From ESOblog (EU): “Ten years exploring the cold dark universe”

From ESOblog (EU)

At

European Southern Observatory [Observatoire européen austral][Europäische Südsternwarte] (EU) (CL)

Antennae Galaxies

On the Ground

8 October 2021

European Southern Observatory/National Radio Astronomy Observatory(US)/National Astronomical Observatory of Japan(JP) ALMA Observatory (CL)

Ten years ago this week, the Atacama Large Millimetre/submillimetre Array, also known as ALMA, officially opened to astronomers for “early science”. The occasion was marked with the publication of its first images, revealing the swirling gas in the colliding Antennae Galaxies. Since then, ALMA has detected complex molecules, discovered discs where planets are forming, and has even helped give us the first glimpse of a black hole. To find out more about how this ambitious project came to be, we spoke to Richard Hills, ALMA Project Scientist; Itziar de Gregorio-Monsalvo, ESO Staff Astronomer when ALMA started operating and now Head of the Office for Science in Chile; and Paola Andreani, Head of the European ALMA Regional Centre at that time and now Head of the Office for Science in Garching.

At 5000 metres above sea level, high in the Chilean Andes, the Chajnantor plateau is one of the loneliest places on Earth. It is, however, home to ALMA, a giant array of 66 antennas spread over 16km, turning their great white heads in graceful unison to look deep into the distant Universe.

“What we can see with ALMA is the cold Universe, regions dark to our eyes but that shine bright at millimetre/submillimetre wavelengths,” explains de Gregorio-Monsalvo. “With ALMA we can mainly see cold dust and gas coming from different regions of the Universe, from very distant galaxies to nearby objects, revealing with unprecedented detail how galaxies, stars and planets form and evolve, and the building blocks of life.”

This panoramic view of the Chajnantor Plateau shows the site of the Atacama Large Millimeter/submillimeter Array (ALMA), taken from near the peak of Cerro Chico. Babak Tafreshi, an ESO Photo Ambassador, has succeeded in capturing the feeling of solitude experienced at the ALMA site, 5000 metres above sea level in the Chilean Andes. Light and shadow paint the landscape, enhancing the otherworldly appearance of the terrain. In the foreground of the image, clustered ALMA antennas look like a crowd of strange, robotic visitors to the plateau. When the telescope is completed in 2013, there will be a total of 66 such antennas in the array, operating together.

ALMA is already revolutionising how astronomers study the Universe at millimetre and submillimetre wavelengths. Even with a partial array of antennas, ALMA is more powerful than any previous telescope at these wavelengths, giving astronomers an unprecedented capability to study the cool Universe — molecular gas and dust as well as the relic radiation of the Big Bang. ALMA studies the building blocks of stars, planetary systems, galaxies, and life itself. By providing scientists with detailed images of stars and planets being born in gas clouds near the Solar System, and detecting distant galaxies forming at the edge of the observable Universe, which we see as they were roughly ten billion years ago, it will let astronomers address some of the deepest questions of our cosmic origins.

ALMA, an international astronomy facility, is a partnership of Europe, North America and East Asia in cooperation with the Republic of Chile. ALMA construction and operations are led on behalf of Europe by European Southern Observatory [Observatoire européen austral][Europäische Südsternwarte](EU)(CL), on behalf of North America by the National Radio Astronomy Observatory (NRAO), and on behalf of East Asia by the National Astronomical Observatory of Japan (NAOJ). The Joint ALMA Observatory (JAO) provides the unified leadership and management of the construction, commissioning and operation of ALMA.

As a project, ALMA is unprecedented both in scale and in its pioneering example of international collaboration in astronomy. Despite the isolation of its surroundings, it was the coming together of different cultures and organisations that made its conception possible. But it wasn’t always going to be that way…

“The ALMA project was a dream that various astronomers across the world began to form back in the 1990s”, explains Hills. “A lot of people working in the field [of millimetre-wavelength astronomy] realised that they needed a much bigger telescope and, in particular, a telescope that used lots of relatively large antennas spread over a really large region.”

Such a telescope is called an interferometer, which works by combining the light from each of its antennas to discern much finer details than would be possible with an individual antenna. The technique is notoriously challenging — “Interferometry is a very tricky beast!” confirms Andreani.

Initially, three separate groups in Europe, Japan and the USA developed plans for such a telescope. But it soon became apparent that the best way to realise this dream would be to merge these projects, creating one large facility instead of three separate ones. The three major astronomical institutes that agreed to undertake this ambitious project were ESO in Europe, the National Radio Astronomy Observatory (NRAO) in the USA, and the National Astronomical Observatory of Japan (NAOJ) in East Asia. The three partners also shared the construction of the antennas, with slightly different designs but ultimately the same specifications. ESO and NRAO would provide 25 12-m antennas each, and NAOJ would contribute 4 12-m antennas and 12 7-m ones.

Once the partners had come together and the plans for the three projects were developed into a single telescope design, ALMA started to come to life in 2001, with plans for a 10-year construction period. Working as a Project Scientist, Hills was able to experience first hand some of the challenges and triumphs of this process. “I think the original plan back in 2000 was that we would be ready for this so-called early science period, in 2007, and by 2007 we hadn’t even got the first antenna!” he says.

Fortunately after a slow start, ALMA’s construction quickly picked up pace. “There was no time to be bored!” says de Gregorio-Monsalvo. “There were so many things to develop and test to make ALMA possible that the first light seemed really far-off. But thanks to the effort of a great team the goal was achieved.”

Assembly of the first European antenna.
Credit: S. Rossi/ESO/ALMA.

A European Atacama Large Millimeter/submillimeter Array (ALMA) antenna takes a ride on Lore, one of the ALMA Transporters, at the 2900-metre altitude Operations Support Facility in the Chilean Andes. This took place on 23 June 2010, and was the first time that European antennas have been lifted with the transporters, a procedure that was fully successful, with both moves completed in a single day.

The first two European antennas for ALMA have been moved to two new outdoor foundation pads in order to perform tests of their dish surface accuracy. In this process, known as holography, the antennas observe the signals from a special transmitter located on a nearby tower. In order to allow parallel assembly of several antennas, two new foundations have recently been built. As the newly built foundations lie between the original positions of the two antennas and the holography tower, the antennas were moved to the new locations.

In September 2011, ALMA opened for its “early science” period, with astronomers from across the globe able to use the new telescope for the first time. At this time only 16 of the eventual 66 antennas were available to use. Even then, ALMA was still bigger in scale than any previous interferometer and the excitement among the astronomical community was palpable. To observe with ALMA –– or any other telescope –– astronomers must submit proposals that are evaluated by a panel of experts; only a few will be successful. For this first observation period, ALMA received over 900 proposals, but only around 100 were selected!

Data from the first “early science” observing night arriving at the consoles in the control room.
Credit: I. de Gregorio-Monsalvo.

“The thing that was amazing was that as soon as all the equipment came together, everything worked more or less out of the box,” remembers Hills. “The first images came out and the scientific results started to flow. The results were fantastic –– well beyond our expectations in many cases.”

“It was amazing in terms of human relation and amazing in terms of scientific discovery.” agrees Adreani.

De Gregorio-Monsalvo also remembers how she felt at ALMA first light: “It was very rewarding for me and I felt very proud of myself and of my ALMA colleagues. When I saw the first light I thought that all the invested effort and all the sleepless nights had been worth it.”

During the construction of ALMA in Chile, other challenges were being tackled behind the scenes as the ALMA partners worked to define how the observatory would be operated. Three ALMA Regional Centres (ARCs) were created to interact with astronomers worldwide. “It was the first time that a big international facility built this kind of user support mode which was spread around,” says Andreani. “The main difficulty really was to communicate, and to convince people that we are always working towards the same goal — we all wanted to make this facility work and be successful. We built the entire operation. The first years were pretty intensive. We set up all the procedures, we agreed on all the policies, we wrote all the documents which are now available both for public and for internal purposes,” she says.

Ultimately the leap into the unknown regarding the organisation of ALMA paid off and Adreani felt the ARCs were especially successful. “I see that still the people supporting the users are doing a wonderful job, they are offering more and more help. I think it’s now a model which many other facilities are copying.”

Now, a decade after it opened for early science, ALMA has been at the forefront of many discoveries. “My favourite scientific discovery made by ALMA was the image of the dust disc surrounding the young star HL Tau, revealing the planetary genesis,” says de Gregorio-Monsalvo. “I still remember the awed silence of the team after we saw that image for the first time!” Hills agrees: “When that first came out it just blew our minds.”

ALMA image of the protoplanetary disc around HL Tauri.

This is the sharpest image ever taken by ALMA — sharper than is routinely achieved in visible light with the NASA/ESA Hubble Space Telescope. It shows the protoplanetary disc surrounding the young star HL Tauri. These new ALMA observations reveal substructures within the disc that have never been seen before and even show the possible positions of planets forming in the dark patches within the system. Credit: ALMA (ESO/NAOJ/NRAO).

Messier 87*, The first image of the event horizon of a black hole. This is the supermassive black hole at the center of the galaxy Messier 87. Image via The Event Horizon Telescope Collaboration released on 10 April 2019 via National Science Foundation(US).

Another scientific highlight with ALMA is the role it played in the Event Horizon Telescope Collaboration to deliver the first image of a black hole, the supermassive black hole at the heart of the M87 galaxy. This was an impressive feat, as it required combining data gathered by several radio telescopes all over the world, functioning as a single planet-sized facility. “When we built the telescope we knew the science specifications that needed to be reached, but we were not prepared to see transformational science in just one single image,” says de Gregorio-Monsalvo.

