Universe Today

The European Space Agency has retired its Ariane 5 rocket, and all eyes are on its next generation, Ariane 6. The rocket’s pieces have been arriving at the Kourou facility in French Guiana and are now assembled.  ESA has now announced they’ll attempt a test launch on July 9th and hope to complete a second flight before the end of 2024. This new heavy-life rocket has a re-ignitable upper stage, allowing it to launch multiple payloads into different orbits.

“Ariane 6 marks a new era of autonomous, versatile European space travel,” said ESA Director General Josef Aschbacher, who announced the launch data at the Innovation and Leadership in Aerospace (ILA) Berlin Air Show on June 5, 2024. “This powerful rocket is the culmination of many years of dedication and ingenuity from thousands across Europe and, as it launches, it will re-establish Europe’s independent access to space. … I would like to thank the teams on the ground for their tireless hard work, teamwork and dedication in this last stretch of the inaugural launch campaign. Ariane 6 is Europe’s rocket for the needs of today, adaptable to our future ambitions.”

An overview of Europe’s new rocket, Ariane 6. Credit: ESA.

Ariane 6 has been in the works since the early 2010s to be a replacement the workhorse Ariane 5, which is no longer in production. Ariane 5’s first successful launch was in 1998, and since then has sent 109 spacecraft on their way, including the first ATV Jules Verne to the International Space Station and the James Webb Space Telescope to the second LaGrange point 1.5 million km (1 million miles) from Earth.

Ariane 6 is an expendable launch vehicle – not reusable like SpaceX’s rockets — that comes in two versions, with a modular design that can be customized: the rocket can use either two or four P120C strap-on boosters, depending on mission requirements. With the various designs, it can put a 4,500 kg payload into a geostationary transfer orbit or 10,300kg into low Earth orbit using the two boosters, and with four side boosters, it can launch 11,500 kg into a geostationary transfer orbit and 20,600kg into low Earth orbit. The re-ignitable upper stage allows for multiple satellites to launch on a single flight.

The Ariane 6 rocket test firing on its launch pad at the European Spaceport in French Guiana. Credit: ESA

Ariane 6 was developed at a cost of just under 4 billion euros ($3.9 billion) and was originally planned for its first launch in July 2020. However, the project has been hampered by several delays, including work-related issues during the Covid-19 pandemic.

The rocket has undergone several tests in the past few years, and in November of 2023, a full fueled Ariane 6 was tested on the launchpad, firing its engines for several minutes, simulating a flight to space.

“The announcement of the scheduled date for Ariane 6’s first flight puts us on the home stretch of the launch campaign and we are fully engaged in completing the very last steps,” said Martin Sion, CEO of ArianeGroup, the prime contractor of the Arian 6. “This flight will mark the culmination of years of development and testing by the teams at ArianeGroup and its partners across Europe. It will pave the way for commercial operations and a significant ramp-up over the next two years. Ariane 6 is a powerful, versatile and scalable launcher that will ensure Europe’s autonomous access to space.”

Part of the first Ariane 6 rocket inside the Vehicle Assembly Building, Kourou, French Guiana earlier in 2024. Credit: ESA/CNES/Arianespace/Arianegroup.

At the Spaceport in French Guiana, various payloads have been integrated on Ariane 6’s payload carrier. One major milestone must be met before launch: a full wet dress rehearsal, which is having a fully fueled vehicle going through all the steps of a countdown, but not the actual ignition of the rocket engines. Once this activity has been completed, the Ariane 6 Task Force will provide an update, confirming the date for the inaugural flight.

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I have always wanted a 3D printer but never quite found a good enough reason to get one. Seeing that NASA are now 3D printing metal is even more tantalising than a plastic 3D printer. However, thinking about it, surely it is just a computer controlled soldering iron! I’m sure it’s far more advanced than that! Turns out that the first print really wasn’t much to right home about, just an s-curve deposited onto a metal plate! It does however prove and demonstrate the principle that a laser can liquify stainless steel and then deposit it precisely in a weightless environment. 

Arguably 3D printers have revolutionised manufacturing and prototyping industry.   The invention of them has been attributed to Chuck Hull who in 1983 but it’s more true to say he laid the foundations. Hull developed a technique known as stereolithography which involved creating 3D objects by curing thin layers of a photopolymer with UV light. The 3D printers that are commercially available came 5 years later in 1988.

NASA and ESA have been interested in 3D printing in space to make repair/improvement engineering far cheaper, sustainable and timely. Instead of waiting for parts to be shipped up to the ISS. To that end there has been a more conventional plastic 3D printer on board the ISS since 2014 because a 3D printed replacement is far simpler and more cost effective. Indeed ESA are trying to create a circular space economy to recycle materials already in orbit. It makes far more sense to repurpose existing materials in orbit – such as metal from old satellites – to make new tools or parts removing the need for rocket launches to transport them.

In November 2014, NASA astronaut Butch Wilmore installed a 3-D printer made by Made in Space in the Columbus laboratory’s Microgravity Science Glovebox on the International Space Station. Credit: NASA TV

The metal printer that is now on board the International Space Station employs stainless steel wire being fed onto the medium being printed upon. A high power laser which is a million times more powerful than a laser pointer then heats it up melting a small section. As the steel wire feeds into the melt pool it melts, adding to the metal, making it slightly raised. 

Unlike a 3D printer you may have (or I may be trying to justify) which you can control from your own computer, the printer on ISS is controlled entirely from the ground. The crew do have tasks however, they have to open a nitrogen and venting valve before the printing can start. I guess it’s almost the equivalent of putting the paper in your printer at home! 

The printer was developed by a team led by Airbus under the ESA Directorate of the Human and Robotic Exploration contract. It arrived on the ISS in January 2024 where the 180kg printer was installed in the ESA Columbus Module. 

The next step for the printer is to print four shapes that have been chosen for full-scale 3D printing. They will then be returned to Earth for analysis and comparison against reference prints already created in normal gravity. The teams hope to explore how microgravity impacts 3D printing. Two of the 3D printed parts will go to the Materials and Electrical Components Lab at ESTEC in Netherlands. The other two will go to the European Astronaut Centre at the Technical University of Denmark.

Source : First metal 3D printing on Space Station

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What is Dark Matter? That question is prominent in discussions about the nature of the Universe. There are many proposed explanations for dark matter, both within the Standard Model and outside of it.

One proposed component of dark matter is primordial black holes, created in the early Universe without a collapsing star as a progenitor.

The dark matter problem is a missing mass problem. Galaxies should not hold themselves together according to their observable mass. Their observable mass is stars, gas, dust, and a sprinkling of planets.

Some other form of mass must be present to prevent galaxies from essentially dissipating. Dark matter is a placeholder name for whatever that missing mass may be. Astronomer Fritz Zwicky first used the term in 1933 when he observed the Coma Cluster and found indications of missing mass. About 90% of the Coma Cluster is missing mass, which Zwicky called “dunkle Materie.”

This Hubble Space Telescope mosaic shows a portion of the immense Coma galaxy cluster that contains more than 1,000 galaxies and is located 300 million light-years away. The rapid motion of its galaxies was the first clue that dark matter existed. Image Credit: NASA, ESA, J. Mack (STScI) and J. Madrid (Australian Telescope National Facility

Primordial black holes (PBHs) are one leading candidate for dark matter. In the Universe’s earliest times, pockets of dense subatomic matter may have formed naturally. Once dense enough, they could’ve collapsed directly into black holes. Unlike their astrophysical counterparts, they had no stellar progenitors.

Recent JWST observations and LIGO/Virgo results support the idea that PBHs are dark matter. Some researchers go further and say that this evidence supports the idea that dark matter is exclusively made of PBHs and has no other components.

New research suggests that some of the early PBHs would merge and that LIGO/Virgo can detect the gravitational waves from mergers. The research is “Constraints on primordial black holes from LIGO-Virgo-KAGRA O3 events.” The lead author is M. Andres-Carcasona, a PhD student at the Institute of High Energy Physics at the Barcelona Institute of Science and Technology.

An image based on a supercomputer simulation of the cosmological environment where primordial gas undergoes the direct collapse into a black hole. Credit: Aaron Smith/TACC/UT-Austin.

In 2015, LIGO (Laser Interferometer Gravitational-Wave Observatory) detected its first black hole merger. At the time, researchers heralded this new window into the Universe. Until then, astronomical observations were based on electromagnetic radiation, but LIGO/Virgo changed that.

Now, Japan has joined the LIGO/Virgo collaboration with their Karga gravitational wave observatory, and the international effort is named LIGO/Virgo/Karga (LVK.) Together, the three observatories gather data on gravitational waves.

“Previous works have explored the use of GW data to find direct or indirect evidence of PBHs,” the authors write. “Specifically targeted searches of subsolar mass compact objects, which would provide a smoking gun signal of the existence of PBHs have so far been unsuccessful.”

The authors point out that within our growing body of GW data, there may be indications of PBHs that were missed by other researchers’ methods. They write that some of the component masses “… fall in regions where astrophysical models do not predict them, potentially suggesting for a PBH population,” they write.

This ESA graphic shows how we might discover primordial black holes and help solve the dark matter mystery using the JWST and LISA, the Laser Interferometer Space Antenna. Unfortunately, LISA’s launch is at least a decade away. Image Credit: ESA

The mass function of PBHs plays a large role in the formation of PBHs. Their goal is to update the mass constraints on PBHs in GW data. “One of our aims is to derive constraints which do not depend significantly on the underlying formation scenario. Thus, we consider a variety of different PBH mass functions,” they explain.

The two underlying formation scenarios they mention are astrophysical and primordial. Within the primordial category, there are different ways that PBHs can form, and they’re all tangled up with mass function. The authors explain that PBHs could explain the totality of dark matter, but only if they’re within the range of 10-16 to 10-12 solar masses.

“Lighter PBHs would be evaporating today and can constitute only a small portion of the DM,” they write.

Astrophysical BHs form binaries and can merge, sending out gravitational waves. If PBHs merge, they would also send out gravitational waves. It’s possible that some of these mergers are behind some of the GW data detected by LIGO/Virgo/Karga in its third observational run. The researchers present their results in terms of a pessimistic case and an optimistic case. The pessimistic case says that all GW observations are from Astrophysical Black Hole (ABH) mergers, while the optimistic case suggests that some are from PBH mergers.

Their research and its results involve an awfully large number of complicated physical terms and relationships. But the main question is whether PBHs can comprise dark matter, either partly or wholly. In that context, what do the results boil down to?

This artist’s illustration shows small black holes in the accretion disk of a supermassive black hole. In early 2024, a team of researchers found evidence of a small black hole inside the accretion disk of a supermassive black hole. The small BH, if it exists, is between 100 to 10,000 solar masses. At the bottom of that range, it’s the same mass as a PBH. It’s not thought to be primordial, but it indicates how much we’ve yet to learn about black holes. Credit: Caltech/R. Hurt (IPAC)

The researchers say that in their analysis of a population of both astrophysical and primordial binaries, PBHs cannot entirely comprise dark matter. At most, they can make up a small portion of it.

