HC3N observations of nearby galaxies | Astronomy & Astrophysics (A&A)

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Table 2

HC₃N 2-1 spectral measurements.

Source	On-time	RMS	δV	ΔV	V₀	I(HC₃N)	S(HC₃N)
	(min)	(mK)	(km s^-1)	(km s^-1)	(km s^-1)	(K km s^-1)	(Jy km s^-1)
(1)	(2)	(3)	(4)	(5)	(6)	(7)	(8)	(9)

NGC 660	28	4.2	32.2	260.7 (90.6)	825 (36)	1.47 (0.40)	0.86 (0.24)	~0.034^a
IC 342	20	6.5	20.1	52.0 (12.9)	45 (6)	0.77 (0.18)	0.45 (0.11)	~0.005^b
M 66	18	7.0	20.1	44.8 (17.7)	775 (7)	0.68 (0.21)	0.4 (0.12)	~0.114^c
NGC 520	14	5.7	...	...	...	<1.02	<0.6	<0.087^d
NGC 891	30	2.3	...	...	...	<0.26	<0.15	<0.033^e
NGC 972	33	3.8	...	...	...	<0.61	<0.36	...
NGC 1068	25	4.0	...	...	...	<0.73	<0.43	<0.013^f
UGC 2855	23	4.9	...	...	...	<0.76^*	<0.45	...
UGC 2866	22	3.6	...	...	...	<0.56^*	<0.33	...
NGC 1569	33	3.0	...	...	...	<0.31	<0.18	...
NGC 2146	24	3.4	...	...	...	<0.67	<0.39	<0.021^e
NGC 2403	30	3.2	...	...	...	<0.33	<0.19	...
M 82	26	5.5	...	...	...	<0.73	<0.43	<0.011^e
NGC 3079	19	5.5	...	...	...	<1.17	<0.69	<0.225^e
NGC 3310	36	2.3	...	...	...	<0.29	<0.17	...
IC 694+NGC3690	47	4.2	...	...	...	<0.72	<0.42	<0.158^g
Mrk 231	44	6.4	...	...	...	<0.91	<0.54	<0.191^g
Arp 220	26	4.5	...	...	...	<0.94	<0.55	<0.069^h
NGC 6946	28	5.1	...	...	...	<0.64	<0.38	<0.018^e

Notes. All the temperature scales are T_mb. The columns are: (1) galaxy name; (2) on-source time for each galaxy; (3) RMS noise of the smoothed spectrum; (4) velocity resolution of the smoothed spectrum; (5) line width (FWHM) of the Gaussian fit of the line (if available); (6) HC₃N emission line center; (7) integrated intensity (and errors) of HC₃N 2−1 emission. For those non-detections, 2σ upper limits are presented (see text in Sect. 3.1); (8) integrated flux density, and (9) flux density ratio between HC₃N 2−1 and HCN 1−0. HCN 1−0 data from:

^(*)

The upper limits of the two galaxies are derived assuming a 200 km s^-1 line width.

^(a)

Baan et al. (2008);

^(b)

Nguyen et al. (1992);

^(c)

Krips et al. (2008);

^(d)

Solomon et al. (1992);

^(e)

Gao & Solomon (2004a);

^(f)

Aladro et al. (2015);

^(g)

Jiang et al. (2011);

^(h)

Wang et al. (2016).

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