Chasing the Eastern Veil: A Delicate Ghost in the Summer Sky

 

There are some deep-sky objects that look impressive in almost any photograph. The Eastern Veil Nebula isn't necessarily one of them—at least not when you first look at the raw data.

It is faint. Very faint.

But once the signal begins to emerge, the Eastern Veil reveals an incredible network of delicate filaments, wisps, and arcs stretching across the field. This is one of those targets where the more data you collect, the more there seems to be hiding in the darkness.

The Target

The Eastern Veil is part of the enormous Veil Nebula complex in the constellation Cygnus. The entire Veil is the remnant of a massive supernova explosion that occurred thousands of years ago.

What we're seeing today is essentially the expanding shock wave from that explosion interacting with the surrounding interstellar gas. The result is an enormous web of glowing filaments.

The Eastern Veil contains some particularly beautiful structures, including NGC 6992, NGC 6995, and the surrounding faint nebulosity. Through a telescope, however, much of that structure is extremely difficult to see. Narrowband astrophotography changes the game.

And that's exactly what I was after with this image.

The Imaging Session

For this project I used hydrogen-alpha and oxygen-III filters, with 240-second exposures.

The initial dataset consisted of:

• 18 × 240-second Ha
• 14 × 240-second OIII
• Total integration: 2 hours 8 minutes

Unfortunately, clouds moved through the area during the OIII portion of the session. Several OIII frames had to be discarded rather than allowing compromised exposures into the final stack.

That left me with considerably less OIII data than I would have liked.

The difference between the two channels was immediately apparent. The hydrogen-alpha signal came through relatively strongly, while the OIII was considerably fainter and noisier.

Rather than trying to force the OIII data during processing, I decided the better solution was simply to collect more of it.

Learning From the Noise

One interesting part of this image was discovering just how much difference proper calibration could make.

My first version was processed without calibration frames. I used a plugin called Astro Flat Pro to deal with vignetting and amp glow, and it did a surprisingly good job.

The resulting image contained plenty of detail, but the background was extremely noisy. There were also numerous tiny bright points scattered throughout the image.

I suspected that some of those could be warm or hot pixels rather than actual stars.

So I went back and took 50 dark frames at the same 240-second exposure length and recalibrated the data.

The difference was noticeable.

The background became cleaner and more uniform, and some of the tiny artifacts disappeared. More importantly, I could see that the underlying nebular data was actually quite good. The problem wasn't a lack of detail—it was the signal-to-noise ratio.

That was an important lesson from this image: sometimes the best processing tool is simply more photons.

The Ha and OIII Balance

The Eastern Veil is a particularly good target for a narrowband approach because the different emission lines reveal different aspects of the structure.

The hydrogen-alpha channel provides the strong red emission that defines much of the nebula, while OIII contributes the blue-green/cyan structures.

In this image, the Ha signal is currently stronger than the OIII. That's partly because I ended up with only 14 usable OIII exposures.

The OIII filaments are there, though—and that's what makes me want to collect more.

My plan is to add another 10–16 OIII exposures, bringing the OIII integration up toward 1½–2 hours. I don't think I need substantially more Ha at this point.

More OIII should allow me to bring out the blue-green filaments without having to push the OIII data so hard that the background noise becomes distracting.

A Work in Progress

This isn't quite the final version.

And that's actually one of the things I like about astrophotography.

The image already contains a tremendous amount of structure, but I know there's more buried in the data. Rather than trying to extract everything from a noisy stack, I'm going to let the telescope do the work.

More OIII.

More signal.

A cleaner stack.

Then I'll start the final processing again.

The Eastern Veil is a perfect example of why patience matters in deep-sky imaging. A few hours of exposure can reveal something beautiful, but adding another hour—or two—can transform the way the image can be processed.

For now, this version gives me a pretty good preview of what's waiting in the final dataset.

And judging by the delicate filaments already visible, I think the Eastern Veil is going to be worth the extra time.

Capturing the Cosmic Flower: Imaging the Iris Nebula (NGC 7023)

There is something inherently captivating about dust in deep-space astrophotography. While crisp emission nebulae glowing in hydrogen-alpha offer striking red contrast, reflection nebulae present a far subtle, delicate challenge. Recently, I set my sights on NGC 7023, the Iris Nebula—a stunning dusty reflection nebula located roughly 1,300 light-years away in the constellation Cepheus.