“… in a population of binaries consisting of primordial and astrophysical black holes, we find that, in every scenario, the PBHs can make up at most fPBH less than or equal to 10-3 of dark matter in the mass range 1-200 solar masses.”

fPBH represents the fraction of dark matter that PBHs can comprise, 10-3 means 0.001, and the solar mass range is self-explanatory. It doesn’t take a physicist to understand what they’re saying. PBHs can make up only a tiny fraction of dark matter in their analysis.

This may not be a headline-generating study. It’s a look under the hood of astrophysics and cosmology, where teams of researchers work hard to incrementally constrain and define different phenomena. But that doesn’t undermine its significance.

One day, there might be a headline that screams, “Physicists Identify Dark Matter! Universe’s Big Questions Answered!”

If that ever happens, hundreds and thousands of studies like this one will be behind it.

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NASA are planning on building a telescope to hunt for habitable worlds. The imaginatively named ‘Habitable Worlds Observatory’ is at least a decade away but NASA have started to develop the underlying technology needed. The contracts have been awarded to three companies to research the next-generation optics, mission designs and telescope features at a cost of $17.5 million. Work should begin late summer 2024.

The Habitable Worlds Observatory (HWO) is a mission to launch a large space telescope with the main purpose of directly imaging Earth-like planets around stars like our Sun. It will also be able to study their atmosphere to look for chemical signatures for signs of life. The mission is very much in its early planning stages with working groups looking at the  science goals and how to achieve them. 

This is an artist’s illustration of the exoplanet TRAPPIST-1d, a potentially habitable exoplanet about 40 light-years away. Image Credit: By NASA/JPL-Caltech – Cropped from: PIA22093: TRAPPIST-1 Planet Lineup – Updated Feb. 2018, Public Domain, https://commons.wikimedia.org/w/index.php?curid=76364484

It is thought that, based on existing exoplanet research, one star in every five is likely to have an Earth-like planet in orbit around it. Of course the whole premise of searching for live in the Universe relies on that life being somewhat similar to our own. There may well be life based on a whole different chemistry but if we are to find life then we may as well look for life like ours rather thank take a punt on something completely different. To that end HWO will be on the lookout for chemicals like Oxygen and methane and other signatures that hint at the presence of life. 

In January of this year, NASA requested proposals that will drive and advance the necessary technologies that will be needed for HWO. This may sound a simple ask but taking into consideration what will be needed such as a coronagraph thousands of times more capable than existing to block out light from the host star and an optical system that can remain stationary to the accuracy of the width of an atom during an observation and you realise the challenges ahead. 

Following on from the first phase, NASA has now selected three proposals for two-year fixed price contracts that total a staggering $17.5 million. Sounds like a lot of money but Hubble cost $16 billion to develop and launch. The work is schedule to begin by late summer 2024. Together the contracts will deliver a framework of technology that will support the next phase of the HWO development and include;

• Modelling and sub-systems for an  ultra-stable’ optical system far beyond current capability. This will be delivered by BAE Systems.
• Develop necessary integrated modelling infrastructure that can navigate and compare design interdependencies. This element will be delivered by Lockheed Martin
• Advance the technologies need to support telescope operations such as deployable optical baffles to reduce stray light ingress and structural support for the optical train.  This final element will be delivered by Northrop Grumman.

Artist impression of the James Webb Space Telescope

NASA will of course be in control the whole way through and the output will enable them to plan for the development and build phase of the mission. The work is not being completed in isolation though as there are learnings from the James Webb Space Telescope and the future Nancy Grace Telescope too. 

Source : NASA Awards Advance Technologies for Future Habitable Worlds Mission

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When the James Webb Space Telescope was launched at the end of 2021, we expected stunning images and illuminating scientific results. So far, the powerful space telescope has lived up to our expectations. The JWST has shown us things about the early Universe we never anticipated.

Some of those results are forcing a rewrite of astronomy textbooks.

Textbooks are regularly updated as new evidence works its way through the scientific process. But seldom does new evidence arrive at the speed the JWST is delivering it. Chapters on the Early Universe are in need of a significant update.

At the recent 2024 International Space Science Institute (ISSI) Breakthrough Workshop in Bern, Switzerland, a group of scientists summed up some of the telescope’s results so far. Their work is in a new paper titled “The First Billion Years, According to JWST.” The list of authors is long, and those authors are quick to point out that an even larger group of international scientists played a role. It takes an international scientific community to use JWST observations and advance the “collective understanding of the evolution of the Early Universe,” as the authors write.

The Early Universe is one of the JWST’s primary scientific targets. Its infrared capabilities allow it to see the light from ancient galaxies with greater acuity than any other telescope. The telescope was designed to directly address confounding questions about the high-redshift Universe.

The following three broad questions are foundational issues in cosmology that the JWST is addressing.

What are the Physical Properties of the Earliest Galaxies? The JWST captured these images of 19 face-on spiral galaxies as part of the Physics at High Angular resolution in Nearby GalaxieS (PHANGS) program. The telescope has shown us that early galaxies were much larger than expected. Image Credit: NASA, ESA, CSA, STScI, J. Lee (STScI), T. Williams (Oxford), PHANGS Team, E. Wheatley (STScI)

The early Universe and its transformations are fundamental to our understanding of the Universe around us today. Galaxies were in their infancy, stars were forming, and black holes were forming and becoming more massive.

The Hubble Space Telescope was limited to observations at about z=11. The JWST has shoved that boundary aside. Its current high-redshift observations have reached z=14.32. Astronomers think that the JWST will eventually observe galaxies at z=20.

The lookback time of extragalactic observations by their redshift up to z=20. Image Credit: By Sandizer – Own work, CC0, https://commons.wikimedia.org/w/index.php?curid=140812763

The first few hundred million years after the Big Bang is called the Cosmic Dawn. JWST showed us that ancient galaxies during the Cosmic Dawn were much more luminous and, therefore, larger than we expected. The galaxy the telescope found at z=14.32, called JADES-GS-z14-0, has several hundred million solar masses. “This raises the question: How can nature make such a bright, massive, and large galaxy in less than 300 million years?” scientists involved with JWST Advanced Deep Extragalactic Survey (JADES) said in a NASA post.

It also showed us that they were differently shaped, that they contained more dust than expected, and that oxygen was present. The presence of oxygen indicates that generations of stars had already lived and died. “The presence of oxygen so early in the life of this galaxy is a surprise and suggests that multiple generations of very massive stars had already lived their lives before we observed the galaxy,” the researchers wrote in the post.

“All of these observations, together, tell us that JADES-GS-z14-0 is not like the types of galaxies that have been predicted by theoretical models and computer simulations to exist in the very early universe,” they continued.

What is the Nature of Active Galactic Nuclei in Early Galaxies? This image shows Hercules A, a galaxy in the Hercules constellation. The X-ray observations show superheated gas, and the radio observations show jets of particles streaming away from the AGN at the center of the galaxy. The jets are almost 1 million light-years long. Image Credits: X-ray: NASA/CXC/SAO; visual: NASA/STScI; radio: NSF/NRAO/VLA.

Active Galactic Nuclei (AGN) are Supermassive Black Holes (SMBHs) that are actively accreting material and emitting jets and winds.

Quasars are a sub-type of AGN that are extremely luminous and distant, and quasar observations show that SMBHs were present in the centers of galaxies as early as 700 million years after the Big Bang. But their origins were a mystery. Astrophysicists think that these early SMBHs were created from black hole “seeds” that were either “light” or “heavy.” Light seeds had about 10 to 100 solar masses and were stellar remnants. Heavy seeds had 10 to 105 solar masses and came from the direct collapse of gas clouds.

The JWST’s ability to effectively look back in time has allowed it to spot an ancient black hole at about z=10.3 that contains between 107 to 108 solar masses. The Hubble Space Telescope didn’t allow astronomers to measure the stellar mass of entire galaxies the way that the JWST does. Thanks to the JWST’s power, astronomers know that the black hole at z=10.3 has about the same mass as the stellar mass of its entire galaxy. This is in stark contrast to modern galaxies, where the mass of the black hole is only about 0.1% of the entire stellar mass.

Such a massive black hole existing only about 500 million years after the Big Bang is proof that early BHs originated from heavy seeds. This is actually in line with theoretical predictions. So, the textbook authors are now in a position to remove the uncertainty.

When and How Did the Early Universe Become Ionized? This graphical timeline of the Universe shows where the Epoch of Reionization fits in. Image Credit: By NASA – NASA, Public Domain, https://commons.wikimedia.org/w/index.php?curid=6272041

“We know that hydrogen reionization happened, but exactly when and how it happened has been a major missing piece in our understanding of the first billion years.”

From “The First Billion Years According to the JWST.”

We know that in the early Universe, hydrogen became ionized during the Epoch of Reionization (EoR). Light from the first stars, accreting black holes, and galaxies heated and reionized the hydrogen gas in the intergalactic medium (IGM), removing the dense, hot, primordial fog that suffused the early Universe.

Young stars were the primary light source for the reionization. They created expanding bubbles of ionized hydrogen that overlapped one another. Eventually, the bubbles expanded until the entire Universe was ionized.

This was a critical phase in the development of the Universe. It allowed future galaxies, especially dwarf galaxies, to cool their gas and form stars. But scientists aren’t certain how black holes, stars, and galaxies contributed to the reionization or the exact time frame in which it took place. “We know that hydrogen reionization happened, but exactly when and how it happened has been a major missing piece in our understanding of the first billion years,” the authors of the new paper write.

Astronomers knew that Reionization ended about one billion years after the Big Bang, at about redshift z=5-6. But before the JWST, it was difficult to measure the properties of the UV light that caused it. With the JWST’s advanced spectroscopic capabilities, astronomers have narrowed down the parameters of reionization. “We have found spectroscopically confirmed galaxies up to z = 13.2, implying reionization may have started just a few hundred million years after the Big Bang,” the authors write.

JWST results also show that accreting black holes and their AGN likely contributed no more than 25% of the UV light that caused reionization.

These results will require some rewriting of textbook chapters on the EOR, even though there are still lingering questions about it. “There is still significant debate about the primary sources of reionization, in particular, the contribution of faint galaxies,” the authors write. Even though the JWST is extraordinarily powerful, some distant, faint objects are beyond its reach.

The James Webb Space Telescope: humanity’s new favourite science instrument. Image Credit: NASA

The JWST is not even halfway through its mission and has already transformed our understanding of the Universe’s first one billion years. It was built to address questions around the Epoch of Reionization, the first black holes, and the first galaxies and stars. There’s definitely much more to come. Who knows what the sum total of its contributions will be?

As an astronomy writer, I’m extremely grateful to all of the people who brought the JWST to fruition. It took a long time to build, cost a lot more than expected, and was almost cancelled by Congress. Its perilous path to completion makes me even more grateful to be covering its results. The researchers using JWST data are clearly grateful, too.

“We dedicate this paper to the 20,000 people who spent decades to make JWST an incredible discovery machine,” they write.

