These 2 planetary nebulae are located in the constellation of Cassiopeia at a declination of +65 degrees. This area of the sky is unique in that it captures two planetary nebula in one relatively narrow field of view. Both nebula are dominated by light in the OIII band and are faint.

Abell 6, at lower right, is the traditional planetary nebula type. It is a magnitude 15 PN with a diameter of 3 arc minutes. It is 3100 light years away and has a true diameter of 2.7 light years.  The outer edge of the nebula is brighter and shows traces of hydrogen. The central star is visible but very faint.  This PN is an average Abell PN in all measures of size, distance and brightness.

The larger and more interesting PN at upper left, HFG 1, was discovered in 1982. It has an apparent diameter of about 8 arc-minutes and is located 2300 light years away.  It has a large PN diameter of 5 light years and its central star is the 14.5 binary star V664 Cas, seen as the bright small cyan star in the exact center of the nebula.

There are many interesting aspects of this nebula. The first is the bright bow shock rim to the lower left, which is separated by a large gap from the central nebula. Three bright bluish lobes lie between the rim and the center. The center area itself is relatively clear of nebulosity. A long, faint reddish trail of hydrogen extends from the center up to the right.  

I am not aware of another PN with a OIII bow shock rim and HII tail like this one.  Studies of this PN have concluded that both characteristics are due to the high motion of the progenitor star to the lower left, interacting with the surrounding ISM and HII signal.  

Also interesting is the small reddish nebulous blob within the HFG 1 PN at 9 o'clock.  This blob has been identified by various sources as a galaxy (LEDA 2797165) and a low excitation PN knot, 2 very different types of objects.  I don’t believe it is a galaxy, because of its red color in my RGB-only subs.  But I also find it difficult to believe that it is a knot, being so far away from the progenitor in the “upwind” direction of progenitor travel.  Like many PNe (and DSOs in general), there are many fascinating questions here for us to ponder.

Finally, here is my old image of these two objects, taken using 3x the integration time of this image, providing a comparison between the results of a refractor and a RASA.