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Table 4

Parameters in the spinning dust models for Perseus and ρ Ophiuchi.

Gas state Molecular Atomic Ionised

Perseus
NH [1021 cm-2] 11.7 1.3 0.4
nH [cm-3] 250 30 1
z [pc] 15.1 14.0 ...
G0 1 2 ...
T [K] 40 100 8 × 103
xH [ppm] 112 410 106
xC [ppm]  <1 100 ...
y 1 0.1 ...
a0 [nm] 0.58 0.53 ...
bC [ppm] 68 68 ...
β ... 1.65 ...
Td [K] ... 18.5 ...
τ250 ... 9.4 × 10-4 ...

ρ Ophiuchi
NH [1021 cm-2] 18.2 0.4 0.4
nH [cm-3] 2 × 104 200 0.5
z [pc] 0.3 0.6 ...
G0 0.4 400 ...
T [K] 20 103 8 × 103
xH [ppm] 9.2 373 106
xC [ppm]  < 1 100 ...
y 1 0.1 ...
a0 [nm] 0.60 0.38 ...
bC [ppm] 65 50 ...
β ... 1.75 ...
Td [K] ... 20.7 ...
τ 250 ... 3.2 × 10-3 ...

Notes. xH and xC are the abundances of H+ and C+; y is the molecular fraction 2nH2/nH; a0 is the centroid of the PAH size distribution; bC is the PAH abundance of carbon in PAHs; and z is the depth of the emission region along the line of sight. The radiation field is that of Mathis et al. (1983) multiplied by the factor G0. The ionised gas accounts for the free-free emission but does not contribute to the spinning dust emission.

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