“Indeed it is delivering very astonishing results in all astronomical fields,” adds Andreani.

In addition to its scientific achievements, all the scientists agree that ALMA has been a triumph of cooperation on a global scale. “It holds up as an example of international collaboration paying off. It certainly couldn’t have been done in its successful form by a single one of the partners,” says Hills.

See the full article here .

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European Southern Observatory [Observatoire européen austral][Europäische Südsternwarte] (EU) is the foremost intergovernmental astronomy organisation in Europe and the world’s most productive ground-based astronomical observatory by far. It is supported by 16 countries: Austria, Belgium, Brazil, the Czech Republic, Denmark, France, Finland, Germany, Italy, the Netherlands, Poland, Portugal, Spain, Sweden, Switzerland and the United Kingdom, along with the host state of Chile. ESO carries out an ambitious programme focused on the design, construction and operation of powerful ground-based observing facilities enabling astronomers to make important scientific discoveries. ESO also plays a leading role in promoting and organising cooperation in astronomical research. ESO operates three unique world-class observing sites in Chile: La Silla, Paranal and Chajnantor. At Paranal, ESO operates the Very Large Telescope, the world’s most advanced visible-light astronomical observatory and two survey telescopes. VISTA works in the infrared and is the world’s largest survey telescope and the VLT Survey Telescope is the largest telescope designed to exclusively survey the skies in visible light. ESO is a major partner in ALMA, the largest astronomical project in existence. And on Cerro Armazones, close to Paranal, ESO is building the 39-metre European Extremely Large Telescope, the E-ELT, which will become “the world’s biggest eye on the sky”.

European Southern Observatory [Observatoire européen austral][Europäische Südsternwarte] (EU) is the foremost intergovernmental astronomy organisation in Europe and the world’s most productive ground-based astronomical observatory by far. It is supported by 16 countries: Austria, Belgium, Brazil, the Czech Republic, Denmark, France, Finland, Germany, Italy, the Netherlands, Poland, Portugal, Spain, Sweden, Switzerland and the United Kingdom, along with the host state of Chile. ESO carries out an ambitious programme focused on the design,

European Southern Observatory(EU) La Silla HELIOS (HARPS Experiment for Light Integrated Over the Sun)

ESO 3.6m telescope & HARPS atCerro LaSilla, Chile, 600 km north of Santiago de Chile at an altitude of 2400 metres.

MPG Institute for Astronomy [Max-Planck-Institut für Astronomie](DE) 2.2 meter telescope at/European Southern Observatory(EU) Cerro La Silla, Chile, 600 km north of Santiago de Chile at an altitude of 2400 metres.

European Southern Observatory(EU)La Silla Observatory 600 km north of Santiago de Chile at an altitude of 2400 metres.

European Southern Observatory(EU) , Very Large Telescope at Cerro Paranal in the Atacama Desert •ANTU (UT1; The Sun ) •KUEYEN (UT2; The Moon ) •MELIPAL (UT3; The Southern Cross ), and •YEPUN (UT4; Venus – as evening star). Elevation 2,635 m (8,645 ft) from above Credit J.L. Dauvergne & G. Hüdepohl atacama photo.

European Southern Observatory(EU)VLTI Interferometer image, Cerro Paranal, with an elevation of 2,635 metres (8,645 ft) above sea level, •ANTU (UT1; The Sun ),
•KUEYEN (UT2; The Moon ),
•MELIPAL (UT3; The Southern Cross ), and
•YEPUN (UT4; Venus – as evening

ESO Very Large Telescope 4 lasers on Yepun (CL)

Glistening against the awesome backdrop of the night sky above ESO’s Paranal Observatory, four laser beams project out into the darkness from Unit Telescope 4 UT4 of the VLT, a major asset of the Adaptive Optics system.

ESO/NTT NTT at Cerro La Silla , Chile, at an altitude of 2400 metres.

Part of ESO’s Paranal Observatory, the VLT Survey Telescope (VISTA) observes the brilliantly clear skies above the Atacama Desert of Chile. It is the largest survey telescope in the world in visible light, with an elevation of 2,635 metres (8,645 ft) above sea level.

European Southern Observatory/National Radio Astronomy Observatory(US)/National Astronomical Observatory of Japan(JP) ALMA Array in Chile in the Atacama at Chajnantor plateau, at 5,000 metres.

European Southern Observatory(EU) ELT 39 meter telescope to be on top of Cerro Armazones in the Atacama Desert of northern Chile. located at the summit of the mountain at an altitude of 3,060 metres (10,040 ft).

European Southern Observatory(EU)/MPG Institute for Radio Astronomy [MPG Institut für Radioastronomie](DE) ESO’s Atacama Pathfinder Experiment(CL) high on the Chajnantor plateau in Chile’s Atacama region, at an altitude of over 4,800 m (15,700 ft).

Leiden MASCARA instrument cabinet at Cerro La Silla, located in the southern Atacama Desert 600 kilometres (370 mi) north of Santiago de Chile at an altitude of 2,400 metres (7,900 ft).

ESO Next Generation Transit Survey telescopes, an array of twelve robotic 20-centimetre telescopes at Cerro Paranal,(CL) 2,635 metres (8,645 ft) above sea level.

TAROT telescope at Cerro LaSilla, 2,635 metres (8,645 ft) above sea level.

European Southern Observatory(EU) ExTrA telescopes at erro LaSilla at an altitude of 2400 metres.

A novel gamma ray telescope under construction on Mount Hopkins, Arizona. A large project known as the Čerenkov Telescope Array composed of hundreds of similar telescopes to be situated in the Canary Islands and Chile at, ESO Cerro Paranal site The telescope on Mount Hopkins will be fitted with a prototype high-speed camera, assembled at the. University of Wisconsin–Madison and capable of taking pictures at a billion frames per second. Credit: Vladimir Vassiliev.

European Space Agency [Agence spatiale européenne][Europäische Weltraumorganisation](EU), The new Test-Bed Telescope 2is housed inside the shiny white dome shown in this picture, at ESO’s LaSilla Facility in Chile. The telescope has now started operations and will assist its northern-hemisphere twin in protecting us from potentially hazardous, near-Earth objects.The domes of ESO’s 0.5 m and the Danish 0.5 m telescopes are visible in the background of this image.Part of the world-wide effort to scan and identify near-Earth objects, the European Space Agency’s Test-Bed Telescope 2 (TBT2), a technology demonstrator hosted at ESO’s La Silla Observatory in Chile, has now started operating. Working alongside its northern-hemisphere partner telescope, TBT2 will keep a close eye on the sky for asteroids that could pose a risk to Earth, testing hardware and software for a future telescope network.

European Space Agency [Agence spatiale européenne][Europäische Weltraumorganisation](EU) The open dome of The black telescope structure of the‘s Test-Bed Telescope 2 peers out of its open dome in front of the rolling desert landscape. The telescope is located at ESO’s La Silla Observatory, which sits at a 2400 metre altitude in the Chilean Atacama desert.

From The New York Times : “This May Be the First Planet Found Orbiting 3 Stars at Once”

From The New York Times

Sept. 28, 2021
Jonathan O’Callaghan

An artist’s animation of the three stars’ movement at the center of GW Orionis, based on a computer model using observations made by the European Southern Observatory’s Very Large Telescope. Credit: L. Calçada/European Southern Observatory [Observatoire européen austral][Europäische Südsternwarte](EU)(CL)/Kraus et al./The University of Exeter (UK).

GW Ori is a star system 1300 light years from Earth in the constellation of Orion. It is surrounded by a huge disk of dust and gas, a common feature of young star systems that are forming planets. But fascinatingly, it is a system with not one star, but three.

As if that were not intriguing enough, GW Ori’s disk is split in two, almost like Saturn’s rings if they had a massive gap in between. And to make it even more bizarre, the outer ring is tilted at about 38 degrees.

Scientists have been trying to explain what is going on there [https://sciencesprings.wordpress.com/2020/09/03/from-european-southern-observatory-new-observations-show-planet-forming-disc-torn-apart-by-its-three-central-stars/]. Some hypothesized that the gap in the disk could be the result of one or more planets [The Astrophysical Journal Letters] forming in the system. If so, this would be the first known planet that orbits three stars at once, also known as a circumtriple planet.

Now the GW Ori system has been modeled in greater detail [MNRAS], and researchers say a planet — a gassy world as massive as Jupiter — is the best explanation for the gap in the dust cloud. Although the planet itself cannot be seen, astronomers may be witnessing it carve out its orbit in its first million years of its existence.

A paper on the finding was published in September in the Monthly Notices of the Royal Astronomical Society [above]. The scientists say it disproves an alternative explanation — that the gravitational torque of the stars cleared the space in the disk. Their paper suggests there is not enough turbulence in the disk, known as its viscosity, for this explanation to suffice.

The finding also highlights how much more there is to learn about the unexpected ways in which planets can form.

An image made by the ALMA telescope, left, shows the GW Ori disc’s ringed structure, with the innermost ring separated from the rest of the disc. The SPHERE observations, right, show the shadow of this innermost ring on the rest of the disc. Credit: L. Calçada/European Southern Observatory [Observatoire européen austral][Europäische Südsternwarte](EU)(CL)/Kraus et al./The University of Exeter (UK)

European Southern Observatory/National Radio Astronomy Observatory(US)/National Astronomical Observatory of Japan(JP) ALMA Observatory (CL)

European Southern Observatory(EU) SPHERE extreme adaptive optics system and coronagraphic facility on the VLT UT3, Cerro Paranal, Chile, with an elevation of 2,635 metres (8,645 ft) above sea level.

