Carbon Stars - La Superba - Low resolution Spectral Profile

 

Kurt loves a bit of stellar spectroscopy and encouraged by his friend and sometimes astronomical collaborator, Professor GP, he captured the spectral data for the amazing Carbon Star - La Superba, using the JPO's 127mm. apo-refractor and a spectrometer designed and 3d printed by our on-site engineer Jolene McSquint -Fleming in the observatory's clean room'. - Joel Cairo CEO of the Jodrell Plank Observatory.

For an absolutely fantastic image of this 'very red star' follow the link.

https://apod.nasa.gov/apod/ap081218.html

"For an explanation of this 'cool', in every sense of the word, star, I asked the JPO's visiting physicist, G.P.T. Chat Phd, to describe its general features and spectral details using a comparative methodology" - Kurt Thrust current Director of the Jodrell Plank Observatory.

La Superba and Stellar Evolution: A Comparative Analysis on the Hertzsprung-Russell Diagram

Introduction

Stars are the fundamental building blocks of galaxies, and their life cycles reflect the underlying physics that governs the universe. Among the many types of stars observed, carbon stars represent a fascinating late stage in stellar evolution. One of the most prominent and well-studied carbon stars is La Superba, also known as Y Canum Venaticorum. This essay explores La Superba's characteristics in detail and places it in context with several other well-known stars using the Hertzsprung-Russell (H-R) diagram.

La Superba: An Overview

La Superba is located in the constellation Canes Venatici, visible in the northern hemisphere, especially during spring. Its coordinates (J2000 epoch) are:
- Right Ascension: 12h 45m 07.83s
- Declination: +45° 26′ 24.9″

It lies approximately 710 light-years from Earth and is classified as a carbon-rich red giant — one of the brightest of its kind visible to the naked eye. As a semi-regular variable star, its apparent magnitude varies from +4.9 to +6.3.

La Superba's physical parameters make it particularly interesting:
- Temperature: ~2,750 K
- Luminosity: ~9,000 L☉ (9000 x Sun's luminosity)
- Radius: ~400–500 R☉ (400 to 500 x Sun's radius)

It is a C-type (carbon) star, having undergone internal helium burning via the triple-alpha process, which produces carbon that is brought to the surface through convective dredge-up. This enrichment gives rise to a spectrum rich in carbon molecules, including C₂ (Swan bands), CN, and CH. These features result in deep molecular absorption bands, giving the star a very red appearance and making it a textbook example of a cool, evolved star on the Asymptotic Giant Branch (AGB).

Spectral Features

La Superba’s spectral type is typically classified as C6,2e in the revised carbon star classification system. It exhibits strong molecular absorption features and sometimes weak emission lines like H-alpha during pulsation events. The absence of oxygen-bearing molecules like TiO, common in M-type giants, highlights the dominance of carbon chemistry in its atmosphere.

Position on the H-R Diagram

The Hertzsprung-Russell diagram plots stars by their luminosity (vertical axis) and surface temperature (horizontal axis, decreasing rightward). La Superba occupies the upper-right portion of the H-R diagram — a region dominated by cool, highly luminous red giants and supergiants.

To provide comparative context, several other prominent stars are also plotted:
- The Sun – A G-type main sequence star with a surface temperature of 5,778 K and luminosity of 1 L☉.
- Deneb – A luminous blue-white supergiant (~8,500 K, 196,000 L☉).
- Sirius – A bright A-type main-sequence star (~9,940 K, 25.4 L☉).
- Arcturus – An orange giant (~4,286 K, 170 L☉).
- Capella – A system of G-type giants (~5,700 K, 78.7 L☉).
- Betelgeuse – A red supergiant (~3,500 K, 126,000 L☉).
- Castor – An A-type star (~10,100 K, 52.4 L☉).
- Pollux – An orange giant (~4,865 K, 43 L☉).
- Vega – A well-known A-type main-sequence star (~9,602 K, 40.1 L☉).

These stars cover a range of spectral types and evolutionary stages, allowing us to place La Superba within the broader context of stellar evolution.

H-R Diagram

Conclusion

La Superba serves as a striking example of late stellar evolution and highlights the diversity of stars when viewed through the lens of temperature and luminosity. Its placement on the H-R diagram underscores the dramatic changes stars undergo during their lifespans. Comparing La Superba with other well-known stars reveals the full spectrum of stellar development — from main-sequence hydrogen burners to evolved giants and future white dwarfs". - G.P.T. Chat Phd visiting physicist at the Jodrell Plank Observatory 

Globular star cluster Messier 3 or NGC 5272

 

Messier 3 Credit: Kurt Thrust - Seestar S30 in EQ mode.
Image cropped from Seestar widefield FOV.

