Friday, January 31, 2025

'Troublesome' radio galaxy 32 times size of Milky Way spotted

The newly-discovered giant radio galaxy ‘Inkathazo’. The glowing plasma jets, as seen by the MeerKAT telescope, are shown in red and yellow. The starlight from other surrounding galaxies can be seen in the background. Credit: K.K.L Charlton (UCT), MeerKAT, HSC, CARTA, IDIA
Licence type: Attribution (CC BY 4.0)

Astronomers have discovered an extraordinary new giant radio galaxy with plasma jets 32 times the size of our Milky Way.

Measuring 3.3 million light-years from end-to-end, the cosmic megastructure was spotted by South Africa's MeerKAT telescope and nicknamed Inkathazo – meaning 'trouble' in the African Xhosa and Zulu languages – because of the difficulty in understanding the physics behind it.

Researchers hope their "exciting and unexpected discovery", published today in Monthly Notices of the Royal Astronomical Society, will shed light on the mysterious origin and evolution of what are some of the largest structures in the Universe.

Giant radio galaxies (GRGs) are cosmic behemoths spewing jets of hot plasma millions of light-years across intergalactic space. These plasma jets, which glow at radio frequencies, are powered by supermassive black holes at the centres of galaxies.

Until recently, GRGs were thought to be quite rare. However, a new generation of radio telescopes, such as South Africa's MeerKAT, have since turned this idea on its head.

"The number of GRG discoveries has absolutely exploded in the past five years thanks to powerful new telescopes like MeerKAT," said Kathleen Charlton, a Master’s student at the University of Cape Town and the first author of the new study.

"Research into GRGs is developing so rapidly that it's becoming hard to keep up. It's incredibly exciting!"

A spectral age map of ‘Inkathazo’. Cyan and green show younger plasma, while purple indicates older plasma. K.K.L Charlton (UCT), MeerKAT, HSC, CARTA, IDIA
Licence type: Atribution (CC BY 4.0)

She added: "We nicknamed this giant galaxy 'Inkathazo,' meaning 'trouble' in isiZulu and isiXhosa because it has been a bit troublesome to understand the physics behind what’s going on here.

"It doesn't have the same characteristics as many other giant radio galaxies. For example, the plasma jets have an unusual shape: rather than extending straight across from end-to-end, one of the jets is bent."

Inkathazo also lives at the very heart of a cluster of galaxies, rather than in relative isolation, which should make it difficult for the plasma jets to grow to such enormous sizes.

"This is an exciting and unexpected discovery," said Dr Kshitij Thorat, a co-author of the study from the University of Pretoria.

"Finding a GRG in a cluster environment raises questions about the role of environmental interactions in the formation and evolution of these giant galaxies."

To try and understand more about this cosmic conundrum, the researchers took advantage of MeerKAT’s exceptional capabilities to create some of the highest-resolution spectral age maps ever made for GRGs. These maps track the age of the plasma across different parts of the GRG, providing clues about the physical processes at work.

The results revealed intriguing complexities in Inkathazo’s jets, with some electrons receiving unexpected boosts of energy. The researchers believe this may occur when the jets collide with hot gas in the voids between galaxies in a cluster.

"This discovery has given us a unique opportunity to study GRG physics in extraordinary detail," said Thorat. "The findings challenge existing models and suggest that we don’t yet understand much of the complicated plasma physics at play in these extreme galaxies."

South Africa's MeerKAT telescope.
South African Radio Astronomy Observatory
Licence type: Attribution (CC BY 4.0)

Most known GRGs have been found at northern latitudes with European telescopes, while the southern sky remains relatively unexplored for such giant objects. Yet Inkathazo is not alone. It is the third GRG to be spotted in a small patch of sky, around the size of five full moons, that astronomers refer to as 'COSMOS'.

When an international team of astronomers named the 'MIGHTEE' collaboration observed COSMOS with the MeerKAT telescope, they immediately spotted the other two other GRGs and published their findings in 2021.

Inkathazo was seen more recently in follow-up observations with MeerKAT, which is operated by the South African Radio Astronomy Observatory.

"The fact that we unveiled three GRGs by pointing MeerKAT at a single patch of sky goes to show that there is likely a huge treasure trove of undiscovered GRGs in the southern sky" said Dr Jacinta Delhaize, a researcher at the University of Cape Town, who led the 2021 publication.

"MeerKAT is incredibly powerful and in a perfect location, so is excellently poised to uncover and learn more about them."

As a precursor to the Square Kilometre Array (SKA) due to begin operations at the end of this decade, MeerKAT offers unprecedented sensitivity and resolution, enabling discoveries like Inkathazo.

"We're entering an exciting era of radio astronomy," said Dr Delhaize. "While MeerKAT has taken us further than ever before, the SKA will allow us to push these boundaries even further and hopefully solve some of the mysteries surrounding enigmatic objects like giant radio galaxies."

Submitted by Sam Tonkin




Media contacts

Sam Tonkin
Royal Astronomical Society
Mob: +44 (0)7802 877 700

press@ras.ac.uk

Dr Robert Massey
Royal Astronomical Society
Mob: +44 (0)7802 877 699

press@ras.ac.uk



Scientific contacts

Kathleen Charlton
University of Cape Town
Tel: +27 (0)832 603 855

CHRKAT009@myuct.ac.za

Dr Jacinta Delhaize
University of Cape Town

drjdelhaize@gmail.com

A/Prof Kshitij Thorat
University of Pretoria

kshitijthorat.astro@gmail.com



Further information

The paper ‘A spatially-resolved spectral analysis of giant radio galaxies with MeerKAT’ by Kathleen Charlton et al. has been published in Monthly Notices of the Royal Astronomical Society. DOI: 10.1093/mnras/stae2543

Notes for editors

About the MIGHTEE collaboration

This work was co-authored by several members of the international MIGHTEE collaboration of astronomers, led by Professor Matt Jarvis (University of Oxford) and with key contributions by Dr Ian Heywood (University of Oxford).

The MeerKAT International Gigahertz Tiered Extragalactic Exploration (MIGHTEE) survey is a Large Survey Project being conducted with the MeerKAT telescope. Its overarching goal is to study the formation and evolution of galaxies. For more information, visit
https://www.mighteesurvey.org/

About MeerKAT

The MeerKAT telescope is located in the Karoo region of South Africa and is comprised of 64 radio dishes. It is managed by the South African Radio Astronomy Observatory (SARAO), which is a facility of the National Research Foundation. Further details are available at: https://www.sarao.ac.za/science/meerkat/

About the Royal Astronomical Society

The Royal Astronomical Society (RAS), founded in 1820, encourages and promotes the study of astronomy, solar-system science, geophysics and closely related branches of science.

The RAS organises scientific meetings, publishes international research and review journals, recognises outstanding achievements by the award of medals and prizes, maintains an extensive library, supports education through grants and outreach activities and represents UK astronomy nationally and internationally. Its more than 4,000 members (Fellows), a third based overseas, include scientific researchers in universities, observatories and laboratories as well as historians of astronomy and others.

