Resolving the chemical substructure of Orion-KL | Astronomy & Astrophysics (A&A)

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Volume 581 (September 2015)

A&A, 581 (2015) A71

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This article has an erratum: [https://doi.org/10.1051/0004-6361/201322725e]

Table 1

Properties of substructures, which are denoted on the continuum image obtained from SMA observations at 1.3 mm (Fig. 2).

Source		RA (α)	Dec (δ)	I _ν ^a	T _rot	N _H₂,1 ^d	N _H₂,2 ^e	Alternative designations
		[J2000]	[J2000]	(Jy/beam)	(K)	(10²³ cm^-2)	(10²³ cm^-2)
		5h35m ~	−5°22^′ ~			3.49″ × 2.57″	5.55″ × 4.35″


					155 ± 16^b₁	23.7 ± 4.6
					121 ± 16^b₂	31.0 ± 6.7
HC		14.6 s	31.0′′	2.75 ± 0.3	126 ± 13^b₃	29.6 ± 5.8	11.9 ± 0.7	Ca^j, SMM3^l, CntB^k
					225 ± 19^b₄	16.3 ± 2.9
					199 ± 45^b₅	18.4 ± 5.1


	hotcore^f	14.58 s	30.97′′
	SMA1^f	14.46 s	32.36′′
	Source I^g	14.51 s	30.53″
	Source N^g	14.35 s	33.49″


					108 ± 4^b₁	11.0 ± 1.7
mm2		14.1 s	27.1′′	0.87 ± 0.10	112 ± 7^b₃	10.5 ± 1.8	9.3 ± 0.1	NWC^h,i, Cc^j, SMM2^l,
					174 ± 14^b₄	6.7 ± 1.2		WCⁿ, CntD^k
					173 ± 40^b₅	6.7 ± 1.9


CR^l		14.0 s	36.9′′					SWCⁱ, SMM1^l


					103 ± 3^b₁	12.8 ± 1.6
	mm3a	14.3 s	37.9′′	0.96 ± 0.09	101 ± 5^b₃	13.1 ± 1.8	6.2 ± 0.07	Cb1^j, CntC^k
					159 ± 12^b₄	8.1 ± 1.3
					101 ± 26^b₅	13.1 ± 3.7


					88 ± 6^b₁	15.9 ± 2.7
	mm3b	14.1s	36.4′′	1.01 ± 0.11	102 ± 5^b₃	13.5 ± 2.1	6.7 ± 0.05	Cb2^j, CntC^k
					160 ± 17^b₄	8.5 ± 1.6
					89 ± 24^b₅	15.6 ± 4.8


NE		14.8 s	19.1′′	0.38 ± 0.09	43 ± 3^b₁	20.1 ± 4.2	3.3 ± 0.06	CntH^k


SR		14.0 s	45.4′′	0.41 ± 0.06	43 ± 3 ^c	14.2 ± 2.9	1.0 ± 0.02	Cd^j, MM23^m

OF1N		13.4 s	20.5′′	σ = 0.04	43 ± 3 ^c	< 4.2	~ 1.1	PK1^o

OF1S		15.3 s	42.5′′	σ = 0.03	43 ± 3 ^c	< 3.1	~ 0.6	PK2^o


BN^o		14.11s	22.7′′

Notes. Positions with upper case are from the references listed in the footnotes, without are from 1.3 mm SMA continuum observations.

^(a)

Peak specific intensity I_ν is obtained from each substructure of SMA-only continuum.

^(b1)

Excitation temperature is from CH₃CN rotation map fitting in Fig. 8.

^(b2)

Excitation temperature is from rotation map fitting in Fig. 8.

^(b3)

Excitation temperature is from HCOOCH₃ rotation map fitting in Fig. 9.

^(b4)

Excitation temperature is from CH₃OH rotation map fitting in Fig. 9.

^(b5)

Excitation temperature is from ³⁴SO₂ rotation map fitting in Fig. 9.

^(c)

Excitation temperature is assumed the same as that in NE from CH₃CN.

^(d)

H₂ column density is calculated from the SMA-only continuum at substructure peak using Eq. (11), performed in Sect. 4.2.2.

^(e)

H₂ column density is calculated from the conversion of combined SMA-30 m C¹⁸O at temperatures derived from HCOOCH₃, performed in Sect. 4.2.2.

Reference. ;

^(f)

Beuther et al. (2004);

^(g)

Menten & Reid (1995);

^(h)

Blake et al. (1996);

⁽ⁱ⁾

Tang et al. (2010);

^(j)

Favre et al. (2011a);

^(k)

Murata et al. (1992);

^(l)

Zapata et al. (2011);

^(m)

Eisner et al. (2008)

⁽ⁿ⁾

Wright et al. (1992);

^(o)

Beckwith et al. (1978).

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