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We make an in-depth comparison of the IllustrisTNG simulations withobservational data on the quenched fractions of central and satellite galaxies,for $M_*=10^{9-12}M_{\odot}$ at $0\leq z\leq3$. We study how analysismethodologies and observational effects impact this comparison. This includesmeasurement choices -- aperture, quenched definition, star formation rate (SFR)indicator timescale -- as well as observational uncertainties and sampleselection issues: projection effects, satellite/central misclassification, andhost mass distribution sampling. The definition used to separate quenched andstar-forming galaxies produces differences of up to 70 (30)$\%$ for centrals(satellites) $>\sim 10^{10.5} M_{\odot}$. Increasing the aperture within whichSFR is measured can suppress the quenched fractions by up to $\sim50\%$,particularly at $z\gtrsim2$. Proper consideration of the stellar and host massdistributions is crucial: naive comparisons to volume-limited samples fromsimulations lead to misinterpretation of the quenched fractions as a functionof $z$ by up to 20$\%$. Including observational uncertainties to theoreticalvalues of $M_*$ and SFR changes the quenched fraction values and their trendand/or slope with mass. Taking projected rather than 3D distances forsatellites decreases the quenched fractions by up to 10$\%$ due to fieldcontamination. Comparing with data, TNG produces quenched fractions broadlyconsistent with observations. TNG predicts quenched fractions up to$\sim80-90\%$ for centrals at $z\leq2-3$, in line with recent observations, andnotably higher than other theoretical models. The quantitative agreement of TNGand SDSS for satellite quenched fractions in groups and clusters dependsstrongly on the galaxy and host mass range. Our mock comparison between TNG andSDSS highlights the importance of properly accounting for observational effectsand biases.

Quenched fractions in the IllustrisTNG simulations: comparison with observations and other theoretical models