23 images have been rejected due to poor guiding and defocus.

For the analysis of the observable transit egress, a collection of 118 images has been finally selected for light curve analysis and transit model calculation.
1 https://tess.mit.edu/followup 2 https://support.itelescope.net/support/solutions/articles/251589

[Figure: Fig. 1. PDCSAP from the TESS light curves for TOI-2147 (upper plot) and TOI-6019 (lower plot). The increased scatter for the TOI-2147 in later sectors is due to the shorter exposure times.]

2.2.3. MuSCAT2
2.3. High angular-resolution imaging To further rule out false-positive scenarios, we collected high angular-resolution imaging observations for both of our targets. We used these to search for unidentified close companions which could be the source of the transit signal, or dilute the transit depth, leading to an underestimated radius for the planet (Ciardi et al. 2015). We observed TOI-2147 on UT 2022 April 21 using the NN-EXPLORE Exoplanet Stellar Speckle Imager (NESSI; Scott et al. 2018), a speckle imaging instrument at the WIYN 3.5 m telescope on Kitt Peak. NESSI was operated with only one wavelength channel this night using a filter centered on λc = 832 nm with a width of 40 nm. The observation consisted of a sequence of 9000 × 40 ms exposures. NESSI’s field of view was set by a 256 × 256 pixel sub-array readout, resulting in 4.6′′ × 4.6′′ images. However, we confined the contrast curve measurements to within 1.2′′ from the target star to avoid the effects of decorrelation in speckle patterns at wider separations. A nearby point source calibration star was also observed immediately following the observation of the TOI for the purpose of estimating the PSF at the time of the science observation. These speckle data were reduced using a pipeline described by Howell et al. (2011). Among the pipeline products is a reconstructed image of the field around TOI-2147. The reconstructed image was used to measure a contrast curve, setting the detection limits on any nearby point sources. No companion stars were detected brighter than the contrast limit. Initially, the contrast
We observed an egress of TOI-6019.01 on September 23rd, 2023, in g′,r′,i′,zs with the MuSCAT2 (Narita et al. 2019) instrument mounted on the 1.52 m TCS telescope at the Teide Observatory in the Canary Islands, Spain. MuSCAT2 is capable of simultaneous imaging in four bands, each using a 1k × 1k CCD camera with a pixel scale of 0."44 pixel−1 and a field of view (FOV) of 7.′4 × 7.′4. To avoid contamination from the nearby star (TIC 125520908; ∆Tmag= 7; r = 8′′), we observed in focus and set the exposure times at (1, 2, 2, 2) s for g′,r′,i′,zs, respectively.
We used the MuSCAT2 pipeline3, described in Parviainen et al. (2020), to perform the data reduction and aperture photometry over a set of comparison stars and aperture sizes. The optimal light curves were determined through a global optimization of a model, consisting of five brightest comparison stars and uncontaminated aperture radii smaller than 5.6′′, while the transit and baseline variations are simultaneously modeled using a linear combination of covariates. As reported in TFOP-SG1, we detected an on-time (Rp/R∗)2 ∼3.5 ppt transit using an achromatic transit model.
3 https://github.com/hpparvi/MuSCAT2_transit_pipeline
Article number, page 3 of 14 limit increases rapidly with angular separation from TOI-2147, from ∆m = 0 at the diffraction limit of 0.06′′ to ∆m = 3.7 at 0.15′′.

The contrast increases more gradually past 0.15′′, reaching ∆m = 5 by 1′′.

TOI-6019 was observed on December 24, 2022, with the Speckle Polarimeter (SPP), a facility instrument on the 2.5-m telescope at the Caucasian Observatory of the Sternberg Astronomical Institute (SAI) of Lomonosov Moscow State University.