Millimeter wave spectroscopy of cyanoketene (NC–CH=C=O) and an observational search in the ISM

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Table 3.

Source parameters assumed for cyanoketene in each of the sets of observations.

Source	Telescope	θ_s^(a)	T_bg	ΔV	T_b ^(†)	T_ex	Refs.
		(″)	(K)	(km s⁻¹)	(mK)	(K)
NGC 6334I	ALMA	–	28.2	3.2	10.0 ^(b)	135	1
Sgr B2(N)	GBT	20	19.2	25.0	3.7	5	2, 14, 15
Sgr B2(N)	IRAM	2.2	5.2	5.0	10.9	120	3
Barnard 1	IRAM	–	2.7	0.8	2.5	10	4, 5
IRAS 4A	IRAM	–	2.7	5.0	2.3	21	4, 6
L1157B1	IRAM	–	2.7	8.0	1.4	60	7
L1157mm	IRAM	–	2.7	3.0	2.8	60	7
L1448R2	IRAM	–	2.7	8.0	2.4	60	8
L1527	IRAM	–	2.7	0.5	1.9	12	8, 9
L1544	IRAM	–	2.7	0.5	2.3	10	10, 11
SVS13A	IRAM	0.3	2.7	3.0	7.5	80	4, 6
TMC1	IRAM	–	2.7	0.3	6.5	7	12, 13

Notes.

^(a)

Except where noted, the source is assumed to fill the beam.

^(b)

For these interferometric observations, the intensity is given in mJy beam⁻¹ rather than mK.

^(†)

Taken either as the 1σ rms noise level at the location of the target line, or for line confusion limited spectra, the reported rms noise of the observations.

References. [1] McGuire et al. (2018a); [2] Neill et al. (2012); [3] Belloche et al. (2013); [4] Melosso et al. (2018); [5] Cernicharo et al. (2018); [6] Higuchi et al. (2018); [7] McGuire et al. (2015); [8] Jørgensen et al. (2002); [9] Araki et al. (2017); [10] Hily-Blant et al. (2018); [11] Crapsi et al. (2005); [12] McGuire et al. (2018b); [13] Gratier et al. (2016); [14] Remijan et al. (2008); [15] McGuire et al. (2016).

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