Showing posts with label radio galaxy. Show all posts
Showing posts with label radio galaxy. Show all posts

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.

The RAS accepts papers for its journals based on the principle of peer review, in which fellow experts on the editorial boards accept the paper as worth considering. The Society issues press releases based on a similar principle, but the organisations and scientists concerned have overall responsibility for their content.


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Monday, July 26, 2021

EHT pinpoints dark heart of the nearest radio galaxy


Distance scales uncovered in the Centaurus A jet. The top left image shows how the jet disperses into gas clouds that emit radio waves, captured by the ATCA and Parkes observatories. The top right panel displays a color composite image, with a 40x zoom compared to the first panel to match the size of the galaxy itself. Submillimeter emission from the jet and dust in the galaxy measured by the LABOCA/APEX instrument is shown in orange. X-ray emission from the jet measured by the Chandra spacecraft is shown in blue. Visible white light from the stars in the galaxy has been captured by the MPG/ESO 2.2-metre telescope. The next panel below shows a 165000x zoom image of the inner radio jet obtained with the TANAMI telescopes. The bottom panel depicts the new highest resolution image of the jet launching region obtained with the EHT at millimeter wavelengths with a 60000000x zoom in telescope resolution. Indicated scale bars are shown in light years and light days. One light year is equal to the distance that light travels within one year: about nine trillion kilometers. In comparison, the distance to the nearest-known star from our Sun is approximately four light years. One light day is equal to the distance that light travels within one day: about six times the distance between the Sun and Neptune. Credit: Radboud University; CSIRO/ATNF/I.Feain et al., R.Morganti et al., N.Junkes et al.; ESO/WFI; MPIfR/ESO/APEX/A. Weiss et al.; NASA/CXC/CfA/R. Kraft et al.; TANAMI/C. Mueller et al.; EHT/M. Janssen et al.
Hi-res image


Highest resolution image of Centaurus A obtained with the Event Horizon Telescope on top of a color composite image of the entire galaxy. Credit: Radboud University; ESO/WFI; MPIfR/ESO/APEX/A. Weiss et al.; NASA/CXC/CfA/R. Kraft et al.; EHT/M. Janssen et al
. Hi-res image

An international team anchored by the Event Horizon Telescope (EHT) Collaboration, which is known for capturing the first image of a black hole in the galaxy Messier 87, has now imaged the heart of the nearby radio galaxy Centaurus A in unprecedented detail. The astronomers pinpoint the location of the central supermassive black hole and reveal how a gigantic jet is being born. Most remarkably, only the outer edges of the jet seem to emit radiation, which challenges our theoretical models of jets. This work, led by Michael Janssen from the Max Planck Institute for Radio Astronomy in Bonn and Radboud University Nijmegen is published in Nature Astronomy on July 19th.

At radio wavelengths, Centaurus A emerges as one of the largest and brightest objects in the night sky. After it was identified as one of the first known extragalactic radio sources in 1949, Centaurus A has been studied extensively across the entire electromagnetic spectrum by a variety of radio, infrared, optical, X-ray, and gamma-ray observatories. At the center of Centaurus A lies a black hole with the mass of 55 million suns, which is right between the mass scales of the Messier 87 black hole (six and a half billion suns) and the one in the center of our own galaxy (about four million suns).

In a new paper in Nature Astronomy, data from the 2017 EHT observations have been analyzed to image Centaurus A in unprecedented detail. “This allows us for the first time to see and study an extragalactic radio jet on scales smaller than the distance light travels in one day. We see up close and personally how a monstrously gigantic jet launched by a supermassive black hole is being born”, says astronomer Michael Janssen.

Compared to all previous high-resolution observations, the jet launched in Centaurus A is imaged at a tenfold higher frequency and sixteen times sharper resolution. With the resolving power of the EHT, we can now link the vast scales of the source, which are as big as 16 times the angular diameter of the Moon on the sky, to their origin near the black hole in a region of merely the width of an apple on the Moon when projected on the sky. That is a magnification factor of one billion.

Understanding jets

Supermassive black holes residing in the center of galaxies like Centaurus A are feeding off gas and dust that is attracted by their enormous gravitational pull. This process releases massive amounts of energy and the galaxy is said to become ‘active’. Most matter lying close to the edge of the black hole falls in. However, some of the surrounding particles escape moments before capture and are blown far out into space: Jets – one of the most mysterious and energetic features of galaxies – are born.

Astronomers have relied on different models of how matter behaves near the black hole to better understand this process. But they still do not know exactly how jets are launched from its central region and how they can extend over scales that are larger than their host galaxies without dispersing out. The EHT aims to resolve this mystery.

The new image shows that the jet launched by Centaurus A is brighter at the edges compared to the center. This phenomenon is known from other jets, but has never been seen so pronouncedly before. “Now we are able to rule out theoretical jet models that are unable to reproduce this edge-brightening. It’s a striking feature that will help us better understand jets produced by black holes”, says Matthias Kadler, TANAMI leader and professor for astrophysics at the University of Würzburg in Germany.

Future observations

With the new EHT observations of the CentaurusA jet, the likely location of the black hole has been identified at the launching point of the jet. Based on this location, the researchers predict that future observations at an even shorter wavelength and higher resolution would be able to photograph the central black hole of Centaurus A. This will require the use of space-based satellite observatories.

“These data are from the same observing campaign that delivered the famous image of the black hole in M87. The new results show that the EHT provides a treasure trove of data on the rich variety of black holes and there is still more to come”, says Heino Falcke, EHT board member and professor for Astrophysics at Radboud University.

Additional Information

To observe the Centaurus A galaxy with this unprecedentedly sharp resolution at a wavelength of 1.3 mm, the EHT collaboration used Very Long Baseline Interferometry (VLBI), the same technique with which the famous image of the black hole in M87 was made. An alliance of eight telescopes around the world, of which ALMA is the most sensitive element, joined together to create the virtual Earth-sized Event Horizon Telescope. The EHT collaboration involves more than 300 researchers from Africa, Asia, Europe, North and South America.

