ap1 A1334-277 ap1
Identification (Å) F I F I F I
$[{\rm O\;II}]\;3727$ $107 \pm 15$ $117 \pm 31$ ... ... $105 \pm 15$ $94 \pm 31$
${\rm H}\beta\;4861$ $100 \pm 10$ $100 \pm 12$ $100 \pm 15$ $100 \pm 19$ $100 \pm 13$ $100 \pm 17$
$[{\rm O\;III}]\;4959$ $163.0 \pm 7.1$ $145 \pm 26$ ... ... $70 \pm 12$ $63 \pm 22$
$[{\rm O\;III}]\;5007$ $456.6 \pm 8.5$ $405 \pm 65$ ... ... $176 \pm 14$ $158 \pm 43$
${\rm H}\alpha\;6563$ $357.4 \pm 7.5$ $286 \pm 47$ $366 \pm 20$ $286 \pm 80$ $291 \pm 12$ $268 \pm 66$
$[{\rm N\;II}]\;6583$ $4.7 \pm 6.1$ $3.7 \pm 5.3$ ... ... $12 \pm 10$ $10 \pm 11$
  A1346-358 H II#A DDO 161 ap1 NGC 5264 ap1
Identification (Å) F I F I F I
$[{\rm O\;II}]\;3727$ $235.5 \pm 1.9$ $415 \pm 36$ $190.5 \pm 3.6$ $315 \pm 29$ $377 \pm 20$ $390 \pm 61$
He II 3834 + H9 $5.3 \pm 1.0$ $13.9 \pm 4.5$ ... ... ... ...
$[{\rm Ne\;III}]\;3869$ $19.8 \pm 1.2$ $31.7 \pm 3.7$ ... ... ... ...
He I 3889 + H8 $18.3 \pm 1.2$ $33.7 \pm 4.4$ ... ... ... ...
$[{\rm Ne\;III}]\;3967 + {\rm H}\epsilon$ $19.05 \pm 0.77$ $32.8 \pm 3.5$ ... ... ... ...
${\rm H}\delta\;4101$ $20.29 \pm 0.79$ $31.7 \pm 3.3$ $14.4 \pm 1.9$ $26.7 \pm 6.2$ ... ...
${\rm H}\gamma\;4340$ $47.14 \pm 0.75$ $60.6 \pm 5.4$ $46.4 \pm 2.4$ $61.4 \pm 7.3$ $27.3 \pm 8.3$ $43 \pm 25$
$[{\rm O\;III}]\;4363$ $1.93 \pm 0.59$ $2.34 \pm 0.82$ < 6.6 < 7.7 ... ...
He I 4472 $3.52 \pm 0.53$ $4.04 \pm 0.81$ ... ... ... ...
${\rm H}\beta\;4861$ $100.0 \pm 1.4$ $100.0 \pm 4.4$ $100.0 \pm 2.1$ $100.0 \pm 4.8$ $100.0 \pm 7.2$ $100.0 \pm 9.3$
$[{\rm O\;III}]\;4959$ $95.6 \pm 2.3$ $90.6 \pm 8.3$ $92.8 \pm 2.3$ $85.9 \pm 8.2$ $34.4 \pm 5.7$ $28.8 \pm 7.6$
$[{\rm O\;III}]\;5007$ $292.8 \pm 2.8$ $273 \pm 24$ $278.9 \pm 2.8$ $254 \pm 23$ $83.4 \pm 7.1$ $69 \pm 13$
He I 5876 $15.46 \pm 0.50$ $11.4 \pm 1.1$ $17.0 \pm 1.9$ $12.4 \pm 2.1$ ... ...
$[{\rm N\;II}]\;6548$ $15.3 \pm 2.7$ $9.9 \pm 2.2$ ... ... $20.4 \pm 7.6$ $15.0 \pm 7.1$
${\rm H}\alpha\;6563$ $443.0 \pm 3.4$ $286 \pm 25$ $440.2 \pm 3.0$ $286 \pm 26$ $374.6 \pm 9.5$ $286 \pm 39$
$[{\rm N\;II}]\;6583$ $39.6 \pm 2.7$ $25.4 \pm 3.2$ $8.9 \pm 2.5$ $5.7 \pm 1.9$ $63.6 \pm 7.8$ $47 \pm 10$
He I 6678 $4.04 \pm 0.68$ $2.55 \pm 0.56$ ... ... ... ...
