Planetary Nebula - Ha - What are they good for ?"

 

M57 The Ring Planetary Nebula
in the constellation Lyra. Imaged by: Pip Stakkert from the JPO
using the Meade 127mm Apo Refractor and the Canon 600d DSLR

M27 The Dumbbell Planetary Nebula
in the constellation Vulpecula. Imaged by: Kurt Thrust from the JPO
using the Meade 127mm Apo Refractor and the Canon 600d DSLR

M76 The Little Dumbbell or Cork Planetary Nebula in the constellation Perseus.
Image created, curated and processed by Kurt Thrust.
Data Credit: COAST Robotic Telescope, Teneriffe.
telescope.org Open Observatories, Open University.

M97 The Owl Planetary Nebula 
in the constellation Ursa Major
Image created, curated and processed by Kurt Thrust.
Data Credit: PIRATE Robotic Telescope, Teneriffe.
telescope.org Open Observatories, Open University.

" The Observatory sponsors recently invested in RC -Astro's excellent 'NoiseXTerminator' plug in for the Affinity Photo 2.65 software, which we use as our core photo editor at the Jodrell Plank Observatory. So the team decided to test it on a selection of images we always considered 'noisy'.

Kurt also thought that Planetary Nebulae had not been featured that often in previous posts and very little had been said about these small and intriguing objects, which irrespective of their generic collective name have absolutely nothing to do with planets" - Joel Cairo CEO of the Jodrell Plank Observatory.

"Observation Report: A Comparative Study of Planetary Nebulae — M57, M27, M76, and M97

Among the most striking celestial objects captured by amateur and professional astronomers alike are the planetary nebulae — delicate, luminous shells of gas cast off by dying stars. Despite their name, these nebulae have nothing to do with planets; the term originates from their round, planet-like appearance in early telescopes. In reality, they represent a fleeting but beautiful phase in stellar evolution, a brief transition between the red giant and white dwarf stages.

Planetary nebulae mark the final breaths of Sun-like stars — those with masses up to roughly eight times that of our Sun. After spending billions of years fusing hydrogen into helium, such a star exhausts its nuclear fuel and swells into a red giant. In its unstable outer layers, pulsations and stellar winds drive away the star’s atmosphere, leaving behind an exposed core. The remnant, an intensely hot white dwarf, bathes the ejected gases in ultraviolet light, causing them to glow in intricate patterns and vivid colors. This process lasts only a few tens of thousands of years — a mere instant in cosmic time — before the nebula dissipates into the interstellar medium. One day, our own Sun will undergo this transformation, shedding its outer layers to illuminate the space once occupied by the Solar System with a faint, spectral glow.

The images presented here — of M57, M27, M76, and M97 — showcase four distinct manifestations of this same underlying process, each a variation on the theme of stellar death and renewal.

M57 — The Ring Nebula in Lyra appears as a nearly perfect oval, a smoke ring suspended against the velvet backdrop of the constellation Lyra. Its symmetry and sharply defined edges make it one of the most iconic planetary nebulae. The bright ring traces dense gas expanding at about 20 km/s, while the interior is filled with a fainter, ionized glow. The white dwarf at its heart shines with a temperature exceeding 100,000 K, illuminating the nebula like a hidden ember lighting a cloud of dust.

M27 — The Dumbbell Nebula in Vulpecula contrasts sharply with M57’s geometric simplicity. Instead of a ring, M27 displays a complex hourglass shape, the result of gas escaping along preferred directions in the star’s equatorial and polar regions. Its relatively large apparent size and brightness make it a favorite target for both observers and imagers. The vivid greens and reds often seen in photographs arise from doubly ionized oxygen and hydrogen-alpha emissions, respectively — spectral fingerprints of the nebula’s composition and excitation.

M76 — The Little Dumbbell Nebula in Perseus presents a more turbulent visage. Its bipolar structure resembles a miniature version of M27 but appears denser and more irregular, suggesting strong stellar winds or interactions between successive shells of ejected gas. Often described as one of the faintest Messier objects, M76 rewards deep exposures with intricate filaments and knots that hint at the chaotic processes shaping planetary nebulae.

Finally, M97 — The Owl Nebula in Ursa Major takes its name from the ghostly “eyes” visible in long-exposure images, dark cavities within an otherwise round shell. Its soft, diffuse glow and subtle color palette contrast with the crisp outlines of M57, giving it a tranquil, almost meditative appearance. The symmetry of M97 suggests a more isotropic mass loss, a calm exhalation of stellar material compared to the more directional outflows of M27 and M76.

Together, these four nebulae form a kind of evolutionary gallery — each a testament to the diversity of outcomes when stars of similar mass approach the end of their lives. Differences in mass, composition, rotation, and surrounding environment sculpt each nebula into a unique shape, much as individual personalities imprint themselves on human lives.

For the casual observer, planetary nebulae may seem serene and static, but in truth they are dynamic, expanding, and evolving. The gas we see today will, in a few millennia, blend into the cosmic medium, seeding new stars and planets. In this sense, planetary nebulae are not symbols of death, but of transformation — reminders that the material of stars, including that of our own Sun, ultimately returns to the galaxy to begin anew". Professor G.P.T Chat visiting astrophysicist at the JPO.

The Comet C:/2025 A6 (Lemmon)

 

Comet C:/2025 A6 (Lemmon) imaged by Kurt Thrust at the JPO
on the 21st October 2025
using a fixed tripod mounted Canon 600d DSLR
 with a 135mm F2 Samyang lens. Stacks of 10x5 sec subs at ISO 1600.

" Kurt was very lucky to capture some short exposure subs of the Comet C/2025 A6 (Lemmon) from the approach road to the Jodrell Plank Observatory, on the 21st October 2025. In the early evening twilight and amongst the clouds and light pollution, the comet was extremely difficult to see with the naked eye. It was located very low in the north west and to the west of the bright star Arcturus, which Kurt used as a guide. In such circumstances it is very useful to have the Stellarium App on your smartphone! 