The EHT consortium consists of 13 stakeholder institutes: the Academia Sinica Institute of Astronomy and Astrophysics, the University of Arizona, the University of Chicago, the East Asian Observatory, Goethe University Frankfurt, Institut de Radioastronomie Millimétrique (MPG/CNRS/IGN), Large Millimeter Telescope, Max Planck Institute for Radio Astronomy, MIT Haystack Observatory, National Astronomical Observatory of Japan, Perimeter Institute for Theoretical Physics, Radboud University and the Center for Astrophysics | Harvard & Smithsonian.

TANAMI (Tracking Active Galactic Nuclei with Austral Milliarcsecond Interferometry) is a multiwavelength program to monitor relativistic jets in active galactic nuclei of the Southern Sky. This program has been monitoring Centaurus A with VLBI at centimeter-wavelengths since the mid 2000s. The TANAMI array consists of nine radio telescopes located on four continents observing at wavelengths of 4 cm and 1.3 cm.

The Atacama Large Millimeter/submillimeter Array (ALMA), an international astronomy facility, is a partnership of the European Organisation for Astronomical Research in the Southern Hemisphere (ESO), the U.S. National Science Foundation (NSF) and the National Institutes of Natural Sciences (NINS) of Japan in cooperation with the Republic of Chile. ALMA is funded by ESO on behalf of its Member States, by NSF in cooperation with the National Research Council of Canada (NRC) and the Ministry of Science and Technology (MOST) and by NINS in cooperation with the Academia Sinica (AS) in Taiwan and the Korea Astronomy and Space Science Institute (KASI).

ALMA construction and operations are led by ESO on behalf of its Member States; by the National Radio Astronomy Observatory (NRAO), managed by Associated Universities, Inc. (AUI), on behalf of North America; and by the National Astronomical Observatory of Japan (NAOJ) on behalf of East Asia. The Joint ALMA Observatory (JAO) provides the unified leadership and management of the construction, commissioning and operation of ALMA.

Scientific Paper 

Source:   Atacama Large Millimeter/submillimeter Array (ALMA)/Press Releases



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Tuesday, August 28, 2018

Gemini Confirms the Most Distant Radio Galaxy


Top: Two-dimensional GMOS spectrum of the strong emission line observed in the radio galaxy TGSS J1530+1049. The size of the emission region is a bit less than one arcsec. Bottom: One-dimensional profile of the observed emission line. The asymmetry indicates that the line is Lyman-α at redshift of z = 5.72, making TGSS J1530+1049 the most distant radio galaxy known to date.

Using the Gemini North telescope in Hawai`i, an international team of astronomers from Brazil, Italy, the Netherlands, and the UK has discovered the most distant radio galaxy to date, at 12.5 billion light years, when the Universe was just 7% of its current age.

The team used spectroscopic data from the Gemini Multi-Object Spectrograph (GMOS-N) to measure a redshift of z = 5.72 for the radio galaxy identified as TGSS J1530+1049. This is the largest redshift of any known radio galaxy. The redshift of a galaxy tells astronomers its distance because galaxies at greater distances move away from us at higher speeds, and this motion causes the galaxy's light to shift farther into the red. Because light has a finite speed and takes time to reach us, more distant galaxies are also seen at earlier times in the history of the Universe.

The study was led by graduate students Aayush Saxena (Leiden Observatory, Netherlands) and Murilo Marinello (Observatório Nacional, Brazil), and the observations were obtained through Brazil's participation in Gemini. "In the Gemini spectrum of TGSS J1530+1049, we found a single emission line of hydrogen, known as the Lyman alpha. The observed shift of this line allowed us to estimate the galaxy's distance," explains Marinello.

The relatively small size of the radio emission region in TGSS J1530+1049 indicates that it is quite young, as expected at such early times. Thus, the galaxy is still in the process of assembling. The radio emission in this kind of galaxy is powered by a supermassive black hole that is sucking in material from the surrounding environment. This discovery of the most distant radio galaxy confirms that black holes can grow to enormous masses very quickly in the early Universe.

The measured redshift of TGSS J1530+1049 places it near the end of the Epoch of Reionization, when the majority of the neutral hydrogen in the Universe was ionized by high-energy photons from young stars and other sources of radiation. "The Epoch of Reionization is very important in cosmology, but it is still not well understood," said Roderik Overzier, also of Brazil's Observatorio Nacional, and the Principal Investigator of the Gemini program. "Distant radio galaxies can be used as tools to find out more about this period."

The research has been published by Monthly Notices of the Royal Astronomical Society. A preprint of the paper is available at astro-ph.



Friday, June 15, 2018

Surprise discovery provides new insights into stellar deaths

Artist conception of a tidal disruption event (TDE) that happens when a star passes fatally close to a supermassive black hole, which reacts by launching a relativistic jet. Image credit: Sophia Dagnello, NRAO/AUI/NSF.  Hi-res image

Astronomers, working on a project to detect supernovas, made a surprise discovery when they found that one supernova explosion was actually a star being pulled apart by a supermassive black hole. ASTRON's Westerbork Synthesis Radio Telescope was involved in the observations.

This rare stellar death, known as a tidal disruption event, or TDE, occurs when the powerful gravity of a supermassive black hole rips apart a star that has wandered too close to the massive monster. 

Theorists have suggested that material pulled from the doomed star forms a rotating disk around the black hole, emitting intense X-rays and visible light, and launches jets of material outward from the poles of the disk close to the speed of light. 

"Never before have we been able to directly observe the formation and evolution of a jet from one of these events," said Miguel Perez-Torres, of the Astrophysical Institute of Andalucia in Granada, Spain. 

Originally, the researchers were monitoring a pair of colliding galaxies known as Arp 299, nearly 150 million light-years from Earth. This area of space is so rich in supernova explosions it has been dubbed the “supernova factory”. However, in January 2005 the researchers discovered a bright burst of infrared emission coming from the nucleus of one of these galaxies, and in July of the same year a new, distinct source of radio emission was witnessed from the same location. 

