  The supernova remnant (SNR) Kes 75/PSR J1846-0258 association can be regarded
as certain due to the accurate location of young PSR J1846-0258 at the center
of Kes 75 and the detected bright radio/X-ray synchrotron nebula surrounding
the pulsar. We provide a new distance estimate to the SNR/pulsar system by
analyzing the HI and $^{13}$CO maps, the HI emission and absorption spectra,
and the $^{13}$CO emission spectrum of Kes 75. No absorption features at
negative velocities strongly argue against the widely-used large distance of 19
to 21 kpc for Kes 75, and show that Kes 75 is within the Solar circle, i.e. a
distance $d<$13.2 kpc. Kes 75 is likely at distance of 5.1 to 7.5 kpc because
the highest HI absorption velocity is at 95 km/s and no absorption is
associated with a nearby HI emission peak at 102 km/s in the direction of Kes
75. This distance to Kes 75 gives a reasonable luminosity of PSR J1846-0258 and
its PWN, and also leads to a much smaller radius for Kes 75. So the age of the
SNR is consistent with the spin-down age of PSR J1846-0258, confirming this
pulsar as the second-youngest in the Galaxy.
