Orion KL: the hot core that is not a “hot core”

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Table 1

Observational and physical parameters of submillimeter and millimeter lines.

	Rest frequency	E_lower/k	Range of velocities	Linewidth^a	LSR velocity	Peak flux
Lines	[GHz]	[K]	[km s^-1]	[km s^-1]	[km s^-1]	[Jy Beam^-1]

CH₃CN(12₃–11₃)	220.7090...	122	−10, + 26	18	7	17
CH₃CN(12₆–11₆)	220.5944...	315	−5, + 15	13	5	12
CH₃CN(12₉–11₉)	220.4039...	636	+ 2, + 12	4	6	1
CH₃OH(7_4,3–6_4,3) A⁻ (ν_t = 1)	337.9694...	373	−5, + 15	5	8	13
CH₃OH(7_4,3–6_4,3) A⁻ (ν_t = 2)	337.8775...	705	−2, + 11	4	8	3
HC₃N(37–36)(ν₇ = 1)	337.8240...	613	−12, + 19	14	4	8
SO₂(21_2,20–21_1,21)(ν₂ = 1)	337.8925...	948	−1, + 13	5	6	2

Notes.

^(a)

For the HC₃N(37−36) and CH₃OH(7_4,3–6_4,3) A⁻ (ν_t = 1) torsionally/vibrationally excited lines the average linewidth given here is the sum of two velocity components, one centered at approximately − 4 km s^-1 and the other one at + 7 km s^-1.

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