Rubin Observatory's COSMOS image reveals more than 500,000 galaxies in an unprecedented deep view of the Universe

The Vera C. Rubin Observatory has once again demonstrated why it is poised to transform modern astronomy by releasing one of the deepest and most detailed images of the Universe ever captured. The newly unveiled view of the famous COSMOS field showcases more than 500,000 galaxies alongside over 50,000 stars from our own Milky Way, offering scientists and the public an extraordinary glimpse into the vastness of the cosmos.

The image represents the first Early Data Preview based on observations made with the Rubin Observatory's revolutionary LSST Camera, the largest digital camera ever built for astronomy. Instead of relying on a single exposure, researchers combined hundreds of individual observations collected between April 2025 and January 2026 to create an exceptionally deep composite image capable of revealing galaxies across billions of years of cosmic history.

What makes this achievement remarkable is not only the staggering number of visible galaxies but also the incredible range of distances they represent. The COSMOS field, located in the constellation Sextans, has long been one of the most intensively studied regions of the sky because it lies away from the dense plane of the Milky Way, allowing astronomers to peer deep into the distant Universe with minimal interference from foreground stars and dust. The Rubin Observatory's new image pushes this field to unprecedented levels of detail, revealing spiral galaxies, elliptical galaxies, galaxy clusters, interacting systems, and countless faint objects that were previously difficult or impossible to study.

The LSST Camera is uniquely designed for this type of scientific work. With an astonishing resolution of 3,200 megapixels, each image covers an area of the sky roughly equivalent to 45 full moons while maintaining extraordinary sharpness. This combination of an enormous field of view and exceptional sensitivity enables Rubin to observe vast regions of the sky without sacrificing fine detail, a capability unmatched by any previous survey telescope.

Although the released image is breathtaking on its own, it represents only a tiny fraction of Rubin Observatory's full scientific mission. During its decade-long Legacy Survey of Space and Time (LSST), the observatory will repeatedly photograph the entire southern sky every few nights. This continuous monitoring will allow astronomers to detect changes across the Universe, from exploding stars and variable galaxies to potentially hazardous asteroids, comets, and other transient phenomena that appear or disappear over time.

Repeated observations also allow scientists to combine multiple exposures into increasingly deeper images. Every new observation adds more light, making extremely faint and distant galaxies easier to detect while improving image quality. The COSMOS release serves as a powerful demonstration of this technique, showing how Rubin's data will become progressively richer throughout its mission.

Beyond creating beautiful astronomical images, Rubin Observatory is expected to address some of the biggest unanswered questions in cosmology. By mapping billions of galaxies and tracking their evolution across cosmic time, researchers hope to better understand the distribution of dark matter, investigate the mysterious force known as dark energy, and reconstruct how large-scale structures formed throughout the Universe. The enormous dataset will also help scientists study galaxy evolution, star formation, black holes, and the history of the cosmos with unprecedented statistical precision.

The observatory's ability to repeatedly scan the night sky will fundamentally change how astronomers study dynamic events. Instead of taking isolated snapshots, Rubin will effectively produce a time-lapse movie of the Universe, capturing changes that occur over days, months, and years. This approach is expected to lead to countless discoveries, many of which cannot yet be predicted.

For the public, the COSMOS image is equally inspiring. Zooming into the full-resolution version reveals an almost endless sea of galaxies, each containing billions of stars and potentially countless planetary systems. Most of the tiny points of light visible in the image are not stars within our own galaxy but entire galaxies located millions or even billions of light-years away, emphasizing both the immense scale of the Universe and humanity's growing ability to explore it.

The Rubin Observatory's latest release is more than just another spectacular space photograph. It is an early demonstration of what promises to become one of the most ambitious astronomical surveys ever undertaken. As the observatory continues collecting data over the coming years, scientists anticipate discoveries that will reshape our understanding of the Universe, while the public gains access to some of the most detailed cosmic views ever produced. The COSMOS image is only the beginning of a scientific journey that is expected to redefine observational astronomy for decades to come.

Kepler-1934 b: everything we know about this scorching Earth-sized exoplanet

Kepler-1934 b is one of thousands of confirmed exoplanets discovered by NASA's Kepler Space Telescope, yet it stands out as an intriguing example of a small, rocky world orbiting perilously close to its parent star. Although it is unlikely to host life as we know it, the planet provides astronomers with valuable insights into the diversity of terrestrial exoplanets and the extreme environments that exist throughout the Milky Way.

The planet was confirmed in 2021 after detailed analysis of data collected during the Kepler mission. Like the overwhelming majority of Kepler's discoveries, Kepler-1934 b was detected using the transit method. This technique identifies planets by measuring the tiny, periodic decrease in a star's brightness as an orbiting planet passes in front of it from our point of view. Even though the resulting dimming is incredibly small, modern space telescopes can measure these subtle changes with extraordinary precision, allowing scientists to determine a planet's size and orbital characteristics.

Kepler-1934 b orbits the Sun-like star Kepler-1934, a G-type star with an effective temperature of approximately 5,930 Kelvin. The star is slightly larger than our Sun and is located roughly 1,400 light-years from Earth in the direction of the constellation Cygnus. Because of this enormous distance, direct imaging of the planet is currently impossible, making transit observations the primary source of information about the system.

The exoplanet itself is remarkably similar to Earth in size. It has a radius of approximately 0.91 Earth radii, making it slightly smaller than our planet. Current estimates place its mass at about 0.70 Earth masses, indicating that it is most likely a terrestrial world composed primarily of rock and metal rather than gas or ice. These measurements distinguish it from the much larger gas giants and mini-Neptunes that dominate many exoplanet catalogs.

Despite its Earth-like dimensions, Kepler-1934 b is anything but Earth-like in terms of its environment. The planet completes an orbit around its host star in just 1.42 days, compared with Earth's 365-day year. This astonishingly short orbital period means it circles extremely close to its star, at an average distance of only about 0.0247 astronomical units. For comparison, Mercury orbits the Sun at approximately 0.39 astronomical units, placing Kepler-1934 b nearly sixteen times closer to its star than Mercury is to ours.

Such proximity exposes the planet to an extraordinary amount of stellar radiation. Estimates suggest that it receives well over 1,800 times the solar energy that Earth receives from the Sun. As a result, its equilibrium temperature is believed to be around 1,700 Kelvin, or roughly 1,430 degrees Celsius. At these temperatures, rocks could partially melt, many metals would become liquid, and no known form of life could survive on the surface.

The orbit of Kepler-1934 b appears to be essentially circular, with an eccentricity very close to zero. Circular orbits are common among planets located extremely close to their stars because tidal forces gradually eliminate orbital eccentricity over millions or billions of years. Those same tidal interactions almost certainly mean that Kepler-1934 b is tidally locked, with one hemisphere permanently facing its star while the opposite side remains in perpetual darkness. This configuration would produce enormous temperature differences between the day and night sides, although any atmosphere—if one still exists—could redistribute some of that heat.

Whether the planet retains a significant atmosphere remains an open question. The intense stellar radiation and powerful stellar winds associated with such close orbits can gradually strip away atmospheric gases. If Kepler-1934 b once possessed a thick atmosphere, much of it may have been lost over geological time. Alternatively, if volcanic activity remains vigorous, the planet could still maintain a thin atmosphere replenished from its interior. Future observations with next-generation telescopes may help answer this question.

Kepler-1934 b also contributes to one of the most important areas of modern exoplanet research: understanding the population of rocky planets in our galaxy. Every newly confirmed terrestrial exoplanet improves statistical models that describe how planets form and evolve. By comparing worlds like Kepler-1934 b with larger super-Earths, mini-Neptunes, and gas giants, astronomers can better understand why planetary systems exhibit such extraordinary diversity.