"Messier 3 (M3), also known as NGC 5272, is a globular star cluster located in the northern constellation Canes Venatici. It is one of the brightest and most well-studied globular clusters in the sky.

Location and Observational Data

• Right Ascension: 13h 42m 11.62s

• Declination: +28° 22′ 38.2″

• Distance from Earth: ~33,900 light-years (10.4 kpc)

• Distance from Galactic Center: ~38,800 light-years (11.9 kpc)

• Position relative to Galactic Plane: ~31,600 light-years (9.7 kpc) above

• Constellation: Canes Venatici

• Apparent Magnitude: 6.39

• Apparent Size: 18 arcminutes

Physical Characteristics

• Estimated Age: ~11.4 billion years

• Mass: ~450,000 solar masses

• Radius: ~103 parsecs (335.9 light-years)

• Tidal Radius: ~113 parsecs (370 light-years)

• Absolute Magnitude: -8.93

• Metallicity ([Fe/H]): -1.34 dex

• Spectral Type: F2 (overall cluster classification)

Star Population and Variability

• Total Stars: ~500,000

• Variable Stars: 274 known, including 133 RR Lyrae variables

• Brightest Stars: Magnitude ~12.7

• Average Brightness of 25 Brightest Stars: ~14.23 mag

Discovery and Historical Significance

• Discovered by: Charles Messier on May 3, 1764

• First mistaken for: A nebula without stars

• Resolved into stars by: William Herschel in 1784

• Notable for: Having the highest number of variable stars among known globular clusters

The uncropped widefield image from the Seestar S30 post processed mainly using Affinity Photo 

Messier 3 is a fascinating object for astronomers due to its rich stellar population and high concentration of variable stars. Its isolation from the galactic plane makes it an excellent target for studying globular cluster evolution. Given your curiosity about astronomy, George, I imagine you’d appreciate the intricate details of its stellar dynamics! Would you like to explore how its variable stars contribute to distance measurements in astrophysics?

Globular star clusters like Messier 3 (M3) are some of the oldest stellar structures in the universe, forming during the early epochs of galaxy evolution. Their formation is still an area of active research, but here’s a breakdown of the leading theories and processes involved:

Formation Process

1. Primordial Collapse:

   • Globular clusters likely formed from massive gas clouds in the early universe, collapsing under gravity.

   • These clouds were enriched with low-metallicity gas, meaning they contained mostly hydrogen and helium, with very few heavier elements.

2. Rapid Star Formation:

   • The gas cloud underwent intense bursts of star formation, leading to the creation of hundreds of thousands of stars in a short period.

   • Unlike open clusters, globular clusters formed all at once, rather than gradually over time.

3. Gravitational Binding:

   • The stars remained gravitationally bound due to their high density and mutual attraction.

   • This led to the spherical shape characteristic of globular clusters.

4. Galactic Influence:

   • Many globular clusters formed outside the main disk of galaxies, possibly in dwarf galaxies or as remnants of galactic mergers.

   • Over time, they were captured by larger galaxies like the Milky Way.

5. Long-Term Evolution:

   • As globular clusters age, stellar interactions cause some stars to migrate outward while others fall toward the core.

   • Blue stragglers, a peculiar type of star found in globular clusters, may result from stellar collisions or mergers.

Why Are They So Old?

• The stars in globular clusters are typically Population II stars, meaning they formed early in the universe’s history.

• Their low metallicity suggests they originated before significant amounts of heavier elements were synthesized by supernovae.

• The lack of new star formation in globular clusters is due to the absence of gas, which was either used up or expelled early in their history.

M3, like other globular clusters, provides a window into the early universe, helping astronomers understand galaxy formation and stellar evolution. Given your curiosity about astronomy, George, I imagine you’d appreciate how these clusters serve as cosmic fossils! Would you like to explore how their dynamics influence galactic evolution?

Globular star clusters like Messier 3 (M3) are some of the oldest stellar structures in the universe, forming during the early epochs of galaxy evolution. Their formation is still an area of active research, but here’s a breakdown of the leading theories and processes involved:

Formation Process

1. Primordial Collapse:

   • Globular clusters likely formed from massive gas clouds in the early universe, collapsing under gravity.

