Wednesday, February 05, 2025

Asteroid Bennu Sample Reveals a Broth of Life’s Ingredients

This mosaic image of asteroid Bennu is composed of 12 PolyCam images collected on Dec. 2 by the OSIRIS-REx spacecraft from a range of 15 miles (24 kilometers). The image was obtained at a 50° phase angle between the spacecraft, asteroid and the Sun, and in it, Bennu spans approximately 1,500 pixels in the camera’s field of view. Instrument Used: OCAMS (PolyCam). © NASA/Goddard/University of Arizona


Picture of the asteroid Bennu sample that was analyzed by the CAS group, with overlayed spectra taken by CAS Raman Microscope and in Helmholtz laboratories. © T. Grassi / B. Giuliano



Studies of rock and dust from asteroid Bennu delivered to Earth by NASA’s OSIRIS-REx spacecraft and analyzed by, among others, researchers from MPE’s Center of Astrochemistry (CAS), have revealed molecules that, on our planet, are key to life, as well as a history of saltwater that could have served as the “broth” for these compounds to interact and combine.

The findings do not show evidence for life itself, but they do suggest the conditions necessary for the emergence of life were widespread across the early solar system, increasing the odds life could have formed on other planets and moons.

"NASA’s OSIRIS-REx mission already is rewriting the textbook on what we understand about the beginnings of our solar system," said Nicky Fox, associate administrator, Science Mission Directorate at NASA Headquarters in Washington. “Asteroids provide a time capsule into our home planet’s history, and Bennu’s samples are pivotal in our understanding of what ingredients in our solar system existed before life started on Earth."

In research papers published Wednesday in the journals Nature and Nature Astronomy, scientists from NASA and other institutions, including MPE, shared results of the first in-depth analyses of the minerals and molecules in the Bennu samples, which OSIRIS-REx delivered to Earth in 2023.

“The CAS group is very proud to have contributed to analyzing the sample from asteroid Bennu using the CAS Raman Microscope. The Bennu sample from the OSIRIS-Rex mission was given to us by our long-term visiting scientist, Prof. Dr. Philippe Schmitt-Kopplin (Helmholtz Zentrum, München)”, says Paola Caselli, director at the Center for Astrochemical Studies (CAS), which contributed to the study. The work done at CAS has been part of the Master’s Thesis of Anique Shahid, under the supervision of Dr. Michela Giuliano, Dr. Tommaso Grassi, Paola Caselli (all CAS) and Prof. Schmitt-Kopplin (Helmholtz).

Detailed in the Nature Astronomy paper, among the most compelling detections were amino acids – 14 of the 20 that life on Earth uses to make proteins – and all five nucleobases that life on Earth uses to store and transmit genetic instructions in more complex terrestrial biomolecules, such as DNA and RNA, including how to arrange amino acids into proteins.




About NASA’s OSIRIS-REx

NASA Goddard provided overall mission management, systems engineering, and the safety and mission assurance for NASA’s OSIRIS-REx (Origins, Spectral Interpretation, Resource Identification and Security–Regolith Explorer). Dante Lauretta of the University of Arizona, Tucson, is the principal investigator. The university leads the science team and the mission’s science observation planning and data processing. Lockheed Martin Space in Littleton, Colorado, built the spacecraft and provided flight operations. NASA Goddard and KinetX Aerospace were responsible for navigating the OSIRIS-REx spacecraft. Curation for OSIRIS-REx takes place at NASA’s Johnson Space Center in Houston. International partnerships on this mission include the OSIRIS-REx Laser Altimeter instrument from CSA (Canadian Space Agency) and asteroid sample science collaboration with JAXA’s (Japan Aerospace Exploration Agency) Hayabusa2 mission. OSIRIS-REx is the third mission in NASA’s New Frontiers Program, managed by the agency’s Marshall Space Flight Center in Huntsville, Alabama, for the agency’s Science Mission Directorate in Washington.



