Last night I had limited time (I had an early appointment Friday morning) and just wanted to get out and do something, the moon is almost full, but I decided on trying to get as much of the nebulosity as I could.  I think the image turned out pretty decent, but am going work on post processing this data again.  I have also been experiencing guiding spikes recently using the AM5 and the ASIAIR Plus.  I had several of them during my session last night, but I cleared calibration and then recalibrated guiding and that seemed to help.  But I didn't lower my guide exposure from 3 seconds, to maybe 1 sec or .5 seconds, the next clear night I am going to give that a go.  I also purchased a filter wheel, even though I have the ASI2600MC camera, I am thinking it will be better for switching out the filters I do have (Optolong UV/IR cut, L-Pro, L-eNhance and L-Ultimate)

Reflection Nebulosity
On clear, dark nights, when the moon is absent, swirls of nebulosity are noticeable around a some of the brighter stars, especially near Merope. Longer exposure photographs, and "rich field" telescopes, reveal that the Pleiades are embedded in nebulous material. The Pleiades nebulae are blue-colored, which indicates that they reflect the light of the bright stars situated near (or within) them. The brightest of these nebulae, around Merope, was discovered in 1859 by Wilhelm Tempel at Venice, Italy with a 4" refractor. The Merope Nebula (NGC 1435) requires a dark sky and is best visible in a rich-field telescope.The nebulae around Maia (NGC 1432), Alcyone, Electra, Celaeno and Taygeta were found on photographs between 1885 and 1888 by the Henry brothers in Paris and by Isaac Roberts in England. In 1890, E. E. Barnard discovered a concentration of nebulous matter very close to Merope (now catalogued as IC 349). Analysis of the spectra of the Pleiades nebulae by Vesto Slipher in 1912 revealed their nature as reflection nebulae, as their spectra are exact copies of the spectra of the stars illuminating themPhysically, the reflection nebulae are unrelated to the Pleiades cluster, as can be seen from the fact their radial velocity differs from the cluster's by 11 km/sec. Instead, the cluster is simply passing through a particularly dusty region of the interstellar medium. The dust is not a remainder of the nebula from which the Pleiades formed, as was formerly thought. At the cluster's age of 100 million years, almost all the dust originally present when it formed would have been dispersed by radiation pressure.
Properties and EvolutionBefore the launch of the Hipparcos satellite in 1991, the Pleiades' distance was thought to be about 440 light years. Hipparcos caused consternation among astronomers by measuring a distance of only 380 light years. This would have required the Pleiades stars to be comparatively fainter, without explanation. However, subsequent investigations by the Hubble Space Telescope, and the Mount Wilson and Palomar Observatories, found that Hipparcos's measurement of the Pleiades' parallax was too small. Their distance is currently thought to be 440 light years, and it is not yet known why the Hipparcos parallax error occurred.The Pleiades' core cluster radius is about 8 light years, and its tidal radius is about 43 light years. The cluster contains over 1,000 confirmed members, with a total mass estimated at about 800 Suns. The stars in the Pleiades are thought to have formed together around 100 million years ago; its brightest members all hot, young, blue-white class B giants and subgiants, with absolute magnitudes from about -1.5 to -2.5.Some of the Pleiades stars are rotating rapidly, with velocities of 150 to 300 km/sec - common among young class B main sequence stars. This rotation gives them oblate spheroid bodies. The rotation can be detected because it broadens their spectral lines as parts of the stellar surface approach us on one side, while those on the opposite side recede. Pleione is the most rapidly rotating star in the cluster, and has ejected a gas shell because of this rotation. It is also variable, between magnitudes 4.77 and 5.50.The Pleiades cluster contains some white dwarf stars. White dwarves cannot have masses above 1.4 Suns (the Chandrasekhar limit). Such low-mass stars take billions of years to evolve into that state, not just the 100-million-year age of the Pleiades cluster. How, then, can white dwarves exist in such a young star cluster? The only possible explanation seems to be that these white dwarf stars were once more massive and evolved faster, but have since lost mass due to strong stellar winds, close neighbors, or fast rotation.The cluster also contains many brown dwarves, which are objects containing less than 8% of the Sun's mass, and are not heavy enough to start nuclear fusion reactions in their cores and thus become proper stars. Brown dwarves may constitute up to 25% of the total population of the cluster, although they contribute less than 2% of its total mass.Eventually, the Pleiades' space motion will carry them below the feet of Orion, as seen from Earth. After that, they will take about 250 million years to disperse, due to gravitational interaction with the galactic neighborhood.

@information from SkySafari