$[{\rm S\;II}]\;6716$ $39.45 \pm 0.80$ $24.8 \pm 2.2$ $22.0 \pm 2.0$ $13.9 \pm 2.0$ $93.4 \pm 7.7$ $68 \pm 12$
$[{\rm S\;II}]\;6731$ $27.45 \pm 0.75$ $17.2 \pm 1.4$ $15.8 \pm 1.9$ $10.0 \pm 1.7$ $60.5 \pm 7.2$ $44.0 \pm 9.6$



 

 
Table 5: Observed and corrected line ratios for Sculptor group dwarf galaxies; same comments as Table 4. NOTE: a The recession velocity of emission lines is $v_{\odot }/c \simeq +0.11$, placing this galaxy in the background. No corrections are applied.
  AM0106-382 ap1 AM0106-382 ap2 AM0106-382 ap3
Identification (Å) F I F I F I
$[{\rm O\;II}]\;3727$ $168 \pm 21$ $155 \pm 40$ $165 \pm 15$ $149 \pm 29$ $178 \pm 17 $ $158 \pm 31$
${\rm H}\beta\;4861$ $100.0 \pm 9.9$ $100.0 \pm 12$ $100.0 \pm 6.4$ $100.0 \pm 8.9$ $100.0 \pm 6.4$ $100.0 \pm 8.9$
$[{\rm O\;III}]\;4959$ $22.3 \pm 7.7$ $20.6 \pm 9.8$ $37.6 \pm 4.7$ $33.9 \pm 7.6$ $45.8 \pm 5.7$ $40.6 \pm 9.1$
$[{\rm O\;III}]\;5007$ $62.4 \pm 7.9$ $58 \pm 15$ $124.8 \pm 5.8$ $113 \pm 18$ $162.1 \pm 7.1$ $144 \pm 22$
$[{\rm N\;II}]\;6548$ ... ... $1.3 \pm 4.2$ $1.1 \pm 3.9$ $2.8 \pm 3.9$ $2.5 \pm 3.7$
${\rm H}\alpha\;6563$ $239.7 \pm 8.9$ $225 \pm 42$ $266.2 \pm 5.3$ $245 \pm 35$ $287.4 \pm 4.9$ $260 \pm 37$
$[{\rm N\;II}]\;6583$ $12.4 \pm 7.2$ $11.4 \pm 8.1$ $7.0 \pm 4.3$ $6.3 \pm 4.4$ $5.02 \pm 3.9$ $4.4 \pm 3.9$
$[{\rm S\;II}]\;6716$ $39.8 \pm 8.0$ $37 \pm 12$ $29.1 \pm 5.2$ $26.3 \pm 7.2$ $23.3 \pm 4.1$ $20.6 \pm 5.6$
$[{\rm S\;II}]\;6731$ $20.7 \pm 7.0$ $19.1 \pm 8.9$ $15.2 \pm 4.4$ $13.7 \pm 5.2$ $15.7 \pm 3.3$ $13.9 \pm 4.3$
  ESO 347-G017 ap1 ESO 347-G017 ap2 ESO 347-G017 ap3
Identification (Å) F I F I F I
$[{\rm O\;II}]\;3727$ $215.3 \pm 3.4$ $200 \pm 22$ $159.7 \pm 4.2$ $171 \pm 21$ $244 \pm 21$ $296 \pm 69$
$[{\rm Ne\;III}]\;3869$ $39.0 \pm 4.3$ $36.1 \pm 6.5$ $44.2 \pm 6.4$ $45.5 \pm 9.9$ ... ...
${\rm H}\gamma\;4340$ $33.5 \pm 1.9$ $42.7 \pm 6.5$ $28.0 \pm 3.1$ $41.7 \pm 9.3$ ... ...
$[{\rm O\;III}]\;4363$ <4.9 (2$\sigma $) <4.4 (2$\sigma $) <4.2 (2$\sigma $) <4.4 (2$\sigma $) ... ...
${\rm H}\beta\;4861$ $100.0 \pm 2.3$ $100.0 \pm 5.8$ $100.0 \pm 3.5$ $100.0 \pm 6.5$ $100 \pm 10$ $100 \pm 13$
$[{\rm O\;III}]\;4959$ $109.2 \pm 3.2$ $98 \pm 11$ $136.0 \pm 3.1$ $118 \pm 14$ $72.6 \pm 6.8$ $62 \pm 14$
$[{\rm O\;III}]\;5007$ $312.4 \pm 3.9$ $281 \pm 31$ $414.0 \pm 3.8$ $359 \pm 42$ $192.5 \pm 8.4$ $160 \pm 31$
${\rm He\;I}\;5876$ $17.2 \pm 2.7$ $15.4 \pm 3.4$ $20.3 \pm 2.4$ $16.3 \pm 3.1$ ... ...
$[{\rm N\;II}]\;6548$ $8.7 \pm 2.8$ $7.7 \pm 2.9$ $7.0 \pm 2.7$ $5.6 \pm 2.5$ ... ...