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Thursday, January 30, 2025

Extreme Variability at the Edge of the Universe

An artist’s illustration of a close-up view of a black hole and its jet, like the one in CFHQS J1429+5447. Image credit: NASA/CXC/M. Weiss (CXC).
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Black holes are the most powerful and scary monsters in our universe, lurking at the centers of galaxies. Some, such as the black hole at the center of our own Milky Way Galaxy, have already finished their cosmic meals, with just occasional nibbles observed today. Others, however, are seen ravenously devouring delicious matter from their surroundings. At such times, black holes are noisy eaters, dominating all the activity in their host galaxy centers. As matter spirals in towards the bottomless maw, it collides, heats up, and becomes very bright from X-ray to infrared energies. The accretion disk around a supermassive black hole can easily outshine the billions of stars in a galaxy, and that incredible brightness can make them some of the most distant objects we can observe in both space and time. Black holes can also be messy eaters, spewing out material in cosmic jets that can reach thousands and even millions of light years from the black hole—material that can then go on to influence the universe around it.

Of the many mysteries that keep astronomers up all night observing and pondering these enigmatic beasts, one of the most perplexing is how black holes grow to such enormous sizes. We see supermassive black holes with masses hundreds of millions of times that of the Sun, observed when the universe was only a few hundred million years old. It’s like finding 7-foot basketball players or 300-pound football players with appetites to match in a Kindergarten classroom: just how were they able to grow so big so quickly?

Recent observations by NASA’s NuSTAR and Chandra X-ray observatories might offer some clues. In a paper recently published by the Astrophysical Journal, scientists led by Lea Marcotulli at Yale University and Thomas Connor at the Center for Astrophysics | Harvard & Smithsonian report on observations of the most X-ray luminous accreting black hole, or quasar, ever discovered in the first billion years of the universe. This quasar, called CFHQS J1429+5447, was initially found 15 years ago using data from a ground-based telescope that surveyed wide patches of the sky. Far more recently it was observed by Chandra, which was able to pick up X-rays from this incredibly distant source. Only four months afterwards, NuSTAR also observed it, finding that the quasar had doubled in X-ray brightness in that time.

Such a dramatic variation in such a short time for something this massive is evidence towards this quasar being a particularly messy eater, expelling a powerful jet of material at close to the speed of light. This jet is pointed straight at Earth—a chance alignment that boosts the amount of light making its way to us, allowing telescopes in Earth's orbit like NuSTAR and Chandra to see it at such a great distance.

"These results have significant implications for supermassive black holes and jet evolution theories," said Marcotulli. "The presence of a jet may be a necessity to grow such extreme black holes so early in the Universe."

Because the light observed from this quasar was emitted when the Universe was still very young, this lets us see into an era soon after the Big Bang called the Epoch of Reionization. This time period was when light began to be able to pass through the Universe unimpeded, which is what allows us to see stars and galaxies and distant quasars today. Exactly what kind of objects helped to clear the way for light to travel through space is a mystery that astronomers are still seeking to unravel, but the discovery of a cosmic jet like this one suggests that the Universe's biggest, messiest eaters might have been involved.



How Many Black Holes Are Hiding? NASA Study Homes in on Answer

A supermassive black hole surrounded by a torus of gas and dust is depicted in four different wavelengths of light in this artist’s concept. Visible light (top right) and low-energy X-rays (bottom left) are blocked by the torus; infrared (top left) is scattered and re-emitted; and some high energy X-rays (bottom right) can penetrate the torus. Credit: NASA/JPL-Caltech.
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Multiple NASA telescopes recently helped scientists search the sky for supermassive black holes — those up to billions of times heavier than the Sun. The new survey is unique because it was as likely to find massive black holes that are hidden behind thick clouds of gas and dust as those that are not.

Astronomers now think that every large galaxy in the universe has a supermassive black hole at its center. But testing this hypothesis is difficult because researchers can’t hope to count the billions or even trillions of supermassive black holes thought to exist in the universe, and instead have to extrapolate from smaller samples to learn about the larger population. So accurately measuring the ratio of hidden supermassive black holes in a given sample will help scientists better estimate the total number of supermassive black holes in the universe.

The new study published in the Astrophysical Journal found that about 35% of supermassive black holes are heavily obscured, meaning the surrounding clouds of gas and dust are so thick they even block low-energy X-ray light. Comparable searches have previously found less than 15%. Scientists think the true split should be closer to 50/50 based on models of how galaxies grow. But if observations continue to show a lower percentage, scientists will need to adjust some key ideas they have about supermassive black holes and the role they play in shaping galaxies.

Hidden Treasure

Although black holes are inherently dark — not even light can escape their gravity — they can also be some of the brightest objects in the universe: When gas gets pulled into orbit around a supermassive black hole, like water circling a drain, the extreme gravity creates such intense friction and heat that the gas reaches hundreds of thousands of degrees and radiates so brightly it can outshine all the stars in the surrounding galaxy.

The clouds of gas and dust that surround and replenish the bright central disk may roughly take the shape of a torus, or doughnut. If the doughnut hole is pointed toward Earth, the bright central disk within it is visible; if the doughnut is edge-on, the disk is obscured. Most telescopes can rather easily identify face-on supermassive black holes, but not edge-on ones.

But there’s an exception to this that the authors of the new paper took advantage of: The doughnut absorbs light from the central source and reemits lower-energy light in the infrared range, or wavelengths slightly longer than what human eyes can detect. Essentially, the doughnuts glow in infrared.

These wavelengths of light were detected by NASA’s Infrared Array Survey, or IRAS, mission, which operated for 10 months in 1983 and was managed by NASA’s Jet Propulsion Laboratory in Southern California. A survey telescope that imaged the entire sky, IRAS was able to see the infrared emissions from the clouds surrounding supermassive black holes. Most importantly, it could spot edge-on and face-on black holes equally well.

IRAS caught hundreds of initial targets. Some of them turned out to not be heavily obscured black holes, but galaxies with high rates of star formation that emit a similar infrared glow. So, the team used ground-based, visible-light telescopes to identify the latter and separate them.

To confirm edge-on, heavily obscured black holes, the researchers relied on NASA’s NuSTAR (Nuclear Spectroscopic Telescope Array), an X-ray observatory also managed by JPL. X-rays are radiated by some of the hottest material around the black hole. Lower-energy X-rays will be absorbed by the surrounding clouds of gas and dust, while the higher-energy X-rays observed by NuSTAR can penetrate and scatter off the clouds. This can take hours of observation, so scientists working with NuSTAR first need a telescope like IRAS to tell them where to look.

“It amazes me how useful IRAS and NuSTAR were for this project, especially despite IRAS being operational over 40 years ago,” said study lead Peter Boorman, an astrophysicist at Caltech in Pasadena, California. “I think it shows the legacy value of telescope archives and the benefit of using multiple instruments and wavelengths of light together.”

Numerical Advantage

Determining the number of hidden black holes compared to non-hidden ones can help scientists understand how these black holes get so big. If they grow by consuming material, then a significant number of black holes should be surrounded by thick clouds and potentially obscured. Boorman and his coauthors say this first unbiased look at the population supports this hypothesis.