The Kepler mission revolutionized astronomy by demonstrating that planets are common throughout the Milky Way. Before its launch in 2009, only a few hundred exoplanets were known. Today, thanks largely to Kepler's observations and subsequent follow-up studies, thousands of confirmed exoplanets have been cataloged. Kepler-1934 b is one of many discoveries that continue to refine our understanding of planetary formation and the frequency of Earth-sized worlds in our galaxy.

Although Kepler-1934 b is far too hot to be considered habitable, its discovery remains scientifically significant. It illustrates that rocky planets can exist under conditions vastly different from those found in our Solar System. Studying these extreme worlds helps astronomers test theories about planetary interiors, atmospheric evolution, tidal interactions, and the long-term effects of intense stellar radiation.

As new observatories continue to expand humanity's ability to study distant planetary systems, worlds like Kepler-1934 b will become increasingly important. While this small, scorched planet may never be a candidate for life, it represents another crucial piece of the cosmic puzzle, reminding us that the universe contains an astonishing variety of planets far beyond anything found in our own celestial neighborhood.

Kepler-1693 c: everything we know about this Earth-sized exoplanet

Kepler-1693 c is an Earth-sized exoplanet orbiting a distant star approximately 2,480 light-years from Earth in the constellation Cygnus. Although it is far too hot to support life as we know it, the planet represents an important piece of the growing catalog of small rocky worlds discovered by NASA's Kepler Space Telescope. Its confirmation demonstrates how modern data analysis techniques continue to uncover previously overlooked planets hidden within the enormous Kepler dataset, expanding our understanding of the diversity and architecture of planetary systems throughout the Milky Way.

The planet orbits the star Kepler-1693, a G-type star that is somewhat smaller and slightly cooler than the Sun. The host star has a radius of roughly 0.86 times that of the Sun and an effective temperature of about 5,500 K, making it broadly solar-like despite being somewhat less luminous. Located nearly 760 parsecs from Earth, the system is too distant for direct imaging with current technology, meaning astronomers rely on indirect observational methods to investigate its planets.

Kepler-1693 c was detected using the transit method, the same technique responsible for the majority of Kepler's discoveries. As the planet passes between its star and Earth, it blocks a tiny fraction of the star's light. These periodic dips in brightness reveal the planet's existence and allow astronomers to determine several of its physical properties. Because the amount of dimming depends on the relative size of the planet and the star, researchers can estimate the planetary radius with remarkable precision, even when the planet itself cannot be seen directly.

Although Kepler originally observed the transit signal years earlier, Kepler-1693 c was not immediately confirmed as a planet. Instead, it remained listed as a planetary candidate while astronomers continued refining detection algorithms and statistical validation techniques. In 2021, it was confirmed as a genuine exoplanet through improved analyses of archival Kepler observations, illustrating how scientific discoveries often continue long after a space mission has ended. Rather than requiring new telescope observations, researchers extracted additional value from existing data by applying more sophisticated computational methods.

Kepler-1693 c has a radius of approximately 0.98 Earth radii, making it almost the same size as our own planet. Because only its radius has been measured directly, its mass remains uncertain. However, planets of this size are generally expected to be predominantly rocky unless future observations suggest otherwise. Without an accurate mass measurement, astronomers cannot yet determine its density, surface gravity, or detailed internal composition with confidence.

The planet completes one orbit around its star every 5.36 days, placing it extremely close to its host star compared with Earth's distance from the Sun. Such a short orbital period means the planet receives an enormous amount of stellar radiation. Estimates indicate that Kepler-1693 c receives nearly 300 times the amount of energy that Earth receives from the Sun, resulting in an equilibrium temperature of roughly 1,060 K, or nearly 790°C (about 1,450°F). At such temperatures, any Earth-like oceans would be impossible, and much of the planetary surface would likely be intensely heated.

Its proximity to the host star also makes tidal locking a plausible outcome. If this has occurred, one hemisphere would permanently face the star while the opposite side would remain in perpetual darkness. Many close-in exoplanets are expected to evolve into this configuration because gravitational interactions gradually synchronize their rotational and orbital periods. Whether Kepler-1693 c is tidally locked has not been directly measured, but theoretical models suggest it is a reasonable possibility for planets orbiting so close to their stars.

The Kepler-1693 system itself is known to host multiple planets. Alongside Kepler-1693 c, astronomers have confirmed Kepler-1693 b, another small planet orbiting farther from the star with a period of approximately 12 days. The system also contains additional planetary candidates that have yet to receive full confirmation. Multi-planet systems like this are especially valuable because they allow scientists to investigate how planetary systems form, migrate, and remain dynamically stable over billions of years.

Because Kepler-1693 c transits its star, it may eventually become a target for future atmospheric studies if observational capabilities improve. At present, however, the star is relatively faint, making detailed atmospheric characterization difficult even for powerful observatories such as the James Webb Space Telescope. Nevertheless, each confirmed Earth-sized transiting planet adds to the statistical sample astronomers use to understand the frequency and diversity of terrestrial worlds across the Galaxy.

Kepler-1693 c is not considered potentially habitable. Its extreme stellar irradiation places it well inside the inner boundary of the habitable zone, where temperatures are far too high for liquid water to remain stable on the surface. Even if the planet formed with substantial amounts of water or a thick atmosphere, prolonged exposure to intense radiation would likely have dramatically altered its environment over time.

Despite its inhospitable conditions, Kepler-1693 c holds considerable scientific importance. Every confirmed Earth-sized planet helps refine theoretical models describing how rocky planets form, evolve, and survive in different stellar environments. Small exoplanets are especially significant because they bridge the gap between our Solar System and the enormous diversity of planetary systems discovered throughout the Milky Way. Understanding why some rocky planets become scorching worlds while others may remain temperate is one of the central goals of modern exoplanet science.

The discovery of Kepler-1693 c also highlights the enduring scientific legacy of NASA's Kepler mission. Although the spacecraft ended operations in 2018, its archive continues to yield new discoveries as researchers develop increasingly sophisticated analytical techniques. The mission transformed planetary science by demonstrating that planets are extraordinarily common throughout our galaxy, with thousands of confirmed worlds ranging from giant gas planets to bodies smaller than Earth. Kepler-1693 c is one more example of how valuable archival astronomical data can remain for decades after it is collected, continually revealing new worlds that deepen our understanding of the universe.

HD 23472 e: a dense Earth-size exoplanet in a remarkable five-planet system

HD 23472 e is a small, intriguing exoplanet orbiting the K-type star HD 23472, also known as TOI-174. Located roughly 127 light-years from Earth, the planet is part of an unusually compact system containing five confirmed worlds. Its discovery and subsequent characterization have attracted particular interest because HD 23472 e is approximately Earth-sized yet appears to have a remarkably high density, raising the possibility that it belongs to the rare class of planets sometimes described as "super-Mercuries."

The planet was identified in 2022 as part of a major study of the HD 23472 planetary system. Researchers combined transit observations with extremely precise radial-velocity measurements obtained with ESPRESSO, the high-resolution spectrograph installed on the European Southern Observatory's Very Large Telescope. This combination was crucial: the transit method revealed the planet's size, while the star's subtle motion under the planet's gravitational influence provided an estimate of its mass. The result was one of the more technically demanding detections of a small exoplanet, demonstrating the ability of modern instruments to measure planetary masses well below that of Earth.