European Southern Observatory(EU) , Very Large Telescope at Cerro Paranal in the Atacama Desert •ANTU (UT1; The Sun ) •KUEYEN (UT2; The Moon ) •MELIPAL (UT3; The Southern Cross ), and •YEPUN (UT4; Venus – as evening star). Elevation 2,635 m (8,645 ft) from above Credit J.L. Dauvergne & G. Hüdepohl atacama photo.

Anyone who has watched George Lucas’ original Star Wars is familiar with planets that can have two stars rising and falling in its skies. Luke Skywalker’s dusty home of Tatooine was in such a binary star system. But a planet orbiting three stars would be more unusual.

If a familiar life form could dwell on a gas giant like the one that would be orbiting GW Ori, it would not actually be able to see the three stars in its skies. Rather, they would see only a pair as the two innermost stars orbit so close as to appear like a single point of light. Yet as the planet rotated, its stars would rise and fall in fascinating sunrises and sunsets unlike any other known world.

“Star Wars missed a trick,” said Rebecca Nealon from The University of Warwick (UK), a co-author on the paper.

Scientists have been on the lookout for a planet orbiting three stars, and found potential evidence in another system, GG Tau A [Nature], located about 450 light years from Earth. But the researchers say the gap in GW Ori’s gas and dust ring makes it a more convincing example.

“It may be the first evidence of a circumtriple planet carving a gap in real time,” said Jeremy Smallwood from the University of Nevada, Las Vegas, lead author of the new paper.

William Welsh, an astronomer at San Diego State University, said the researchers “make a good case. If this turns out to be a planet, it would be fascinating.”

Alison Young from the University of Leicester in England who has argued that GW Ori’s stars caused the gap in the system’s disk, rather than a planet, notes that observations from the ALMA telescope and Very Large Telescope in Chile in the coming months could end the debate.

“We’ll be able to look for direct evidence of a planet in the disk,” Dr. Young said.
—
If the planet hypothesis is confirmed, the system would reinforce the idea that planet formation is common. Several worlds, known as circumbinary planets, are already known to orbit two stars at once. But circumtriple planets have been harder to come by — despite estimates that at least a tenth [ApJS] of all stars cluster in systems of three or more. Yet their possible existence suggests that planets spring up in all sorts of places, even here in this most bizarre of systems.

“Three stars is not enough to kill planet formation,” Dr. Nealon said.

That suggests that exoplanets are likely to arise in more and more unusual locations. “What we’ve learned is any time planets can form, they do,” said Sean Raymond, an astronomer from the University of Bordeaux in France who was not involved in the paper.

Perhaps even a world orbiting four, or five, or six stars at once?

“I don’t see why not,” he said.

See the full article here .

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From ALMA Observatory (CL) : “ALMA Discover Most Ancient Spiral Galaxy”

European Southern Observatory [Observatoire européen austral][Europäische Südsternwarte](EU)(CL)/National Radio Astronomy Observatory(US)/National Astronomical Observatory of Japan(JP)

From ALMA Observatory (CL)

20 May, 2021

Nicolás Lira
Education and Public Outreach Coordinator
Joint ALMA Observatory, Santiago – Chile
Phone: +56 2 2467 6519
Cell phone: +56 9 9445 7726
Email: nicolas.lira@alma.cl

Masaaki Hiramatsu
Education and Public Outreach Officer, NAOJ Chile
Observatory
, Tokyo – Japan
Phone: +81 422 34 3630
Email: hiramatsu.masaaki@nao.ac.jp

Bárbara Ferreira
ESO Public Information Officer
Garching bei München, Germany
Phone: +49 89 3200 6670
Email: pio@eso.org
Amy C. Oliver
Public Information & News Manager
National Radio Astronomical Observatory (NRAO), USA
Phone: +1 434 242 9584
Email: aoliver@nrao.edu

All general references:
ALMA Observatory (CL)
European Southern Observatory(EU)
National Astronomical Observatory of Japan(JP)
National Radio Astronomy Observatory(US)

ALMA image of the galaxy BRI 1335-0417 at 12.4 billion years ago. ALMA detected emissions from carbon ions in the galaxy. Spiral arms are visible on both sides of the compact, bright area in the galaxy center. Credit: T. Tsukui & S. Iguchi ALMA (ESO/NAOJ/NRAO)

Supercomputer simulation of spiral galaxy formation. Over about 13.5 billion years, small galaxies merge one after another into a single giant spiral galaxy. Please note that this video was created in 2007 and is not a reproduction of the current study. Credit: Takaaki Takeda, Sorahiko Nukatani, Takayuki Saito, 4D2U Project, NAOJ.

Analyzing data obtained with the Atacama Large Millimeter/submillimeter Array (ALMA), researchers found a galaxy with a spiral morphology in the Universe, only 1.4 billion years after the Big Bang. This is the most ancient galaxy of its kind ever observed. The discovery of a galaxy with a spiral structure at such an early stage is an essential clue to solve the classic questions of astronomy: “How and when did spiral galaxies form?”

“I was excited because I had never seen such clear evidence of a rotating disk, spiral structure, and centralized mass structure in a distant galaxy in any previous literature,” says Takafumi Tsukui, a graduate student at SOKENDAI-Graduate University for Advanced Studies [総合研究大学院大学] (JP) and the lead author of the research paper published in the journal Science. “The quality of the ALMA data was so good that I was able to see so much detail that I thought it was a nearby galaxy.”

The Milky Way Galaxy, where we live, is a spiral galaxy. Spiral galaxies are fundamental objects in the Universe, accounting for as much as 70% of the total number of galaxies. However, studies have shown that the proportion of spiral galaxies declines rapidly as we look back through the history of the Universe. So, when were the spiral galaxies formed?

Tsukui and his supervisor Satoru Iguchi, a professor at SOKENDAI and the National Astronomical Observatory of Japan, noticed a galaxy called BRI 1335-0417 in the ALMA Science Archive. The galaxy existed 12.4 billion years ago and contained a large amount of dust which obscures the starlight, making it difficult to study this galaxy in detail with visible light. On the other hand, ALMA can detect radio emissions from carbon ions in the galaxy, enabling astronomers to investigate what is going on in the galaxy.

The researchers found a spiral structure extending about 15,000 light-years from the center of the galaxy: one-third of the size of the Milky Way. The estimated total mass of stars and interstellar matter in BRI 1335-0417 is roughly identical to that of the Milky Way.

“As BRI 1335-0417 is a very distant object, we might not be able to see the true edge of the galaxy in this observation,” comments Tsukui. “For a galaxy that existed in the early Universe, BRI 1335-0417 was giant.”

Then the question becomes, how was this distinct spiral structure formed in only 1.4 billion years after the Big Bang? The researchers considered multiple possible causes and suggested that it could be due to an interaction with a small galaxy. BRI 1335-0417 is actively forming stars, and the researchers found that the gas in the outer part of the galaxy is gravitationally unstable, which is conducive to star formation. This situation is likely to occur when a large amount of gas is supplied from the outside, possibly due to collisions with smaller galaxies.

The fate of BRI 1335-0417 is also shrouded in mystery. Galaxies that contain large amounts of dust and actively produce stars in the ancient Universe are thought to be the ancestors of the giant elliptical galaxies in the present Universe. In that case, BRI 1335-0417 changes its shape from a disk galaxy to an elliptical one in the future. Or, contrary to the conventional view, the galaxy may remain a spiral galaxy for a long time. BRI 1335-0417 will play an essential role in studying the evolution of galaxy shape evolution over the long history of the Universe.

“Our Solar System lodges in one of the Milky Way spiral arms,” explains Iguchi. “Tracing the roots of spiral structure will provide us with clues as to the environment in which the Solar System was born. I hope that this research will further advance our understanding of the formation history of galaxies.”

Additional Information

These research results are presented in Science on Thursday, 20 May 2021.

See the full article here .

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The Atacama Large Millimeter/submillimeter Array (ALMA)(CL) , an international astronomy facility, is a partnership of Europe, North America and East Asia in cooperation with the Republic of Chile. ALMA is funded in Europe by the European Organization for Astronomical Research in the Southern Hemisphere (ESO), in North America by the U.S. National Science Foundation (NSF) in cooperation with the National Research Council of Canada (NRC) and the National Science Council of Taiwan (NSC) and in East Asia by the National Institutes of Natural Sciences (NINS) of Japan in cooperation with the Academia Sinica (AS) in Taiwan.

ALMA construction and operations are led on behalf of Europe by European Southern Observatory(EU), on behalf of North America by the National Radio Astronomy Observatory (NRAO), which is managed by Associated Universities, Inc. (US) and on behalf of East Asia by the National Astronomical Observatory of Japan (NAOJ). The Joint ALMA Observatory (JAO) provides the unified leadership and management of the construction, commissioning and operation of ALMA.

ALMA is a time machine!

