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The population of satellite galaxies in a host galaxy is a combination of thecumulative accretion of subhaloes and their associated star formationefficiencies, therefore, the luminosity distribution of satellites providesvaluable information of both dark matter properties and star formation physics.Recently, the luminosity function of satellites in nearby Milky Way-massgalaxies has been well measured to satellites as faint as Leo I with $M_{V}\sim -8$. In addition to the finding of the diversity in the satelliteluminosity functions, it has been noticed that there is a big gap among themagnitude of satellites in some host galaxies, such as M101, where the gap isaround 5 in magnitude, noticeably larger than the prediction from the haloabundance matching method. The reason of this gap is still unknown. In thispaper, we use a semi-analytical model of galaxy formation, combined withhigh-resolution N-body simulation, to investigate the probability and origin ofsuch big gap in M101-alike galaxies. We found that, although M101 analogues arevery rare with probability of \sim 0.1%-0.2% in the local universe, theirformation is a natural outcome of the CDM model. The gap in magnitude is mainlydue to the mass of the accreted subhaloes, not from the stochastic starformation in them. We also found that the gap is correlated with the totalsatellite mass and host halo mass. By tracing the formation history of M101type galaxies, we find that they likely formed after $z \sim 1$ due to thenewly accreted bright satellites. The gap is not in a stable state, and it willdisappear in ~7 Gyr due to mergers of bright satellites with the centralgalaxy.

The Formation of M101-alike Galaxies in the Cold Dark Matter Model