Contacts:

Prof. Dr. Paola Caselli
Director of the CAS group at MPE
tel:+49 89 30000-3400
fax:+49 89 30000-3399

caselli@mpe.mpg.de
Max Planck Institute for Extraterrestrial Physics, Garching

Dr. Barbara Michela Giuliano
scientist in CAS group
tel:+49 89 30000-3317

giuliano@mpe.mpg.de
Max Planck Institute for Extraterrestrial Physics

Dr. Tommaso Grassi
Wissenschaftlicher Mitarbeiter, IT
tel:+49 89 30000-3639

tgrassi@mpe.mpg.de

Prof. Dr. Dr. Philippe Schmitt-Kopplin
Director of the Research Unit Analytical Biogeochemistry
tel:+49 89 3187-3246

philippe.schmittkopplin@helmholtz-munich.de
https://www.helmholtz-munich.de/en/bgc/pi/philippe-schmitt-kopplin
Helmholtz Munich




Further Information

Official Press release of NASA about analysis of Bennu asteroid.






Tuesday, February 04, 2025

Debugging Galaxy Evolution with L-GALAXIES

The semi-analytical model L-GALAXIES simulates astrophysical phenomena to predict galaxy properties and scaling relations. Composite image: MPA

The three plots show the L-GALAXIES model predictions (solid lines) for Milky Way-mass galaxies compared to observational data points at the corresponding redshift. The left plot demonstrates that the model fails to produce a sufficient number of quenched galaxies. The middle plot indicates that the model overestimates the sizes of quenched galaxies. The plot on the right shows that quenched galaxies in the model are not sufficiently compact. © MPA


The plot illustrates the gas fractions within galaxy halos as a function of halo mass for six redshift intervals (various colors) from two simulations (dashed and solid lines). The lack of redshift evolution suggests that the physical processes governing gas retention within halos in the L-GALAXIES model are largely time-independent. The AGN feedback in L-GALAXIES primarily prevents hot gas cooling without significantly altering its spatial distribution. © MPA



The formation and evolution of galaxies are among the most complex challenges in astrophysics. Recent advancements with instruments like JWST and ALMA have shed light on high-redshift galaxies – those that existed billions of years ago. However, most theoretical models are tuned to match galaxies in the local universe. Researchers from the Max Planck Institute for Astrophysics and the University of Bonn now comprehensively evaluated the Munich semi-analytical model L-GALAXIES using the latest observations and found that while the model aligns well with the properties of local galaxies, it struggles with key aspects of high-redshift galaxies. Particularly, the study highlights critical issues with the model’s predictions of quenched galaxies, those that have ceased star formation. Their results suggest a need to revise the implementation of processes driving star formation quenching, including supermassive black hole feedback and galaxy mergers.

Observations from surveys such as SDSS, CANDELS, and COSMOS provide essential insights into galaxy properties and scaling relations. However, to uncover the underlying processes driving galaxy evolution, astronomers need to simulate the relevant astrophysical phenomena. The Munich semi-analytical model, L-GALAXIES, offers a self-consistent framework for tackling these challenges. Over the past three decades, L-GALAXIES has undergone continuous development, primarily at the Max Planck Institute for Astrophysics (MPA) in collaboration with international teams, establishing itself as a corner-stone tool for studying galaxy evolution. The model strikes a balance between computational efficiency and detailed physical modelling, making it a powerful complement to computationally demanding hydro-dynamical simulations.

The L-GALAXIES model builds upon its previous generation with a series of advancements that are motivated both by new observational data and a resulting deeper physical understanding of complex processes such as gas accretion and cooling, star formation, chemical enrichment, and stellar and black hole feedback. The most recent versions incorporate advanced environmental mechanisms like ram-pressure and tidal stripping. The models are calibrated using Monte Carlo Markov Chain (MCMC) techniques and constrained by low-redshift observational data. Together, these updates and calibrations represent the cutting edge of semi-analytical galaxy formation modelling.

Recent observational campaigns, particularly those utilizing advanced ground- and space-based instruments such as the Hubble Space Telescope (HST), the Atacama Large Millimeter/submillimeter Array (ALMA), and the James Webb Space Telescope (JWST), have provided unprecedented insights into the evolution of high-redshift galaxies. These observations reveal the size, compactness, and abundance of quenched galaxies at redshifts around z=2 (when the universe was just 3 billion years old) and beyond, offering a unique opportunity to rigorously test L-GALAXIES predictions well outside its original calibration regime. In particular, they are identifying areas where the model aligns with or deviates from observed trends, providing crucial guidance for improving its treatment of high-redshift galaxy populations.

