<table><caption>**Table C.1.** Times of mid-eclipse for HW Vir.</caption><thead><tr><th>E</th><th>BJD<sub>TDB</sub> - 2450000</th><th>O-C [s]</th><th>Source</th></tr></thead><tbody><tr><td>-3327</td><td>8870.840247 ± 0.000003</td><td>-0.73</td><td>SAINT-EX</td></tr><tr><td>-3326</td><td>8870.956983 ± 0.000010</td><td>+0.75</td><td>Szombathely</td></tr><tr><td>-3312</td><td>8872.591046 ± 0.000004</td><td>-0.07</td><td>Konkoly</td></tr><tr><td>-3303</td><td>8873.641542 ± 0.000005</td><td>+1.72</td><td>Konkoly</td></tr><tr><td>-3300</td><td>8873.991684 ± 0.000007</td><td>+0.26</td><td>Szombathely</td></tr><tr><td>-3294</td><td>8874.692014 ± 0.000034</td><td>+1.41</td><td>Konkoly</td></tr><tr><td>-3274</td><td>8877.026415 ± 0.000006</td><td>+2.37</td><td>Szombathely</td></tr><tr><td>-3249</td><td>8879.944358 ± 0.000005</td><td>-1.47</td><td>Szombathely</td></tr><tr><td>-3184</td><td>8887.531126 ± 0.000013</td><td>-1.28</td><td>SPECULOOS</td></tr><tr><td>-3184</td><td>8887.531138 ± 0.000009</td><td>-0.29</td><td>Konkoly</td></tr><tr><td>-3175</td><td>8888.581616 ± 0.000012</td><td>-0.06</td><td>SPECULOOS</td></tr><tr><td>-3175</td><td>8888.581617 ± 0.000007</td><td>+0.03</td><td>Konkoly</td></tr><tr><td>-3175</td><td>8888.581621 ± 0.000016</td><td>+0.40</td><td>SPECULOOS</td></tr><tr><td>-3164</td><td>8889.865522 ± 0.000009</td><td>-0.71</td><td>SAINT-EX</td></tr><tr><td>-3164</td><td>8889.865538 ± 0.000009</td><td>+0.67</td><td>Szombathely</td></tr><tr><td>-3073</td><td>8900.487001 ± 0.000015</td><td>-0.21</td><td>SPECULOOS</td></tr><tr><td>-3064</td><td>8901.537480 ± 0.000013</td><td>+0.07</td><td>SPECULOOS</td></tr><tr><td>-3004</td><td>8908.540642 ± 0.000004</td><td>-0.48</td><td>SPECULOOS</td></tr><tr><td>-2994</td><td>8909.707834 ± 0.000002</td><td>-0.71</td><td>SAINT-EX</td></tr><tr><td>-2962</td><td>8913.442867 ± 0.000012</td><td>+0.13</td><td>SPECULOOS</td></tr><tr><td>-2679</td><td>8946.474476 ± 0.000012</td><td>-0.29</td><td>SPECULOOS</td></tr><tr><td>-2679</td><td>8946.474493 ± 0.000012</td><td>+1.15</td><td>Szombathely</td></tr><tr><td>-2645</td><td>8950.442886 ± 0.000020</td><td>-4.88</td><td>SPECULOOS</td></tr><tr><td>-12</td><td>9257.765364 ± 0.000004</td><td>+0.88</td><td>SAINT-EX</td></tr><tr><td>-5</td><td>9258.582389 ± 0.000007</td><td>-0.18</td><td>SPECULOOS</td></tr><tr><td>-4</td><td>9258.699094 ± 0.000011</td><td>-1.35</td><td>SPECULOOS</td></tr><tr><td>4</td><td>9259.632884 ± 0.000007</td><td>+1.51</td><td>SPECULOOS</td></tr><tr><td>12</td><td>9260.566620 ± 0.000008</td><td>-0.19</td><td>SPECULOOS</td></tr><tr><td>21</td><td>9261.617083 ± 0.000021</td><td>-1.25</td><td>WHT</td></tr><tr><td>38</td><td>9263.601332 ± 0.000008</td><td>+0.29</td><td>Baja</td></tr><tr><td>83</td><td>9268.853714 ± 0.000003</td><td>+0.70</td><td>SAINT-EX</td></tr><tr><td>98</td><td>9270.604514 ± 0.000010</td><td>+1.37</td><td>SPECULOOS</td></tr><tr><td>106</td><td>9271.538264 ± 0.000013</td><td>+0.85</td><td>SPECULOOS</td></tr><tr><td>107</td><td>9271.654977 ± 0.000013</td><td>+0.27</td><td>SPECULOOS</td></tr><tr><td>132</td><td>9274.572938 ± 0.000010</td><td>-2.03</td><td>SPECULOOS</td></tr><tr><td>288</td><td>9292.781183 ± 0.000008</td><td>-1.64</td><td>SAINT-EX</td></tr><tr><td>425</td><td>9308.771773 ± 0.000005</td><td>+0.01</td><td>SAINT-EX</td></tr><tr><td>417</td><td>9307.838014 ± 0.000006</td><td>-0.23</td><td>SAINT-EX</td></tr><tr><td>3071</td><td>9617.611554 ± 0.000016</td><td>-0.89</td><td>Asiago</td></tr><tr><td>3225</td><td>9635.586426 ± 0.000076</td><td>+5.04</td><td>Asiago</td></tr><tr><td>3250</td><td>9638.504352 ± 0.000015</td><td>-0.27</td><td>Asiago</td></tr><tr><td>3327</td><td>9647.491752 ± 0.000010</td><td>-0.42</td><td>Asiago</td></tr><tr><td>3364</td><td>9651.810399 ± 0.000007</td><td>+1.80</td><td>Szombathely</td></tr><tr><td>3382</td><td>9653.911306 ± 0.000006</td><td>-2.00</td><td>Szombathely</td></tr><tr><td>3465</td><td>9663.599056 ± 0.000009</td><td>+0.68</td><td>SAINT-EX</td></tr><tr><td>3498</td><td>9667.450785 ± 0.000022</td><td>-0.60</td><td>Asiago</td></tr><tr><td>3517</td><td>9669.668467 ± 0.000004</td><td>+0.43</td><td>SAINT-EX</td></tr><tr><td>3737</td><td>9695.346783 ± 0.000002</td><td>+1.97</td><td>SAAO</td></tr></tbody></table>

