The Pillars of Creation as seen by Webb

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By combining images of the iconic Pillars of Creation from two cameras aboard the James Webb Space Telescope, the Universe has been framed in its infrared glory. Webb's near-infrared image was fused with its mid-infrared image, setting this star-forming region ablaze with new details.

Myriad stars are spread throughout the scene. The stars primarily show up in near-infrared light, marking a contribution of Webb's Near-Infrared Camera (NIRCam). Near-infrared light also reveals thousands of newly formed stars – look for bright orange spheres that lie just outside the dusty pillars.

In mid-infrared light, the dust is on full display. The contributions from Webb's Mid-Infrared Instrument (MIRI) are most apparent in the layers of diffuse, orange dust that drape the top of the image, relaxing into a V. The densest regions of dust are cast in deep indigo hues, obscuring our view of the activities inside the dense pillars.

Dust also makes up the spire-like pillars that extend from the bottom left to the top right. This is one of the reasons why the region is overflowing with stars – dust is a major ingredient of star formation. When knots of gas and dust with sufficient mass form in the pillars, they begin to collapse under their own gravitational attraction, slowly heat up, and eventually form new stars. Newly formed stars are especially apparent at the edges of the top two pillars – they are practically bursting onto the scene.

At the top edge of the second pillar, undulating detail in red hints at even more embedded stars. These are even younger, and are quite active as they form. The lava-like regions capture their periodic ejections. As stars form, they periodically send out supersonic jets that can interact within clouds of material, like these thick pillars of gas and dust. These young stars are estimated to be only a few hundred thousand years old, and will continue to form for millions of years.

Almost everything you see in this scene is local. The distant universe is largely blocked from our view both by the interstellar medium, which is made up of sparse gas and dust located between the stars, and a thick dust lane in our Milky Way galaxy. As a result, the stars take center stage in Webb’s view of the Pillars of Creation.

The Pillars of Creation is a small region within the vast Eagle Nebula, which lies 6,500 light-years away.

MIRI was contributed by ESA and NASA, with the instrument designed and built by a consortium of nationally funded European Institutes (The MIRI European Consortium) in partnership with JPL and the University of Arizona.

Webb's NIRCam was built by a team at the University of Arizona and Lockheed Martin's Advanced Technology Center.

Image Credit: NASA, ESA, CSA, STScI, J. DePasquale (STScI), A. Pagan (STScI), A. M. Koekemoer (STScI)

Image enhancement: Jean-Baptiste Faure

Star-Forming Region N11 in the LMC

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This Hubble Space Telescope picture features a cloudy starscape from an impressive star cluster. This scene is located in the Large Magellanic Cloud, a dwarf galaxy situated about 160 000 light-years away in the constellations Dorado and Mensa. With a mass equal to 10–20% of the mass of the Milky Way, the Large Magellanic Cloud is the largest of the dozens of small galaxies that orbit our galaxy.

The Large Magellanic Cloud is home to several massive stellar nurseries where gas clouds, like those strewn across this image, coalesce into new stars. This image depicts a portion of the galaxy's second-largest star-forming region, which is called N11. (The most massive and prolific star-forming region in the Large Magellanic Cloud, the Tarantula Nebula, is a frequent target for Hubble.) We see bright, young stars lighting up the gas clouds and sculpting clumps of dust with powerful ultraviolet radiation.

This image marries observations made roughly 20 years apart, a testament to Hubble's longevity. The first set of observations, which were carried out in 2002–2003, capitalised on the exquisite sensitivity and resolution of the then-newly-installed Advanced Camera for Surveys. Astronomers turned Hubble toward the N11 star cluster to do something that had never been done before at the time: catalogue all the stars in a young cluster with masses between 10% of the Sun's mass and 100 times the Sun's mass.

The second set of observations came from Hubble's newest camera, the Wide Field Camera 3. These images focused on the dusty clouds that suffuse the cluster, bringing a new perspective on cosmic dust.

Image Credit: ESA/Hubble and NASA, C. Murray, J. Maíz Apellániz

Image enhancement: Jean-Baptiste Faure

Open Cluster Westerlund 2 as seen by Webb

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This star cluster, known as Westerlund 2, resides in a stellar breeding ground known as Gum 29, located 20,000 light-years away from Earth in the constellation Carina (the Keel).