In addition, black holes influence the galaxies they live in, mostly by impacting how galaxies grow. This happens because black holes surrounded by massive clouds of gas and dust can consume vast — but not infinite — amounts of material. If too much falls toward a black hole at once, the black hole starts coughing up the excess and firing it back out into the galaxy. That can disperse gas clouds within the galaxy where stars are forming, slowing the rate of star formation in the galaxy.

“If we didn’t have black holes, galaxies would be much larger,” said Poshak Gandhi, a professor of astrophysics at Southampton University in the United Kingdom and a coauthor on the new study. “So if we didn’t have a supermassive black hole in our Milky Way galaxy, there might be many more stars in the sky. That’s just one example of how black holes can influence a galaxy’s evolution.”




More About NuSTAR

NuSTAR launched on June 13, 2012. A Small Explorer mission led by Caltech in Pasadena, California, and managed by JPL for NASA’s Science Mission Directorate in Washington, it was developed in partnership with the Danish Technical University (DTU) and the Italian Space Agency (ASI). The telescope optics were built by Columbia University, NASA’s Goddard Space Flight Center in Greenbelt, Maryland, and DTU. The spacecraft was built by Orbital Sciences Corp. in Dulles, Virginia. The NuSTAR mission’s operations center is at the University of California, Berkeley, and the official data archive is at NASA’s High Energy Astrophysics Science Archive Research Center. ASI provides the mission’s ground station and a mirror data archive. Caltech manages JPL for NASA.



News Media Contact:

Calla Cofield

Jet Propulsion Laboratory, Pasadena, Calif.
626-808-2469

calla.e.cofield@jpl.nasa.gov


Wednesday, January 29, 2025

Scientists reveal structure of 74 exocomet belts orbiting nearby stars

Millimetre continuum images for the REASONS resolved sample of 74 exocomet belts
Credit:
Luca Matra, Trinity College Dublin, and colleagues

An international team of astrophysicists has imaged a large number of exocomet belts around nearby stars, and the tiny pebbles within them.

The crystal-clear images show light being emitted from these millimetre-sized pebbles within the belts that orbit 74 nearby stars of a wide variety of ages – from those that are just emerging to those in more mature systems like our own Solar System.

The REASONS (REsolved ALMA and SMA Observations of Nearby Stars) study, led by Trinity College Dublin and involving researchers from the University of Cambridge, is a milestone in the study of exocometary belts because its images and analyses reveal where the pebbles, and the exocomets, are located. They are typically tens to hundreds of astronomical units (the distance from Earth to the Sun) from their central star.

In these regions, it is so cold (-250 to -150 degrees Celsius) that most compounds are frozen as ice on the exocomets. What the researchers are therefore observing is where the ice reservoirs of planetary systems are located. REASONS is the first programme to unveil the structure of these belts for a large sample of 74 exoplanetary systems. The results are reported in the journal Astronomy & Astrophysics.

This study used both the Atacama Large Millimeter/submillimeter Array (ALMA) in Chile and the Submillimeter Array (SMA) in Hawai‘i to produce the images that have provided more information on populations of exocomets than ever before. Both telescope arrays observe electromagnetic radiation at millimetre and submillimetre wavelengths.

“Exocomets are boulders of rock and ice, at least one kilometre in size, which smash together within these belts to produce the pebbles that we observe here with the ALMA and SMA arrays of telescopes,” said lead author Luca Matrà from Trinity College Dublin. “Exocometary belts are found in at least 20% of planetary systems, including our own Solar System.”

“The images reveal a remarkable diversity in the structure of belts,” said co-author Dr Sebastián Marino from the University of Exeter. “Some are narrow rings, as in the canonical picture of a ‘belt’ like our Solar System’s Edgeworth-Kuiper belt. But a larger number of them are wide, and probably better described as ‘disks’ rather than rings.”

Some systems have multiple rings/disks, some of which are eccentric, providing evidence that yet undetectable planets are present and their gravity affects the distribution of pebbles in these systems.

“The power of a large study like REASONS is in revealing population-wide properties and trends,” said Matrà.

For example, the study confirmed that the number of pebbles decreases for older planetary systems as belts run out of larger exocomets smashing together, but showed for the first time that this decrease in pebbles is faster if the belt is closer to the central star. It also indirectly showed – through the belts’ vertical thickness – that objects as large as 140 km across and even Moon-size objects are likely present in these belts.

“We have been studying exocometary belts for decades, but until now only a handful had been imaged,” said co-author Professor Mark Wyatt from Cambridge’s Institute of Astronomy. “This is the largest collection of such images and demonstrates that we already have the capabilities to probe the structures of the planetary systems orbiting a large fraction of the stars near to the Sun.”

“Arrays like the ALMA and SMA used in this work are extraordinary tools that are continuing to give us incredible new insights into the universe and its workings,” said co-author Dr David Wilner from the Center for Astrophysics | Harvard & Smithsonian “The REASONS survey required a large community effort and has an incredible legacy value, with multiple potential pathways for future investigation.”




Reference:


Adapted from a Trinity College Dublin media release.



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Tuesday, January 28, 2025

Zooming in on a supermassive black hole in action

An image of the spiral galaxy NGC 1068 (Messier 77) obtained by the European Southern Observatory’s (ESO) Very Large Telescope (VLT). The galaxy has a distance of 14.4 Mpc (47 million light-years) and is one of the nearest galaxies with an active galactic nucleus. © ESO

A new type of observation reveals what makes the cores of active galaxies glow

Using the Large Binocular Telescope Interferometer, a team of astronomers led by scientists from the Max Planck Institute for Astronomy (MPIA) and the University of Arizona (UofA) has disentangled the sources of infrared radiation near the supermassive black hole at the centre of the galaxy NGC 1068. They discovered that the surrounding dusty wind is heated by the hot central accretion disk and shocks generated by a collimated gas jet. These findings and additional features support the unified model of active galactic nuclei, which explains their varying appearances.

Active galactic nuclei (AGN) are supermassive black holes at the centre of certain galaxies. When these black holes attract matter, a quickly rotating disk of hot gas forms, releasing enormous amounts of energy before plunging into the black hole. Such AGN belong to the most energetic phenomena observed in space. As a result, they also influence processes occurring in their host galaxies. The details are a field of ongoing research.

A team around former MPIA student Jacob Isbell, now a postdoc at the Steward Observatory of the University of Arizona, aimed the Large Binocular Telescope (LBT) at the galaxy NGC 1068, also known as Messier 77, to study the minute details in its centre at thermal infrared wavelengths. This galaxy is one of the nearest with an AGN. The observations had the proper spatial resolution to focus on the components emitting this kind of radiation. The results are now published in Nature Astronomy.

An optical image of the spiral galaxy NGC 1068 (Messier 77) overlaid with an insert with the image obtained by the Large Binocular Telescope Interferometer (LBTI) at thermal infrared wavelengths (8.7 micrometres). The false-colour image depicts the brightness variation of mostly warm dust surrounding the supermassive black hole in the centre of that galaxy. By comparing the image with previous observations at various wavelengths, the researchers identified the hot and bright disk of gas and dust and the collimated gas jet as their heat sources. The components identified in the image confirm the unified model of active galactic nuclei. © ESO / J. Isbell (UofA, MPIA) / MPIA


Disentangling the AGN components

The bright, hot disk surrounding the supermassive black hole emits an enormous amount of light that drives the dust apart as if the individual grains were tiny sails – a phenomenon known as radiation pressure. The images revealed the glowing dust, a warm, outflowing wind caused by that mechanism, which was heated by the hot central disk.

