Hubble's New Image of NGC 346 Reveals Star Formation in the Small Magellanic Cloud

This splendid, new image of the young star cluster NGC 346 is part of the celebrations for the 35th anniversary of Hubble.

The cluster is located in the Small Magellanic Cloud (SMC), a satellite galaxy of the Milky Way, about 200,000 light-years away in the constellation of Tucana.

The image combines infrared, optical, and ultraviolet data, providing a complete view of the cluster and its surrounding nebula. For example, infrared allows researchers to penetrate the dust clouds, revealing hidden stars, while ultraviolet highlights regions of ionized gas.

NGC 346 hosts over 2,500 newborn stars, some of which are significantly more massive than the Sun. The associated nebula, called N66, is an H II region with the highest rate of star formation, which is an area of ​​ionized gas illuminated by ultraviolet light emitted by young, hot stars. N66 is, in fact, the largest and brightest H II region in the SMC, characterized by a bright pink color and dark, snake-like clouds that weave into the structure. 

Hubble observations, conducted over a period of 11 years, made it possible to trace the movements of the stars within the cluster. The data reveal that the stars are spiraling toward the center of the cluster, driven by gas flows coming from outward that fuel star formation. This dynamic motion is crucial to understand how interstellar matter contributes to the growth and evolution of the cluster.

The most massive stars in NGC 346, estimated to be just a few million years old, emit intense radiation and stellar winds that carve bubbles out of the surrounding nebula. These processes disperse the gas, creating complex structures and influencing the formation of new stars. The image captures such interactions, showing how stars not only form, but actively shape their environments.

The SMC is an irregular dwarf galaxy with significantly lower metallicity than the Milky Way. Metallicity, in astronomy, refers to the fraction of the mass composed of elements heavier than helium, such as carbon, oxygen, and iron, that form inside stars and are lost into the interstellar environment during events such as supernovae. The SMC's low metallicity makes it similar to conditions in the early universe; in short a "natural laboratory" to study star formation processes in the first billion years of the Universe.

The observation of NGC 346 is therefore significant for research on galactic and stellar evolution. In particular, it helps to understand the evolution of dwarf galaxies and star formation in environments with low metallicity.

-----------------------------------

Image credits: ESA/Hubble & NASA, A. Nota, P. Massey, E. Sabbi, C. Murray, M. Zamani (ESA/Hubble)

Reference➡️ Hubble Spots Stellar Sculptors in Nearby Galaxy

Cosmic Dance: A Dual Quasar Or A Single Lensed Quasar At Cosmic Noon?

A recent study has presented JWST observations of an object called J0749+2255, a candidate dual quasar very far from us at a redshift of 2.17 (which means it is distant 10.661 billion light-years ).

Initially identified as a single quasar in the Sloan Digital Sky Survey (SDSS), J0749+2255 was later flagged as a candidate dual quasar with the VODKA technique based on Gaia data.

J0749+2255 appears to be formed by two quasars, which are two extremely luminous galactic nuclei powered by supermassive black holes (SMBHs), separated by a distance of about 3.8 kpc (1 pc equals about 3.26 ly), which makes J0749+2255 one of the most distant small-separation dual quasars known.

The researchers used a special instrument on JWST, called NIRSpec IFU, to study the light from these quasars and their host galaxy.

Thanks to these observations, they discovered that the two quasars are surrounded by a "host" galaxy clearly visible for the first time, with ionized gas (i.e. gas charged with energy) that extends for about 20,000 parsecs. The two quasars, called J0749+2255-NE and J0749+2255-SW, have very similar characteristics: they emit light with the same intensity (more than 10^46 erg per second, a very high value), have black holes with masses about a billion times that of the Sun and show almost identical spectral lines.

Finding two quasars (dating back to a phase of the universe called cosmic noon when star formation and black hole activity were at their peak) so close together is an exceptional event and could tell us a lot about how SMBHs grow and how galaxies merge over time.

The data suggests that the two quasars could be in a phase of synchronized growth, a rare phenomenon possible precisely because they are located in the same gas-rich environment, which supplies matter to both. It's a hypothesis that researchers are still testing, but preliminary data seems to support it.

The NIRSpec instrument made it possible to analyze the light emitted by the gas and stars around the quasars. The light was broken down into a spectrum, revealing information about the composition, speed and distribution of the gas.

However, not everything is clear in this study. Are these really two distinct quasars? While the data is compelling, it is possible that one of the sources is a gravitational lensing effect.