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On January 19th, 2024, the Japanese Aerospace Exploration Agency (JAXA) successfully landed its Smart Lander for Investigating Moon (SLIM) on the lunar surface. In so doing, JAXA became the fifth national space agency to achieve a soft landing on the Moon – after NASA, the Soviet space program (Interkosmos), the European Space Agency, and the China National Space Agency (CNSA). SLIM has since experienced some technical difficulties, which included upending shortly after landing, and had to be temporarily shut down after experiencing power problems when its first lunar night began.

On the Moon, the day/night cycle lasts fourteen days at a time, which has a drastic effect on missions that rely on solar panels. Nevertheless, SLIM managed to reorient its panels and recharge itself and has survived three consecutive lunar nights since it landed. However, when another lunar night began on May 27th, JAXA announced that they had failed to establish communications with the lander. As a result, all science operations were terminated while mission controllers attempt to reestablish communications, which could happen later this month.

As JAXA stated via its official X account (formerly Twitter):

“We tried again on the night of the 27th, but there was no response from #SLIM. As the sun went down around SLIM on the night of the 27th, it became impossible to generate electricity, so unfortunately this month’s operation will end. Thank you very much for the overwhelming support you have shown us since our post the day before.”

27??????????????????#SLIM ???????????????27??????SLIM??????????????????????? ?????????????????????????????????????????????????????#JAXA

— ????????SLIM (@SLIM_JAXA) May 28, 2024

JAXA further indicated that the command transmission to restore communication was performed using an “unplanned ground station antenna” and with the cooperation of JAXA’s tracking network.” They also indicated that they plan to try reestablishing communications once the current lunar night ends later this month – at which point, they expect the lander will be recharged. “The power was turned off overnight, so we hope that the whole system will be reset and restarted,” they wrote.

The SLIM mission also carried two rovers, which separated from it in lunar orbit and landed independently on the same day. Known as the Lunar Excursion Vehicle-1 and -2 (LEV-1 and LEV-2), these rovers are the first Japanese robotic missions to traverse and explore the lunar surface. According to JAXA, LEV-1 is the world’s first “hopping exploration rover” while LEV-2 is the world’s smallest and lightest. During the four months since they landed, LEV-1 has measure the local temperatures, topography, and taken images.

The rovers can conduct operations autonomously and transmit data to Earth directly without assistance from the lander. As such, JAXA’s mission controllers are still likely to hear from LEV-1 and LEV-2 while attempting to restore communications with SLIM.

Further Reading: Twitter.com

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For a small, lumpy chunk of rock that barely reflects any light, Mars’ Moon Phobos draws a lot of attention. Maybe because it’s one of only two moons to orbit the planet, and its origins are unclear. But some of the attention is probably because we have such great images of it.

Phobos is the largest of Mars’ two moons, the other one being Deimos. Scientists are uncertain about their history. They could be a pair of captured main-belt asteroids, two lobes of what once was a binary asteroid until capture separated them, or a second-generation object formed after Mars had already formed. Or they could be surviving fragments from an ancient collision between more massive objects.

Phobos isn’t very large. It’s about 26 km × 23 km × 18 km and not massive enough to be rounded. Studies of its density show that it’s a rubble-pile body loosely held together by its own gravity.

When the ESA launched its Mars Express Orbiter in 2003, its mission was to study Mars. One of its instruments is the High-Resolution Stereo Camera, a German contribution that produces colour images with up to two meters resolution. The instrument also has a black-and-white mode, and the original image of Phobos was black-and-white.

Andrea Luck is a skilled image processor from Glasgow, Scotland, with a healthy enthusiasm for space images. He decided the original B&W image, which he describes as epic, needed to be updated to colour. “I was kinda tired of seeing this epic photo online only in black and white, so I decided to jazz it up with some colours!” he wrote on his Flickr page.

It’s interesting to note that it’s a single image, not a composite.

Here’s the original B&W image.

This is the original image from the High-Resolution Stereo Camera (HRSC) on ESA’s Mars Express spacecraft. It caught Phobos over Mars’ limb on March 26, 2010. The waviness of Mars in the background is a by-product of HRSC’s line-scanning operation. Image Credit: ESA / DLR / FU Berlin (G. Neukum)

The HRSC’s mission is to take stereographic images of Mars’ surface, capturing geological and morphological details. The goal is to map as much of the surface as possible. But at the bottom of its list of objectives are images of Phobos and Deimos.

The HRSC captured this image of Phobos in 2017. It shows the Stickney Crater, Phobos’ largest impact crater, and the unusual grooves on the moon’s surface. Mars Express images helped scientists conclude that the grooves are likely from impact ejecta. Image Credit: ESA/DLR/FU Berlin. CC BY-SA 3.0 IGO

Images of Phobos have helped scientists better understand the odd moon, but they’re not enough to reach solid conclusions. Fortunately, a mission to Phobos and its sibling Deimos will be launched in a couple of years.

JAXA, the Japan Aerospace Exploration Agency, is launching the MMX mission in 2026. MMX stands for Martian Moons Exploration. Its goal is to understand the origins of Phobos and Deimos. MMX will also return a sample from Phobos in 2031. Once in Earthly labs, those samples should reveal a lot.

But for now, we can enjoy this processed image of Phobos, which captures its nature as a fast-moving, rubble-pile moon with uncertain origins.

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There are plenty of problems that spacecraft designers have to consider. Getting smacked in the sensitive parts by a rock is just one of them, but it is a very important one. A micrometeoroid hitting the wrong part of the spacecraft could jeopardize an entire mission, and the years of work it took to get to the point where the mission was actually in space in the first place. But even if the engineers who design spacecraft know about this risk, how is it best to avoid them? A new programming library from research at NASA could help.

Admittedly, engineers already have a tool for this purpose. NASA’s Meteoroid Engineering Model (MEM) allows them to plug in a planned trajectory for their spacecraft and receive an output that defines where and from which direction they are likely to encounter micrometeoroids.

The James Webb Space Telescope is a perfect example of why such a system is necessary. On its way to the L2 Lagrange point, it has already suffered at least 20 micrometeoroid impacts, at least one of which hit the space telescope’s primary mirror, leaving a dent that still affects the quality of its images to this day.

How do micrometeroids affect spacecraft?
Credit – Chris Pattison YouTube Channel

Due to such high-profile occurrences, spacecraft designers are already aware of the risks. However, many don’t know their trajectories when designing their systems. Without a planned trajectory, the MEM is all but useless.

Enter Althea Moorhead from NASA’s Meteoroid Environment Office at Marshall Space Flight Center and her colleagues Katie Milbrandt from Auburn and Aaron Kingery from ERC, Inc., also based at Marshall. They improved the MEM’s functionality by introducing a library of known spacecraft trajectories and the MEM outputs for each.

Instead of knowing their end trajectory, spacecraft designers would be able to simply look at the library and determine whether there are any significant risks from meteoroids on any number of potential trajectories. In particular, the library includes data on orbital paths around every significant planet, some transfer orbits, and at least two “halo” orbits, where the spacecraft would take advantage of the relative stability of a planet’s Lagrange points.

How Webb deals with the micrometeroid impacts its already suffere.
Credit – Launch Pad Astronomy

The output of the library allows for visualizations of the risks the spacecraft would encounter, which is much easier to understand than complex equations and probabilities for designers who don’t necessarily specialize in micrometeoroid hazards. That was the original impetus for developing the library – to provide generalists who don’t necessarily have time to grok the details of micrometeoroid location and risks but still need to consider it as part of their mission design.

The paper authors stress that the library shouldn’t be used for the formal risk assessment that NASA requires of all missions destined for launch. That requirement can still be met by the MEM itself, along with a well-established orbit. But, if that orbit happens to be informed by the library described in the paper, all the better for it.

Learn More:
Moorhead, Milbrandt, & Kingery – A library of meteoroid environments encountered by spacecraft in the inner solar system
UT – NASA has a Plan to Minimize Future Micrometeoroid Impacts on JWST
UT – What Does Micrometeoroid Damage do to Gossamer Structures Like Webb’s Sunshield?
UT – Ouch. Canadarm2 Took a Direct Hit From a Micrometeorite

Lead Image:
Visualization of one of the trajectories planned out in the new micrometeroid library.
Credit – Moorhead, Milbrandt, & Kingery

The post NASA has a New Database to Predict Meteoroid Hazards for Spaceflight appeared first on Universe Today.

The Standard Model of particle physics does a good job of explaining the interactions between matter’s basic building blocks. But it’s not perfect. It struggles to explain dark matter. Dark matter makes up most of the matter in the Universe, yet we don’t know what it is.

The Standard Model says that whatever dark matter is, it can’t interact with itself. New research may have turned that on its head.

Physicists propose many different candidates for dark matter, including dark photons, weakly interacting massive particles (WIMPs), primordial black holes, and more. Each one is intriguing in its own way, but there’s no confirmation regarding any of them. And each one is a proposed part of the Standard Model.

New research in the journal Astronomy and Astrophysics suggests we may be barking up the wrong tree. It suggests that another model, called the Self-Interacting Dark Matter model, can explain dark matter while the Standard Model and its Lambda Cold Dark Matter (Lambda CDM) simply can’t.

The paper is “An N-body/hydrodynamical simulation study of the merging cluster El Gordo: A compelling case for self-interacting dark matter?” The lead author is Riccardo Valdarnini of SISSA’s (Scuola Internazionale Superiore di Studi Avanzati) Astrophysics and Cosmology group.

El Gordo is an extremely massive, extremely distant galaxy cluster more than seven billion light-years away from Earth. It’s comprised of two galaxy sub-clusters that are colliding with one another at several million kilometres per hour. It’s at the center of a back-and-forth over dark matter and the Lambda CDM.

A 2021 paper claimed that El Gordo presents a challenge for the Lambda-CDM model because it appeared so early in cosmic history, is extremely massive, and has such a high collisional velocity. “Such a fast collision between individually rare massive clusters is unexpected in Lambda cold dark matter cosmology at such high z,” the authors of that paper wrote.

A later paper from 2021 arrived at a lower mass estimate for El Gordo, one that was consistent with Lambda CDM. “Such an extreme mass of El Gordo has stimulated a number of discussions on whether or not the presence of the cluster is in tension with the Lambda CDM paradigm,” those authors wrote. “The new mass is compatible with the current Lambda CDM cosmology.”

A key part of Lambda CDM is that dark matter is both cold and collisionless. In that model, it’s impossible for dark matter particles to collide with one another; they can only interact through gravity and possibly the weak force. This study challenges that notion.

Proving that dark matter can interact with itself via collisions is difficult and complicated. El Gordo is a good place to study the Self-Interacting Dark Matter (SIDM) idea. “There are, however, unique
laboratories that can prove very useful for this purpose, many light years away from us,” said lead author Valdarnini. “These are the massive galaxy clusters, gigantic cosmic structures that, upon collision, determine the most energetic events since the Big Bang.” El Gordo is one of them.

Galaxy clusters like El Gordo can be divided into three components: the galaxies, the dark matter, and the gas mass. The Standard Model says that the colliding gas loses some of its initial energy during the collision. “This is why, after the collision, the peak of gas mass density will lag behind those of dark matter and galaxies,” Valdarnini explained.