According to the NASA Exoplanet Archive, HD 23472 e has a radius of approximately 0.82 times that of Earth and a mass of about 0.72 Earth masses, although the mass uncertainty is substantial. Its orbital period is just 7.91 days, meaning that a year on HD 23472 e lasts less than eight Earth days. The planet orbits its host star at an average distance of approximately 0.068 astronomical units, far closer to its star than Earth is to the Sun. The measured orbital eccentricity is modest, around 0.07, although the uncertainty is large enough that the precise shape of its orbit remains relatively poorly constrained.

Its physical properties make HD 23472 e particularly interesting. Combining its estimated mass and radius gives an average density of roughly 7.5 grams per cubic centimeter, with large uncertainties. For comparison, Earth's mean density is about 5.5 grams per cubic centimeter, while Mercury's is approximately 5.4 grams per cubic centimeter. The central estimate for HD 23472 e is therefore surprisingly high for a planet of its size. The original research suggested that the two innermost planets in the system, HD 23472 d and HD 23472 e, could be "super-Mercuries"—small planets with unusually large iron cores relative to their overall size. This interpretation is not yet definitive, however, because the uncertainties in their masses and densities remain significant.

The term "super-Mercury" is useful as a description of a possible composition rather than a formally established planetary category. In the case of HD 23472 e, the hypothesis is that a substantial fraction of the planet's interior could consist of iron and other dense materials, leaving a relatively small rocky mantle. Such a structure could have important implications for planetary formation. One possibility is that intense irradiation from the host star removed part of an originally more volatile-rich planet. Another is that the planet formed from material unusually enriched in refractory elements, or that giant impacts stripped away a significant portion of its mantle. At present, the available observations do not uniquely distinguish between these possibilities.

The location of HD 23472 e within its planetary system makes the story even more compelling. The planet is not an isolated world but one member of a tightly packed sequence of five planets. Moving outward from the star, the system contains HD 23472 d, e, f, b, and c, with orbital periods of approximately 3.98, 7.91, 12.16, 17.67, and 29.80 days, respectively. Their estimated radii range from less than Earth's size for the two innermost planets to roughly twice Earth's radius for the two outermost planets. This architecture provides astronomers with a natural laboratory for investigating how planets with different compositions can emerge from the same protoplanetary environment.

HD 23472 e was also challenging to detect because of its proximity to the orbit of HD 23472 d. The two planets have orbital periods of approximately 3.98 and 7.91 days, placing them close to a 2:1 period relationship. The original study noted that HD 23472 e's small size, its proximity to the transit signal of planet d, and its near-resonant orbital relationship contributed to the difficulty of identifying it. The planet's eventual characterization highlights how signals from multiple worlds can overlap or complicate the interpretation of observations, particularly when astronomers are searching for planets only slightly smaller than Earth.

The system's compact architecture may also provide clues about how planetary systems evolve under intense stellar irradiation. The research team found a broad trend in which the estimated gas and water fractions of the planets increase with distance from the host star. The innermost worlds appear to be denser and more likely to be dominated by rocky and metallic material, while the outer planets may retain larger amounts of volatile material. This pattern is consistent with a scenario in which irradiation has played a major role in shaping the planets over billions of years, although the exact evolutionary history remains uncertain.

This makes HD 23472 e scientifically valuable beyond its own characteristics. Comparing it with its neighboring planets allows researchers to study planetary diversity while controlling for some of the variables that normally complicate exoplanet research. All five planets orbit the same star and therefore formed within the same broad protoplanetary disk. Their contrasting sizes, masses, and inferred compositions offer an opportunity to investigate why planets born in the same system can evolve into such different worlds.

The planet's estimated equilibrium temperature also emphasizes how different its environment is from Earth's. NASA's catalog lists an equilibrium temperature of approximately 723 K based on the adopted planetary parameters. This is not a direct measurement of the planet's actual surface temperature and should not be interpreted as a weather forecast or atmospheric temperature. Equilibrium temperature is a model-dependent quantity that generally assumes a simplified energy balance and does not capture the full effects of atmospheric circulation, greenhouse warming, or heat redistribution. Nevertheless, the value indicates that HD 23472 e receives substantially more stellar energy than Earth does.

Because HD 23472 e is relatively small and likely has a rocky composition, it is not an obvious target for atmospheric characterization in the same way as a large, inflated gas giant. Its small radius produces a comparatively weak transit signal, while its proximity to the host star places it in a challenging observational environment. Even so, the system could become increasingly important as observational techniques improve. Better measurements of the planet's mass and radius would directly refine its density and help determine whether the super-Mercury interpretation is robust.

One of the most important limitations in our current understanding of HD 23472 e is therefore the uncertainty surrounding its interior. The published estimate of approximately 0.76 Earth masses, later represented in the NASA Exoplanet Archive at around 0.72 Earth masses, carries an uncertainty of roughly 0.3 Earth masses. Its radius estimate of about 0.82 Earth radii also has significant uncertainty. Because density depends strongly on both mass and radius, these uncertainties propagate into the inferred interior composition. The evidence for a dense, Mercury-like interior is intriguing, but it should be regarded as a scientific hypothesis supported by current measurements rather than a definitive description of the planet's internal structure.

The discovery of HD 23472 e also illustrates the importance of combining different exoplanet detection techniques. Transit observations are particularly effective at measuring planetary radii, but they do not directly reveal mass. Radial-velocity observations provide the complementary information needed to estimate how strongly a planet gravitationally tugs on its star. For a small planet such as HD 23472 e, that stellar motion is extremely subtle. The ability of ESPRESSO to extract such a signal demonstrates the extraordinary precision now possible in exoplanet astronomy and represents an important step toward characterizing increasingly Earth-like worlds.

HD 23472 e is not considered a second Earth, despite its broadly Earth-sized dimensions. Its short orbital period, intense stellar irradiation, and potentially iron-rich interior make it a radically different world from our planet. Its scientific importance lies precisely in that contrast. By studying a planet that is similar to Earth in size but potentially very different in composition and environment, astronomers can test theories about how rocky planets form, lose volatile material, acquire their internal structures, and respond to the radiation of their host stars.

Ultimately, HD 23472 e is best understood as one piece of a much larger planetary puzzle. Its small size, high estimated density, close orbit, and position within a five-planet system make it an exceptional target for comparative exoplanet science. The possibility that it is a super-Mercury is particularly fascinating, but the most valuable feature of the system may be the opportunity to compare several planets that formed around the same star yet appear to have followed very different evolutionary paths. As future observations refine the masses and compositions of HD 23472 e and its neighboring worlds, this compact system could become an important benchmark for understanding why planetary systems produce such a remarkable diversity of worlds.

HD 23472 d: the tiny, ultra-dense exoplanet that may be a super-Mercury

HD 23472 d is a remarkable exoplanet for one simple reason: it is small, extremely dense, and located in a compact planetary system that gives astronomers an unusual laboratory for studying how rocky worlds form and evolve. Orbiting a K-type star roughly every four days, the planet has a radius of about 75% that of Earth but an estimated mass of only around half an Earth mass. Its measured density is therefore surprisingly high, leading researchers to identify it as a strong candidate for a so-called super-Mercury—a small, metal-rich planet with an unusually large iron core relative to its overall size.

HD 23472 d belongs to the five-planet system surrounding the star HD 23472, also known as TOI-174. The system is particularly interesting because its planets occupy tightly packed orbits, with orbital periods ranging from approximately 3.98 days for planet d to nearly 30 days for the outermost known planet, HD 23472 c. The system therefore contains several worlds that formed and evolved under different levels of stellar irradiation, providing astronomers with an opportunity to investigate how a planet's environment can influence its composition.