Distinguishing between lensed quasars and dual quasars is particularly challenging, especially for small-separation pairs at higher redshifts.

In the context of the study, the possibility of a dual quasar (i.e. two separate SMBHs in a binary system) is the most likely explanation based on the data collected, but the researchers cannot completely rule out gravitational lensing.

Why do they consider this possibility?

The researchers note that the 3.8 kpc separation between the two sources is quite small on cosmic scales, but not so small that a lensing effect is impossible.

They have not yet observed an evident massive object (such as a massive galaxy) between us and the system that could be causing the lensing, but there could be some hidden or less visible mass.

In summary, the gas distribution and spectral features could be consistent with either two real quasars or a single lensed quasar.

However, the gravitational lensing hypothesis is less favored than the dual quasar hypothesis because the NIRSpec observations show that the gas around the two quasars appears to move coherently with a disk, which supports the idea of two distinct sources influencing the same environment.

Furthermore, the spectral properties of the two sources show some differences, suggesting that they could be two physically separate objects, not just images of the same quasar.

Ultimately, the researchers are cautious: they are proposing the "synchronized growth of two SMBHs" as the 

main explanation, but they leave the door open to other possibilities, such as gravitational lensing, that future studies (for example with more detailed observations or theoretical models) will have to confirm or deny.

----------------------------------

Image: A Hubble image of the J0749+2255 system (Release Date: April 5, 2023)  ➡️ Source

Credit: NASA, ESA, Yu-Ching Chen (UIUC), Hsiang-Chih Hwang (IAS), Nadia Zakamska (JHU), Yue Shen (UIUC)

Reference

Scientific Paper "VODKA-JWST: Synchronized Growth of Two Supermassive Black Holes in a Massive Gas Disk? A 3.8 kpc Separation Dual Quasar at Cosmic Noon with the NIRSpec Integral Field Unit"➡️ Source

M67 Stars Sing The Past And The Future: New Discoveries About The Red Giants

A recent study explores how the acoustic vibrations of stars in the open cluster M67, located 2,700 ly from Earth in the Milky Way, can reveal crucial information about their internal structure and evolution.

This study, led by UNSW Sydney researchers, focuses on 27 stars with similar ages and compositions to our Sun, but in different evolutionary stages.

Let's dig deeper.

Stars, like the Sun, vibrate because of sound waves generated within them. These vibrations, called 'acoustic modes', can be detected by observing small variations in their brightness. By analysing these oscillations in the 27 stars of M67, the researchers studied two types of differences in the frequencies of the vibrations: 'large separations' (they indicate the distance between the main frequencies and reflect the overall density of the star) and 'small separations' (these are finer differences between nearby frequencies and usually reflect conditions in the core). As stars evolve from subgiants to red giants, they develop a deeper outer convective zone, a layer where stellar material mixes with motions similar to boiling water.

The study found that as these stars age and become red giants, the patterns of 'small separations' deviate from what was expected. This deviation is due to the influence of the lower boundary of the convective zone, which deepens over time as the stars evolve. In effect, acoustic vibrations allow researchers to “see” how the internal structure of stars changes over time.

This work is significant because it offers a new key to understanding stellar evolution. Traditionally, 'small separations' were thought to lose importance in stars with inert cores (such as red giants), but this study shows that they can still provide valuable information, related to the convective zone. Furthermore, the observation of a “plateau” in the vibration patterns represents a novel clue, which could become a new tool to measure the age and evolutionary state of stars. Since M67 contains stars similar to the Sun, these results also help researchers better understand the past and future of our Sun.

On a practical level, this research refines the methods of asteroseismology, a powerful tool that uses stellar vibrations to study their interior, much like seismologists use earthquakes to explore the interior of the Earth. Improving researcher's ability to interpret these vibrations means they can more precisely determine the age and composition of stars in other clusters or galaxies. This has implications for mapping the universe, understanding star formation, and even finding planetary systems, since the age of a star affects the habitability of its planets.

In essence, this research not only expands our theoretical understanding of stellar evolution, but also offers practical tools for future astronomical observations, making asteroseismology an increasingly powerful means for exploring the cosmos.

----------------------------

Image: The M67 open cluster contains a population of giant, evolved stars.

Credit: Sloan Digital Sky Survey | CC BY 4.0

References

UNSW Sydney Press Release

Scientific Paper: 'Acoustic modes in M67 cluster stars trace deepening convective envelopes'

-------------------------------------------

NOTE: I report a couple of questions to which I have provided answers that may be of interest to someone.

Q: "Stars, like the Sun, vibrate because of sound waves generated inside them."