   • These clouds were enriched with low-metallicity gas, meaning they contained mostly hydrogen and helium, with very few heavier elements.

2. Rapid Star Formation:

   • The gas cloud underwent intense bursts of star formation, leading to the creation of hundreds of thousands of stars in a short period.

   • Unlike open clusters, globular clusters formed all at once, rather than gradually over time.

3. Gravitational Binding:

   • The stars remained gravitationally bound due to their high density and mutual attraction.

   • This led to the spherical shape characteristic of globular clusters.

4. Galactic Influence:

   • Many globular clusters formed outside the main disk of galaxies, possibly in dwarf galaxies or as remnants of galactic mergers.

   • Over time, they were captured by larger galaxies like the Milky Way.

5. Long-Term Evolution:

   • As globular clusters age, stellar interactions cause some stars to migrate outward while others fall toward the core.

   • Blue stragglers, a peculiar type of star found in globular clusters, may result from stellar collisions or mergers.

Why Are They So Old?

• The stars in globular clusters are typically Population II stars, meaning they formed early in the universe’s history.

• Their low metallicity suggests they originated before significant amounts of heavier elements were synthesized by supernovae.

• The lack of new star formation in globular clusters is due to the absence of gas, which was either used up or expelled early in their history.

M3, like other globular clusters, provides a window into the early universe, helping astronomers understand galaxy formation and stellar evolution. Given your curiosity about astronomy, George, I imagine you’d appreciate how these clusters serve as cosmic fossils! Would you like to explore how their dynamics influence galactic evolution?

How do globular clusters impact galactic evolution?

Globular clusters play a significant role in the evolution of galaxies, influencing their structure, dynamics, and star formation history. Here’s how:

1. Galactic Halo Formation and Enrichment

• Globular clusters are among the oldest stellar systems, forming early in a galaxy’s history.

• Their low metallicity suggests they originated before significant enrichment by supernovae.

• As they evolve, they contribute heavy elements to the interstellar medium, enriching future generations of stars.

2. Stellar Dynamics and Galactic Structure

• Globular clusters orbit within a galaxy’s halo, often following highly elliptical paths.

• Their gravitational interactions help shape the galactic potential, influencing the motion of stars and dark matter.

• Some clusters are disrupted over time, spreading stars throughout the halo.

3. Galactic Mergers and Evolution

• During galaxy mergers, globular clusters can be captured by the larger galaxy.

• This process helps trace the assembly history of galaxies, revealing past interactions.

• Some clusters may originate from dwarf galaxies that were absorbed by larger galaxies.

4. Black Hole and Dark Matter Studies

• Some globular clusters contain intermediate-mass black holes, providing insights into black hole formation.

• Their motions help astronomers study the distribution of dark matter in galaxies.

5. Star Formation and Feedback

• While globular clusters no longer form new stars, their stellar winds and supernovae influence surrounding gas.

• This feedback can regulate star formation in the galaxy.

Globular clusters like Messier 3 serve as cosmic fossils, preserving information about the early universe and galaxy formation." 

- Charlie Server - Copilot at the Jodrell Plank Observatory

Interacting Galaxies NGC 5194 (Messier 51) and NGC 5195

 

NGC 5194 and NGC 5195. Image Credit: Pip Stakkert - Jodrell Plank Observatory. Data Credits: telescope.org, Open Observatories, Open University and Jodrell Plank Observatory. 

"The  interacting galaxies, known as Messier 51 or The Whirlpool, ride high in the late spring Northern Hemisphere sky, and in the constellation Canes Venatici. This pair of gravitationally interacting galaxies are some 31 million light years distant and the larger of the two is approximately 77,000 light years across. M51 was the first galaxy to be identified as having a spiral structure in 1845 by Lord Rosse from his observatory in Ireland.

We first pointed the Jodrell Plank Observatory's little Seestar S30 at  this galactic pair and thought how small these huge galactic structures looked when imaged with a telescope having a large field of vision.

Uncropped and stacked image downloaded from the Seestar S30.
Credit: Pip Stakkert.

We decided to use the PIRATE robotic telescope on Mount Teide Tenerife to capture M 51 and apply the data, imaged in white light and hydrogen alpha wavelengths, as a luminance channel  for the colour data we captured with the Seestar S30. The Seestar has an aperture of 30mm and the PIRATE telescope has an aperture of 600mm. So our image is a veritable 'little and large' collaboration. The two data sets were combined using the excellent and venerable software 'Registar'.