Bearing in mind the shortness of the sub exposures a reasonable amount of detail can be seen in Kurt's two stacked images. Close inspection reveals: a small green coma around the comet nucleus, separate ion and dust clouds and some disturbance in the fainter part of the ion tail created by the current strong solar wind". - Joel Cairo CEO of the Jodrell Plank Observatory.

"Comet C/2025 A6 (Lemmon) is a long-period comet discovered on 3 January 2025 by the Mount Lemmon Survey at Mount Lemmon, Arizona. 

 It is notable for its striking greenish coma and its relatively rare visit to the inner Solar System, offering a “once-in-a-millennium” viewing opportunity.

Orbital and Physical Characteristics:

Perihelion distance (q): ~0.5299 AU from the Sun.

Closest approach to Earth: ~0.596 AU (~89 million km) on 21 October 2025. 

Orbital eccentricity: approximately 0.9957 (inbound) indicating a very elongated trajectory. 

Inclination: ~143.66° relative to the ecliptic. 

Estimated orbital period before perturbations: ~1,350 years. 

The comet’s coma displays a green hue, attributed to diatomic carbon (C₂) fluorescing under solar ultraviolet radiation. 

Observational History and Brightness Evolution:

Upon discovery, the comet had a magnitude of ~21.6 while at ~4.5 AU from the Sun. 

 As it moved inward, its brightness increased more rapidly than initially predicted, making it an excellent target for astrometric monitoring and public sky-watching.

By late September and early October 2025, the comet’s magnitude had improved to around +8 to +6.6, with a visible ion tail several degrees long in photographs. 

 Projections suggested it might reach magnitudes around +3.5 to +4 at closest approach — potentially visible to the naked eye under dark skies. 

Coma and Tail Morphology:

The nucleus of the comet is surrounded by a diffuse coma of sublimated ices and entrained dust. As the comet approached perihelion, solar heating drove the sublimation of volatile ices, producing jets and releasing dust particles. These created a dual-tail structure:

An ion tail, composed of ionised gas interacting with the solar wind, giving a straight, bluish or greenish stream pointing away from the Sun. 

A dust tail, composed of larger dust grains lagging behind the nucleus, giving a broader, more curved appearance. 

On 2 October 2025, a tail‐disconnection event was reported — a phenomenon where part of the ion tail is severed by a magnetic shock in the solar wind. 

Significance and Future Return:

Because of its long period and highly elongated orbit, Comet Lemmon is not expected to return for ~1,000 years or more — making this passage effectively a once-in-a-human-lifetime event. 

 Moreover, its green coma offers both aesthetic and scientific interest: the chemistry of C₂ and other radicals in cometary comae is a window into the pristine ices preserved since the Solar System’s formation.

Viewing Circumstances (for Northern Hemisphere):

From mid- to late October 2025, the comet became progressively favourably placed in the evening sky. It moved through constellations such as Boötes and Serpens, and at its peak was visible at solar elongations of ~30-40°. 

 Observers are advised to look from a dark site, away from light pollution, and employ binoculars or small telescopes to first locate the object; naked-eye spotting is possible under very good conditions. 

Scientific Importance:

Comets such as C/2025 A6 (Lemmon) are fragments from the outer Solar System (likely the Oort Cloud) that are only occasionally perturbed into the inner region. Studying their composition, dust and gas production rates, and response to solar heating helps refine models of Solar System evolution, volatile delivery to the terrestrial planets, and the dynamics of cometary orbits. Moreover, morphological changes (such as tail disconnection events) provide in situ diagnostics of the solar wind–comet interaction.

Summary:

Comet C/2025 A6 (Lemmon) presents a rare observational opportunity: a long‐period comet with a greenish coma, brightening unexpectedly to visibility, and approaching within ~0.6 AU of Earth in October 2025, with perihelion at ~0.53 AU in November. Its highly elongated orbit, infrequent return, and the dual‐tail morphology make it both a compelling target for amateur and professional astronomers, and a valuable subject for cometary science". Professor G.P.T. Chat visiting astrophysicist at the Jodrell Plank Observatory.

Star cluster in the heart of the Rosette - NGC 2244

 

NGC 2244, Open Star cluster in the Rosette Nebula located in the constellation Monoceros the Unicorn.
Data credit: COAST robotic telescope - SHO filters - blended Sll and Ha for luminance, telescope org. Open Observatories, Open University.
Image Credit: Kurt Thrust at the JPO.

" The Essex based astroimager, Nik Szymanek , has been writing an interesting series of articles in the magazine Astronomy Now, showcasing the ways in which SHO palette images may be processed using the Sll and Ha data as a synthetic luminance layer. I was much intrigued with this idea and and wondered if the Rosette Nebula might respond well to using a blended Sll and Ha synthetic luminance layer. The particular blend I used accentuated Sll (ionised sulphur}over and above the Ha (Hydrogen alpha) content. I believe this image processing method has made for the more dramatic photograph above" - Kurt Thrust current Director of the Jodrell Plank Observatory. 

The Rosette Nebula; Seestar S30 with Dual Band nebula filter, 
flipped vertically to match orientation with the top detail image 
Processed to emphasise the H alpha component of the image.
Image Credit: Pip Stakkert at the JPO

The Rosette Nebula; Seestar S30 with Dual Band nebula filter,
flipped vertically to match orientation with the other images .
Processed to emphasise the 3 dimensional nature of the nebula
with reduced emphasis on the H alpha component of the image.
Image Credit: Pip Stakkert at the JPO

A Brief Report on the Open Cluster NGC 2244 and Ionised Gas in the Rosette Nebula

The open star cluster NGC 2244 is located at the centre of the Rosette Nebula (Caldwell 49), a large H II region in the constellation Monoceros, at an approximate distance of 1.5–1.6 kiloparsecs (about 5,000 light-years) from the Sun. The cluster has an estimated age of 2–6 million years and is composed primarily of young, massive O- and B-type stars. These hot, luminous members are the principal sources of the nebula’s ionisation and play a dominant role in shaping its morphology through intense ultraviolet radiation and stellar winds.

