Multiline observations of hydrogen, helium, and carbon radio-recombination lines toward Orion A: A detailed dynamical study and direct determination of physical conditions

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Table 12

Results of Bayesian analysis using results from the non-LTE excitation code.

Source	n_e	T_e	N(C⁺)	τ_[CII]	T_ex([CII])	p_th/k_B
	(cm⁻³)	(K)	(10¹⁸ cm⁻²)		(K)	(K cm⁻³)
BAR-INSIDE	$20_{- 10}^{+ 20}$ $20_{ - 10}^{ + 20}$	$230_{- 30}^{+ 50}$ $230_{ - 30}^{ + 50}$	${3.5}_{- 1.0}^{+ 1.5}$ $3.5_{ - 1.0}^{ + 1.5}$	${1.5}_{- 0.5}^{+ 0.5}$ $1.5_{ - 0.5}^{ + 0.5}$	$220_{- 20}^{+ 40}$ $220_{ - 20}^{ + 40}$	3 × 10⁷
BNKL-PDR^(a)	$40_{- 20}^{+ 100}$ $40_{ - 20}^{ + 100}$	$240_{- 30}^{+ 140}$ $240_{ - 30}^{ + 140}$	${5.0}_{- 2.5}^{+ 3.9}$ $5.0_{ - 2.5}^{ + 3.9}$	${2.0}_{- 1.3}^{+ 1.5}$ $2.0_{ - 1.3}^{ + 1.5}$	$230_{- 20}^{+ 140}$ $230_{ - 20}^{ + 140}$	6 × 10⁷
TRAP-PDR^(b)	$140_{- 50}^{+ 60}$ $140_{ - 50}^{ + 60}$	$360_{- 60}^{+ 80}$ $360_{ - 60}^{ + 80}$	${2.8}_{- 0.6}^{+ 0.7}$ $2.8_{ - 0.6}^{ + 0.7}$	${0.7}_{- 0.2}^{+ 0.3}$ $0.7_{ - 0.2}^{ + 0.3}$	$350_{- 50}^{+ 80}$ $350_{ - 50}^{ + 80}$	3 × 10⁸
EAST-PDR-2	$20_{- 10}^{+ 90}$ $20_{ - 10}^{ + 90}$	$210_{- 30}^{+ 200}$ $210_{ - 30}^{ + 200}$	${3.5}_{- 1.8}^{+ 2.1}$ $3.5_{ - 1.8}^{ + 2.1}$	${1.6}_{- 1.2}^{+ 1.0}$ $1.6_{ - 1.2}^{ + 1.0}$	$200_{- 20}^{+ 200}$ $200_{ - 20}^{ + 200}$	3 × 10⁷
ORI-P1-1	$2_{- 1}^{+ 1}$ $2_{ - 1}^{ + 1}$	$100_{- 10}^{+ 10}$ $100_{ - 10}^{ + 10}$	${5.0}_{- 2.1}^{+ 2.1}$ $5.0_{ - 2.1}^{ + 2.1}$	${5.4}_{- 0.6}^{+ 1.4}$ $5.4_{ - 0.6}^{ + 1.4}$	$90_{- 10}^{+ 10}$ $90_{ - 10}^{ + 10}$	1 × 10⁶
ORI-P1-2	$8_{- 3}^{+ 100}$ $8_{ - 3}^{ + 100}$	$150_{- 10}^{+ 190}$ $150_{ - 10}^{ + 190}$	${1.6}_{- 0.9}^{+ 0.6}$ $1.6_{ - 0.9}^{ + 0.6}$	${1.8}_{- 1.5}^{+ 0.9}$ $1.8_{ - 1.5}^{ + 0.9}$	$140_{- 10}^{+ 190}$ $140_{ - 10}^{ + 190}$	8 × 10⁶
ORI-P2	$2_{- 1}^{+ 2}$ $2_{ - 1}^{ + 2}$	$140_{- 10}^{+ 10}$ $140_{ - 10}^{ + 10}$	${4.5}_{- 1.2}^{+ 0.5}$ $4.5_{ - 1.2}^{ + 0.5}$	${2.6}_{- 1.0}^{+ 0.1}$ $2.6_{ - 1.0}^{ + 0.1}$	$120_{- 10}^{+ 10}$ $120_{ - 10}^{ + 10}$	2 × 10⁶
ORI-P3-2^(c)	—	—	${1.6}_{- 0.8}^{+ 3.4}$ $1.6_{ - 0.8}^{ + 3.4}$	${1.2}_{- 1.0}^{+ 3.6}$ $1.2_{ - 1.0}^{ + 3.6}$	$130_{- 30}^{+ 300}$ $130_{ - 30}^{ + 300}$	—
ORI-P4	$3_{- 2}^{+ 62}$ $3_{ - 2}^{ + 62}$	$140_{- 20}^{+ 330}$ $140_{ - 20}^{ + 330}$	${1.4}_{- 0.7}^{+ 1.4}$ $1.4_{ - 0.7}^{ + 1.4}$	${1.2}_{- 1.0}^{+ 1.7}$ $1.2_{ - 1.0}^{ + 1.7}$	$120_{- 30}^{+ 330}$ $120_{ - 30}^{ + 330}$	3 × 10⁶
ORI-P5	$2_{- 1.5}^{+ 12}$ $2_{ - 1.5}^{ + 12}$	$180_{- 50}^{+ 220}$ $180_{ - 50}^{ + 220}$	${1.8}_{- 0.7}^{+ 1.4}$ $1.8_{ - 0.7}^{ + 1.4}$	${0.9}_{- 0.7}^{+ 1.3}$ $0.9_{ - 0.7}^{ + 1.3}$	$140_{- 40}^{+ 190}$ $140_{ - 40}^{ + 190}$	1 × 10⁶
ORI-P6	$1_{- 0.1}^{+ 1}$ $1_{ - 0.1}^{ + 1}$	$130_{- 10}^{+ 10}$ $130_{ - 10}^{ + 10}$	${5.0}_{- 0.5}^{+ 0.6}$ $5.0_{ - 0.5}^{ + 0.6}$	${5.2}_{- 0.1}^{+ 0.1}$ $5.2_{ - 0.1}^{ + 0.1}$	$120_{- 10}^{+ 10}$ $120_{ - 10}^{ + 10}$	8 × 10⁵

Notes. Errors are given at 1σ. The electron densities may be converted to hydrogen nuclei densities by dividing by the carbon gas-phase abundance in Orion, 𝒜_C = 1.4 × 10⁻⁴. ^(a)We used [¹³C II] F=1–0 and F=1–1 satellites. ^(b)[¹³C II] line in TRAP-PDR weaker than expected given the isotopic ratio of Orion. ^(c)CRRL in ORI-P3 does not match PDR component, hence only [C II] properties.

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