Simultaneously, farther out, much material is way brighter than it should have been if it was illuminated only by the bright accretion disk. By comparing the new images to past observations at various wavelengths, the researchers tied this finding to a collimated jet of hot gas emanating from the disk centre. While blasting through the galaxy, it hits and heats clouds of molecular gas and dust, leading to the unexpected bright infrared signal. Such jets are particularly bright at radio wavelengths when interacting with gas and particles in the environment around the supermassive black holes.

Altogether, the result confirms the so-called unified model of AGN. It promotes a configuration of a supermassive black hole in the centre of a galaxy, which attracts and collects gas and dust from the surrounding host galaxy, accumulating in an inner bright and hot disk. In addition, an outer, larger structure of cooler, outflowing material obstructs the view. Finally, a powerful gas jet is ejected from the centre. Different components are exposed to the observer, depending on the viewing angle. Although the observed features vary significantly between objects, the unified model proposes that those variations derive from intrinsically similar configurations of structures around the supermassive black hole, powering the AGN phenomenon.

View from the dome of the Large Binocular Telescope (LBT) through the open dome doors. In the foreground are the two large primary mirrors with the support structure for the secondary mirrors. © Marc-André Besel & Wiphu Rujopakarn


LBT – A precursor of future segmented-mirror telescopes

The LBT is located on Mount Graham, northeast of Tucson, USA, and operates its two 8.4-metre mirrors independently of each other, essentially functioning like two separate telescopes mounted side by side and aligned in parallel. MPIA is a member of the LBT Corporation via the LBT-Beteiligungsgesellschaft (holding company), which supplies 25% of all operations funding.

Combining the light from both mirrors, the LBT becomes an imaging interferometer (LBTI), allowing for approximately three times higher resolution observations than would be possible with each mirror on its own. To stabilize this high-resolution imaging machine, LBTI regularly deploys the OVMS+ vibration control system developed under MPIA leadership by MPIA’s Jörg-Uwe Pott to enable these challenging observations of distant galaxies. This imaging technique has been successfully employed to study volcanoes on the surface of Jupiter’s moon Io. The Jupiter results encouraged the researchers to use the interferometer to look now at an AGN.

“The AGN within the galaxy NGC 1068 is especially bright, so it was the perfect opportunity to test this method,” Isbell said. “These are the highest resolution direct images of an AGN taken so far.” In this context, direct images mean, they contain all faint and diffuse radiation from the structures observed. In contrast, images from other interferometers, such as the Very Large Telescope Interferometer (VLTI), are reconstructed from computations interpolating the missing imaging information.

Combining both mirrors produces images directly on the detector, very much like telescopes with segmented mirrors do, such as the James Webb Space Telescope, as well as the future 25-metre Giant Magellan Telescope (GMT) and the upcoming 39-metre Extremely Large Telescope (ELT), both being built in Chile. This way, Isbell and his collaborators produced the first ELT-like images of an AGN. As a result, the LBTI observations resolved individual features of up to 20 light-years at a distance of 47 million light-years. Previously, the various processes were blended due to low resolution, but now it is possible to view their individual impact.

A test for future observations

The study shows that the environments of AGN can be complex. The new findings help us understand the intricate ways in which AGN interact with their host galaxies. By probing distant galaxies in the early universe, when the galaxies were still young, we cannot achieve the same level of detail. Therefore, these results are like a local analogue.

“This type of imaging can be used on any astronomical object,” Isbell said. “We’ve already started looking at disks around stars and very large, evolved stars, which have dusty envelopes around them.”

Additional information

The MPIA team involved in this study comprised Jacob W. Isbell (now Steward Observatory, The University of Arizona, Tucson, USA) and Jörg-Uwe Pott.

Other researchers included Steve Ertel (Steward Observatory and Large Binocular Telescope Observatory, The University of Arizona, Tucson, USA), Gerd Weigelt (Max Planck Institute for Radio Astronomy, Bonn, Germany), and Marko Stalevski (Astronomical Observatory, Belgrade, Serbia and Sterrenkundig Observatorium, Universiteit Gent, Belgium).

This press release is based on the one published by the University of Arizona.




Contacts:

Dr. Markus Nielbock
Press and outreach officer

+49 6221 528-134
pr@mpia.de
MPIA press department
Max Planck Institute for Astronomy, Heidelberg, Germany

Dr. Jacob W. Isbell
jwisbell@arizona.edu
Jacob Isbell / UofA
Steward Observatory, The University of Arizona, Tucson, AZ, USA

Dr. Jörg-Uwe Pott
+49 6221 528-202
jpott@mpia.de
Jörg-Uwe Pott / MPIA
Max Planck Institute for Astronomy, Heidelberg, Germany



Original publication

Jacob W. Isbell, S. Ertel, J.-U. Pott et al.
Direct imaging of active galactic nucleus outflows and their origin with the 23 m Large Binocular Telescope
Nature Astronomy (2025)

Source | DOI



Video

The Unified Model of active galactic nuclei

Credit: ESO/L. Calçada and M. Kornmesser



Links

Nature Astronomy embargo policy
Ring of cosmic dust hides a supermassive black hole in Active Galactic Nucleus


February 16, 2022
Image of warm dust emission from the heart of an active galactic nucleus shows a ring-like structure that obscures the black hole


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One in a hundred

In the exact centre a supernova is seen as a small but bright blue dot. It lies atop the outer disc of a hazy-looking galaxy, which has a somewhat warped shape. Around this are a number of much more minor galaxies visible as glowing discs, and some points of light that are stars near to us, on a black background. X-shaped spikes around each star are optical artefacts from the telescope. Credit: ESA/Hubble & NASA, R. J. Foley (UC Santa Cruz).
Hi-res image

The subject of this NASA/ESA Hubble Space Telescope Picture of the Week is a supernova-hosting galaxy located about 600 million light-years away in the constellation Gemini. This picture was taken roughly two months after a supernova named SN 2022aajn was discovered in this galaxy. The supernova is visible as a blue dot at the centre of the image, brightening the hazy body of the galaxy.

Other than the announcement of its discovery in November 2022, SN 2022aajn has never been the subject of published research. Why, then, would Hubble observe this supernova? SN 2022aajn is what’s known as a Type Ia supernova, which results from the explosion of the core of a dead star. Supernovae of this type help astronomers measure the distance to faraway galaxies. This is possible because Type Ia supernovae are thought to be of the same intrinsic luminosity — no matter how bright they seem from Earth, they put out the same amount of light as other Type Ia supernovae. Thus, by comparing the observed brightness to the expected brightness, researchers can calculate the distance to the supernova and its host galaxy.

