Search for methylamine in high mass hot cores

N. F. W. Ligterink; E. D. Tenenbaum; E. F. van Dishoeck

doi:10.1051/0004-6361/201424845

Free Access

Issue		A&A Volume 576, April 2015


Article Number		A35
Number of page(s)		11
Section		Interstellar and circumstellar matter
DOI		https://doi.org/10.1051/0004-6361/201424845
Published online		23 March 2015

Online material

Appendix A: Methylamine and other transitions

Fig. A.1

Bargraph plot of the integrated main-beam intensities for the six investigated methylamine transitions. values were calculated for a total column density of 3.4 × 10¹⁷ cm^-2 as inferred toward G31.41+0.31 from the 6₂ → 6₁ transition, assuming a rotational temperature of 120 K. The horizontal line shows the 0.077 K km s^-1 3σ value for G31.41+0.31. It is unlikely that the detection of the 236 408 feature (green) in this hot core is methylamine, since the main-beam intensities of other CH₃NH₂ transitions are above the 3σ value. Particularly the 4₂ → 4₁ and 2₂ → 2₁ transition (blue) should be visible in our spectra. The remaining transitions (red) are either below detection limit or not observed toward this source.

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Table A.1

All identified transitions for the sources G31.41+0.31 and W3(H₂O), with integrated peak area listed.

	Fig. A.2 Blow-up of the spectral region around the 2₂→ 2₁ transition at 237143 MHz of all analysed hot cores. Despite being a particularly strong transition, it was not observed in any of the spectra.
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Appendix B: ALMA

In the following figure the simulated spectrum of methylamine is shown for a column density of 1.0 × 10¹⁵ cm^-2 at an excitation temperature of 120 K. Simulations were done with CASSIS using the JPL spectroscopic database. The frequency ranges were taken to cover ALMA Bands 6 and 7. The resolution was set at 0.1 MHz for this spectrum.

	Fig. B.1 211 to 373 GHz spectrum of methylamine, covering ALMA bands 6 and 7. A column density of 10¹⁵ cm^-2, T_rot and beam size of 1′′ are used.
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Table B.1

Methylamine transition target candidates for ALMA Band 6 and 7.

© ESO, 2015

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