The discovery and characterization of HD 23472 d were part of a 2022 study led by astronomers using observations from the European Southern Observatory's ESPRESSO spectrograph. The planet was identified through a combination of transit observations and precise radial-velocity measurements. The transit method detects the tiny dip in a star's brightness that occurs when a planet passes across the stellar disk, allowing researchers to estimate the planet's radius. Radial-velocity observations measure the subtle gravitational tug that the planet exerts on its host star, providing information about its mass. Together, these techniques make it possible to estimate a planet's bulk density—one of the most valuable clues to its internal composition.

According to the NASA Exoplanet Archive, HD 23472 d has a radius of approximately 0.75 Earth radii and an estimated mass of about 0.55 Earth masses, although the uncertainties are substantial. It completes one orbit in about 3.9766 days and travels at an average orbital distance of roughly 0.043 astronomical units from its star. For comparison, Mercury orbits the Sun at an average distance of about 0.39 astronomical units. HD 23472 d is therefore extraordinarily close to its host star by Solar System standards.

That proximity has major consequences. The planet receives an estimated 117 times as much stellar energy as Earth receives from the Sun, and its calculated equilibrium temperature is approximately 909 kelvin, or about 636 degrees Celsius. An equilibrium temperature is not the same as a measured surface temperature—it is a theoretical temperature that depends on assumptions about how the planet absorbs and redistributes incoming energy—but it provides an important indication of the extreme environment in which HD 23472 d exists.

The most intriguing feature of HD 23472 d is its density. The current values listed by the NASA Exoplanet Archive give an estimated bulk density of approximately 7.5 grams per cubic centimeter, with large uncertainties. Earth's mean density is about 5.5 grams per cubic centimeter, while Mercury's is about 5.4 grams per cubic centimeter. HD 23472 d's central estimate is therefore unusually high for a planet of its size, although the uncertainty range is broad enough that its exact composition remains unresolved.

This is where the term "super-Mercury" becomes relevant. In exoplanet science, a super-Mercury is generally understood as a small rocky planet with an unusually high proportion of iron and other heavy elements, giving it a disproportionately large metallic core. The term does not mean that the planet is simply a larger version of Mercury. Rather, it describes a class of planets whose bulk composition appears to be more metal-rich than that of typical rocky planets. The 2022 study of HD 23472 proposed that planets d and e could be super-Mercuries based on their high inferred densities and internal-structure modelling.

The comparison with Mercury is especially interesting because both worlds are close to their respective stars, but the resemblance should not be overstated. Mercury is the innermost planet of our Solar System and has a large iron core relative to its size, while HD 23472 d is much smaller than Earth and orbits a different type of star under a radically different set of planetary-system conditions. The evidence for a super-Mercury interpretation comes primarily from the planet's inferred bulk density and models of its interior, not from direct observations of its core. Astronomers therefore cannot yet say with certainty exactly how much iron lies beneath its surface.

HD 23472 d's small size is itself significant. With a radius of only about three-quarters that of Earth, HD 23472 d lies firmly in the realm of small terrestrial-size exoplanets. Measuring the masses of such low-mass planets is technically difficult because their gravitational influence on their host stars is extremely weak. The 2022 research highlighted the ability of ESPRESSO to obtain radial-velocity measurements precise enough to characterize planets among the lowest-mass worlds for which such measurements had been obtained at the time.

HD 23472 d is also important because it is not an isolated planet. It is part of a tightly packed system containing at least five confirmed planets. The innermost three—HD 23472 d, e, and f—are approximately Earth-sized, while planets b and c are larger, with radii around two Earth radii and 1.85 to 1.9 Earth radii, respectively, according to the 2022 characterization and current NASA Exoplanet Archive data. Their orbital periods increase outward from about four days to nearly 30 days.

The architecture of this system may provide clues about how its planets formed. The 2022 study found a pattern in which the estimated gas and water fractions generally increase with distance from the host star. The researchers argued that this trend is consistent with a system shaped by irradiation: planets closer to the star would have experienced stronger heating, potentially losing volatile material more readily, while planets farther away could retain greater amounts of water or gaseous material. In that picture, HD 23472 d represents an especially extreme inner member of a planetary system whose composition changes systematically with distance from its star.

This interpretation also helps explain why HD 23472 d and its neighboring planet HD 23472 e attracted particular attention. Both are small, dense planets on very short-period orbits. The study estimated similar bulk densities for the two worlds and suggested that they could represent a rare pair of super-Mercuries. If that interpretation is confirmed, the system would be an exceptional test case for competing theories of how metal-rich rocky planets form.

One possible explanation for super-Mercury formation is that intense stellar irradiation and atmospheric loss stripped away lighter materials, leaving behind a relatively metal-rich remnant. Another possibility is that the planets formed with unusually large iron cores from the beginning, perhaps because of the conditions in the protoplanetary disk or through giant impacts that removed part of their rocky mantles. Determining which scenario is correct requires more than measuring density alone. Astronomers need better mass and radius measurements, improved models of planetary interiors, and a larger population of comparable planets for statistical comparison.

HD 23472 d is also a reminder of how much information astronomers can extract from tiny changes in starlight and stellar motion. The planet cannot be photographed directly with current instruments, and its physical surface has not been observed. Instead, researchers infer its properties from the way it affects its star. Its radius comes primarily from transit geometry, while its mass is inferred from the star's motion. From these measurements, scientists can estimate density and then test possible interior structures. It is an indirect process, but one that has transformed the study of planets beyond the Solar System.

There is, however, an important scientific caution when discussing HD 23472 d. Calling it a "super-Mercury" is a compelling interpretation, not a direct observation of its core. The mass and density measurements carry significant uncertainties, and different assumptions about a planet's interior can produce different compositional models. The NASA Exoplanet Archive currently lists a mass estimate of about 0.55 Earth masses with an uncertainty of roughly 0.2 Earth masses and a radius of about 0.75 Earth radii with an uncertainty of approximately 0.06 Earth radii. Those uncertainties propagate into the density estimate, which is itself correspondingly uncertain.

Even so, HD 23472 d remains scientifically valuable. Its combination of small size, short orbital period, high irradiation, and apparently high density makes it a particularly useful target for studying the boundary between ordinary rocky planets and metal-rich worlds. Its position within a five-planet system adds another layer of significance: instead of studying one unusual planet in isolation, astronomers can compare multiple worlds that formed around the same star but now experience very different environments.

For now, HD 23472 d is best described as a small, hot, high-density exoplanet and a strong candidate for a super-Mercury composition. Its estimated radius is around 75% that of Earth, its orbital period is just under four days, and its inferred density is high enough to make a metal-rich interior a plausible explanation. Yet the most important story may not be the planet itself, but the planetary system around it. By comparing HD 23472 d with its four known companions, astronomers can investigate how stellar irradiation, orbital architecture, volatile loss, and planetary composition interact over billions of years.

HD 23472 d therefore occupies an intriguing place in modern exoplanet science. It is neither an Earth twin nor a conventional super-Earth, and its extreme environment makes it an unlikely candidate for habitability. Its real importance lies elsewhere: it may preserve evidence of a radically different planetary formation history, encoded in an unusually dense interior. As observations improve and the population of known small exoplanets grows, worlds like HD 23472 d will help scientists determine whether super-Mercuries are rare cosmic oddities or a common outcome of planet formation around other stars.

