An extreme [O III] emitter at z = 3.2: a low metallicity Lyman continuum source

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Volume 585 (January 2016)

A&A, 585 (2016) A51

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Table 1

Emission line properties.

Line	Flux^a	Dust corrected flux^b	FWHM ^c	EW ^d	z

Lyα	15.4 ± 1.0 ^e		240 ± 60 ^f	94 ± 20 ^e	3.2183^f± 0.003
Lyα (blue)	5.1	...	...	...	3.2126 ± 0.005
Lyα (red)	10.3	...	...	...	3.2183 ± 0.003
N vλ1240	<0.16	<0.4	...	...	...
C ivλ1550	<0.18	<0.4	...	...	...
He iiλ1640^g	0.6 ± 0.3		...	...	...
O iii]λ1666^g	0.5 ± 0.3		...	...	...
C iii]λ1909	1.3 ± 0.3		400 ± 90 ^h		3.2127
[O ii]λ3727ⁱ	1.5 ± 1.5		...	<50	3.2126
Hβ^g	1.5 ± 0.8		...	112 ± 60	3.2128 ± 0.005
[O iii]λ4959	5.4 ± 0.8 (7.4 ± 1.1)		155 ± 70	365 ± 70	3.2128 ± 0.0008
[O iii]λ5007	22.1 ± 0.8		147 ± 30	1103 ± 60	3.2126 ± 0.0006

Notes.

^(a)

Observed emission line flux and error corrected for slit losses (50%) in units of 10^-17 erg s^-1 cm^-2. In parenthesis, the [O iii]λ4959 flux adopting the theoretical ratio [ O iii ] λ5007 / [ O iii ] λ4959 = 3 (Storey & Zeippen 2000).

^(b)

The emission line dust correction method is described in Appendix A.

^(c)

FWHM (instrumental corrected) and error in units of km s^-1.

^(d)

Equivalent width and error in units of Å.

^(e)

Sum of the two components.

^(f)

Main component.

^(g)

Marginal detections (Fig. 6): S/N(O iii ] λ1666) ~ 1.7, S/N(He iiλ1640) ~ 2, and S/N(Hβ) ~ 2.

^(h)

FWHM is the contribution of the two blended components, 1907–1909 Å.

⁽ⁱ⁾

The error is large because the line is on the top of a sky line (Fig. 4).

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