Massive star formation in Wolf-Rayet galaxies - II. Optical spectroscopy results

A. R. López-Sánchez; C. Esteban

doi:10.1051/0004-6361/200912042

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Volume 508 / No 2 (December III 2009)

A&A, 508 2 (2009) 615-640

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Table A.15:

Dereddened line intensity ratios with respect to I(H $\beta$ ) = 100 for knots analyzed in III Zw 107 (regions A, B, and C) and Tol 9 (spectra obtained with 2.5 m INT and 2.56 m NOT).
Line	$f(\lambda)$	III Zw 107 A	III Zw 107 B	III Zw 107 C	Tol 9 INT	Tol 9 NOT
3554.42 He I	0.283	...	...	...	3.8 $\pm$ 1.4	...
3728.00 [O II]	0.256	213 $\pm$ 12	306 $\pm$ 23	20.32:	142 $\pm$ 10	177 $\pm$ 27
3770.63 H I	0.249	1.00:	0.54:	...	0.56:	...
3797.90 H I	0.244	2.37:	...	...	0.83:	...
3835.39 H I	0.237	3.60 $\pm$ 0.95	1.69:	5.02:	1.94:	...
3868.75 [Ne III]	0.230	23.3 $\pm$ 2.1	21.1 $\pm$ 4.0	20.64:	10.9 $\pm$ 2.0	12.08:
3889.05 H I	0.226	12.6 $\pm$ 1.7	11.1 $\pm$ 4.2	8.84:	6.9 $\pm$ 2.1	...
3967.46 [NeIII]H7	0.210	17.1 $\pm$ 1.7	22.4 $\pm$ 2.9	...	21.6 $\pm$ 1.9	...
4068.60 [S II]	0.189	2.26 $\pm$ 0.82	4.69:	...	3.3 $\pm$ 1.1	...
4101.74 H I	0.182	26.2 $\pm$ 1.8	26.1 $\pm$ 4.2	27.5 $\pm$ 6.5	25.3 $\pm$ 2.5	26.3 $\pm$ 4.0
4340.47 H I	0.127	46.7 $\pm$ 2.8	46.9 $\pm$ 4.8	47.5 $\pm$ 7.9	45.8 $\pm$ 3.2	46.9 $\pm$ 5.8
4363.21 [O III]	0.121	3.14 $\pm$ 0.67	1.97:	...	0.55:	...
4471.48 He I	0.095	4.08 $\pm$ 0.75	3.40:	...	3.94 $\pm$ 0.65	3.96:
4658.10 [Fe III]	0.050	1.06:	...	...	1.09:	...
4686.00 He II	0.043	...	...	...	0.33:	...
4814.55 [Fe II]	0.012	...	...	...	0.85:	...
4861.33 H I	0.000	100.0 $\pm$ 5.3	100.0 $\pm$ 8.2	100 $\pm$ 15	100.0 $\pm$ 6.0	100 $\pm$ 10
4921.93 He I	-0.015	0.42:	...	...	...	...
4958.91 [O III]	-0.024	123.7 $\pm$ 6.5	99.5 $\pm$ 8.1	93 $\pm$ 14	78.3 $\pm$ 5.2	75.5 $\pm$ 9.1
5006.84 [O III]	-0.036	375 $\pm$ 18	293 $\pm$ 19	257 $\pm$ 32	236 $\pm$ 13	225 $\pm$ 21
5197.90 [N I]	-0.082	1.08:	2.07:	...	...	...
5200.26 [N I]	-0.083	0.36:	...	...	2.63 $\pm$ 0.78	...
5517.71 [Cl III]	-0.154	0.22:	...	...	0.57:	...
5537.88 [Cl III]	-0.158	0.20:	...	...	0.64:	...
5754.64 [N II]	-0.198	...	...	...	0.41:	...