${\rm H}\alpha\;6563$ $315.9 \pm 3.5$ $286 \pm 31$ $363.6 \pm 3.4$ $286 \pm 33$ $418 \pm 12$ $286 \pm 55$
$[{\rm N\;II}]\;6583$ $11.8 \pm 2.9$ $10.5 \pm 3.2$ $12.2 \pm 2.8$ $9.6 \pm 2.8$ $10.8 \pm 9.8$ $5.8 \pm 7.7$
$[{\rm S\;II}]\;6716$ $42.0 \pm 1.8$ $37.0 \pm 4.6$ $24.6 \pm 2.0$ $18.7 \pm 3.0$ $41.9 \pm 7.9$ $27.8 \pm 9.1$
$[{\rm S\;II}]\;6731$ $25.3 \pm 1.6$ $22.3 \pm 3.1$ $17.3 \pm 1.9$ $13.1 \pm 2.4$ $20.7 \pm 6.3$ $13.7 \pm 6.1$
  ESO 348-G009 ap1 ESO 348-G009 ap2 a UGCA 442 H II#2
Identification (Å) F I F I F I
$[{\rm O\;II}]\;3727$ $317 \pm 29$ $283 \pm 72$ $589 \pm 54$ ... $221.4 \pm 4.9$ $237 \pm 27$
${\rm H}\gamma\;4340$ ... ... ... ... $36.2 \pm 2.4$ $47.3 \pm 7.6$
$[{\rm O\;III}]\;4363$ ... ... ... ... <3.8 (2$\sigma $) <3.6 (2$\sigma $)
${\rm H}\beta\;4861$ $100 \pm 12$ $100 \pm 15$ $100 \pm 33$ ... $100.0 \pm 2.5$ $100.0 \pm 5.9$
$[{\rm O\;III}]\;4959$ $53 \pm 10$ $47 \pm 16$ $101 \pm 32$ ... $53.6 \pm 2.2$ $47.5 \pm 5.9$
$[{\rm O\;III}]\;5007$ $118 \pm 12$ $106 \pm 28$ $583 \pm 41$ ... $155.0 \pm 2.7$ $137 \pm 15$
${\rm He\;I}\;5876$ ... ... ... ... $16.5 \pm 2.8$ $13.5 \pm 3.2$
$[{\rm N\;II}]\;6548$ ... ... ... ... $6.3 \pm 2.3$ $4.9 \pm 2.2$
${\rm H}\alpha\;6563$ $254.1 \pm 9.1$ $233 \pm 49$ ... ... $356.2 \pm 2.9$ $286 \pm 32$
$[{\rm N\;II}]\;6583$ $10.7 \pm 7.3$ $9.6 \pm 8.0$ ... ... $14.3 \pm 2.4$ $11.3 \pm 2.6$
$[{\rm S\;II}]\;6716$ $44.2 \pm 7.7$ $39 \pm 13$ ... ... $36.8 \pm 1.5$ $28.7 \pm 3.6$
$[{\rm S\;II}]\;6731$ $20.6 \pm 5.9$ $18.4 \pm 8.1$ ... ... $22.7 \pm 1.4$ $17.7 \pm 2.5$



  \begin{figure} \par\includegraphics[width=16.7cm,clip]{h3953_f1.ps} % \end{figure} Figure 1: Long-slit spectra. The flux per unit wavelength is plotted against wavelength in each panel.


  \begin{figure} \par\includegraphics[angle=-90,width=11.2cm,clip]{h3953_f2.ps} % \end{figure} Figure 2: IC 1613 H II#37: The spectrum is redisplayed to highlight faint emission lines and broad Wolf-Rayet (W-R) features. The forbidden line [Ar IV]$\lambda $4711 is likely blended with He I$\lambda $4713.


 

 
Table 6: Observed and corrected line ratios for other southern dwarf galaxies; same comments as Table 4. ESO302-G014 #1 is not included here, as only [O III] $\lambda 5007$ and H$\alpha $ were detected; the measured fluxes in ergs s-1 cm-2 are $(2.13 \pm 0.44) \times 10^{-15}$ and $(2.73 \pm 0.43) \times 10^{-15}$, respectively. NOTE: a A broad Wolf-Rayet feature was detected near He I$\lambda $4472.
  A0355-465 H II#B ESO358-G060 ap1 IC 1613 H II#13
Identification (Å) F I F I F I
$[{\rm O\;II}]\;3727$ $185.9 \pm 5.3$ $277 \pm 28$ $66.1 \pm 4.9$ $64 \pm 12$ $256.7 \pm 6.1$ $251 \pm 28$
$[{\rm Ne\;III}]\;3869$ $41.8 \pm 7.0$ $58 \pm 13$ $7.2 \pm 2.1$ $7.0 \pm 2.6$ ... ...