The energetic radiation field of NGC 2244 drives a strong ionisation front, producing extensive emission in the H α (656.3 nm) recombination line of hydrogen, characteristic of classical H II regions. The nebula’s interior exhibits strong [O III] (495.9 and 500.7 nm) emission, arising from doubly ionised oxygen in regions of higher excitation closer to the cluster core. In contrast, [S II] (671.6 and 673.1 nm) lines are more prevalent along the periphery of the nebula and in dense ionisation fronts, where lower excitation and partially ionised zones are found.

The spatial distribution of these emission lines delineates the stratified ionisation structure typical of massive star-forming regions: [O III] tracing the hottest, most highly ionised gas; H α marking the main ionised hydrogen volume; and [S II] outlining the transition to neutral material. Together, these diagnostics reveal the ongoing interaction between the cluster’s massive stars and their natal molecular cloud, providing a detailed view of stellar feedback processes in early cluster evolution. - Professor G.P.T Chat visiting astrophysicist at the Jodrell Plank Observatory.

"And now for something completely different"

 

The Double Quasar in the Constellation Ursa Major. Data Credit: the COAST robotic telescope, BVR filters, Tenerife. telescope.org. Open Observatories, Open University. Image Credit: Kurt Thrust at the JPO.

" I was going through the JPO archive of data obtained via Open Observatories and discovered that in February 2024, my friend Kurt Thrust had programmed the COAST robotic telescope to image two Quasars. A quasar is an extremely luminous, active galactic nucleus powered by a supermassive black hole at the center of a distant galaxy. As gas and dust fall into the black hole, they form a superheated accretion disk that emits massive amounts of energy across the electromagnetic spectrum, often outshining its host galaxy. These objects can also produce powerful jets of radiation and are among the brightest objects in the universe. The 'Double Quasar in Ursa Major, is remarkable in that in reality it is one object that appears as two because of gravitational lensing. 

The Double Quasar and Neighboring Galaxies in Ursa Major

 The Double Quasar (Q0957+561)

The object known as Q0957+561, often referred to as the Double Quasar, is one of the most celebrated examples of gravitational lensing in extragalactic astronomy. It resides in the constellation Ursa Major, at a redshift of z ≈ 1.41, corresponding to a light-travel distance of roughly 8.7 billion light-years.

What makes Q0957+561 remarkable is its appearance as two nearly identical quasar images separated by about 6 arcseconds on the sky. These twin images  are not two distinct quasars, but rather light from a single background quasar that has been gravitationally lensed by an intervening galaxy and its surrounding cluster of galaxies at z ≈ 0.36. The foreground lensing galaxy, a massive elliptical designated G1, lies directly between the two quasar images.

The Double Quasar
showing the lensing galaxy cluster
image credit: ESA/Hubble

This system provided the first confirmed case of gravitational lensing of a quasar, discovered in 1979 by Dennis Walsh, Robert Carswell, and Ray Weymann. The discovery confirmed one of the key predictions of Einstein’s general theory of relativity: that massive bodies curve spacetime sufficiently to split and magnify light from background sources.

Subsequent long-term monitoring of the Double Quasar has revealed a measurable time delay of about 417 days between variations in brightness of the two images. This delay arises because the two light paths have slightly different lengths and traverse different gravitational potentials. Measurement of this delay has been used to estimate cosmological parameters such as the Hubble constant, making Q0957+561 a cornerstone object in observational cosmology.

At the eyepiece, Q0957+561 is an extremely faint object of approximately magnitude 16.5, appearing star-like even in large amateur telescopes. Only with high-resolution imaging or long-exposure CCD observations can the twin images be resolved.

NGC 3079

Located roughly 10 arcminutes south of Q0957+561, NGC 3079 is a striking edge-on spiral galaxy in Ursa Major, at a distance of about 50 million light-years (z ≈ 0.0037). Classified as type SBc, it exhibits a strong central starburst and nuclear activity, often cited as an example of a Seyfert 2 or LINER galaxy.

High-resolution imaging reveals a prominent dust lane bisecting its stellar disk and a biconical outflow of hot gas extending several kiloparsecs from the nucleus. X-ray and radio observations indicate the presence of superbubbles and galactic-scale winds driven by intense star formation and possibly a weak active nucleus. NGC 3079 is therefore a laboratory for studying feedback processes between star formation, black hole activity, and the interstellar medium.

n small telescopes, NGC 3079 appears as a slender, elongated streak of light—an impressive edge-on system that offers a vivid contrast to the much more distant and exotic Double Quasar nearby on the sky.

 NGC 3703

Farther east in Ursa Major lies NGC 3703, a relatively faint spiral galaxy (type Sc) situated at a distance of approximately 90–100 million light-years. With an apparent magnitude near 12.8, it is considerably fainter and less studied than NGC 3079. Its disk shows loosely wound spiral arms and moderate star-forming activity. NGC 3703 belongs to the same general region of the sky as the Ursa Major Cluster of galaxies, though it may lie slightly in the background relative to the cluster’s core.

While lacking the dramatic features of NGC 3079 or the cosmological significance of the Double Quasar, NGC 3703 serves as a representative example of a normal, late-type spiral galaxy, offering a useful photometric and spectroscopic comparison to more active systems in the same constellation.

Astronomical Context

• The region of Ursa Major containing Q0957+561 and NGC 3079 is an area of considerable astrophysical diversity. Within a single degree of sky, one can observe:
• A galaxy-scale gravitational lens probing the structure of spacetime and the expansion of the universe;
• A starburst galaxy exhibiting large-scale feedback and nuclear outflows; and
• A normal spiral system representative of the quiescent star-forming population.

Together, these objects demonstrate the richness of extragalactic phenomena observable in a single patch of the northern sky — from the nearby universe of tens of millions of light-years to the deep cosmos nearly nine billion years in the past.

Distance to the Double Quasar Q0957+561

• Redshift (z): ≈ 1.41

This redshift means the light we see from the quasar left it when the universe was much younger — less than half its current age.