What are these sound waves generated by?

A: Sound waves inside stars, such as the Sun, are generated primarily by turbulent movements of plasma in the convective zone, a region beneath the stellar surface where heat is transported outward through the movement of matter. In the case of the Sun, the convection zone is located just below the photosphere, the visible layer.

The turbulent movements are caused by thermal energy produced in the core of the star through nuclear fusion. In the core, hydrogen is transformed into helium, releasing enormous amounts of energy in the form of radiation and particles. This energy heats the surrounding plasma, creating temperature gradients that lead to instabilities: hot plasma rises to the surface, while the colder, denser plasma sinks inward. The convection process generates oscillations and turbulence that produce sound waves.

The waves propagate within the star, bouncing and interfering with each other, and can be studied using helioseismology (in the case of the Sun) or asteroseismology (for other stars). The resulting vibrations provide valuable information about the internal structure of stars, such as density, temperature and chemical composition. 

In practice, stars "ring" like cosmic bells, and we can "listen" to them by analyzing variations in light or movement on their surfaces!

Q: What exactly is the plateau that the research talks about and that you mentioned in your post?

A: The “plateau” refers to a phenomenon observed in the patterns of the frequencies of acoustic vibrations (or acoustic modes) of the stars in the M67 cluster, in particular in the so-called “small separations”. To understand it clearly, we need to take a step back and understand what these separations are and why the plateau is an important discovery.

Stars vibrate due to internal sound waves, and these vibrations produce a series of frequencies that scientists can measure. Between these frequencies, there are regular differences:

- Large separations indicate the distance between the main frequencies and reflect the overall density of the star.

- Small separations are finer differences between nearby frequencies and, in stars like the Sun, are related to the conditions of the core (for example, how dense or rich in helium it is).

As a star evolves from a subgiant to a red giant, its core contracts and the outer convective zone (the layer where the material mixes) deepens. Traditionally, it was thought that in red giants, small separations become meaningless, because the core becomes less influential than the outer layers.

The “plateau” is an unexpected behavior observed in these small separations in the stars of M67. Instead of continuously decreasing or disappearing altogether as the star evolves, the small separations stabilize at a constant value for some time, forming a sort of “plateau” in the data. This happens because the lower boundary of the convective zone, which moves inward as the star ages, begins to influence the acoustic vibrations in a new and measurable way.

In simple terms, it is as if the vibrations “feel” this deepening boundary and, at a certain point, produce a stable signal instead of constantly changing. 

The plateau is a scientific surprise because it reveals that small separations are not only an indicator of the core, but can also tell us something about the structure of the outer layers of stars, in particular the convective zone. This makes it a new “hallmark” of stellar evolution.

Scientifically, it suggests that theoretical models of stellar evolution need to be updated to account for this effect.

Practically, it offers scientists a new tool to estimate the age and evolutionary state of stars: by measuring the plateau, they can understand how deep the convective zone is and therefore where the star is in its life.

Warm Gas Near A Supermassive Black Hole: Key To Finding Early Universe Hidden Black Holes

An international team using ALMA detected high-resolution radio signals from warm gas surrounding a supermassive black hole (SMBH) dating back about 13 billion years, when the Universe was very young.

The warm gas, detected thanks to high-energy carbon monoxide (CO) emissions, is organized in a disk-like structure around the black hole, inside the quasar J2310+1855, an extremely luminous object powered by the intense activity of the black hole itself.

This observation is significant because many SMBHs in the early Universe are hidden by thick clouds of cosmic dust, which block visible light and X-rays, making them difficult to detect. However, the radio waves emitted by the warm gas and detected by ALMA are not absorbed by the dust, thus offering a new technique to find them.

The technique opens, in fact, a window into the early universe, allowing researchers to explore SMBHs when the universe was less than a billion years old, offering clues about their growth and the evolution of galaxies.

In this case, the black hole has an estimated mass greater than a billion times that of our Sun. The research team observed it, highlighting how the X-rays emitted by the quasar heat the surrounding gas to extreme temperatures.

This discovery not only allows scientists to study the conditions near black holes in the early universe, but could also help them understand how black holes formed and evolved. The researchers plan to apply this technique to other objects to obtain a more complete census of hidden black holes and delve deeper into their history.

In essence, the discovery of warm gas around a SMBH 12.9 billion light-years away represents a step forward in identifying hidden black holes and understanding their role in the young universe, thanks to the unique capabilities of the Atacama Large Millimeter/submillimeter Array (ALMA).