He I 3889 + H8 $16.7 \pm 5.6$ $31 \pm 16$ $8.5 \pm 2.7$ $11.5 \pm 6.0$ ... ...
$[{\rm Ne\;III}]\;3967 + {\rm H}\epsilon$ $19.1 \pm 4.9$ $32 \pm 12$ $9.7 \pm 2.7$ $12.8 \pm 6.0$ $19.08 \pm 4.1$ $22.9 \pm 7.5$
${\rm H}\delta\;4101$ $29.8 \pm 4.5$ $43 \pm 10$ $20.5 \pm 3.8$ $23.2 \pm 7.2$ $20.9 \pm 3.4$ $24.0 \pm 6.1$
${\rm H}\gamma\;4340$ $45.5 \pm 4.5$ $57.1 \pm 9.6$ $42.8 \pm 3.4$ $45.0 \pm 8.7$ $38.8 \pm 3.1$ $41.1 \pm 6.5$
$[{\rm O\;III}]\;4363$ <6.4 (2$\sigma $) <7.1 (2$\sigma $) <5.8 (2$\sigma $) <5.6 (2$\sigma $) <7.3 (2$\sigma $) <7.1 (2$\sigma $)
${\rm H}\beta\;4861$ $100.0 \pm 2.8$ $100.0 \pm 5.1$ $100.0 \pm 4.1$ $100.0 \pm 8.1$ $100.0 \pm 2.3$ $100.0 \pm 5.7$
$[{\rm O\;III}]\;4959$ $166.8 \pm 5.2$ $156 \pm 16$ $68.7 \pm 2.8$ $66 \pm 11$ $67.1 \pm 1.6$ $65.6 \pm 7.3$
$[{\rm O\;III}]\;5007$ $486.1 \pm 6.4$ $450 \pm 43$ $202.4 \pm 3.4$ $196 \pm 29$ $204.4 \pm 1.9$ $200 \pm 22$
${\rm He\;I}\;5876$ ... ... ... ... $11.4 \pm 4.3$ $11.2 \pm 4.9$
$[{\rm N\;II}]\;6548$ ... ... ... ... $7.3 \pm 1.7$ $7.2 \pm 2.1$
${\rm H}\alpha\;6563$ $403.6 \pm 3.7$ $286 \pm 27$ $258.2 \pm 3.2$ $251 \pm 37$ $227.5 \pm 2.1$ $223 \pm 24$
$[{\rm N\;II}]\;6583$ $15.6 \pm 3.0$ $10.9 \pm 2.7$ $4.5 \pm 2.6$ $4.4 \pm 2.9$ $10.9 \pm 1.7$ $10.7 \pm 2.4$
$[{\rm S\;II}]\;6716$ $32.6 \pm 3.5$ $22.5 \pm 3.8$ $12.3 \pm 2.1$ $11.9 \pm 3.2$ $19.7 \pm 1.8$ $19.3 \pm 3.1$
$[{\rm S\;II}]\;6731$ $23.1 \pm 3.3$ $15.9 \pm 3.2$ $6.0 \pm 1.7$ $5.8 \pm 2.2$ $11.2 \pm 1.6$ $10.9 \pm 2.3$
  IC 1613 H II#37 IC 2032 ap1 IC 5152 H II#A
Identification (Å) F I F I F I
$[{\rm O\;II}]\;3727$ $61.0 \pm 1.6$ $70.1 \pm 7.7$ $320 \pm 28$ $286 \pm 59$ $220.0 \pm 2.5$ $211 \pm 22$
He II 3834 + H9 $6.3 \pm 1.1$ $7.9 \pm 2.1$ ... ... ... ...
$[{\rm Ne\;III}]\;3869$ $47.7 \pm 1.4$ $53.5 \pm 6.0$ $55 \pm 14$ $49 \pm 18$ $21.3 \pm 2.7$ $20.3 \pm 3.8$
He I 3889 + H8 $15.6 \pm 1.2$ $18.0 \pm 2.7$ ... ... $12.5 \pm 2.1$ $16.9 \pm 4.7$
$[{\rm Ne\;III}]\;3967 + {\rm H}\epsilon$ $31.6 \pm 1.1$ $35.2 \pm 4.1$ ... ... $11.7 \pm 2.0$ $16.4 \pm 4.7$
${\rm H}\delta\;4101$ $20.16 \pm 0.89$ $22.3 \pm 2.7$ ... ... $18.3 \pm 1.8$ $22.5 \pm 4.2$
${\rm H}\gamma\;4340$ $47.52 \pm 0.84$ $50.4 \pm 5.4$ ... ... $42.1 \pm 1.3$ $45.1 \pm 5.2$
$[{\rm O\;III}]\;4363$ $13.83 \pm 0.70$ $14.5 \pm 1.8$ ... ... $3.6 \pm 1.1$ $3.4 \pm 1.2$
He I 4472 ... a ... ... ... $5.98 \pm 0.89$ $5.7 \pm 1.2$
He II 4686 $21.45 \pm 0.85$ $21.7 \pm 2.5$ ... ... ... ...