Using the latest ΛCDM cosmological parameters (H₀ = 70 km s⁻¹ Mpc⁻¹, Ωₘ = 0.3, ΩΛ = 0.7), we can derive several commonly used distance measures:

Distance Type	Value	Meaning
Light-travel time distance	≈ 8.7 billion light-years	How long the photons have been en route to us.
Comoving radial distance	≈ 9.3 billion light-years	The current proper distance to where the quasar is now, accounting for cosmic expansion.
Luminosity distance	≈ 10.6 billion light-years	Used in converting apparent to absolute brightness, factoring in redshift dimming.

Thus, the Double Quasar is among the most distant objects visible in amateur-sized telescopes — you are seeing it as it appeared when the universe was only about 4.5 billion years old, roughly one-third of its current age.

Foreground lens galaxy

The massive elliptical galaxy G1, which lenses the background quasar, has a redshift of z ≈ 0.36, corresponding to a light-travel time of about 4.0 billion light-years.

The geometry of these two distances — a lens about halfway between us and the quasar — is what produces the beautiful and scientifically rich double image observed as Q0957+561 A and B.

In summary:

Q0957+561 lies roughly 8.7 billion light-years away, making it one of the farthest celestial objects ever discovered by purely optical means and the first gravitationally-lensed quasar confirmed in human history."

 - Karl Segin  outreach co-ordinator at the JPO and Professor G.P.T Chat.

The Double Cluster re-visited

 

The Double Cluster - NGC 869 and NGC 884. Modded Canon 200d DSLR with Dual Band Filter and 135mm Samyang Lens.

Map Credit: freestarcharts.com

" Both Kurt and Pip have never believed that they have done the Double Cluster justice. When you look at this pair of open star clusters, through binoculars or a widefield eyepiece on  a telescope at low magnification, it is truly magnificent.  The Double Cluster, viewed through the JPO's tripod mounted 11x80mm.binoculars, is a joy to see in its jewel like appearance. If you have a pair of binoculars and it's a clear night in the Northern Hemisphere, why not try and find it between Cassiopeia and Perseus? - Joel Cairo CEO of the Jodrell Plank Observatory.

"The Double Cluster in Perseus, catalogued as NGC 869 and NGC 884, is a striking pair of young, massive open star clusters located in the Perseus arm of the Milky Way Galaxy. Situated at an approximate distance of 7,500 light-years (2.3 kpc) from Earth, the system lies within the Perseus OB1 association, an active star-forming region rich in hot, luminous stars.

Both clusters are estimated to be relatively young, with ages on the order of 12–14 million years, placing them in a comparable evolutionary stage. Their stellar populations are dominated by early-type B-class main-sequence stars and a notable complement of evolved blue and red supergiants, evidence of rapid stellar evolution in high-mass stars. Integrated spectral analyses indicate a near-solar metallicity, consistent with their origin in a typical Galactic spiral-arm environment.

The clusters are physically separated by only a few hundred light-years, suggesting a common origin from the same giant molecular cloud. Their projected angular separation on the sky is approximately 30 arcminutes (roughly the apparent diameter of the full Moon), making them easily distinguishable yet visually connected in telescopic and binocular observations.

Photometric studies of NGC 869 and NGC 884 reveal high stellar densities in their cores, with mass estimates of several thousand solar masses each, placing them among the most massive open clusters in the Milky Way. Their combined luminosity and concentration of bright, blue stars make the Double Cluster an archetypal laboratory for studying the early dynamical evolution of clustered stellar populations.

Owing to their brightness (apparent magnitudes ~+4.3 and +4.4) and their location near the Perseus–Cassiopeia border, the Double Cluster has been recognized since antiquity, though it was first catalogued systematically by Hipparchus around the 2nd century BCE. Today, the system remains a prominent observational target for both professional astrophysical research and amateur astronomy, offering insight into star cluster formation, stellar evolution, and Galactic structure". - Professor G.P.T. Chat visiting astrophysicist at the Jodrell Plank Observatory.

The Heart of the matter

 

IC 1805 and Melotte 15.

"The above images captured at the Jodrell Plank Observatory and also by the PIRATE robotic telescope on Mount Teide, Tenerife (credit telescope .org, Open Observatories, Open University) show the Heart Nebula, IC1805 in increasing detail and reducing field of vision. The top, widefield image was captured with the JPOs modded Canon 200d Camera with a Dual Band filter and a Samyang 135mm lens. The other two were captured by the PIRATE telescope with SHO filters. Pip Stakkert used a number of processing techniques to emphasise the nebulosity". - Kurt Thrust current Director of the JPO.

"The Heart Nebula (IC 1805) is a large emission nebula located in the Perseus Arm of the Milky Way, within the constellation Cassiopeia. At an estimated distance of approximately 6,000–7,500 light-years from Earth, it extends over nearly 200 light-years in diameter, making it one of the more prominent star-forming complexes in the northern sky. Its common name derives from the overall morphology of its extended H II region, which, in wide-field optical images, presents an outline reminiscent of a stylized human heart.

The nebula is primarily excited by the young stellar population of the open cluster Melotte 15, situated near the nebula’s center. This cluster, containing numerous hot O-type and early B-type stars, serves as the dominant ionizing source for the surrounding gas. The intense ultraviolet radiation emitted by these massive stars ionizes the hydrogen in the surrounding molecular cloud, producing the characteristic red glow of Hα emission. Stellar winds and radiation pressure also drive large-scale feedback processes that shape the morphology of the nebula, generating bright ridges, cavities, and dark, pillar-like structures of dense gas.

Of particular note is the brighter nebulosity concentrated near the nebula’s core. This region surrounds Melotte 15 and exhibits a higher surface brightness due to the proximity of the ionizing sources and the resulting density contrast between ionized and neutral gas. Within this core, the interplay between radiation, stellar winds, and turbulence has carved out intricate filaments and luminous fronts, where shock compression has enhanced local gas densities. These conditions are conducive to ongoing star formation: observations at infrared and radio wavelengths reveal embedded protostars and compact H II regions tracing younger generations of stellar objects still enshrouded in dust.

