Table 3: Relative line fluxes.
  Area BI Area BII Area E
Line (Å) Fa Ib S/Nc F I S/N F I S/N
H$\beta$ 4861 9 35 (27) 11 35 (11) 13 35 (25)
4959 6 20 (20) 11 31 (12) 7 18 (17)
5007 7 29 (33) 14 39 (18) 18 43 (39)
[O I] 6300 4 5 (35) 6 7 (14) 6 7 (33)
6548 26 26 (160) 20 20 (44) 16 15 (74)
H$\alpha $ 6563 100 100 (441) 100 100 (162) 100 100 (276)
6583 81 79 (373) 63 62 (109) 47 47 (163)
6716 30 27 (161) 28 26 (52) 19 18 (81)
6731 24 21 (129) 22 20 (41) 14 13 (62)
Absolute H$\alpha $ flux$^{\rm d}$ 3 2 7
/H$\alpha $ 0.50 $\pm$ 0.03 0.48 $\pm$ 0.07 0.33 $\pm$0.02
F(6716)/F(6731) 1.29 $\pm$ 0.10 1.32 $\pm$ 0.25 1.38 $\pm$0.12
[N II]/H$\alpha $ 1.07 $\pm$ 0.02 0.83 $\pm$ 0.04 0.63 $\pm$0.01
/H$\beta$ 1.40 $\pm$ 0.09 2.00 $\pm$ 0.30 1.73 $\pm$0.12
c(H$\beta$) 1.68 $\pm$ 0.05 1.38 $\pm$ 0.11 1.17 $\pm$0.05
EB-V 1.16 $\pm$ 0.03 0.95$\pm$ 0.08 0.81 $\pm$ 0.03
a Observed fluxes normalized to F(H$\alpha $) = 100 and uncorrected for interstellar extinction.

b Intrinsic fluxes normalized to F(H$\alpha $) = 100 and corrected for interstellar extinction.

c Numbers in parentheses represent the signal-to-noise ratio of the quoted fluxes.
d In units of 10-16 erg s-1 cm-2 arcsec-2.

Listed fluxes are a signal-to-noise weighted average of two fluxes for areas BI and BII.
The emission line ratios [S  II]/H$\alpha $, F(6716)/F(6731) and [O  III]/H$\beta$ are calculated using the values corrected for interstellar extinction.
The errors of the emission line ratios, c(H$\beta$) and EB-V, are calculated through standard error propagation.


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