This image of Westerlund 2 uses data from Webb's Near-InfraRed Camera (NIRCam) and Mid-InfraRed Instrument (MIRI). The cluster measures between 6 light-years and 13 light-years across, and is host to some of our Milky Way galaxy's hottest, brightest, and most massive stars. It was also the feature of Hubble's 25th anniversary image in 2015.

This new Webb image captures the bright, brilliant cluster near the top that is packed with young, massive stars whose intense light shapes the entire scene. Below and around them, swirls of orange and red gas form sculpted walls and tangled clouds – material that is being pushed, eroded, and illuminated by the cluster's powerful radiation. Threaded throughout the view are countless tiny stars just beginning to shine, some still surrounded by the gas and dust from which they formed. The soft blues and pinks are wisps of thinner material drifting between the denser clouds. Scattered across the field are also many bright stars much closer to us, whose sharp, star-shaped patterns are created by Webb's optics. The result is a vivid portrait of a stellar nursery in action, where intense energy from newborn stars carves dramatic shapes into the surrounding nebula and drives the ongoing cycle of star formation.

These new Webb observations of Westerlund 2 have revealed, for the first time, the full population of brown dwarfs in this extremely massive young star cluster, including objects as small as about 10 times the mass of Jupiter. This data is allowing astronomers to find several hundred stars with discs in various evolutionary states to facilitate our understanding of how discs evolve and how planets form in such massive young clusters. This image was developed using data from Webb's programme #3523 (M. Guarcello) as part of the Extended Westerlund 1 and 2 Open Clusters Survey (EWOCS).

Image Credit: ESA/Webb, NASA and CSA, V. Almendros-Abad, M. Guarcello, K. Monsch, and the EWOCS team.

Image enhancement: Jean-Baptiste Faure

The Trifid Nebula as seen by Rubin

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The star-forming Trifid Nebula, also known as Messier 20 (M20), as imaged by NSF–DOE Vera C. Rubin Observatory. The Trifid Nebula is an unusual combination of an open cluster of stars, an emission nebula (the pink region), a reflection nebula (the blue region), and a dark nebula (the dark regions).

Image Credit: RubinObs/NOIRLab/SLAC/NSF/DOE/AURA

Image enhancement: Jean-Baptiste Faure

Trifid and Lagoon Nebulae as seen by Rubin

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In this immense image NSF-DOE Vera C. Rubin Observatory offers a brand new view of two old friends: the Trifid and Lagoon Nebulae. The image provides a demonstration of what makes Rubin unique: its combination of an extremely wide field of view and the speed that allows it to take lots of big images in a very short time. Combining images reveals subtle details in the clouds of gas and dust. The more images we can combine, the more detail we see!

This almost 5-gigapixel image combines 678 exposures taken in just 7.2 hours of observing time, and was composed from about two trillion pixels of data in total. No other observatory is capable of producing an image of such a wide area so quickly and with this much depth.

The Trifid Nebula (also referred to as Messier 20) is a standout in the sky. It's a bright, colorful cloud of gas and dust about 5,000 light-years away in the constellation Sagittarius. What makes it especially striking is the combination of features packed into one place: a glowing pink emission nebula, a cool blue reflection nebula, and dark dust lanes that split it into three sections – hence the name "Trifid". Inside, new stars are forming and blasting out strong winds and radiation, carving up the gas around them. It gives us a dramatic glimpse at how massive stars shape their surroundings even as they're being born.

Below the Trifid Nebula in this image is the Lagoon Nebula (or Messier 8), another vibrant stellar nursery glowing about 4,000 light-years away. You can actually spot the Lagoon with just a pair of binoculars or a small telescope. At its heart is a cluster of young, massive stars – their intense radiation lights up the surrounding gas and shapes the swirling clouds into intricate patterns. The Lagoon nebula provides scientists with a great place to study the earliest stages of star formation – how giant clouds collapse, how star clusters take shape, and how newborn stars start to reshape their environment.

This expansive image of Trifid and Lagoon together exposes an intricate web of dust lanes and star clusters that make this part of the Milky Way come alive with cosmic activity. The exquisite detail in the structure of the nebulosity shown here demonstrates the exceptional quality of Rubin's entire system – from its light-collecting power, to its sensitive camera, to its efficient data transfer and processing system. Over ten years, Rubin Observatory will take millions of images and will image each place in the sky, including this one, about 800 times.

Every time we look at the Universe in a new way, we discover new things we never could have predicted – and with Rubin we will see more than we ever have before.

