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Home All issues Volume 503 / No 1 (August III 2009) A&A, 503 1 (2009) 129-136 Full HTML
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Table 2:

Relative line fluxes.
  Area 1a Area 1b Area 1c Area 1d Area 2a
Line (Å) Fa Ib S/Nc F I S/N F I S/N F I S/N F I S/N
H$\beta$ 4861 15 36 (6) 26 33 (43) 24 34 (26) 20 34 (11) 24 34 (28)
4959 99 226 (39) 35 44 (61) 32 45 (40) - - - 31 43 (39)
5007 317 702 (114) 107 134 (177) 103 142 (115) - - - 92 126 (111)
[O I] 6300 11 11 (7) 5 5 (17) - - - - - - 7 7 (10)
[O I] 6364 - - - - - - - - - - - - 2 2 (3)
6548 40 40 (27) 25 25 (68) 25 25 (50) 15 15 (21) 27 27 (54)
H$\alpha $ 6563 100 100 (47) 100 100 (158) 100 100 (133) 100 100 (105) 100 100 (147)
6583 141 140 (72) 79 79 (148) 84 84 (35) 47 47 (53) 89 89 (144)
6716 91 86 (55) 50 49 (119) 51 50 (87) 29 28 (41) 68 66 (125)
6731 68 64 (40) 36 35 (76) 37 36 (67) 21 20 (23) 49 48 (94)
Absolute H$\alpha $ fluxd 2 2.1 3.9 1.3 2.5
/H$\alpha $ 1.50 $\pm$ 0.04 0.84 $\pm$ 0.01 0.86 $\pm$ 0.01 0.48 $\pm$ 0.01 1.14$\pm$ 0.01
F(6716)/F(6731) 1.34 $\pm$ 0.04 1.39 $\pm$ 0.03 1.38 $\pm$ 0.03 1.38 $\pm$ 0.07 1.39$\pm$ 0.02
[N II]/H$\alpha $ 1.80 $\pm$ 0.05 1.04 $\pm$ 0.02 1.09 $\pm$ 0.01 0.62 $\pm$ 0.01 1.16$\pm$ 0.01
/H$\beta$ 25.8 $\pm$ 4.3 5.40 $\pm$ 0.13 5.50 $\pm$0.21 - 5.00 $\pm$ 0.18
c(H$\beta$) 1.10 $\pm$ 0.20 0.31 $\pm$ 0.03 0.44 $\pm$0.05 0.67 $\pm$ 0.12 0.44 $\pm$ 0.05
EB-V 0.73 $\pm$ 0.13 0.21 $\pm$ 0.02 0.29 $\pm$ 0.03 0.44 $\pm$ 0.08 0.29$\pm$ 0.03

Area 2b Area 2c Area 2d Area 2e Area 2f
Line (Å) Fa Ib S/Nc F I S/N F I S/N F I S/N F I S/N
H$\beta$ 4861 24 34 (35) 23 34 (25) 25 34 (21) 24 34 (38) 29 33 (17)
4959 18 25 (30) 25 36 (30) 32 43 (29) 39 54 (69) 5 6 (2)
5007 56 77 (88) 72 101 (83) 97 128 (87) 119 164 (190) 12 14 (9)
[O I] 6300 9 9 (17) 7 7 (9) 10 10 (10) 6 6 (12) 10 10 (5)
[O I] 6364 2 2 (5) 3 3 (5) 3 3 (5) - - - - - -
6548 24 24 (60) 21 21 (41) 23 23 (36) 26 26 (72) 17 17 (19)
H$\alpha $ 6563 100 100 (174) 100 100 (140) 100 100 (109) 100 100 (197) 100 100 (77)
6583 78 78 (159) 69 68 (111) 71 71 (89) 84 84 (189) 48 48 (44)
6716 63 62 (159) 51 50 (92) 44 43 (64) 50 49 (130) 30 30 (44)
6731 45 44 (102) 36 35 (69) 32 31 (49) 36 35 (99) 22 22 (25)
Absolute H$\alpha $ fluxd 4.2 2.1 2.2 3.7 1.5
/H$\alpha $ 1.06 $\pm$ 0.01 0.85 $\pm$ 0.01 0.74 $\pm$0.01 0.84 $\pm$ 0.01 0.52 $\pm$ 0.01
F(6716)/F(6731) 1.40 $\pm$ 0.02 1.42 $\pm$ 0.03 1.38 $\pm$0.04 1.39 $\pm$ 0.02 1.36 $\pm$ 0.07
[N II]/H$\alpha $ 1.02 $\pm$ 0.01 0.89 $\pm$ 0.01 0.94 $\pm$0.01 1.10 $\pm$ 0.01 0.65 $\pm$ 0.01
/H$\beta$ 3.00 $\pm$ 0.09 4.00 $\pm$ 0.18 5.00 $\pm$0.25 6.40 $\pm$ 0.17 0.60 $\pm$ 0.07
c(H$\beta$) 0.44 $\pm$ 0.04 0.47 $\pm$ 0.05 0.38 $\pm$0.07 0.44 $\pm$ 0.04 0.16 $\pm$ 0.08
EB-V 0.29 $\pm$ 0.03 0.31 $\pm$ 0.03 0.25 $\pm$0.05 0.29 $\pm$ 0.03 0.11 $\pm$ 0.06
The emission line ratios [S  II]/H$\alpha $, F(6716)/F(6731), [N II]/H$\alpha $ 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.