The current study evaluates the latest version of L-GALAXIES alongside its two preceding iterations, focusing on their ability to reproduce the evolution of galaxy number density, size, and surface density across cosmic time. The analysis spans the history of the universe, from 500 million years after the Big Bang to the present day (~13.5 billion years later), with a specific focus on the first few billion years. It marks the first comprehensive comparison of L-GALAXIES predictions to high-redshift observations.

Galaxies were classified as star-forming or quenched based on their near-ultraviolet (NUV) to near-infrared (J-band) color. Sizes and surface densities were determined using methodologies consistent with observational studies. Additionally, X-ray data from instruments such as Chandra and XMM-Newton, along with microwave and longer wavelength data from Planck, were incorporated to examine baryon and gas distributions within host halos, shedding light on the interaction between baryonic matter and galaxy processes.

Although the model shows significant agreement with the properties of star-forming galaxies at both low and high redshifts, the study highlights significant discrepancies in the model’s predictions for quenched galaxies, particularly for Milky Way-mass and more massive systems at the times when the Universe was younger than 2 billion years old. The model underestimates the abundance of quenched galaxies by a factor of 60 and over-predicts the fraction of baryonic matter within galaxy clusters by around 15-20%. Moreover, the predicted sizes of galaxies are several times larger than observed, pointing to deficiencies in the modelling of star formation suppression mechanisms such as active galactic nucleus (AGN) feedback and galaxy mergers.




Author:

Akash Vani

tel:2298
vani@mpa-garching.mpg.de

Original publication

Akash Vani, Mohammadreza Ayromlou, Guinevere Kauffmann, Volker Springel
Probing galaxy evolution from z = 0 to z ≃ 10 through galaxy scaling relations in three L-GALAXIES flavours
Monthly Notices of the Royal Astronomical Society, Volume 536, Issue 1, January 2025, Pages 777–806


Source | DOI

More Information

LGalaxies website


Monday, February 03, 2025

Researchers capture direct high-definition image of the “Cosmic Web”

Simulation of a vast region of the Universe based on the current cosmological model and performed using supercomputers. In the image, the faint glow of the gas within the cosmic filaments, forming a dense cosmic web, is shown in white. At the intersections of these filaments, the gas within galaxies, which fuels the formation of new stars, is highlighted in red. © Alejandro Benitez-Llambay/Universität Mailand-Bicocca/MPA


The image shows the diffuse gas (yellow to purple) contained within the cosmic filament connecting two galaxies (yellow stars), extending across a vast distance of 3 million light-years. © Davide Tornotti/University of Milano-Bicocca


A twin of the cosmic filament observed in the MUDF as seen in a supercomputer simulation describing the large-scale distribution of gas in the Universe. The gas flowing within the cosmic web, feeding galaxy formation at filament intersections, is shown in purple. Davide Tornotti/University of Milano-Bicocca/MPA




Matter in intergalactic space is distributed in a vast network of interconnected filamentary structures, collectively referred to as the cosmic web. With hundreds of hours of observations, an international team of researchers has now obtained an unprecedented high-definition image of a cosmic filament inside this web, connecting two active forming galaxies – dating back to when the Universe was about 2 billion years old.

A pillar of modern cosmology is the existence of dark matter, which constitutes about 85% of all matter in the Universe. Under the influence of gravity, dark matter forms an intricate cosmic web composed of filaments, at whose intersections the brightest galaxies emerge. This cosmic web acts as the scaffolding on which all visible structures in the Universe are built: within the filaments, gas flows to fuel star formation in galaxies. Direct observations of the fuel supply of such galaxies would advance our understanding of galaxy formation and evolution

. However, studying the gas within this cosmic web is incredibly challenging. Intergalactic gas has been detected mainly indirectly through its absorption of light from bright background sources. But the observed results do not elucidate the distribution of this gas. Even the most abundant element, hydrogen, emits only a faint glow, making it basically impossible for instruments of the previous generation to directly observe such gas.

In this new study, an international team led by researchers at the University of Milano-Bicocca and including scientists at the Max Planck Institute for Astrophysics (MPA) obtained an unprecedented high-definition image of a cosmic filament using MUSE (Multi-Unit Spectroscopic Explorer), an innovative spectrograph installed on the Very Large Telescope at the European Southern Observatory in Chile. Even with the advanced capabilities of this sophisticated instrument, the research group had to carry out one of the most ambitious MUSE observation campaigns ever completed in a single region of the sky, acquiring data over hundreds of hours to detect the filament at high significance.