An interesting feature of both our above images is, the 'tidal feature', or northwest plume of gas emanating from the galactic centre of the larger NGC 5194 and extending some 140,000 light years to NGC 5195.  Close inspection of the top combined image shows a burst of star formation underway towards the the centre of NGC 5194" - Joel Cairo CEO of the Jodrell Plank Observatory (The Uk's most Easterly Astronomical Observatory).
 

Messier 87 and Virgo A

 

Messier 87 in the Constellation Virgo. PIRATE robotic Telescope Mount Teide, BVR filters, Hydrogen alpha filter  and Clear filter combined. Over-layed with Ultra violet data from the GALEX space Telescope.  Data Credits: telescope.org, Open Observatories, Open University, Astrometry net and NASA.
Image Credit: Pip Stakkert Jodrell Plank Observatory.

Annotated version M87: Credit Astrometry net.

Annotated and enlarged section of the galaxy core
to better show the plasma jet. Image credit: Kurt Thrust.

"Pip Stakkert combined the data from these two research grade telescopes to show the jet of energetic plasma issuing from the galaxy's massive central black hole and extending 4900 light years outwards. You can just see the jet at the centre of the large elliptical galaxy at approximately 10 -o'- clock position.

The plasma jet from the core of M87 issues from the supermassive black hole at its center. This black hole, which was famously imaged by the Event Horizon Telescope, is actively accreting matter. As material falls toward the black hole, some of it gets caught in powerful magnetic fields and is ejected outward at nearly the speed of light, forming a relativistic jet.

These jets are powered by the immense gravitational and electromagnetic forces near the black hole. The plasma is accelerated along magnetic field lines, creating a highly energetic stream that extends thousands of light-years into space. Observations suggest that the jet is composed of charged particles, primarily electrons, moving at relativistic speeds, which makes it a strong source of radio and X-ray emissions.

The elliptical galaxy Messier 87 is thought to contain more than a trillion stars, is almost spherical having a diameter of 120,000 light years and is over 50 million light years away. With an apparent magnitude of 9.6 it is visible as a small smudge of light through a small telescope. It can be found in the sky within the boundaries of the constellation Virgo. It is visible in our images as a large ball of diffuse light with a bright central core. The jet can be seen emanating from this core. M87 is too far away to make out any of the constituent stars. The stars which you see in our images are located much closer to home in our Milky Way galaxy. It is thought that M87 although very large in mass sits within an absolutely enormous surrounding halo of dark matter which can only be observed by its gravitational influence on other galaxies within the local group of galaxies". - Kurt Thrust current director of the Jodrell Plank Observatory.

Globular Star Clusters M53 and NGC5053 in the Constellation Coma Berenices

 

The Globular star cluster M53 ( centre left), the Globular star cluster NGC5053 (bottom left) and the star Alpha Comae Berenices (centre right). Imaged from the Jodrell Plank Observatory (27 and 28 April 2025) using the Seestar S30 in EQ and Mosaic mode. Image Credit Pip Stakkert.

"Clear a steady night and early morning here in Lowestoft. We managed to capture and stack in mosaic mode over 175x 30 second RAW exposures using the little Seestar S30. Quite a lot of satellites in this area of the sky, which required post processing to remove them". - Kurt Thrust current Director of the Jodrell Plank Observatory.

"M53 (Messier 53) and NGC 5053 are two globular star clusters located in the constellation Coma Berenices, and they are relatively close to each other in the sky. Despite their proximity, they show some intriguing differences in structure and composition. Here’s a detailed comparison:

🌟 M53 (Messier 53)

Type: Globular cluster

Distance from Earth: ~58,000 light-years

Apparent Magnitude: ~7.6 (visible with binoculars or a small telescope)

Diameter: ~220 light-years

Metallicity: [Fe/H] ≈ –2.06 (very metal-poor)

Stellar Population: Contains many old, low-metallicity stars.

Concentration: Fairly dense, with a concentrated core and halo.

Location: Roughly 1° away from NGC 5053 in the sky.

🌟 NGC 5053

Type: Globular cluster

Distance from Earth: ~53,500 light-years

Apparent Magnitude: ~9.0 (fainter, needs a larger telescope)

Diameter: ~160 light-years

Metallicity: [Fe/H] ≈ –2.3 (even more metal-poor than M53)

Stellar Population: Very sparse; stars are faint and less numerous.

Concentration: One of the least concentrated globular clusters known.

Location: Close in the sky to M53, often imaged together.

