Isochrone Fitting of Galactic Globular Clusters -- VI. High-latitude Clusters NGC5024 (M53), NGC5053, NGC5272 (M3), NGC5466, and NGC7099 (M30)

We fit various colour-magnitude diagrams (CMDs) of the high-latitude Galactic globular clusters NGC\, 5024 (M53), NGC\, 5053, NGC\, 5272 (M3), NGC\, 5466, and NGC\, 7099 (M30) by isochrones from the Dartmouth Stellar Evolution Database and Bag of Stellar Tracks and Isochrones for -enrichment /Fe=+0. 4. For the CMDs, we use data sets from Hubble Space Telescope, Gaia, and other sources utilizing, at least, 25 photometric filters for each cluster. We obtain the following characteristics with their statistic uncertainties for NGC\, 5024, NGC\, 5053, NGC\, 5272, NGC\, 5466, and NGC\, 7099, respectively: metallicities Fe/H=-1. 930. 02, -2. 080. 03, -1. 600. 02, -1. 950. 02, and -2. 070. 04 dex with their systematic uncertainty 0. 1 dex; ages 13. 000. 11, 12. 700. 11, 11. 630. 07, 12. 150. 11, and 12. 800. 17 Gyr with their systematic uncertainty 0. 8 Gyr; distances (systematic uncertainty added) 18. 220. 060. 60, 16. 990. 060. 56, 10. 080. 040. 33, 15. 590. 030. 51, and 8. 290. 030. 27 kpc; reddenings E (B-V) =0. 0230. 004, 0. 0170. 004, 0. 0230. 004, 0. 0230. 003, and 0. 0450. 002 mag with their systematic uncertainty 0. 01 mag; extinctions AV=0. 080. 01, 0. 060. 01, 0. 080. 01, 0. 080. 01, and 0. 160. 01 mag with their systematic uncertainty 0. 03 mag, which suggest the total Galactic extinction AV=0. 08 across the whole Galactic dust to extragalactic objects at the North Galactic pole. The horizontal branch morphology difference of these clusters is explained by their different metallicity, age, mass-loss efficiency, and loss of low-mass members in the evolution of the core-collapse cluster NGC\, 7099 and loose clusters NGC\, 5053 and NGC\, 5466.