‘Faint Main Belt’, showing only bodies with the absolute magnitude close to the limit of the Catalina Sky Survey, id est, H ≳ 19.25 + 5(log(2.2(l − 0.1)) + log(2.2 − 1))) − 5(log(a(l − e)) + log(a − 1))). The proper semimajor axis a_p versus eccentricity e_p (bottom) versus inclination sin i_p (top) are plotted; together with locations of the mean-motion resonances (vertical lines), IRAS dust bands (horizontal lines), and known asteroid families (Nesvorný et al. 2015) (labels). Big and old ones are almost invisible here (e.g. ‘4’ Vesta). Small and young ones − having a steep SFD − are prominent. The distribution of faint bodies is surprisingly irregular. The concentrations are directly related to the sources of meteorites: L .. ‘20’ Massalia (Marsset et al. 2024), H .. ‘158’ Koronis (Brož et al. 2024), CM .. ‘490’ Veritas, CI.. ‘142’ Polana, CO/CV/CK .. ‘221’ Eos, M .. ‘293’ Brasilia, or M .. ‘606’ Brangäne (this work).