"As time passed, the new object stayed bright at infrared and radio wavelengths, but not in visible light and X-rays," said Seppo Mattila, of the University of Turku in Finland. "The most likely explanation is that thick interstellar gas and dust near the galaxy's centre absorbed the X-rays and visible light, then re-radiated it as infrared," he added. The researchers used the Nordic Optical Telescope on the Canary Islands and NASA's Spitzer space telescope to follow the object's infrared emission. 

Over the course of the next decade, the team continued to observe the radio emission using a technique known as Very Long Baseline Interferometry (VLBI). VLBI involves the remote coordination of multiple telescopes across the globe to focus on a single radio source at a given time. 

This technique provides extremely high resolution imaging when studying a radio source in space, providing the researchers with detailed data on the TDE. Telescopes in the European VLBI Network (EVN) and the Very Long Baseline Array (VLBA) were used for the observations, while the data collected was correlated at the Joint Institute for VLBI ERIC (JIVE), the Netherlands, and the Very Large Array (VLA), USA, respectively. 

This extensive monitoring revealed in 2011 that the radio-emitting portion was expanding in one direction, forming an elongation called a jet, as previously predicted by theorists. The measured expansion indicated that the material in the jet moved at an average of one-fourth the speed of light.

Most galaxies have supermassive black holes at their cores with masses that are millions to billions of times greater than the Sun. This mass is so concentrated that the resulting gravitational pull does not even allow light to escape. In this instance, the black hole is actively drawing material from its surroundings and ripping apart a star that is twice the Sun’s mass. This material forms a rotating disk around the black hole, and superfast jets of particles are launched outward – a phenomenon seen in radio galaxies and quasars. 

"Much of the time, however, supermassive black holes are not actively devouring anything, so they are in a quiet state," Perez-Torres explained. "Tidal disruption events can provide us with a unique opportunity to advance our understanding of the formation and evolution of jets in the vicinities of these powerful objects," he added. 

"Because of the dust that absorbed any visible light, this particular tidal disruption event may be just the tip of the iceberg of what until now has been a hidden population," Mattila said. "By looking for these events with infrared and radio telescopes, we may be able to discover many more, and learn from them," he said. 

Such events may have been more common in the distant Universe, so studying them could help scientists to better understand the environment in which galaxies developed billions of years ago.

Mattila and Perez-Torres led a team of 36 scientists from 26 institutions around the world in the observations of Arp 299. Their findings are published in the journal Science, which can be accessed here: http://science.sciencemag.org/lookup/doi/10.1126/science.aao4669

More information: 

The European VLBI Network (EVN) is a network of radio telescopes located primarily in Europe and Asia, with additional antennas in South Africa and Puerto Rico, which performs very high angular resolution observations of cosmic radio sources. 

Collectively the EVN forms the most sensitive radio telescope array at both centimetre wavelengths and millarcsecond resolution. The data collected at each of the individual stations is collated centrally at the correlator – a data processor housed at the Joint Institute for VLBI ERIC (JIVE) in Dwingeloo, the Netherlands.
 
The following EVN antennas observed at one or more epochs: Kunming, Seshan, Urumqi (China), Effelsberg, Wettzell (Germany), Medicina, Noto (Italy), Irbene (Latvia), Torun (Poland), Badary, Svetloe, Zelenchukskaya (Russia), Robledo, Yebes (Spain), Onsala (Sweden), Westerbork (The Netherlands), Cambridge and Jodrell Bank (The United Kingdom). 

Article: Mattila, S., Pérez-Torres, M., et al. 2018. A dust enshrouded tidal disruption event with a resolved radio jet in a galaxy merger. Science. DOI: 10.1126/science.aao4669 




Monday, October 17, 2016

Discovering the Treasures in Chandra’s Archives

Each year, NASA’s Chandra X-ray Observatory helps celebrate American Archive Month by releasing a collection of images using X-ray data in its archive.

The Chandra Data Archive is a sophisticated digital system that ultimately contains all of the data obtained by the telescope since its launch into space in 1999. Chandra’s archive is a resource that makes these data available to the scientific community and the general public for years after they were originally obtained.

Each of these six new images also includes data from telescopes covering other parts of the electromagnetic spectrum, such as visible and infrared light. This collection of images represents just a small fraction of the treasures that reside in Chandra’s unique X-ray archive.
From left to right, starting on the top row, the objects are:

 Westerlund 2, 3C31, PSR J1509-5850, Abell 665, RX J0603.3+4214 and CTB 37A


Westerlund 2: A cluster of young stars – about one to two million years old – located about 20,000 light years from Earth.  Data in visible light from the Hubble Space Telescope (green and blue) reveal thick clouds where the stars are forming. High-energy radiation in the form of X-rays, however, can penetrate this cosmic haze, and are detected by Chandra (purple).

3C31: X-rays from the radio galaxy 3C31 (blue), located 240 million light years from Earth, allow astronomers to probe the density, temperature, and pressure of this galaxy, long known to be a powerful emitter of radio waves. The Chandra data also reveal a jet blasting away from one side of the central galaxy, which also is known as NGC 383.  Here, the Chandra X-ray image has been combined with Hubble’s visible light data (yellow).

PSR J1509-5850: Pulsars were first discovered in 1967 and today astronomers know of over a thousand such objects. The pulsar, PSR J1509-5850, located about 12,000 light years from Earth and appearing as the bright white spot in the center of this image, has generated a long tail of X-ray emission trailing behind it, as seen in the lower part of the image. This pulsar has also generated an outflow of particles in approximately the opposite direction. In this image, X-rays detected by Chandra (blue) and radio emission (pink) have been overlaid on a visible light image from the Digitized Sky Survey of the field of view.

Abell 665: Merging galaxy clusters can generate enormous shock waves, similar to cold fronts in weather on Earth. This system, known as Abell 665, has an extremely powerful shockwave, second only to the famous Bullet Cluster. Here, X-rays from Chandra (blue) show hot gas in the cluster. The bow wave shape of the shock is shown by the large white region near the center of the image. The Chandra image has been added to radio emission (purple) and visible light data from the Sloan Digital Sky Survey showing galaxies and stars (white).

