Processing an astronomic image may be a journey that reveals unexpected features. Or, at the contrary, sometimes we are close to something interesting and we oversee it and fail to enhance or even suppress it.
In the case of this landscape image I was not looking for anything else but the multitude of open clusters present in the field. And instead, it came out an animated background/foreground, with the dark nebula visible on the top, and the diffused central nebulosity that probably has to do with the molecular cloud that originated most of the clusters visible. I like the cirrus just right of M103, probably named PGCC G127.77-01.68, but take this information with benefit of inventory. At the end I have run the risk of making the image less "nice" by enhancing these non-stellar structures.

This is the first light of this configuration with the APO 80 mm with the camera TS2600.

Many of the star clusters portrayed here are assumed to form part of the stellar association Cassiopeia OB8, that is located in the Perseus arm of the Milky Way, along with the open clusters M103, NGC 654, NGC 659, and some supergiant stars scattered between them, all of them having similar ages and distances.

M103
M103 (also known as NGC 581) is an open cluster where a few hundred, mainly very faint, stars figure in Cassiopeia. It was discovered in 1781 by Charles Messier's friend and collaborator Pierre Méchain. It is located between 8,000 to 9,500 light-years (2500 pc) from the Solar System and ranging over about 15 light years. It holds about 40 certain-member stars, two of which have magnitudes 10.5, and a 10.8 red giant (Admiral William Henry Smyth was the first to see it), which is the brightest within the cluster. A bright known foreground object is the star Struve 131, not a member of the cluster. The cluster may have 172 stars if including those down to 50% probability of a gravitational tie. M103 is about 22 million years old.

NGC663
NGC663, also known as Caldwell 10, is a young open cluster in the constellation of Cassiopeia. It has an estimated 400 stars and spans about a quarter of a degree across the sky.
It is located about 2100 parsecs distant with an estimated age of 20–25 million years. This means that stars of spectral class B2 or higher (in the sense of higher mass), are reaching the end of their main sequence lifespan. This cluster appears to be located in front of a molecular cloud, although the two are not physically associated. This cloud has the effect of blocking background stars from the visual image of the cluster as it lies at a distance of 300 parsecs.
This cluster is of interest because of the high number of Be stars, with a total of about 24 discovered.  There are at least five blue stragglers in the cluster. These are stars that formed by the merger of two other stars.

NGC654
NGC654 is 2,400 parsec away. It is a very young cluster, aged approximately 15 million years, but it could be as old as 40 million years, with a time spread of star formation of at least ~20 Myr. The central region of the cluster shows less reddening than the rest of the cluster. One explanation is that between the Solar System and the cluster lie two dust layers, one at 200pc and one more at 1Kpc.

NGC659
NGC659 is an open cluster approximately placed 2500 pc away.

IC166
It is a very distant open cluster located about 5000 pc away. The great distance and the dust amassed on the galactic plane are probably responsible of the visible star reddening and attenuation.

Czernik5, Czernik4, Trumpler1 (Collinder 15), Berkeley 6
They are open clusters located about 4000 pc, 2100 pc, 2700 pc, 3050 pc away.

(Info from Simbad and Wikipedia)