ALMA-In Search of our Cosmic Origins

From ALMA Observatory (CL): “ALMA Unveils Galaxies at Cosmic Dawn That Were Hiding Behind the Dust”

European Southern Observatory [Observatoire européen austral][Europäische Südsternwarte](EU)(CL)/National Radio Astronomy Observatory(US)/National Astronomical Observatory of Japan(JP)

From ALMA Observatory (CL)

22 September, 2021

Nicolás Lira
Education and Public Outreach Coordinator
Joint ALMA Observatory, Santiago – Chile
Phone: +56 2 2467 6519
Cell phone: +56 9 9445 7726
Email: nicolas.lira@alma.cl

Masaaki Hiramatsu
Education and Public Outreach Officer, NAOJ Chile
Observatory
, Tokyo – Japan
Phone: +81 422 34 3630
Email: hiramatsu.masaaki@nao.ac.jp

Bárbara Ferreira
ESO Public Information Officer
Garching bei München, Germany
Phone: +49 89 3200 6670
Email: pio@eso.org
Amy C. Oliver
Public Information & News Manager
National Radio Astronomical Observatory (NRAO), USA
Phone: +1 434 242 9584
Email: aoliver@nrao.edu

All general references:
ALMA Observatory (CL)
European Southern Observatory(EU)
National Astronomical Observatory of Japan(JP)
National Radio Astronomy Observatory(US)

Distant galaxies imaged with ALMA, the Hubble Space Telescope, and the European Southern Observatory’s VISTA telescope.

National Aeronautics and Space Administration(US)/European Space Agency [Agence spatiale européenne] [Europäische Weltraumorganisation] (EU) Hubble Space Telescope

Part of ESO’s Paranal Observatory the VLT Survey Telescope (VISTA) observes the brilliantly clear skies above the Atacama Desert of Chile. It is the largest survey telescope in the world in visible light, with an elevation of 2,635 metres (8,645 ft) above sea level.

Green and orange colors represent radiations from ionized carbon atoms and dust particles, respectively, observed with ALMA, and blue represents near-infrared radiation observed with VISTA and Hubble Space Telescopes. REBELS-12 and REBELS-29 detected both near-infrared radiation and radiation from ionized carbon atoms and dust. On the other hand, REBELS-12-2 and REBELS-29-2 have not been detected in the near-infrared, which suggests that these galaxies are deeply buried in dust. Credit: ALMA (ESO/NAOJ/NRAO), NASA/ESA Hubble Space Telescope, ESO, Fudamoto et al.

A schematic of the results of this research. ALMA revealed a hitherto undiscovered galaxy as it is buried deep in dust (artist’s impression in upper right) in a region where the Hubble Space Telescope could not see anything (left). Researchers serendipitously discovered the new hidden galaxy while observing an already well-known typical young galaxy (artist’s impression in lower right) Credit: ALMA (ESO/NAOJ/NRAO), NASA/ESA Hubble Space Telescope.

While investigating the data of young, distant galaxies observed with the Atacama Large Millimeter/submillimeter Array (ALMA), Yoshinobu Fudamoto from Waseda University [早稲田大学](JP) and the National Astronomical Observatory of Japan noticed unexpected emissions coming from seemingly empty regions in space that, a global research team confirmed, came actually from two hitherto undiscovered galaxies heavily obscured by cosmic dust. This discovery suggests that numerous such galaxies might still be hidden in the early Universe, many more than researchers were expecting.

When astronomers peer deep into the night sky, they observe what the Universe looked like a long time ago. Because the speed of light is finite, studying the most distant observable galaxies allows us to glimpse billions of years into the past when the Universe was very young and galaxies had just started to form stars. Studying this “early Universe” is one of the last frontiers in Astronomy and is essential for constructing accurate and consistent astrophysics models. A key goal of scientists is to identify all the galaxies in the first billion years of cosmic history and to measure the rate at which galaxies were growing by forming new stars.

Various efforts have been made over the past decades to observe distant galaxies, which are characterized by electromagnetic emissions that become strongly redshifted (shifted towards longer wavelengths) before reaching the Earth. So far, our knowledge of early galaxies has mostly relied on observations with the Hubble Space Telescope (HST) and large ground-based telescopes, which probe their ultra-violet (UV) emission. However, recently, astronomers have started to use the unique capability of the Atacama Large Millimeter/submillimeter Array (ALMA) telescope to study distant galaxies at submillimeter wavelengths. This could be particularly useful for studying dusty galaxies missed in the HST surveys due to the dust absorbing UV emission. Since ALMA observes in submillimeter wavelengths, it can detect these galaxies by observing the dust emissions instead.

In an ongoing large program called REBELS (Reionization-Era Bright Emission Line Survey), astronomers are using ALMA to observe the emissions of 40 target galaxies at cosmic dawn. Using this dataset, they have recently discovered that the regions around some of these galaxies contain more than meets the eye.

While analyzing the observed data for two REBELS galaxies, Fudamoto noticed strong emission by dust and singly ionized carbon in positions substantially offset from the initial targets. To his surprise, even highly sensitive equipment like the HST couldn’t detect any UV emission from these locations. To understand these mysterious signals, Fudamoto and his colleagues investigated matters further.

In their latest paper published in Nature, astronomers presented a thorough analysis, revealing that these unexpected emissions came from two previously unknown galaxies located near the two original REBELS targets. These galaxies are not visible in the UV or visible wavelengths as they are almost completely obscured by cosmic dust. One of them represents the most distant dust-obscured galaxy discovered so far.

What is most surprising about this serendipitous finding is that the newly discovered galaxies, which formed more than 13 billion years ago, are not strange at all when compared with typical galaxies at the same epoch. “These new galaxies were missed not because they are extremely rare, but only because they are completely dust-obscured,” explains Fudamoto. However, it is uncommon to find such “dusty” galaxies in the early period of the Universe (less than 1 billion years after the Big Bang), suggesting that the current census of early galaxy formation is most likely incomplete, and would call for deeper, blind surveys. “It is possible that we have been missing up to one out of every five galaxies in the early Universe so far,” Fudamoto adds.

The researchers expect that the unprecedented capability of the James Webb Space Telescope (JWST) and its strong synergy with ALMA would lead to significant advances in this field in the coming years. “Completing our census of early galaxies with the currently missing dust-obscured galaxies, like the ones we found this time, will be one of the main objectives of JWST and ALMA surveys in the near future,” states Pascal Oesch from University of Geneva.

Overall, this study constitutes an important step in uncovering when the very first galaxies started to form in the early Universe, which in turn shall help us understand where we are standing today.

See the full article here .

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Please help promote STEM in your local schools.

Stem Education Coalition

The Atacama Large Millimeter/submillimeter Array (ALMA)(CL) , an international astronomy facility, is a partnership of Europe, North America and East Asia in cooperation with the Republic of Chile. ALMA is funded in Europe by the European Organization for Astronomical Research in the Southern Hemisphere (ESO), in North America by the U.S. National Science Foundation (NSF) in cooperation with the National Research Council of Canada (NRC) and the National Science Council of Taiwan (NSC) and in East Asia by the National Institutes of Natural Sciences (NINS) of Japan in cooperation with the Academia Sinica (AS) in Taiwan.

ALMA construction and operations are led on behalf of Europe by European Southern Observatory(EU), on behalf of North America by the National Radio Astronomy Observatory (NRAO), which is managed by Associated Universities, Inc. (US) and on behalf of East Asia by the National Astronomical Observatory of Japan (NAOJ). The Joint ALMA Observatory (JAO) provides the unified leadership and management of the construction, commissioning and operation of ALMA.

ALMA is a time machine!

ALMA-In Search of our Cosmic Origins

From ALMA Observatory (CL) /European Southern Observatory (EU)(CL)/National Radio Astronomy Observatory(US)/National Astronomical Observatory of Japan(JP): “ALMA Reveals Carbon-Rich Organic Birth Environments of Planets”

European Southern Observatory [Observatoire européen austral][Europäische Südsternwarte](EU)(CL)/National Radio Astronomy Observatory(US)/National Astronomical Observatory of Japan(JP) ALMA Observatory (CL)

15 September, 2021

Nicolás Lira
Education and Public Outreach Coordinator
Joint ALMA Observatory, Santiago – Chile
Phone: +56 2 2467 6519
Cell phone: +56 9 9445 7726
Email: nicolas.lira@alma.cl

Masaaki Hiramatsu
Education and Public Outreach Officer, NAOJ Chile
Observatory
, Tokyo – Japan
Phone: +81 422 34 3630
Email: hiramatsu.masaaki@nao.ac.jp

Bárbara Ferreira
ESO Public Information Officer
Garching bei München, Germany
Phone: +49 89 3200 6670
Email: pio@eso.org
Amy C. Oliver
Public Information & News Manager
National Radio Astronomical Observatory (NRAO), USA
Phone: +1 434 242 9584
Email: aoliver@nrao.edu

All general references:
ALMA Observatory (CL)
European Southern Observatory(EU)
National Astronomical Observatory of Japan(JP)
National Radio Astronomy Observatory(US)

This composite image of ALMA data from the young star HD 163296 shows hydrogen cyanide emission laid over a starfield. The MAPS project zoomed in on hydrogen cyanide and other organic and inorganic compounds in planet-forming disks to gain a better understanding of the compositions of young planets and how the compositions link to where planets form in a protoplanetary disk. Credit: ALMA (ESO/NAOJ/NRAO)/D. Berry (NRAO), K. Öberg et al (MAPS)

An international collaboration of scientists using the Atacama Large Millimeter/submillimeter Array (ALMA) has completed the most extensive chemical composition mapping of the protoplanetary disks around five nearby young stars at high resolution, producing images that capture the molecular composition associated with planetary births, and a roadmap for future studies of the makeup of planet- and comet-forming regions. The new study unlocks clues about the role of molecules in planetary system formation, and whether these young planetary systems in the making have what it takes to host life. The results of the program, appropriately called MAPS, or Molecules with ALMA at Planet-forming Scales, will appear in an upcoming 20-paper special edition of The Astrophysical Journal Supplement Series.

