Vibrationally excited HC3N in NGC 4418 | Astronomy & Astrophysics (A&A)

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Volume 515 (June 2010)

A&A, 515 (2010) A71

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Table 1:

Observed HC₃N Lines Properties.
Transition	Rest frequency	Tuning frequency	HPBW^a	$\int{T_{\rm A}^\star {\rm d}v}$	$T_{\rm b}$ ^b	$\Delta V$ ^c	$\eta_{mb}$ ^d	$A_{u\ell}$ ^e	E_u^f	Ref.^g
J_u-J_l (v₆,v₇)	[GHz]	[GHz]	['']	[mK km s^-1]	[K]	[km s^-1]		[s^-1]	[K]

10-9 (0, 0)	90.979	91.114	27	711 $\pm$ 20	1.5	134	0.77	5.8e-05	24.1	IRAM 07-08
(1e, 0)	91.128	''	27	<70	-	-	0.77	5.8e-05	736.6	IRAM 07-08
(0, 1e)	91.202	''	27	159 $\pm$ 17	0.4	108	0.77	5.8e-05	342.6	IRAM 07-08
(0, 1f)	91.333	''	27	155 $\pm$ 14	0.4	110	0.77	5.8e-05	342.6	IRAM 07-08
16-15 (0, 0)	145.561	145.561	17	1700 $\pm$ 80	1.7	130	0.70	2.4e-04	59.4	Aalto 2007
17-16 (0, 0)	154.657	154.948	16	469 $\pm$ 52	0.5	117	0.67	2.9e-04	67.3	IRAM 07-08
(1e, 0)	155.032	''	16	<150	-	-	0.67	2.9e-04	779.2	IRAM 07-08
(0, 1e)	155.037	''	16	316 $\pm$ 59	0.3	141	0.67	2.9e-04	385.2	IRAM 07-08
(0, 1f)	155.259	''	16	316 $\pm$ 59	0.3	141	0.67	2.9e-04	385.3	IRAM 07-08
(1e, 0)	154.911	''	16	<150	-	-	0.67	2.9e-04	779.2	IRAM 07-08
25-24 (0, 0)	227.418	227.757	11	2020 $\pm$ 140	1.1	140	0.54	9.3e-04	143.0	IRAM 12-07
(1e, 0)	227.793	''	11	480 $\pm$ 110	0.3	125	0.54	9.3e-04	853.9	IRAM 12-07
(0, 1e)	227.977	''	11	928 $\pm$ 120	0.6	125	0.54	9.3e-04	459.9	IRAM 12-07
28-27 (0, 0)	254.699	254.699	10	1720 $\pm$ 100	0.9	141	0.47	1.3e-03	178.6	IRAM 12-07
28-27 (0, 0)	254.699	255.018	10	1315 $\pm$ 100	0.7	159	0.47	1.3e-03	178.6	IRAM 07-08
(1e, 0)	255.119	''	9.7	<200	-	-	0.47	1.3e-03	889.1	IRAM 07-08
(0, 1e)	255.324	''	9.7	327 $\pm$ 82	0.3	83	0.47	1.3e-03	495.2	IRAM 07-08
30-29 (0, 0)	272.884	272.884	9	1300 $\pm$ 200	0.5	182	0.44	1.6e-03	204.6	IRAM 07-08
38-37 (0, 0)	345.609	345.609	14	1930 $\pm$ 250 $^{{\rm h}}$	1.8	120	0.63	3.3e-03	326.0	JCMT 2007

Notes. ^(a) Half power beam width. ^(b) Brightness temperature, assuming a 2'' source size. ^(c) Full width at half maximum from Gaussian fit. ^(d) Main beam efficiency. ^(e) Einstein's transition coefficient. ^(f) Energy above ground of the upper level. ^(g) Telescope and epoch. ^(h) From Gaussian fit to the CO 3-2 spectrum, see Fig. 1.

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