This seemingly simple measurement method is complicated by cosmic dust. The farther away a supernova is, the fainter and redder it will appear — but intergalactic dust can make a supernova appear fainter and redder as well. To understand this complication, researchers will use Hubble to survey a total of 100 Type Ia supernovae in seven wavelength bands from the ultraviolet to the near-infrared. This image combines data taken at four infrared wavelengths. Infrared light passes through dust more easily than visible or ultraviolet light. By comparing the brightness of the sampled supernovae across different wavelengths, researchers can disentangle the effects of dust and distance, helping to improve measurements of galaxies billions of light-years away and even the expansion of our Universe.



Monday, January 27, 2025

Catching Core-Collapse Supernovae Before They Happen

A still frame from an animation showing a huge star that expelled a shell of gas and dust about a year before going supernova. Credit:
NASA/JPL-Caltech

As scientists excitedly await the first light of the Vera C. Rubin Observatory, a recent study has projected that this facility will aid in identifying hundreds of massive stars on the cusp of death.

Before Detonation

Throughout their lifetimes, stars burn through hydrogen in their cores — million-degree furnaces smashing atoms together to form new ones. Massive stars, many times the mass of our Sun, have very high temperatures and pressures in their cores, causing them to live fast and die young. When all the fuel is burned, the star no longer produces enough thermal pressure to balance gravity, and the star dies in a rapid and massive explosion known as a Type II (or core-collapse) supernova.

But the final stages of a massive star’s life are not yet fully understood. Observations of Type II supernovae show narrow emission lines that indicate that their progenitor stars were surrounded by circumstellar material — material that was shed from the star as it evolved. However, the exact mechanism through which these stars lose mass is unclear, but if we can catch a star nearing its end but before its deadly detonation, we can better understand these massive stars’ elusive final days.

Artist’s illustration of the Rubin Observatory observing the sky searching for supernovae. The large field of view of the telescope captures large areas of sky in a single image. Credit:
NOIRLab/NSF/AURA/P. Marenfeld; CC BY 4.0

Rubin’s Remedy

Looking to explore many facets of the universe, the Vera C. Rubin Observatory’s Legacy Survey of Space and Time (LSST), first light anticipated July 2025, will scan the Southern Hemisphere sky searching for transient events like supernovae. Recognizing the power of LSST, Alexander Gagliano (The NSF AI Institute for Artificial Intelligence and Fundamental Interactions) and collaborators run simulated observations to predict how many stars LSST will catch in their final days, before they explode as supernovae.

Previous observations of Type II supernovae reveal enhanced emission in the months to years prior to explosion, and as LSST monitors the sky, it will be able to capture this pre-explosion emission. The authors carefully model the expected light curves for various types of core-collapse supernova precursors based on the handful of pre-explosion emission events observed thus far. With these models, the authors simulate LSST observations, applying two methods that would allow for the detection of stars gearing up to explode. The first being single-visit observations in which the enhanced emission is detected using differential photometry prior to the star’s explosion, independent of detecting the subsequent supernova. The second method involves going back after a supernova has been detected. By performing binned photometry of the star with observations taken of it prior to its explosion, the preceding emission can be recovered. From here, the authors can predict how many events LSST will recover after it goes online.

All core-collapse supernova precursors for both detection methods from one year of synthetic LSST observations. Each color corresponds to each model light curve used. Credit: Gagliano et al 2025


Power in Numbers

Based on their analysis, the authors predict that LSST will detect ~150–240 Type II supernova progenitors per year with single-visit photometry. Over the course of the first three years of LSST, they anticipate 150–400 detections from the binned photometry. This projected frequency of detections will launch the study of late-stage stellar life to new levels, increasing the observed sample of Type II supernova progenitors astronomically. As these detections come in, the observations will reveal the properties and behaviors of these stars in their final days. This opens the door to understanding how end-stage massive stars lose mass and ignite into the most powerful events in the universe.

By Lexi Gault

Citation

“Finding the Fuse: Prospects for the Detection and Characterization of Hydrogen-rich Core-collapse Supernova Precursor Emission with the LSST,” A. Gagliano et al 2025 ApJ 978 110.  doi:10.3847/1538-4357/ad9748



Exoplanets Need to be Prepared for Extreme Space Weather, Chandra Finds

Wolf 359
Credit: X-ray: NASA/CXC/SAO/S.Wolk, et al.; Illustration: NASA/CXC/SAO/M.Weiss; Image processing: NASA/CXC/SAO/N. Wolk





This artist’s illustration represents the results from a new study that examines the effects of X-ray and other high-energy radiation unleashed on potential exoplanets from a host star. As outlined in our latest press release, astronomers using NASA’s Chandra X-ray Observatory and ESA’s XMM-Newton observed Wolf 359, a red dwarf that is only 7.8 light-years from Earth, making it one of the closest stars to the Earth other than the Sun.

The artist’s rendering shows Wolf 359 in the foreground and a potential planet in orbit around it in the background. Red dwarfs are the most common type of star in the Universe. They are much smaller and dimmer than Sun-like stars, which allows them to last for trillions of years. This would give planets in orbit around them ample time for life to form and emerge, which makes them particularly interesting to scientists looking for life beyond the Solar System.

In the new study, researchers used Chandra and XMM to study the impact of steady X-ray and energetic ultraviolet (UV) radiation from Wolf 359 on the atmospheres of planets that might be orbiting the star. They found that only a planet with greenhouse gases like carbon dioxide in its atmosphere and at a relatively large distance away from Wolf 359 would have a chance to support life as we know it around a nearby star. The planet is depicted with the heavy cloud cover expected from the effects of greenhouse gases.

Animation of a Sun & Planet System
Animation Credit: NASA/CXC/SAO/A.Jubett)

Their work suggests that just being far enough away from the star’s harmful radiation would not be enough to allow a planet around Wolf 359 to sustain life. The team looked at the “habitable zone,” the region around a star where liquid water could exist on a planet’s surface, for Wolf 359. They found that an Earth-like planet in the middle of the habitable zone blanketed with greenhouse gases should be able to sustain an atmosphere for almost two billion years.

In addition to the dangers posed by the steady, everyday high-energy radiation from a star like Wolf 359, any orbiting planets would be subjected to occasional giant bursts of X-rays. Using observations with Chandra and XMM-Newton, astronomers discovered 18 X-ray flares, or outbursts, from Wolf 359 in under 4 days. Chandra data of Wolf 359 is shown in the inset. Extrapolating from these observed flares, the team expects that much more powerful and damaging flares would occur over longer periods of time. The combined effects of the steady X-ray and UV radiation and the flares means that any planet located in the habitable zone is unlikely to have a significant atmosphere long enough for multicellular life, as we know it on Earth, to form and survive. (Evidence suggests that it took at least 3 billion years for multicellular life to emerge on Earth.) The exception is the habitable zone's outer edge if a planet has a significant greenhouse effect.

The researchers used a special technique to estimate the energetic UV radiation from Wolf 359 using Chandra. The team looked at the difference in radiation measured with the High Resolution Camera (HRC) using two different filters: first, a thick filter that allows only X-rays to be detected, and second, a thinner filter that allows both X-rays and UV radiation to be detected. There are currently no specialized space missions for studying the most energetic ultraviolet radiation.

