Observations of nitrogen isotope fractionation in deeply embedded protostars

Free Access

Issue		A&A Volume 572, December 2014


Article Number		A24
Number of page(s)		16
Section		Interstellar and circumstellar matter
DOI		https://doi.org/10.1051/0004-6361/201423773
Published online		21 November 2014

Online material

Appendix A: Observational details

Fig. A.1

Comparison of the H¹³CO⁺(3−2) line from IRAS 16293A observed with APEX. The spectra resulting from phase 1 (corresponding to off position on one side of the source in symmetric wobbler switching mode) and phase 2 (off position on the other side) are shown in blue and red, respectively. The spectra have been baseline subtracted and normalized to the average peak intensity of the two spectra. Data from 2012-04-01.

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	Fig. A.2 Like Fig. A.1 but for H¹³CN(3−2). Includes a sinusoidal baseline for standing wave removal.
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	Fig. A.3 Like Fig. A.1 but for R CrA IRS7B. Data from 2012-09-27.
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	Fig. A.4 Like Fig. A.3 but for H¹³CN(3−2).
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	Fig. A.5 Like Fig. A.1 but for OMC-3 MMS6. Data from 2012-11-22.
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	Fig. A.6 Like Fig. A.5 but for H¹³CN(3−2).
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Table A.1

Observational details.

Appendix B: Literature values

Table B.1

Measurements of the ¹⁴N/¹⁵N ratio in solar system materials from the literature. (B) Stands for “bulk” measurements and (HS) for “hotspot”.

Table B.2

Integrated intensities for IRAS 16293-2422 from the surveys by Caux et al. (2011) and Blake et al. (1994); van Dishoeck et al. (1995).

© ESO, 2014

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