--------------------------

Image: This illustration shows how intense X-ray radiation from the vicinity of a SMBH heats the surrounding gas. When viewed from the side, visible light and X-rays are blocked by the disk, effectively hiding the SMBH.

Credit: ALMA (ESO/NAOJ/NRAO), K. Tadaki et al.

References

ALMA Press Release

Scientific paper: Warm gas in the vicinity of a supermassive black hole 13 billion years ago 

A Rare Astronomical Event: A Triple Eclipse On Jupiter

This breathtaking image, taken by Hubble on 28 March 2004, shows a truly fascinating astronomical event: a rare triple eclipse on Jupiter due to an equally rare alignment of three of its largest moons– Io, Ganymede, Callisto – across the planet's face.

At first glance, Jupiter appears to have five distinct spots on its upper surface: one white, one blue, and three black.

In reality, Io is the white circle in the center, and Ganymede is the blue circle. Callisto is out of the image and to the right, and so not visible. The three black circles are the shadows cast by the three moons.

In fact, the shadows of Io, Ganymede, and Callisto are visible because the three moons, lying between Jupiter and the Sun, block sunlight and create an effect similar to a solar eclipse on Earth.

Io's shadow is just above the center and slightly to the left;

Ganymede's shadow is on the left limb of the planet; Callisto's shadow is near the right edge.

The image, taken with Hubble's Near Infrared Camera and Multi-Object Spectrometer (NICMOS), which operates in the near-infrared, explains Jupiter's pastel colors, different from those we see with the naked eye or in visible light.

The image is particularly captivating and significant both visually and scientifically.

A triple eclipse on Jupiter, in which the shadows of three moons simultaneously cross the planet's disk, is a rare phenomenon, occurring only once or twice every ten years, due to the different orbital periods of the moons. Furthermore, in this particular image, Io and Ganymede cross Jupiter's disk at the same time as the three shadows: an even rarer event.

The event, captured in this image, provides a unique opportunity to observe the interactions between Jupiter and its Galilean moons (including Europa, not visible here). The moons' shadows and positions allow scientists to analyze their orbits, sizes, and physical characteristics.

Shadows cast on Jupiter's layers of cloud provide contrast that helps scientists study the structure and composition of its atmosphere. Sunlight, filtered through Jupiter's atmosphere and visible around the shadows, can reveal details about particles and gases in the upper clouds.

The parallel between this type of eclipse on Jupiter and solar eclipses on Earth allows astronomers to delve into the dynamics of eclipses in settings other than our Earth-Moon system.

This event, captured by Hubble, is a testament to the beauty and complexity of our cosmic neighborhood.

-------------------------------------------

Image Credit: NASA, ESA, and E. Karkoschka (University of Arizona)

Reference and Image Source  

Most Galaxies In The Deep Universe Appear To Rotate In The Same Direction

 

A recent study, using data from JWST, analyzed the rotation of 263 distant galaxies, surprisingly finding that about 2/3 of them rotate clockwise, while only 1/3 rotates counterclockwise.

This imbalance challenges current cosmological theories, which predict a more or less equal distribution of the rotation directions of galaxies in an isotropic universe, that is, without a preferred direction.

The study was led by Lior Shamir, associate professor of computer science at Kansas State University, as part of the JWST Advanced Deep Extragalactic Survey (JADES) program.Shamir used high-resolution images from JWST to study the galaxies' shapes and determine their rotation direction. The difference between the number of galaxies rotating clockwise and counterclockwise becomes even more pronounced when observing galaxies at greater distances, corresponding to older times in the universe.

The study suggests that this asymmetry may not be random and raises fundamental questions about the structure and origin of the universe. According to Shamir, there are two primary possible explanations for this phenomenon:

- The universe itself could have been born with an intrinsic rotation, an idea that contradicts the standard cosmological model according to which the universe is isotropic and homogeneous. If confirmed, this theory would imply that our current knowledge of the cosmos is incomplete and requires revision.

- The rotation of the Earth around the center of the Milky Way could influence observations. Light from galaxies, rotating in the opposite direction to the Earth's motion, appears brighter due to the Doppler effect, leading to an overrepresentation of these galaxies in the data. If this hypothesis is correct, measurements of cosmic distances could be incorrect and would require recalibration.