  Area 3a Area 3b Area 3c Area 3d Area 4a
Line (Å) Fa Ib S/Nc F I S/N F I S/N F I S/N F I S/N
H$\beta$ 4861 25 34 (83) 28 34 (12) 26 33 (19) 25 34 (23) 27 34 (9)
4959 9 12 (33) 26 31 (12) 32 40 (24) 14 19 (15) 11 14 (3)
5007 25 33 (89) 84 100 (37) 109 136 (80) 46 61 (48) 57 70 (20)
[O I] 6300 7 7 (40) - - - - - - - - - 50 51 (10)
[O I] 6364 3 3 (18) - - - - - - - - - 17 17 (5)
6548 22 22 (127) 27 27 (20) 18 18 (23) 24 24 (40) - - -
H$\alpha $ 6563 100 100 (383) 100 100 (59) 100 100 (98) 100 100 (123) 100 100 (44)
6583 72 72 (317) 82 82 (53) 65 65 (72) 76 76 (107) 43 43 (17)
6716 65 64 (301) 55 54 (39) 45 44 (55) 44 43 (67) 95 94 (42)
6731 46 45 (218) 36 35 (27) 31 30 (38) 32 31 (52) 64 63 (31)
Absolute H$\alpha $ fluxd 6.9 1.6 1.8 3.7 0.5
/H$\alpha $ 1.09 $\pm$ 0.01 0.89 $\pm$ 0.02 0.74 $\pm$0.01 0.74 $\pm$ 0.01 1.57 $\pm$ 0.05
F(6716)/F(6731) 1.41 $\pm$ 0.01 1.53 $\pm$ 0.07 1.45 $\pm$0.05 1.37 $\pm$ 0.03 1.48 $\pm$ 0.06
[N II]/H$\alpha $ 0.94 $\pm$ 0.01 1.09 $\pm$ 0.02 0.83 $\pm$0.01 1.00 $\pm$ 0.01 0.43 $\pm$ 0.01
/H$\beta$ 1.32 $\pm$ 0.02 3.80 $\pm$ 0.32 5.30 $\pm$ 0.28 2.40 $\pm$ 0.11 2.50 $\pm$0.31
c(H$\beta$) 0.38 $\pm$ 0.02 0.24 $\pm$ 0.11 0.31 $\pm$0.07 0.38 $\pm$ 0.06 0.28 $\pm$ 0.15
EB-V 0.25 $\pm$ 0.01 0.16 $\pm$ 0.07 0.21 $\pm$0.05 0.25 $\pm$ 0.04 0.19 $\pm$ 0.10
  Area 4b Area 4c Area 4d Area 4e Area 4f
Line (Å) Fa Ib S/Nc F I S/N F I S/N F I S/N F I S/N
H$\beta$ 4861 26 33 (30) 23 34 (22) 22 34 (37) 28 34 (30) 35 36 (29)
4959 7 9 (10) 6 9 (7) 11 16 (20) 11 13 (15) 14 15 (14)
5007 35 44 (46) 37 52 (39) 50 73 (92) 41 49 (50) 52 54 (48)
[O I] 6300 - - - 6 6 (7) 11 12 (24) 10 10 (12) 13 13 (9)
[O I] 6364 - - - - - - 3 3 (8) 4 4 (6) 3 3 (2)
6548 28 28 (59) 20 20 (34) 29 29 (86) 24 24 (46) 18 18 (27)
H$\alpha $ 6563 100 100 (156) 100 100 (118) 100 100 (215) 100 100 (144) 100 100 (109)
6583 88 88 (148) 66 66 (90) 101 101 (233) 80 80 (127) 57 57 (73)
6716 66 65 (127) 51 49 (78) 68 66 (182) 55 54 (101) 37 37 (58)
6731 48 47 (100) 34 33 (56) 49 47 (131) 41 40 (81) 26 26 (42)
Absolute H$\alpha $ fluxd 2.6 3.4 2.7 2.6 1.9
/H$\alpha $ 1.12 $\pm$ 0.01 0.82 $\pm$ 0.01 1.13 $\pm$ 0.01 0.94 $\pm$ 0.01 0.63 $\pm$ 0.01
F(6716)/F(6731) 1.38 $\pm$ 0.02 1.48 $\pm$ 0.03 1.40 $\pm$ 0.01 1.35 $\pm$ 0.02 1.42 $\pm$ 0.04
[N II]/H$\alpha $ 1.16 $\pm$ 0.01 0.86 $\pm$ 0.01 1.30 $\pm$ 0.01 1.04 $\pm$ 0.01 0.75 $\pm$ 0.01
/H$\beta$ 1.60 $\pm$ 0.06 1.80 $\pm$ 0.09 2.60 $\pm$ 0.08 1.82 $\pm$ 0.07 1.92 $\pm$ 0.08
c(H$\beta$) 0.31 $\pm$ 0.04 0.47 $\pm$ 0.06 0.53 $\pm$ 0.04 0.24 $\pm$ 0.04 0.16 $\pm$ 0.05
EB-V 0.21 $\pm$ 0.03 0.31 $\pm$ 0.04 0.35 $\pm$ 0.03 0.16 $\pm$ 0.03 0.11 $\pm$ 0.03
a Observed surface brightness normalized to F(H$\alpha $) = 100 and uncorrected for interstellar extinction.
b Intrinsic surface brightness normalized to F(H$\alpha $) = 100 and corrected for interstellar extinction.
c Numbers in parentheses represent the signal-to-noise ratio of the quoted fluxes.
d In units of 10-16 erg s-1 cm-2 arcsec-2.
The letters next to the areas number indicate different apertures extracted along the slit.
Listed fluxes are a signal-to-noise weighted average of two fluxes for areas 2, 3 and 4.
The emission line ratios [N II]/H$\alpha $ and [O  III]/H$\beta$ are calculated using the values corrected for interstellar extinction.

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