5875.64 He I	-0.215	12.5 $\pm$ 1.1	13.1 $\pm$ 2.3	12.94:	12.6 $\pm$ 1.4	16.3 $\pm$ 3.8
6300.30 [O I]	-0.282	4.56 $\pm$ 0.61	6.1 $\pm$ 2.0	7.57:	7.78 $\pm$ 0.71	7.32 $\pm$ 0.96
6312.10 [S III]	-0.283	1.02 $\pm$ 0.23	...	...	0.66:	0.66:
6363.78 [O I]	-0.291	1.55 $\pm$ 0.42	2.01:	3.58:	2.14 $\pm$ 0.59	2.30 $\pm$ 0.91
6548.03 [N II]	-0.318	9.98 $\pm$ 0.75	12.1 $\pm$ 1.4	13.6 $\pm$ 4.5	23.8 $\pm$ 1.8	24.3 $\pm$ 2.3
6562.82 H I	-0.320	282 $\pm$ 16	273 $\pm$ 18	280 $\pm$ 35	267 $\pm$ 18	284 $\pm$ 30
6583.41 [N II]	-0.323	28.7 $\pm$ 1.8	37.0 $\pm$ 3.2	41.4 $\pm$ 8.3	72.2 $\pm$ 4.9	82.1 $\pm$ 7.3
6678.15 He I	-0.336	3.17 $\pm$ 0.50	4.01:	...	3.16 $\pm$ 0.64	4.1 $\pm$ 1.3
6716.47 [S II]	-0.342	19.6 $\pm$ 1.3	36.4 $\pm$ 4.3	52.2 $\pm$ 8.7	37.0 $\pm$ 2.6	42.1 $\pm$ 3.9
6730.85 [S II]	-0.344	15.9 $\pm$ 1.1	27.5 $\pm$ 3.6	35.6 $\pm$ 6.9	29.8 $\pm$ 2.2	35.7 $\pm$ 3.4
7065.28 He I	-0.387	2.27 $\pm$ 0.40	...	...	1.93 $\pm$ 0.51	2.41 $\pm$ 0.94
7135.78 [Ar III]	-0.396	11.4 $\pm$ 0.9	9.4 $\pm$ 1.7	...	10.5 $\pm$ 1.0	10.8 $\pm$ 1.5
7318.39 [O II]	-0.418	2.12 $\pm$ 0.58	...	...	1.96:	1.57 $\pm$ 0.43
7329.66 [O II]	-0.420	2.48 $\pm$ 0.66	...	...	1.08:	1.30 $\pm$ 0.34
7751.10 [Ar III]	-0.467	...	...	...	...	2.68 $\pm$ 0.68
Aperture size (arcsec)		7.2 $\times$ 1	5.6 $\times$ 1	5.2 $\times$ 1	6.4 $\times$ 1	3.8 $\times$ 1
Distance (arcsec)^a		-	7.2	12.4	-	-
F(H $\beta$ )^b		22.3 $\pm$ 0.8	8.6 $\pm$ 0.4	1.56 $\pm$ 0.14	23.4 $\pm$ 0.9	3.8 $\times$ 0.3
C(H $\beta$ )		0.68 $\pm$ 0.04	0.15 $\pm$ 0.02	0.22 $\pm$ 0.03	0.50 $\pm$ 0.05	0.40 $\pm$ 0.05
$W_{\rm abs}$ (Å)		2.0 $\pm$ 0.3	1.30 $\pm$ 0.10	0.50 $\pm$ 0.10	7.5 $\pm$ 0.8	6.2 $\pm$ 0.6
-W(H $\alpha$ ) (Å)		306 $\pm$ 18	76 $\pm$ 5	30 $\pm$ 4	178 $\pm$ 12	186 $\pm$ 15
-W(H $\beta$ ) (Å)		44 $\pm$ 3	15 $\pm$ 2	4.7 $\pm$ 0.7	33 $\pm$ 2	17 $\pm$ 3
-W(H $\gamma$ ) (Å)		16.4 $\pm$ 1.0	5.5 $\pm$ 0.6	1.8 $\pm$ 0.3	12.3 $\pm$ 0.8
-W([O III]) 5007 (Å)		172 $\pm$ 8	41 $\pm$ 3	11.6 $\pm$ 1.5	77 $\pm$ 4	32 $\pm$ 4

^a Relative distance of the knot with respect to the main region in the galaxy; ^b in units of 10^-15 erg s^-1 cm^-2 and not corrected for extinction.

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