Planets form in the disks of dust and gas—also called protoplanetary disks—surrounding young stars. The chemical makeup of—or molecules contained within—these disks may have an impact on the planets themselves, including how and where planetary formation occurs, the chemical composition of the planets, and whether those planets have the organic composition necessary to support life. MAPS specifically looked at the protoplanetary disks surrounding the young stars IM Lup, GM Aur, AS 209, HD 163296, and MWC 480, where evidence of ongoing planet formation has already been detected. The project led to multiple exciting discoveries, including a link between dust and chemical substructures and the presence of large reservoirs of organic molecules in the inner disk regions of the stars.

“With ALMA we were able to see how molecules are distributed where exoplanets are currently assembling,” said Karin Öberg, an astronomer at the Center for Astrophysics | Harvard & Smithsonian (CfA)(US) and the Principal Investigator for MAPS. “One of the really exciting things we saw is that the planet-forming disks around these five young stars are factories of a special class of organic molecules, so-called nitriles, which are implicated in the origins of life here on Earth.”

Simple organic molecules like HCN, C2H, and H2CO were observed throughout the project in unprecedented detail, thanks to the sensitivity and resolving power of ALMA’s Band 3 and Band 6 receivers. “In particular, we were able to observe the amount of small organic molecules in the inner regions of disks, where rocky planets are likely assembling,” said Viviana V. Guzmán, an astronomer at The Pontifical Catholic University of Chile [Pontificia Universidad Católica de Chile] (CL)’s Institute of Astrophysics[Instituto de Astrofísica](CL), lead author on MAPS VI and a MAPS co-Principal Investigator. “We’re finding that our own Solar System is not particularly unique, and that other planetary systems around other stars have enough of the basic ingredients to form the building blocks of life.”

Scientists also observed more complex organic molecules like HC3N, CH3CN, and c-C3H2—notably those containing carbon, and therefore most likely to act as the feedstock of larger, prebiotic molecules. Although these molecules have been detected in protoplanetary disks before, MAPS is the first systematic study across multiple disks at very high spatial resolution and sensitivity, and the first study to find the molecules at small scales and in such significant quantities. “We found more of the large organic molecules than expected, a factor of 10 to 100 more, located in the inner disks on scales of the Solar System, and their chemistry appears similar to that of Solar System comets,” said John Ilee, an astronomer at The University of Leeds (UK) and the lead author of MAPS IX. “The presence of these large organic molecules is significant because they are the stepping-stones between simpler carbon-based molecules such as carbon monoxide, which is found in abundance in space, and the more complex molecules that are required to create and sustain life.”

Molecules are not distributed uniformly across planet-forming disks, however, as evidenced in MAPS III and IV, which revealed that while the general disk compositions appear to be similar to the Solar System, zooming in at high resolution reveals some diversity in composition that could result in planet-to-planet differences. “Molecular gas in protoplanetary disks is often found in sets of distinct rings and gaps,” said Charles Law, CfA astronomer and lead author on MAPS III and IV. “But the same disk observed in different molecular emission lines often looks completely different, with each disk having multiple molecular faces. This also means that planets in different disks or even in the same disk at different locations may form in radically different chemical environments.” This means that some planets form with the necessary tools for building and sustaining life while other nearby planets may not.

One of those radically different environments occurs in the space surrounding Jupiter-like planets, where scientists found the gas to be poor in carbon, oxygen, and heavier elements, while rich in hydrocarbons, such as methane. “The chemistry that is seen in protoplanetary disks should be inherited by forming planets,” said Arthur Bosman, an astronomer at The University of Michigan (US) and lead author of MAPS VII. “Our findings suggest that many gas giants may form with extremely oxygen-poor (carbon-rich) atmospheres, challenging current expectations of planet compositions.”

Taken all together, MAPS is providing exactly that: a map for scientists to follow, connecting the dots between the gas and dust in a protoplanetary disk and the planets that eventually form from them to create a planetary system. “A planet’s composition is a record of the location in the disk in which it was formed,” said Bosman. “Connecting planet and disk composition enables us to peer into the history of a planet and helps us to understand the forces that formed it.”

Joe Pesce, astronomer and ALMA program officer at the National Science Foundation (US) notes, “whether life exists beyond Earth is one of humanity’s fundamental questions. We now know planets are found everywhere, and the next step is to determine if they have the conditions necessary for life as we know it (and how common that situation might be). The MAPS program will help us better answer these questions. ALMA’s search for precursors to life far from Earth complements studies conducted in laboratories, and in places like hydrothermal vents on Earth.”

Öberg added, “MAPS is the culmination of decades of work on the chemistry of planet-forming disks by scientists using ALMA and its precursors. Although MAPS has surveyed just five disks at this time, we had no idea how chemically complex and visually stunning these disks really were until now. MAPS has first answered questions we could not have imagined asking decades ago, and also presented us with many more questions to answer.”

Additional Information

The highlighted papers of this research are:

“Molecules with ALMA at Planet-forming Scales (MAPS) I: Program overview and highlights,” K. Öberg et al, ApJS, preview [ https://arxiv.org/pdf/2109.06268.pdf ]

“Molecules with ALMA at Planet-forming Scales (MAPS) III: Characteristics of radial chemical substructures,” C. Law et al, ApJS, preview [ https://arxiv.org/pdf/2109.06210.pdf ]

“Molecules with ALMA at Planet-forming Scales (MAPS). IV: Emission Surfaces and Vertical Distribution of Molecules,” C. Law, ApJS, preview [ https://arxiv.org/pdf/2109.06217.pdf ]

“Molecules with ALMA at Planet-forming Scales (MAPS) VI: Distribution of the small organics HCN, C2H, and H2CO,” V. Guzmán et al, ApJS, preview [ https://arxiv.org/pdf/2109.06391.pdf ]

“Molecules with ALMA at Planet-forming Scales (MAPS) VII: Substellar O/H and C/H and superstellar C/O in planet-feeding gas,” A. Bosman et al, ApJS, preview [ https://arxiv.org/pdf/2109.06221.pdf ]

“Molecules with ALMA at Planet-forming Scales (MAPS) IX: “Distribution and properties of the large organic molecules HC3N, CH3CN, and c-C3H2,” J. Ilee et al, ApJS, preview [ https://arxiv.org/pdf/2109.06319.pdf ]

See the full article here .

five-ways-keep-your-child-safe-school-shootings

Please help promote STEM in your local schools.

Stem Education Coalition

The Atacama Large Millimeter/submillimeter Array (ALMA)(CL) , an international astronomy facility, is a partnership of Europe, North America and East Asia in cooperation with the Republic of Chile. ALMA is funded in Europe by the European Organization for Astronomical Research in the Southern Hemisphere (ESO), in North America by the U.S. National Science Foundation (NSF) in cooperation with the National Research Council of Canada (NRC) and the National Science Council of Taiwan (NSC) and in East Asia by the National Institutes of Natural Sciences (NINS) of Japan in cooperation with the Academia Sinica (AS) in Taiwan.

ALMA construction and operations are led on behalf of Europe by European Southern Observatory(EU), on behalf of North America by the National Radio Astronomy Observatory (NRAO), which is managed by Associated Universities, Inc. (US) and on behalf of East Asia by the National Astronomical Observatory of Japan (NAOJ). The Joint ALMA Observatory (JAO) provides the unified leadership and management of the construction, commissioning and operation of ALMA.

ALMA is a time machine!

ALMA-In Search of our Cosmic Origins

From ALMA [The Atacama Large Millimeter/submillimeter Array] (CL) : “ALMA Goes to New (Wave) Lengths”

European Southern Observatory/National Radio Astronomy Observatory(US)/National Astronomical Observatory of Japan(JP) ALMA Array in Chile in the Atacama at Chajnantor plateau, at 5,000 metres.

From ALMA [The Atacama Large Millimeter/submillimeter Array] (CL)

8 September, 2021

Nicolás Lira
Education and Public Outreach Coordinator
Joint ALMA Observatory, Santiago – Chile
Phone: +56 2 2467 6519
Cell phone: +56 9 9445 7726
Email: nicolas.lira@alma.cl

Masaaki Hiramatsu
Education and Public Outreach Officer, NAOJ Chile
Observatory
, Tokyo – Japan
Phone: +81 422 34 3630
Email: hiramatsu.masaaki@nao.ac.jp

Bárbara Ferreira
ESO Public Information Officer
Garching bei München, Germany
Phone: +49 89 3200 6670
Email: pio@eso.org

Amy C. Oliver
Public Information & News Manager
National Radio Astronomical Observatory (NRAO), USA
Phone: +1 434 242 9584
Email: aoliver@nrao.edu

Band-1 cold cartridge assemblies at the Band-1 Integration and Verification Laboratory at Aeronautical Systems Research Division TAF Labs (TW). Credits: ASIAA/Yuh-Jing Hwang and ASRD.

Band-1 warm cartridge assemblies integrated and tested at the Band-1 Integration and Verification Laboratory at ASRD in Taiwan. Credits: ASIAA/Yuh-Jing Hwang and ASRD.

Band-1 receiver with cold cartridge assembly (front), lens (middle) and warm cartridge assembly (right) ready for installation at the ALMA OSF in Chile. Credit: G.Siringo – ALMA (ESO/NAOJ/NRAO.

First Band-1 receiver installed into cryostat (blue) at the ALMA OSF in Chile for noise measurement. The center white circular structure is the lens for the Band-1 receiver with the cold cartridge assembly mounted behind it. Credit: Yuh-Jing Hwang – ASIAA

The Atacama Large Millimeter/submillimeter Array (ALMA) achieved first light with new Band 1 receivers, setting a new record for the most extended wavelengths capabilities with its radio antennas. This achievement opens a window on the Universe previously inaccessible at the telescope, thanks to an international team of engineers.

