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


Table 2

Identification of saturated COMs and complex carbon chains in Orion-KL.

Species Identification Peak Column density at peak (cm-2) Other interferometric detections

CH3CN, SMA1 1.4(17), 9.4(14) a, b, e, i
CH2CHCN North to hotcore 5.0(15) b, d, e
CH3CH2CN hotcore 1.1(16) a, b, d, e, i, k
CH3OH SMA1 & mm3a 2.5(17) a, b, d, e, f, i, m
HCOOCH3 mm3a & mm3b 9.7(16) b, d, e, g, i, k
CH3COCH3 SMA1 1.5(16) c, i, k
CH3OCH3 mm3a & mm3b 2.0(17) b, d, e, h, i, j
CH3CH2OH near SMA1 & mm3a ≥ 1.5(16) d (×), e and j (only 1 line)
(CH2OH)2 ×
CH2OHCHO × g. (some lines <3σ)
HCOOH × d (×), l (<3σ), i (only from the extended configuration)
CH3CHO * mm3a & mm3b 1.3(16) d (×), i (×), n (CARMA and ALMA)
C6H * SMA1 1.0(15)
HC7N * North to hotcore 1.0(16)

Notes. Confirmed COMs are marked with “”, tentative detections with “*”, and nondetections with “×”. At each of their main emission peak (Fig. 5), column density of CH3CN is obtained with optical depth correction, while column densities of the rest molecules are obtained at the temperature of an adjacent substructure from synthetic fittings, with an assumption that the species lines are optically thin (we denote them by “”), x(y) = x × 10y.

Reference. a) Wright et al. (1996); b) Beuther et al. (2005); c) Friedel et al. (2005); d) Friedel & Snyder (2008); e) Guélin et al. (2008); f) Zapata et al. (2011); g) Favre et al. (2011a); h) Favre et al. (2011b); i) Widicus Weaver & Friedel (2012); j) Brouillet et al. (2013); k) Peng et al. (2013); l) Liu et al. (2002); m) Peng et al. (2012a); n) Loomis (priv. comm.).

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