In summary, IC 1805 exemplifies the dual role of massive stars in galactic ecology: while their radiation and winds sculpt and erode the parent molecular cloud, they also trigger subsequent episodes of star formation. The central bright nebulosity of the Heart Nebula, therefore, represents not only a visually striking concentration of emission but also the dynamic hub of stellar feedback and continuing stellar genesis within the complex". -Professor G.P.T Chat and Karl Segin outreach coordinator at the JPO.

The Iris Reflection nebula in the constellation Cepheus

The Iris Nebula in modified SHO format. The PIRATE Robotic Telescope,Mount Teide, Teneriffe.   Data Credit: telescope.org. Open Observatories, Open University. Image Credit: Kurt Thrust.

" Kurt was feeling a little better today and so he and the JPO engineer, Jolene McSquint-Fleming, were busy remaking a diffraction grating for the Seestar S30. They decided to make a grating, which covers the full aperture of the little scope rather than  partially. It will be interesting to see whether this affects the accuracy of the scope's guidance and goto software". - Joel Cairo CEO at the JPO.

The new-recycled magnetic 50 lines/mm
full aperture grating for the Seestar 30

Spectrum produced by the above grating
using the JPO Visitor Centre door security peep hole
as an artificial star.

" If we get a clear night soon, we will try the new grating out and develop a capture process, which enables the removal of stars and hot spots, which otherwise corrupt the  target and calibration spectra". - Kurt Thrust current Director of the JPO.

" The Iris Nebula, cataloged as NGC 7023, is a bright reflection nebula located in the constellation Cepheus, approximately 1,300 light-years from Earth. It is a striking example of a dust cloud illuminated by starlight rather than by its own emission. At its center lies a young, hot star designated HD 200775, whose intense blue-white radiation reflects off surrounding interstellar dust grains. This scattering process preferentially reflects shorter wavelengths, giving the nebula its characteristic bluish hue, much like the mechanism that makes Earth’s sky appear blue.

The nebula spans roughly six light-years across and is embedded within a larger molecular cloud complex. Its structure reveals striking contrasts: bright filaments and wisps where dust strongly reflects starlight, interspersed with dark lanes where dense concentrations of material obscure illumination. Infrared observations have shown that the dust contains complex carbon-rich molecules, including polycyclic aromatic hydrocarbons (PAHs), which are thought to play a role in interstellar chemistry and may represent building blocks of more complex organic compounds.

Unlike emission nebulae, which glow due to ionized gas, the Iris Nebula remains primarily a reflection nebula because the radiation from its central star is not energetic enough to fully ionize the surrounding hydrogen gas. Instead, the nebula’s beauty lies in the interplay of light and shadow, highlighting the distribution of interstellar dust and providing astronomers with insights into the conditions of stellar nurseries". - Professor G.P.T Chat visiting astrophysicist at the Jodrell Plank Observatory.

Enlarged and cropped view of the spectacular Iris reflection Nebula

IC 5070 or the Pelican Nebula in modified SHO format

Ionization fronts and cold gas in the Pelican Nebula. Data Credit: PIRATE robotic telescope SHO filters. Mount Teide, Tenerife. telescope.org Open Observatories, Open University. Image credit: Pip Stakkert at the JPO..

"The Pelican Nebula is a goto target for Northern Hemisphere  summer astro-imagers and sits next to the North America Nebula NGC7000 in the constellation Cygnus. The above narrowband image shows the delicate interplay of light and shadow: the glowing plasma energized by young stars and the cold dark lanes marking where future stars are gestating. The visible filaments trace the ionization fronts—the boundaries between the ultraviolet-irradiated cavities and the shielded interiors of molecular clouds.

In effect, the above image is a portrait of cosmic evolution in progress: the raw interstellar medium being sculpted into stars, planetary systems, and eventually the building blocks of life itself". - Joel Cairo CEO of the Jodrell Plank Observatory.

The North America and Pelican Nebulae in the Constellation Cygnus. Image credit: Kurt Thrust at the JPO

"Our narrow band SHO image, captured with the PIRATE telescope, depicts IC 5070, more commonly known as the Pelican Nebula, a large emission nebula located in the constellation Cygnus, not far from its companion, the North America Nebula (NGC 7000). Both regions are part of an extended complex of ionized hydrogen gas (an H II region) that lies about 1,800 light-years away in the Orion Arm of our Milky Way galaxy.

What we have imaged is essentially a stellar nursery: a vast cloud of hydrogen, dust, and other trace elements undergoing active star formation. The striking forms in IC 5070—its ridges, filaments, and dark channels—arise from the interaction between intense ultraviolet radiation from nearby massive stars and the dense molecular cloud material.

Ionization and Emission

The gas in IC 5070 glows because young, hot O- and B-type stars in the region emit torrents of ultraviolet light.

This radiation strips electrons from surrounding hydrogen atoms, a process known as photoionization. When the electrons recombine with protons, they emit visible light—most notably in the red H-alpha line (656.3 nm). This is why narrowband astrophotography often reveals IC 5070 with a red or magenta dominance.

Dark Dust Lanes

The jagged black regions cutting through the glowing gas are dense molecular clouds of dust and cold gas.

These clouds absorb and scatter visible light, producing the intricate silhouetted structures that make the Pelican Nebula so recognizable. Within these dark regions, protostars are forming, hidden from optical wavelengths but detectable in infrared.

Stellar Feedback

The radiation pressure and stellar winds from massive young stars push against the molecular material, carving cavities, compressing clouds, and triggering further star formation at the boundaries of these regions.

This feedback loop is a defining characteristic of giant H II regions: they are both destroyers and creators—dissipating the nebula even as they seed new generations of stars.

Overall Context

IC 5070, along with NGC 7000, is part of a giant molecular cloud complex spanning several degrees of sky, visible in wide-field astrophotography, (see Kurt's above  image) as a grand tapestry of glowing hydrogen and sculpted dust.