**Notes.** Residuals from the quadratic ephemeris derived from ground-based observations of HW Vir are given in the column headed *O-C*.

predicted time of mid-eclipse from the quadratic ephemeris provided above, is 0.46 ± 0.14 seconds, with an RMS residual of 0.60 s. The agreement between CHEOPS data and the predicted times demonstrates that the timestamps provided with the light curve data fulfil the requirement for an accuracy of 1 second, as shown in Fig. C.1.

<figure><img src="image_41.png" /><figcaption>**Fig. C.1.** Residuals from the quadratic ephemeris for HW Vir determined from the ground-based data, shown with open circles (light blue). Times of mid-eclipse measured using CHEOPS data are shown using filled circles (dark blue).</figcaption></figure>

## Appendix D: Calculation of dark, hot, and RTS pixel frames

During a dark M&C observation, two sets of full-frame images are acquired: one set consists of ten ‘60 s frames’ with an exposure time of 60 seconds each, and the other set consists of ten ‘zero frames’ with an exposure time of 0.001 seconds each. The purpose of the first set is to capture thermal electrons in hot pixels, while the goal of the second set is to measure the gradient of the dark current during the read-out process. The pointing is intentionally shifted between exposures to prevent field stars from falling onto the same CCD spot.

The initial steps involve calibration and filtering processes. Calibration includes bias, gain, and non-linearity corrections based on standard procedures (as outlined in Hoyer et al. 2020). Filtering is applied to discard images with high background flux levels from further analysis. Afterwards, the dark frame is constructed through the following steps:

1. A single short frame is generated from the 10 zero-frames by taking their median.

2. The short frame is subtracted from each of the 60s frames.

3. The corrected 60s frames are normalised by the exposure time difference (59.999 seconds) in the next step.

4. The median of these normalised images is computed, resulting in the final dark frame.

5. The error of the frame is calculated as the standard error of the normalised image cube.

It is important to note that this dark frame includes not only the ‘true dark current’ of the electronics but also the zodiacal light due to the lack of a shutter. The zodiacal light and bulk thermal dark current must be removed to measure the dark current in the hot pixels. The first three steps of the process are the same as for the dark frame, but in the fourth step, a 2D median filter with a 3×3 pixel kernel is applied to the 60s frames. This step helps eliminate larger background variations caused by structures like stars and aligns the images to a consistent background level. The final step and error calculation remains the same. This resulting frame is used to identify hot pixels and measure their dark current levels. A pixel is categorised as a hot pixel if its flux exceeds 3 electrons per second.