He I 4713 $4.31 \pm 0.68$ $4.35 \pm 0.96$ ... ... ... ...
$[{\rm Ar\;IV}]\;4740$ $2.01 \pm 0.68$ $2.02 \pm 0.80$ ... ... ... ...
${\rm H}\beta\;4861$ $100.0 \pm 1.6$ $100.0 \pm 5.3$ $100.0 \pm 9.4$ $100 \pm 11$ $100.0 \pm 1.3$ $100 \pm 5.3$
$[{\rm O\;III}]\;4959$ $176.2 \pm 4.4$ $174 \pm 19$ $79.0 \pm 7.6$ $70 \pm 15$ $98.1 \pm 3.4$ $94 \pm 11$
$[{\rm O\;III}]\;5007$ $531.6 \pm 5.5$ $523 \pm 55$ $213.9 \pm 9.3$ $189 \pm 32$ $294.3 \pm 4.2$ $282 \pm 30$
${\rm He\;I}\;5876$ $6.94 \pm 0.68$ $6.4 \pm 1.1$ ... ... $12.7 \pm 1.3$ $12.1 \pm 2.0$
$[{\rm O\;I}]\;6300$ $4.35 \pm 0.77$ $3.95 \pm 0.94$ ... ... $5.59 \pm 0.76$ $5.4 \pm 1.1$
$[{\rm S\;III}]\;6312$ $1.11 \pm 0.67$ $1.01 \pm 0.67$ ... ... ... ...
$[{\rm O\;I}]\;6363$ $1.78 \pm 0.59$ $1.62 \pm 0.63$ ... ... $1.38 \pm 0.60$ $1.32 \pm 0.65$
$[{\rm N\;II}]\;6548$ $4.6 \pm 2.2$ $4.1 \pm 2.3$ ... ... $11.4 \pm 2.8$ $10.9 \pm 3.3$
${\rm H}\alpha\;6563$ $307.0 \pm 2.8$ $277 \pm 29$ $316.6 \pm 8.94$ $286 \pm 46$ $270.8 \pm 3.5$ $262 \pm 27$
$[{\rm N\;II}]\;6583$ $4.7 \pm 2.3$ $4.2 \pm 2.3$ $19.8 \pm 7.2$ $17.4 \pm 8.4$ $20.8 \pm 2.9$ $20.0 \pm 4.0$
${\rm He\;I}\;6678$ $2.29 \pm 0.46$ $2.05 \pm 0.53$ ... ... $4.54 \pm 0.53$ $4.34 \pm 0.78$
$[{\rm S\;II}]\;6716$ $12.93 \pm 0.54$ $11.6 \pm 1.4$ $48.3 \pm 8.3$ $42 \pm 12$ $19.93 \pm 0.59$ $19.1 \pm 2.1$
$[{\rm S\;II}]\;6731$ $8.45 \pm 0.50$ $7.55 \pm 0.99$ $42.9 \pm 8.3$ $38 \pm 12$ $14.35 \pm 0.56$ $13.7 \pm 1.6$



 

 
Table 7: Observed and corrected line ratios for other southern dwarf galaxies; same comments as Table 4.
  NGC 2915 ap1 NGC 2915 ap2 NGC 3109 H II#6 ap1 NGC 3109 H II#6 ap2
Identification (Å) F I F I F I F I
$[{\rm O\;II}]\;3727$ $396 \pm 15$ $660 \pm 110$ $306 \pm 35$ $440 \pm 110$ $178 \pm 26$ $152 \pm 60$ $65 \pm 16$ $51 \pm 25$
${\rm H}\beta\;4861$ $100.0 \pm 7.5$ $100 \pm 12$ $100.0 \pm 9.4$ $100 \pm 12$ $100 \pm 18$ $100 \pm 23$ $100 \pm 17$ $100 \pm 23$
$[{\rm O\;III}]\;4959$ $198.9 \pm 7.7$ $115 \pm 20$ $63 \pm 10$ $54 \pm 15$ $36 \pm 18$ $30 \pm 23$ $91 \pm 11$ $72 \pm 26$
$[{\rm O\;III}]\;5007$ $549.6 \pm 9.2$ $310 \pm 50$ $216 \pm 13$ $181 \pm 34$ $166 \pm 24$ $142 \pm 56$ $200 \pm 13$ $157 \pm 50$
$[{\rm N\;II}]\;6548$ $22.1 \pm 6.5$ $6.7 \pm 2.8$ $11.4 \pm 8.2$ $7.0 \pm 5.9$ ... ... ... ...