But the SIDM says something different. It says that the points where the dark matter reaches its maximum density, called centroids, should be physically separated from the other mass components. The peculiarities of that separation are a signature of SIDM.

Observations of El Gordo show that it consists of two large sub-clusters, the northwest (NW) and the southeast (SE), which are merging into one.

This Hubble Space Telescope image shows El Gordo’s two main components, the NW and SE sub-clusters. Image Credit: NASA, ESA, and J. Jee (University of California, Davis)

X-ray images show different peak locations for the different mass components. The X-ray image below shows a single X-ray emission peak in the SE subcluster and two faint tails elongated beyond the X-ray peak. The X-ray peak precedes the dark matter peak. The Brightest Cluster Galaxy (BCG) is also offset from the SE mass centroid. BCGs are the brightest galaxies in a given cluster, are extremely massive, and are centers of mass in clusters.

“Another notable aspect can be seen in the NW cluster, where the galaxy number density peak is spatially offset from the corresponding mass peak,” Valdarnini explained.

This combined X-ray and infrared image shows X-rays from Chandra in pink, and the blue shows where dark matter is found. Image Credit: X-ray: NASA/CXC/Rutgers/J. Hughes et al.; Infrared: NASA/ESA/CSA, J.M. Diego (IFCA), B.Frye (Univ. of Arizona), P.Kamieneski, T.Carleton & R.Windhorst (ASU)

But those observations alone aren’t enough. In the new paper in Astronomy and Astrophysics, Valdarnini employed a large number of N-body/hydrodynamical simulations to study El Gordo’s physical properties. The systematic simulations aim to match the observations. Each simulation has slightly different parameters, and when a simulation matches observations, those parameters are likely to offer some explanation of the observations.

Valdarnini explains it clearly in the paper. “… the aim of this paper is to determine whether it is possible to construct merger models for the El Gordo cluster that can consistently reproduce the observed X-ray morphology, as well as many of its physical properties.”

The critical part of this work and its simulations concerns the separations between the centers of mass in El Gordo. If simulations can produce that, it’s evidence in favour of SIDM.

“The most significant result of this simulation study is that the relative separations observed between the different mass centroids of the “El Gordo” cluster are naturally explained if the dark matter is self-interacting,” states Valdarnini.

This figure from the research shows some of the simulation results. The red contours show X-ray surface brightness, and the white shows mass density. Green crosses are mass centroids, and red crosses are X-ray surface brightness centroids. Each row is from a separate simulation run with different parameters, and each panel represents a different viewing angle. The middle top panel is of particular interest. It recreates El Gordo’s twin tails particularly well. Image Credit: Valdarnini et al. 2024.

“For this reason, these findings provide an unambiguous signature of a dark matter behaviour that exhibits collisional properties in a very energetic high-redshift cluster collision,” he continued.

It’s a classic “tip of the iceberg scenario.” While these results are in favour of the Self Interacting Dark Matter model, they’re nowhere near conclusive, as Valdarnini makes clear when he talks about inconsistencies in the results.

Valdarnini’s work shows that while the results are an approximation of how dark matter may behave during cluster mergers, there’s a lot more to it. The “underlying physical processes” are extremely complex.

“The study makes a compelling case for the possibility of self-interacting dark matter between colliding clusters as an alternative to the standard collisionless dark matter paradigm,” he concludes.

For most of the eight billion human beings alive today, dark matter is of little consequence in daily life. But if we want to entertain hopes and enjoy daydreams of human civilization lasting for centuries, millennia, or even longer, expanding into space and travelling to other stars, it’s critical that we understand everything we can about nature. The history of human progress parallels our growing understanding of nature.

Understanding dark matter is critical to understanding nature. If we want civilization to persist, a better understanding of everything about nature is the best way forward.

Now, back to our daily lives under the Standard Model.

The post Evidence of Dark Matter Interacting With Itself in El Gordo Merger appeared first on Universe Today.

Our Moon is shrinking and has been doing so since just after its formation ~4.5 billion years ago from a collision with the young Earth. That shrinkage, along with a constant rain of micrometeorites, causes lunar seismic activity. NASA plans to send two instruments to the Moon to measure its moonquakes. Those dual seismometers share technology first used on Mars by the InSight lander to measure more than a thousand marsquakes.

The seismometers make up part of the Farside Seismic Suite (FSS). It will be delivered to the Moon’s Schrödinger Basin at the South Pole, the first such instrument package deployed since the Apollo program seismic payload operated for a brief time in 1971. That program sent back the first moonquake measurements. Subsequent Apollo missions deployed other seismic instruments that transmitted lunar data until late 1977.

JPL engineers and technicians prepare NASA’s Farside Seismic Suite for testing in simulated lunar gravity, which is about one-sixth of Earth’s. The seismometers in the payload will gather the agency’s first seismic data from moonquakes in nearly 50 years. Credit: NASA/JPL-Caltech

The FSS will send back the first such measurements from the Moon’s far side since Apollo days. Its two seismometers will record a “hum” of seismic background vibrations from icrometeorites pelting the surface. In addition, they will record lunar quakes and return data about their intensity and location.

What Do Moonquakes Tell Us?

Quakes give a great deal of information about more than their location and intensity. The way seismic waves travel through the Moon’s structure should give some insight into the density of its various parts. In addition, they help scientists understand the lunar “shrinkage”.

On Earth, seismic waves travel differently through liquid and solid layers. On the Moon, the Apollo 11 seismic experiment gave planetary scientists the first “look” at the lunar interior. For each moonquake, the instrument recorded the strength, duration, and suspected direction of the event.

Apollo 15’s Lunar Surface Experiments Package (ALSEP). It carried a suite of science instruments, including a seismic experiment to detect moonquakes. Courtesy NASA.

Interestingly, that experiment and others did not detect much seismic activity on the lunar far side. Something in the Moon’s interior plays a role in absorbing the waves from far-side quakes. Scientists want to know what that structure is and what properties prevent transmission of quake waves. Of course, not as many quakes occur on the far side. Interestingly, the surface of the far side is much different than the near side. Are these two related? “FSS will offer answers to questions we’ve been asking about the Moon for decades,” said Mark Panning, the FSS principal investigator at JPL and project scientist for InSight. “We cannot wait to start getting this data back.”

From Marsquakes to Moonquakes

In late 2018, the Mars InSight Lander settled onto the surface of the Red Planet. Its mission was to study the interior of Mars. Essentially, it used the Seismic Experiment for Interior Structure (SEIS) to take the planet’s pulse and measure its interior motions. It measured the strength, duration, and direction of marsquakes. It also detected tiny mini-quakes generated by meteorite impacts. Along with a suite of other instruments that measured wind, temperature, and magnetic field variations, SEIS was able to sense vibrations from wind storms and other atmospheric phenomena.

Engineers at NASA Jet Propulsion Laboratory adapted the seismometer technology used on InSight for the FSS suite. There were a few major differences, however. For one thing, lunar gravity is much less than Mars’s, so they had to adapt the seismic suite’s performance to take that into account. Also, temperatures on the Moon are much colder, and of course, there’s no atmosphere to measure.

The FSS suite contains the Very Broadband Seismometer, which is so sensitive it detects ground motions smaller than the size of a hydrogen atom. The other seismometer is called the Short Period sensor and it measures ground motion in three directions using tiny sensors etched onto chips.

FSS’s Science Goals

This payload, its power sources, and thermal controls are expected to operate for a long time, measuring quakes and background “noise” in the lunar structure. Although scientists know a fair amount about the Moon’s interior, the FSS’s sensitive instruments should help them get a more detailed understanding of its structure. The Moon is a differentiated body—meaning that it has layers beneath it crust.

The Apollo mission instruments measured the thickness of the lunar crust, and the GRAIL mission provided more detailed data. The FSS measurements should determine the thickness of the next layer—the deep mantle. That should come from data recordings and measurements of deep moonquakes. The FSS’s landing site in Schrödinger crater is a great location for quake measurements. It’s an impact basin refilled by rock melted during an impact that occurred some 3.8 billion years ago. There is a great deal of evidence for other volcanic activity in the region, including vents and subsequent lava flows.

Seen here during assembly in November 2023, Farside Seismic Suite’s inner cube houses the NASA payload’s large battery (at rear) and its two seismometers. The gold, puck-shaped device holds the Short Period sensor, while the silver enclosure contains the Very Broadband seismometer. These devices will detect moonquakes on the Moon’s far side. Credit: NASA/JPL-Caltech

The FSS seismometer package is slated for launch in 2025 with a projected landing date in 2026. It’s part of a NASA initiative to work with companies to deliver lunar science and technology packages during the Artemis mission timeline. Artemis astronauts will deploy a seismic network using a distributed acoustic sensing capability to do further work in assessing the Moon’s interior.

For More Information

NASA to Measure Moonquakes With Help From InSight Mars Mission
Apollo 11 Seismic Experiment
InSight Lander

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Radio telescopes have an advantage over optical telescopes, in that radio telescope can be used even in cloudy conditions here on Earth. That’s because the longer wavelengths of radio waves can pass through clouds unhindered. However, some wavelengths are still partially obscured by portions of Earth’s atmosphere, especially by the ionosphere which traps human-made Radio Frequency Interference (RFI).  

Astronomers have developed a new calibration technique that allows them to take sharp images in low radio frequencies — between 16 and 30 MHz — for the first time, bypassing the influence of the ionosphere. The astronomers say this will allow them to study things like plasmas emanating from ancient black holes and perhaps even detect exoplanets that orbit small stars.

The technique was developed by an international team of researchers led by astronomers from Leiden University in the Netherlands.

“It’s like putting on a pair of glasses for the first time and no longer seeing blurred,” said Christian Groeneveld from Leiden University, who led the research.

The LOFAR central stations on a specially engineered field (“superterp”) between Exloo and Buinen in Drenthe, in the north east of the Netherlands. Image: Aerophoto Eelde.

The astronomers used the LOFAR telescope in Drenthe, the Netherlands, which is currently one of the best low-frequency radio telescopes in the world. They modified a calibration technique that has been used to improve observations for observing in radio at higher frequencies, around 150 MHz.

“We hoped that we could also extend this technique to lower frequencies, below 30 MHz,” said, Reinout van Weeren, also from Leiden University, who came up with the idea. “And we succeeded.”

To test their technique, they studied several galaxy clusters that had previously only been studied in detail at higher frequencies.

“Our observing strategy consisted of simultaneously observing a bright primary calibrator and the target fields,” the team wrote in their paper. “By scheduling the observation after midnight, we minimized RFI caused by the internal reflection of terrestrial RFI by the ionosphere, which is significantly worse during the day, as ionizing radiation from the Sun increases the column density of ions in the ionosphere.”

Then, they split up their field of view into several smaller “facets” and self-calibrated each facet individually, against the calibrator object. “This yields an improved image and model of the sky, partly corrected for direction dependent effects,” they wrote. They then repeated the calibrations three more times.

Left shows an image of a piece of sky observed with the hitherto best calibration technique. Right shows the same piece of sky with the new technique. More detail is visible, and what were once large, blurry patches now appear as single points. (c) LOFAR/Groeneveld et al.