The distribution of dark current levels in the hot pixels is depicted in Fig. D.1. This distribution spans over more than 1000
<table><caption>**Table C.2.** Times of mid-eclipse for HW Vir measured using CHEOPS.</caption><thead><tr><th>File key</th><th>T<sub>exp</sub> [s]</th><th>Cycle</th><th>T<sub>mid</sub> (BJD<sub>TDB</sub>)</th><th>O-C [s]</th></tr></thead><tbody><tr><td>CH_PR300006_TG000101_V0200</td><td>10.0</td><td>-3018</td><td>2458906.5564151 ± 0.0000013</td><td>-0.11</td></tr><tr><td>CH_PR300006_TG000102_V0200</td><td>10.0</td><td>-2995</td><td>2458909.2409654 ± 0.0000015</td><td>+0.08</td></tr><tr><td>CH_PR300006_TG000103_V0200</td><td>10.0</td><td>-2992</td><td>2458909.5911211 ± 0.0000026</td><td>-0.15</td></tr><tr><td>CH_PR300051_TG000301_V0200</td><td>30.0</td><td>-2911</td><td>2458919.0454007 ± 0.0000041</td><td>-0.02</td></tr><tr><td>CH_PR300058_TG000201_V0200</td><td>30.0</td><td>-2701</td><td>2458943.5564912 ± 0.0000015</td><td>-0.08</td></tr><tr><td>CH_PR300058_TG000101_V0200</td><td>30.0</td><td>-2687</td><td>2458945.1905725 ± 0.0000021</td><td>+0.66</td></tr><tr><td>CH_PR310080_TG000301_V0200</td><td>30.0</td><td>-11</td><td>2459257.5319233 ± 0.0000014</td><td>+0.79</td></tr><tr><td>CH_PR310080_TG000901_V0200</td><td>30.0</td><td>119</td><td>2459272.7054623 ± 0.0000030</td><td>+1.21</td></tr><tr><td>CH_PR310080_TG001401_V0200</td><td>30.0</td><td>345</td><td>2459299.0840663 ± 0.0000010</td><td>+1.07</td></tr><tr><td>CH_PR320089_TG001001_V0200</td><td>30.0</td><td>3397</td><td>2459655.3119826 ± 0.0000022</td><td>+1.18</td></tr><tr><td>CH_PR320089_TG001002_V0200</td><td>30.0</td><td>3404</td><td>2459656.1290317 ± 0.0000030</td><td>+2.26</td></tr><tr><td>CH_PR320089_TG001003_V0200</td><td>30.0</td><td>3508</td><td>2459668.2678384 ± 0.0000025</td><td>+0.36</td></tr><tr><td>CH_PR320089_TG001004_V0200</td><td>30.0</td><td>3551</td><td>2459673.2867777 ± 0.0000055</td><td>+0.40</td></tr><tr><td>CH_PR320089_TG001501_V0200</td><td>11.3</td><td>3682</td><td>2459688.5770259 ± 0.0000028</td><td>-0.22</td></tr><tr><td>CH_PR320089_TG001401_V0200</td><td>30.0</td><td>3698</td><td>2459690.4445438 ± 0.0000021</td><td>+0.28</td></tr><tr><td>CH_PR320089_TG001402_V0200</td><td>30.0</td><td>3708</td><td>2459691.6117403 ± 0.0000017</td><td>+0.40</td></tr><tr><td>CH_PR320089_TG001403_V0200</td><td>30.0</td><td>3712</td><td>2459692.0786155 ± 0.0000022</td><td>+0.16</td></tr><tr><td>CH_PR320089_TG001404_V0200</td><td>30.0</td><td>3722</td><td>2459693.2458109 ± 0.0000104</td><td>+0.18</td></tr><tr><td>CH_PR320089_TG001405_V0200</td><td>30.0</td><td>3727</td><td>2459693.8294090 ± 0.0000015</td><td>+0.23</td></tr></tbody></table>

**Notes.** Residuals from the quadratic ephemeris derived from ground-based observations of HW Vir are given in the column headed *O* − *C*.

<figure><img src="image_42.png" /><figcaption>**Fig. D.1.** Evolution of the distribution of the dark current in hot pixels. The colours indicate the time when the dark M&C were taken.</figcaption></figure>

days and is presented in 8 snapshots. Notably, the distribution's shape remains consistent over time, indicating that there are no significant distortions or variations. Hot pixels with higher dark current levels are less frequent. The distribution has no prominent value or peak, suggesting unexpectedly higher occurrences of hot pixels at specific dark current values.