The image was captured by Rubin Observatory using the 3200-megapixel LSST Camera – the largest digital camera in the world.

Image Credit: RubinObs/NOIRLab/SLAC/NSF/DOE/AURA

Image enhancement: Jean-Baptiste Faure

Emission Nebula and Open Cluster IC 2948

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Exploring the gas cloud known as IC 2948 means finding your way across countless nascent stars born in this enormous stellar nursery. And yet, this is just a snippet of a much larger object: the Running Chicken Nebula. This nebula spans an area on the night sky close to 25 full moons, and yet, the area you see here is not even a third of a full moon. Obtaining such a detailed snippet of the nebula was possible thanks to a 1.5-billion-pixel image taken by the VLT Survey Telescope (VST), hosted and operated by ESO.

Located in the constellation of the Centaur (Centaurus), the Running Chicken Nebula is a labyrinth of gas, dust and young stars whose highly intense radiation erodes away the surrounding material. The gas cloud IC 2948 is the brightest region of the nebula. Here, we find creeping dark clouds, shaped like open hands about to grab their surrounding blooming stars.

First discovered more than a century ago, this gas cloud is helping us understand how stars form and behave during their infancy. To spot IC 2948 within the much larger Running Chicken Nebula, locate the chicken’s rear end (or its head, as some people claim). In your search, you may come across other areas like the stunning GUM 41 nebula.

Image Credit: ESO/VPHAS+ team. Acknowledgement: CASU

Image enhancement: Jean-Baptiste Faure

Rosette Nebula NGC 2237 and Open Cluster NGC 2244

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Cradled within the fiery petals of the Rosette Nebula (NGC 2237) is NGC 2244, the young star cluster which it nurtured. The cluster's stars light up the nebula in vibrant hues of red, gold and purple, and opaque towers of dust rise from the billowing clouds around its excavated core. This image, captured by 570-megapixel Department of Energy-fabricated Dark Energy Camera (DECam), mounted on the U.S. National Science Foundation Víctor M. Blanco 4-meter Telescope at Cerro Tololo Inter-American Observatory, a Program of NSF NOIRLab, is being released in celebration of NOIRLab's fifth anniversary.

Image Credit: CTIO/NOIRLab/DOE/NSF/AURA

Image Processing: T.A. Rector (University of Alaska Anchorage/NSF NOIRLab), D. de Martin and M. Zamani (NSF NOIRLab)

Emission Nebula RCW 7

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A visually striking collection of interstellar gas and dust is the focus of this Hubble picture. Named RCW 7, the nebula is located just over 5300 light-years from Earth in the constellation Puppis.

Nebulae are areas of space that are rich in the raw material needed to form new stars. Under the influence of gravity, parts of these molecular clouds collapse until they coalesce into protostars, surrounded by spinning discs of leftover gas and dust. In the case of RCW 7, the protostars forming here are particularly massive, giving off strongly ionising radiation and fierce stellar winds that have transformed it into what is known as a H II region.

H II regions are filled with hydrogen ions – where H I refers to a normal hydrogen atom, H II is hydrogen that has lost its electron. The ultraviolet radiation from the massive protostars excites the hydrogen, causing it to emit light and giving this nebula its soft pinkish glow. Here Hubble is studying a particular massive protostellar binary named IRAS 07299-1651, still in its glowing cocoon of gas in the curling clouds towards the top of the nebula. To expose this star and its siblings, this image was captured using the Wide Field Camera 3 in near-infrared light. The massive protostars here are brightest in ultraviolet light, but they emit plenty of infrared light which can pass through much of the gas and dust around them and be seen by Hubble. Many of the other, larger-looking stars in this image are not part of the nebula, but sit between it and our Solar System.

The creation of an H II region marks the beginning of the end for a molecular cloud. Over only a few million years, the radiation and winds from the massive stars gradually disperse the gas – even more so as the most massive stars come to the end of their lives in supernova explosions. Only a fraction of the gas will be incorporated into new stars in this nebula, with the rest being spread throughout the galaxy to eventually form new molecular clouds.

Image Credit: ESA/Hubble and NASA, J. Tan (Chalmers University and University of Virginia), R. Fedriani (Institute for Astrophysics of Andalusia)

Image enhancement: Jean-Baptiste Faure

Star-Forming Region M42 as seen by the Subaru Telescope

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The Orion Nebula, aka Messier 42 (M42), is a star-forming region in the winter constellation. It is located at a distance of 1,500 light-years from Earth and is known as one of the nearest star-forming regions. Due to its large apparent size, the Orion Nebula is easy to find with the naked eye, and many stars can be seen through an amateur telescope.

