Thursday, 26 June 2025

The Tadpoles aka IC410 in Seestar S30 RGBSHO format.

 

The Tadpoles (centre right) Seestar  S30 (RGB SHO format).
Image credit: Pip Stakkert and Kurt Thrust.

"Mid-summer at the Jodrell Plank Observatory in Lowestoft, the nights are only truly dark for two or three hours, so June is the month, when we maintain our equipment, make new bits of kit and learn new skills. Kurt since returning from holiday, has been busy making a new solar white light filter for the 125mm Meade refractor and designing a transmission grating for the Seestar S30. Pip has been hard at study investigating the use of SIRIL software as a preprocessing first stage in the creation of deepsky images like the one above. In future we shall be using SIRIL to undertake initial stretching of data and the photometric calibration of colour in all our imagery. We hope you all approve!" - Joel Cairo CEO of the Jodrell Plank Observatory.

Widefield view of IC410 and NGC1893
data captured with the Seestar S30 robotic telescope

"Nestled deep in the rich star fields of the constellation Auriga lies a compelling region of stellar birth and evolution known as IC 410, a glowing emission nebula that encapsulates the dynamic story of cosmic creation. This region, set approximately 12,000 light-years from Earth, is more than just a celestial spectacle; it is a living laboratory of astrophysical processes shaped by the energetic lives of massive stars. At the heart of this nebula resides the young open star cluster NGC 1893, whose powerful influence has sculpted the surrounding clouds of gas and dust into mesmerizing structures, including the enigmatic “Tadpoles” of IC 410.

The Nebula IC 410

IC 410 is classified as an emission nebula, a vast cloud of ionized hydrogen gas (H II region) that glows in visible light as it is energized by the ultraviolet radiation of nearby hot stars. The reddish hues that dominate images of IC 410 are primarily due to the H-alpha emissions from excited hydrogen atoms, giving the nebula its distinctive fiery appearance. Extending over roughly 100 light-years, the nebula is part of a larger region of ongoing star formation.

IC 410’s radiance is not uniform. It contains darker dust lanes, filamentary structures, and bright knots—evidence of complex interactions between stellar winds, radiation pressure, and turbulent gas flows. This interplay creates shock fronts and compression zones, setting the stage for future generations of star formation.

Star Cluster NGC 1893

Embedded within IC 410, the open cluster NGC 1893 provides the energy and dynamism that drives much of the nebula’s current activity. Composed of several thousand stars, NGC 1893 is a relatively young cluster, estimated to be around 4 million years old. Among these stars are numerous hot, massive O- and B-type stars whose intense radiation and stellar winds exert a powerful influence on the surrounding interstellar medium.

The feedback from these massive stars—both through radiation pressure and mechanical outflows—has a dual effect. It can erode and disperse the surrounding gas, halting star formation in some areas, while simultaneously compressing other regions, triggering the collapse of gas clouds and the birth of new stars. This process, known as triggered star formation, is believed to play a key role in shaping IC 410’s morphology and fueling its continued evolution.

The Tadpoles of IC 410

Among the most visually and scientifically intriguing features within IC 410 are the structures known as the “Tadpoles.” These are elongated, cometary-shaped clouds of gas and dust that appear to be swimming through the glowing plasma of the nebula. There are two primary Tadpoles, officially designated as Sim 129 and Sim 130, named after astronomer Colin T. Simmons who cataloged them.

Each Tadpole is several light-years in length and has a dense, globule-like head followed by a trailing tail. These features are aligned in a direction that points away from the central cluster, suggesting they have been sculpted by the intense stellar winds and radiation emanating from the hot stars of NGC 1893. The leading edges of the Tadpoles are shielded from the full brunt of the radiation, allowing gas to survive in denser form, while the tails are formed as material is photoevaporated and swept back.

Observations in the infrared and radio wavelengths have revealed signs of star formation occurring within the heads of the Tadpoles. These proto-stellar objects, embedded in dense molecular material, suggest that even in the harsh environment of a bright emission nebula, pockets of gas can remain stable enough to collapse under their own gravity and give rise to new stars.

Formation and Evolutionary Processes

The formation of IC 410 and NGC 1893 likely began as a giant molecular cloud collapsed under gravitational instability, forming the first generation of massive stars that now dominate the cluster. The intense radiation and mechanical energy from these stars initiated a feedback loop that shaped the surrounding gas into arcs, filaments, and pillar-like structures such as the Tadpoles.