The Target: A Stellar Diamond in the Dust

Unlike glowing emission clouds powered by ionized gas, the Iris Nebula shines by reflecting the light of a massive, bright central star (HD 200775) embedded within a vast cosmic dust cloud. The central blue "petals" spill into faint, rusty brown filaments of dark interstellar dust stretching across the field of view. To capture that delicate blue glow alongside the dark surrounding dusty structures requires steady skies, good signal-to-noise ratio, and patient processing.

The Setup & Capture Strategy

To frame the nebula's central core while retaining surrounding dust, I brought out the broad-spectrum RGB setup:

• Telescope: Astro-Tech AT102ED refractor

• Camera: QHY163M monochrome CMOS

• Exposures: 50–60 second RGB sub-exposures

Rather than running a dedicated Luminance filter—which can easily overwhelm or bleed out the bright central star's core—I decided to shoot exclusively short RGB exposures. This strategy preserved star color and helped manage star halos early in the capture phase.

In the Processing Lab: Unlocking the Blue Petals

Bringing out fine dust while keeping stars tight and noise under control is always a balancing act. Working with raw FITS data and TIFF exports, my processing workflow focused heavily on separation and local contrast:

1. Star-Nebula Separation: Using StarNet to separate the background nebula from the star field allowed independent processing of the faint, dusty structural layers without bloating the stars.

2. Managing Halos: The bright central star, HD 200775, likes to leave its mark. To tame unwanted star halos around the bright stellar core, selective adjustments in Photoshop—specifically desaturating and darkening the magenta channel—kept the central region clean.

3. Layer Blending & Noise Control: I process the object by creating a "Starless" image of the object using a program called "Starnet".  Combining the StarNet layer and the original image with the stars using a Lighten blend mode to preserve subtle dusty details while keeping background noise artifacts in check before applying final curves and stretch actions.  

I have  never been able to get this much of the surrounding dust in previous images of the Iris, so I'm really happy with how this one turned out.

The Crescent Nebula — NGC 6888

 

The Crescent Nebula has always been one of those objects that seems to reveal more the longer you spend imaging it. At first glance, it is an interesting, crescent-shaped nebula surrounded by a field of stars. But once enough exposure is collected and the image is stretched, a much larger structure begins to emerge around it.

This image was another narrowband project, using hydrogen-alpha and oxygen-III to bring out both the bright Crescent and the much fainter nebulosity surrounding it.

Equipment Used

• Astro-Tech AT102ED refractor

• Field flattener

• QHY163M monochrome camera

• QHY CFW3M-SR filter wheel

• Astronomik H-alpha and OIII filters

• ZWO EAF electronic focuser

• Orion guide scope and guide camera

• Sky-Watcher EQ-AL55i Pro mount

• NINA for image acquisition and sequencing

• PHD2 for guiding

The main data for this image came from four-minute narrowband exposures. I spent additional time on the H-alpha channel because the surrounding hydrogen emission is surprisingly extensive. The goal wasn't simply to produce another close-up of the Crescent, but to preserve as much of the surrounding structure as possible.

And that's what I really like about this image.

The Crescent itself is relatively small in the field, but the surrounding nebulosity fills a huge portion of the frame. There are faint, twisting curtains and filaments of hydrogen extending well beyond the bright central nebula. Some of that structure is extremely subtle and would be easy to lose during processing.

I also wanted to keep the OIII contribution fairly natural. The blue-green emission around the Crescent gives the nebula some additional depth without overpowering the extensive red hydrogen emission.

About the Crescent Nebula

The Crescent Nebula, cataloged as NGC 6888, is located in the constellation Cygnus, roughly 5,000 light-years from Earth.

What makes the Crescent particularly interesting is that it isn't simply a cloud of gas illuminated by nearby stars. The nebula was created largely by the interaction between the powerful stellar wind from a massive Wolf-Rayet star and material that the star had expelled during an earlier stage of its life.

The Wolf-Rayet star, WR 136, is an enormous, extremely hot star that is nearing the end of its stellar life. Its incredibly powerful stellar wind is traveling outward at thousands of kilometers per second. That wind is running into material the star lost earlier in its evolution, compressing and heating the gas and producing the glowing shell we see as the Crescent.

