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Table 4.

Observing conditions of ADI sequences from the VLT/SPHERE-IRDIS instrument considered in this paper.

Target ESO ID Obs. date T λ (μm) Δpar (°) NDIT DIT (s) τ0 (ms) Seeing (″) Related paper
HR 4796A 095.C-0298 2015-02-03 110 1.59 48.5 8 32 11.8 0.67 Milli et al. (2017)
RY Lupi 097.C-0865 2016-04-16 80 1.59 71.0 4 64 61.4 0.36 Langlois et al. (2018)
SAO 206462 095.C-0298 2015-05-15 63 2.11 63.6 4 64 85.0 0.50 Maire et al. (2017)
PDS 70 100.C-0481 2018-02-24 90 2.11 95.7 3 96 71.5 0.46 Müller et al. (2018)
HIP 80019( * ) 095.C-0389 2015-04-21 116 2.11 42.8 11 8 23.2 0.80

Notes. Columns are: target name, ESO survey ID, observation date, number T of available temporal frames, spectral filter λ, total amount of field rotation Δpar of the field of view, number NDIT of sub-integration exposures, individual exposure time DIT, DIMM coherence time τ0, seeing value at the beginning of the observations and the first paper reporting analysis of the same data. All the observations are performed with the apodized Lyot coronagraph (APLC; Carbillet et al. 2011) of the VLT/SPHERE instrument. ( * )The ADI sequence of HIP 80019 was made of 176 temporal frames but we have discarded the 60 first frames manually. This sequence contains no detectable off-axis sources based on the application of PACO and REXPACO algorithms. If off-axis sources are present at an undetectable level of contrast, they would introduce a negligible bias in comparison to the levels of contrast considered in our experiments. This ADI sequence is used in Sect. 2 to perform injections of fake disks.

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