RX J0603.3+4214: The phenomenon of pareidolia is when people see familiar shapes in images. This galaxy cluster has invoked the nickname of the “Toothbrush Cluster” because of its resemblance to the dental tool. In fact, the stem of the brush is due to radio waves (green) while the diffuse emission where the toothpaste would go is produced by X-rays observed by Chandra (purple). Visible light data from the Subaru telescope show galaxies and stars (white) and a map from gravitational lensing (blue) shows the concentration of the mass, which is mostly (about 80%) dark matter.

CTB 37A: Astronomers estimate that a supernova explosion should occur about every 50 years on average in the Milky Way galaxy. The object known as CTB 37A is a supernova remnant located in our Galaxy about 20,000 light years from Earth. This image shows that the debris field glowing in X-rays (blue) and radio waves (pink) may be expanding into a cooler cloud of gas and dust seen in infrared light (orange).

NASA's Marshall Space Flight Center in Huntsville, Alabama, manages the Chandra program for NASA's Science Mission Directorate in Washington. The Smithsonian Astrophysical Observatory in Cambridge, Massachusetts, controls Chandra's science and flight operations. 


Read More from NASA's Chandra X-ray Observatory.


For more Chandra images, multimedia and related materials, visit: http://www.nasa.gov/chandra


Molly Porter
Marshall Space Flight Center, Huntsville, Ala.
256-544-0034

molly.a.porter@nasa.gov

Megan Watzke
Chandra X-ray Center, Cambridge, Mass.
617-496-7998

mwatzke@cfa.harvard.edu

Editor: Lee Mohon

Sunday, June 28, 2015

Star Formation Near Supermassive Black Holes

The bright radio galaxy 3C219. The blue object at the center is its active nucleus powered by a supermassive black hole; red shows the extent of the radio emission. Infrared observations of a complete set of similar galaxies dating from about seven billion years ago find that although star formation is active in these objects, the nuclear activity dominates the luminosity. Credit: NRAO and Parijskij et al.


Most if not all galaxies are thought to host a supermassive black hole in their nuclei, a finding that is both one the most important and amazing in modern astronomy. A supermassive black hole grows by accreting mass, and while growing its feeding frenzy is not hidden from our view -- it generates large amounts of energy. 

During the evolutionary phase in which it is most active, the object is known as an active galactic nucleus (AGN). Although there is a difference of a factor of about one billion in physical size scales between the black hole’s accreting environment and its host galaxy, the two sizes are found to be closely correlated, suggesting that there is some kind of feedback between the growth of the black hole and that of its host galaxy. Understanding what the feedback mechanisms are, and how they affect the growth of the galaxy (in particular its star formation), are of paramount importance for our understanding galaxy formation and evolution. Both processes are thought to peak in activity when the universe was only a few billion years old. Neither is particularly well understood.

CfA astronomers Belinda Wilkes, Joanna Kuraszkiewicz, Steve Willner, Matt Ashby, and Giovanni Fazio, along with their colleagues, used the Herschel Space Telescope to study the infrared emission from sixty-four bright, radio and X-ray emitting galaxies with AGN nuclei, and which contain more than one hundred billion solar-masses of stars. Their set is a complete sample of objects of a well-defined class dating from about seven billion years ago, and includes some of the most powerful quasars known. All the objects have large bipolar jets that were driven into intergalactic space by the AGN. The scientists set out to determine how much of the luminosity in these powerful galaxies was due to the AGN and how much was due to star formation activity. The infrared is emitted by dust heated by these two processes, and details of the emission (its typical temperature for example) can help sort out the relative contributions of the two processes.

The astronomers conclude that the star formation rates in these monsters run into the hundreds of solar-masses per year, and therefore reject suggestions that the AGN outflows will quench the star formation in such galaxies. Whatever the details of the growth feedback mechanism, therefore, they do not suppress the star formation. Nevertheless, despite the active star formation underway, the majority of the luminosity is due to the AGN, even during periods when the star formation is most active. Their paper is also significant because it can explain the principal observational differences between the galaxies in this set simply by the orientation of their disk to our line-of-sight, with the large, double-lobed jet sources being seen edge on and the quasars being seen more face-on.

Reference(s):


"Star Formation in z > 1 3CR Host Galaxies as Seen by Herschel," Podigachoski, P.; Barthel, P. D.; Haas, M.; Leipski, C.; Wilkes, B.; Kuraszkiewicz, J.; Westhues, C.; Willner, S. P.; Ashby, M. L. N.; Chini, R.; Clements, D. L.; Fazio, G. G.; Labiano, A.; Lawrence, C.; Meisenheimer, K.; Peletier, R. F.; Siebenmorgen, R.; Verdoes Kleijn, G., A&A, 575, 80, 2015.


Monday, June 08, 2015

The Ages of Extragalactic Jets

The bright radio galaxy NGC 4261 as seen in visible light (white) and radio (orange), showing a pair of opposed jets emanating from the nucleus. Astronomers have determined that the lobes are about thirty million years old, and were produced from multiple outbursts from around the nuclear black hole. Credit: Wide-Field and Planetary Camera of the Hubble Space Telescope, and National Radio Astronomy Observatory


The longest known highly collimated structures in the universe are the narrow jets that emanate from the vicinity of powerful black holes in certain types of galactic nuclei. These narrow beams, often in pairs propagating in opposite directions, can stretch across millions of light-years. They transport huge amounts of energy from the nuclear black hole regions where they originate into intergalactic space. The jets were discovered at radio wavelengths but they emit at X-ray wavelengths as well because the electrons in the jets move at close to the speed of light. These galaxies are active areas of research both because they are among the most energetic phenomena in the universe and because they are the primary mechanism that injects energy into the clusters of galaxies in which these radio monsters reside.