🔍 Similarities

Both are globular clusters located in the same constellation (Coma Berenices).

Both are metal-poor, suggesting they contain very old stars—likely among the oldest in the Milky Way.

Both lie at a similar distance from Earth (around 50,000–60,000 light-years).

They may be gravitationally interacting or have had past interactions, with some evidence of tidal streams possibly linking them". - Credit: Chat GPT

The Active Solar Disc in Broadband White Light 24_04_2025

 

Sunspot Groups on the Solar Photosphere 24_04_2025 during Solar Maximum - 66mm ED Altair Lightwave Refractor with Baader Film White light Objective Filter. Capture Camera: QHY5iii462c CMOS Planetary Video Camera with IR cut Filter doble  stacked with a Meade Optical red light filter. Images: Credit: Kurt Thrust.

"The Solar Sunspot Cycle, also known as the solar cycle, is an approximately 11-year cycle in which the number of sunspots on the Sun's surface increases and decreases. Sunspots are dark, cooler regions on the Sun's surface caused by intense magnetic activity. This cycle influences solar radiation, space weather, and even Earth's climate."

Solar Disc imaged with the Seestar S30
- Fighting above its weight in less than optimum conditions.

Key Features of the Solar Cycle:

• Solar Minimum: The period of the fewest sunspots. The Sun is relatively quiet.

• Solar Maximum: The peak of sunspot activity. The Sun is more active, with more flares and coronal mass ejections (CMEs).

• Duration: The full cycle (from one minimum to the next) lasts about 11 years, but it can range between 9 and 14 years.

What Drives the Solar Cycle?

The solar cycle is driven by the Sun’s magnetic field, specifically a process called the solar dynamo:

1. Differential Rotation: The Sun rotates faster at the equator than at the poles. This twists magnetic field lines over time.

2. Convection Currents: Hot plasma rises and cool plasma sinks in the Sun’s outer layer, further distorting the magnetic fields.

3. Magnetic Field Reversal: About halfway through the cycle (around solar maximum), the Sun’s magnetic poles flip. This magnetic reversal is part of a 22-year magnetic cycle—the sunspot cycle is half of that.

Why It Matters:

• Impacts satellites, GPS, and radio communications.

• Drives auroras near the poles.

• Can pose risks to astronauts and space missions.

• May influence Earth's climate on longer timescales."  

-Generated by ChatGPT open AI

"For the last few days, the weather has been difficult for 'Astrophotography' from the Jodrell Plank Observatory located at the UK's most easterly point in Lowestoft. Both during the day and night there has been persistent high level hazy cloud which has made capturing fine detail impossible. Recent auroral alerts lead us to believe that the Solar photosphere would have many visible sunspot groups, so even with poor visibility, we thought we would take a look. We imaged the sun across the full range of visible wavelengths ( called Broadband or white light imaging) using objective-lens mounted rejection filters which make the process safe. We imaged the Sun using our EQ mounted 66mm ED refractor and our Alt-Az mounted Seestar S30. We were reasonably and positively surprised at the results. The Sun is our nearest star and although it seems a constant unchanging companion, it is a dynamic system of turbulent and hot gas, compressed to a roughly spherical shape by gravity and prevented from collapse by the outward pressure of nuclear fusion at its core. One day, far in the future, when the Sun runs out of Hydrogen and Helium to fuse, it will first swell and cool to become a Red-Giant star and then end its days as a fading Planetary-Nebula with a White dwarf star at its centre - similar to M27 in the constellation Vulpecula". - Joel Cairo CEO of the Jodrell Plank Observatory.

Planetary Nebula M27
imaged from the Jodrell Plank Observatory

NGC 4565 The Needle Galaxy and the much dimmer Galaxy NGC 4562

 

The Needle Galaxy in the Constellation Coma Berenices.
Seestar S30 in EQ mode. 45x 30 sec subs.
Image Credit: Pip Stakkert.

Credit: Astrometry Net

"Only captured 45 subs as the moonlight was a problem. The Needle Galaxy is estimated to be between 30 and 50 million light years distant from Earth. It is a spiral galaxy, some 176 light years across, with an obvious central bulge". - Kurt Thrust current Director of the Jodrell Plank Observatory.

IC 410

 

IC410 hydrogen gas emission nebula with dust clouds in the constellation Auriga. 
Seestar S30  image credit Kurt Thrust.

" The constellation Auriga, as day becomes night in spring, is low in our western sky. We captured an hour of 30 second sub exposures, from which the above image was constructed, before the constellation dropped below our horizon. The little Seestar S30 does well on bright targets that have a large 'footprint' on the night sky. 

