From ESOblog (EU): “A 40-year-long mystery- heavy elements unveil the origin of the giant Leo Ring”

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From ESOblog (EU)

Not all spiral galaxies have to be picture-perfect to be striking. Messier 96, also known as NGC 3368, is a case in point: its core is displaced from the centre, its gas and dust are distributed asymmetrically and its spiral arms are ill-defined. But this portrait, taken with the FORS1 instrument on ESO’s Very Large Telescope, shows that imperfection is beauty in Messier 96.

The galaxy’s core is compact but glowing, and the dark dust lanes around it move in a delicate swirl towards the nucleus. And the spiral arms, patchy rings of young blue stars, are like necklaces of blue pearls.

Messier 96 lies in the constellation of Leo (The Lion). It is the largest galaxy in the Leo I group of galaxies; including its outermost spiral arms, it spans some 100 000 light-years in diameter — about the size of our Milky Way. Its graceful imperfections likely result from the gravitational pull of other members in the group, or are perhaps due to past galactic encounters.

A multitude of background galaxies peers through the dusty spiral. Perhaps the most striking of these objects is an edge-on galaxy that — because of a chance alignment — appears to interrupt the outermost spiral arm to the upper left of Messier 96’s core.

This image was processed by ESO using the observational data found by Oleg Maliy from Ukraine, who participated in ESO’s Hidden Treasures 2010 astrophotography competition [1], organised in October–November 2010, for everyone who enjoys making beautiful images of the night sky using astronomical data obtained with professional telescopes. The image was made with data taken at visible and infrared wavelengths through B, V, and I filters.

[1] ESO’s Hidden Treasures 2010 competition gave amateur astronomers the opportunity to search through ESO’s vast archives of astronomical data, hoping to find a well-hidden gem that needed polishing by the entrants. To find out more about Hidden Treasures, visit

Credit: ESO/Oleg Maliy9 April 2021, Science@ESO

Nearly 40 years ago, astronomers made a serendipitous discovery when they pointed a radio telescope at an “empty” patch of sky in the Leo constellation: a giant cloud of gas, massive enough to form a galaxy but unlike anything seen before. This started the decades-long quest to discover the origin of this gigantic structure, known as the Leo Ring. Astronomers first theorised that it was a remnant leftover from when the first stars formed within this group of galaxies. Now research using the MUSE instrument on ESO’s Very Large Telescope (VLT) has provided a definite answer to the question of the Leo Ring’s origin.

European Southern Observatory(EU) , Very Large Telescope at Cerro Paranal in the Atacama Desert •ANTU (UT1; The Sun ) •KUEYEN (UT2; The Moon ) •MELIPAL (UT3; The Southern Cross ), and •YEPUN (UT4; Venus – as evening star). Elevation 2,635 m (8,645 ft) from above Credit J.L. Dauvergne & G. Hüdepohl atacama photo.

In 1983, a team of astronomers led by PhD student Stephen E. Schneider was aiming to measure the properties of a distant galaxy and needed a “blank sky” reference measurement. Pointing the US Arecibo radio telescope at what they thought was an unremarkable patch of the sky, they found it was actually populated with cold hydrogen gas, revealing a giant gas cloud six times larger in diameter than the Milky Way. It was named the Leo Ring after its shape and for lying in the direction of the Leo constellation in the sky.

The discovery of such a large gas cloud, and the lack of any stars detected in the ring, raised questions on how galaxies form and evolve. A gas cloud of this size should have collapsed under gravity to become one or more galaxies containing many stars.

If the gas forming this structure had never been part of a galaxy, could the Leo Ring be an ancient cloud of gas left over from billions of years ago when galaxies were still forming? Or perhaps the gas was part of a galaxy, but it was stripped away from it and expanded to form the Leo Ring? However, even in the latter case, we would still expect to see some stars, either left over from a galaxy or created in the violent process of gas expansion.

