Direct estimation of electron density in the Orion Bar PDR from mm-wave carbon recombination lines

S. Cuadrado; P. Salas; J. R. Goicoechea; J. Cernicharo; A. G. G. M. Tielens; A. Báez-Rubio

doi:10.1051/0004-6361/201935556

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Volume 625 (May 2019)

A&A, 625 (2019) L3

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Table A.1.

Line spectroscopic parameters obtained from Gaussian fits to the observed mmCRLs (see Sect. 2).

Line	Frequency	∫T_MB dv^(a)^,^(b)	v_LSR^(b)	Δv^(b)	T_MB^(a)	S/N^(c)	HPBW ^(d)
	(MHz)	(mK km s⁻¹)	(km s⁻¹)	(km s⁻¹)	(mK)		(arcsec)
C42α	85731.14	226.8 (10.5)	10.6 (0.1)	2.6 (0.1)	83.1	21	28.7
C41α	92080.35	248.9 (14.2)	10.8 (0.1)	2.7 (0.1)	85.6	17	26.7
C40α	99072.36	172.6 (7.2)	10.7 (0.1)	2.5 (0.1)	63.6	23	24.8
C39α	106790.61	190.9 (13.3)	10.7 (0.1)	2.9 (0.2)	53.5	12	23.0
C38α	115331.91	163.9 (19.6)	10.9 (0.2)	2.4 (0.3)	65.4	5	21.3

C52β	88449.80	53.8 (9.4)	10.7 (0.2)	2.9 (0.5)	24.5	6	27.8
C51β	93654.02	55.2 (8.3)	10.5 (0.2)	2.9 (0.6)	24.8	6	26.3
C50β	99274.72	47.7 (6.0)	10.7 (0.1)	2.7 (0.3)	23.6	8	24.8
C49β	105354.40	42.4 (8.5)	10.6 (0.2)	2.6 (0.5)	21.5	4	23.3
C48β	111940.89	36.9 (11.0)	10.6 (0.2)	2.3 (0.6)	21.8	4	22.0

C60γ	84956.76	27.8 (8.2)	10.5 (0.2)	1.7 (0.5)	22.3	5	29.0
C59γ	89243.05	35.1 (8.3)	10.9 (0.3)	3.0 (0.6)	15.4	4	27.6

Notes.

^(a)

Intensities in main beam temperature (in units of mK).

^(b)

Parentheses indicate the uncertainty obtained by the Gaussian fitting routine.

^(c)

Signal-to-noise ratio with respect to the peak line temperature in velocity resolution channels of 0.7 km s⁻¹.

^(d)

The half power beam width (HPBW) of the IRAM 30 m telescope is well described by HPBW[arcsec] ≈ 2460/Frequency[GHz].

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