On the massive star content of the nearby dwarf irregular Wolf-Rayet galaxy IC 4662

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Volume 499 / No 2 (May IV 2009)

A&A, 499 2 (2009) 455-464

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Table 1:

Observed line fluxes, $F_{\lambda }$ , and intensities, $I_{\lambda }$ , of nebular and stellar (Wolf-Rayet, WR) lines in each of the four VLT/FORS2 IC 4662 apertures, relative to H $\beta =100$ . H $\beta$ fluxes are shown separate from normalised values in units of 10^-13 erg s^-1 cm^-2.
$\lambda$ (Å)	ID		#1		#2		#3		#4
			$F_{\lambda }$	$I_{\lambda }$	$F_{\lambda }$	$I_{\lambda }$	$F_{\lambda }$	$I_{\lambda }$	$F_{\lambda }$	$I_{\lambda }$
3727	[O II]		66.2	83.8	102.2	113.9	146.7	174.8	142.2	163.6
3867	[Ne III]		40.6	50.1	57.6	62.6	10.1	11.8	183.6	204.7
3968	[Ne III] + H7		24.8	30.1	22.4	24.2	6.2	7.1	115.0	127.1
4058	N IV	WR	1.8	2.1	-	-	1.8	2.1	0.5	0.6
4100	H $\delta$		21.1	25.4	23.9	27.1	22.9	26.4	25.0	28.5
4340	H $\gamma$		41.4	46.4	45.9	49.9	42.3	45.5	42.8	46.4
4363	[O III]		7.1	7.9	6.4	7.4	6.4	7.0	6.8	7.4
4659	[Fe III]		0.41	0.43	0.47	0.49	6.3	6.5	0.57	0.59
4686 $^{\ast}$	He II	WR	8.5	8.9	2.1	2.2	4.17	4.25	14.6	15.3
4712	[Ar IV]		2.0	2.1	1.5	1.5	0.96	0.99	1.2	1.2
4741	[Ar IV]		0.96	0.99	0.70	0.72	0.36	0.37	0.54	0.56
4861	H $\beta$		100	100	100	100	100	100	100	100
4959	[O III]		213.8	206.3	198.4	198.5	184.8	180.4	203.6	202.0
5007	[O III]		630.0	604.0	583.0	590.6	542.9	528.6	604.4	607.8
5411	He II	WR	0.56	0.50	-	-	-	-	1.16	1.15
5808	C IV	WR	-	-	-	-	2.7	2.4	-	-
5876	He I		12.1	9.8	11.7	11.3	13.9	12.0	11.9	11.1
H $\beta$			0.44	1.12	0.39	0.49	0.44	0.86	0.13	0.20
E(B-V)			0.28 $\pm$ 0.05		0.08 $\pm$ 0.05		0.20 $\pm$ 0.05		0.12 $\pm$ 0.05
$T_{\rm e}$ (K)			12 900 $\pm$ 700		12 700 $\pm$ 900		12 900 $\pm$ 700		12 500 $\pm$ 400
O⁺/H ( $\times10^{-5}$ )			1.20 $\pm$ 0.07		1.7 $\pm$ 0.1		2.5 $\pm$ 0.18		2.6 $\pm$ 0.2
O²⁺/H ( $\times10^{-5}$ )			10.3 $\pm$ 0.53		10.6 $\pm$ 0.61		9.0 $\pm$ 0.65		11.2 $\pm$ 0.87
12 + $\log$ (O/H)			8.06 $\pm$ 0.02		8.09 $\pm$ 0.02		8.06 $\pm$ 0.03		8.14 $\pm$ 0.03

$^{\ast}$ He II $\lambda$ 4686 fluxes are the sum of nebular and stellar components.

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