Observations for the detection of RTS pixels are scheduled four times a year. Each visit involves observing a dark region of the sky for the duration of ten CHEOPS orbits. However, due to data volume limitations, only the window images corresponding to the active window location are downlinked to the ground. Within these ten orbits, approximately 1000 images are captured, each with a 60 s exposure time. It is worth noting that only 50–80% of these images can be utilised for RTS pixel detection, primarily due to factors such as Earth occultations and images affected by high background contamination, including instances

of elevated stray light and SAA crossings. Following the standard calibration process, a subset of images is further processed by calculating the median of each group of five consecutive frames. This step helps eliminate any remaining spatial contamination and cosmic ray effects in the images. Fig. D.2 shows the positions and variability of the RTS pixels at the end of the nominal mission in the active window.

## Appendix E: Noise due to hot pixels

To identify the most suitable window location, we employed aperture photometry on the hot pixel map across every feasible pixel coordinate on the CCD. This technique involves a 2D convolution of two signals, where the aperture serves as the kernel applied to the hot pixel map. This approach, termed convolutional photometry, employs the DRP DEFAULT
Variability of RTS pixels in the latest RTS observation (win)

<figure><img src="image_43.png" /><figcaption>**Fig. D.2.** Variability of RTS pixels in the active window frame. The bigger and redder the circle, the more variable the RTS pixel is. The magnitude of the oscillation is calculated for a 1-minute exposure.</figcaption></figure>

Maximum expected noise in a region of 3 pixels

<figure><img src="image_44.png" /><figcaption>**Fig. E.1.** Maximum expected noise in ppm per minute due to hot pixels using the flux of a *G* = 12 mag star as reference. The estimations comprise two distinct noise components: shot noise and jitter noise. Jitter noise is a consequence of telescope jitter, leading to the PSF's movement on the CCD. Consequently, the edge of the default aperture (*r* = 25 px) intersects hot pixels, inducing fluctuations in flux due to the hot pixels intermittently entering and exiting the aperture. The 'noise rings' seen in the image result from the convolution of the exact noise map with a circle of *r* = 3 px (all potential target locations for the intended one). That is, from all the noise values calculated in the exact map for the pixels within each circle, the maximum one is assigned to each pixel. Green circles indicate the regions of the CCD with the smallest and highest noise attributable to hot pixels.</figcaption></figure>

aperture (*r* = 25 px) to scan the entire CCD (except for a 25-pixel-wide strip at the CCD's edges). For the calculations, we utilised a reference observation from the beginning of the mission (CH_PR300061_TG000301) with a low number of hot pixels in the window frame. The target is a relatively quiet star (TYC 5502-1037-1, *G* = 12 mag) with minimal flux variations. This normalisation by the reference star's flux allows us to estimate the noise contribution from hot pixels. The outcome is a map illustrating the anticipated noise at every pixel on the CCD.

Shot noise is the square root of the total flux within the aperture, and a single application of convolutional photometry on the hot pixel map suffices to determine it. Jitter noise, however, is contingent upon pointing stability, which governs how the PSF (and consequently, the aperture) moves during an observation. The changing position of the aperture relative to the hot pixels leads to fluctuations in the number of hot pixels within the aperture and, consequently, in the aperture's flux. This results in noisy light curves. To calculate this noise, multiple aperture photometry measurements must be conducted for each jitter position at every pixel location on the CCD. Subsequently, the standard deviation of the relevant light curves (one for each pixel position on the CCD) is calculated. The positions of the aperture are determined using the centroid algorithm of the DRP. Finally, the shot and jitter noise maps are combined in quadrature to estimate the expected noise contribution.

In an ideal scenario, this 'exact' noise map would suffice if the PSF were precisely centred within the window frame and the aperture was perfectly aligned with the PSF's centre. However, practical considerations, such as the PSF's triangular shape and its slight offset from the window centre, the uncertainty between the intended star position in the CCD and the actual one, and the pointing jitter (which will follow a unique path per observation) render this map insufficient for pinpointing the optimal window location. To address this, a circle with a radius of three pixels is defined, encompassing (with margin) all potential PSF real positions. A subsequent noise map is generated to display the

mean, minimum, or maximum anticipated noise within this circumscribed region. Fig. E.1 shows the maximum expected noise map of the CCD at the end of the nominal mission for the reference star (*G* = 12 mag). We note that the location of the active window (coordinates of its bottom left corner: (193, 731)) places the PSF in a low noise region.

*Noise evolution in the window frame.* We also monitored the expected noise due to bad pixels at the precise PSF location of the target. This approach involves creating a simulated observation that includes all the hot pixels within the window frame. We initiated this process using our reference observation as a baseline (target: TYC 5502-1037-1, visit ID: CH_PR300061_TG000301) and selected a subset of images with a duration of 300 frames. This choice strikes a balance between reasonable processing time, the high CPU demands, and the lengthy processing times of the DRP routines we employ for re-processing the data.