The development of these jets, their ages, and their ultimate dispositions are only vaguely understood. Astronomers suspect their lives have three phases, starting with the supersonic inflation of lobes of hot gas around the particle jets. It appears that in most sources this first phase is brief. Afterwards, the lobes expand gradually until their internal temperatures and pressures drop down to the values of the ambient gas. In the final phase, the jet ejection mechanisms shut down and the associated lobes become unobservable. There are numerous examples of galaxies at these various stages that provide the basis for these notions.

CfA astronomers Ewan O’Sullivan, Diana Worrall, and Mark Birkinshaw, together with four colleagues, examined the jets in the powerful radio galaxy 3C270 (also known as NGC 4261). This source has its brightest radio emission knots closest to the black hole nucleus (the other common type of radio jet galaxy has its brightest regions farthest away from the nucleus). The projected linear scale for the lobes in this source is about 250 thousand light-years at its maximum extent. The scientists used new and archival radio observations of the lobes, taken at twelve different wavelengths, combined with X-ray observations, to model the emission mechanisms throughout the lobes more precisely than previously done. The multi-wavelength data allow them to map how the character of the emission (i.e., its relative strength at different wavelengths) varies, and to model those variations. They conclude that the two lobes are respectively about twenty-nine and thirty-seven million years old, contrary to the conventional wisdom that they are about twice as old based on dynamical models. They also conclude that the lobes are the result of multiple outbursts of activity from the vicinity of black hole. The total energy needed to heat these lobes is stupendous, roughly equivalent to the Sun’s total power output over a million billion years, more than the age of the universe.

Reference(s):

"New Insights into the Evolution of the FR I Radio Galaxy 3C 270 (NGC 4261) from VLA and GMRT Radio Observations,” Kolokythas, Konstantinos, O'Sullivan, Ewan, Giacintucci, Simona, Raychaudhury, Somak, Ishwara-Chandra, C. H., Worrall, Diana M., Birkinshaw, Mark, MNRAS, 450, 1732, 2015.

Thursday, May 28, 2015

Merging galaxies break radio silence

Artist’s illustration of galaxy with jets from a supermassive black hole 


Galaxies with relativistic jets

Radio galaxy 3C 297

Radio galaxy 3C 454.1
 
Radio galaxy 3C 356 





Videos
 
Artist’s animation of galaxy with jets from a supermassive black hole
Artist’s animation of galaxy with jets from a supermassive black hole

Fulldome clip showing animation of galaxy with jets from a supermassive black hole
Fulldome clip showing animation of galaxy with jets from a supermassive black hole 






Large Hubble survey confirms link between mergers and supermassive black holes with relativistic jets

In the most extensive survey of its kind ever conducted, a team of scientists have found an unambiguous link between the presence of supermassive black holes that power high-speed, radio-signal-emitting jets and the merger history of their host galaxies. Almost all of the galaxies hosting these jets were found to be merging with another galaxy, or to have done so recently. The results lend significant weight to the case for jets being the result of merging black holes and will be presented in the Astrophysical Journal.

A team of astronomers using the NASA/ESA Hubble Space Telescope’s Wide Field Camera 3 (WFC3) have conducted a large survey to investigate the relationship between galaxies that have undergone mergers and the activity of the supermassive black holes at their cores.

The team studied a large selection of galaxies with extremely luminous centres — known as active galactic nuclei (AGNs) — thought to be the result of large quantities of heated matter circling around and being consumed by a supermassive black hole. Whilst most galaxies are thought to host a supermassive black hole, only a small percentage of them are this luminous and fewer still go one step further and form what are known as relativistic jets [1]. The two high-speed jets of plasma move almost with the speed of light and stream out in opposite directions at right angles to the disc of matter surrounding the black hole, extending thousands of light-years into space. The hot material within the jets is also the origin of radio waves.

It is these jets that Marco Chiaberge from the Space Telescope Science Institute, USA (also affiliated with Johns Hopkins University, USA and INAF-IRA, Italy) and his team hoped to confirm were the result of galactic mergers [2].

The team inspected five categories of galaxies for visible signs of recent or ongoing mergers — two types of galaxies with jets, two types of galaxies that had luminous cores but no jets, and a set of regular inactive galaxies [3].

“The galaxies that host these relativistic jets give out large amounts of radiation at radio wavelengths,” explains Marco. “By using Hubble’s WFC3 camera we found that almost all of the galaxies with large amounts of radio emission, implying the presence of jets, were associated with mergers. However, it was not only the galaxies containing jets that showed evidence of mergers!” [4].

“We found that most merger events in themselves do not actually result in the creation of AGNs with powerful radio emission,” added co-author Roberto Gilli from Osservatorio Astronomico di Bologna, Italy. “About 40% of the other galaxies we looked at had also experienced a merger and yet had failed to produce the spectacular radio emissions and jets of their counterparts.” 

Although it is now clear that a galactic merger is almost certainly necessary for a galaxy to host a supermassive black hole with relativistic jets, the team deduce that there must be additional conditions which need to be met. They speculate that the collision of one galaxy with another produces a supermassive black hole with jets when the central black hole is spinning faster — possibly as a result of meeting another black hole of a similar mass — as the excess energy extracted from the black hole’s rotation would power the jets.

“There are two ways in which mergers are likely to affect the central black hole. The first would be an increase in the amount of gas being driven towards the galaxy’s centre, adding mass to both the black hole and the disc of matter around it,” explains Colin Norman, co-author of the paper. “But this process should affect black holes in all merging galaxies, and yet not all merging galaxies with black holes end up with jets, so it is not enough to explain how these jets come about. The other possibility is that a merger between two massive galaxies causes two black holes of a similar mass to also merge. It could be that a particular breed of merger between two black holes produces a single spinning supermassive black hole, accounting for the production of jets.” 

Future observations using both Hubble and ESO’s Atacama Large Millimeter/submillimeter Array (ALMA) are needed to expand the survey set even further and continue to shed light on these complex and powerful processes.


