The distribution of equivalent widths in long GRB afterglow spectra

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Volume 548 (December 2012)

A&A, 548 (2012) A11

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Table 3

Fits to the distribution of lines, including the number of detections and detection limits for each species.

Feature	Det.	Lim.	10⟨log EW⟩ (Å)	σ _{log (EW/Å)}

Si ii/S iiλλ1260, 1260	15	20	1.08	0.34
O i/Si iiλλ1302, 1304^a	22	15	1.95	0.29
C iiλ1335^a	23	16	1.64	0.30
Si ivλ1394	19	19	0.88	0.37
Si ivλ1403	19	19	0.74	0.39
Si iiλ1527	27	16	1.05	0.43
C ivλλ1548, 1551	35	7	2.37	0.30
Fe iiλ1608	19	24	0.71	0.61
Al iiλ1671	26	13	1.27	0.41
Al iiiλ1855	15	27	0.70	0.60
Al iiiλ1863	14	29	0.58	0.53
Zn ii/Cr iiλλ2026, 2026	16	27	0.75	0.37
Zn ii/Cr iiλλ2063, 2062	11	26	0.50	0.49
Fe iiλ2344^a	23	14	1.59	0.33
Fe iiλ2374	17	20	1.08	0.45
Fe iiλ2383^a	23	15	2.00	0.25
Fe iiλ2587	20	16	1.45	0.39
Fe iiλ2600^a	18	16	1.78	0.42
Mg iiλλ2796, 2803	27	4	3.76	0.30
Mg iλ2852	12	18	0.84	0.49
Ca iiλ3935	7	8	1.29	0.31
Ca iiλ3970	7	8	0.93	0.34

Notes. We show 10⟨log EW⟩ instead of ⟨log EW⟩ as it allows a more intuitive interpretation.

^(a)

In some cases this line is blended with a fine structure transition of the same species. This can be significant in early spectra, as the fine structure line is normally excited by the prompt GRB emission.

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