The study, led by Davide Tornotti, PhD student at the University of Milano-Bicocca, used this ultrasensitive data to produce the sharpest image ever obtained of a cosmic filament spanning 3 million light-years and connecting two galaxies, each hosting an active supermassive black hole. The discovery, recently published in Nature Astronomy opens new avenues to directly constrain gas properties within intergalactic filaments and to refine our understanding of galaxy formation and evolution.

“By capturing the faint light emitted by this filament, which travelled for just under 12 billion years to reach Earth, we were able to precisely characterize its shape, explains Davide Tornotti. “For the first time, we could trace the boundary between the gas residing in galaxies and the material contained within the cosmic web through direct measurements.” The researchers took advantage of supercomputer simulations of the Universe run at MPA to calculate predictions of the expected filamentary emission given the current cosmological model. “When comparing to the novel high-definition image of the cosmic web, we find substantial agreement between current theory and observations,” Tornotti adds.

This discovery and the encouraging agreement with supercomputer simulations are key to understanding the tenuous gas environment around galaxies and open up novel possibilities to pin down the galaxies’ fuel supply. Fabrizio Arrigoni Battaia, MPA staff scientist involved in the study, concludes: “We are thrilled by this direct, high-definition observation of a cosmic filament. But as people say in Bavaria: ‘Eine ist keine’ – one doesn’t count. So we are gathering further data to uncover more such structures, with the ultimate goal to have a comprehensive vision of how gas is distributed and flows in the cosmic web.”




Contact:

Fabrizio Arrigoni Battaia
Scientific Staff
tel:2288

arrigoni@mpa-garching.mpg.de



Original publication

Davide Tornotti et al.
High-definition imaging of a filamentary connection between a close quasar pair at z=
Nature Astronomy, 29 January 2025


Source



More Information

Revealing a filament from the cosmic web
ESO Press Release


Sunday, February 02, 2025

Black Holes Can Cook for Themselves, Chandra Study Shows

Perseus Cluster & the Centaurus Cluster
Credit: Perseus Cluster: X-ray: NASA/CXC/SAO/V. Olivares et al.; Optical/IR: DSS; H-alpha: CFHT/SITELLE; Centaurus Cluster: X-ray: NASA/CXC/SAO/V. Olivaresi et al.; Optical/IR: NASA/ESA/STScI; H-alpha: ESO/VLT/MUSE; Image Processing: NASA/CXC/SAO/N. Wolk





Astronomers have taken a crucial step in showing that the most massive black holes in the universe can create their own meals. Data from NASA’s Chandra X-ray Observatory and the Very Large Telescope (VLT) provide new evidence that outbursts from black holes can help cool down gas to feed themselves.

This study was based on observations of seven clusters of galaxies. The centers of galaxy clusters contain the universe’s most massive galaxies, which harbor huge black holes with masses ranging from millions to tens of billions of times that of the Sun. Jets from these black holes are driven by the black holes feasting on gas.

These images show two of the galaxy clusters in the study, the Perseus Cluster and the Centaurus Cluster. Chandra data represented in blue reveals X-rays from filaments of hot gas, and data from the VLT, an optical telescope in Chile, shows cooler filaments in red.

The results support a model where outbursts from the black holes trigger hot gas to cool and form narrow filaments of warm gas. Turbulence in the gas also plays an important role in this triggering process.

According to this model, some of the warm gas in these filaments should then flow into the centers of the galaxies to feed the black holes, causing an outburst. The outburst causes more gas to cool and feed the black holes, leading to further outbursts.

This model predicts there will be a relationship between the brightness of filaments of hot and warm gas in the centers of galaxy clusters. More specifically, in regions where the hot gas is brighter, the warm gas should also be brighter. The team of astronomers has, for the first time, discovered such a relationship, giving critical support for the model.

This result also provides new understanding of these gas-filled filaments, which are important not just for feeding black holes but also for causing new stars to form. This advance was made possible by an innovative technique that isolates the hot filaments in the Chandra X-ray data from other structures, including large cavities in the hot gas created by the black hole’s jets.

The newly found relationship for these filaments shows remarkable similarity to the one found in the tails of jellyfish galaxies, which have had gas stripped away from them as they travel through surrounding gas, forming long tails. This similarity reveals an unexpected cosmic connection between the two objects and implies a similar process is occurring in these objects.