${\rm H}\alpha\;6563$ $886.6 \pm 8.1$ $286 \pm 45$ $447 \pm 10$ $286 \pm 47$ $264 \pm 18$ $237 \pm 78$ $300 \pm 17$ $248 \pm 78$
$[{\rm N\;II}]\;6583$ $74.8 \pm 6.6$ $22.4 \pm 4.8$ $64.2 \pm 8.4$ $39 \pm 10$ ... ... ... ...
$[{\rm S\;II}]\;6716$ $101.7 \pm 5.5$ $29.4 \pm 5.4$ $73.6 \pm 7.6$ $44 \pm 10$ ... ... ... ...
$[{\rm S\;II}]\;6731$ $70.2 \pm 5.3$ $20.2 \pm 4.1$ $32.5 \pm 6.8$ $19.4 \pm 6.4$ ... ... ... ...
  NGC 3109 H II#6 ap3 NGC 3109 H II#6 ap4 NGC 3109 H II#6 ap5    
Identification (Å) F I F I F I    
$[{\rm O\;II}]\;3727$ $110.5 \pm 8.6$ $106 \pm 20$ $108.9 \pm 3.7$ $109 \pm 16$ $115.6 \pm 3.8$ $121 \pm 18$    
$[{\rm Ne\;III}]\;3967 + {\rm H}\epsilon$ ... ... $15.2 \pm 3.8$ $18.1 \pm 7.0$ $15.8 \pm 4.1$ $19.3 \pm 7.6$    
${\rm H}\delta\;4101$ ... ... $13.1 \pm 2.9$ $16.8 \pm 6.2$ $15.8 \pm 2.8$ $19.7 \pm 5.9$    
${\rm H}\gamma\;4340$ ... ... $45.8 \pm 4.0$ $49.5 \pm 9.7$ $47.3 \pm 2.9$ $51.3 \pm 8.8$    
${\rm H}\beta\;4861$ $100.0 \pm 5.2$ $100.0 \pm 8.9$ $100.0 \pm 2.9$ $100.0 \pm 7.5$ $100.0 \pm 2.6$ $100.0 \pm 7.3$    
$[{\rm O\;III}]\;4959$ $59.4 \pm 5.2$ $54 \pm 11$ $94.2 \pm 3.1$ $86 \pm 13$ $82.4 \pm 2.8$ $77 \pm 11$    
$[{\rm O\;III}]\;5007$ $195.4 \pm 6.4$ $178 \pm 29$ $289.5 \pm 3.8$ $265 \pm 38$ $251.5 \pm 3.4$ $234 \pm 33$    
He I 5876 $16.4 \pm 5.0$ $14.7 \pm 5.9$ $14.2 \pm 2.9$ $12.5 \pm 3.6$ $13.7 \pm 2.7$ $12.2 \pm 3.5$    
$[{\rm N\;II}]\;6548$ ... ... $3.4 \pm 3.1$ $2.9 \pm 2.9$ $7.2 \pm 2.7$ $6.3 \pm 2.8$    
${\rm H}\alpha\;6563$ $318.3 \pm 5.6$ $286 \pm 45$ $320.9 \pm 3.8$ $286 \pm 41$ $323.5 \pm 3.3$ $286 \pm 40$    
$[{\rm N\;II}]\;6583$ $15.1 \pm 4.5$ $13.4 \pm 5.3$ $14.7 \pm 3.1$ $12.7 \pm 3.8$ $16.7 \pm 2.7$ $14.5 \pm 3.6$    
$[{\rm S\;II}]\;6716$ $23.4 \pm 2.8$ $20.6 \pm 4.7$ $22.9 \pm 1.7$ $19.8 \pm 3.4$ $22.5 \pm 1.5$ $19.5 \pm 3.3$    
$[{\rm S\;II}]\;6731$ $14.9 \pm 2.6$ $13.2 \pm 3.7$ $13.8 \pm 1.5$ $11.9 \pm 2.4$ $14.1 \pm 1.4$ $12.1 \pm 2.4$    
  NGC 3109 H II#6 ap6 NGC 3109 H II#6 ap7 Sag DIG H II#3    
Identification (Å) F I F I F I    
$[{\rm O\;II}]\;3727$ $118.8 \pm 4.0$ $129 \pm 19$ $204 \pm 27$ $270 \pm 100$ $71.5 \pm 6.9$ $95 \pm 17$    
$[{\rm Ne\;III}]\;3967 + {\rm H}\epsilon$ $14.3 \pm 3.8$ $18.0 \pm 6.3$ ... ... ... ...    
