I reprocessed my original files using Drizzle in the latest version of Siril and used the "Human Weighted Luminance" in  "Generalized Hyperbolic Stretch Transformation", 

Messier 3, NGC 5272Messier 3, in the constellation Canes Venatici, is one of the three brightest globular clusters in the northern sky. It lies on the border of Canes Venatici with Bootes, about 6° NNE of Beta Comae Berenices.

M 3 was discovered by Charles Messier in 1764, and first resolved into stars by William Herschel around 1784.Messier 3 is one of the most beautiful and easily seen globulars. With an apparent magnitude of 6.2, it is visible to the naked eye under dark conditions - and a superb object with the slightest optical aid. In binoculars, it appears as a hazy, nebulous patch. A 4-inch telescope shows a bright compact core within a round and mottled, grainy glow, which fades slowly and uniformly to the outer edges.In an 8-inch telescope, the cluster is fully resolved. It is a glittering ball of stars with an extremely bright, rich, elongated core measuring 1.1' in diameter, and surrounded by an 18'-diameter halo of pinpoint stars. The stars are well resolved across the core, and radiate outward from it in curved chains. The cluster's brightest stars are of magnitude 12.7.Properties and EvolutionAt a distance of 33,900 light years, M 3 is further away than the center of the Milky Way. Its absolute magnitude is -8.93, corresponding to a luminosity of about 300,000 Suns. Its apparent diameter corresponds to a linear size of about 180 light years. Its tidal radius, beyond which member stars would be torn away by the tidal gravitational force of the Milky Way galaxy, is even larger: the cluster gravitationally dominates a spherical volume 760 light-years in diameter. Its total mass has been estimated at 245,000 solar masses.Situated in the galactic halo, about 40,000 light-years from the Galactic Center, M 3 is moving in an inclined orbit that takes it 49,000 light-years above and below the galactic plane; currently it is about 33,000 light-years above that plane. Its orbital eccentricity of e=0.55 takes it up to 66,000 light-years from the galactic center. But its perigalactic distance is only 22,000 light-years; at that distance, its tidal radius will go below 200 light-years, so its outermost stars may escape.M 3 contains approximately 500,000 stars. It is famous for the large number of variable stars discovered in it, the first discovered by E. C. Pickering in 1889. These stars have served as "standard candles" to determine the cluster's distance.The cluster has an age of roughly 8 billion years and contains mostly old, red stars. But it also contains a relatively large number of so-called "Blue Stragglers", blue main-sequence stars which appear to be much younger than the rest of the globular's stellar population. Once puzzling to astronomers, these stars are now thought to form as a result of stellar interactions; their cooler outer layers are stripped away in close encounters, which occur when they pass through the dense central regions of the cluster. (Information fro SkySafari)