Astronomers often study it as an analog for stellar nurseries in other galaxies, since its proximity gives us a clearer laboratory for understanding massive star formation and interstellar medium dynamics". -Kurt Thrust current Director of the  JPO and Professor G.P.T Chat visiting astrophysicist .

NGC 281 'The Pac-man' Nebula

 

NGC 281- Part of the Pac-man Nebula. Data Credit: PIRATE robotic telescope, SHO filters, Mount Teide, Tenerife. telescope.org. Open Observatories, Open University. Image Credit: Kurt Thrust.

The Constellation Cassiopeia (The big 'W' asterism in the Northern Sky)
A compilation - 3 pane, widefield image.
Captured with the Jodrell Plank Observatory's mini-rig : Canon 600d DSLR
with a 135mm F2 Samyang Lens all on a Star Adventurer EQ mount.
  - Image Credit: Pip Stakkert

" The weather remains poor on the East Coast and sadly Kurt has been laid low by an auto-immune disorder,consequentially, little astronomy has been pursued at the JPO. Kurt did however, enjoy an hour working upon the Pac-man data obtained via the PIRATE robotic scope on Tenerife". - Joel Cairo CEO of the JPO.

NGC 281 in detail

"The NGC 281 nebula, often nicknamed the Pacman Nebula due to its resemblance to the iconic video game character in optical images, is a large, active star-forming region located in the Perseus spiral arm of the Milky Way. Situated in the northern constellation Cassiopeia, this emission nebula lies approximately 9,200 light-years (2.8 kiloparsecs) from Earth. With an angular diameter of nearly 35 arcminutes—comparable to the size of the full Moon—it corresponds to a physical span of over 100 light-years across.

NGC 281 is classified as an H II region, a vast cloud of ionized hydrogen gas energized by the intense ultraviolet radiation from its embedded young stars. At its core lies the open star cluster IC 1590, which hosts a population of hot, massive O- and B-type stars. Among them, the O6 star HD 5005 is particularly dominant, providing much of the ionizing flux that causes the surrounding hydrogen gas to glow in vivid emission lines, especially the characteristic red Hα radiation.

The nebula’s structure is rich and complex, sculpted by stellar winds and radiation. Prominent features include dense Bok globules—cold, dark molecular clumps that appear as silhouettes against the luminous background. These globules are active nurseries where protostars are forming, their growth regulated by the interplay between self-gravity and external radiation pressure. Infrared observations from the Spitzer Space Telescope and more recent surveys with the James Webb Space Telescope (JWST) have revealed numerous young stellar objects (YSOs) and protostellar disks within NGC 281, highlighting its ongoing role as a cradle of stellar birth.

The nebula is also notable for being the site of significant molecular outflows and stellar feedback processes. Winds from the massive stars in IC 1590 compress nearby gas, triggering sequential star formation along the peripheries of the nebula—a process sometimes described as “collect and collapse.” This makes NGC 281 a textbook example for studying how massive stars regulate the evolution of their parent molecular clouds.

From an observational perspective, NGC 281 is accessible with modest amateur telescopes under dark skies, appearing as a faint glowing patch of nebulosity surrounding a small star cluster. Through long-exposure astrophotography, its intricate structure becomes clear, with reddish emission nebulae, dark dust lanes, and striking cavities carved by stellar activity.

In summary:

NGC 281 in Cassiopeia is a luminous emission nebula and star-forming complex, powered by the young cluster IC 1590. Spanning over 100 light-years, it contains dark Bok globules, active protostars, and striking examples of stellar feedback shaping the interstellar medium. Its combination of visual beauty and astrophysical richness has made it both a popular target for amateur astronomers and a significant object of study for professional astrophysics, particularly in the fields of star formation, stellar feedback, and nebular evolution". - Professor G.P.T Chat visiting astrophysicist at he Jodrell Plank Observatory.

Messier 31 revisited

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Messier 31 The Andromeda Galaxy Group. Altair Lightwave 66mm ED refractor and Canon 600d DSLR.
Image Credit Kurt Thrust.

"Our nearest spiral galaxy neighbour the Andromeda Galaxy is riding high in the Northern Hemisphere autumn sky. The weather has been far from kind and the JPO team has been laid low by a rather nasty virus which may be the latest variant of  Covid. Anyway, as the team has been wrapped up warm for a while, Kurt decided to reprocess this data captured in a previous year.

The above image shows the three galaxies M31 (the large central inclined spiral), M32 the elliptical galaxy (appears as a fuzzy spot on the upper edge of the M31 spiral) and M110 a dwarf elliptical galaxy ( just below and to the centre right of M31). 

So let Professor G.P.T. Chat, our visiting astrophysicist, compare and contrast these nearby galaxies (approximately 2.5 million light years distant) with our home Milky Way galaxy". - Joel Caio CEO of the Jodrell Plank Observatory.

Milky Way – Our Home Galaxy

The Milky Way is itself a barred spiral galaxy, somewhat smaller than M31. Its disk extends ~100,000–120,000 light-years, with a mass of about 1 trillion solar masses and a few hundred billion stars. Structurally, it resembles M31: both have stellar halos, bulges, bars, spiral arms, and satellite galaxies. In cosmic terms, the Milky Way is the second major member of the Local Group, and the future collision and merger of the Milky Way and M31 will reshape them into a single giant elliptical galaxy in several billion years.

M31 – The Andromeda Galaxy

Andromeda is the giant of this quartet. With a disk spanning about 220,000 light-years, it is roughly twice the diameter of the Milky Way. Its stellar population approaches one trillion, compared with the Milky Way’s 200–400 billion. In both size and luminosity, M31 slightly outclasses our own Galaxy, and it exerts enough gravitational pull to dominate the Local Group, which also contains the Milky Way and dozens of smaller galaxies.

• Diameter: ~220,000 light-years (about twice the Milky Way’s diameter).
• Mass: ~1.5 trillion solar masses.
• Stars: ~1 trillion.
• Luminosity: ~2.6 × 10¹⁰ solar luminosities.