${\rm H}\delta\;4101$ $18.9 \pm 3.2$ $22.7 \pm 6.4$ ... ... $17.5 \pm 3.3$ $24.6 \pm 7.3$    
${\rm H}\gamma\;4340$ $46.4 \pm 3.9$ $50.4 \pm 9.6$ ... ... $48.2 \pm 4.4$ $57 \pm 10$    
${\rm H}\beta\;4861$ $100.0 \pm 3.2$ $100.0 \pm 7.6$ $100 \pm 18$ $100 \pm 22$ $100.0 \pm 3.8$ $100.0 \pm 6.5$    
$[{\rm O\;III}]\;4959$ $67.4 \pm 3.0$ $65 \pm 10$ $31 \pm 16$ $28 \pm 21$ $54.1 \pm 4.0$ $51.5 \pm 8.0$    
$[{\rm O\;III}]\;5007$ $203.2 \pm 3.6$ $195 \pm 28$ $111 \pm 19$ $98 \pm 40$ $165.8 \pm 5.0$ $157 \pm 19$    
He I 5876 $12.7 \pm 2.3$ $11.7 \pm 3.2$ ... ... ... ...    
$[{\rm N\;II}]\;6548$ $11.3 \pm 2.5$ $10.1 \pm 3.1$ ... ... $4.4 \pm 3.2$ $3.4 \pm 2.7$    
${\rm H}\alpha\;6563$ $318.3 \pm 3.2$ $286 \pm 41$ $407 \pm 17$ $286 \pm 86$ $369.1 \pm 4.1$ $286 \pm 33$    
$[{\rm N\;II}]\;6583$ $18.4 \pm 2.6$ $16.4 \pm 3.8$ $46 \pm 14$ $32 \pm 17$ $3.5 \pm 3.3$ $2.7 \pm 2.7$    
$[{\rm S\;II}]\;6716$ $23.5 \pm 1.6$ $20.9 \pm 3.6$ ... ... $18.5 \pm 5.6$ $14.1 \pm 5.3$    
$[{\rm S\;II}]\;6731$ $14.9 \pm 1.5$ $13.3 \pm 2.6$ ... ... $9.7 \pm 4.4$ $7.4 \pm 3.9$    


Derived properties are listed in Table 8. The listed properties include H$\beta $ intensities corrected for underlying Balmer absorption and reddening, derived and adopted values of the reddening, observed H$\beta $ emission equivalent widths, and derived O+ and O+2 electron temperatures (see next section). Despite the small number, the three [O III] $\lambda 4363$ detections are found in galaxies where $W_e(\hbox{H$\beta$ }) \ga 40$ Å and $I(\hbox{H$\beta$ }) \ga 7 \times 10^{-15}$ erg s-1 cm-2.

 

 
Table 8: Derived properties. Column (1): H II region. Column (2): H$\beta $ intensity, corrected for underlying Balmer absorption and adopted reddening. Columns (3) and (4): Computed and adopted reddening values. Column (5): Observed H$\beta $ emission equivalent width. Column (6): Electron density. Column (7): O+2 electron temperature arising from [O III] $\lambda 4363$ detection or upper limit. Column (8): O+ electron temperature. NOTE: a Background galaxy with $v_{\odot }/c \simeq +0.11$. Observed (uncorrected) H$\beta $ flux and H$\beta $ emission equivalent width are listed.
    Derived Adopted        
  I(H$\beta)$ E(B-V) E(B-V) $W_{\rm em}$(H$\beta $) ne Te(O+2) Te(O+)
H II Region (ergs s-1 cm-2) (mag) (mag) (Å) (cm-3) (K) (K)
(1) (2) (3) (4) (5) (6) (7) (8)
Centaurus A group dwarfs
A1243-335 H II#A $(4.44 \pm 0.54) \times 10^{-16}$ $+0.14 \pm 0.16$ +0.14 $18.3 \pm 2.1$ 100 ... ...
A1324-412 ap1 $(1.88 \pm 0.34) \times 10^{-15}$ $+0.14 \pm 0.14$ +0.14 $14.7 \pm 2.4$ 100 ... ...
A1334-277 ap1 $(1.15 \pm 0.19) \times 10^{-16}$ $-0.07 \pm 0.25$ 0 $17.2 \pm 2.5$ 100 ... ...
A1346-358 H II#A $(7.73 \pm 0.34) \times 10^{-15}$ $+0.427 \pm 0.087$ +0.427 $103.7 \pm 4.3$ 100 10935 11504
DDO 161 ap1 $(3.71 \pm 0.18) \times 10^{-15}$ $+0.399 \pm 0.091$ +0.399 $43.6 \pm 1.4$ 31 <15460 <13970
NGC 5264 ap1 $(5.66 \pm 0.52) \times 10^{-16}$ $+0.15 \pm 0.14$ +0.15 $11.09 \pm 0.84$ 100 ... ...