Now, nearly 40 years after its discovery, a new team of astronomers led by Edvige Corbelli from Arcetri Astrophysical Observatory, National Institute for Astrophysics (INAF) in Italy have tackled these questions conclusively.

Stars are the key to determining the history of the Leo Ring. “The only way to solve the mystery of the Leo Ring’s origins is to measure the amount of heavy elements dispersed in the hydrogen gas,” explains Corbelli. “These elements are created by stars and, if found in large amounts, they could give a clear signal that the gas is not primordial.”

The Leo Ring was widely believed to be a primordial cloud of gas, containing only the lightest elements — hydrogen, helium and a trace amount of lithium — that were created in the Big Bang, with no stars. Then in 2009, a team led by David Thilker of the John Hopkins University (US) were studying the first ultraviolet (UV) observation of Messier 96, when they made a serendipitous discovery. On noticing that the Leo Ring was visible at the edge of their image, they were able to identify clumps shining brightly in the UV that were possibly associated with the ring and could signal the presence of massive stars. This challenged the then-held theory that the ring lacked stars. However, astronomers could still not say for certain whether stars were forming in the Leo Ring, or whether they were picking up signatures of stars much further away in the background.

The search was on to find stars born within the Leo Ring, young and massive enough to light up the heavy elements in the surrounding gas. These stars might be so faint and sparse that the hot regions around them might have escaped detection for decades — detecting them would require a powerful instrument and telescope, such as the MUSE instrument on ESO’s VLT. Giovanni Cresci, who is also from INAF and was involved in the research recently published in The Astrophysical Journal Letters, said, “We were already using MUSE and other instruments at ESO to study nearby and distant galaxies. So, when Edvige told us of the Leo Ring mystery, we realised that MUSE would be ideal to finally provide an answer about the origin of this huge structure”.

“For the first time within the ring, we have detected nebulae ionised by rare and isolated massive stars, 30–40 times more massive than our Sun.”

By using MUSE, the astronomers looked at three clumps of hydrogen gas where UV radiation had been found. “For the first time within the ring, we have detected nebulae ionised by rare and isolated massive stars, 30–40 times more massive than our Sun,” says Corbelli. The presence of these stars and nebulae meant the team was able to measure the abundance of heavy elements within the nebulae, which proved the stars were in the Leo Ring and suggested the gas was not primordial.

Filippo Mannucci, an astronomer at INAF-Arcetri, says, “We have been measuring chemical abundances in galaxies for many years, but we had never applied our methods to such a special object.” During their lifetimes, massive stars produce heavier and heavier elements until they reach iron, run out of fuel and explode as supernovae. Cresci expands, “Our observations allowed us to see for the first time these faint and rare little spots of gas ionised by the few young, massive stars in the ring.”

This is an optical image of galaxies in the Messier 96 group, with contours of the gas in the Leo Ring from the Arecibo radio telescope in blue and from the Very Large Array in magenta (taken from Schneider et al 1986). White squares indicate the locations Corbelli’s team observed with the VLT’s MUSE instrument, with the boxes showing the more detailed MUSE observations. Here, the labels mark the locations of the detected nebular regions powered by massive stars. Credit:ESO/E. Corbelli, Sloan Digital Sky Survey, Arecibo/VLA/Schneider.

The team found a large abundance of heavy elements throughout the structure. “To pollute the ring with so many heavy elements, we would need many more stars than we observed,” says Corbelli. The lack of stars then raises more questions: how were these heavy elements dispersed throughout the structure?

Without the presence of many additional stars, the gas must have been enriched with these elements in a place where a lot of older stars are found, for example in an older galaxy.

“This means the ring is not a leftover gas cloud sitting around from the time when other galaxies were forming. The gas has been enriched by heavy elements in a galaxy disc, and later removed by the gravitational pull of a galaxy-galaxy encounter before forming the ring,” explains Corbelli.

