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Appendix A: Table and plots of all uv points

Table A.1 lists all measurements of the Circinus galaxy obtained with MIDI, that is all uv points. The columns are: (1) a running number of the measurement; (2) the date and time at the start of the fringe track, i.e. the interferometric observation; (3) modified Julian date, MJD; (4) telescope combination used for the observation; (5) projected baseline length; (6) position angle of the projected baseline; (7) adaptive optics system used, either STRAP or MACAO (“_T” indicates additional usage of the technical CCD); (8) usage of IRIS with: “n/a” – IRIS not available, “off” – IRIS not used for field stabilisation, “on” – IRIS used for field stabilisation, a number – IRIS used with the integration time specified in seconds (before 2011 no IRIS integration times were stored with the data); (9) mode of the interferometric observations with: “0OPD” – tracking with a scan length of 84.2 μm at zero OPD, “OFF” – tracking with a scan length of 84.2 μm at an offset of 40 μm, “SHRT” – tracking with a reduced scan length of 53.0 μm at an offset of 40 μm; (10) detector integration time of MIDI; (11) chopping frequency for the observations of the total flux spectra with the single dishes; (12) airmass; (13) seeing; (14) coherence time; (15) name of the calibrator star; (16) time of the calibrator observation; (17) correlated flux and its error at 12 μm, if the observation was successful and is used for the further analysis. Measurements were considered successful if a fringe signal was tracked and sufficient signal was detected (mostly equivalent to more than 1500 good frames used for the averaging). No entry in the chop frequency column indicates that no photometry was observed.

All dispersed correlated fluxes are shown in Fig. A.1, the differential phases are plotted in Fig. A.2. The data is plotted in blue, the correlated fluxes and differential phases of the model from fit 3 are plotted in red. As in Table A.1, the measurements are ordered by observing date and time. The numbering is also the same as in Table A.1, however unsuccessful measurements are not plotted.

	Fig. A.1 Correlated fluxes of all uv points (blue). The correlated fluxes of our three-component model (fit 3) are plotted in red.
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	Fig. A.1 continued.
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	Fig. A.1 continued.
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	Fig. A.2 Differential phases of all uv points (blue). The differential phases of our model (fit 3) are plotted in red.
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	Fig. A.2 continued.
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	Fig. A.2 continued.
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© ESO, 2014