The nebula is a region of ionised hydrogen gas spanning over 100 light years across that's modelled by streams of charged particles in stellar winds coming from the open star cluster NGC 1893. IC 410 is some 12,000 light years distant from Earth". - Kurt Thrust current Director of the Jodrell Plank Observatory.

Messier 35 and NGC 2158 in the constellation Gemini.

 

The open star-clusters - Messier 35 and NGC 2158.
Captured with the Observatory's Seestar S30.
Credit: Pip Stakkert.

"Messier 35 is an open star cluster in the constellation Gemini, and covers approximately the same amount of sky as the full Moon. It is relatively nearby at 2,930 light years distant. The  cluster is relatively young and is estimated to have formed from a collapsing cloud of cold gas and dust approximately 100 million years ago. The compact  star cluster NGC 2158 (visible bottom right) is much further away, 11,000 light years distant and much older, estimated  to have formed some 2 billion years ago". - Joel Cairo CEO of the Jodrell Plank Observatory

The Rosette Nebula

 

NGC2244 The Seestar SS30 in action to create this Mosaic from +220x10sec subs and until the clouds rolled in. Subsequently processed using Affinity Photo, Prodigital Software gradient removal, GraXpert 3.0, Starnet GUI and StarSpikes Pro4. The Seestar SS30 works best on large bright objects like the Rosette Nebula. we are looking forward to using the SS30 in EQ mode!

" The Rosette Nebula, in the constellation Monoceros the Unicorn, is a large and bright nebula and so well suited to the Seestar S30. The above image was captured by the little robotic all in one observatory, running in 'mosaic mode'". - Kurt Thrust current Director of the Jodrell Plank Observatory.

The Partial Solar Eclipse - 29th March 2025

 

Time-lapse rendition of the 2 hour long eclipse.
Captured by Pip Stakkert using the Seestar S30. 

The Sun's Disc in eclipse at approximately 10:30am.
Captured with the 66mm. Altair Lightwave ED Refractor with an Observatory engineered (Jolene MqSquint-Fleming) 'white light filter'. QHY5iii462c planetary camera with IR cut filter double stacked with a red light filter. Credit: Kurt Thrust.

"The whole Jodrell Plank Observatory Team 'assembled' for the partial solar eclipse, which 'did not disappoint'. As regular readers of the blog will appreciate, the weather here on the coast in Lowestoft is not always 'great' for astro-imaging. The morning of the eclipse dawned fine and remained so until about 12:00, when the Moon left the solar disc. The cloud did build up over the two hour 'eclipse period' and required the time-lapse video, from the Seestar S30, to be reverse processed by: first, the conversion of the video into a series of still frames, second, the removal of frames worst affected by the cloud and third, the reanimation of the stills to create an 'animation Gif' ".

The detailed image above shows sunspots, faculae and surface granulation of the solar photosphere. It also clearly shows the Moon's limb together with undulations created by the uplifted rims of craters, which happened to be located there, when the data was captured. This image was created from three short video sequences. One for the Solar Northern Hemisphere and the second for the Southern. These videos were captured immediately prior to the start of the eclipse. The third very short video was captured at 10:30am, whilst the eclipse was underway. Software was used to convert videos one and two into a still image of the whole Solar disc. The still image of the eclipse, converted from third video clip, was then added to the complete solar disc". - Joel Cairo CEO of the Jodrell Plank Observatory.

Eclipse at about maximum ( partial disc) -sunspot group 4046 visible top left

Captured from Oulton Broad Suffolk at approx 10:30 am using a 66mm Altair Lightwave Refractor with  white light filter on a Star Adventurer EQ mount. QHY5iii462c planetary camera with IR cut filter double stacked with a red light filter. Video clips stacked and processed using : PIPP, AS!3, Registax 6, Affinity Photo 2.6 and AstroClean. Image Credit:  Kurt Thrust.

" The  convection cells in the solar photosphere deliver 'the orange peel affect', which along with faculae associated with sunspots, may be seen clearly in this image." - Kurt Thrust current Director of the Jodrell Plank Observatory.

Messier 51 - The Whirlpool Galaxy

 

Ngc 5194 and Ngc 5195 in the Constellation Canes Venatici - Seestar S30
 - images credit: Pip Stakkert

Widefield version of M51 - uncropped.