To simulate the presence of hot pixels, we generated an image that exclusively contains hot pixels. This was accomplished by extracting the relevant window frame from the comprehensive hot pixel map and aligning it with the current window's location. Subsequently, we introduced Poisson noise to emulate the behaviour of hot pixels. The dark current of these simulated hot pixels was calibrated based on the exposure time of the reference observation. This sequence results in the creation of an image cube with only hot pixels, maintaining dimensions consistent with those of the reference observation.
<figure><img src="image_45.png" /><figcaption>**Fig. E.2.** Progression of noise since the beginning of nominal operations, calculated through the PyCHEOPS package according to the minimum error algorithm (Maxted et al. 2022a). The figure shows the estimated noise of a 3 h bin by using a simulated dataset wherein hot pixels were injected into the reference visit and subsequently processed by the DRP with dark correction module OFF.</figcaption></figure>

Following the image generation process, we conducted a basic arithmetic addition between the newly created image cube and the reference observation image cube. This merged image cube was then subjected to the DRP pipeline for processing and was subsequently analysed using the PyCHEOPS package. We note that the dark correction feature was either disabled or unavailable in earlier versions of the DRP. This was done deliberately to assess the direct effect of hot pixels. We utilised the minimum error algorithm as implemented in PyCHEOPS (Maxted et al. 2022a) to estimate the noise of the light curve within a 3-hour bin. The outcomes of these analyses are presented as a plot, illustrating the noise evolution over time since the satellite's launch, as shown in Fig. E.2.

## Appendix F: Glossary

Table F.1 contains the symbols and acronyms used in this paper.