From a scientific perspective, this discovery is significant because it calls into question some of the foundations of modern cosmology. The standard model of the universe, based on the cosmological principle of homogeneity and isotropy, predicts that galaxies have randomly distributed directions of rotation. The observation of such a strong asymmetry could indicate that the universe has a "preferential direction" or that the physical processes, governing the formation of galaxies ,are more complex than previously thought. Furthermore, if the universe was born in rotation, this could link to speculative theories, such as that our universe is inside a rotating black hole, an idea proposed by some theoretical physicists.

Another important aspect is that this asymmetry increases with distance: the further back in time you look (and therefore further into space), the greater the imbalance. This suggests that the phenomenon could be linked to the initial conditions of the universe, offering a unique window to study the Big Bang and cosmic evolution.

Practically speaking, Shamir's results could have direct implications for observational astronomy. If the asymmetry is due to a bias related to the rotation of the Milky Way, as suggested by the Doppler effect, this would mean that measurements of the distances to distant galaxies – which are essential for calculating the expansion rate of the universe (the Hubble constant) – could be inaccurate. A recalibration of these measurements could resolve some known discrepancies in cosmology, such as differences in the values of the Hubble constant measured by different methods or the existence of galaxies apparently older than the universe itself according to current estimates.

In addition, the James Webb Telescope, with its ability to observe distant galaxies in unprecedented detail, remains a game-changer. This study demonstrates how its technology can not only confirm existing theories, but also raise new questions that push the limits of our understanding of the cosmos.

In essence, Shamir's study highlights a fascinating and potentially revolutionary anomaly: most of the galaxies observed by JWST appear to be rotating in the same direction, an observation that could reflect a fundamental property of the universe or an error in our measurement techniques. Scientifically, it opens the way for new research to test these hypotheses and delve deeper into the nature of the cosmos. In practice, it could lead to a revision of the methods by which we measure the universe, improving the precision of our cosmic maps.

-------------------------------------

References

K-State press release

Science paper 

Image description: "Spiral galaxies imaged by JWST that rotate in the same direction relative to the Milky Way (red) and in the opposite direction relative to the Milky Way (blue). The number of galaxies rotating in the opposite direction relative to the Milky Way as observed from Earth is far higher (Shamir 2024e)".

Credit: Kansas State University

Devil's Horns: Stunning Eclipse Sunrise Over Persian Gulf

This extraordinary photograph, taken by Elias Chasiotis, captures an unusual sunrise over the Persian Gulf, Qatar: due to a solar eclipse, the Sun appears partially covered by the Moon, creating a shape resembling two “devil's horns” .

To be precise, it was the annular solar eclipse of December 26, 2019 (Saros cycle 132), a phenomenon in which the Moon positions itself between the Earth and the Sun, but is not close enough to completely cover it, leaving a ring of sunlight visible around its edge. Some observers in a narrow strip of land east of Qatar were able to witness a complete annular solar eclipse, in which the Moon appears surrounded by a “ring of fire” from the Sun.

However, in Chasiotis' photo, the eclipse was captured at sunrise, when the Earth's horizon and the position of the Moon helped create this unique shape, different from the full ring typical of an annular eclipse.

This photo highlights a further captivating phenomenon.

Near the top of the Sun, made reddish by the atmosphere, a dark circle can be seen: it is the Moon that partially obscures the Sun during the eclipse. Surprisingly, under this circle there is another dark "peak", also part of the Moon. This effect is due to a rare optical phenomenon: the Earth's atmosphere, in which there was an inversion layer of unusually warm air in the Persian Gulf, acted as a giant refractive lens, creating a second distorted image of the Sun and the Moon. In short a mirage/mirror effect visible in the lower part of the "devil's horns". 

The phenomenon, known as the "Etruscan vase effect", occasionally occurs during normal sunrises or sunsets, but in this case it was amplified by the eclipse.

---------------------------

Image source

Further reading and references

Etruscan Vase or Omega Sunsets

Solar eclipse of December 26, 2019 

What Is The Mineral Moon?

This photo from Alexandru Barbovschi and Marek Stromayer shows the International Space Station transiting the full mineral Moon as observed from the Republic of Moldovia, on March 26, 2021.

But what is the mineral Moon? Well, it's always our Moon, of course.

Seriously, the mineral Moon is a photography technique which involves capturing wide-field images of our satellite by color sensors, and processing them in order to extrapolate the large amount of information contained in the pics.

This technique was utilized in the early 1990s by Galileo spacecraft that photographed the Moon's colors.

For example, the following image is a mosaic of 53 images, recorded by the Jupiter-bound Galileo spacecraft as it passed near our Moon in 1992. The pics, recorded through three spectral filters, were combined in an exaggerated false-color scheme.

More at this link.