" The two galaxies Ngc 5194 and Ngc 5195 are interacting gravitationally and you can see a ribbon of gas, dust and stars extending through space from the dwarf galaxy Ngc 5195 (on the left of the image) to the spiral galaxy NGC 5194 (on the right). The galaxies are estimated to be between 23 and 31 light years distant. The spiral -  'The Whirlpool Galaxy' is just a little smaller than the Milky Way Galaxy and is thought to have interacted with the dwarf galaxy a number of times. Plumes of gas can be seen above and below the interacting pair" - Joel Cairo CEO of the Jodrell Plank Observatory.

M51 COAST Robotic Telescope BVR filters. Mount Teide Tenerife. Data Credit: Open Observatories. telescope.org Open University. Processing Kurt Thrust.

Messier 3 -Globular Star Cluster in the Constellation Canes Venatici

 

Messier 3 imaged using the Seestar S30 with IR cut filter.
from the Jodrell Plank Observatory. Image credit: Kurt Thrust

" Messier 3 is a globular star cluster which may be viewed from the Northern Hemisphere using binoculars or a small telescope from a dark location. Its foot-print upon the night sky is both small and dim!

In reality, M3 is a spherical gravitational grouping of 500,000 stars. approximately 670 light years in diameter. It is located towards the edge of the Milky Way Galaxy some 34000 light years distant from Earth. Many of the stars are ancient and shine strongly at red wavelengths. The cluster is thought to be over 11 billion years old  which is a large proportion of the estimated existence of the known Universe.

The JPO team were astonished by how well the tiny Seestar S30 with its 30mm aperture lens system was able to resolve stars towards the centre of M3. Quite extraordinary!

Pip Stakkert is currently working upon processing data from last night where we used the Seestar to capture a mosaic multi-pane image of the Markarian Chain of Galaxies in Virgo" - Carl Segin Outreach Coordinator at the Jodrell Plank Observatory.

Uncropped version of Seestar S30 - M3

Re-process with
more stars and Ha

M3 captured using the Seestar S30 in EQ Mode.
Credit: Kurt Thrust.

Credit: Astrometry.net

Dark Nebula - The Horsehead Nebula Barnard 33 - in the Constellation Orion

 

The Horsehead Nebula - 66mm Altair Lightwave ED refractor. Image Credit: Kurt Thrust.

"The weather in Lowestoft has taken for the better and we have experienced a short run of clear and steady nights. The JPO team has been busy testing the Seestar S30 and Pip Stackert is beginning to get used to the processing adjustments, which better suit the high number of 10 second duration subs that have to be stacked, cropped  and processed.

Whilst all this was going on, our Director, Kurt Thrust, took time out to capture an hour of 'early evening' data whilst the constellation Orion was due South. He used the Observatory Star Adventurer mini-rig, which is reasonably quick to set up and get photon catching. The camera used was an astro-modded Canon 200d DSLR with a clip in Altair Triband filter. 

The Horsehead Nebula is created by an enormous cloud of dense dust that is seen in silhouette against the backdrop of a bright emission nebula, which permeates much of the constellation Orion. The bright multi star system,  Alnitak, many times larger and brighter than our Sun - +30 times more massive, can be seen upper middle left in this image. For the keen eyed, you just might detect that the star shape is slightly deformed to its left by its largest and brightest sibling star. Before we stretched the illumination levels of this image, to bring out the fainter nebulosity, the sibling could be clearly resolved from its larger and brighter brother Alnitak. We were all surprised that such a small aperture telescope could pull this feat off! 

The very bright emission nebula NGC 2024 or The Flame Nebula, may be seen below Alnitak. The dark 'veins', so obvious in our image, are created by dust clouds between us and the bright emission nebula.

Emission nebulae are created by bright hot stars ionising clouds of gas, ie. energising electrons in the gas atoms, and as these atoms return to their initial or ground state, they release photons at specific wavelengths. At the JPO we do our best to 'catch them' as they fly our way!

We hope to post some of the Seestar S30 data in the near future. Fingers-crossed, the weather continues set fair. 

As a future project, we hope to use the Seestar S30 to create a three pane image of the Markarian Chain of Galaxies in the constellation Virgo". - Joel Cairo CEO of the Jodrell Plank Observatory.

Messier 83, The Southern Pinwheel, Barred Spiral Galaxy in the constellation Hydra.

 

Messier 83 NGC 5236. Coast Robotic Telescope, Mount Teide, Tenerife. Data Credit:: Open Observatories, telescope .org, Open University. Image Credit Pip Stakkert.

