The supernova remnant ( SNR ) Kes 75/PSR J1846-0258 association can be regarded as a certainty 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 .
That there are no absorption features at negative velocities strongly argues against the widely-used large distance of 19 to 21 kpc for Kes 75 , and shows that Kes 75 is within the Solar circle , i.e .
a distance d < 13.2 kpc .
Kes 75 is likely at a 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 .