This is a region in Cygnus (West) that is on the edge of the deeper hydrogen alpha signals throughout this vast molecular cloud complex.  The working name for this during framing and data collection was Berkeley 88.  The dearth of significant, well-known feature names led me to this obscure open cluster for a name, any name.  Turns out my final framing left Berkeley 88 off frame!  The Ha signals seem to all fall into a number of LBN features also known as DWB, from numbers ~145 to 177.  The principal stars seen here however are interesting in themselves.  The two red giants are eclipsing binaries and the other bright star is a peculiar chemical spinning magnetic star!  Need to research that a bit more.  I thought all stars had some sort of magnetic fields.  My guess is these are probably metal rich.  But my guess would be wrong.  The unique features are not that the stars have magnetic fields (they do, as do most as I guessed), but the magnetic poles are highly orthogonal to their rotational poles.  This odd feature causes metallic elements (anything other than hydrogen or helium to star scientists!) to be stirred to the surface of the magnetic poles leading to odd spectroscopic features.  That these features reside closer to their equators means that these features actually spin about the rotational axis.  You might say they become spectroscopic pulsars!  That allows scientists to study rotational dynamics of any sort.  My guess is that if we could see these up close, the magnetic poles of these stars would look like big fat sun spots that very stable.

Aside from the Ha and stars, there are some, invisible to me, reflection nebulae (yes even on DSS2 color images).  The filament kind of looks like a SNR to me.  But I guess it is not.  I have no idea which stars are enlightening these Ha structures or even the distance to them.  In the end, this data may go into a wider field mosaic, but if my plans work out, I will probably do that with a different setup.  I have only a few more data sets taken with this 61mm "finder" scope, and that will probably end that exercise there...

There is also a couple small very dense molecular clouds in the upper left quadrant of the image.  Could not find any designation for these in the Aladin databases, and yes, even the mouse-over AB plate solve.  So I am going to claim priority on these and name the darkest one Brunelle 1.  Yes B1.  Good idea, right?!

I recall wanting to see what I could make of the edge of this greater Ha region using my 61mm scope and also for "what the heck reason" to see if the fast f2 Halpha filter might work.  I bought this a few years ago hoping to use it to tease out the Flying Dragon, but have never put it to use.  In fact I was able to pull that Dragon out of the stars without using it.  Not only that, but this scope is f5.9 and the filter ought not be ideal, let alone I used this with a OSC camera!  Even still worse!  But, Ha I did capture!  I think being fast Ha filter just means that it is a very broad "narrow" band.  Some say they also have a band shift, but that makes no sense because light entering the central part of a fast primary lens is effectively the same as the light from a stopped down slow lens, so to include all the light from a fast Ha filter, it needs to stick to the original band.  Though it probably means the broadening of the band is skewed in a single direction.  So, if true, a fast Ha filter ought to work fine with a slow telescope.  I won't go into how I included the signal into the image.  I probably did it wrong.  Looking at both the Ha image and the OSC image, the signal strength for the Ha was not that different.  Yes the Ha stars were much reduced.  Which offered no advantage in processing.  I think the Ha structures were actually better defined.  And the background noise was less.  Surprised, since the conventional wisdom comments I have heard about the use of narrow band filters with OSC sensors is that noise and resolution will be worse.  I think that signifies an incorrect understanding about how debayering is actually achieved.  I used the Ha probably mostly to sharpen those Ha clouds.  I cannot say it contributed at all to the signal dynamic of the image in the end.  And I did not want it to really change the appearance within the context of an RGB image.  Yes, there was much star reduction done here.  And that led to a whole host of other work to make it look nice.  But not so for the original data nor the marriage of Ha to OSC.