ALMA observes the Universe over a wide range of radio wavelengths within the millimeter and submillimeter section of the electromagnetic spectrum with the help of specialized receivers. Each one is sensitive to a particular “band” of wavelengths. So far eight out of ten receivers have been mounted on the antennas covering altogether the window between 0.3 and 3.6 millimeters.

The international team worked hard to integrate the receiver in the ALMA telescope and perform test observations under challenging conditions. “One of the most challenging issues has been the remote coordination of the activities of all the people involved,” says Giorgio Siringo, ALMA Senior Engineer. “That have been carried out from different continents during the pandemic emergency.”

For any new receiver, the successful ‘first light’ marks a major breakthrough as it is the first time that an astronomical signal (light) goes through the entire telescope, from the antenna that is collecting the light, through the receiver with all the backend electronics, to a computer screen at the end displaying the result. It is the ultimate test that design; fabrication; and assembly are all perfect. After around 10 years of hard and meticulous work, the Band 1 receiver successfully achieved first light with successful observations of the edge of the Moon on 14 August 2021, followed by the first successful interferometry test observations with two antennas with Band 1 receivers on 17 August, and the acquisition of the first radio spectrum on 27 August. During the test observations the new receivers successfully received signals from various objects from near to far, including planets (Venus, and Mars), evolved stars and molecular clouds (Orion KL and VY Canis Majoris) in our Galaxy, and extra-galactic distant quasars (3C 279), and the team confirmed the receiver’s performance.

The Band 1 receiver once installed on all 66 ALMA antennas will break new ground in various science areas. The new receiver will allow astronomers to peer out at the distant redshifted Universe further than any other receiver on ALMA. Band 1 is also much anticipated to make the next breakthrough discoveries in the study of planet formation. The production of receivers for all ALMA antennas is currently being completed in Taiwan, aiming to offer this new band for open-use observations from Cycle 10, starting in 2023.

“It will enable the detection of centimeter-sized dust grains and small pebbles in regions where planets can form. With this we can study the growth of dust grains and eventually understand how planets form out of interstellar dust”, says Hsi-Wei Yen, the Band 1 project scientist at Taiwan’s Academia Sinica Institute of Astronomy and Astrophysics (ASIAA).

The development of the ALMA Band 1 is led by Academia Sinica Institute of Astronomy and Astrophysics(TW), supported by an international team comprising the National Astronomical Observatory of Japan (NAOJ), The University of Chile [Universidad de Chile](CL), the National Radio Astronomy Observatory (NRAO), The Herzberg Institute of Astrophysics (CA) and the The National Chung-Shan Institute of Science and Technology [ 國家中山科學研究院] (TW). Since the beginning,The University of Chile [Universidad de Chile](CL) has been involved in the project, helping to develop and produce optical elements such as the lenses and horn antennas for the Band 1 receivers.

Recently, the ALMA board signed a contract to develop the last missing set of ALMA receivers (Band 2), which a consortium of European institutions will lead.

See the full article here .

five-ways-keep-your-child-safe-school-shootings

Please help promote STEM in your local schools.

Stem Education Coalition

The Atacama Large Millimeter/submillimeter Array (ALMA) (CL) , an international astronomy facility, is a partnership of Europe, North America and East Asia in cooperation with the Republic of Chile. ALMA is funded in Europe by the European Organization for Astronomical Research in the Southern Hemisphere (ESO), in North America by the U.S. National Science Foundation (NSF) in cooperation with the National Research Council of Canada (NRC) and the National Science Council of Taiwan (NSC) and in East Asia by the National Institutes of Natural Sciences (NINS) of Japan in cooperation with the Academia Sinica (AS) in Taiwan.

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

ALMA is a time machine!

ALMA-In Search of our Cosmic Origins

From IAC Institute of Astrophysics of the Canary Islands [Instituto de Astrofísica de Canarias] (ES) : “Dust in the central parsecs of unobscured AGN provide more challenges to the torus”

From IAC Institute of Astrophysics of the Canary Islands [Instituto de Astrofísica de Canarias] (ES)

04/09/2021

M Almudena, Prieto Escudero, J. Nadolny
Instituto de Astrofísica de Canarias (IAC)

J. A. Fernández-Ontiveros
Istituto di Astrofisica e Planetologia Spaziali (IT)

M. Mezcua
Institute of Space Studies of Catalonia [Institut d’Estudis Espacials de Catalunya](ES)

The image shows the process of nuclear feeding of a black hole in the galaxy NGC 1566, and how the dust filaments – seen in white-blue colors- are trapped and rotating in a spiral around the black hole until the black hole swallows them. Credit: ESO.

The black holes at the centres of galaxies are the most mysterious objects in the Universe, not only because of the huge quantities of material within them, millions of times the mass of the Sun, but because of the incredibly dense concentration of matter in a volume no bigger than that of our Solar System. When they capture matter from their surroundings they become active, eventually giving rise to the ejection of huge amounts of energy. It is however difficult to detect the black hole during these capture episodes because the event is rare. We detected long and narrow dust filaments surrounding and feeding the black hole in the centres of several galaxies. These filaments could furthermore be the natural cause of the darkening of the centre of many galaxies when their nuclear black holes become active. The discovery of these filaments and the understanding of their nature have been made possible by using extremely sharp images obtained with the Hubble Space Telescope, the Very Large Telescope (VLT) at the European Southern Observatory (ESO), and the Atacama Large Millimetre Array (ALMA) in Chile.

National Aeronautics and Space Administration(US)/European Space Agency [Agence spatiale européenne] [Europäische Weltraumorganisation] (EU) Hubble Space Telescope

European Southern Observatory(EU) , Very Large Telescope at Cerro Paranal in the Atacama Desert •ANTU (UT1; The Sun ) •KUEYEN (UT2; The Moon ) •MELIPAL (UT3; The Southern Cross ), and •YEPUN (UT4; Venus – as evening star). Elevation 2,635 m (8,645 ft) from above Credit J.L. Dauvergne & G. Hüdepohl atacama photo.

[Observatoire européen austral][Europäische Südsternwarte] (EU)/National Radio Astronomy Observatory(US)/National Astronomical Observatory of Japan(JP) ALMA Array in Chile in the Atacama at Chajnantor plateau, at 5,000 metres.

Each of these images provides us with a different view of the various states of the interstellar medium in which these filaments reside. Their combined analysis led to a direct visualisation of filaments feeding the black hole. A first estimate of the amount of matter in the filaments indicates an inflow equivalent to the mass of the Sun per year.

Science paper:
MNRAS

See the full article here .

five-ways-keep-your-child-safe-school-shootings

Please help promote STEM in your local schools.

Stem Education Coalition

IAC Institute of Astrophysics of the Canary Islands [Instituto de Astrofísica de Canarias] (ES) operates two astronomical observatories in the Canary Islands:

Roque de los Muchachos Observatory on La Palma
Teide Observatory on Tenerife.

The Instituto de Astrofísica the headquarters, which is in La Laguna (Tenerife).

Observatorio del Roque de los Muchachos at La Palma (ES) at an altitude of 2400m,.

The seeing statistics at ORM make it the second-best location for optical and infrared astronomy in the Northern Hemisphere, after Mauna Kea Observatory Hawaii (US).

Maunakea Observatories Hawai’i (US) altitude 4,213 m (13,822 ft)

The site also has some of the most extensive astronomical facilities in the Northern Hemisphere; its fleet of telescopes includes the 10.4 m Gran Telescopio Canarias, the world’s largest single-aperture optical telescope as of July 2009, the William Herschel Telescope (second largest in Europe), and the adaptive optics corrected Swedish 1-m Solar Telescope.

Gran Telescopio Canarias [Instituto de Astrofísica de Canarias ](ES) sited on a volcanic peak 2,267 metres (7,438 ft) above sea level.

Isaac Newton Group 4.2 meter William Herschel Telescope at Roque de los Muchachos Observatory on La Palma in the Canary Islands(ES), 2,396 m (7,861 ft)

The Swedish 1m Solar Telescope SST at the Roque de los Muchachos observatory on La Palma Spain, Altitude 2,360 m (7,740 ft).

The observatory was established in 1985, after 15 years of international work and cooperation of several countries with the Spanish island hosting many telescopes from Britain, The Netherlands, Spain, and other countries. The island provided better seeing conditions for the telescopes that had been moved to Herstmonceux by the Royal Greenwich Observatory, including the 98 inch aperture Isaac Newton Telescope (the largest reflector in Europe at that time). When it was moved to the island it was upgraded to a 100-inch (2.54 meter), and many even larger telescopes from various nations would be hosted there.

Tiede Observatory, Tenerife, Canary Islands (ES)

Teide Observatory [Observatorio del Teide], IAU code 954, is an astronomical observatory on Mount Teide at 2,390 metres (7,840 ft), located on Tenerife, Spain. It has been operated by the Instituto de Astrofísica de Canarias since its inauguration in 1964. It became one of the first major international observatories, attracting telescopes from different countries around the world because of the good astronomical seeing conditions. Later the emphasis for optical telescopes shifted more towards Roque de los Muchachos Observatory on La Palma.

From California Institute of Technology (US) : “Observatory in Chile Takes Highest-Resolution Measurements of Asteroid Surface Temperatures Ever Obtained from Earth”

From California Institute of Technology (US)

August 05, 2021

The study’s target, Psyche, is the destination of an upcoming NASA mission.

