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20573 simulations of planetary transits around spotted stars were conductedusing the transit-starspot model, \texttt{PRISM}. In total 3888 differentscenarios were considered using three different host star spectral types, M4V,M1V and K5V. The mean amplitude of the starspot anomaly was measured andcompared to the photometric precision of the light curve, to determine if thestarspot anomaly's characteristic "blip" was noticeable in the light curve. Thesimulations show that, starspot anomalies will be observable in TESS 2\,mincadence data. The smallest starspot detectable in TESS transit light curves hasa radius of $\approx1900$\,km. The starspot detection limits for the three hoststars are: $4900\pm1700$\,km (M4V), $13800\pm6000$\,km (M1V) and$15900\pm6800$\,km (K5V). The smallest change in flux of the starspot ($\DeltaF_\mathrm{spot} = 0.00015\pm0.00001$) can be detected when the ratio betweenthe planetary and stellar radii, $k = 0.082\pm0.004$. The results confirm knowndependencies between the amplitude of the starspot anomaly and the photometricparameters of the light curve. The results allowed the characterisation of therelationship between the change in flux of the starspot anomaly and the changein flux of the planetary transit for TESS transit light curves.

Simulations of starspot anomalies within TESS exoplanetary transit light curves -- I. The detection limits of starspot anomalies in TESS light curves