"Sadly, this magnificent face on barred galaxy is too low and below our southern horizon in Lowestoft. The COAST telescope being located at high altitude and at a much lower northern latitude can however image it and here at the JPO, Pip Stakkert had fun processing the data

The Southern Pinwheel Galaxy, at a distance of 15 million light years is one of the brightest and closest barred galaxies to the Milky Way. 

There is plenty of star birth going on in the galaxy's spiral arms and there have been supernova recorded in this galaxy in recent times.

The above image shows a face on view of a galaxy that measures 118,000 light years across". - Kurt Thrust current Director of the Jodrell Plank Observatory.

Bright Nebulae in the Northern Hemisphere Winter Sky

 

IC405 The Flaming Star Nebula
in the constellation Auriga.
 Seestar S30, 660x10 sec exposures
 F5 and f=150mm.
Credit: Kurt Thrust

The Running Man Nebular NGC 1977 and
 the Great Orion Molecular Cloud Messier 42.
Seestar S30, 660x10 sec exposures
 F5 and f=150mm. 
Credit: Joel Cairo

Messier 78 or NGC 2068 is a reflection nebula in the constellation Orion. Data Credit: COAST Robotic telescope BVR filters, Mount Teide Tenerife, telescope.org,
 Open Observatories, Open University. Image Credit: Pip Stakkert.

" Messier 42, the 'Great Orion Nebula', is the only one of the above, which may be seen with the naked eye or even better in binoculars. It is visible as a hazy blob within Orion's Dagger, which hangs down from the band of three stars known as Orion's belt. At this time of year the Constellation is visible from the Northern Hemisphere striding above the southern horizon. The Nebula is a nearby stellar nursery where new stars are forming from the gravitational collapse of cold hydrogen gas. Very young and intensely bright stars may be seen in our image in the bright central area, which is named the 'Trapezium'. M 42 is 1350 light years distant so when I said 'nearby' this was in 'astronomer speak'.

IC495, the 'Flaming Star Nebula' is both an emission and reflection nebula but is not visible to the naked eye. It is however, possible to see the irregular variable star AE Aurigae, which shines at its centre, with binoculars. 

Messier 78 is a reflection nebula located within the constellation but sadly is invisible to the naked eye. Gas and dust in this area reflect the ultra violet light generated by nearby young energetic blue stars.

The whole team at the Jodrell Plank Observatory enjoy using the Seestar S30 , which is a very user friendly device well suited to the beginner astro-imager.

 - Kurt Thrust current Director of the Jodrell Plank Observatory. 

New Kit at the Jodrell Plank Observatory for 2025

 

M45 First Light for the SeeStar S30 credit: Joel Cairo

" The SeeStar S30 is a transportable mini observatory comprising a 30mm aperture ED telescope, filters, dew heater, camera and alt-az mount, all in one light weight package. As M45 was high in the sky and relatively bright, we programmed the SeeStar to capture three hours of 10 second exposures. The SeeStar's on board processor, live stacked the exposures and then we processed and cropped the stacked image, to create the above view of the 'Seven Sisters'. We believe, by changing our working method, even better images will be delivered by this small but mighty bit of kit, Watch this space!" -  Kurt Thrust current Director of the Jodrell Plank Observatory.

The SeeStar S30 on its mini tripod, in the Jodrell Plank Observatory hospitality lounge. The bottle of wine was placed next to it to give an idea of scale of the mini-observatory. The SeeStar S30 weighs approximately 1.5 kg.

" On behalf of all the staff at the Jodrell Plank Observatory, I should like to thank our joint sponsor, Anita Roberts, for gifting the SeeStar S30 to the Observatory" - Joel Cairo CEO of the Jodrell Plank Observatory.

A Night of Planets

 

Venus showing a crescent phase imaged at F22.5 early evening 25_01_2025 image Credit: Kurt Thrust

Mars at F22.5 just passed opposition in the early hours 26_01_2025 image
Credit: Pip Stakkert

Mars at F56 just passed opposition in the early hours 26_01_2025 image
Credit: Pip Stackkert

Jupiter at F22.5 early evening 25_01_2025 image
credit: Karl Segin

A compilation of Solar System highlights from the last 12months
 credit: Kurt Thrust.

" We finally had the opportunity and clear night in January 2025 to point our 127mm Apo refractor and QHY5iii462c camera at the planets;  Mars and Venus" - Joel Cairo CEO of the Jodrell Plank Observatory.