Notes

[1] Relativistic jets travel at close to the speed of light, making them one of the fastest astronomical objects known.

[2] The new observations used in this research were taken in collaboration with the 3CR-HST team. This international team of astronomers is currently led by Marco Chiaberge and has conducted a series of surveys of radio galaxies and quasars from the 3CR catalogue using the Hubble Space Telescope.

[3] The team compared their observations with the swathes of archival data from Hubble. They directly surveyed twelve very distant radio galaxies and compared the results with data from a large number of galaxies observed during other observing programmes.

[4] Other studies had shown a strong relationship between the merger history of a galaxy and the high levels of radiation at radio wavelengths that suggests the presence of relativistic jets lurking at the galaxy’s centre. However, this survey is much more extensive, and the results very clear, meaning it can now be said with almost certainty that radio-loud AGNs, that is, galaxies with relativistic jets, are the result of galactic mergers.

Note for Editors

Image credit: NASA, ESA, M. Chiaberge (STScI)

Contacts

Marco Chiaberge
Space Telescope Science Institute, USA
Johns Hopkins University, USA, INAF-IRA, Italy
Tel: +1 410 338 4980
Email:
marcoc@stsci.edu

Roberto Gilli
INAF
Osservatorio Astronomico di Bologna, Italy
Tel: +39 051 2095 719
Cell: +39 347 4139847
Email:
roberto.gilli@oabo.inaf.it

Mathias Jäger
ESA/Hubble, Public Information Officer
Garching bei München, Germany
Cell: +49 176 62397500
Email:
mjaeger@partner.eso.org


Tuesday, September 10, 2013

Jets blow gas out of a galaxy

Optical image (blue) of the galaxy 4C12.50. The inset shows a zoom in of the plasma jet and the cold gas (orange). The gas is distributed in a compact cloud (dark orange) and filaments (light orange) as result of the strong impact with the plasma jet. Credit: optical: HST/STSci/Tadhunter et al.; radio: VLBI, Morganti et al. 2013. 

The jets which are shot away into space by the supermassive black hole in the centre of a galaxy, clear gas away from the galaxy. The first clear evidence of this was obtained by a team led by Raffaella Morganti (ASTRON, University of Groningen). The results will be published in Science on the 6th of September.
 
Astronomers have been puzzled by the fact that many galaxies in the Universe seem to be depleted of their gas and are therefore unable to form any new stars. Fast outflows of gas have been observed in the past, but the mechanism driving these outflows was not understood. The suspicion that the powerful plasma jets that are shot into space by the central supermassive black hole are responsible for the expulsion of the gas has now been confirmed.
 
The nucleus of the galaxy 4C12.50 was observed with ultra-high resolution using a global Very Long Baseline Interferometry (VLBI) network, an array of radio telescopes across different continents which form a telescope the size of the earth. The high-resolution images resulting from the VLBI observations allowed the team to pin down the location of the gas outflow and to determine the speed with which the gas leaves the galaxy.
 
Morganti: "We suspected the importance of these radio jets from previous studies using for example the Westerbork Synthesis Radio Telescope. With these observations at much higher resolution we were finally able to map the distribution of the gas. It could not have been in better agreement with our expectations!"
 
The astronomers found that the gas is flowing out of the galaxy at a velocity of 1000 kilometers per second. Despite the strong push received from the jet, the temperature of the gas is low. quot;This was quite unexpected", says coauthor Tom Oosterloo (ASTRON, University of Groningen). "But this is exactly what is needed to make theory of galaxy formation and observations to agree. It is in particular cold gas that is the fundamental building block of new stars, but this gas is being expelled by the jet".
 
Using a global array of radio telescopes we are able to peek into the nucleus of 4C12.50, located two billion light years from the earth. Zsolt Paragi, astronomer at JIVE and coauthor: "These observations, combining telescopes from both the European VLBI Network and the Very Long Baseline Array in the U.S., allowed us to trace gas at the immediate proximity - just 300 light years - of the black hole of 4C12.5."
 
The success of the observations means that VLBI is a suitable technique to study the effect of the super massive black hole on the gas in its vicinity. Morganti will use this technique to study more objects where gas outflows are suspected to exist in the project ‘Exploiting new radio telescopes to understand the role of AGN in galaxy evolution', for which Morganti received a ERC Advanced Grant last year.
 
***

More information:
 
About ASTRON
ASTRON is the Netherlands Institute for Radio Astronomy (www.astron.nl). Its mission is to make discoveries in radio astronomy happen, via the development of novel and innovative technologies, the operation of world-class radio astronomy facilities, and the pursuit of fundamental astronomical research.
 
About JIVE
The Joint Institute for VLBI in Europe (JIVE, www.jive.nl) is a scientific foundation with a mandate to support the operations of the European VLBI Network (EVN, www.evlbi.org). For this purpose it maintains, operates and develops the EVN data correlator, a powerful supercomputer that combines the signals from radio telescopes located across the planet.
 
Contact:
 
Prof. dr. Raffaella Morganti, ASTRON, RuG
E-mail:
morganti@astron.nl
Tel:      +31(0)521-595100
Mob:   +31 (0)6-11952523

 
Prof. dr. Tom A. Oosterloo, ASTRON, RUG
E-mail:
oosterloo@astron.nl
Tel:      +31(0)521-595779 
 
Dr. Zsolt Paragi
E-mail:
paragi@jive.nl
Tel: +31(0)521-596536
 
Article:
 
Radio Jets Clearing the Way Through a Galaxy: Watching Feedback in Action,  R. Morganti, J. Fogasy, Z. Paragi, T. Oosterloo, M. Orienti, Science, 6 September 201.

 

Thursday, November 29, 2012

A Multi-Wavelength View of Radio Galaxy Hercules A

 
Radio Galaxy Hercules A
Credit: NASA, ESA, S. Baum and C. O'Dea (RIT), R. Perley and W. Cotton (NRAO/AUI/NSF), and the Hubble Heritage Team (STScI/AURA) .    