## Appendix G: List of CHEOPS visits used to perform the analyses in this paper

Table G.1 provides a comprehensive list of the CHEOPS visits employed to generate the results presented in this paper.
<table><caption>**Table F.1.** Symbols and acronyms.</caption><thead><tr><th>Acronym</th><th>Definition</th><th>Acronym</th><th>Definition</th></tr></thead><tbody><tr><td>ACF</td><td>Autocorrelation Function</td><td>ppm</td><td>parts-per-million</td></tr><tr><td>ADU</td><td>Analogue-to-Digital Units</td><td>PSF</td><td>Point Spread Function</td></tr><tr><td>AOCS</td><td>Attitude and Orbital Control System</td><td>PST</td><td>Point Source Transmission function</td></tr><tr><td>CCD</td><td>Charged-Coupled Device</td><td>px</td><td>pixel</td></tr><tr><td>CHEOPS</td><td>Characterising ExOPlanet Satellite</td><td>QE</td><td>Quantum Efficiency</td></tr><tr><td>CTI</td><td>Charge Transfer Inefficiency</td><td>r</td><td>Radius</td></tr><tr><td>DRP</td><td>Data Reduction Pipeline</td><td>R<sub>star</sub></td><td>Radius of the star</td></tr><tr><td>DRT</td><td>Data Reduction Tool</td><td>RMS</td><td>Root Mean Square</td></tr><tr><td>ESA</td><td>European Space Agency</td><td>RTS</td><td>Random Telegraphic Signal</td></tr><tr><td>ETC</td><td>Exposure Time Calculator</td><td>SAA</td><td>South Atlantic Anomaly</td></tr><tr><td>FEE</td><td>Front End Electronics</td><td>SC</td><td>Spacecraft</td></tr><tr><td>FoV</td><td>Field of View</td><td>SciReq.</td><td>Science Requirement</td></tr><tr><td>G</td><td>Gaia G magnitude</td><td>SEM</td><td>Sensor Electronic Module</td></tr><tr><td>HK</td><td>Housekeeping</td><td>SOC</td><td>Science Operation Centre</td></tr><tr><td>IFSW</td><td>In-Flight software</td><td>T<sub>eff</sub></td><td>Stellar Effective Temperature</td></tr><tr><td>IOC</td><td>In-Orbit Commissioning</td><td>t<sub>exp</sub></td><td>Exposure time</td></tr><tr><td>LEO</td><td>Low-Earth Orbit</td><td>UTC</td><td>Universal Time Coordinated</td></tr><tr><td>LoS</td><td>Line of Sight</td><td>V</td><td>Visual magnitude</td></tr><tr><td>LTAN</td><td>Local Time of the Ascending Node</td><td>VOD</td><td>Output transistor Drain Voltage</td></tr><tr><td>M&C</td><td>Monitoring and Characterisation Programme</td><td>VOG</td><td>Output Gate Voltage</td></tr><tr><td>MOC</td><td>Mission Operation Centre</td><td>VRD</td><td>Reset transistor Drain Voltage</td></tr><tr><td>NOPITL</td><td>NO Payload In The Loop</td><td>VSS</td><td>Substrate Voltage</td></tr><tr><td>OBT</td><td>Onboard Time</td><td></td><td></td></tr><tr><td>OTA</td><td>Optical Telescope Assembly</td><td></td><td></td></tr><tr><td>PCA</td><td>Principal Component Analysis</td><td></td><td></td></tr><tr><td>PF</td><td>Platform</td><td></td><td></td></tr><tr><td>PID</td><td>Proportional Integral Derivative</td><td></td><td></td></tr><tr><td>PITL</td><td>Payload In The Loop</td><td></td><td></td></tr><tr><td>PIPE</td><td>PSF Imagette Photometric Extraction</td><td></td><td></td></tr></tbody></table>
<table><caption>**Table G.1.** Visits used for the analyses presented in this paper.</caption><thead><tr><th>Section</th><th>File key</th><th>Date</th><th>Target</th><th>Gmag</th></tr></thead><tbody><tr><td>Sect. 2.4.2</td><td>CH_PR330096_TG0007</td><td>02/03/2023</td><td>HD 88742</td><td>6.38</td></tr><tr><td>Sect. 3.2.3</td><td>CH_PR100041_TG000201</td><td>19/03/2020</td><td>WASP-189</td><td>6.55</td></tr><tr><td>Sect. 4.4.1</td><td>CH_PR100018_TG040003</td><td>20/09/2022</td><td>GJ 908</td><td>8.15</td></tr><tr><td>Sect. 5.1 and 5.2</td><td>CH_PR300005_TG000101</td><td>22/02/2020</td><td>HD 88111</td><td>8.97</td></tr><tr><td>Sect. 5.1 and 5.2</td><td>CH_PR300005_TG000501</td><td>21/03/2020</td><td>TYC 5502-1037-1</td><td>11.98</td></tr><tr><td>Sect. 