CD-35 2722 b: the young, massive exoplanet companion challenging how we define a planet

CD-35 2722 b is one of the most unusual objects in the nearby exoplanet population. Discovered in 2011 through direct imaging, this enormous world orbits the young M-dwarf star CD-35 2722 at a projected distance of roughly 67 astronomical units, placing it far beyond the orbital region occupied by the giant planets of our Solar System. With a mass estimated at about 29.5 Jupiter masses and a radius of approximately 1.55 times that of Jupiter, it sits in the poorly defined territory between giant planets and brown dwarfs. Its remarkable properties make it valuable not only for studying how massive planetary companions form, but also for understanding the earliest stages of substellar evolution.

The system is located roughly 22 parsecs, or about 72 light-years, from Earth. Its host star, CD-35 2722 A, is a relatively cool M1-type dwarf with a mass of approximately 0.55 times that of the Sun and a radius of about 0.56 solar radii according to current NASA Exoplanet Archive parameters. The star is also young, with an estimated age of around 100 million years, although age estimates for young stellar systems can carry substantial uncertainty. The companion's youth is particularly important because young substellar objects retain heat from their formation and therefore remain much brighter in the infrared than comparable objects of the same mass would be after billions of years of cooling.

The object now cataloged as CD-35 2722 b was originally identified as CD-35 2722 B, a substellar companion to the nearby young M dwarf. The discovery came from the Gemini NICI Planet-Finding Campaign, which used high-contrast near-infrared imaging to search for faint companions around nearby stars. Astronomers detected the companion at a wide separation of about 67 AU and used observations at multiple epochs to establish that it was physically associated with the star rather than a distant background object. Near-infrared spectroscopy classified the companion as approximately an L4 dwarf, while its spectral characteristics and relatively low surface gravity were consistent with a young substellar object.

Direct imaging was crucial to the discovery. Unlike the transit method, which finds planets when they pass in front of their stars, or the radial-velocity method, which measures the gravitational wobble induced in a star, direct imaging attempts to detect the companion's own light. This is particularly effective for young, massive planets and brown dwarfs because they can still radiate substantial amounts of thermal energy left over from their formation. The challenge is that the host star is vastly brighter than its companion, so sophisticated coronagraphy, adaptive optics, image processing, and infrared observations are required to separate the two signals. CD-35 2722 b became an important example of what these techniques can reveal about young planetary systems.

The object's mass is where the terminology becomes especially interesting. Early evolutionary modeling based on the companion's luminosity and the estimated age of the system produced a mass of about 31 ± 8 Jupiter masses. More recent values listed by the NASA Exoplanet Archive give a mass of approximately 29.5 Jupiter masses, with uncertainties of roughly +5.1 and −4.3 Jupiter masses. These estimates place CD-35 2722 b well above the conventional deuterium-burning threshold often used as a rough dividing line between planets and brown dwarfs, although that threshold is not a universally accepted physical definition of a brown dwarf.

This distinction matters because mass alone does not necessarily tell the complete story of an object's origin. In astronomy, the difference between a planet and a brown dwarf is often discussed in terms of formation history as well as mass. A planet is generally expected to form within a circumstellar disk through processes such as core accretion or gravitational instability, while a brown dwarf can form more like a star through the collapse and fragmentation of a molecular cloud. At roughly 30 Jupiter masses, CD-35 2722 b is massive enough that its formation mechanism is a central scientific question.

Its enormous separation from its host star provides an important clue. At a projected distance of about 67 AU, the companion orbits much farther from its star than Jupiter does from the Sun. Recent studies of its atmospheric chemistry and the chemical relationship between the companion and its host star have suggested that gravitational instability may be a plausible formation pathway. The companion's mass, wide orbit, and estimated planet-to-host mass ratio of roughly 0.05 are consistent with a scenario in which the young circumstellar environment became unstable and fragmented, producing a massive substellar object at a large distance from the star. However, formation histories of individual objects are difficult to establish with absolute certainty, and alternative pathways cannot necessarily be excluded.

The physical appearance of CD-35 2722 b is equally fascinating. Its radius is estimated at about 1.55 times Jupiter's radius, while its mass is nearly 30 times greater than Jupiter's. That combination implies an object with much greater mass but only moderately larger size, reflecting the unusual physics of gas giants and brown dwarfs. As substellar objects become increasingly massive, their interiors become strongly compressed by gravity, so their radii do not increase proportionally with mass. In fact, objects spanning a broad range of brown-dwarf and giant-planet masses can have surprisingly similar physical dimensions.

The companion's atmosphere also offers a window into the physics of young L dwarfs. The original discovery study estimated an effective temperature in the range of approximately 1,700 to 1,900 kelvin and found evidence of relatively low surface gravity. These characteristics are consistent with a young object that has not yet contracted and cooled to the state expected of an old field brown dwarf. Its infrared spectrum showed similarities to dusty L dwarfs, while its colors and absolute magnitudes also resembled those of some much younger planetary-mass companions. This made CD-35 2722 b an especially useful benchmark for comparing the atmospheres of young brown dwarfs and directly imaged giant planets.

More recent atmospheric work has added another layer to the story. High-resolution spectroscopy has been used to investigate the chemical composition of CD-35 2722 b and compare it with that of its host star. The results indicate that, after accounting for systematic uncertainties, the atmospheric metallicity and carbon-isotope measurements of the companion are broadly compatible with the chemical composition of the star. This chemical similarity supports the idea that the two objects formed from the same original reservoir of material and is consistent with a formation scenario involving gravitational instability. The study also found no clear evidence for clouds in the analyzed data, despite the companion's red photometric appearance and its classification as a mid-L dwarf, illustrating how complex the relationship between observed colors and atmospheric cloud properties can be.

CD-35 2722 b also demonstrates why directly imaged companions are so important to exoplanet science. Most exoplanets discovered by transit and radial-velocity surveys are relatively close to their host stars, partly because those methods are much more sensitive to short-period systems. A massive companion separated by dozens of astronomical units would be extraordinarily difficult to detect through the small gravitational wobble of the host star or through a transit. Direct imaging, by contrast, is naturally suited to finding young, luminous objects on wide orbits. As a result, systems such as CD-35 2722 provide astronomers with rare opportunities to study planetary-mass and substellar companions in regions of planetary systems that remain largely inaccessible to conventional detection techniques.

The orbit itself is also extraordinarily long. NASA lists an orbital period of approximately 867.6 years for CD-35 2722 b, based on an orbital radius of about 67 AU. That means astronomers cannot simply watch the object complete an orbit within a human lifetime. Instead, orbital characterization depends on precise astrometric measurements accumulated over many years and on combining those observations with models of the system's dynamics. Continued monitoring will gradually improve estimates of the companion's orbit, inclination, and true separation, potentially helping researchers determine how its current configuration arose.

The system has become even more scientifically intriguing in 2026. A study published in Nature reported evidence for a planetary-mass object orbiting the brown-dwarf companion CD-35 2722 B itself. The researchers used radial-velocity measurements obtained from high-resolution spectra of the brown dwarf with the VLT/CRIRES+ instrument. Their best-fitting model indicated a satellite with a minimum mass of roughly 0.9 Jupiter masses and an orbital period of around 170 days. The result is potentially groundbreaking, but the authors emphasize that the terminology is complicated: the candidate orbits a brown dwarf rather than a conventional planet, and the criteria for calling such an object an exomoon are not formally settled.

If this signal is confirmed through independent observations, the CD-35 2722 system could become a uniquely important laboratory for studying hierarchical systems that do not fit neatly into the familiar categories of star, planet, and moon. The proposed companion is massive enough to resemble a planet, yet it appears to orbit a brown dwarf that itself circles a star. In other words, the system may contain a star, a brown dwarf, and a planetary-mass satellite-like object arranged in a configuration with no close analogue in our Solar System. The researchers' best-fitting model also included a second, less certain candidate with a minimum mass of about 0.28 Jupiter masses and an orbital period of approximately 87 days, although that signal is considerably less secure.