In summary, different colors of the Moon’s surface  represent different chemical compositions. For instance, blue areas are rich in titanium, orange ones are titanium poor. Regions abundant in titanium are of interest because lunar titanium is bound to oxygen.

The mineral distribution on the lunar surface was mapped in great detail by the US Clementine probe, launched on 25 January 1994.

For over two months Clementine mapped the Moon, producing the first multispectral global digital map of the Moon, the first global topographic map, and contributing several other important scientific discoveries.

To conclude you can produce images of the Moon, showing colors of its surface, without having to launch a spacecraft to do so.

Here is a tutorial, if you are interested. 

First image's source and further reading. 

New Results From The First 3 Years Of DESI Data Show A Preference For Evolving Dark Energy

This figure shows a slice of the universe mapped by the DR1 data, showing the four major galaxy samples. See the figure in the paper for more details. Credit: Claire Lamman

The Dark Energy Spectroscopic Instrument (DESI) collaboration published a new analysis of dark energy on 19 March 2025.

DESI created the largest three-dimensional map of the universe ever made, using data from nearly 15 million galaxies and quasars collected in the first three years of observations. This map covers 11 billion years of cosmic history.

Dark energy has long been considered a constant (called the “cosmological constant” in the standard Lambda CDM model), that is, a force that does not change over time and that pushes the universe to expand faster and faster. However, the new DESI data, combined with other observations (such as those of the cosmic microwave background, supernovae and weak gravitational lensing), suggest that dark energy may not be constant. Instead, it appears that its influence may change over time, perhaps weakening. This is an important clue, because if it were true, the standard model of cosmology (Lambda CDM) would not be able to explain everything and may need to be revised.

DESI researchers looked at a feature called baryon acoustic oscillations (BAO), which acts as a “cosmic ruler.” By measuring how matter is distributed in the universe at different times in its history, they can work out how much dark energy has influenced the expansion. The new data show that this influence may vary, and the evidence for “evolving” dark energy is stronger than the results from DESI’s first year.

However, the scientists stress that more data is needed to be sure, and they are continuing to run tests to rule out errors or unknown effects.

In short, DESI is finding increasingly compelling evidence that dark energy may not be constant, but changing over time, opening the door to new discoveries about the nature of the universe.

How reliable is the hint that dark energy is evolving?

To evaluate its reliability, we must consider several aspects:

- DESI data is robust and precise: DESI used a huge amount of data (15 million galaxies and quasars) and advanced techniques such as BAO, which are considered very reliable in cosmology. Compared to the first-year results, this new analysis has more than double the data, which increases the precision and confidence in the results. The researchers also ran multiple tests to ensure that the results were not influenced by errors or unexpected effects.

- Taken alone, the DESI data are compatible with the Lambda CDM model, which assumes constant dark energy. However, when combined with other observations (cosmic microwave background, supernovae, gravitational lensing), discrepancies emerge. This suggests that a model with variable dark energy might better fit the overall data.

- Scientists speak of “clues” and “preference” for evolving dark energy, but not definitive proof. In physics, a discovery is considered certain only when it reaches a statistical significance level of 5 sigma (a probability of error of less than 0.00006%). The DESI results, combined with other data, arrive at a level between 2.8 and 4.2 sigma, depending on the combinations used. This means that there is a low probability (about 0.3% at 3 sigma) that it is a coincidence, but it is still not enough to declare an official discovery. With more data, this significance could increase or decrease.

- This is not the first time that a variable dark energy has been hypothesized. The data from the first year of DESI (2024) also suggested something similar, and now the evidence is getting stronger. However, in the past some 3 sigma signals in physics have disappeared with more data, so caution is needed.

- DESI is a five-year project, and we are only in the third year. In addition, other future experiments (such as those with more powerful telescopes) will provide complementary data. If the next results continue to support this trend, the idea will become more solid.

In conclusion, the suggestion that dark energy is evolving is very interesting and based on solid data, but it is not yet definitive. The evidence is stronger than in the past and DESI's work is serious and well monitored. However, we are not yet at the point where we can say with certainty that the Lambda CDM model is wrong or that dark energy really changes. It is a promising hypothesis, which could revolutionize our understanding of the universe, but it still needs time and further confirmation. For now, it is an idea that scientists take seriously and that deserves to be explored further.

--------------------------------

Reference: New DESI Results Strengthen Hints That Dark Energy May Evolve

You can consult the DESI Key Publications (numerous papers delving into the technical details) at this link

DESI DR2 Results: March 19 Guide

DESI's website