This work was led by Valeria Olivares from the University of Santiago de Chile, and was published Monday in Nature Astronomy and is available online. The study brought together international experts in optical and X-ray observations and simulations from the United States, Chile, Australia, Canada, and Italy. The work relied on the capabilities of the MUSE (Multi Unit Spectroscopic Explorer) instrument on the VLT, which generates 3D views of the universe.

NASA's Marshall Space Flight Center in Huntsville, Alabama, 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 composite images shown side-by-side of two different galaxy clusters, each with a central black hole surrounded by patches and filaments of gas. The galaxy clusters, known as Perseus and Centaurus, are two of seven galaxy clusters observed as part of an international study led by the University of Santiago de Chile.

In each image, a patch of purple with neon pink veins floats in the blackness of space, surrounded by flecks of light. At the center of each patch is a glowing, bright white dot. The bright white dots are black holes. The purple patches represent hot X-ray gas, and the neon pink veins represent filaments of warm gas. According to the model published in the study, jets from the black holes impact the hot X-ray gas. This gas cools into warm filaments, with some warm gas flowing back into the black hole. The return flow of warm gas causes jets to again cool the hot gas, triggering the cycle once again.

While the images of the two galaxy clusters are broadly similar, there are significant visual differences. In the image of the Perseus Cluster on the left, the surrounding flecks of light are larger and brighter, making the individual galaxies they represent easier to discern. Here, the purple gas has a blue tint, and the hot pink filaments appear solid, as if rendered with quivering strokes of a paintbrush. In the image of the Centaurus Cluster on the right, the purple gas appears softer, with a more diffuse quality. The filaments are rendered in more detail, with feathery edges, and gradation in color ranging from pale pink to neon red.




Fast Facts for Perseus Cluster:

Credit: X-ray: NASA/CXC/SAO/V. Olivares et al.; Optical/IR: DSS; H-alpha: CFHT/SITELLE; Image Processing: NASA/CXC/SAO/N. Wolk
Scale: Image is about 6.4 arcmin (450,000 light-years) across.
Category: Groups and Clusters of Galaxies
Coordinates (J2000): RA 3h 19m 47.71 | Dec +41° 31´ 15.8"
Constellation: Perseus
Observation Dates: 29 observations between Sep 20, 1999 and Nov 7, 2016
Observation Time: 416 hours 45 minutes (17 days 8 hours 45 minutes)
Obs. ID: 428, 502, 503, 3209, 3404, 1513, 4289, 4946, 4947, 3939-4953, 6139, 6145, 6146, 11713-11716, 12025, 12033, 12036, 12037, 19568, 19913-19915

Instrument: ACIS
References: Olivares, V. et al. 2025, Nature Astronomy; arXiv:2501.01902
Color Code: X-ray: blue; Optical: red, green, blue; H-alpha: red
Distance Estimate: About 240 million light-years from Earth



Fast Facts for Centaurus Cluster:

Credit: X-ray: NASA/CXC/SAO/V. Olivaresi et al.; Optical/IR: NASA/ESA/STScI; H-alpha: ESO/VLT/MUSE; Image Processing: NASA/CXC/SAO/N. Wolk
Scale: Image is about 1.4 arcmin (57,000 light-years) across.
Category: Groups and Clusters of Galaxies
Coordinates (J2000): RA 12h 48m 49.2s | Dec -41° 18´ 43.8"
Constellation: Centaurus
Observation Dates: 16 observations from May 22, 2000 to Jun 05, 2014
Observation Time: 240 hours 1 minute (10 days 1 minutes)
Obs. ID: 504 ,505 ,1560 ,4190, 4191, 4954, 4955 ,5310, 16223-16225 ,16534 ,16607-16610
Instrument: ACIS
References: Olivares, V. et al. 2025, Nature Astronomy; arXiv:2501.01902
Color Code: X-ray: blue; Optical/IR: red, green, blue; H-alpha: red
Distance Estimate: About 145 million light-years from Earth


Saturday, February 01, 2025

NSF VLA Contributes Crucial Puzzle Piece to ‘Peculiar’ High Energy Transient

Illustration of a tidal disruption event
Credit: ESA/C. Carreau

Hi-Res File

An artist's concept of the Einstein probe
Credit: NSF/AUI/NSF NRAO/J.Hellerman

Hi-Res File



Non-detection at radio wavelengths may prove to be the critical clue toward categorizing EP240408a as an entirely new phenomenon