5.1</td><td>CH_PR100011_TG023501</td><td>20/04/2020</td><td>GJ 536</td><td>8.86</td></tr><tr><td>Sect. 5.1</td><td>CH_PR100011_TG023701</td><td>24/04/2020</td><td>GJ 581</td><td>9.41</td></tr><tr><td>Sect. 5.1</td><td>CH_PR100011_TG023001</td><td>03/05/2020</td><td>61 Vir</td><td>4.48</td></tr><tr><td>Sect. 5.1</td><td>CH_PR100011_TG023301</td><td>12/05/2020</td><td>GJ 3779</td><td>11.63</td></tr><tr><td>Sect. 5.1</td><td>CH_PR100011_TG023901</td><td>13/05/2020</td><td>GJ 628</td><td>8.79</td></tr><tr><td>Sect. 5.1</td><td>CH_PR100011_TG024101</td><td>08/05/2020</td><td>HD 125612</td><td>8.16</td></tr><tr><td>Sect. 5.1</td><td>CH_PR100011_TG035801</td><td>24/06/2020</td><td>HD 125612</td><td>8.16</td></tr><tr><td>Sect. 5.1</td><td>CH_PR100011_TG024701</td><td>22/05/2020</td><td>HD 181433</td><td>8.09</td></tr><tr><td>Sect. 5.1</td><td>CH_PR100011_TG024702</td><td>01/06/2020</td><td>HD 181433</td><td>8.09</td></tr><tr><td>Sect. 5.1</td><td>CH_PR100011_TG036001</td><td>26/07/2020</td><td>HD 175986</td><td>8.14</td></tr><tr><td>Sect. 5.1</td><td>CH_PR100011_TG036201</td><td>17/07/2020</td><td>HD 190360</td><td>5.33</td></tr><tr><td>Sect. 5.1</td><td>CH_PR100011_TG035901</td><td>13/09/2020</td><td>HD 215152</td><td>7.8</td></tr><tr><td>Sect. 5.2</td><td>CH_PR310080_TG000101</td><td>03/01/2021</td><td>HD 88111</td><td>8.97</td></tr><tr><td>Sect. 5.2</td><td>CH_PR320089_TG000101</td><td>15/02/2022</td><td>HD 88111</td><td>8.97</td></tr><tr><td>Sect. 5.2</td><td>CH_PR330096_TG000101</td><td>15/03/2023</td><td>HD 88111</td><td>8.97</td></tr><tr><td>Sect. 5.2</td><td>CH_PR310080_TG000201</td><td>26/02/2021</td><td>TYC 5502-1037-1</td><td>11.98</td></tr><tr><td>Sect. 5.2</td><td>CH_PR320089_TG000301</td><td>28/02/2022</td><td>TYC 5502-1037-1</td><td>11.98</td></tr><tr><td>Sect. 5.2</td><td>CH_PR330096_TG000301</td><td>31/03/2023</td><td>TYC 5502-1037-1</td><td>11.98</td></tr><tr><td>Sect. 5.2</td><td>CH_PR100016_TG010201</td><td>02/11/2020</td><td>WASP-12</td><td>11.6</td></tr><tr><td>Sect. 5.2</td><td>CH_PR100016_TG010202</td><td>09/11/2020</td><td>WASP-12</td><td>11.6</td></tr><tr><td>Sect. 5.2</td><td>CH_PR100016_TG010203</td><td>10/11/2020</td><td>WASP-12</td><td>11.6</td></tr><tr><td>Sect. 5.2</td><td>CH_PR100016_TG010204</td><td>12/11/2020</td><td>WASP-12</td><td>11.6</td></tr><tr><td>Sect. 5.2</td><td>CH_PR100016_TG010205</td><td>20/11/2020</td><td>WASP-12</td><td>11.6</td></tr><tr><td>Sect. 5.2</td><td>CH_PR100016_TG010206</td><td>21/11/2020</td><td>WASP-12</td><td>11.6</td></tr><tr><td>Sect. 5.2</td><td>CH_PR100016_TG010207</td><td>29/11/2020</td><td>WASP-12</td><td>11.6</td></tr><tr><td>Sect. 5.2</td><td>CH_PR100016_TG010208</td><td>30/11/2020</td><td>WASP-12</td><td>11.6</td></tr><tr><td>Sect. 5.2</td><td>CH_PR100016_TG010209</td><td>04/12/2020</td><td>WASP-12</td><td>11.6</td></tr><tr><td>Sect. 5.2</td><td>CH_PR100016_TG010210</td><td>05/12/2020</td><td>WASP-12</td><td>11.6</td></tr><tr><td>Sect. 5.2</td><td>CH_PR100016_TG010211</td><td>06/12/2020</td><td>WASP-12</td><td>11.6</td></tr><tr><td>Sect. 5.2</td><td>CH_PR100016_TG010212</td><td>09/12/2020</td><td>WASP-12</td><td>11.6</td></tr><tr><td>Sect. 5.2</td><td>CH_PR100013_TG001201</td><td>12/01/2021</td><td>WASP-12</td><td>11.6</td></tr><tr><td>Sect. 5.2</td><td>CH_PR100013_TG001701</td><td>01/11/2021</td><td>WASP-12</td><td>11.6</td></tr><tr><td>Sect. 5.2</td><td>CH_PR100013_TG001702</td><td>10/11/2021</td><td>WASP-12</td><td>11.6</td></tr><tr><td>Sect. 5.2</td><td>CH_PR100013_TG001703</td><td>11/11/2021</td><td>WASP-12</td><td>11.6</td></tr><tr><td>Sect. 5.2</td><td>CH_PR100016_TG015001</td><td>05/12/2021</td><td>WASP-12</td><td>11.6</td></tr><tr><td>Sect. 5.2</td><td>CH_PR100013_TG001704</td><td>05/12/2021</td><td>WASP-12</td><td>11.6</td></tr><tr><td>Sect. 