These results were presented at the 245th meeting of the American Astronomical Society in National Harbor, MD and are being prepared for publication in a journal. NASA's Marshall Space Flight Center manages the Chandra program. The Smithsonian Astrophysical Observatory's Chandra X-ray Center controls science operations from Cambridge, Massachusetts, and flight operations from Burlington, Massachusetts.



Visual Description:

This release features an artist's illustration of the red dwarf star Wolf 359, with a small orbiting planet in the distance. An inset image is included at our lower right.

Wolf 359 occupies much of the illustration. The fiery orange and yellow star fills the lower right corner of the image, extending well beyond the edges of the frame. The star's exterior appears to churn, with white hot flares bursting off the surface. A glowing yellow and orange haze surrounds the star, blanketing white flares and tendrils of hot gas.

In the distance, at our upper left, is an illustration of a small planet set against a black background dotted with faint specks of light. This represents one of two planets that may be in orbit around Wolf 359. Here, the orbiting planet has a blue-grey surface beneath a layer of swirling clouds. The water-like surface and cloudy atmosphere suggest that in this depiction, the planet is in Wolf 359's habitable zone, which may allow life to flourish.

Inset at our lower righthand corner is an X-ray image of Wolf 359. Here, the red dwarf star is a distant lavender dot glowing with purple haze, set against a pitch black background.



Fast Facts for Wolf 359:

Scale: Image is about 10 arcsec (3.8 billion km or 0.0004 light-years) across.
Category: Normal Stars & Star Clusters
Coordinates (J2000): RA 10h 56m 29s | Dec +07° 00´ 52"
Constellation: Leo
Observation Dates: 2 observations Nov 9-10, 2023
Observation Time: 244 hours 4 minutes (4 hours 4 minutes)
Obs. ID: 26490, 29051
Instrument: HRC
References: S. Wolk et al., 2025, 245th AAS meeting
Color Code: X-ray: purple
Distance Estimate: About 7.9 light-years


Sunday, January 26, 2025

DECam and Gemini South Discover Three Tiny ‘Stellar-Ghost-Town’ Galaxies

PR Image noirlab2502a
Sculptor Galaxies






Videos

Cosmoview Episode 92: DECam and Gemini South Discover Three Tiny ‘Stellar-Ghost-Town’ Galaxies
PR Video noirlab2502a
Cosmoview Episode 92: DECam and Gemini South Discover Three Tiny ‘Stellar-Ghost-Town’ Galaxies

Cosmoview Episodio 92: DECam y Gemini Sur descubren tres diminutas ciudades fantasmas
PR Video noirlab2502b
Cosmoview Episodio 92: DECam y Gemini Sur descubren tres diminutas ciudades fantasmas

The Sculptor galaxies relative to NGC 300 (3D Visualization)
PR Video noirlab2502c
The Sculptor galaxies relative to NGC 300 (3D Visualization)

Panning across the Sculptor galaxies
PR Video noirlab2502d
Panning across the Sculptor galaxies



Rare ultra-faint dwarf galaxies beyond the influence of other galaxies show evidence that star formation was stifled long ago

By combining data from the DESI Legacy Imaging Surveys and the Gemini South telescope, astronomers have investigated three ultra-faint dwarf galaxies that reside in a region of space isolated from the environmental influence of larger objects. The galaxies, located in the direction of NGC 300, were found to contain only very old stars, supporting the theory that events in the early Universe cut star formation short in the smallest galaxies.

Ultra-faint dwarf galaxies are the faintest type of galaxy in the Universe. Typically containing just a few hundred to a thousand stars — compared with the hundreds of billions that make up the Milky Way — these small diffuse structures usually hide inconspicuously among the many brighter residents of the sky. For this reason, astronomers have previously had the most luck finding them nearby, in the vicinity of our own Milky Way Galaxy.

But this presents a problem for understanding them; the Milky Way’s gravitational forces and hot corona can strip away the dwarf galaxies’ gas and interfere with their natural evolution. Additionally, further out beyond the Milky Way, ultra-faint dwarf galaxies increasingly become too diffuse and unresolvable for astronomers and traditional computer algorithms to detect.

That’s why a manual, by-eye search by University of Arizona astronomer David Sand was needed to discover three faint and ultra-faint dwarf galaxies located in the direction of spiral galaxy NGC 300 and the Sculptor constellation. “It was during the pandemic,” recalls Sand. “I was watching TV and scrolling through the DESI Legacy Survey viewer, focusing on areas of sky that I knew hadn't been searched before. It took a few hours of casual searching, and then boom! They just popped out.”

The images uncovered by Sand were taken for the DECam Legacy Survey (DECaLS), one of three public surveys, known as the DESI Legacy Imaging Surveys [1], that jointly imaged 14,000 square degrees of sky to provide targets for the ongoing Dark Energy Spectroscopic Instrument (DESI) Survey. DECals was conducted using the 570-megapixel Department of Energy-fabricated Dark Energy Camera (DECam), mounted on the U.S. National Science Foundation (NSF) Víctor M. Blanco 4-meter Telescope at Cerro Tololo Inter-American Observatory (CTIO) in Chile, a Program of NSF NOIRLab.

The Sculptor galaxies, as they are referred to in the paper, are among the first ultra-faint dwarf galaxies found in a pristine, isolated environment free from the influence of the Milky Way or other large structures. To investigate the galaxies further, Sand and his team used the Gemini South telescope, one half of the International Gemini Observatory, partly funded by the NSF and operated by NSF NOIRLab. The results from their study are presented in a paper appearing in The Astrophysical Journal Letters, as well as at a press conference at the AAS 245 meeting in National Harbor, Maryland.

Gemini South’s Gemini Multi-Object Spectrograph (GMOS) captured all three galaxies in exquisite detail. An analysis of the data showed that they appear to be empty of gas and contain only very old stars, suggesting that their star formation was stifled a long time ago. This bolsters existing theories that ultra-faint dwarf galaxies are stellar ‘ghost towns’ where star formation was cut off in the early Universe.

This is exactly what astronomers would expect for such tiny objects. Gas is the crucial raw material required to coalesce and ignite the fusion of a new star. But ultra-faint dwarf galaxies just have too little gravity to hold onto this all-important ingredient, and it is easily lost when they are buffeted by the dynamic Universe they are part of.

But the Sculptor galaxies are far from any larger galaxies, meaning their gas could not have been removed by giant neighbors. An alternative explanation is an event called the Epoch of Reionization — a period not long after the Big Bang when high-energy ultraviolet photons filled the cosmos, potentially boiling away the gas in the smallest galaxies. Another possibility is that some of the earliest stars in the dwarf galaxies underwent energetic supernova explosions, emitting ejecta at up to 35 million kilometers per hour (about 20 million miles per hour) and pushing the gas out of their own hosts from within.

If reionization is responsible, these galaxies would open a window into studying the very early Universe. “We don’t know how strong or uniform this reionization effect is,” explains Sand. “It could be that reionization is patchy, not occurring everywhere all at once. We’ve found three of these galaxies, but that isn’t enough. It would be nice if we had hundreds of them. If we knew what fraction was affected by reionization, that would tell us something about the early Universe that is very difficult to probe otherwise.”

