Extinction AV, R towards emission nebulae derived from common upper level Paschen-Balmer hydrogen lines

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Table 5:

Line strengths, sky line blends, emission line blends (H $\beta$ = 100).
n	Pn	I(Pn)/H $\beta$	Blend (sky)^a	Hn	I(Hn)/H $\beta$	Blend^b
			OH (v'-v'')
6	10 938	9		4101	26
7	10 049	5.5		3970	16
8	9545	3.5		3889	10	He I 3889 (15.0)*
9	9229	2.5		3835	7	He I 3834 (0.06)
10	9015	1.8		3798	5	[SIII] 3799 (5.4)*
11	8863	1.4	8867(7-3)	3770	4	He I 3769 (0.02)
12	8750	1.1		3750	3	O II 3749 (0.12)
13	8665	0.8		3734	2.5	He I 3733 (0.05)
14	8598	0.7	8597(6-2)	3721	2	[OII] 3726,3729 (56)*
						[SIII] 3721
15	8545	0.5	8549(6-2)	3712	1.5	O II 3713 (0.03), Ne II 3713 (0.05)
16	8502	0.45	8505(6-2)	3703	1.3	He I 3705 (0.7)*
17	8467	0.4	8465(6-2)	3697	1.1
18	8438	0.3		3691	1.0
19	8413	0.3	8415(6-2)	3686	0.8
20	8392	0.25		3683	0.7

Notes. ^(a) From Osterbrock $\&$ Martel (1992). ^(b) Nebular emission line, strong line: *; in brackets: line strength in the Orion nebula (Esteban et al. 2004).

Source LaTeX | All tables | In the text

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