  The present work aims to determine the source regions of carbonaceous
chondrites (CM, CI, CO, CV, CK, CR, CH, CB, or C-ungrouped). We studied 38
individual asteroid families, including young and old ones, and determined
their contributions to the NEO populations at metre and kilometre sizes using
collisional and orbital models. Our models are in agreement with spectroscopic
observations of NEOs, cosmic-ray exposure ages of meteorites, statistics of
bolides, infrared emission from dust bands, composition of interplanetary dust
particles (IDPs), or abundance of extraterrestrial helium-3. We identified the
Veritas, Polana and Eos families as the primary sources of CM/CR, CI and
CO/CV/CK chondrites, respectively. Substantial contributions are also expected
from CM-like K\"onig and CI-like Clarissa, Misa and Hoffmeister families. The
source regions of kilometre-sized bodies are generally different. The Adeona
family is by far the main source of CM-like NEOs, whereas the Polana (low-i)
and Euphrosyne (high-i) families are at the origin of most CI-like NEOs. The
Polana family is the likely source of both Ryugu and Bennu. We were able to
link spectroscopically and dynamically several NEOs to the Baptistina family.
Finally, it appears that the pre-atmospheric flux of carbonaceous chondrites at
metre sizes is about the same as that of ordinary chondrites. Given the
difference in fall statistics between the two groups (80\% versus 4.4\%), this
implies either substantial atmospheric fragmentation of carbonaceous bodies at
the level of ${\sim}0.5\,{\rm MPa}$, or destruction by thermal cracking and
water desorption. The source regions of most meteorites and kilometre-sized
NEOs have now been determined; including some minor classes like enstatite
chondrites and achondrites (Nysa, Hungaria), acapulcoites/lodranites (Iannini).