This was the first time radio images at frequencies between 16 and 30 MHz have been taken. Because of this data, the astronomers said that the radio emissions from these clusters is not evenly distributed across the entire cluster, but rather there is a spot pattern.

According to the researchers, the new calibration technique makes it possible to study radio phenomena in frequencies that were previously hidden.

“There is, of course, a chance that we will eventually discover something unexpected,” said Groeneveld.

Read the press release from Astronomy Netherlands
Read the team’s paper

The post Astronomers Have a New Way to Bypass Earth's Atmosphere appeared first on Universe Today.

The Hubble Space Telescope has been shut down temporarily after one of its gyroscopes sent faulty telemetry readings back to Earth in late May. The venerable space-based observatory, which has been responsible for some of the most remarkable scientific advances of the last three decades, and stunning astrophotography that became a cultural mainstay, is in its thirty-fourth year of operation.

Hubble’s many and varied accomplishments have been achieved despite a plague of technical challenges over the years. Right out of the gate, it launched with blurry vision, due to an improperly polished lens. The problem was fixed with a space shuttle servicing mission in 1993, three years after launch. Four more servicing missions between 1997 and 2009 repaired and upgraded various parts of the spacecraft.

With the retirement of the space shuttle, the space telescope has now been operating for 15 years without servicing.

Pauses in science operations like the current one are common events for Hubble these days, occurring several times a year in recent times. Hubble’s gyroscopes are the usual culprit.

In fact, a faulty gyroscope previously caused a shutdown barely a month ago, in April 2024, and did the same back in November 2023. In every case, NASA was able to get the space telescope back up and running in short order.

That doesn’t mean there is no cause for concern. Gyroscopes help the telescope orient itself in space, keeping it stable to point at astronomical targets in the distant universe. The last servicing mission in 2009 left the telescope with six operational gyroscopes, but it has been running on three since 2018.

Hubble needs all three to operate at full capacity.

The end of a Hubble gyro reveals the hair-thin wires known as flex leads. They carry data and electricity inside the gyro, and their corrosion has caused gyroscope failures in the past. NASA

But having two wouldn’t necessarily be the end of the mission. It would reduce the area of the sky Hubble can observe, and slow down science operations.

Regardless of the outcome of the current troubles, NASA appears confident that this is not the end of the line, stating in a press release on May 31:

“NASA anticipates Hubble will continue making discoveries throughout this decade and possibly into the next, working with other observatories, such as the agency’s James Webb Space Telescope for the benefit of humanity.”

It doesn’t appear that that will be the last word on the subject, however. A press conference has been called for 4PM EDT on June 4, where NASA’s Director of the Astrophysics Division, Mark Clampin, and Hubble’s project Manager, Patrick Crouse, are expected to give an update on Hubble’s condition.

In the event that Hubble is reduced to two working gyroscopes, NASA recently indicated that it would likely put one of them into safe mode, relying on just one gyroscope and keeping the last in good working order for the future.

With just one gyroscope in operation, magnetometers, sun sensors, and star trackers will need to make up for the work that the other gyroscopes used to do. This takes more time, and would reduce Hubble’s working capacity by 20-25%. Hubble would no longer be able to look at objects closer to Earth than Mars, it would be less capable of catching transient events at a moment’s notice, and it would have to pause observations during parts of its orbit when the Moon and Earth get in the way of its star trackers.

But it would keep the mission alive longer, which is good news for astronomers and astronomy fans everywhere. There is even hope for a future Hubble repair mission, an idea proposed by Jared Isaacman, a private astronaut who will command the upcoming Polaris Dawn mission aboard SpaceX’s Dragon capsule. Currently, Dragon is incapable of docking with Hubble, leaving the idea firmly in the speculative stage for the moment.

As for more immediate plans, we’ll have to see what NASA has to say. Stay tuned for the press conference at 4PM June 4.

The post Hubble Pauses its Science Again appeared first on Universe Today.

China says its Chang’e-6 spacecraft has gathered up soil and rocks from the far side of the moon and has lifted off from the surface, beginning a journey to bring the samples back to Earth. The probe’s payload represents the first lunar samples ever collected from the far side.

In a status update, the China National Space Administration said the Chang’e-6 ascent module successfully reached lunar orbit, where it’s due to transfer the samples to a re-entry capsule hooked up to the probe’s orbiter.

If all goes according to plan, the orbiter will leave the moon’s orbit, head back to Earth and drop off the re-entry capsule for retrieval in China’s Inner Mongolia region sometime around June 25.

This mosaic of color images was taken by the panoramic camera on China’s Chang’e-6 lander, looking toward the north. One of the lander’s legs is seen in the foreground of the fisheye view, and the upper part of the image shows Chaffee Crater, north of the landing site. (Credit: CLEP / CNSA)

Chang’e-6 was launched on its mission on May 3 and landed in the South Pole-Aitken Basin region on June 2 (Beijing time). Using its drill and its robotic arm, the lander collected as much as 2 kilograms (4.4 pounds) of rocks and soil from the landing site. Meanwhile, a mini-rover rolled out onto the surface and took pictures looking back at the lander.

CNSA said scientific readings were also collected, using a lunar mineral spectrometer, a negative ion analyzer, a radon detector and a lunar structure detector. An Italian-built retro-reflector, installed on the top of the lander, served as a position control point that can be used for distance measurement. Data and telemetry were transmitted back to Earth via China’s Queqiao-2 relay satellite.

“After the collection was completed, the five-star red flag carried by the Chang’e-6 lander was successfully unfolded on the far side of the moon,” CNSA said. “This is the first time that China has independently and dynamically displayed the national flag on the far side of the moon, The flag is made of new composite materials and special technology.”

Here's a taste of the sampling action from the past couple of days, since the Chang'e-6 landing late on June 1 UTC. pic.twitter.com/jw2DlPToVf

— Andrew Jones (@AJ_FI) June 4, 2024

The space agency said the Chang’e-6 ascent module lifted off at 7:38 a.m. June 4 Beijing time (11:38 p.m. GMT June 3) and fired its engine for about six minutes to reach lunar orbit. After the ascent module’s rendezvous with the orbiter and the transfer of the samples, the orbiter and the re-entry capsule will continue to circle the moon, “waiting for the right time to return for the lunar-to-Earth transfer,” CNSA said. The flight plan follows the model that was set in 2020 when Chang’e-5 brought back samples from the moon’s Earth-facing side.

The findings from Chang’e-6 could provide new insights about the moon’s south polar region. That area is of particular interest because it’s thought to contain water ice reserves that could support lunar settlement. NASA is targeting the south polar region for its upcoming VIPER rover mission — and for a crewed lunar landing that’s currently scheduled for 2026. China’s space program has its own ambitions for increased lunar exploration — including another robotic mission planned for 2026, known as Chang’e-7, and a crewed landing that it’s aiming to accomplish by 2030.

The lunar surface has been a popular destination for robotic probes over the past year or so. The successful missions include India’s Chandrayaan-3, Japan’s SLIM and Intuitive Machines’ Odysseus. Russia’s Luna 25, iSpace’s Hakuto-R and Astrobotic’s Peregrine were among the not-so-successful missions.

The post Chinese Probe Collects Moon Samples and Heads for Earth appeared first on Universe Today.

The Artemis Program represents NASA’s effort to return to the Moon. One of the goals of the project is to set up long-term exploration of the Earth’s only natural satellite. This will need much bulkier equipment than what the Apollo astronauts carried though, and this equipment needs to be transported to the Moon’s surface. Blue Origin and SpaceX, contracted by NASA to provide human landing systems, have begun developing vehicles that can safely deliver this equipment from space to the Moon’s surface.

The Artemis program is far more ambitious than Apollo. The goal is not simply to land more humans on the moon, but to conduct scientific research, build a space station in lunar orbit, and lay a foundation for future expeditions to Mars. Artemis III, the first phase in which humans will land on the Moon, is currently expected to launch at a date no earlier than September 2026. NASA have contracted Blue Origin and SpaceX to build lander craft for Artemis III, and all future Artemis missions. The lander will dock with the lunar Gateway, bring the astronauts safely to the surface of the Moon, and then bring them back into orbit, where they will return to the Gateway station. But future Artemis missions will have much more demanding requirements, and involve much longer stays on the Moon. This will require a lot of heavy equipment that needs to be delivered from the Earth to the Moon.

“It’s essential that NASA has the capability to land not just astronauts, but large pieces of equipment, such as pressurized rovers, on the Moon for maximum return on science and exploration activities,” says Lisa Watson-Morgan, Human Landing System Program Manager at NASA’s Marshall Space Flight Center in Huntsville, Alabama. “Beginning this work now allows SpaceX and Blue Origin to leverage their respective human lander designs to provide cargo variants that NASA will need in the future.”

Since the vehicles that can fill this requirement do not exist yet, NASA has contracted SpaceX and Blue Origin to begin designing heavy cargo versions of their human lander craft. They must be able to cope with loads with a mass of 12 to 15 tonnes, in order to fulfill mission requirements, and must be ready to fly in time for Artemis VII. NASA does not expect a completely new design, however. They expect that the cargo landers will be modified versions of the human lander. The cargo version will need to include deployment mechanisms to unload the cargo, as well as payload interfaces. They will be uncrewed, though, which means that they will not need to include heavy and complicated life support systems.

The work is currently at an early stage. Both companies are working on preliminary designs, which will be submitted for review. Feedback from this process will inform further design work, and establish a baseline from which the final detailed designs can be created.

Artemis will allow NASA to explore the moon more completely than was ever possible with Apollo. Astronauts will spend far more time on the Moon’s surface, and learn how to live and work on another world. They will conduct research on previously unexplored regions of the Moon, and lay the critical groundwork to establishing a permanent base — a vital step on the road to building a settlement on Mars. It is a highly ambitious program, combining the efforts of space agencies around the world, private companies, and the academic sector. It requires massive investment and innovation, combining the SLS (Space Launch System) rocket, the Orion spacecraft, the human and cargo landing systems, next generation space suits, pressurized rovers, and the Gateway lunar orbital space station. If successful, Artemis will mark the beginning of humanity’s settlement of deep space.

The Artemis program is supported by Space Policy Directive 1, which changed US space policy to work on a program to return humans to the Moon. It is meant to be a US-led international mission, involving the private sector, and calls on NASA to “lead an innovative and sustainable program of exploration with commercial and international partners to enable human expansion across the Solar System and to bring back to Earth new knowledge and opportunities” The goal is to build a foundation for the eventual human exploration of Mars.

Artemis 1, which launched in November 2022, was a test flight of the SLS, which ended with the Orion spacecraft splashing down into the Pacific Ocean. Artemis 2, currently scheduled for September 2025, will fly a crewed Orion spacecraft in a Lunar flyby. Artemis 3 will land astronauts on the Moon, and is planned to launch in September 2026. Artemis 4 is hoped to launch in September 2028. It will deliver the first components of the Lunar Gateway station, and also land a crew of astronauts on the Moon. Artemis 5 and 6, scheduled for 2030 and 2031, will both dock an Orion spacecraft with the Lunar Gateway, add additional segments to the station, and land astronauts on the Moon.

