Kinetic temperature of massive star-forming molecular clumps measured with formaldehyde - III. The Orion molecular cloud 1

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Table 1

Comparison of temperatures derived from different tracers.

Region	H₂CO	NH₃	CH₃CCH	CO(1–0)	CO(6–5)	MIR	FIR
	K	K	K	K	K	K	K

KL	120–290	>100	50–60	78–88	>150	>150	45–60
South	~74	~50	~46	81–92	>150	~75	~30
North	~40	20–30	13–40	43–60	...	...	26–30
Northeast	70–160	>50	40–51	60–78	...	...	30–44
Bar (clump)	~73	>50	...	...	>150	~70	33–50
Bar (edge)	100–130	>100	...	...	>100	>100	41–51

Notes. Column 2: kinetic temperatures derived from para-H₂CO line ratios (see Sect. 3.2). Column 3: kinetic temperatures derived from the NH₃ (2, 2)/(1, 1) line ratios taken from Friesen et al. (2017). Column 4: rotation temperatures obtained from CH₃CCH (6–5) taken from Bergin et al. (1994). Columns 5 and 6: excitation temperatures of CO (1–0) and CO (6–5) taken from Bergin et al. (1994) and Peng et al. (2012), respectively. Columns 7 and 8: mid (MIR) and far infrared (FIR) dust temperatures taken from Downes et al. (1981), Vaillancourt (2002), Lombardi et al. (2014), Salgado et al. (2016), and Kauffmann et al. (2017).

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