Sculptor group dwarfs
AM0106-382 ap1 $(3.30 \pm 0.40) \times 10^{-16}$ ... 0 $24.3 \pm 2.7$ 100 ... ...
AM0106-382 ap2 $(9.28 \pm 0.82) \times 10^{-16}$ ... 0 $18.4 \pm 1.3$ 100 ... ...
AM0106-382 ap3 $(5.86 \pm 0.52) \times 10^{-16}$ ... 0 $15.4 \pm 1.0$ 100 ... ...
ESO347-G017 ap1 $(2.46 \pm 0.14) \times 10^{-15}$ $+0.02 \pm 0.11$ +0.02 $17.91 \pm 0.45$ 100 <13680 <13090
ESO347-G017 ap2 $(2.33 \pm 0.15) \times 10^{-15}$ $+0.14 \pm 0.12$ +0.14 $14.86 \pm 0.54$ 100 ... ...
ESO347-G017 ap3 $(8.1 \pm 1.0) \times 10^{-16}$ $+0.25 \pm 0.19$ +0.25 $12.5 \pm 1.3$ 100 ... ...
ESO348-G009 ap1 $(9.8 \pm 1.4) \times 10^{-16}$ ... 0 $16.6 \pm 2.2$ 100 ... ...
ESO348-G009 ap2 a $(2.32 \pm 0.76) \times 10^{-15}$ ... ... $5.2 \pm 1.7$ ... ... ...
UGCA 442 H II#2 $(2.23 \pm 0.13) \times 10^{-15}$ $+0.13 \pm 0.11$ +0.13 $17.08 \pm 0.47$ 100 <17480 <14830
Other southern dwarfs
A0355-465 H II#B $(2.70 \pm 0.14) \times 10^{-15}$ $+0.318 \pm 0.095$ +0.318 $50.2 \pm 2.3$ 100 ... ...
ESO358-G060 ap1 $(1.35 \pm 0.11) \times 10^{-15}$ $-0.13 \pm 0.15$ 0 $56.8 \pm 4.3$ 100 <18160 <15090
IC 1613 H II#13 $(4.25 \pm 0.18) \times 10^{-15}$ ... 0 $89.1 \pm 4.6$ 100 <14540 <16760
IC 1613 H II#37 $(1.275 \pm 0.068) \times 10^{-14}$ $+0.10 \pm 0.11$ +0.10 $514 \pm 97$ 100 17910 14990
IC 2032 ap1 $(1.94 \pm 0.22) \times 10^{-16}$ $+0.01 \pm 0.16$ +0.01 $15.0 \pm 1.5$ 100 ... ...
IC 5152 H II#A $(1.732 \pm 0.091) \times 10^{-14}$ ... 0 $44.90 \pm 0.85$ 37 12360 12360
NGC 2915 ap1 $(1.84 \pm 0.21) \times 10^{-14}$ $+0.72 \pm 0.16$ +0.72 $4.94 \pm 0.26$ 100 ... ...
NGC 2915 ap2 $(7.62 \pm 0.88) \times 10^{-16}$ $+0.36 \pm 0.17$ +0.36 $13.8 \pm 1.4$ 100 ... ...
NGC 3109 H II#6 ap1 $(2.67 \pm 0.59) \times 10^{-16}$ $-0.19 \pm 0.33$ 0 $11.9 \pm 2.3$ 100 ... ...
NGC 3109 H II#6 ap2 $(2.99 \pm 0.65) \times 10^{-16}$ $-0.15 \pm 0.31$ 0 $7.3 \pm 1.2$ 100 ... ...
NGC 3109 H II#6 ap3 $(9.91 \pm 0.83) \times 10^{-16}$ $+0.03 \pm 0.16$ +0.03 $21.0 \pm 1.2$ 100 ... ...
NGC 3109 H II#6 ap4 $(2.46 \pm 0.18) \times 10^{-15}$ $+0.06 \pm 0.14$ +0.06 $23.25 \pm 0.80$ 100 ... ...
NGC 3109 H II#6 ap5 $(4.58 \pm 0.33) \times 10^{-15}$ $+0.08 \pm 0.14$ +0.08 $31.3 \pm 1.1$ 100 ... ...
NGC 3109 H II#6 ap6 $(1.92 \pm 0.14) \times 10^{-15}$ $+0.08 \pm 0.14$ +0.08 $67.5 \pm 4.5$ 100 ... ...
NGC 3109 H II#6 ap7 $(6.2 \pm 1.3) \times 10^{-16}$ $+0.28 \pm 0.30$ +0.28 $20.7 \pm 4.3$ 100 ... ...
Sag DIG H II#3 $(8.82 \pm 0.57) \times 10^{-16}$ $+0.23 \pm 0.12$ +0.23 $67.0 \pm 4.8$ 100 ... ...


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