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]

Issue		A&A Volume 581, September 2015


Article Number		A71
Number of page(s)		50
Section		Interstellar and circumstellar matter
DOI		https://doi.org/10.1051/0004-6361/201322725
Published online		04 September 2015

Online material

Appendix A

Table A.1

Identified emission lines from the SMA-30 m combined dataset.

Table A.2

Laboratory parameters of CH₃CN and and the intensity integrated over the width of each line , which is used for rotation diagrams in Fig. 8.

Table A.3

The laboratory parameters and the intensity integrated over the width of each line , which is used for rotation diagrams in Fig. 9.

Table A.4

Intensity integrated over the width of each line, corresponding to the transitions shown in Fig. A.3.

Table A.5

Column densities and abundances for O-bearing molecules and carbon chains from different substructures in Orion-KL denoted in Figs. 4 and 5.

Table A.6

Column densities and abundances for N-bearing molecules from different substructures in Orion-KL denoted in Figs. 4 and 5.

Table A.7

Column densities and abundances for S-bearing molecules from different substructures in Orion-KL denoted in Fig. 4.

	Fig. A.1 Spectrum from the HC, with identified strong lines marked. From 220.5 GHz to 220.8 GHz, CH₃CN and are labelled in red and blue, respectively. COMs containing only C, H, O elements and other tentatively detections are labelled in Fig. A.2.
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Fig. A.2

Synthetic spectrum fitting of COMs towards their emission peaks (V_lsr of each species are corrected according to V_peak from Fig. A.3). The black histograms are the observed spectra, overlaid with a best fit model spectrum for given uniform FWHM linewidth (△ V) (fit from Fig. A.3), T_rot (assumed from an adjacent substructure), and N_mol (adjusted based on N_T in Tables A.5I−A.7I) listed on top of each panel. Blue lines mark the central frequency of each transition. Uncertainties of the fitting to observations come from the assumption that under LTE, the candidate molecule lines are optically thin, and each species has the same line width at different transitions. Referenced molecular data are from CDMS/JPL (Sanchez-Monge 2011; Palau et al. 2011).

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	Fig. A.2 continued.
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	Fig. A.2 continued.
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	Fig. A.2 continued.
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Fig. A.3

Line profiles of identified species from each continuum peak. In measuring the main V_peak and ΔV of each line at each substructure, lines in green and notes in blue (in the form of “value(error)”) are given by the Gaussian fittings using Gildas software. Multi-Gaussian fittings are used to CH₃CN, , HCOOCH_{3 (ν = 0)}, and CH₃COCH₃ due to blending, and to SO₂, ³⁴SO₂, and SO due to the second velocity component (the second velocity component of HNCO measured from multi-Gaussian fittings are given in Fig. 7). Single Gaussian fittings are used to the rest lines, while lines whose V_peak cannot be measured by Gaussian fittings owing to strong self-absorption are marked with “**”, and non-detections are not marked. Two red vertical lines in each panel mark the velocity range over which the emission from each species is integrated to make the distribution maps shown in Figs. 4 and 5.

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	Fig. A.3 continued.
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	Fig. A.3 continued.
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	Fig. A.3 continued.
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	Fig. A.3 continued.
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Fig. A.4

Line wing flux integration maps from the combined SMA-30 m data at 1.3 mm. The grey maps show the intensity integrated ranging through the main emission of their linewidth in Fig. A.3. Red and blue contours show the red-shifted and blue-shifted gas, with the intensity integrated as labelled. Yellow lines sketch the outflow directions. Black crosses denote the hotcore, SMA1, Source I, and Source N; white crosses denote the BN object and CR.

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	Fig. A.5 Channel maps of the second velocity component (V_peak ~ 22 km s^-1) of the strongest unblended ³⁴SO₂ and SO₂ line, as well as of SO(6₅ → 5₄).
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Fig. A.6

Channel maps of unblended CH₃OH lines show multiple velocity-dependent emission peaks: 2.4 − 3.6 km s^-1 towards SMA1, ~4.8 − 6 km s^-1 towards HC, 7.2 − 9.6 km s^-1 towards HC/mm3a/mm3b, 10.8 km s^-1 towards mm3a/mm3b/mm2 and >12 km s^-1 towards mm2. Green lines sketch the outflow directions. Black crosses denote the hotcore, SMA1, Source I, and Source N; white crosses denote the BN object and the CR.

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© ESO, 2015

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