A close examination of the millimeter-wavelength emissions from the asteroid Psyche, which NASA intends to visit in 2026, has produced the first temperature map of the object, providing new insight into its surface properties. The findings, described in a paper published in Planetary Science Journal on August 5, are a step toward resolving the mystery of the origin of this unusual object, which has been thought by some to be a chunk of the core of an ill-fated protoplanet.

Psyche orbits the sun in the asteroid belt, a donut-shaped region of space between Earth and Jupiter that contains more than a million rocky bodies that range in size from 10 meters to 946 kilometers in diameter.

The inner Solar System, from the Sun to Jupiter. Also includes the asteroid belt (the white donut-shaped cloud), the Hildas (the orange “triangle” just inside the orbit of Jupiter), the Jupiter trojans (green), and the near-Earth asteroids. The group that leads Jupiter are called the “Greeks” and the trailing group are called the “Trojans” (Murray and Dermott, Solar System Dynamics, pg. 107)This image is based on data found in the en:JPL DE-405 ephemeris, and the en:Minor Planet Center database of asteroids (etc) published 2006 Jul 6. The image is looking down on the en:ecliptic plane as would have been seen on 2006 August 14. It was rendered by custom software written for Wikipedia. The same image without labels is also available at File:InnerSolarSystem.png. Mdf at English Wikipedia.

With a diameter of more than 200 km, Psyche is the largest of the M-Type asteroids, an enigmatic class of asteroids that are thought to be metal rich and therefore potentially may be fragments of the cores of proto-planets that broke up as the solar system formed.

“The early solar system was a violent place, as planetary bodies coalesced and then collided with one another while settling into orbits around the sun,” says Caltech’s Katherine de Kleer, assistant professor of planetary science and astronomy and lead author of the PSJ article. “We think that fragments of the cores, mantles, and crusts of these objects remain today in the form of asteroids. If that’s true, it gives us our only real opportunity to directly study the cores of planet-like objects.”

Studying such relatively tiny objects that are so far away from Earth (Psyche drifts at a distance that ranges between 179.5 and 329 million km from Earth) poses a significant challenge to planetary scientists, which is why NASA plans to send a probe to Psyche to examine it up close.

NASA Psyche spacecraft depiction.

Typically, thermal observations from Earth—which measure the light emitted by an object itself rather than light from the sun reflected off of that object—are in infrared wavelengths and can produce only 1-pixel images of asteroids. That one pixel does, however, reveal a lot of information; for example, it can be used to study the asteroid’s thermal inertia, or how fast it heats up in sunlight and cools down in darkness.

“Low thermal inertia is typically associated with layers of dust, while high thermal inertia may indicate rocks on the surface,” says Caltech’s Saverio Cambioni, postdoctoral scholar in planetary science and co-author of the PSJ article. “However, discerning one type of landscape from the other is difficult.” Data from viewing each surface location at many times of day provide much more detail, leading to an interpretation that is subject to less ambiguity, and which provide a more reliable prediction of landscape type prior to a spacecraft’s arrival.

De Kleer and Cambioni, together with co-author Michael Shepard of Bloomsburg University (US) in Pennsylvania, took advantage of the Atacama Large Millimeter/submillimeter Array (ALMA) in Chile, which became fully operational in 2013, to obtain such data.

[Observatoire européen austral][Europäische Südsternwarte] (EU)/National Radio Astronomy Observatory(US)/National Astronomical Observatory of Japan(JP) ALMA Array in Chile in the Atacama at Chajnantor plateau, at 5,000 metres.

The array of 66 radio telescopes enabled the team to map the thermal emissions from Psyche’s entire surface at a resolution of 30 km (where each pixel is 30 km by 30 km) and generate an image of the asteroid composed of about 50 pixels.

This was possible because ALMA observed Psyche at millimeter wavelengths, which are longer (ranging from 1 to 10 millimeters) than the infrared wavelengths (typically between 5 and 30 microns). The use of longer wavelengths allowed the researchers to combine the data collected from the 66 telescopes to create a much larger effective telescope; the larger a telescope, the higher the resolution of the images it produces.

The study confirmed that Psyche’s thermal inertia is high compared to that of a typical asteroid, indicating that Psyche has an unusually dense or conductive surface. When de Kleer, Cambioni, and Shepard analyzed the data, they also found that Psyche’s thermal emission—the amount of heat it radiates—is just 60 percent of what would be expected from a typical surface with that thermal inertia. Because surface emission is affected by the presence of metal on the surface, their finding indicates that Psyche’s surface is no less than 30 percent metal. An analysis of the polarization of the emission helped the researchers to roughly determine what form that metal takes. A smooth solid surface emits well-organized polarized light; the light emitted by Psyche, however, was scattered, suggesting that rocks on the surface are peppered with metallic grains.

“We’ve known for many years that objects in this class are not in fact solid metal but what they are and how they formed is still an enigma,” de Kleer says. The findings reinforce alternative proposals for Psyche’s surface composition, including that Psyche could be a primitive asteroid that formed closer to the sun than it is today instead of a core of a fragmented protoplanet.

The techniques described in this study provide a new perspective on asteroid surface compositions. The team is now expanding its scope to apply these techniques to other large objects in the asteroid belt.

The study was enabled by a related project by the team led by Michael Shepard at Bloomsburg University that utilized de Kleer’s data in combination with data from other telescopes, including Arecibo Observatory in Puerto Rico, to pin down the size, shape, and orientation of Psyche. That in turn allowed the researchers to determine which pixels that had been captured actually represented the asteroid’s surface. Shepard’s team was scheduled to observe Psyche again at the end of 2020, but damage from cable failures shut the telescope down before the observations could be made.

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Caltech campus

The California Institute of Technology (US) is a private research university in Pasadena, California. The university is known for its strength in science and engineering, and is one among a small group of institutes of technology in the United States which is primarily devoted to the instruction of pure and applied sciences.

Caltech was founded as a preparatory and vocational school by Amos G. Throop in 1891 and began attracting influential scientists such as George Ellery Hale, Arthur Amos Noyes, and Robert Andrews Millikan in the early 20th century. The vocational and preparatory schools were disbanded and spun off in 1910 and the college assumed its present name in 1920. In 1934, Caltech was elected to the Association of American Universities, and the antecedents of National Aeronautics and Space Administration (US)’s Jet Propulsion Laboratory, which Caltech continues to manage and operate, were established between 1936 and 1943 under Theodore von Kármán.

Caltech has six academic divisions with strong emphasis on science and engineering. Its 124-acre (50 ha) primary campus is located approximately 11 mi (18 km) northeast of downtown Los Angeles. First-year students are required to live on campus, and 95% of undergraduates remain in the on-campus House System at Caltech. Although Caltech has a strong tradition of practical jokes and pranks, student life is governed by an honor code which allows faculty to assign take-home examinations. The Caltech Beavers compete in 13 intercollegiate sports in the NCAA Division III’s Southern California Intercollegiate Athletic Conference (SCIAC).

As of October 2020, there are 76 Nobel laureates who have been affiliated with Caltech, including 40 alumni and faculty members (41 prizes, with chemist Linus Pauling being the only individual in history to win two unshared prizes). In addition, 4 Fields Medalists and 6 Turing Award winners have been affiliated with Caltech. There are 8 Crafoord Laureates and 56 non-emeritus faculty members (as well as many emeritus faculty members) who have been elected to one of the United States National Academies. Four Chief Scientists of the U.S. Air Force and 71 have won the United States National Medal of Science or Technology. Numerous faculty members are associated with the Howard Hughes Medical Institute(US) as well as National Aeronautics and Space Administration(US). According to a 2015 Pomona College(US) study, Caltech ranked number one in the U.S. for the percentage of its graduates who go on to earn a PhD.

Research

Caltech is classified among “R1: Doctoral Universities – Very High Research Activity”. Caltech was elected to the Association of American Universities in 1934 and remains a research university with “very high” research activity, primarily in STEM fields. The largest federal agencies contributing to research are National Aeronautics and Space Administration(US); National Science Foundation(US); Department of Health and Human Services(US); Department of Defense(US), and Department of Energy(US).

In 2005, Caltech had 739,000 square feet (68,700 m^2) dedicated to research: 330,000 square feet (30,700 m^2) to physical sciences, 163,000 square feet (15,100 m^2) to engineering, and 160,000 square feet (14,900 m^2) to biological sciences.

In addition to managing JPL, Caltech also operates the Caltech Palomar Observatory(US); the Owens Valley Radio Observatory(US);the Caltech Submillimeter Observatory(US); the W. M. Keck Observatory at the Mauna Kea Observatory(US); the Laser Interferometer Gravitational-Wave Observatory at Livingston, Louisiana and Richland, Washington; and Kerckhoff Marine Laboratory(US) in Corona del Mar, California. The Institute launched the Kavli Nanoscience Institute at Caltech in 2006; the Keck Institute for Space Studies in 2008; and is also the current home for the Einstein Papers Project. The Spitzer Science Center(US), part of the Infrared Processing and Analysis Center(US) located on the Caltech campus, is the data analysis and community support center for NASA’s Spitzer Infrared Space Telescope [no longer in service].

Caltech partnered with University of California at Los Angeles(US) to establish a Joint Center for Translational Medicine (UCLA-Caltech JCTM), which conducts experimental research into clinical applications, including the diagnosis and treatment of diseases such as cancer.

Caltech operates several Total Carbon Column Observing Network(US) stations as part of an international collaborative effort of measuring greenhouse gases globally. One station is on campus.

