An ALMA Early Science survey of molecular absorption lines toward PKS 1830−211 - Analysis of the absorption profiles

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Volume 566 (June 2014)

A&A, 566 (2014) A112

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Issue		A&A Volume 566, June 2014


Article Number		A112
Number of page(s)		21
Section		Extragalactic astronomy
DOI		https://doi.org/10.1051/0004-6361/201423646
Published online		20 June 2014

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Appendix A: ALMA cycle 0 data

Table A.1

Lines detected at z = 0.89 toward PKS 1830−211 in the ALMA cycle 0 survey.

	Fig. A.1 ALMA cycle 0 B3–100 GHz spectra, after self-bandpass of the SW spectra by the NE spectra. Absorption lines from the SW line-of-sight appear as <1-feature, while the absorption lines from the NE line-of-sight appear as >1-feature.
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	Fig. A.2 ALMA cycle 0 B6–250 GHz spectra, after self-bandpass of the SW spectra by the NE spectra. Absorption lines from the SW line-of-sight appear as <1-feature, while the absorption lines from the NE line-of-sight appear as >1-feature.
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	Fig. A.3 ALMA cycle 0 B7–290 GHz spectra, after self-bandpass of the SW spectra by the NE spectra. Absorption lines from the SW line-of-sight appear as <1-feature, while the absorption lines from the NE line-of-sight appear as >1-feature.
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	Fig. A.4 ALMA cycle 0 B7–300 GHz spectra, after self-bandpass of the SW spectra by the NE spectra. Absorption lines from the SW line-of-sight appear as <1-feature, while the absorption lines from the NE line-of-sight appear as >1-feature.
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Table A.2

O₃ atmospheric lines in the observed bands.

	Fig. A.5 Time variations toward the SW image between 2012 April 09 and 2012 May 23.
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	Fig. A.6 Time variations toward the SW image between 2012 May 22 and 2012 Jun 04.
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	Fig. A.7 Time variations toward the SW image between 2012 Jun. 04 and 2012 Jun. 15.
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	Fig. A.8 Time variations toward the SW image between 2012 May 22 and 2012 Jun. 15.
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	Fig. A.9 Composite ALMA B3 spectra (observed in 2012, in black) overlaid on top of the ATCA-3mm spectra obtained in July 2011 (in magenta) by Muller et al. (2013). The ALMA spectra has been recomposed using the spectra from both images (unresolved in the ATCA observations), assuming ℜ = F_NE/F_SW = 1.35, f_c(SW) = 92%, and f_c(NE) = 100%.
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	Fig. A.10 Comparison of the integrated opacities of the same lines between ATCA observations in July 2011 and ALMA observations in spring 2012.
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© ESO, 2014

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