Mid-infrared interferometric variability of DG Tauri: Implications for the inner-disk structure

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Table 1

Overview of VLTI/MIDI observations of DG Tau.

Target							Calibrator
Date and time	Telescopes	B	φ _B	Resolution	Seeing	Airmass	Name	Time
(UTC)		(m)	(°)	(au)	(′′)			(UTC)

2011-10-10 06:37	U1–U2	33	30	5.7	0.8	1.7	HD 27482	06:51
2011-10-10 07:43	U1–U3	76	45	2.5	0.8	1.6	HD 27482	07:29
2011-12-13 01:53	U1–U3	56	36	3.4	0.8^a	1.8	HD 27482	01:32
2011-12-13 02:59	U1–U2	37	34	5.1	0.7	1.6	HD 27482	02:38
							HD 27482	03:19
2012-02-04 01:02^b	U1–U2	45	40	4.2	1.5	1.6	HD 27482	00:42
							HD 27482	01:23
2012-02-05 00:46	U1–U2	44	39	4.3	1.1	1.6	HD 27482	00:29
							HD 27482	01:02
2012-02-06 00:39^c	U1-U3	83	46	2.3	0.9	1.6	HD 27482	00:22
2012-11-03 05:07	U1–U3	64	41	2.9	0.9	1.7	HD 27482	04:29
2014-01-14 02:39	U1–U3	88	45	2.1	0.8	1.7	HD 20644	01:17
							HD 25604	02:27
2014-01-15 01:47	U2–U4	89	83	2.1	1.5	1.6	HD 20644	00:42
							HD 25604	02:43
							HD 20644	02:03
2014-01-15 02:17	U2–U4	89	80	2.1	0.9	1.6	HD 20644	00:42
							HD 25604	02:43
							HD 20644	02:03
2014-01-15 02:22	U2–U4	89	80	2.1	0.7	1.6	HD 20644	00:42
							HD 25604	02:43
							HD 20644	02:03

Notes. B is the projected baseline length and φ_B is the projected position angle of the baseline (measured from North through East). The resolution is the approximate diameter of the beam at 10.7 μm, converted to physical scale. In the last two columns we list the name of the calibrators and the time of their measurement.

^(a)

The seeing for this epoch was missing from the observation data. We indicate here an interpolated value.

^(b)

According to the ESO observing log, this observation had to be repeated the following day because of its poor quality. Therefore we do not use these data in our work.

^(c)

The total flux observation was not of adequate quality so it was discarded.

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