Modelling the dust emission from dense interstellar clouds: disentangling the effects of radiative transfer and dust properties

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Table 3

Parameters defining the gas distribution of the modelled clouds.

DHGL (Dust at high galactic latitude)

A_v	1	2	3.5	5	7.5	10	12.5	15	17.5	20
ρ_C (H/cm³)	460	2900	11 480	26 800	69 300	135 350	225 500	341 000	481 500	647 750
H₀ (pc)	0.74	0.16	0.065	0.039	0.022	0.015	0.011	0.0090	0.0075	0.0063

Accreted grains
ρ_C	370	2300	9350	22 000	56 800	111 000	185 600	282 000	398 000	536 500
H₀	1.04	0.18	0.073	0.044	0.025	0.017	0.013	0.010	0.0083	0.0070

Aggregates 0%
ρ_C	590	3620	14 100	32 800	84 500	164 500	273 800	413 000	581 800	783 000
H₀	0.55	0.13	0.057	0.034	0.020	0.014	0.010	0.0081	0.0067	0.0057

Aggregates 10%
ρ_C	520	3240	12 700	29 700	76 500	149 000	248 300	375 000	528 600	711 100
H₀	0.64	0.14	0.061	0.037	0.021	0.014	0.011	0.0086	0.0071	0.0060

Aggregates 25%
ρ_C	420	2700	10 620	24 900	64 350	125 800	209 700	317 500	448 200	603 400
H₀	0.84	0.16	0.068	0.041	0.023	0.016	0.012	0.0094	0.0078	0.0066

Aggregates 40%
ρ_C	340	2200	8850	20 800	54 000	105 500	176 500	268 000	378 800	510 800
H₀	1.24	0.19	0.076	0.045	0.026	0.018	0.013	0.010	0.0085	0.0072

Notes. Central density (ρ_C in H/cm³) and internal flat radius (H₀ in pc) for the clouds with visual extinction at the centre A_V = 1 to 20, and for all the dust populations considered in the paper (see Table 2).

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