Notes: A vast spiral galaxy with an extensive stellar halo and a large, bright disk. It dominates the Local Group both in size and gravitational influence.

M32 – Compact Elliptical

Placed against the scale of the Milky Way, M32 looks minuscule. With only ~3 billion stars in a body just 6,500 light-years across, it is smaller than even some of the Milky Way’s largest globular clusters when measured by diameter. Where the Milky Way’s spiral disk is rich in gas and dust and actively forming stars, M32 is stripped bare, almost entirely quiescent. Its compact, blazing core makes it bright for its size, but compared with the Milky Way, it is less than 1% as luminous.

• Diameter: ~6,500 light-years (tiny compared with M31).
• Mass: ~3 × 10⁹ solar masses.
• Stars: ~3 billion.
• Luminosity: ~3 × 10⁸ solar luminosities.

Notes: Dense and bright, especially in its central regions. Its outer stars and gas are thought to have been stripped by M31, leaving only the compact core we see today.

M110 – Dwarf Elliptical

M110 sits somewhere between M32 and the Milky Way in scale. Its 15,000–17,000 light-year span is still tiny compared with the Milky Way’s disk, and its ~10 billion stars are a mere fraction of the Milky Way’s population. Unlike M32, however, M110 retains some irregular features, dust, and evidence of star formation. It is a faint satellite, thousands of times less luminous than the Milky Way, but still large enough to stand as one of the more substantial dwarf galaxies in the Local Group.

• Diameter: ~15,000–17,000 light-years.
• Mass: ~1–2 × 10⁹ solar masses.
• Stars: ~10 billion.
• Luminosity: ~9 × 10⁸ solar luminosities.

Notes: More diffuse than M32, with some evidence of dust lanes and past star formation. Its structure is irregular compared with typical smooth ellipticals, likely reflecting tidal interaction with M31.

Comparative Perspective

M31 and the Milky Way are the two great spirals of the Local Group, differing mainly in scale (M31 being the larger).

M32 is a stripped-down remnant, a tiny elliptical companion of M31, utterly dwarfed by both the Milky Way and Andromeda.

M110 is a diffuse dwarf elliptical, more extended than M32 but still only a faint shadow of the Milky Way’s scale and richness.

Together, these four galaxies illustrate the hierarchy of galactic forms: two massive spirals shaping the Local Group, orbited by much smaller companions that bear the scars of their gravitational relationship with the giants.

The Approaching Collision

• The Milky Way and M31 are moving toward each other at about 110 km/s.

• In roughly 4–5 billion years, their outer halos will begin to overlap, triggering the first close passage.

• The collision will not be like two solid bodies smashing together; instead, stars will mostly pass by one another because of the vast spaces between them. But gas, dust, and dark matter halos will interact strongly, producing shocks, bursts of star formation, and tidal distortions.

The Merger

• After a series of close encounters, the Milky Way and M31 will merge into a single giant elliptical galaxy — sometimes nicknamed “Milkomeda” or “Milkdromeda.”

• This process will take several billion years to settle into a stable form. The final product will likely resemble today’s giant elliptical galaxies, with a vast stellar halo and little organized spiral structure.

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The Fate of M32

• M32, already stripped and compact, is tightly bound to M31.

• During the merger, it will almost certainly be swallowed whole by the combined Milky Way–Andromeda system.

• Its compact nature means it will survive tidal forces fairly well, likely ending as a dense nucleus or central star cluster within the merged galaxy.

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The Fate of M110

• M110, being larger and more diffuse, will fare differently.

• It may be torn apart by tidal forces during the merger, with its stars spread out into long stellar streams and absorbed into the halo of the new galaxy.

• Some fraction of its stars may survive as a remnant dwarf core, but it will be much more disrupted than M32.

The Long-Term Result

• The Local Group will transform from a system dominated by two spirals into a single elliptical super-galaxy, containing perhaps 2 trillion stars.

• The smaller companions, including M32, M110, and the Milky Way’s own satellites (like the Magellanic Clouds), will either be absorbed into the giant remnant or left orbiting as faint shells and streams.

• From a cosmic distance, the Local Group will eventually resemble a single luminous elliptical galaxy, drifting in relative isolation as the universe continues to expand.

 In short: M31 and the Milky Way will merge into one great elliptical galaxy; M32 will likely become part of its core, while M110 will be torn apart and assimilated into its halo.

Messier 71, the easy to miss Globular Star Cluster.

 

The Globular Star Cluster Messier 71. Data Credit: PIRATE robotic telescope, BVR filters. Mount Teide, Tenerife. telescope.org. Open Observatories, Open University. Image Credit: Kurt Thrust at the JPO.

" Messier 71, sits in the  small constellation Sagitta the arrow. This area of the sky is associated with the plane of the Milky Way's disc and is literally awash with stars when viewed with binoculars or a widefield telescope. Messier 71 being a small globular cluster, is therefore easy to miss within this plethora of stars. As I processed the data and watched the above image materialise, I  was amazed at how many stars I could see!" - Kurt Thrust current Director of the Jodrell Plank Observatory.

A Comparative Report on the Globular Cluster Messier 71

Messier 71 (M71), located in the small constellation Sagitta, is one of the more unusual globular clusters in the Messier catalogue. At a distance of roughly 13,000 light-years, it appears as a loose, irregular grouping of stars through modest telescopes, and for much of the 19th and 20th centuries it was debated whether M71 was in fact a globular or a rich open cluster. Advances in stellar photometry and spectroscopy have since clarified its nature: M71 is a genuine globular cluster, though a relatively low-mass, metal-rich, and loosely concentrated one. Comparison with the more archetypal clusters Messier 13 (M13), Messier 3 (M3), and Messier 4 (M4) underscores the peculiarities of M71.