The Tadpoles are thought to be remnants of denser clumps of gas that were originally part of the molecular cloud. As the surrounding material was eroded away, these clumps resisted dispersal due to their higher density. Over time, they were shaped by the erosive forces of UV radiation, developing the characteristic head-tail morphology seen today.

Astronomers have used data from telescopes such as Spitzer, Chandra, and Hubble, as well as ground-based observatories, to study IC 410 across multiple wavelengths. X-ray emissions detected by Chandra reveal high-energy processes and young, embedded stars, while infrared observations from Spitzer show warm dust and the earliest stages of stellar formation.

Overview

IC 410, together with the open cluster NGC 1893 and the Tadpoles Sim 129 and Sim 130, represents a dynamic example of the cycle of stellar birth and feedback. The interaction between massive stars and their environment drives both destruction and creation, sculpting the nebula and triggering new generations of stars in a cosmic relay that spans millions of years.

In studying regions like IC 410, astronomers gain crucial insights into the processes that govern star formation across the galaxy. These structures not only illuminate the physics of interstellar matter and radiation, but also echo the early conditions under which our own Sun and solar system may have formed, making IC 410 not just a window into the distant cosmos, but a reflection of our own origins".

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

Sunday, 22 June 2025

M16 and the Pillars of Creation

 

M16 and the Pillars of Creation
 - Data Credit: telescope.org, Open Observatories, Open University.
Image Credit: Kurt Thrust at the Jodrell Plank Observatory.



" The 'Pillars of Creation' may be seen virtually at the centre of this image. The data was curated from both the COAST and PIRATE robotic telescopes using SHO filters on Mount Teide,  Tenerife as programmed by Kurt. Nebulae shown red relate to Sulphur11, shown green or white relate to Hydrogen alpha and  shown blue relate to Oxygen111. There are also a lot of dark dust clouds in this image" - Joel Cairo CEO of the Jodrell Plank Observatory. 

Messier 16 
- captured with the Seestar S30 in EQ mode and Neb filter. 60x30 second subs.
Credit: Kurt Thrust.

" Messier 16 is an interesting nebulous region in the constellation Serpens. Sadly, Messier 16  aka the Eagle Nebula never gets that high above our southern horizon at the Jodrell Plank Observatory. The little Seestar provides a less detailed but wider view (Field of vision - FOV) than the robotic telescopes on Mount Teide. So all three help to provide a better representation of this interesting part of the night sky. Our visiting astrophysicist, G.P.T Chat, will provide further details". - Kurt Thrust current Director of the Jodrell Plank Observatory.

" Messier 16 (M16), also known as the Eagle Nebula, is a young open star cluster embedded within a diffuse emission nebula located in the constellation Serpens, approximately 7,000 light-years from Earth. The nebula is most famous for containing the "Pillars of Creation", a striking region of active star formation made famous by the Hubble Space Telescope.


1. Structure and Components of Messier 16

a. Open Star Cluster (NGC 6611)

Age: Approximately 1–2 million years old.


Stellar Population: Contains several thousand stars, including massive O-type and B-type stars.


These stars are young, hot, and very luminous, providing the energy that excites the surrounding nebula.


The ultraviolet radiation from these massive stars plays a critical role in shaping the surrounding nebula.


b. Emission Nebula

Type: H II region (a cloud of ionized hydrogen).


The emission nebula is a region of interstellar gas and dust that is ionized by high-energy UV radiation from the hot stars of NGC 6611.


As the hydrogen atoms recombine, they emit light in specific emission lines, especially the H-alpha line, giving the nebula its characteristic reddish glow in optical wavelengths.


2. Glowing Nebula: Physical Mechanism

The glow of the Eagle Nebula arises primarily from photoionization:


High-energy UV photons from O- and B-type stars ionize the surrounding hydrogen gas.


Electrons recombine with protons, and during this recombination, hydrogen emits photons, particularly in the Balmer series (notably H-alpha at 656.3 nm).


This process creates the glowing reddish-pink emission seen in visible light.


Additional emissions also come from ionized oxygen ([O III], giving a greenish hue) and sulfur ([S II]), especially in narrowband imaging.


3. Dark Pillars and Clouds

The dark, finger-like features known as the Pillars of Creation are dense molecular clouds composed of cold gas and dust.


a. Nature of the Pillars

These are evaporating gaseous globules (EGGs), where regions of dense gas resist the ionizing radiation longer than their surroundings.


They are several light-years long and are sites of ongoing star formation.