 A 3-D Perspective on Hercules A
Credit: NASA, ESA, and Z. Levay, F. Summers, G. Bacon, T. Davis, and L. Frattare (Viz 3D Team/STScI)  .  See All the Videos

This video envisions a three-dimensional look at the combined visible light and radio emission from the active galaxy Hercules A. Unusually, this giant elliptical galaxy is not found in a large cluster of galaxies, but rather within a comparatively small group of galaxies. The supermassive black hole in its core, however, spews out strong jets of energetic particles that produce enormous lobes of radio emission. The size of these radio lobes dwarfs the large galaxy and extends throughout the volume of the galaxy group. This visualization is intended only to be a scientifically reasonable illustration of the three-dimensional structures. In particular, the galaxy distances are based on a statistical model, and not measured values.

Spectacular jets powered by the gravitational energy of a supermassive black hole in the core of the elliptical galaxy Hercules A illustrate the combined imaging power of two of astronomy's cutting-edge tools, the Hubble Space Telescope's Wide Field Camera 3, and the recently upgraded Karl G. Jansky Very Large Array (VLA) radio telescope in New Mexico.

Some two billion light-years away, the yellowish elliptical galaxy in the center of the image appears quite ordinary as seen by Hubble in visible wavelengths of light. The galaxy is roughly 1,000 times more massive than the Milky Way and harbors a 2.5-billion-solar-mass central black hole that is 1,000 times more massive than the black hole in the Milky Way. But the innocuous-looking galaxy, also known as 3C 348, has long been known as the brightest radio-emitting object in the constellation Hercules. Emitting nearly a billion times more power in radio wavelengths than our Sun, the galaxy is one of the brightest extragalactic radio sources in the entire sky.

The VLA radio data reveal enormous, optically invisible jets that, at one-and-a-half million light-years wide, dwarf the visible galaxy from which they emerge. The jets are very-high-energy plasma beams, subatomic particles and magnetic fields shot at nearly the speed of light from the vicinity of the black hole. The outer portions of both jets show unusual ring-like structures suggesting a history of multiple outbursts from the supermassive black hole at the center of the galaxy.

The innermost parts of the jets are not visible because of the extreme velocity of the material, which causes relativistic effects that beam the light away from us. Far from the galaxy, the jets become unstable and break up into the rings and wisps.

The entire radio source is surrounded by a very hot, X-ray-emitting cloud of gas, not seen in this optical-radio composite.
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Hubble's view of the field also shows a companion elliptical galaxy very close to the center of the optical-radio source, which may be merging with the central galaxy. Several other elliptical and spiral galaxies that are visible in the Hubble data may be members of a cluster of galaxies. Hercules A is by far the brightest and most massive galaxy in the cluster.

For more information, contact:

Ray Villard
Space Telescope Science Institute, Baltimore, Md.
410-338-4514
villard@stsci.edu

John Stoke
National Radio Astronomy Observatory, Charlottesville, Va.
434-244-6896
jstoke@nrao.edu

Dave Finley
National Radio Astronomy Observatory, Socorro, N.M.
575-835-7302
dfinley@nrao.edu

Friday, November 16, 2012

Galactic fireflies

 4C 73.08
A gigantic elliptical galaxy
Credit: ESA/Hubble & NASA

Luminous galaxies glow like fireflies on a dark night in this image snapped by the NASA/ESA Hubble Space Telescope. The central galaxy in this image is a gigantic elliptical galaxy designated 4C 73.08. A prominent spiral galaxy seen from "above" shines in the lower part of the image, while examples of galaxies viewed edge-on also populate the cosmic landscape.

In the optical and near-infrared light captured to make this image, 4C 73.08 does not appear all that beastly. But when viewed in longer wavelengths the galaxy takes on a very different appearance. Dust-piercing radio waves reveal plumes emanating from the core, where a supermassive black hole spews out twin jets of material. 4C 73.08 is classified as a radio galaxy as a result of this characteristic activity in the radio part of the electromagnetic spectrum.

Astronomers must study objects such as 4C 73.08 in multiple wavelengths in order to learn their true natures, just as seeing a firefly’s glow would tell a scientist only so much about the insect. Observing 4C 73.08 in visible light with Hubble illuminates galactic structure as well as the ages of constituent stars, and therefore the age of the galaxy itself. 4C 73.08 is decidedly redder than the prominent, bluer spiral galaxy in this image. The elliptical galaxy’s redness comes from the presence of many older, crimson stars, which shows that 4C 73.08 is older than its spiral neighbour.

The image was taken using Hubble’s Wide Field Camera 3 through two filters: one which captures green light, and one which captures red and near-infrared light.

Source: ESA/Hubble - Space Telescope

Friday, September 21, 2012

Discovery of an Ancient Celestial City Undergoing Rapid Growth: A Young Protocluster of Active Star-Forming Galaxies


Using the Multi-Object Infrared Camera and Spectrograph (MOIRCS) mounted on the Subaru Telescope, a team of astronomers led by Dr. Masao Hayashi (National Astronomical Observatory of Japan or NAOJ) and Dr. Tadayuki Kodama (Subaru Telescope, NAOJ) has discovered a protocluster of galaxies in the midst of a vigorous process of formation. It is the densest and most active protocluster ever identified at so great a distance, 11 billion light years away from Earth (Note 1). The star formation rate in the protocluster is intense, sometimes reaching a rate over 100 times greater than that of the Milky Way Galaxy. Although old, inactive elliptical galaxies dominate present-day galaxy clusters, the recently discovered protocluster is a site where progenitors of clusters of current elliptical galaxies were just forming and growing rapidly. It will serve as an ideal laboratory for investigating how a cluster develops and how a special, dense environment can influence the formation and evolution of galaxies. 