5.2</td><td>CH_PR100013_TG001705</td><td>07/12/2021</td><td>WASP-12</td><td>11.6</td></tr><tr><td>Sect. 5.2</td><td>CH_PR100016_TG015002</td><td>07/12/2021</td><td>WASP-12</td><td>11.6</td></tr><tr><td>Sect. 5.2</td><td>CH_PR100013_TG001706</td><td>15/12/2021</td><td>WASP-12</td><td>11.6</td></tr><tr><td>Sect. 5.2</td><td>CH_PR100016_TG015003</td><td>16/12/2021</td><td>WASP-12</td><td>11.6</td></tr><tr><td>Sect. 5.2</td><td>CH_PR100013_TG001707</td><td>16/12/2021</td><td>WASP-12</td><td>11.6</td></tr><tr><td>Sect. 5.2</td><td>CH_PR100016_TG015004</td><td>17/12/2021</td><td>WASP-12</td><td>11.6</td></tr><tr><td>Sect. 5.2</td><td>CH_PR100016_TG015005</td><td>24/12/2021</td><td>WASP-12</td><td>11.6</td></tr><tr><td>Sect. 5.2</td><td>CH_PR100013_TG001708</td><td>26/12/2021</td><td>WASP-12</td><td>11.6</td></tr><tr><td>Sect. 5.2</td><td>CH_PR100013_TG001709</td><td>29/12/2021</td><td>WASP-12</td><td>11.6</td></tr><tr><td>Sect. 5.2</td><td>CH_PR100016_TG015006</td><td>30/12/2021</td><td>WASP-12</td><td>11.6</td></tr><tr><td>Sect. 5.2</td><td>CH_PR100013_TG001710</td><td>30/12/2021</td><td>WASP-12</td><td>11.6</td></tr><tr><td>Sect. 5.2</td><td>CH_PR100016_TG015007</td><td>31/12/2021</td><td>WASP-12</td><td>11.6</td></tr><tr><td>Sect. 5.2</td><td>CH_PR100013_TG001711</td><td>04/01/2022</td><td>WASP-12</td><td>11.6</td></tr><tr><td>Sect. 5.2</td><td>CH_PR100013_TG001712</td><td>06/01/2022</td><td>WASP-12</td><td>11.6</td></tr><tr><td>Sect. 5.2</td><td>CH_PR100016_TG015008</td><td>07/01/2022</td><td>WASP-12</td><td>11.6</td></tr><tr><td>Sect. 5.2</td><td>CH_PR100013_TG001713</td><td>09/01/2022</td><td>WASP-12</td><td>11.6</td></tr><tr><td>Sect. 5.2</td><td>CH_PR100013_TG001714</td><td>19/01/2022</td><td>WASP-12</td><td>11.6</td></tr><tr><td>Sect. 5.2</td><td>CH_PR100013_TG001715</td><td>26/01/2022</td><td>WASP-12</td><td>11.6</td></tr><tr><td>Sect. 5.2</td><td>CH_PR100013_TG001716</td><td>29/01/2022</td><td>WASP-12</td><td>11.6</td></tr></tbody></table>
<table><caption>**Table G.1.** continued.</caption><thead><tr><th>Section</th><th>File key</th><th>Date</th><th>Target</th><th>Gmag</th></tr></thead><tbody><tr><td>Sect. 5.2</td><td>CH_PR100013_TG001717</td><td>03/02/2022</td><td>WASP-12</td><td>11.6</td></tr><tr><td>Sect. 5.2</td><td>CH_PR100013_TG001718</td><td>04/02/2022</td><td>WASP-12</td><td>11.6</td></tr><tr><td>Sect. 5.2</td><td>CH_PR100013_TG001719</td><td>08/02/2022</td><td>WASP-12</td><td>11.6</td></tr><tr><td>Sect. 5.2</td><td>CH_PR100013_TG001720</td><td>18/02/2022</td><td>WASP-12</td><td>11.6</td></tr><tr><td>Sect. 5.2</td><td>CH_PR100016_TG015601</td><td>23/02/2022</td><td>WASP-12</td><td>11.6</td></tr><tr><td>Sect. 5.2</td><td>CH_PR100016_TG015602</td><td>24/02/2022</td><td>WASP-12</td><td>11.6</td></tr><tr><td>Sect. 5.2</td><td>CH_PR100016_TG015603</td><td>22/11/2022</td><td>WASP-12</td><td>11.6</td></tr><tr><td>Sect. 5.2</td><td>CH_PR100016_TG015604</td><td>23/11/2022</td><td>WASP-12</td><td>11.6</td></tr><tr><td>Sect. 5.2</td><td>CH_PR330093_TG000201</td><td>21/12/2022</td><td>WASP-12</td><td>11.6</td></tr><tr><td>Sect. 5.2</td><td>CH_PR100016_TG015605</td><td>24/12/2022</td><td>WASP-12</td><td>11.6</td></tr><tr><td>Sects. 5.3.1 and 5.4.1</td><td>CH_PR100041_TG000601</td><td>23/03/2020</td><td>55 Cnc</td><td>5.71</td></tr><tr><td>Sect. 5.3.1</td><td>CH_PR300059_TG001201</td><td>06/04/2020</td><td>TYC2502-71-1</td><td>11.185</td></tr><tr><td>Sect. 5.5</td><td>CH_PR300005_TG000201</td><td>27/02/2020</td><td>TYC 5502-1037-1</td><td>11.98</td></tr><tr><td>Sect. 6.2</td><td>CH_PR100015_TG009101</td><td>22/05/2020</td><td>WASP-38</td><td>9.21</td></tr><tr><td>Appendix E</td><td>CH_PR300061_TG000301</td><td>11/04/2020</td><td>TYC 5502-1037-1</td><td>11.98</td></tr></tbody></table>