Messier 13, the “Great Hercules Cluster,” is perhaps the best-known northern globular cluster. It contains several hundred thousand stars in a compact halo over 140 light-years across, with a dense, bright core that exemplifies the globular class. By contrast, M71 contains perhaps only 20,000–50,000 stars spread across a mere 27 light-years. Its lower concentration and modest size explain why early observers mistook it for an open cluster. Whereas M13 presents a dazzling display of densely packed stars and exhibits a well-defined horizontal branch, M71 has only a stubby red giant branch and no extended blue horizontal branch, making its stellar population appear more subdued.

Messier 3 provides another instructive comparison. Situated in Canes Venatici, M3 is among the richest and most extensively studied globular clusters, hosting over half a million stars and more than 200 known variables, including numerous RR Lyrae stars. Its variable population and prominent horizontal branch have made it a cornerstone for calibrating stellar evolution models. M71, on the other hand, lacks a significant RR Lyrae population and is chemically distinct. Its relatively high metallicity ([Fe/H] ≈ –0.8) is atypical for globular clusters, especially when contrasted with the metal-poor stars of M3. This implies that M71 formed later in the Galactic halo’s history, from interstellar gas already enriched with heavier elements, and therefore represents a younger evolutionary epoch within the globular cluster system.

Messier 4, in Scorpius, provides a comparison from the opposite end of the structural spectrum. Though M4 is one of the closest globular clusters to Earth (about 7,200 light-years), and not especially rich in stars compared to giants like M3 or M13, it nevertheless displays a clear globular morphology with a strong central concentration. M4 is notable for its rich population of evolved stars, a well-populated horizontal branch, and chemical peculiarities linked to multiple stellar generations. In terms of mass and richness, M4 is closer to M71 than are M13 or M3, yet it retains the compact, globular appearance that M71 lacks. The difference lies primarily in concentration: M4 is compact and easily recognisable as a globular cluster, while M71 is diffuse, giving it a hybrid appearance that complicated its classification.

In conclusion, M71 highlights the diversity within the globular cluster family. It lacks the immense stellar density and archetypal morphology of Messier 13, the vast population and chemical simplicity of Messier 3, and even the structural clarity of Messier 4. Instead, it is a relatively loose, metal-rich, and moderately populated globular cluster, whose transitional characteristics blur the distinction between open and globular clusters. Its study provides valuable insight into the chemical enrichment of the Galaxy and the lower-mass limits of globular cluster formation.

Professor G.P.T. Chat visiting astrophysicist at the Jodrell Plank Observatory.

The Wizard of Cepheus NGC 7380

 

NGC 7380 The Wizard Nebula in the constellation Cepheus.
Data Credit: PIRATE robotic telescope, SHO filters. Mount Teide.  Tenerife
telescope.org. Open Observatories, Open University.
Image Credit Pip Stakkert at the JPO.

Annotated version of the image. Credit: astrometry.net.

" Pip has taken his own view on the final colours used in this narrow band image. The original data was captured with SHO filters which were mapped to RGB. Hydrogen alpha emission is particularly strong in NGC7380 and therefore 'green' predominates. Pip has adjusted the colour intensity to bring out the 'red' (Sulphur ll) and  blue (Oxygen lll) datas".

I should like to thank Alan Waffles and Waffles Construction Ltd for coming at short notice, to batten down one of the rooves at the JPO, prior to the arrival of high winds and heavy rain. In the event, the storm  wasn't as bad as was predicted and no damage was sustained".- Joel Cairo CEO of the Jodrell Plank Observatory.

" I asked Karl Segin, the JPO's outreach officer and Professor G.P.T Chat our visiting astrophysicist, to put together a brief description of the Wizard Nebula. I hope, like me, you find this enigmatic object interesting" - Kurt Thrust current Director of the Jodrell Plank Observatory.

 NGC 7380: The Wizard Nebula

NGC 7380, commonly referred to as the Wizard Nebula, is a young open star cluster surrounded by an extensive emission nebula. It is located in the constellation Cepheus, at an estimated distance of about 7,200 light-years from Earth. The nebula spans approximately 100 light-years across, making it a prominent star-forming region visible in long-exposure astrophotography. Its popular name arises from the resemblance of the illuminated gas clouds to a robed, wizard-like figure when viewed in visible light images.

The central feature of NGC 7380 is the open star cluster, cataloged by Caroline Herschel in 1787 and later added to William Herschel’s general catalog. This cluster is only a few million years old and contains a rich population of hot, massive O-type and B-type stars, whose strong ultraviolet radiation energizes the surrounding hydrogen gas. The nebula itself is classified as an H II region, a vast cloud of ionized hydrogen where new stars are actively forming.

The process that created the Wizard Nebula follows the standard sequence of stellar nursery evolution. A large molecular cloud of hydrogen and trace elements began to collapse under the influence of its own gravity. Local density enhancements triggered pockets of rapid star formation. As the most massive stars ignited nuclear fusion in their cores, they released intense radiation and powerful stellar winds. This feedback carved cavities in the surrounding cloud, compressing some regions while dispersing others. The result is the sculpted appearance of bright ridges, dark dust lanes, and filamentary structures that give the nebula its dramatic shape.

Embedded within the nebula are protostars and young stellar objects still accreting matter from their natal environment. Observations in infrared wavelengths, which can penetrate the obscuring dust, have revealed numerous stars still in their formative stages. Some of these may eventually join the cluster, while others will disperse as the nebula continues to evolve.

The fate of NGC 7380 will be shaped by its most massive stars. Within a few million years, these stars will end their lives as supernovae, enriching the interstellar medium with heavy elements and possibly triggering further rounds of star formation in the region. Over time, the gas and dust of the Wizard Nebula will disperse into the wider galaxy, leaving behind the open cluster, which itself will gradually lose cohesion due to gravitational interactions.

Today, NGC 7380 is an object of great interest to both professional astronomers and astrophotographers. It provides a natural laboratory for studying the physics of star formation, stellar feedback, and nebular evolution. Its striking appearance, combined with its role as an active stellar nursery, makes the Wizard Nebula one of the most evocative examples of the dynamic processes shaping our Milky Way galaxy.