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.
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