High-energy transient signals are most often determined to be gamma-ray burst events, but the recently-launched Einstein Probe has expanded astronomers’ ability to quickly respond to similar signals occurring at X-ray wavelengths. Now, a multi-wavelength study of EP240408a concludes that while many of the signal’s characteristics might lead to the conclusion that it is a gamma-ray burst, the non-detection at radio wavelengths precludes that possibility. Instead, the international team of astronomers suggest that EP240408a is either a rare jetted tidal disruption event or, perhaps, an entirely new type of astronomical phenomenon. This was discovered in only the first two months of the commissioning phase.

Tidal disruption events (TDEs) occur when a star is shredded by a nearby black hole; these events are themselves rare, with fewer than 100 discovered so far. In even more rare cases, the black hole’s powerful tidal forces propel some of the shredded stellar material outward in high-velocity jets, which then interact with nearby clouds of dust and gas and shine brightly in X-ray and radio. Thus far, only four TDEs are known to have relativistic-velocity jets associated with them

An international team of astronomers led by Brendan O’Connor, an astronomer at Carnegie Mellon University, analyzed the signal from EP240408a across the span of wavelengths from radio to X-ray and concluded that this X-ray transient is—thus far—unique. “It ticks the boxes for a bunch of different kinds of phenomena, but it doesn’t tick all of the boxes for anything,” O’Connor summarizes. “And I think the radio non-detection is a massive box that we don’t know how to not tick.”

The team’s expansive follow-up campaign further characterized the X-ray emissions from EP240408a and identified a potential host galaxy in optical wavelengths. Crucially, however, O’Connor notes the non-detection in radio wavelengths as potentially the deciding factor in fully categorizing the source. Observations from the U.S. National Science Foundation Very Large Array (NSF VLA), operated by the U.S. National Science Foundation National Radio Astronomy Observatory (NSF NRAO), at 11 days, 158 days, and 258 days after EP240408a’s initial discovery indicated no radio emission from the source.

“I think where radio really fits in is that when we see something this bright, for this long, in X-rays, it usually has an extremely luminous radio counterpart. And here we see nothing, which is extremely peculiar,” O’Connor says.

After methodically eliminating a number of potential explanations including active galactic nuclei, fast blue optical transients, fast X-ray transients, and other variations of previously-characterized phenomena, O’Connor and his co-authors conclude that EP240408a is extragalactic in origin and is most likely a relativistically-jetted Tidal Disruption Event.

“Because of this new wide field view of the X-ray universe, there’s a diverse range of phenomena we can see that weren’t possible before. And it looks like this transient, EP 240408a, is new. It’s something that we don’t think we’ve seen before,” O’Connor says. “It’s falling in a range of energy, of wavelengths, that it can be detected at, and the time scales are so short, that it’s probably something that we’ve just missed before now.”

O’Connor emphasizes that the current lack of radio emissions is pivotal, but that follow-up observations in radio wavelengths will hopefully yield future detections as the material within the jets slows down to energies corresponding to radio—a process expected to occur on timescales of roughly 1000 days. Thus, follow-up radio observations with the NRAO VLA will be imperative.

Thus, EP240408a appears to be giving astronomers an in-between glimpse of a high-energy transient’s signal after its initial X-ray outburst but before its relativistic-speed jet flares in radio. “It seems to me that this is the most likely explanation for why we aren’t seeing radio emission. Hopefully, eventually, we will see a jet at radio wavelengths, either with the current setup of the VLA or the Next Generation VLA, and we can monitor it for years to come in order to learn even more about this explosion,” O’Connor muses;

“These results highlight the importance of multiwavelength observations in fully understanding the astronomical object,” says Joe Pesce, NSF Program Director for the NRAO. “The complete picture of what’s really happening requires a holistic study.”

An international team of astronomers were involved in the study, including Dheeraj Pasham at MIT, Igor Andreoni at the University of North Carolina Chapel Hill, Jeremy Hare at the Catholic University of America, Paz Beniamini at the Open University of Israel, and Eleonora Troja at the University of Rome Tor Vergata, among others. You can read the full scientific paper here.

The National Radio Astronomy Observatory (NRAO) is a facility of the U.S. National Science Foundation, operated under cooperative agreement by Associated Universities, Inc.



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



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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.