Table 9
Summary of published properties of Galactic PDRs sorted by the spectral type of the primary exciting star.
| Spectral | Inter-clump phase | Dense phase | |||||||
| Object | type | G 0 | n | G 0 a | n | ϵ | I158/I63b | I145/I63b | References |
| [Habing units] | [cm-3] | [Habing units] | [cm-3] | ×10-3 | |||||
|
|
|||||||||
| H ii Region PDRs: | |||||||||
| 30 Dor | O3c | 7.8 × 103 | 6.8 × 103 | – | – | – | – | – | 1, 2 |
| M17 | O4c | 5.6 × 105 | 3.0 × 104 | – | 5.0 × 105 | 2.3 | 0.17 | 0.13 | 3 |
| M17 | O4c | – | 1.0 × 103 | – | – | – | – | – | 4 |
| M17 | O4c | – | – | 1–8 × 104 | 2.0 × 107 | – | – | – | 5 |
| W49A | O5c | 3.2 × 105 | 1.0 × 104 | – | – | 0.14-0.36 | 0.34 | 0.15 | 6 |
| Orion Bar | O6 | 4.4 × 104 | 2.0 × 105 | – | ~107 | – | 0.11 | 0.07 | 7, 8, 9, 10 |
| Cepheus B | OB assoc | – | – | 1.7 × 103 | 1.0 × 106 | – | – | – | 11 |
| S 106d | O7-9 | 1.6 × 104 | 0.6 – 3 × 104 | 1.6 × 105 | 3.1 × 105 | 1.0 | 0.13 | 0.15 | This paper |
| S 106 | O8 | – | – | > 105 | 105 – 106 | – | – | – | 12 |
| S 106 | O7-9 | > 103 | ~3 × 104 | 1–2 × 105 | 1–3 × 105 | – | 0.11 | 0.17 | 13 |
| Sgr B2 | O7 | 5 × 103 | 5 × 103 | – | – | – | – | – | 14 |
| IRAS 23133+6050d | O8.5-9.5 | 1.0 × 104 | 0.3–1.2 × 104 | 1.6 × 105 | 3.1 × 105 | 1.1 | 0.21 | 0.15 | This paper |
| NGC 2024−IRS 2b | O8-B2 | ~5 × 104 | ~5 × 105 | – | – | – | – | – | 15, 16 |
| S 140 | B0 | 255 | 2.0 × 103 | – | 2.0 × 104 | – | – | – | 17 |
| W3 IRS 5 | B0.5 | 1.0 × 106 | 1.5 × 104 | – | 1.8 × 105 | – | – | – | 18, 19 |
| S 125 | B0.5 | 9.0 × 102 | 1.8 × 102 | – | – | – | – | – | 20 |
| Reflection Nebula PDRs: | |||||||||
| NGC 2023 | B1.5 | 1.5 × 104 | 2.0 × 104 | – | – | 2.6 | 0.19 | 0.06 | 21 |
| NGC 2023 | B1.5 | – | – | 1.7 × 104 | 2.0 × 105 | – | – | – | 22 |
| NGC 2316 | B2-3 | 8.1 × 104 | 1.0 × 104 | – | – | 1.8 | 0.42 | 0.13 | 23 |
| NGC 7023 | B3 | 2.6 × 103 | 4.0 × 103 | – | – | 2.9 | 0.85 | – | 24 |
| NGC 7023 | B3 | 2.0 × 103 | 7.0 × 103 | – | – | – | – | – | 25 |
| NGC 2245 | B7-8 | 3.5 × 102 | 5.0 × 103 | – | – | 7.6 | 0.75 | 0.14 | 23 |
Notes.
For these sources the PDR is illuminated by a cluster of stars, in the spectral type column we have indicated the hottest star detected in the literature (e.g., Hoffmeister et al. 2008 for M17 and De Pree et al. 1997 for W49A).
For S 106 and IRAS 23133+6050 we quote the Interclump G0 and n values indicated using the combinations of [O i] 63, 145 μm, [C ii] 158 μm and the total FIR flux reported in rows 3−4 of Table 5. The dense phase (clump) values arising from the average of the high-J CO lines and the cooling lines/FIR flux (rows 7−8 in Table 5).
Reference. (1) Bosch et al. (1999); (2) Poglitsch et al. (1995); (3) Meixner et al. (1992); (4) Pérez-Beaupuits et al. (2010); (5) Sheffer & Wolfire (2013); (6) Vastel et al. (2001); (7) Tielens & Hollenbach (1985a); (8) Tielens et al. (1993); (9) Herrmann et al. (1997); (10) Goudis (1982); (11) Mookerjea et al. (2012); (12) van den Ancker et al. (2000); (13) Schneider et al. (2003); (14) Goicoechea et al. (2004); (15) Bik et al. (2003); (16) Giannini et al. (2000); (17) Spaans & van Dishoeck (1997); (18) Kramer et al. (2004); (19) Megeath et al. (2005); (20) Aannestad & Emery (2003); (21) Steiman-Cameron et al. (1997); (22) Sheffer et al. (2011); (23) Young Owl et al. (2002); (24) Chokshi et al. (1988); (25) Joblin et al. (2010).
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