The result is this remarkable bubble of energized gas.

And when viewed through narrowband filters, the Crescent becomes even more interesting. Hydrogen-alpha reveals the extensive red emission throughout the region, while OIII brings out areas of ionized oxygen and gives portions of the nebula that characteristic blue-green appearance.

More Than Just a Crescent

One of the things I particularly enjoy about this image is that the Crescent isn't the entire story.

The bright nebula immediately catches your eye, but once you look around the frame, there is nebulosity almost everywhere. The enormous clouds and filaments surrounding NGC 6888 are part of the much larger complex of gas and dust occupying this region of Cygnus.

That's one of the reasons I decided to keep a relatively wide field of view rather than cropping tightly around the Crescent. The surrounding structure gives the image a sense of scale and shows just how much activity is taking place in this part of the Milky Way.

This was also a good example of why I enjoy narrowband astrophotography. Much of this nebulosity is far too faint to appreciate in a normal visible-light photograph, but with enough H-alpha and OIII exposure, it becomes possible to pull these incredibly delicate structures out of the darkness.

The Crescent may be the star of the show, but the faint nebulosity surrounding it is what makes this particular view interesting to me.

— Mike

Messier 27 — Bringing Out the Faint Outer Shell

Equipment Used

This image of Messier 27, the Dumbbell Nebula, was captured using an AT102ED refractor paired with a QHY163M monochrome camera. Focusing was handled by a ZWO EAF electronic focuser, while the system was mounted on a Sky-Watcher EQ-AL55i Pro equatorial mount.  My CGEM died again, so I ordered the Sky-watcher mount to replace it.

Acquisition and imaging were performed with N.I.N.A., with guiding handled through PHD2 using the guide port on the guide camera. The image was built from hydrogen-alpha (Ha) and oxygen-III (OIII) data, with the Ha data playing an especially important role in bringing out the red emission surrounding and within the nebula.

The Image

M27 is one of those objects that looks deceptively simple at first glance. The bright central "dumbbell" is easy to capture, but the much fainter material extending well beyond the main nebula is where the challenge—and much of the beauty—is found.

For this processing, I wanted to preserve that faint outer structure without allowing the background to become either too bright or artificially black. The final image retains a substantial amount of the extremely faint nebulosity surrounding the bright central region.

The central portion shows a strong blue-green/teal appearance from the oxygen emission, while the hydrogen-alpha data provides the contrasting red structures. One of the final processing adjustments was a slight S-curve applied to the red channel, increasing contrast toward the upper end of the red data. That relatively small change brought out considerably more detail in the red structures within and immediately around the core without simply increasing the overall red saturation.

The result is a M27 with a strong contrast between the cooler oxygen-rich interior and the warmer hydrogen-alpha emission surrounding it. The numerous stars remain visible throughout the field, while the faint outer shell gradually emerges from the background rather than being forced into visibility through excessive processing.

For me, that balance is what makes this version work. The goal wasn't simply to make M27 brighter—it was to reveal how much larger and more complex the nebula actually is beyond the familiar bright "dumbbell."

About Messier 27

Messier 27, also designated NGC 6853, is a planetary nebula located in the constellation Vulpecula, the Fox. It lies approximately 1,200–1,240 light-years from Earth and has an apparent magnitude around 7.5, making it one of the brighter planetary nebulae in the night sky.

Despite its name, a planetary nebula has nothing to do with planets. The name dates back to the early days of astronomy, when these objects sometimes appeared somewhat planet-like through small telescopes. M27 is actually the expanding remains of a dying star that shed its outer layers. The exposed stellar remnant at its center is now an extremely hot white dwarf, whose ultraviolet radiation causes the surrounding gas to glow.

Charles Messier discovered M27 in 1764, making it the first planetary nebula ever discovered. It subsequently became famous for its distinctive dumbbell-like appearance, which gives the object its popular name.

What makes M27 particularly fascinating is that the bright central structure is only part of the story. The nebula contains numerous knots and filaments of gas and dust, with some structures extending far beyond the bright central region. These complex structures are part of the continuing interaction between the material expelled by the dying star and the stellar winds and radiation from the hot central remnant.