At the center of the Orion Nebula is a cluster of massive newborn stars called Trapezium that ionize surrounding hydrogen gas by their ultraviolet light. The ionized gas emits a red glow.

Image Credit: NAOJ

Image enhancement: Jean-Baptiste Faure

Emission and Reflection Nebula Gum 3

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This picture shows the brightly coloured Gum 3 nebula as seen with the VLT Survey Telescope (VST), hosted at ESO's Paranal Observatory in the Chilean Atacama Desert. Attentive viewers may find that part of Gum 3 resembles a Koi fish in this VST image. Equipped with the OmegaCAM instrument, an enormous 268-megapixel camera, the telescope is designed to survey large areas of the southern sky in visible light and take stunning images like this one.

Gum 3 is an interstellar cloud of gas and dust located about 3600 light-years away, between the Monoceros and Canis Major constellations. It is named after Colin Stanley Gum, an Australian astronomer who catalogued 84 nebulae in the southern sky.

When the intense ultraviolet radiation from nearby young stars hits hydrogen atoms in the cloud, they emit visible light at very specific colours, which we see as shades of red and pink in the image. At the same time, tiny particles of dust within the cloud reflect starlight, especially blue colours, similar to what makes the sky look blue here on Earth. This play of colours makes nebulae like this spectacular to look at.

This image shows not only colour, but also the lack of it. Look closely at the area just right of the brightest part of the cloud – right of the pink "Koi-smic fish". Does anything look odd to you? It's not that there really are fewer stars in this dark area; instead, there is a big clump of dust that blocks part of the visible light, hiding the stars from VST and us.

Image Credit: ESO/VPHAS+ team. Ack.: CASU

Image enhancement: Jean-Baptiste Faure

Emission Nebula NGC 6357

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This image, taken by astronomers using the US Department of Energy-fabricated Dark Energy Camera on the Víctor M. Blanco 4-meter Telescope at Cerro Tololo Inter-American Observatory, a Program of NSF's NOIRLab, captures the emission nebula and star-forming region NGC 6357, which is located 8000 light-years away in the direction of the constellation Scorpius. This image reveals bright, young stars surrounded by billowing clouds of dust and gas inside NGC 6357, which is also known as the Lobster Nebula.

NGC 6357 is spanning about 400 light years. The central region in this image is home to Pismis 24, a star cluster that includes some of the most massive stars in our galaxy, some hundreds of times more massive than our own sun.

Image Credit: CTIO/NOIRLab/DOE/NSF/AURA

T.A. Rector (University of Alaska Anchorage/NSF's NOIRLab), J. Miller (Gemini Observatory/NSF's NOIRLab), M. Zamani and D. de Martin (NSF's NOIRLab)

Image enhancement: Jean-Baptiste Faure

Star-Forming Region NGC 604 as seen by Webb

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This image from the James Webb Space Telescope's NIRCam (Near-Infrared Camera) of star-forming region NGC 604 shows how stellar winds from bright, hot young stars carve out cavities in surrounding gas and dust.

Sheltered among NGC 604's dusty envelopes of gas are more than 200 of the hottest, most massive kinds of stars, all in the early stages of their lives. These types of stars are known as B-types and O-types, the latter of which can be more than 100 times the mass of our own Sun. It’s quite rare to find this concentration of them in the nearby Universe. In fact, there’s no similar region within our own Milky Way galaxy. This concentration of massive stars, combined with its relatively close distance, means NGC 604 gives astronomers an opportunity to study these objects at a fascinating time early in their life.

In Webb's near-infrared NIRCam image, the most noticeable features are tendrils and clumps of emission that appear bright red, extending out from areas that look like clearings, or large bubbles in the nebula. Stellar winds from the brightest and hottest young stars have carved out these cavities, while ultraviolet radiation ionises the surrounding gas. This ionised hydrogen appears as a white and blue ghostly glow.

The bright orange streaks in the Webb near-infrared image signify the presence of carbon-based molecules known as polycyclic aromatic hydrocarbons, or PAHs. This material plays an important role in the interstellar medium and the formation of stars and planets, but its origin is a mystery. As you travel further from the immediate clearings of dust, the deeper red signifies molecular hydrogen. This cooler gas is a prime environment for star formation.

