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The surface brightness fluctuation (SBF) technique is one of the distancemeasurement methods that has been applied on the low surface brightness galaxyNGC 1052-DF2 yielding a distance of about 20 Mpc implying it to be a darkmatter deficient galaxy. We assume the number of giant stars above a givenluminosity threshold to represent the SBF magnitude. The SBF magnitude dependson the distance, but this is degenerate with the star formation history (SFH).Using a stellar population synthesis model we calculate the number of giantstars for stellar populations with different galaxy-wide stellar initial massfunctions (gwIMFs), ages, metallicities and SFHs. If the gwIMF is the invariantcanonical IMF, the 1$\sigma$ (3$\sigma$) uncertainty in colour allows adistance as low as 12 Mpc (8 Mpc). If instead the true underlying gwIMF is theintegrated galaxy-wide IMF (IGIMF) then overestimating distances for low-massgalaxies would be a natural result, allowing NGC 1052-DF2 to have a distance of11 Mpc within the 1$\sigma$ colour uncertainty. Finally, we show that our mainconclusion on the existence of a bias in the SBF distance estimation is notmuch affected by changing the luminosity lower limit for counting giant stars.

monthly notices of the royal astronomical society

IMF-induced intrinsic uncertainties on measuring galaxy distances based  on the number of giant stars: the case of the ultra-diffuse galaxy NGC  1052-DF2