“The Epoch of Reionization potentially connects the current day structure of all galaxies with the earliest formation of structure on a cosmological scale,” says Martin Still, NSF program director for the International Gemini Observatory. “The DESI Legacy Surveys and detailed follow-up observations by Gemini allow scientists to perform forensic archeology to understand the nature of the Universe and how it evolved to its current state.”

To speed up the search for more ultra-faint dwarf galaxies, Sand and his team are using the Sculptor galaxies to train an artificial intelligence system called a neural network to identify more. The hope is that this tool will be able to automate and accelerate discoveries, offering a much vaster dataset from which astronomers can draw stronger conclusions.





Notes

[1] The DESI Legacy Imaging Surveys data are served to the astronomical community via the Astro Data Lab at NSF NOIRLab’s Community Science and Data Center (CSDC).



More information

TThis research was presented in a paper entitled “Three Quenched, Faint Dwarf Galaxies in the Direction of NGC 300: New Probes of Reionization and Internal Feedback” to appear in The Astrophysical Journal Letters. DOI: 10.3847/2041-8213/ad927c

The team is composed of David J. Sand (University of Arizona), Burçin Mutlu-Pakdil (Dartmouth College), Michael G. Jones (University of Arizona), Ananthan Karunakaran (University of Toronto), Jennifer E. Andrews (International Gemini Observatory/NSF NOIRLab), Paul Bennet (Space Telescope Science Institute), Denija Crnojević (University of Tampa), Giuseppe Donatiello (Unione Astrofili Italiani), Alex Drlica-Wagner (Fermi National Accelerator Laboratory, Kavli Institute for Cosmological Physics, University of Chicago), Catherine Fielder (University of Arizona), David Martínez-Delgado (Unidad Asociada al CSIC), Clara E. Martínez-Vázquez (International Gemini Observatory/NSF NOIRLab), Kristine Spekkens (Queen’s University), Amandine Doliva-Dolinsky (Dartmouth College, University of Tampa), Laura C. Hunter (Dartmouth College), Jeffrey L. Carlin (AURA/Rubin Observatory), William Cerny (Yale University), Tehreem N. Hai (Rutgers, the State University of New Jersey), Kristen B.W. McQuinn (Space Telescope Science Institute, Rutgers, the State University of New Jersey), Andrew B. Pace (University of Virginia), and Adam Smercina (Space Telescope Science Institute)

Data for DECaLS were obtained at the U.S. National Science Foundation Víctor M. Blanco 4-meter telescope at NSF Cerro Tololo Inter-American Observatory, a Program of NSF NOIRLab. Pipeline processing and analyses of the data were supported by NOIRLab and the Lawrence Berkeley National Laboratory (LBNL). The Legacy Surveys project is supported by the U.S. Department of Energy (DOE) Office of Science, DOE Office of High Energy Physics, the National Energy Research Scientific Computing Center and by the U.S. National Science Foundation, Division of Astronomical Sciences.


NSF NOIRLab, the U.S. National Science Foundation center for ground-based optical-infrared astronomy, operates the International Gemini Observatory (a facility of NSF, NRC–Canada, ANID–Chile, MCTIC–Brazil, MINCyT–Argentina, and KASI–Republic of Korea), NSF Kitt Peak National Observatory (KPNO), NSF Cerro Tololo Inter-American Observatory (CTIO), the Community Science and Data Center (CSDC), and NSF–DOE Vera C. Rubin Observatory (in cooperation with DOE’s SLAC National Accelerator Laboratory). It is managed by the Association of Universities for Research in Astronomy (AURA) under a cooperative agreement with NSF and is headquartered in Tucson, Arizona.

The scientific community is honored to have the opportunity to conduct astronomical research on I’oligam Du’ag (Kitt Peak) in Arizona, on Maunakea in Hawai‘i, and on Cerro Tololo and Cerro Pachón in Chile. We recognize and acknowledge the very significant cultural role and reverence of I’oligam Du’ag (Kitt Peak) to the Tohono O’odham Nation, and Maunakea to the Kanaka Maoli (Native Hawaiians) community.



Links




Contacts

David Sand
Professor & Astronomer
University of Arizona/Steward Observatory
Email:
dsand@arizona.edu

Josie Fenske
Jr. Public Information Officer
NSF NOIRLab
Email:
josie.fenske@noirlab.edu


Close look at a local galaxy

An oval-shaped spiral galaxy, seen close-up. Its core is a compact, pale spot that glows brightly, filling the disc with bluish light. Faint strands of pale reddish dust swirl out from the core to the far sides of the disc. They each join up with an arm of thick, cloudy, red dust with brighter orange patches, that follows the edge of the disc around to the opposite end and a little off the galaxy. ESA/Webb, NASA & CSA, A. Leroy



The galaxy filling the frame in this NASA/ESA/CSA James Webb Space Telescope Picture of the Month is NGC 2566, a spiral galaxy located in the constellation Puppis. The image combines observations from two of Webb’s instruments, the Near-InfraRed Camera (NIRCam) and Mid-InfraRed Instrument (MIRI), to show off NGC 2566’s well-defined spiral arms, long central bar and delicate tracery of gas, dust and stars.

At 76 million light-years away, NGC 2566 is considered a nearby galaxy, making it an excellent target for studying fine details like star clusters and gas clouds. The new Webb images of NGC 2566 were collected as part of an observing programme (#3707) dedicated to understanding the connections between stars, gas and dust in nearby star-forming galaxies. NGC 2566 is just one of the 55 galaxies in the local Universe examined by Webb for this programme.

The mid-infrared wavelengths captured by MIRI highlight NGC 2566’s warm interstellar dust, including complex, sooty molecules called polycyclic aromatic hydrocarbons. The near-infrared NIRCam data give a detailed view of the galaxy’s stars, even those that are deeply embedded within clouds of gas. The NIRCam data also capture some of the light from the hydrocarbon molecules.

To gain a full understanding of the star-formation process in nearby galaxies, astronomers will combine Webb data with observations from other telescopes. At the long-wavelength end of the electromagnetic spectrum, the 66 radio dishes of the Atacama Large Millimeter/submillimeter Array (ALMA) provide a detailed view of the cold, turbulent clouds where stars are born. The NASA/ESA Hubble Space Telescope has also cast its gaze on NGC 2566, and a new Hubble image of this galaxy was released earlier this week. The Hubble data will help researchers take a census of the stars in nearby galaxies, especially the young stars that are bright at the ultraviolet and visible wavelengths to which Hubble is sensitive. Together, the Webb, Hubble and ALMA data provide a rich view of the cold gas, warm dust and brilliant stars in NGC 2566.

The Webb data are part of a Treasury programme, which means that the data may help answer multiple important questions about our Universe. Treasury data are available for use by scientists and the public without a waiting period, amplifying the scientific impact and allowing exploration to begin immediately.