Webb's exquisite resolution also provides insights into features that previously appeared unrelated to the main cloud. For example, in Webb's image, there are two bright, young stars carving out holes in dust above the central nebula, connected through diffuse red gas. In visible-light imaging from the Hubble Space Telescope, these appeared as separate splotches.

Webb's view in mid-infrared wavelengths also illustrates a new perspective on the diverse and dynamic activity of this region. Some of the stars seen in this image from the surrounding galaxy are red supergiants – stars that are cool but very large, hundreds of times the diameter of our Sun. Additionally, some of the background galaxies that appeared in the NIRCam image also fade.

NGC 604 is estimated to be around 3.5 million years old. The cloud of glowing gases extends to some 1300 light-years across.

Image Credit: NASA, ESA, CSA, STScI

Image enhancement: Jean-Baptiste Faure

Star-Forming Region N79

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This image from the James Webb Space Telescope features an H II region in the Large Magellanic Cloud (LMC), a satellite galaxy of our Milky Way. This nebula, known as N79, is a region of interstellar atomic hydrogen that is ionised, captured here by Webb's Mid-InfraRed Instrument (MIRI).

N79 is a massive star-forming complex spanning roughly 1630 light-years in the generally unexplored southwest region of the LMC. N79 is typically regarded as a younger version of 30 Doradus (also known as the Tarantula Nebula), another of Webb's recent targets. Research suggests that N79 has a star formation efficiency exceeding that of 30 Doradus by a factor of two over the past 500 000 years.

This particular image centers on one of the three giant molecular cloud complexes, dubbed N79 South (S1 for short). The distinct "starburst" pattern surrounding this bright object is a series of diffraction spikes. All telescopes which use a mirror to collect light, as Webb does, have this form of artifact which arises from the design of the telescope. In Webb's case, the six largest starburst spikes appear because of the hexagonal symmetry of Webb's 18 primary mirror segments. Patterns like these are only noticeable around very bright, compact objects, where all the light comes from the same place. Most galaxies, even though they appear very small to our eyes, are darker and more spread out than a single star, and therefore do not show this pattern.

At the longer wavelengths of light captured by MIRI, Webb's view of N79 showcases the region's glowing gas and dust. This is because mid-infrared light is able to reveal what is happening deeper inside the clouds (while shorter wavelengths of light would be absorbed or scattered by dust grains in the nebula). Some still-embedded protostars also appear in this field.

Star-forming regions such as this are of interest to astronomers because their chemical composition is similar to that of the gigantic star-forming regions observed when the Universe was only a few billion years old and star formation was at its peak. Star-forming regions in our Milky Way galaxy are not producing stars at the same furious rate as N79, and have a different chemical composition. Webb is now providing astronomers the opportunity to compare and contrast observations of star formation in N79 with the telescope's deep observations of distant galaxies in the early Universe.

These observations of N79 are part of a Webb programme that is studying the evolution of the circumstellar discs and envelopes of forming stars over a wide range in mass and at different evolutionary stages. Webb's sensitivity will enable scientists to detect for the first time the planet-forming dust discs around stars of similar mass to that of our Sun at the distance of the LMC.

This image includes 7.7-micron light shown in blue, 10 microns in cyan, 15 microns in yellow, and 21 microns in red (770W, 1000W, 1500W, and 2100W filters, respectively).

Image Credit: ESA/Webb, NASA and CSA, O. Nayak, M. Meixner

Image enhancement: Jean-Baptiste Faure

Emission Nebula IC 1284

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There are two different types of nebulae brought to you in this picture. Each appears with a distinct colour in the visible sky and are captured here using the wide-field camera OmegaCAM on the VLT Survey Telescope (VST), hosted at ESO's Paranal Observatory in the Chilean desert.

The large, bright emission nebula at the center, IC 1284, is a star-forming region composed primarily of hydrogen. Its rosy glow comes from electrons within the hydrogen atoms: they're excited by the radiation from young stars, but then they lose energy and emit a specific colour or wavelength of light. One of the filters on OmegaCAM lets through this particular reddish colour, hence the nebula's look. Meanwhile, another colour filter highlights the blue reflection nebulae NGC 6589 and NGC 6590 in the lower right corner. The dust in a reflection nebula preferentially scatters shorter, bluer wavelengths of light from nearby stars, which is what gives these nebulae their eerie glow. It's the same reason why the sky is blue!