Reference: https://www.nasa.gov/directorates/esdmd/artemis-campaign-development-division/human-landing-system-program/work-underway-on-large-cargo-landers-for-nasas-artemis-moon-missions/

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One underappreciated aspect of the current flood of exoplanet discoveries is the technical marvels that enable it. Scientists and engineers must capture and detect minute signals from stars and planets light years away. With the technologies of even a few decades ago, that would have been impossible – now it seems commonplace. However, there are still some technical hurdles to overcome before finding the “holy grail” of exoplanet hunting – an Earth analog. To help that discussion, a team of researchers led by Bertrand Mennesson at NASA’s Jet Propulsion Laboratory has released a paper detailing the current experimental and theoretical work around one of the most critical technical aspects of researching exoplanet atmospheres – starshades.

In particular, the paper discusses the technical hurdles of one of the most interesting upcoming space technology concepts. The Habitable Worlds Observatory (HWO) was called for as part of NASA’s recent decadal survey. While it is still early in its development cycle, the general outlines of how the HWO will work are evident, even if some technical details aren’t. And those general outlines point to the need for a starshade or coronagraph – or both.

The paper details the difference between a starshade and a coronagraph. By its definition, a starshade is a filter placed between the primary telescope mirror and the object it is observing. In contrast, a coronagraph is a filter placed between the primary mirror and the telescope’s sensor. Both methods have advantages and disadvantages regarding the data they allow the telescope to collect, but they can also be combined.

Starshades aren’t only useful for space telescopes, as Fraser discusses with Dr. Markus Janson in this video.

Several labs worldwide have been working on developing starshade and coronagraph technology. However, several nuances to the test set-ups affect their work’s applicability to the HWO project. Some tests are performed in a vacuum, while others are performed in air. Some tests are performed on monolith mirrored telescopes, while others are performed on segmented mirrors. Currently, the baseline operational mode of HWO is a space-based telescope, which, given current launch size constraints, also means it has to be segmented. So, only some tests performed to validate coronagraph and starshade technologies apply to the HWO use case.

For the relevant tests, there are three particular “key performance parameters” (KPPs), as the paper calls them, which can impact the technology’s viability. These are the image’s “raw” contrast, the “post-calibration” contrast, and the “off-axis throughput.” Each of these has thoroughly technical definitions described in the paper. But the first two can be thought of as how easy it is to see an exoplanet before (“raw”) and after (“post-calibration”) an image is run through a data processing algorithm. Off-axis throughput is the percentage of light from the planet through the starlight suppression system.

Each of these three KPPs represents a trade-off with the other two. Optimizing a starlight suppression system, such as a coronagraph or starshade, requires understanding and validating those design trade-offs. The paper mentions that the details of the HWO are still in flux, so it is impossible to determine what trade-offs must be made to have a fully functional system. Factors such as the number of exoearths the HWO is expected to observe, their orbital parameters, and how long the observatory will be allowed to capture data on any particular planetary system will all feed into the simulated trade-offs considered in the paper.

The Nancy Grace Roman Space Telescope is another candidate for exoplanet hunting with an advanced starlight suppression system, as Fraser discusses in this video.

Most importantly, the paper’s authors stated they intended to inform the technical committees of the HWO project about these trade-offs and to help guide the selection of mission parameters that might fit in with the current (or near-term) state of technical development of one of the most critical technologies for the optimal operation of the system. HWO is still in the early planning stages and has no expected launch date. Work has started around defining the teams that will make the technical determinations to inform the selection of a starlight suppression system for the HWO. Dr. Mennesson, the paper’s lead author, also happens to be one of the co-chairs of one of the committees.

But for now, there is plenty of time to flesh out the HWO design and continue developing and testing different starlight suppression technologies. If the remarkable pace of exoplanet discovery is any indication, with a little more time and attention, the telescope development community will develop an optimally designed system to help find one of the most sought-after discoveries in modern science.

Learn More:
Mennesson et al. – Current laboratory performance of starlight suppression systems, and potential pathways to desired Habitable Worlds Observatory exoplanet science capabilities
UT – Astronomers Identify 164 Promising Targets for the Habitable Worlds Observatory
UT – The Habitable Worlds Observatory Could See Lunar and Solar ‘Exo-Eclipses’
UT – Planning is Underway for NASA’s Next Big Flagship Space Telescope

Lead Image:
Image of exoplanets

The post Suppressing Starlight: How to Find Other Earths appeared first on Universe Today.

Back in December, NASA officials, space industry experts, members of the academic community, and science communicators descended on Washington, D.C., for the Achieving Mars Workshop X (AM X). This workshop is hosted by Explore Mars Inc., a non-profit organization dedicated to bringing leading experts from disparate fields together to contribute to creating the first crewed missions to Mars. On May 17th, the results of this year’s workshop were summarized in a report titled “The Tenth Community Workshop for Achievability and Sustainability of Human Exploration of Mars.”

Erik Antonsen, Bruce Jakosky, and Lisa May co-chaired the workshop, which took place from December 5th to 7th at George Washington University. Antonsen is the CTO of Advancing Frontiers, a consulting company providing spaceflight integration services, and an Associate Professor of Space Medicine and Emergency Medicine with the Center for Space Medicine at the Baylor College of Medicine (BCM). Jakosky is a Professor Emeritus of Geological Sciences and the Associate Director of the Laboratory for Atmospheric and Space Physics (LASP) at UC Boulder. May is the Chief Technologist for Lockheed Martin’s Commercial and Civil Space Advanced Programs.

As always, the workshop featured presentations and discussions that addressed the challenges, benefits, and ongoing efforts to realize the human exploration of Mars. But this year was special in several ways, not just because it was the tenth anniversary of the AM series. In addition, AM X took place during an auspicious time for NASA, space agencies, international organizations, and commercial space companies supporting human spaceflight. Between the impending return to the Moon through the Artemis programs and uncertainties about the first crewed missions to Mars, there was a lot to discuss!

For instance, last year’s workshop (AM IX) addressed the pressing question of whether NASA would be able to mount a crewed mission to Mars by 2033. This has been a key aspect of NASA’s Moon-to-Mars (M2M) mission architecture, detailed in the agency’s annual Architecture Concept Reviews (ACRs). It is also in keeping with Explore Mars’ goal of advancing the “human exploration of Mars and beyond no later than the 2030s.” Alas, in recent years, there has been growing skepticism that several key technologies will be ready to meet this deadline.

As Universe Today reported at the time, these doubts were raised at AM IX, and there was no consensus regarding potential solutions. This included the possibility of a flyby mission by 2033 and whether or not a nuclear-thermal propulsion (NTP) system, which can potentially reduce transit times to Mars (45 to 100 days), would be ready in time. In addition, there were the comments of Deputy Administrator Jim Reuters, who acknowledged that sending astronauts to Mars by 2040 was “an audacious goal for us to meet… It may sound like a lot, but it is [a] very short time to develop technologies we need to develop.”

As with previous AM workshops, cooperation and effective communication were emphasized. This includes coordinating robotic and human spaceflight missions and broader cooperation between space agencies, government, and industry. A key concern that was identified was the process through which NASA’s mission architecture evolves. While participants agreed that the M2M ADD “provides a strong starting point for an iterative architecture process,” they also concluded that the development process was insufficient. As stated in the AM X Report:

“Participants observed that despite recent progress, existing channels were insufficient to adequately integrate human capabilities and limitations as well as science objectives into the architecture development process. Similarly, sustainable human exploration of the Moon and Mars will not occur unless science and human exploration objectives are infused early and continuously into the systems engineering processes.”

Artwork for the AM X Workshop Report. Credit: Explore Mars Inc.

To address these concerns, the workshop participants came up with four recommendations for improving existing channels and the architecture development process. They include:

Public Outreach & Involvement

First, the AM X Workshop Report recommended that public interactive forums be more frequent to develop inputs to NASA’s Architecture Definition Documents. The communities emphasized for engagement include operations, human research, science, international organizations, and others “that empower cross-disciplinary teaming, welcome broad participation from external experts, and provide a pathway to incorporate community recommendations and findings into Mars mission planning.”

The need to coordinate with diverse science communities to prioritize and narrow science objectives was also noted, as was the possible need for certification paths for external groups “to provide input in
smaller settings and more frequently than once a year at the ACR.”

The Report also emphasizes the need for initiatives and workshops that focus on the development and integration of “intelligent systems” and “data analytics” that will be critical for missions operating farther from Earth for extended periods. According to NASA’s mission architecture, this applies to Phase III of the Moon to Mars plan (aka. “Earth Independent”), where operations will shift from cislunar to deep space. This will include transits to and from Mars using the Deep Space Transport (DST) and science operations on the Martian surface.

Risk Mitigation

Second, the Report acknowledges the historical trend where certain priorities (like discovery science, technology, and infrastructure development) are often sacrificed for short-term needs. To this end, it is recommended that NASA acknowledge and address tensions between scientific investment for “risk mitigation purposes and investment for discovery science in planning for M2M missions.” While there is no reference to the sacrifices made to realize the Artemis Program and a return to the Moon by 2024, there are some hints that this could be the case.

An illustration of the Gateway’s Power and Propulsion Element and Habitation and Logistics Outpost in orbit around the Moon. Credits: NASA

The shifting priorities brought about by the expedited timetable have led to the deprioritizing of mission elements crucial to reaching Mars by the 2030s – like the Lunar Gateway. As acting Deputy Administrator Doug Loverro explained in March of 2020 during a NASA Advisory Council science committee, the Gateway was deprioritized to “de-risk” Artemis so NASA could focus on meeting the mandatory goals of Artemis and its 2024 deadline. Meanwhile, no design or feasibility studies have been performed for the DST or a Mars orbital habitat (a la the Mars Base Camp) since 2018/19, coinciding with the Artemis “shake-up.”

Regardless, the Report cites the need for increased funding to ensure “technology maturation, demonstration, and infusion to incorporate capabilities.” This is understandable, given that budget concerns have been an issue since NASA began planning missions to the Moon and Mars. In addition to speeding the development of technology, an increase in funding is also desirable to incorporate rapidly advancing technologies such as “artificial intelligence, data management, in-space manufacturing,” and others that are still relatively early in the development process.

Another important factor emphasized here is Health and Human Performance (HPP), which clearly refers to strategies for mitigating the health risks associated with deep space transits. These include extended periods spent in microgravity and long-term exposure to elevated levels of solar and cosmic radiation. To date, NASA has explored multiple possibilities for addressing these concerns, but no concrete plans have emerged just yet.

Evolving Architectures

Further to Recommendation I, the Report states that NASA and commercial companies invested in Mars exploration should continue designing “evolvable mission and campaign architectures.” The purpose of this is to allow for new technologies to be incorporated along the way and prevent the current state of technology from limiting plans. As per the Report, this will help ensure that “we do not design architecture and hardware applicable only for the first mission without allowing both to evolve for subsequent missions.” To this end, NASA and commercial industries are encouraged to:

• Develop common standards, requirements, and interfaces to allow the incorporation of multiple technologies, capabilities, and/or solutions as technology progresses over the next two decades.
• Create and implement a Human and System Readiness Level verification process to assess if the human, hardware, software, and planning systems are sufficiently mature as an integrated system.
• Ensure that the architecture is sufficiently flexible that it can address a wide range of missions beyond the first one.