Links


Saturday, January 25, 2025

Scientists Make First-Ever Detection of Mid-IR Flares in Sgr A*

This artist’s conception of the mid-IR flare in Sgr A* captures the variability, or changing intensity, of the flare as the black hole’s magnetic field lines approach each other. The byproduct of this magnetic reconnection is synchrotron emission. The emission seen in the flare intensifies as energized electrons travel along the SMBH’s magnetic field lines at close to the speed of light. The labels mark how the flare’s spectral index changes from the beginning to the end of the flare. Credit: CfA/Mel Weiss.
High Resolution Image

This artist’s animated conception of the mid-IR flare in Sgr A* captures the variability, or changing intensity, of the flare as the black hole’s magnetic field lines approach each other. The byproduct of this magnetic reconnection is synchrotron emission. The emission seen in the flare intensifies as energized electrons travel along the SMBH’s magnetic field lines at close to the speed of light. Credit: CfA/Mel Weiss, Amy C. Oliver.
Animation

This artist's conception of the mid-IR flare in Sgr A* captures the apparent movement of the flare as energized electrons spiral along the magnetic field lines of the supermassive black hole, and spike its intensity. These changes, or variability in intensity are known as synchrotron emission. Credit: CfA/Mel Weiss.
High Resolution Image

This 360-degree panoramic image reveals the plane of our Milky Way Galaxy edge-on from our perspective on Earth, and provides an almost “outside looking in” view of its disk, and central bulge. Scientists have, for the first time ever, successfully observed a mid-IR flare in Sgr A*, the supermassive black hole that resides at the heart of the Milky Way. Credit: ESO, S. Brunier.
High Resolution Image



An international team of scientists, including multiple astronomers from CfA, have made the first-ever detection of a mid-IR flare from Sgr A*

National Harbor, MD - Using the James Webb Space Telescope (JWST), a team of scientists led by astronomers from the Center for Astrophysics | Harvard & Smithsonian (CfA) detected a Mid-Infrared (mid-IR) flare from the supermassive black hole (SMBH) at the heart of the Milky Way galaxy for the first time. In simultaneous observations, the team found a radio counterpart flare lagging behind.

Scientists have been actively observing Sgr A*— a SMBH roughly 4 million times the mass of the Sun— since the early 1990s. Sgr A* regularly exhibits flares that can be observed in multiple wavelengths, allowing scientists to see different views of the same flare. This characteristic also helps them understand how it emits flares and on what timescales they occur. Despite a long history of successful observations, including imaging of this cosmic beast by the Event Horizon Telescope in 2022, one crucial piece of the puzzle— mid-IR observations— was missing until now.

Infrared light is a type of electromagnetic radiation. It has longer wavelengths than visible light, but shorter wavelengths than radio light. Mid-IR sits in the middle of the IR spectrum, and allows astronomers to observe objects, such as flares, that are often difficult to observe in other wavelengths due to impenetrable dust. Until the recent study, no team had yet successfully detected Sgr A*’s variability in the mid-IR range, leaving a gap in scientists’ understanding of what causes flares and questions about whether their theoretical models are complete.

"Sgr A*’s flare evolves and changes quickly, in a matter of hours, and not all of these changes can be seen at every wavelength," said Joseph Michail, one of the lead authors on the paper and a NSF Astronomy and Astrophysics Postdoctoral Fellow at the Smithsonian Astrophysical Observatory, which is a part of the CfA. "For over 20 years, we’ve known what happens in the radio and Near-infrared (NIR) ranges, but the connection between them was never 100% clear. This new observation in mid-IR fills in that gap."

Scientists aren’t 100% sure what causes flares, so they rely on models and simulations, which they compare with observations to try to understand the cause. Many simulations suggest that the flares in Sgr A* are caused by the interaction of magnetic field lines in the SMBH’s turbulent accretion disk. When two magnetic field lines approach each other they can connect to each other and release a large amount of their energy. A byproduct of this magnetic reconnection is synchrotron emission. The emission seen in the flare intensifies as energized electrons travel along the SMBH’s magnetic field lines at close to the speed of light.

Michail said, "Because mid-IR sits between the submillimeter and the NIR, it was keeping secrets locked away about the role of electrons, which have to cool to release energy to power the flares. Our new observations are consistent with the existing models and simulations, giving us one more strong piece of evidence to support the theory of what’s behind the flares."

Simultaneous observations with the SAO’s Submillimeter Array— a facility of the CfA, NASA’s Chandra X-ray Observatory (which is operated by the SAO), and NASA’s Nuclear Spectroscopic Telescope Array (NuSTAR) filled in an additional part of the story. No flare was detected during the X-ray observations, likely because this particular flare didn’t accelerate electrons to energies as high as some other flares do. But the team hit paydirt when they turned to the SMA, which detected a millimeter (mm) flare lagging roughly 10 minutes behind the mid-IR flare.

"Our research indicates that there may be a connection between the observed mm-variability and the observed MIR flare emission," said Sebastiano D. von Fellenberg, a postdoctoral researcher at the Max Planck Institute for Radio Astronomy (MPIfR) and the " lead author of the new paper. He added that the results underscore the importance of expanding multi-wavelength studies of not just Sgr A*, but other SMBHs, like M87*, to get a clear picture of what’s really happening within and beyond their accretion disks.

"While our observations suggest that Sgr A*’s mid-IR emission does indeed result from synchrotron emission from cooling electrons, there’s more to understand about magnetic reconnection and the turbulence in Sgr A*’s accretion disk," said von Fellenberg. "This first-ever mid-IR detection, and the variability seen with the SMA, has not only filled a gap in our understanding of what has caused the flare in Sgr A* but has also opened a new line of important inquiry."

Michail added, "We still want to know, and need to find out… what other secrets is Sgr A* holding that the mid-IR can unlock? What’s really behind the flare’s variable emission? There’s a wealth of knowledge stored up inside this black hole’s region just waiting for us to access it."

The new observations were presented today in a press conference at the 245th proceedings of the American Astronomical Society (AAS) in National Harbor, Maryland, and are accepted for publication in the Astrophysical Journal Letters (ApJL) .

Located near the summit of Maunakea on the Big Island of Hawaii, the Submillimeter Array (SMA) is one of the flagship observatories of the CfA. The observatory consists of eight radio dishes working together as one telescope, giving astronomers a window on a wide range of astronomical objects and phenomena: planets and comets in our own Solar System; the birth of stars and planets; and the supermassive black holes hidden at the centers of the Milky Way and other galaxies. The SMA is operated jointly by the CfA and the Academia Sinica in Taiwan.

Another version of this press release was issued by the Max Planck Institute for Radio Astronomy (MPIfR).




About the Center for Astrophysics | Harvard & Smithsonian

The Center for Astrophysics | Harvard & Smithsonian is a collaboration between Harvard and the Smithsonian designed to ask—and ultimately answer—humanity's greatest unresolved questions about the nature of the universe. The Center for Astrophysics is headquartered in Cambridge, MA, with research facilities across the U.S. and around the world.



Resource:

von Fellenberg, S., Roychowdhury, T., Michail, J. et al. "First mid-infrared detection and modeling of a flare from Sgr A*," Astrophysical Journal Letters, arxiv:



Media Contact:

Amy C. Oliver
Public Affairs Officer
Center for Astrophysics | Harvard & Smithsonian

amy.oliver@cfa.harvard.edu