The millimeter-wave spectrum of methyl ketene and the astronomical search for it

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Volume 619 (November 2018)

A&A, 619 (2018) A92

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Table 5.

Physical parameters of the considered cloud cores.

Source	Coordinates (J2000.0)	HPBW^a (″)	Frequencies^b (GHz)	v_LSR (km s⁻¹)	Δv_FWHM (km s⁻¹)	d_sou (″)	T_rot (K)	N(CH₃CHCO) ×10¹⁴ (cm⁻²)
Orion KL	α = 5^h35^m14.5^s	30–8	80–307	8	3	5	150	≤(5.0 ± 2.5)
(IRAM 30 m)	δ = −05^∘22′30.0″

Orion KL	α = 05^h35^m14.5^s	∼1.9 × 1.4	213.7–246.7	8	3	3	150	≤(10 ± 5)
(ALMA SV)	δ = −05^∘22′32.5″
Hot core

Orion KL	α = 05^h35^m14.1^s	∼1.9 × 1.4	213.7–246.7	7.5	2	3	100	≤(3.0 ± 1.5)
(ALMA SV)	δ = −05^∘22′36.9″
Compact ridge

Orion KL	α = 05^h35^m14.2^s	∼1.9 × 1.4	213.7–246.7	3	3	3	150	≤(5.0 ± 2.5)
(ALMA SV)	δ = −05^∘22′31.1″			5	8	3	150	≤(2.0 ± 1.0)
MM4

Sgr B2(N)	(IRAM 30 m)	30–21	80–115.5	63	9	3	100	≤(100 ± 50)
	α = 17^h47^m20.0^s			72	8	3	100	≤(100 ± 50)
	δ = −28^∘22′19.0″
	(GBT 100m)	80–15	7–50
	α = 17^h47^m19.8^s
	δ = −28^∘22′17.0″

B1-b	α = 03^h33^m20.0^s	30–21	80–115.5	6.7	0.7	60	12	≤(0.010 ± 0.005)
(IRAM 30 m)	δ = 31^∘07′34.0″

TMC-1	α = 04^h41^m41.88^s	30–21	80–115.5	6.0	0.7	60	10	≤(0.010 ± 0.005)
(IRAM 30 m)	δ = 25^∘41′27.0″

Notes.

^(a)

HPBW (half power beam width) for observations with single dish telescope (IRAM 30 m and GBT 100 m) and synthetic beam for the ALMA SV observations.

^(b)

Range of frequencies considered in the analysis.

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