The frame of this image covers an area roughly equivalent in the sky to a full Moon. This image was captured as part of a large ESO public survey, the VST Photometric H alpha Survey of the Southern Galactic Plane and Bulge (VPHAS+), which observes nebulae and stars in visible light to help astronomers understand how stars are born, live and die.

Image Credit: ESO/VPHAS+ team

Image enhancement: Jean-Baptiste Faure

Star-Forming Region Sagittarius C by Webb

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The full view of the James Webb Space Telescope's NIRCam (Near-Infrared Camera) instrument reveals a 50 light-years-wide portion of the Milky Way's dense center. An estimated 500,000 stars shine in this image of the Sagittarius C (Sgr C) region, along with some as-yet unidentified features.

A vast region of ionised hydrogen, shown in cyan, wraps around an infrared-dark cloud, which is so dense that it blocks the light from distant stars behind it. Intriguing needle-like structures in the ionised hydrogen emission lack any uniform orientation. Researchers note the surprising extent of the ionised region, covering about 25 light-years.

A cluster of protostars – stars that are still forming and gaining mass – are producing outflows that glow like a bonfire at the base of the large infrared-dark cloud, indicating that they are emerging from the cloud's protective cocoon and will soon join the ranks of the more mature stars around them. Smaller infrared-dark clouds dot the scene, appearing like holes in the starfield.

Researchers say they have only begun to dig into the wealth of unprecedented high-resolution data that Webb has provided on this region, and many features bear detailed study. This includes the rose-coloured clouds on the right side of the image, which have never been seen in such detail.

Image Credit: NASA, ESA, CSA, STScI, S. Crowe (UVA)

Image enhancement: Jean-Baptiste Faure

Emission Nebula LBN 867

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Observing the night sky has never been so delightful as with this image of LBN 867, the Raspberry Nebula. Captured here by the Nicholas U. Mayall 4-meter Telescope using the Mosaic-3 detector at Kitt Peak National Observatory (KPNO), a Program of NSF's NOIRLab, this nebula is located in the constellation Orion. LBN 867's overall structure, though, is more like an onion than a raspberry: it hosts three different celestial objects in one! The characteristic red bloom of LBN 867 is an emission nebula. It glows as a result of the ionization of hydrogen gas by the light from the star HD 34989. From the center of the image, this main sequence star shines prominently, though it is about as bright as the planet Uranus as seen from Earth. The last object is hidden in plain sight. Notice the subtle bluish glow around HD 34989? This is the reflection nebula vdB 38, which reflects the blue-white light of its host star off local interstellar dust. Combined, the nebulae and star become a cosmic treat for any keen astronomer.

Image Credit: KPNO/NOIRLab/NSD/AURA/T.A. Rector (University of Alaska Anchorage/NSF's NOIRLab)

Image processing: T.A. Rector (University of Alaska Anchorage/NSF's NOIRLab), M. Zamani (NSF's NOIRLab) & D. de Martin (NSF's NOIRLab)

Image enhancement: Jean-Baptiste Faure

Dark Nebula LDN 1622

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The shadowy clouds of Lynds' Dark Nebula (LDN) 1622 are pictured in this observation from the Nicholas U. Mayall 4-meter Telescope at Kitt Peak National Observatory (KPNO), a Program of NSF's NOIRLab. This image was captured in 2018 by the Mosaic-3 instrument, a wide-field camera used to capture large swaths of the night sky from Kitt Peak in Arizona. Mosaic-3 has since been retired to make way for the Dark Energy Spectroscopic Instrument (DESI), the most powerful multi-object survey spectrograph in the world. This swap highlights one of the benefits of ground-based astronomy: the ability to upgrade and replace instruments as new technologies become available.

LDN 1622 is a dark nebula, so called because these dense interstellar clouds of gas and dust blot out light from background objects, appearing as ink-dark clouds against a backdrop of stars. This enigmatic cosmic cloud lies 1300 light-years from Earth in the nearby Orion complex, a star-forming region thronging with young stars and other dark nebulae.

This observation was taken before the 2022 Contreras Fire, which affected KPNO.

Image Credit: KPNO/NOIRLab/NSF/AURA/T. A. Rector Image processing: T.A. Rector (University of Alaska Anchorage/NSF's NOIRLab), M. Zamani (NSF’s NOIRLab) & D. de Martin (NSF's NOIRLab)

Image enhancement: Jean-Baptiste Faure

Variable Star V 372 Orionis

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The bright variable star V 372 Orionis takes center stage in this image from the Hubble Space Telescope, which has also captured a smaller companion star in the upper left of this image. Both stars lie in the Orion Nebula, a colossal region of star formation roughly 1450 light years from Earth.