In other words, what we're seeing in this image is not simply a colorful cloud in space. We're looking at the remains of a star much like our Sun, caught in the process of transforming itself into a white dwarf. M27 gives us a glimpse of one possible future for our own Sun, billions of years from now.

Four Globular Clusters During a Bright Almost Full Moon

 These 4 images were taken on May 28, 2026 using the 8" Newtonian and QHY163M camera using the RGB filter set.

Messier 5

Messier 5 (M5) is one of the most impressive globular clusters visible from Earth. Located about 24,500 light-years away in the constellation Serpens, it contains hundreds of thousands of stars packed into a roughly spherical shape. First observed by Gottfried Kirch in 1702 and later cataloged by Charles Messier in 1764, M5 appears as a faint, fuzzy patch of light through binoculars but reveals a stunning swarm of individual stars when viewed through a telescope.

What makes Messier 5 particularly remarkable is its great age. Astronomers estimate that the cluster is more than 12 billion years old, meaning its stars formed not long after the Milky Way galaxy itself began to take shape. Spanning about 165 light-years in diameter, M5 is home to numerous variable stars and some of the oldest known stars in our galaxy. Its brightness, rich stellar population, and ease of observation have made it a favorite target for both amateur astronomers and professional researchers studying the history and evolution of the Milky Way.

Messier 3

Messier 3 (M3) is one of the largest and brightest globular clusters in the northern sky. Located in the constellation Canes Venatici, approximately 34,000 light-years from Earth, it contains an estimated 500,000 stars packed into a dense spherical formation. Discovered by Charles Messier in 1764, M3 appears as a faint fuzzy patch through binoculars but becomes a spectacular sight in even modest telescopes, where countless individual stars can be resolved around its bright central core.

M3 is also notable for its great age and scientific importance. Astronomers estimate that the cluster is more than 11 billion years old, making it a relic from the early history of the Milky Way. It contains an unusually large number of variable stars, which have helped researchers study stellar evolution and measure cosmic distances. Because of its brightness, rich stellar population, and accessibility to amateur observers, Messier 3 remains one of the most popular globular clusters for both astronomical research and visual observation.

Messier 13

Messier 13 (M13), often called the Great Hercules Cluster, is one of the most famous and spectacular globular clusters in the night sky. Located in the constellation Hercules, approximately 22,000 light-years from Earth, M13 contains several hundred thousand stars packed into a spherical region about 145 light-years across. Discovered by Edmond Halley in 1714 and later added to Charles Messier's catalog, the cluster is bright enough to be seen with binoculars under dark skies and becomes a breathtaking sight through even a modest telescope.

M13 is estimated to be nearly 12 billion years old, making it one of the oldest known objects in the Milky Way. Its dense core and vast population of ancient stars provide astronomers with valuable clues about the formation and evolution of our galaxy. For amateur astronomers, M13 is often considered the finest globular cluster visible from northern latitudes, offering stunning views of countless stars that appear to sparkle outward from its brilliant center. Its beauty and accessibility have made it a favorite target for observers for generations.

And finally,

Messier 53

Messier 53 (M53) is a globular cluster located in the constellation Coma Berenices, approximately 58,000 light-years from Earth. Discovered by Johann Elert Bode in 1775 and later added to Charles Messier's catalog, M53 appears as a faint, round glow through binoculars and small telescopes. Larger telescopes reveal a dense concentration of ancient stars surrounding a bright central core. Although not as well known as some of the brighter globular clusters, M53 is a rewarding target for observers due to its compact structure and its location in a region of the sky rich with deep-sky objects.

M53 is estimated to be more than 12 billion years old, making it one of the oldest members of the Milky Way's halo population. The cluster contains hundreds of thousands of stars that formed during the early stages of our galaxy's history. Astronomers have studied M53 to better understand stellar evolution, variable stars, and the chemical composition of ancient star systems. Its great age and distance offer a glimpse into the Milky Way's distant past, while its delicate appearance in the eyepiece makes it a favorite challenge for amateur astronomers observing under dark skies.

All of these actually consists of 12 - 60 second subs through each RGB filter.  These objects are less affected by a bright sky due to light pollution or a full moon, which made them the logical targets during a bright moon.