Protostars can be embedded within these pillars, slowly accreting material from their surroundings.


b. Erosion by Radiation and Winds

The edges of the pillars are illuminated by the intense UV radiation from nearby massive stars.


Photoevaporation occurs at the surfaces: UV photons heat and ionize the outer layers, causing the gas to stream away.


Stellar winds and radiation pressure further sculpt and compress these clouds, triggering gravitational collapse in some regions—leading to new star formation (a process called radiation-driven implosion).


4. Astrophysical Significance

M16 is a classic example of feedback in star formation: newly formed massive stars influence their environment, possibly triggering or inhibiting further star formation.


The Eagle Nebula's structure gives insights into early stellar evolution, molecular cloud dynamics, and interactions between stars and the interstellar medium (ISM).


Summary

Feature Description

Distance ~7,000 light-years

Type Open cluster with emission nebula

Main Components NGC 6611 (young stars), H II region, molecular pillars

Ionization Source UV radiation from hot, massive stars

Nebular Glow Hydrogen recombination (H-alpha), [O III], [S II] lines

Dark Clouds Dense, cold molecular gas and dust (EGGs, pillars)

Activity Active star formation, photoevaporation, feedback mechanisms


M16 remains one of the most studied star-forming regions in our galaxy, particularly due to the "Pillars of Creation", which vividly illustrate the complex processes driving the birth and evolution of stars". - Professor G.P.T. Chat 











Tuesday, 17 June 2025

Messier 4 in the constellation Scorpius

 

Messier 4 captured with the Seestar S30
from Giardini Naxos Sicily in June 2025

Messier 4 (M4), located in the constellation Scorpius, is a prominent example of a globular star cluster. When described comparatively with other globular clusters, several features stand out:


1. Proximity: Closest Known Globular Cluster

  • M4 is the closest globular cluster to Earth, at a distance of about 7,200 light-years.

  • In contrast, many other well-known clusters, such as M13 in Hercules (approx. 22,200 light-years) or Omega Centauri (approx. 15,800 light-years), are much farther away.

  • This proximity makes M4 easier to study in detail, especially with ground-based telescopes.


2. Size and Brightness: Modest Compared to Giants

  • M4 spans about 75 light-years in diameter, which is relatively small for a globular cluster.

  • Its apparent magnitude is +5.9, making it visible to the naked eye under dark skies.

  • However, compared to Omega Centauri, which is the largest and brightest globular cluster visible from Earth and contains several million stars, M4 is more modest, containing about 100,000 stars.


3. Core Structure: Loosely Concentrated

  • M4 has a Class IX concentration on the Shapley–Sawyer scale (I = most concentrated, XII = least).

  • This means its core is relatively loose and less dense than those of more tightly packed clusters like M15 (Class IV) or M30 (Class II).

  • As a result, M4 does not show the same dramatic central condensation as these denser clusters.


4. Stellar Content: Old but with Peculiarities

  • Like other globular clusters, M4 is very old, with an estimated age of about 12.2 billion years.

  • Notably, M4 contains white dwarf stars with well-determined cooling ages, which have been used to help constrain the age of the Milky Way.

  • It also contains millisecond pulsars and variable stars, similar to many other globular clusters, but its proximity makes these objects easier to resolve.


5. Horizontal Branch Morphology: Red-Dominated

  • M4 has a redder horizontal branch than some other clusters, such as M13, which has a bluer and more extended horizontal branch.

  • This difference relates to its metallicity (M4 is relatively metal-rich for a globular cluster, with [Fe/H] ≈ –1.1), affecting the evolution and appearance of its stars.


Summary of Comparisons

PropertyM4M13Omega CentauriM15
Distance (light-years)~7,200~22,200~15,800~33,600
Stars~100,000~300,000~10 million~500,000
Core ConcentrationLoose (Class IX)Intermediate (Class V)Dense (Class III)Very Dense (Class IV)
Apparent Magnitude+5.9+5.8+3.7+6.2
Metallicity [Fe/H]~–1.1~–1.5~–1.6~–2.3
Notable FeaturesClosest; white dwarfs studiedBlue HB; well studiedLargest GC; multiple popsVery old; dense core

Final Notes:

Messier 4 stands out for its closeness, modest size, and observational accessibility, making it a crucial target for studies of stellar evolution and Galactic history. While not as massive or dense as some other clusters, its unique proximity allows astronomers to resolve individual stars with greater precision than in nearly any other globular cluster. - Joel Cairo CEO of the Jodrell Plank Observatory

Combined image showing the relative star densities
 of M13 (left) and M4 (Right) (not to size scale)