Artist’s representation of NASA’s “Moon to Mars” mission architecture. Credit: NASA Commercial Partnerships

Finally, the Report encourages NASA to continue investing and cooperating with commercial partners to realize lunar capabilities and technologies that will help them reach Mars. This goes to the heart of the M2M mission architecture, which prioritized a return to the Moon during the 2020s to develop the necessary technologies, systems, and expertise to create a pathway to Mars by the 2030s. “The Moon is how we learn to get to Mars,” it reads, “and we want companies thinking not just about getting to the Moon but, at the same time, how getting there prepares us for the more challenging missions to Mars.”

As usual, the prospect of sending crewed missions to Mars raised many concerns at this year’s workshop. This should come as no surprise, as the goal itself is incredibly ambitious and presents many major challenges. If there is a takeaway from this year’s workshop, it is that there is plenty of work to be done before a mission can be realized. This work must take place at the architectural level, emphasizing wider public engagement, advancing technologies, and a commitment to long-term goals.

Further Reading: Explore Mars

The post Highlights from the 10th Achieving Mars Workshop appeared first on Universe Today.

The Martian surface shows ample evidence of its warm, watery past. Deltas, ancient lakebeds, and dry river channels are plentiful. When the Curiosity rover found organic matter in ancient sediments in the Jezero Crater paleolake, it was tempting to conclude that life created the matter.

However, new research suggests that non-living processes are responsible.

There are three carbon isotopes on Earth: carbon-12 (12C), carbon-13 (13C), and carbon-14 (14C). Earth’s carbon is almost entirely carbon-12. It makes up 99% of the carbon on Earth, with carbon-13 making up the other 1%. (14C is extremely rare and unstable, so it decays into nitrogen-14.)

In 2022, MSL Curiosity took an inventory of organic carbon in sediments at Gale Crater. Organic carbon is usually described as carbon atoms bonded covalently to hydrogen atoms and is the basis for organic molecules. The carbon in organic carbon can be either carbon-12 or carbon-13, and the amounts are important. At Gale Crater, Curiosity found about 200 to 273 parts per million of organic carbon. “This is comparable to or even more than the amount found in rocks in very low-life places on Earth, such as parts of the Atacama Desert in South America, and more than has been detected in Mars meteorites,” said Jennifer Stern, a Space Scientist at NASA’s Goddard Space Flight Center when the results came in.

This is the Stimson sandstone formation in Gale Crater on Mars. This is where the Curiosity Rover drilled the Edinburgh hole and found enriched Carbon 12. Image Credit: NASA/Caltech-JPL/MSSS

This carbon is important evidence in understanding Mars’ history. It can tell scientists about the planet’s atmospheric processes and environmental conditions and even shed light on potential life. In fact, understanding Martian carbon can aid our understanding of habitability and prebiotic chemistry on distant exoplanets. The isotope ratio in this carbon is different than on Earth. It has a lower amount of carbon-13 relative to carbon-12 compared to Earth. Why the discrepancy?

In recent research in Nature Geoscience, a team of researchers tried to understand the difference between Earth’s and Mars’s carbon isotope ratios. The work is titled “Synthesis of 13C-depleted organic matter from CO in a reducing early Martian atmosphere.” The lead author is Yuichiro Ueno, a biogeochemist in the Department of Earth and Planetary Sciences at the Tokyo Institute of Technology.

“Strong 13C depletion in sedimentary organic matter at Gale crater was recently detected by the Curiosity rover,” the authors write. “Although this enigmatic depletion remains debated, if correct, a mechanism to cause such strong 13C depletion is required.” 

The amount of carbon-13 in the Martian sediments is far lower than in Earth’s sediments.

“On measuring the stable isotope ratio between 13C and 12C, the Martian organic matter has a 13C abundance of 0.92% to 0.99% of the carbon that makes it up,” lead author Ueno explained in a press release. “This is extremely low compared to Earth’s sedimentary organic matter, which is about 1.04%, and atmospheric CO2, around 1.07%, both of which are biological remnants and are not similar to the organic matter in meteorites, which is about 1.05%.”

The meteorite data is important because a four billion-year-old Martian meteorite named ALH 84001 is enriched in carbon-13, adding to the enigma of Mars’ carbon. Somehow, carbon-13 became depleted in the intervening billions of years. Solar escape is one possible reason for the carbon-13 depletion, but the authors discount that. There likely wasn’t enough time for enough carbon-13 to escape. “Furthermore, based on geomagnetic observations, early Mars probably had a geomagnetic field before 4?Ga,” the authors write. That field would’ve prevented solar escape.

To determine what’s behind this discrepancy, Ueno and his co-researchers simulated different Martian atmospheric conditions to see what would happen.

Their results show that isotope fractionation by solar UV light is responsible for Mars’ 13C depletion.

This graphic outlines the process that creates atmospheric organic matter that finds its way into the Martian sediments sampled by MSL Curiosity. Image Credit: Ueno et al. 2024.

Carbon-12 and carbon-13 respond differently to UV light. Carbon-12 preferentially absorbs UV, which dissociates it into carbon monoxide that’s depleted in carbon-12. What’s left behind is CO2 enriched with carbon-13.

Scientists have observed this process in the upper atmospheres of Earth and Mars. In Mars’ reducing atmosphere, where oxygen was depleted, the CO2 enriched with carbon-13 would’ve transformed into formaldehyde and possibly methanol. But those compounds didn’t remain stable. In Mars’ early days, the surface temperature was close to the freezing point of water, and it never exceeded about 27 Celsius (80 F.) In that temperature range, the formaldehyde and other compounds could’ve dissolved in water. From there, they gathered in sediments.

But that’s not the end of Mars’ carbon isotope story.

The researchers used models to show that in a Mars atmosphere with a CO2 to CO ratio of 90:10, 20% of the CO2 would have converted to CO, leading to the sedimentary carbon isotope ratio we see today. The remaining atmospheric CO2 would be higher in C-13, and both values are in line with what Curiosity found, and with the ancient Martian meteorite ALH 84001.

This is a plausible scenario that can explain Curiosity’s curious carbon findings.

The team’s study also includes some other important details. For instance, atmospheric CO may not have come solely from photolysis by UV light. Some could have come from volcanic eruptions. And atmospheric CO may not have been the sole source of organics that found their way into the sediments. But either way, the results tell scientists something about Mars’ carbon cycle.

It also tells us to expect to find more organics in Martian sediments in the future.

“If the estimation in this research is correct, there may be an unexpected amount of organic material present in Martian sediments. This suggests that future explorations of Mars might uncover large quantities of organic matter,” said Ueno.

While the research shows us that life needn’t be present to produce these organics, it can’t rule life out. Nobody can, at least not yet.

The research also shows how complex atmospheric chemistry can be and how difficult it can be to draw conclusions from atmospheric studies of exoplanets. The JWST has examined several exoplanet atmospheres and found some interesting results. But there’s so much we don’t know. This research is a reminder that any conclusions are likely premature.

The post Life Probably Played No Role in Mars’ Organic Matter appeared first on Universe Today.

As we discover more and more exoplanets – and the current total is in excess of 5,200 – we continue to try to learn more about them. Astrobiologists busy themselves analysing their atmospheres searching for anything that provides a sign of life. It is quite conceivable of course that the Universe is teeming with life based on very different chemistry to ours but we often look to life on Earth to know what to look for. On Earth for example, ozone forms through photolysis of molecular oxygen and is an indicator of life. Using the James Webb Space Telescope astronomers are searching stars in the habitable zone of their star for the presence of ozone and how it impacts their climate.

It’s tantalising that 425 of the exoplanets detected so far, exist in their stars habitable zone. It is in this region where the climate on the planet may well be suitable to sustain life. A significant subset of those planets are Earth-like in nature and will therefore have a fairly temperate climate. In addition, they all seem to orbit M-dwarf type stars which means they are likely to be impacted by tidal spin-synchronisation (due to the effects of the tides, one face of the planet may well be kept facing the star). One impact of this is the potential for large contrast in daytime and night-time irradiation which can drive strong convection on the day side of the planet.  

The strong convection can drive winds around the equatorial region that are persistently higher faster than the rotation of the planet. It can also create Rosby Waves which naturally occur in the Earth’s ocean and atmosphere – in any rotating fluids or gas. Together these can control the distribution of chemicals in the atmosphere, in particular ozone. 

In Earth’s atmosphere the presence of molecular oxygen is an indicator of life since it is produced largely from photosynthesis in plants. The molecular oxygen collides with nitrogen in the atmosphere to produce ozone so the presence of the latter is an indicator of biological processes. There is a chance though that the molecular oxygen in exoplanet atmospheres are the result of different ratios of near and far UV that can drive a non-biological build up. 

In a new piece of research reported in a paper by lead author Paolo De Luca and team, they report their findings having leveraged climate model simulations on Proxima Centauri b. The Earth-sized exoplanet orbits the red dwarf star Proxima Centauri, the closest star to our own at a distance of 4,.2 light years. 

An artist’s conception of a violent flare erupting from the red dwarf star Proxima Centauri. Such flares can obliterate atmospheres of nearby planets. Credit: NRAO/S. Dagnello.

They report that the analysis of atmospheres of tidally locked Earth-like exoplanets received a massive boost as a result of the development of the James Webb Telescope. The team reveal that their climate modelling (including the use of interactive ozone) globally increases temperature in the stratosphere. This in turn induces regional variations of surface temperature and also reduces the temperature contrast between day and night side. 

Whilst the team have not been able to identify life on exoplanets, that was not their intention. What they have achieved is the ability to understand the exoplanet atmospheres using the James Webb Space Telescope, some of the processes that lead to atmospheric ozone and the impacts on temperatures. 

Source : The impact of Ozone on Earth-like exoplanet climate dynamics: the case of Proxima Centauri b

The post What Impact Does Ozone Have on an Exoplanet? appeared first on Universe Today.

To reach the Green Bank Observatory, you take the road less traveled, winding through scenic and remote regions of the Allegheny Mountains and the Monongahela National Forest of West Virginia. About an hour away, you’ll start to lose cell phone service. The Green Bank Observatory – a collection of radio telescopes that search the heavens for faint radio signals from black holes, pulsars, neutron stars or gravitational waves — sits near the heart of the United States National Radio Quiet Zone, a unique area the encompasses an area of approximately 13,000 square miles, spanning the border between Virginia and West Virginia.

Here in the NRQZ, human-generated radio transmissions are limited to shield the radio telescopes from Earth-based radio signals called RFI (Radio Frequency Interference), which are high-frequency electromagnetic waves that emanate from electronic devices such as computers, cell phones, microwave ovens, and even digital cameras. Even the weakest RFI signals can drown out the faint radio waves coming from the cosmos.

A view of the Green Bank Observatory’s Science Center and some of the telescopes. Credit: Jay Young for the Green Bank Observatory.