This possible discovery does not change the established properties of CD-35 2722 b itself, but it does make the system even more significant. The brown dwarf traditionally identified as CD-35 2722 B is now also cataloged as CD-35 2722 b in major exoplanet databases, reflecting the evolving conventions used to classify massive substellar companions. The underlying scientific reality, however, remains more nuanced than a simple label: with a mass around 30 Jupiter masses, the object lies firmly in the brown-dwarf regime under commonly used mass-based definitions, even though it is listed in exoplanet catalogs and was originally discovered as a substellar companion through direct imaging.

For researchers, that ambiguity is part of what makes CD-35 2722 b so valuable. It provides a natural test case for examining where the boundary between planets and brown dwarfs should be drawn, whether formation history should be given greater weight than mass, and how objects formed in different environments evolve atmospherically. Its youth makes it bright enough for detailed observations, its wide separation makes it accessible to direct-imaging techniques, and its high mass makes it an important benchmark for theories of substellar formation.

CD-35 2722 b is therefore much more than a distant giant world orbiting a small star. It is a massive, young, directly imaged substellar object whose properties sit at the intersection of planetary science and brown-dwarf astronomy. Its wide orbit challenges simple models of planet formation, its atmosphere offers a rare opportunity to study the evolution of young L dwarfs, and the possible presence of a planetary-mass satellite around its brown-dwarf host could make the broader system one of the most extraordinary known nearby substellar architectures. As astronomers continue to collect astrometric, spectroscopic, and high-resolution infrared observations, CD-35 2722 b is likely to remain an important reference point in the effort to understand how massive worlds form, how they evolve, and where the boundaries between planets, brown dwarfs, and moons truly lie.

K2-413 b: everything we know about the tiny scorching exoplanet orbiting its star in just 19 hours

K2-413 b is one of the smallest confirmed rocky exoplanets discovered by NASA's extended Kepler mission, K2. Although it is far too hot to support life, this remarkable world provides astronomers with valuable insights into the formation, evolution, and survival of terrestrial planets orbiting extremely close to their host stars. Its compact size, ultra-short orbital period, and membership in a multi-planet system make it an important target for researchers seeking to understand how planetary systems develop throughout the Milky Way.

The planet was officially announced in 2022 after being identified through the transit method, which detects the tiny decrease in a star's brightness when a planet passes in front of it. This technique has become one of the most successful methods for discovering exoplanets and was responsible for thousands of discoveries during NASA's Kepler and K2 missions. K2-413 b was identified alongside a second planet in the same system, K2-413 c, demonstrating that even relatively small stars can host multiple compact rocky worlds.

K2-413 b orbits a K-type star, which is cooler and smaller than the Sun. The host star has an estimated surface temperature of about 4,129 Kelvin and lies approximately 285 parsecs, or roughly 930 light-years, from Earth. K-type stars are particularly interesting for exoplanet studies because they combine long lifetimes with relatively stable energy output, making them attractive environments for planetary systems, even though K2-413 b itself is far too close to its star to be habitable.

One of the planet's most striking characteristics is its incredibly short year. K2-413 b completes a full orbit in only about 0.81 days, or approximately 19.5 hours. It circles its star at a distance of just 0.0117 astronomical units, placing it nearly one hundred times closer to its star than Earth is to the Sun. At such a tiny orbital distance, the planet is exposed to intense stellar radiation, producing surface temperatures that would make the existence of liquid water impossible.

Despite its extreme environment, K2-413 b is scientifically fascinating because of its size. The planet has a radius of approximately 0.76 times that of Earth, making it significantly smaller than our planet and one of the smallest confirmed exoplanets known. Current estimates place its mass at around 0.36 Earth masses, suggesting that it is a rocky terrestrial world rather than a gas-rich mini-Neptune or sub-Neptune. Its relatively low mass also indicates a weaker gravitational pull compared with Earth.

The existence of such a small planet so close to its host star raises important questions about planetary formation and survival. Astronomers continue to investigate whether planets like K2-413 b formed near their present locations or migrated inward after forming farther away in the protoplanetary disk. The intense radiation from the star could also have stripped away any primordial atmosphere over billions of years, leaving behind only the dense rocky core observed today. These processes are central to understanding how planetary systems evolve.

The K2-413 system itself offers additional scientific value because it contains at least two confirmed planets. The outer companion, K2-413 c, orbits every 5.33 days and is slightly larger than K2-413 b. Studying both planets within the same stellar environment allows astronomers to compare how orbital distance influences planetary composition, atmospheric evolution, and long-term stability. Such comparisons help refine theoretical models of compact planetary systems that have become increasingly common among Kepler and K2 discoveries.

Although K2-413 b has no realistic potential for habitability, its discovery contributes to the broader effort of understanding rocky planets throughout the galaxy. Every confirmed terrestrial exoplanet improves statistical models describing how frequently Earth-sized worlds occur around different types of stars. These data are essential for future missions that aim to identify planets located within habitable zones where liquid water could exist.

NASA's K2 mission, which continued after the original Kepler spacecraft lost two reaction wheels, demonstrated remarkable resilience by observing different regions of the sky along the ecliptic plane. Despite operating under significant engineering limitations, K2 successfully discovered hundreds of new exoplanets, including compact systems like K2-413. These discoveries continue to expand the catalog of known worlds and provide valuable targets for future observations with advanced observatories such as the James Webb Space Telescope and upcoming next-generation missions.

K2-413 b may never become one of the most famous exoplanets, but it represents an important piece of the growing puzzle of planetary diversity. Its tiny size, rocky composition, blistering orbit, and membership in a multi-planet system illustrate just how varied planetary systems can be across the galaxy. As astronomers continue to refine observational techniques and discover even smaller worlds, planets like K2-413 b help bridge the gap between theoretical models and the astonishing reality of the universe beyond our Solar System.

K2-411 b: exploring the Earth-sized exoplanet orbiting a Sun-like star

K2-411 b is one of the many fascinating rocky worlds discovered beyond our Solar System, yet it stands out because of its remarkable similarity to Earth in terms of size and mass. Although it is far too close to its host star to support life as we know it, this terrestrial exoplanet provides astronomers with an important opportunity to study the diversity of rocky planets throughout the Milky Way and to better understand how Earth-sized worlds form and evolve.

Discovered in 2022, K2-411 b was identified using the transit method, one of the most successful techniques in modern exoplanet science. This method detects tiny decreases in a star's brightness as a planet passes in front of it from our point of view. The discovery was made using data from NASA's extended Kepler mission, known as K2, which continued searching for planets after the original Kepler spacecraft lost two of its reaction wheels. The K2 mission has been responsible for discovering hundreds of confirmed exoplanets, significantly expanding our understanding of planetary systems across the galaxy.

K2-411 b orbits the star K2-411, a G-type main-sequence star with a surface temperature of approximately 5,700 Kelvin, making it broadly comparable to our own Sun in spectral classification. However, despite orbiting a Sun-like star, the planet's environment is dramatically different from anything found within the Solar System because of its extraordinarily tight orbit.

The planet completes one orbit in only about 3.2 Earth days. Its orbital distance is just 0.0511 astronomical units, meaning it circles its host star at only around five percent of the distance between Earth and the Sun. For comparison, Mercury orbits at roughly 0.39 astronomical units, making K2-411 b nearly eight times closer to its star than Mercury is to ours. At such a short distance, the planet is bombarded by intense stellar radiation and experiences extreme temperatures that make the existence of liquid water on its surface highly unlikely.

