Table 3
Physical and dust parameters for different PDR environments.
| PDR | G0 | Teff (K) | Ma–C/MH | amin,a–C (nm) | α | (n0, z0) (105 H cm−3, 10−3 pc) | lPDR (pc) |
|---|---|---|---|---|---|---|---|
| Horsehead | |||||||
| This work | 100 | 35 000 | ≥ 0.3 × 10−2 | 0.4 ± 0.05 | −3.5 | (4 ± 1, 7 ± 1) | ≤ 1.5 × 10−2 |
| Schirmer+2020a | 100 | 35 000 | (0.02 ± 0.01) × 10−2 | 0.77 ± 0.03 | −6 ± 0.5 | (2, 60) | 0.25 |
| Orion Barb | 26 000 | 38 000 | 0.01 × 10−2 | ≤ 0.5 | −5 | (0.9, 3) | 0.12 |
| Diffuse ISMc | 1 | − | 0.17 × 10−2 | 0.4 | −5 | − | − |
Notes. Physical parameters: G0 = radiation field strength (Habing units), Teff = effective temperature of illuminating star. Dust parameters: Ma–C/MH, = nano-grain abundance relative to gas, amin,a–C= minimum grain size, α = size distribution slope. Density parameters: n0 = initial density, z0 = density scale height. lPDR= PDR length along line of sight. (a)Schirmer et al. (2020) focused on the bright filament, while this work probes the illuminated edge at spatial scales inaccessible to Spitzer (see Sect. 6.3). (b)Atomic PDR; Elyajouri et al. (2024). (c)Diffuse interstellar medium; Jones et al. (2013).
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