Hot HCN around young massive stars at 0.1′′ resolution

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Volume 529 (May 2011)

A&A, 529 (2011) A76

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Table 2

Parameters of absorption lines shown in Fig. 1.

Hii region	RA	Dec	Continuum^a	Line width^b	Velocity	Line/continuum	τ	HCN column density^c
	(J2000)	(J2000)	(K)	(km s^-1)	(km s^-1)			(cm^-2)

G10.47+0.03 B1	18 08 38.243	−19 51 50.22	2600	18.9	65.8	0.72	0.33	5.5(19)
G10.47+0.03 B2	18 08 38.22	−19 51 50.62	1800	18.5	66.4	0.776	0.25	4.1(19)
G10.47+0.03 A	18 08 38.188	−19 51 49.74	750	10.3	68	0.67	0.4	3.6(19)

SgrB2-N K2	17 47 19.882	−28 22 18.45	1150	10.0	63.6	0.16	1.83	1.6(20)
SgrB2-N K3	17 47 19.902	−28 22 17.18	1200	7.3	64.3	0.652	0.43	2.8(19)

SgrB2-M F1c	17 47 20.126	−28 23 03.9	2650	11.5	60.4	0.664	0.41	4.1(19)
SgrB2-M F1e	17 47 20.131	−28 23 04.02	2300	9.2	60.9	0.474	0.75	6.1(19)
SgrB2-M F1f	17 47 20.147	−28 23 03.88	3500	15.3	55.2	0.714	0.34	4.4(19)
SgrB2-M F3	17 47 20.172	−28 23 04.58	5350	6.7	71.2	0.696	0.36	2.1(19)

Notes. The beam size is 0.14′′ × 0.1′′ for G10.47+0.03 and 0.15′′ × 0.11′′ for SgrB2. The rms on 1 km s^-1 channels is 120 − 150 K. Results of Gaussian fits and lower limits on the optical depth τ and on the column density of hot HCN are given.

^(a)

The continuum flux density is the brightness temperature at the given locations in the line maps (which have a larger beam than the pure continuum maps). To convert from K to mJy/Beam, one has to divide by 53 for G10.47+0.03 and by 45 for SgrB2.

^(b)

Full Width at Half Maximum (FWHM) of the Gaussian.

^(c)

The numbers in parentheses are powers of 10.

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