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Table 3

Scattered and in situ line emission derived from the TPN and DC 303 spectra.

Line ΔIl(rim) ΔIl(core) (rim) (core) EW
(rim) (core) (sky)
cgs Åa cgs Å cgs Å
(1) (2) (3) (4) (5) (6) (7) (8) (9) (10)

TPN
Hα+[N ii] 234 ± 27 −228 ± 32 42 20.0 20.2 ± 0.85 967 ± 54 1060(50) 424(20) 170(8)
 [S   ii 0 ± 27 −241 ± 32 42.5 22.5 6.29 ± 0.83 502 ± 55 275(50) 121(22) 44(8)
Hβ 0 ± 42 −148 ± 32 32 7.0 3.74 ± 1.10 274 ± 55 130(42) 53(17) 28(9)
Hαb 786 ± 158

DC 303
Hα+[N ii] 559 ± 29 −309 ± 28 42.5 4.5 20.2 ± 0.85 548 ± 42 1081(51) 233(11) 174(8)
 [S   ii 96 ± 29 −126 ± 28 43 5.0 6.29 ± 0.83 252 ± 41 286(52) 63(11.5) 44(8)
Hβ 0 ± 28 −95 ± 28 25 −5.0 3.74 ± 1.10 155 ± 41 108(35) 31(10) 28(9)
Hαb 445 ± 118

Brandt & Draine (2012)
Hα+[N ii] 21.5 ± 0.9
 [S   ii 10.0 ± 0.9
Hβ 4.8 ± 0.7

Witt et al. (2010)
Hα+[N ii] 14.4
 [S   ii 4.5

Notes. In Cols. 8–10 the numbers in parentheses are the corresponding scattered continuum intensities in cgs units.The [N ii] line strengths include λ6583 and λ6548 lines and [S ii] includes λ6716 and λ6731 lines. In the lower part of the table the line equivalent widths are given as observed by Brandt & Draine (2012) for diffuse dust and by Witt et al. (2010) for the dark nebula L 1780.

(a)

cgs = 10-9  erg  cm-2  s-1  sr-1  Å-1 ;

(b)

assuming Hα/Hβ = 2.87.

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