GMASS ultradeep spectroscopy of galaxies at z ~ 2 - VI. Star formation, extinction, and gas outflows from UV spectra

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Volume 539 (March 2012)

A&A, 539 (2012) A61

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Table 1

Spectral lines in a SFG rest-frame UV spectrum.

Ion	Vacuum	Rest-frame	Origin
	wavelength (Å)	EW^a (Å)

C III	1175.71	1.70 ± 0.12	stellar (photospheric)
N V	1238.82, 1242.80	–1.11 ± 0.20	ISM
Si II	1260.42	1.47 ± 0.09	ISM
Si II*	1264.74	–0.36 ± 0.25	Fine-structure emission (ISM)
O I - Si II^b	1302.17, 1304.37	2.43 ± 0.26^d	ISM
Si II*	1309.28	–1.26 ± 0.25	Fine-structure emission (ISM)
C II	1334.53	2.09 ± 0.15	ISM
O IV	1343.35	0.27 ± 0.07	stellar (photospheric)
Si IV^c	1393.76	2.02 ± 0.09	ISM + stellar wind (P-Cygni profile)
Si IV^c	1402.77	1.42 ± 0.05	ISM + stellar wind (P-Cygni profile)
Si III	1417.24	0.72 ± 0.29	stellar (photospheric)
S V	1501.76	0.54 ± 0.13	stellar (photospheric)
Si II	1526.71	1.94 ± 0.08	ISM
C IV^b^c	1548.20, 1550.78	3.24 ± 0.16^d	ISM + stellar wind (P-Cygni profile)
Fe II	1608.45	1.31 ± 0.11	ISM
He II	1640.42	–1.02 ± 0.10	stellar wind
Al II	1670.79	1.54 ± 0.08	ISM
Ni II	1709.60	0.70 ± 0.35	ISM
N IV	1718.55	1.14 ± 0.18	stellar wind (P-Cygni profile)
Ni II	1741.55	0.25 ± 0.41	ISM
Ni II	1751.91	0.39 ± 0.41	ISM
Si II	1808.01	0.76 ± 0.09	ISM
Si I	1845.52	0.53 ± 0.21	ISM
Al III^c	1854.72	1.20 ± 0.21	ISM + stellar wind (P-Cygni profile)
Al III^c	1862.79	0.85 ± 0.11	ISM + stellar wind (P-Cygni profile)
C III]^b,c	1906.68, 1908.68	–1.02 ± 0.15^d	nebular
Fe II	2249.88	0.60 ± 0.22	ISM
Fe II	2260.78	0.50 ± 0.31	ISM
C III	2297.58	0.28 ± 0.24	stellar (photospheric)
C II]	2326.00	–1.24 ± 0.20	nebular
Fe II	2344.21	2.45 ± 0.13	ISM
Fe II*	2365.66	–0.74 ± 0.38	Fine-structure emission (ISM)
Fe II^c	2374.46	1.87 ± 0.13	ISM
Fe II^c	2382.76	2.22 ± 0.15	ISM
Fe II*	2396.15	–1.12 ± 0.18	Fine-structure emission (ISM)
Fe II^c	2586.65	2.65 ± 0.17	ISM^e
Fe II^c	2600.17	2.77 ± 0.14	ISM^e
Fe II*	2612.65	–1.07 ± 1.35	Fine-structure emission (ISM)
Fe II*	2626.45	–1.17 ± 0.41	Fine-structure emission (ISM)
Mg II^c	2796.35	2.43 ± 0.10	ISM^f
Mg II^c	2803.53	2.07 ± 0.10	ISM^f
Mg I	2852.96	1.75 ± 0.68	ISM

Notes.

^(a)

EWs measured in the composite spectrum of 74 SFGs. Their values are negative for emission lines and positive for absorption lines.

^(b)

Blended at our spectral resolution.

^(c)

Doublet.

^(d)

The measurement of the EW refers to the blend of the two lines.

^(e)

Possible stellar wind contribution.

^(f)

Possible photospheric stellar contribution.

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