“You can only use basic, old-style film cameras here within 2 miles of the Green Bank Telescope,” said Paul Vosteen, Media Specialist at Green Bank Observatory who provided a tour of the facilities. Vosteen recounted a time he took a group out to see the gigantic (and very photogenic) 100-meter Green Bank Telescope (GBT) and unwittingly, a member of the group started snapping photos with a digital camera. While he quickly got the photographer stopped, Vosteen later coyly checked in with technicians who had been running diagnostics on the GBT that day. They were scratching their heads about a strange spike in signals earlier that morning. Turns out, it was the exact moment the photographer used their digital camera. 

“The slightest electronic signal can cause interference,” Vosteen explained. “We can only use diesel vehicles here on the premises because gasoline engines have spark plugs. Everything that sparks produces radio waves.” Diesel engines, on the other hand, ignite by compression.

GBT Control Room. Credit NSF/GBO/Jill Malusky.

To keep the amount of interference on-site in check, the observatory’s control room and the nearby Science Center’s exhibit hall are completely surrounded by copper Faraday cages, wire-mesh devices built into the walls to block electromagnetic signals. Even windows are covered with a thin wire mesh, and the heavy door to the control room opens and closes like an entrance to a high-security bank vault.

Green Bank is home to six large radio telescopes ranging in size from 14 meters to 100 meters in diameter. The 20-meter and the 40-foot telescopes are full-time educational telescopes used by students around the country.

UT journalist Nancy Atkinson by the Reber Telescope, the world’s first parabolic dish built by Grote Reber in his Illinois backyard. The dish was moved to the Green Bank Observatory site in the 1960s. Credit: Nancy Atkinson.

The observatory also contains many relics of radio astronomy history. There’s an exact replica of the dipole array antenna Karl Jansky used when he discovered quite by accident that radio waves were emanating from the center of the Milky Way. That was the beginning of radio astronomy as we know it today. There’s also the actual parabolic dish radio telescope (the world’s first) built by Grote Reber in 1937 to follow up on Jansky’s detection. Then there’s the 85-foot Howard E. Tatel telescope that Frank Drake used in 1960 to perform the world’s first search for extraterrestrial intelligence with Project Ozma.

GBT – “Great Big Thing”

At 485 feet (148 meters) tall, the Robert C. Byrd Green Bank Telescope (GBT – sometimes called ‘Great Big Thing’ by locals) is the tallest and most eye-catching dish at the observatory, and the largest steerable radio telescope in the world. The maneuverability of its large 100-meter dish allows it to quickly track objects across its field of view, and see 85% of the sky.

While the GBT has been in operation since 2000, as we discussed in an article last week, a new upgrade for the telescope is under development. ngRADAR is a next-generation radar system that will allow the GBT to track and map asteroids with unprecedented resolution, making GBT the most advanced planetary radar system in the world. It will also be able to study comets, moons and planets in our Solar System. When finished it will not only help astronomers study the composition of other planetary bodies, but also help defend against potential large meteor strikes on Earth by mapping the precise trajectories of asteroids that cross Earth’s orbit.

Astronomers study the Universe by capturing light from stars, planets, and galaxies. But they can also study nearby objects by shining radio light on them and analyzing the signals that echo back. This is called planetary radar, and the process can reveal incredibly detailed information about our planetary neighbors.

The Robert C. Byrd Green Bank Telescope. Credit: Jay Young.

“When astronomers are studying light that is being made by a star, or galaxy, they’re trying to figure out its properties,” said Patrick Taylor, the project director for ngRADAR and the radar division head for the National Radio Astronomy Observatory, in our article last week. “But with radar, we already know what the properties of the signals are, and we leverage that to figure out the properties of whatever we bounced the signals off of. That allows us to characterize planetary bodies – like their shape, speed, and trajectory. That’s especially important for hazardous objects that might stray too close to Earth.”

Previously, the workhorse for planetary radar was the 1,000-foot-diameter (305 meters) Arecibo Observatory which collapsed in 2020, as well as the Goldstone 70-meter dish in California, which is primarily used for communicating with spacecraft as part of NASA’s Deep Space Network. Taylor said that the idea for ngRADAR has been discussed for years — even before Arecibo’s demise — but with the loss of Arecibo, the upgrade is even more important.

Radar signals transmitted by the ngRADAR at the GBT will reflect off astronomical objects, and those reflected signals will be received by the Very Long Baseline Array (VLBA), a network of ten observing stations located across the United States.

A Synthetic Aperture Radar image of the Moon’s Tycho Crater using the ngRADAR prototyope, showing 5-meter resolution detail. Image credit Raytheon.

“The idea is for GBT is to do the transmitting almost constantly and the VLBA — either all ten of those or any subset of those telescopes — doing the receiving,” said Taylor. “This new system will allow us to characterize the surfaces of many different objects in a different frequency or wavelength that hasn’t been used before.”

Radio Frequencies

All light travels through space in waves – think of how ripples move across a pond. Each ripple has a peak and a trough, which is called a cycle. An object emitting radio waves produces many cycles in a very short period. During each cycle, the wave moves a short distance, which is called its wavelength. Radio waves have the longest wavelengths in the electromagnetic spectrum. They range from sub-millimeter lengths to over 100 kilometers.

For radio waves of all wavelengths, the number of cycles per second is called a frequency, with one cycle per second being one hertz. That means one thousand cycles per second is a kilohertz and a billion cycles per second is a gigahertz. Radio astronomers are interested in objects in a wide range of frequencies, but mostly from between 3 kilohertz and about 900 gigahertz.

“Arecibo worked at 2.38 gigahertz, the Goldstone 70-meter primarily works at 8.56 gigahertz,” said Taylor. “For ngRADAR, we are looking at even higher frequencies, at 13.7 gigahertz, something that really hasn’t been used for planetary radar before. This is a way to offer something new and different, while the capabilities of the two instruments – GBT and Goldstone – also would complement each other.”

But more importantly, since Goldstone is now “the only planetary radar game in town,” as Taylor described it, that means planetary radar in the US has a single point failure. The antennas of Goldstone Deep Space Communications Complex are busy 24 hours a day communicating with spacecraft around the Solar System.

“If Goldstone is down for whatever reason or if it’s not available because of its work with the DSN,” said Taylor, “having a radar transmitter on the GBT gives us more flexibility and redundancy.”

Taylor said there are several applications for the future of radar, from not only advancing our knowledge of objects in the Solar System and characterizing asteroids and comets, but also aiding in future robotic and crewed spaceflight.

The Green Bank Telescope Credit: Dave Green

The GBT worked with the Goldstone telescope to help confirm the success of NASA’s Double Asteroid Redirection Test (DART) mission in 2022, the first test to see if humans could successfully alter the trajectory of an asteroid. In a two-week campaign, the radio telescopes were able to track how the orbit of Dimorphos, the asteroid that was hit by DART, changed after the impact.

But the main goal ngRADAR is for is planetary defense.

“That will be one of the highest priority uses for the radar system, where we can track and characterize near earth-asteroids and comets to evaluate any hazard they might present to Earth in the future. Radar delivers very precise data that allows you to predict where these small bodies will be in the future. We can determine its size, how it rotates, what it might be made of, is it just a round ball, or does it look like a potato, or does it have a moon that you also must worry about.”

Building ngRADAR

Raytheon’s prototype radar system deployed on the prime focus boom of the Green Bank Telescope over its 100-meter collecting dish. Credit: Green Bank Observatory.

As we discussed last week, a scaled-down prototype of ngRADAR at the GBT produced some of the highest resolution planetary radar images ever captured from Earth. Not only will the new full-scale system need to be built, but several changes will need to be made to the GBT. 

“This will be a pretty intensive infrastructure project,” Taylor explained. “We’ll have to build the transmitter and mount it onto the GBT. With the size and weight of the system, as well as the cooling systems that will be needed, extra structures will be needed to support all that.”

Taylor said the timeline for completion would depend on funding, but a reasonable goal is that in the next five years – perhaps by 2029-2030 – ngRADAR could be up and running.

But Taylor feels that ngRADAR will allow the GBT to come full circle.

“Some of the first science done with GBT was receiving radar signals when it was first inaugurated,” he said. “It’s been a receiver for radar for over 20 years but now we are trying to take the next step and have it be a transmitter as well.”

Read part 1 of this series, Next Generation Radar Will Map Threatening Asteroids.

The post Part 2: The History and Future of Planetary Radar appeared first on Universe Today.

After touching down on the moon’s far side, China’s Chang’e-6 lander is collecting samples to bring back to Earth — and sending back imagery documenting its mission.

Chang’e-6, which was launched May 3, went through weeks’ worth of in-space maneuvers that climaxed with its weekend landing in the moon’s South Pole-Aitken Basin region. The mission plan calls for the probe to collect samples of lunar soil and rock over the course of about two days, and then pack them up for the return trip.

If the operation is successful, Chang’e-6 would bring back the first fresh lunar samples ever collected on the moon’s far side — following up on the Chang’e-5 mission in 2020, which returned samples from the moon’s Earth-facing side.

The China National Space Administration said the lander used its onboard camera during its powered descent to detect obstacles autonomously and select a safe landing site. Chang’e-6 captured video imagery during the final phase of the lander’s descent and transmitted the views back to Earth. One video frame shows the shadow of the lander itself moments before touchdown.

Chang’e-6 is built to collect samples using a drill and a robotic arm. It’s also expected to gather scientific data about its surroundings using a radon detector, a negative-ion detector and a mini-rover. During surface operations, data and telemetry are being relayed between Chang’e-6 and Earth via China’s Queqiao-2 satellite.

Up to 2 kilograms (4.4 pounds) of lunar samples will be stowed inside the lander’s “ascender” stage. The rocket-powered ascender will then lift off from the surface and transfer the samples to the Chang’e-6 orbiter, which is currently in lunar orbit. Following the model set by Chang’e-5, the orbiter will head back toward Earth and release the sample capsule for atmospheric re-entry and touchdown in Inner Mongolia.

An image captured by a camera aboard the Chang’e-6 lander shows the spacecraft’s shadow on the lunar surface just moments before touchdown. (Credit: CLEP / CNSA)

The moon’s south polar region is of particular interest because it’s thought to harbor reserves of water ice that could support lunar settlement. Studying fresh samples from the South Pole-Aitken Basin could help scientists and mission planners learn more about the region’s resources.

Chang’e-6 is the latest spacecraft in an international armada of moon landers — including Russia’s Luna 25, iSpace’s Hakuto-R and Astrobotic’s Peregrine, which were unsuccessful, plus more fruitful missions such as India’s Chandrayaan-3, Japan’s SLIM and Intuitive Machines’ Odysseus.

Coming attractions include NASA’s VIPER rover, which is currently due to be delivered to the moon late this year; and China’s Chang’e-7 mission, which features a hopping probe and is set for launch in 2026. Looking further ahead, China aims to send astronauts to the lunar surface by 2030 — not long after NASA’s Artemis 3 crewed lunar landing, currently scheduled for 2026.

The post Chinese Probe Lands on Moon’s Far Side to Collect Samples for Return appeared first on Universe Today.