V 372 Orionis is a particular type of variable star known as an Orion Variable. These young stars experience some tempestuous moods and growing pains, which are visible to astronomers as irregular variations in luminosity. Orion Variables are often associated with diffuse nebulae, and V 372 Orionis is no exception; the patchy gas and dust of the Orion Nebula pervade this scene.

This image overlays data from two of Hubble's instruments. Data from the Advanced Camera for Surveys and Wide Field Camera 3 at infrared and visible wavelengths were layered to reveal rich details of this corner of the Orion Nebula. Hubble also left its own subtle signature on this astronomical portrait in the form of the diffraction spikes surrounding the bright stars. These prominent artefacts are created by starlight interacting with Hubble's inner workings, and as a result they reveal hints of Hubble's structure. The four spikes surrounding the stars in this image are created by four vanes inside Hubble supporting the telescope's secondary mirror. The diffraction spikes of the James Webb Space Telescope, on the other hand, are six-pointed as a result of Webb’s hexagonal mirror segments and 3-legged support structure for the secondary mirror.

Image Credit: ESA/Hubble and NASA, J. Bally, M. Robberto

Image enhancement: Jean-Baptiste Faure

30 Doradus: the Tarantula Nebula

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A snapshot of the Tarantula Nebula (also known as 30 Doradus) is the most recent Picture of the Week from the Hubble Space Telescope. The Tarantula Nebula is a large star-forming region of ionised hydrogen gas that lies 161 000 light years from Earth in the Large Magellanic Cloud, and its turbulent clouds of gas and dust can be seen swirling between the region’s bright, newly-formed stars.

The Tarantula Nebula is a familiar site for Hubble. It is the brightest star-forming region in our galactic neighbourhood and home to the hottest, most massive stars known. This makes it a perfect natural laboratory in which to test out theories of star formation and evolution, and a rich variety of Hubble images of this region have been released to the public in recent years. The James Webb Space Telescope also recently delved into this region, revealing thousands of never-before-seen young stars.

This new image combines data from two different observing proposals. The first was designed to explore the properties of the dust grains that exist in the void between stars and which make up the dark clouds winding through this image. This proposal, which astronomers named Scylla, complements another Hubble observing proposal called Ulysses and is revealing how interstellar dust interacts with starlight in a variety of environments. This image also incorporates data from an observing programme studying star formation in conditions similar to the early Universe, as well as cataloguing the stars of the Tarantula Nebula for future science with Webb.

Image Credit: ESA/Hubble and NASA, C. Murray, E. Sabbi

Acknowledgement: Y.-H. Chu

Image enhancement: Jean-Baptiste Faure

The Tarantula Nebula as seen by Webb

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In this mosaic image stretching 340 light-years across, Webb's Near-Infrared Camera (NIRCam) displays the Tarantula Nebula star-forming region in a new light, including tens of thousands of never-before-seen young stars that were previously shrouded in cosmic dust. The most active region appears to sparkle with massive young stars, appearing pale blue. Scattered among them are still-embedded stars, appearing red, yet to emerge from the dusty cocoon of the nebula. NIRCam is able to detect these dust-enshrouded stars thanks to its unprecedented resolution at near-infrared wavelengths.

To the upper left of the cluster of young stars, and the top of the nebula's cavity, an older star prominently displays NIRCam's distinctive eight diffraction spikes, an artefact of the telescope's structure. Following the top central spike of this star upward, it almost points to a distinctive bubble in the cloud. Young stars still surrounded by dusty material are blowing this bubble, beginning to carve out their own cavity. Astronomers used two of Webb’s spectrographs to take a closer look at this region and determine the chemical makeup of the star and its surrounding gas. This spectral information will tell astronomers about the age of the nebula and how many generations of star birth it has seen.

Farther from the core region of hot young stars, cooler gas takes on a rust colour, telling astronomers that the nebula is rich with complex hydrocarbons. This dense gas is the material that will form future stars. As winds from the massive stars sweep away gas and dust, some of it will pile up and, with gravity's help, form new stars.

Image Credit: NASA, ESA, CSA, and STScI

Image enhancement: Jean-Baptiste Faure