One of the most interesting aspects of K2-411 b is its physical similarity to Earth. The planet has a radius of approximately 0.99 times that of Earth and a mass of roughly 0.94 Earth masses. These measurements strongly suggest that it is a terrestrial planet composed primarily of rock and metal rather than a gaseous or icy body. Its density is expected to be close to Earth's, indicating a solid surface and an internal structure likely consisting of a metallic core surrounded by a rocky mantle.

Because K2-411 b orbits so closely to its star, astronomers believe it is almost certainly tidally locked. This means one hemisphere permanently faces the star while the opposite side remains in perpetual darkness. Such a configuration creates enormous temperature differences between the day and night sides, potentially driving powerful atmospheric circulation if the planet possesses any significant atmosphere. However, the intense stellar irradiation may have stripped away much or all of any original atmosphere over billions of years, leaving behind a barren rocky surface exposed directly to space.

The discovery of K2-411 b contributes to an increasingly important category of exoplanets: Earth-sized rocky worlds. While many early exoplanet discoveries were giant gas planets similar to Jupiter, improvements in observational techniques now allow astronomers to detect planets with sizes and masses remarkably close to our own world. These discoveries help researchers investigate the transition between rocky planets and those possessing thick gaseous envelopes, improving models of planetary formation and evolution.

Although K2-411 b itself is not considered habitable, studying such planets remains scientifically valuable. By comparing rocky planets under very different environmental conditions, astronomers can better understand how planetary atmospheres evolve, how stellar radiation affects surface conditions, and which factors ultimately determine whether a planet can support life. Every confirmed terrestrial exoplanet adds another data point that refines theories about the frequency of Earth-like planets throughout the galaxy.

K2-411 b also demonstrates the effectiveness of the transit method for characterizing distant worlds. Each transit allows astronomers to determine the planet's radius with remarkable precision, while complementary observations can estimate its mass and orbital characteristics. Together, these measurements provide insights into the planet's composition, density, and likely internal structure. As future observatories continue to improve measurement precision, planets like K2-411 b may become targets for even more detailed investigations of their atmospheres, thermal properties, and interactions with their host stars.

The host system lies approximately 298 parsecs, or about 970 light-years, from Earth. While this distance places it well beyond the reach of any foreseeable spacecraft, it remains accessible to modern astronomical instruments that can continue monitoring the system for additional planets or subtle orbital variations. The possibility of undiscovered companions within the K2-411 system cannot be ruled out, making it an interesting target for future observations.

K2-411 b represents the remarkable progress achieved in exoplanet research over the past few decades. Once, the existence of planets around other stars was purely speculative. Today, astronomers can identify worlds nearly identical to Earth in size, measure their masses, determine their orbital periods with extraordinary precision, and infer their likely compositions from hundreds of light-years away. While K2-411 b is an inhospitable world scorched by its nearby star, it nevertheless serves as an important laboratory for understanding rocky exoplanets and refining the search for truly Earth-like worlds elsewhere in the universe.

LHS 1140 b: the most promising potentially habitable exoplanet discovered so far?

Among the thousands of exoplanets identified over the past three decades, few have generated as much scientific excitement as LHS 1140 b. Located approximately 49 light-years from Earth in the constellation Cetus, this intriguing super-Earth has steadily emerged as one of the strongest candidates in the search for a potentially habitable world beyond our Solar System. Thanks to increasingly precise observations from ground-based observatories and the James Webb Space Telescope (JWST), astronomers now believe that LHS 1140 b may be an ocean-rich planet with a dense atmosphere capable of supporting liquid water under the right conditions. Although there is no evidence of life, the planet has become a primary target in one of modern astronomy's most ambitious quests: determining whether habitable environments exist around other stars.

LHS 1140 b was discovered in 2017 by the MEarth Project, which specializes in detecting Earth-sized planets orbiting nearby red dwarf stars. The planet circles the red dwarf star LHS 1140, an M-type star significantly smaller, cooler, and less luminous than the Sun. Red dwarfs are the most common stars in the Milky Way, making them attractive targets for exoplanet research. Their smaller size also makes it easier to detect planets through the transit method, in which astronomers measure the slight dimming of a star as a planet passes in front of it.

LHS 1140 b orbits its host star every 24.7 days while remaining within the star's habitable zone—the region where temperatures may allow liquid water to exist on a planetary surface if an appropriate atmosphere is present. Because LHS 1140 is much cooler than the Sun, its habitable zone lies much closer to the star than Earth's orbit does around our own. Despite its close orbit, the planet receives only about 40 to 45 percent of the stellar energy that Earth receives from the Sun, resulting in a relatively moderate equilibrium temperature.

The planet belongs to the class known as super-Earths. It has a radius approximately 1.73 times that of Earth and a mass around 5.6 Earth masses, making it substantially larger and heavier than our planet while still appearing to be primarily rocky. Earlier estimates suggested an exceptionally dense world with a massive iron core. However, improved measurements have significantly revised its density downward, indicating that its interior is more complex than initially believed. Rather than being an oversized rocky Earth, LHS 1140 b may contain a substantial amount of water or other volatile materials, fundamentally changing scientists' understanding of its nature.

One of the most important breakthroughs came in 2024 when astronomers analyzed transmission spectra obtained by JWST. As the planet transited its star, a small fraction of the starlight filtered through the planet's atmosphere before reaching the telescope. This technique allows researchers to identify atmospheric gases by detecting their unique spectral fingerprints.

The observations ruled out the possibility that LHS 1140 b possesses a thick hydrogen-rich atmosphere similar to those surrounding mini-Neptunes. Instead, the data favored a much heavier atmosphere, potentially dominated by nitrogen with smaller amounts of water vapor and carbon dioxide. Such an atmosphere would resemble Earth's more closely than that of a gas-rich world, although the evidence remains tentative and requires additional observations for confirmation.

The revised density and atmospheric measurements have led researchers to propose that LHS 1140 b may be a genuine water world. Current models suggest that between roughly 9 and 19 percent of the planet's mass could consist of water, compared with less than 0.1 percent for Earth. Rather than being covered by a global deep ocean, however, climate simulations indicate a more fascinating possibility. Because the planet is probably tidally locked, with one hemisphere permanently facing its star, the dayside could contain a large liquid-water ocean surrounded by an icy surface extending across much of the planet. This "eyeball planet" configuration features a central circular ocean directly beneath the star, while the remainder of the surface remains frozen under perpetual darkness or twilight.

Tidally locked planets were once considered unlikely places for life because scientists feared that one hemisphere would become unbearably hot while the other froze completely. Modern climate models paint a more optimistic picture. If a sufficiently thick atmosphere exists, winds and atmospheric circulation can efficiently transport heat from the illuminated hemisphere to the dark side, moderating temperatures across the globe. Oceans would further stabilize the climate by redistributing thermal energy. These mechanisms make tidally locked planets around red dwarfs far more promising than previously assumed.

Another important advantage of the LHS 1140 system is the relatively calm nature of its host star. Many red dwarfs produce frequent energetic flares capable of stripping planetary atmospheres through intense ultraviolet and X-ray radiation. LHS 1140 appears considerably quieter than many of its stellar counterparts, increasing the likelihood that its planet has retained an atmosphere over billions of years. This stellar stability substantially improves the long-term prospects for habitability.