Research to Investigate the Formation of Protoclusters

The properties of galaxies strongly depend upon where they reside. Some galaxies occupy crowded, gravitationally bound regions called "galaxy clusters" and "galaxy groups" while others live in deserted areas called "general fields". In the present-day Universe, galaxy clusters generally contain old, elliptical galaxies that are not actively forming stars, and general fields usually encompass young disk galaxies that are actively forming stars. Why do these galaxies segregate into different habitats in the Universe? Investigation of the formation of distant protoclusters that are progenitors of local galaxy clusters may provide an answer. Clusters or "ancient cities" of galaxies are not everywhere. Discovering them in their "adolescence", when the surrounding environment influences their development, is likely to yield the best basis for studying how clusters of galaxies form. 

The current research team focused their search on star-forming galaxies associated with the protocluster USS1558-003 (Note 2), which is 11 billion light years way from Earth. This target is a very dense region of old, mature or "red-burning" galaxies (Note 3), and occurs in the epoch from 9 to 11 billion years ago when the adolescent galaxies were growing vigorously. The team used MOIRCS mounted on the Subaru Telescope for their research; they also fitted MOIRCS with a narrowband filter customized for this target to capture the H-alpha emission lines (Note 4) coming from the star-forming regions (Figure 1). In addition, they searched for extremely red galaxies that are inactive and passively evolving.





Figure 1: Two views of the protocluster. (Left) A near-infrared, false-color image of the region (clump 2) where galaxies in the protocluster most strongly cluster. The objects marked with open green circles are H-alpha emitting galaxies. North is up, and east is to the left. (Right) Blinking images of broadband (Ks) and narrowband (H-alpha) emitters. The encircled objects showing H-alpha emitting galaxies are much brighter in the narrowband than in the Ks-band. (Credit: NAOJ)


Results Showing an Ancient Celestial City Undergoing Rapid Growth

The wide-field observations revealed that three notable galaxy groups of various sizes (Figure 2) make up the protocluster. The number of galaxies concentrated in these clumps is very high, about 15 times greater than that of general fields in the Universe at the same cosmic time. No other region known so far in the ancient Universe of 11 billion years ago or more has so many strongly clustered galaxies. The intense star-forming activity in the entire observed region of the protocluster amounts to new star formation equivalent to 10,000 Suns per year. The activity is analogous to watching the swift construction of an ancient, developing city, when elliptical galaxies were very young and growing rapidly in a dense environment.



Figure 2: A wide-field map of an ancient celestial city, the USS1558-003 protocluster. The map shows the distances of the three clumps of galaxies from each other relative to the radio galaxy USS1558-003 located at (0,0). More specifically, the horizontal and vertical axes show relative distances in right ascensions and declinations in arcminute units with respect to the radio galaxy. North is up, and east is to the left. The black dots are all galaxies selected in this field. Magenta dots show old, passively evolving galaxies. Blue squares represent star-forming galaxies with H-alpha emission lines, while red ones show red-burning galaxies. Large gray circles show the three clumps of galaxies. (Credit: NAOJ)

Another important discovery about this protocluster is that almost all of the transitioning red-burning galaxies tend to be confined to the dense clumps. Their apparent preference for a location in the densest environment probably means that the protocluster is actually in its growth phase and having some environmental effects on the galaxies. The research team plans to examine the individual galaxies more closely in order to reveal what is actually happening as the cluster is forming.


Future Prospects from the MAHALO-Subaru Project

The results presented in this article are among the many exciting new findings that are just emerging from the "MAHALO-Subaru" project (Note 5), which focuses on identifying the fundamental physical processes that determine the properties of galaxies in dense environments. The project's research team, led by Dr. Kodama, is conducting systematic observations of a large sample of galaxy clusters and protoclusters at various distances, hence at various cosmic times. The results show that galaxy clusters observed at distances greater than 9 billion light years away generally have active star formation, even in their densest central regions, in contrast to present-day clusters in which old, inactive elliptical galaxies dominate. It appears that clusters grow from the inside out. They first grow rapidly in cores of protoclusters, and the sites of active growth of galaxies spread to the surrounding outskirts, like suburbs forming at the periphery of a city.

The research contributes to an understanding of how clusters and the galaxies within them form and grow with cosmic time. The research team sums it up: "We are now at the stage when we are using various new instruments to show in detail the internal structures of galaxies in formation so that we can identify the physical mechanisms that control and determine the properties of galaxies."

References:

These results are published in the September 20, 2012 edition of the Astrophysical Journal (Hayashi et al., 2012, ApJ, 757, 15).
 The authors of the paper are:
Masao Hayashi, National Astronomical Observatory of Japan (NAOJ), Japan
Tadayuki Kodama, Subaru Telescope, NAOJ, Hawaii
Ken-ichi Tadaki, University of Tokyo, Japan
Yusei Koyama, Durham University, United Kingdom
Ichi Tanaka, Subaru Telescope, NAOJ, Hawaii

Acknowledgements:

The authors thank Subaru Telescope for providing them with an opportunity to perform these exciting, important observations.

Support for this research was provided by The Japan Society for the Promotion of Science through Grant-in-Aid for Scientific Research 18684004 and 21340045.

Notes:
  1. At a redshift of 2.53, this is about 2.6 billion years since the Big Bang.
  2. The protocluster is located toward the constellation Serpens in the equatorial region of the sky and is associated with the radio galaxy USS1558-003 at (16:01:17.3 -00:28:48:00)
  3. A red-burning galaxy is a galaxy population in transition between actively forming stars in bursts and losing its star-forming activities. See the Subaru Telescope press release entitled "Red-Burning Galaxies Hold the Key to Galaxy Evolution"
  4. H-alpha is a characteristic spectral line originating from star-forming regions within the galaxy. More specifically, it is a nebular emission line of neutral hydrogen's Balmer series at rest-frame 6563 angstrom. An emission line is a type of spectral line that indicates the radiation received from an object and provides information about its temperature and composition. Hydrogen is one of the most abundant elements in the early Universe, and it creates an H-alpha spectral line when ionized hydrogen recombines with an electron (a particle with a negative electrical charge).
  5. MAHALO-Subaru: MApping H-Alpha and Lines of Oxygen with Subaru. Mahalo means "thank you" in the Hawaiian language.