The answer of how the Leo Ring came to be is through the collision of two galaxies. This massive energetic event spanning millions of years had such a strong gravitational force that gas, and heavy elements, were pulled from within a galaxy and dispersed throughout space. Previous work led by Leo Michel-Dansac at the University of Lyon in 2010 using computer simulations suggested that two galaxies, Messier 96 and NGC 3384, may have collided to form the Leo Ring. Corbelli’s team have now confirmed that a close encounter between galaxies is the most likely scenario for the formation of this mysterious object.

This climactic solution to the Leo Ring mystery came through decades worth of research and innovation. After nearly 40 years, we finally have closure on its origin and can appreciate how existing theories were challenged and changed in the light of new evidence. However, the Leo Ring has yet to yield all of its secrets. Corbelli concludes, “Now that we have established that the gas has been removed from a galaxy during a galaxy-galaxy encounter, the big question for the future is: why did the ring not manage to form more stars?”

See the full article here .


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ESO (EU) is the foremost intergovernmental astronomy organisation in Europe and the world’s most productive ground-based astronomical observatory by far. It is supported by 16 countries: Austria, Belgium, Brazil, the Czech Republic, Denmark, France, Finland, Germany, Italy, the Netherlands, Poland, Portugal, Spain, Sweden, Switzerland and the United Kingdom, along with the host state of Chile. ESO carries out an ambitious programme focused on the design, construction and operation of powerful ground-based observing facilities enabling astronomers to make important scientific discoveries. ESO also plays a leading role in promoting and organising cooperation in astronomical research. ESO operates three unique world-class observing sites in Chile: La Silla, Paranal and Chajnantor. At Paranal, ESO operates the Very Large Telescope, the world’s most advanced visible-light astronomical observatory and two survey telescopes. VISTA works in the infrared and is the world’s largest survey telescope and the VLT Survey Telescope is the largest telescope designed to exclusively survey the skies in visible light. ESO is a major partner in ALMA, the largest astronomical project in existence. And on Cerro Armazones, close to Paranal, ESO is building the 39-metre European Extremely Large Telescope, the E-ELT, which will become “the world’s biggest eye on the sky”.

ESO VLT at Cerro Paranal in the Atacama Desert, •ANTU (UT1; The Sun ),
•KUEYEN (UT2; The Moon ),
•MELIPAL (UT3; The Southern Cross ), and
•YEPUN (UT4; Venus – as evening star).
elevation 2,635 m (8,645 ft) from above Credit J.L. Dauvergne & G. Hüdepohl atacama photo.

Glistening against the awesome backdrop of the night sky above ESO_s Paranal Observatory, four laser beams project out into the darkness from Unit Telescope 4 UT4 of the VLT, a major asset of the Adaptive Optics system.

ESO VLT 4 lasers on Yepun.

Part of ESO’s Paranal Observatory, the VLT Survey Telescope (VISTA) observes the brilliantly clear skies above the Atacama Desert of Chile. It is the largest survey telescope in the world in visible light at an elevation of 2,635 metres (8,645 ft) above sea level.

ESO/Cerro LaSilla, 600 km north of Santiago de Chile at an altitude of 2400 metres.

ESO/NRAO/NAOJ ALMA Array in Chile in the Atacama at Chajnantor plateau, at 5,000 metres.

ESO ELT 39 meter telescope to be on top of Cerro Armazones in the Atacama Desert of northern Chile. located at the summit of the mountain at an altitude of 3,060 metres (10,040 ft).

ESO/MPIfR APEX high on the Chajnantor plateau in Chile’s Atacama region, at an altitude of over 4,800 m (15,700 ft).

A novel gamma ray telescope under construction on Mount Hopkins, Arizona. a large project known as the Čerenkov Telescope Array, composed of hundreds of similar telescopes to be situated in the Canary Islands and Chile. The telescope on Mount Hopkins will be fitted with a prototype high-speed camera, assembled at the University of Wisconsin–Madison, and capable of taking pictures at a billion frames per second. Credit: Vladimir Vassiliev .