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Table 1

Observing log, excesses, and variability.

HD Night fCSE [%] ΔCSE
2262 2012-10-151 0.67 ± 0.17 ± 0.06 0.91
2013-08-10 0.40 ± 0.15 ± 0.06 –0.45
2014-10-11 0.42 ± 0.15 ± 0.06 –0.34
7788 2012-07-231 1.43 ± 0.16 ± 0.05 3.0
2013-08-10 0.07 ± 0.15 ± 0.05 –4.12
2014-10-11 1.16 ± 0.17 ± 0.05 1.55
20794 2012-12-161 1.64 ± 0.26 ± 0.26 1.59
2013-08-10 0.75 ± 0.20 ± 0.24 –0.65
2014-10-12 0.77 ± 0.24 ± 0.18 –0.60
28355 2012-12-151 0.88 ± 0.08 ± 0.05 1.0
2014-10-11 0.52 ± 0.12 ± 0.05 –1.63
39060 2010-12-042 1.48 ± 0.20 ± 0.05 0.45
(β Pic) 2010-12-202
2011-11-02 1.32 ± 0.15 ± 0.05 –0.32
2012-10-161 0.88 ± 0.22 ± 0.05 –2.05
2013-08-10 1.81 ± 0.38 ± 0.05 1.11
2014-10-11 1.47 ± 0.11 ± 0.05 0.64
172555 2012-07-241 0.55 ± 0.25 ± 0.05 –0.59
2013-04-18 0.93 ± 0.59 ± 0.05 0.34
2014-10-12 0.80 ± 0.18 ± 0.05 0.32
210302 2012-07-241 0.83 ± 0.24 ± 0.05 2.77
2013-08-10 −0.16 ± 0.13 ± 0.05 –1.48
2014-10-11 0.11 ± 0.14 ± 0.05 0.11

Notes. fCSE is the flux ratio between the circumstellar emission and the star. ΔCSE is the significance of the deviation of this value from the error weighted mean of all considered measurements of this target (Eq. (1)). Uncertainties on the flux ratios are separated in statistical errors (first value) and systematic errors (see Sect. 4 for details). The two values should be added in quadrature to obtain the total uncertainties used in this work.

(1)

Survey detection (Ertel et al. 2014).

(2)

Data obtained on 2010-12-04 and on 2010-12-20 are combined to one measurement in order to improve the accuracy since no variability is seen between the two observations.

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