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Table 1

Log of photometric observations.

Data ID Start date (UTC) Duration (h) Frames Nexp × Texp (s) Efficiency(a) (%) Planet(s) in transit
CHEOPS CH_PR100041_TG000901_V0200 2020-04-04T15:07 11.58 558 26 × 1.7(b) 59.2 b
CHEOPS CH_PR100041_TG000101_V0200 2020-04-14T16:23 10.99 567 26 × 1.7 63.3 c
CHEOPS CH_PR100041_TG000902_V0200 2020-04-16T03:59 11.62 580 26 × 1.7 61.2 b
CHEOPS CH_PR100041_TG001101_V0200 2020-04-27T18:00 12.84 661 26 × 1.7 63.2 b
CHEOPS CH_PR100041_TG001001_V0200 2020-06-08T21:33 11.65 551 26 × 1.7 58.1 c,d
CHEOPS CH_PR100041_TG001501_V0200 2020-07-06T10:40 11.56 496 26 × 1.7 52.7 b, c
CHEOPS CH_PR100031_TG039201_V0200 2021-04-24T22:11 92.11 4 720 26 × 1.7 62.9 d
TESS S12-0000000136916387-0144-s 2019-05-21T11:00 672 20 119 1 × 120 99.8 2×b, 1×c
TESS S38-0000000136916387-0209-a_fast 2021-04-29T08:35 648 18482(c) 1 × 20 95.1 2 × b, 1 × c

Notes. The spectroscopic observations with HARPS at ESO 3.6m are those from Udry et al. (2019). TESS sector 12 data and CHEOPS 2020 data have previously been reported by Kane et al. (2020) and Delrez et al. (2021), respectively. (a) The efficiency quantifies the interruption of CHEOPS observations due to Earth occultations and passages through the South Atlantic Anomaly. It is calculated as Nexp × Texp × frames/duration. (b) Each CHEOPS subarray image results from the on-board co-addition of 26 exposures of 1.7 s. (c) After binning the 20 s exposures to the 2 min cadence.

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