Observations with the Hubble Space Telescope and JWST have also explored the possibility of water vapor in the atmosphere. Although some spectral features are consistent with water, scientists remain cautious because stellar activity can complicate the interpretation of transit data. Sophisticated analyses that account for starspots and bright regions on the stellar surface have strengthened confidence that the observed signals are not solely artifacts of stellar variability, but no single atmospheric molecule has yet been detected with overwhelming statistical certainty.

In 2026, researchers announced another milestone by reporting the first confirmed detection of an atmosphere around a rocky exoplanet located within the habitable zone. Using infrared observations, astronomers identified helium escaping from the upper atmosphere of LHS 1140 b. The escaping helium indicates that the planet has successfully retained an atmosphere despite billions of years of stellar radiation. Scientists interpret this as strong evidence that heavier gases, potentially including nitrogen, carbon dioxide, and water vapor, remain trapped in the lower atmosphere, where they could help maintain stable surface conditions.

Despite these encouraging discoveries, many uncertainties remain. Researchers do not yet know the precise composition of the atmosphere, whether stable liquid water currently exists on the surface, how deep any oceans might be, or whether geological activity continues to recycle carbon through volcanic processes. No biosignatures have been detected, and there is currently no evidence whatsoever for extraterrestrial life on LHS 1140 b.

Nevertheless, the planet represents one of the most attractive laboratories for studying planetary habitability outside the Solar System. Unlike many previously discovered exoplanets that are either too hot, too large, or orbit highly active stars, LHS 1140 b combines several favorable characteristics: a rocky composition, location within the habitable zone, a relatively quiet host star, evidence pointing toward a substantial atmosphere, and the possibility of abundant surface water. Together, these factors make it one of the most compelling worlds known for future atmospheric characterization.

The coming years promise even greater advances. Additional JWST observations will refine measurements of atmospheric gases, while next-generation observatories such as the Extremely Large Telescope in Chile and future dedicated space missions will provide much higher sensitivity. These instruments may eventually determine whether the atmosphere contains gases associated with geological activity or, in the most optimistic scenario, potential biosignatures.

LHS 1140 b has rapidly evolved from an interesting exoplanet into one of astronomy's highest-priority targets. Although it is far too early to describe it as an inhabited world, the accumulating evidence suggests that it may possess many of the fundamental ingredients required for habitability. Every new observation helps narrow the possibilities, bringing scientists closer to answering one of humanity's oldest questions: whether Earth is unique or merely one of many life-friendly worlds scattered throughout our galaxy.

Kepler-138 e: the hidden exoplanet at the edge of its star's habitable zone

The discovery of thousands of exoplanets has revealed that planetary systems are often far more diverse than our own Solar System. Among these remarkable discoveries, the Kepler-138 system has emerged as one of the most intriguing. While much of the scientific attention has focused on the likely water worlds Kepler-138 c and Kepler-138 d, another member of the system has captured the imagination of astronomers: Kepler-138 e. Unlike its siblings, this planet has never been directly observed transiting its host star. Instead, its existence was inferred through its gravitational influence on the other planets, making it one of the most fascinating hidden worlds discovered to date.

Kepler-138 is a relatively small and cool red dwarf star located approximately 218 light-years from Earth in the constellation Lyra. Red dwarfs are the most common type of star in the Milky Way, and because of their low luminosity, their habitable zones lie much closer to the star than the Earth's distance from the Sun. The Kepler Space Telescope originally detected three planets orbiting this star, but subsequent observations using NASA's Hubble Space Telescope, the retired Spitzer Space Telescope, and high-precision measurements from the Keck Observatory revealed that the system is more complex than initially believed. Detailed photodynamical modeling uncovered evidence for a previously unknown fourth planet, Kepler-138 e, whose presence explains subtle variations in the timing of the other planets' transits.

Unlike the three inner planets, Kepler-138 e does not pass directly between its star and Earth. As a result, astronomers cannot determine its radius through the transit method, nor can they directly study its atmosphere using transit spectroscopy. Instead, researchers identified the planet by carefully analyzing transit timing variations, a technique that measures tiny changes in when planets cross in front of their star. Every planet exerts a gravitational pull on its neighbors, causing slight deviations from perfectly regular orbits. By modeling these complex interactions, scientists concluded that the observed variations could only be explained by the existence of an additional planet orbiting farther from the star.

Current models indicate that Kepler-138 e orbits near the inner edge of the star's habitable zone. This is the region around a star where temperatures could potentially allow liquid water to exist on a planet's surface under suitable atmospheric conditions. However, being located within the habitable zone does not automatically make a planet habitable. The actual surface environment depends on many factors, including atmospheric composition, pressure, cloud cover, planetary mass, magnetic field strength, geological activity, and the long-term behavior of the host star. Since none of these properties are currently known for Kepler-138 e, any discussion of its habitability remains speculative.

The Kepler-138 system has become particularly important because it challenged long-standing assumptions about small exoplanets. For years, astronomers believed that planets smaller than about 1.7 times Earth's radius were almost always rocky "super-Earths." However, detailed studies of Kepler-138 c and Kepler-138 d revealed that although they are only about 1.5 times Earth's diameter, their masses and densities indicate they likely contain enormous amounts of water or other volatile materials rather than being composed primarily of rock and metal. Researchers estimate that as much as half of their volume could consist of water existing as high-pressure ice, supercritical fluid, or steam beneath dense atmospheres. These findings provided some of the strongest evidence yet for the existence of genuine water worlds.

The existence of these neighboring water-rich planets naturally raises questions about Kepler-138 e. Could it also be a water world? At present, astronomers simply do not know. Without direct measurements of its size and density, it is impossible to determine its internal composition. Nevertheless, because all four planets likely formed from the same protoplanetary disk, researchers consider it plausible that Kepler-138 e shares certain characteristics with its neighboring planets. If so, it could possess a significant inventory of water and volatile materials. Whether those materials exist as deep oceans, high-pressure ice layers, or thick steam envelopes depends on conditions that remain beyond current observational capabilities.

One of the greatest challenges in studying Kepler-138 e is that it does not transit its host star. Most of the detailed information astronomers have obtained about exoplanets—including their radii, atmospheric compositions, and even weather patterns—comes from transit observations. Because Kepler-138 e never crosses the stellar disk from our viewpoint, many of these powerful observational techniques cannot currently be applied. Future advances in high-precision radial velocity measurements or direct imaging technologies may eventually provide additional information, but for now the planet remains largely hidden from view.

The discovery of Kepler-138 e also demonstrates the extraordinary precision of modern exoplanet science. Rather than observing the planet directly, astronomers detected its gravitational fingerprint within an intricate system of orbital interactions. This achievement highlights how invisible planets can still be discovered through their effects on neighboring worlds, allowing scientists to reconstruct entire planetary systems using sophisticated mathematical models.

Kepler-138 e is therefore significant not because it has already revealed all its secrets, but because it represents the frontier of exoplanet research. It sits within a planetary system that has already transformed our understanding of small planets, showing that Earth-sized worlds are not necessarily rocky and that water-rich planets may be more common than previously believed. As next-generation observatories and more sensitive instruments come online over the coming decades, Kepler-138 e may eventually become one of the most important targets for studying the diversity of potentially habitable planets orbiting red dwarf stars.

Although much about Kepler-138 e remains unknown, its discovery underscores one of the most exciting realities of modern astronomy: even worlds that cannot be seen directly can reveal themselves through the subtle laws of gravity. Every improvement in observational precision brings scientists closer to understanding these hidden planets, expanding our knowledge of how planetary systems form, evolve, and perhaps, under the right conditions, support environments where life could exist.