From ALMA(CL) via SciTechDaily : “ALMA Dives into Black Hole’s Sphere of Influence”

European Southern Observatory/National Radio Astronomy Observatory(US)/National Astronomical Observatory of Japan(JP) ALMA Array in Chile in the Atacama at Chajnantor plateau, at 5,000 metres.

From ALMA(CL)/ European Southern Observatory/National Radio Astronomy Observatory(US)/National Astronomical Observatory of Japan(JP)

via

SciTechDaily

7 August, 2019 [Originally presented by NRAO, re-issued here 8.1.21 by ALMA via SciTechDaily]

Nicolás Lira
Education and Public Outreach Coordinator
Joint ALMA Observatory, Santiago – Chile
Phone: +56 2 2467 6519
Cell phone: +56 9 9445 7726
Email: nicolas.lira@alma.cl

Masaaki Hiramatsu
Education and Public Outreach Officer, NAOJ Chile
Observatory
, Tokyo – Japan
Phone: +81 422 34 3630
Email: hiramatsu.masaaki@nao.ac.jp

Bárbara Ferreira
ESO Public Information Officer
Garching bei München, Germany
Phone: +49 89 3200 6670
Email: pio@eso.org

Amy C. Oliver
Public Information & News Manager
National Radio Astronomical Observatory (NRAO), USA
Phone: +1 434 242 9584
Email: aoliver@nrao.edu

All general references:
ALMA Observatory (CL)
European Southern Observatory(EU)
National Astronomical Observatory of Japan(JP)
National Radio Astronomy Observatory(US)

Artist impression of disk of material rotating around a supermassive black hole. Credit: NRAO/Associated Universities Inc (US)/National Science Foundation (US).

What happens inside a black hole stays inside a black hole, but what happens inside a black hole’s “sphere of influence” – the innermost region of a galaxy where a black hole’s gravity is the dominant force – is of intense interest to astronomers and can help determine the mass of a black hole as well as its impact on its galactic neighborhood.

New observations with the Atacama Large Millimeter/submillimeter Array (ALMA) provide an unprecedented close-up view of a swirling disk of cold interstellar gas rotating around a supermassive black hole. This disk lies at the center of NGC 3258-a massive elliptical galaxy about 100 million light-years from Earth. Based on these observations, a team led by astronomers from Texas A&M University (US) and The University of California-Irvine (US), have determined that this black hole weighs a staggering 2.25 billion solar masses, the most massive black hole measured with ALMA to date.

Though supermassive black holes can have masses that are millions to billions of times that of the Sun, they account for just a small fraction of the mass of an entire galaxy. Isolating the influence of a black hole’s gravity from the stars, interstellar gas, and dark matter in the galactic center is challenging and requires highly sensitive observations on phenomenally small scales.

“Observing the orbital motion of material as close as possible to a black hole is vitally important when accurately determining the black hole’s mass.” said Benjamin Boizelle, a postdoctoral researcher at Texas A&M University and lead author on the study appearing in The Astrophysical Journal. “These new observations of NGC 3258 demonstrate ALMA’s amazing power to map the rotation of gaseous disks around supermassive black holes in stunning detail.”

Astronomers use a variety of methods to measure black hole masses. In giant elliptical galaxies, most measurements come from observations of the orbital motion of stars around the black hole, taken in visible or infrared light. Another technique, using naturally occurring water masers (radio-wavelength lasers) in gas clouds orbiting around black holes, provides higher precision, but these masers are very rare and are associated almost exclusively with spiral galaxies having smaller black holes.

During the past few years, ALMA has pioneered a new method to study black holes in giant elliptical galaxies. About 10 percent of elliptical galaxies contain regularly rotating disks of cold, dense gas at their centers. These disks contain carbon monoxide (CO) gas, which can be observed with millimeter-wavelength radio telescopes.

By using the Doppler shift of the emission from CO molecules, astronomers can measure the velocities of clouds, and ALMA makes it possible to resolve the very centers of galaxies where the orbital speeds are highest.

“Our team has been surveying nearby elliptical galaxies with ALMA for several years to find and study disks of molecular gas rotating around giant black holes,” said Aaron Barth of UC Irvine, a co-author on the study. “NGC 3258 is the best target we’ve found, because we’re able to trace the disk’s rotation closer to the black hole than in any other galaxy.”

Just as the Earth orbits around the Sun faster than Pluto does because it experiences a stronger gravitational force, the inner regions of the NGC 3258 disk orbit faster than the outer parts due to the black hole’s gravity. The ALMA data show that the disk’s rotation speed rises from 1 million kilometers per hour at its outer edge, about 500 light-years from the black hole, to well over 3 million kilometers per hour near the disk’s center at a distance of just 65 light-years from the black hole.

The researchers determined the black hole’s mass by modeling the disk’s rotation, accounting for the additional mass of the stars in the galaxy’s central region and other details such as the slightly warped shape of the gaseous disk. The clear detection of rapid rotation enabled the researchers to determine the black hole’s mass with a precision better than one percent, although they estimate an additional systematic 12 percent uncertainty in the measurement because the distance to NGC 3258 is not known very precisely. Even accounting for the uncertain distance, this is one of the most highly precise mass measurements for any black hole outside of the Milky Way galaxy.

“The next challenge is to find more examples of near-perfect rotating disks like this one so that we can apply this method to measure black hole masses in a larger sample of galaxies,” concluded Boizelle. “Additional ALMA observations that reach this level of precision will help us better understand the growth of both galaxies and black holes across the age of the universe.”

See the full article here .

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The Atacama Large Millimeter/submillimeter Array (ALMA)(CL) , an international astronomy facility, is a partnership of Europe, North America and East Asia in cooperation with the Republic of Chile. ALMA is funded in Europe by the European Organization for Astronomical Research in the Southern Hemisphere (ESO), in North America by the U.S. National Science Foundation (NSF) in cooperation with the National Research Council of Canada (NRC) and the National Science Council of Taiwan (NSC) and in East Asia by the National Institutes of Natural Sciences (NINS) of Japan in cooperation with the Academia Sinica (AS) in Taiwan.

ALMA construction and operations are led on behalf of Europe by European Southern Observatory(EU), on behalf of North America by the National Radio Astronomy Observatory (NRAO), which is managed by Associated Universities, Inc. (US) and on behalf of East Asia by the National Astronomical Observatory of Japan (NAOJ). The Joint ALMA Observatory (JAO) provides the unified leadership and management of the construction, commissioning and operation of ALMA.

ALMA is a time machine!

ALMA-In Search of our Cosmic Origins

From Yale University (US) : “Catching a cosmic boomerang in action”

From Yale University (US)

July 29, 2021
By Jim Shelton

Media Contact
Fred Mamoun
fred.mamoun@yale.edu
203-436-2643

Zoomed in view of an ALMA (red/orange) and Hubble Space Telescope (optical) composite of NGC4921. This composite highlights filament structures resulting from the effects of ram pressure stripping. Ram pressure stripping is a process known to strip gas out of galaxies, leaving them without the material needed to form new stars. A new study indicates that some material may not be stripped away from the galaxy, and is instead, reaccreted, potentially with the help of magnetic fields, slowing down the process of galaxy death. Credit: L. Shatz/ALMA Observatory(CL) (European Southern Observatory [Observatoire européen austral][Europäische Südsternwarte] (EU)(CL) /National Astronomy Observatory of Japan (JP)/ S. Dagnello National Radio Astronomy Observatory (US))/, National Aeronautics Space Agency (US)/European Space Agency [Agence spatiale européenne][Europäische Weltraumorganisation](EU)/Hubble/K. Cook (DOE’s Lawrence Livermore National Laboratory (US)).

For the first time, astronomers have observed a cosmic boomerang effect — streams of heavy, molecular gas that are stripped away from a distant galaxy only to circle back and return later.

Astronomers at Yale and Arizona State University (US) led the research team that made the discovery, which had been theorized in simulations but not observed in detail. Their findings are published in The Astrophysical Journal.

The observation offers new insights into the life cycle of galaxies and the structural formations within galaxies, as traced by molecular gas. In particular, the research focuses on a process called ram pressure stripping, in which gas from galaxy clusters acts like a wind that strips away the star-making material inside a galaxy — hastening its demise.

“Astronomers are interested in studying how galaxies grow, live, and die,” said lead author William Cramer, who began the research as a Yale graduate student and is now a postdoctoral research scholar at Arizona State. “Effects like ram pressure that can speed up the normal galaxy lifecycle are very important to understand for this reason. Furthermore, the molecular gas in galaxies is the birthplace of new stars, and therefore studying the effect of ram pressure on it is of paramount importance.”

This side-by-side composite shows ALMA (red/orange) data laid over Hubble Space Telescope (optical) images of NGC4921. A new study of the spiral bar galaxy revealed filament structures similar to the Pillars of Creation but significantly larger. These structures are caused by a process known as ram pressure stripping, which pushes gas out of galaxies, leaving them without the material needed to form new stars. Credit: L. Shatz/ ALMA (ESO/NAOJ/NRAO)/S. Dagnello (NRAO), NASA/ESA/Hubble/K. Cook (LLNL).

For the study, the researchers used the Atacama Large Millimeter Array (ALMA) radio telescope, located in northern Chile, to create a high-resolution map of dense molecular gas in the galaxy NGC 4921 as it experiences ram pressure stripping.

National Aeronautics and Space Administration(US)/European Space Agency [Agence spatiale européenne] [Europäische Weltraumorganisation] (EU) Hubble Space Telescope

European Southern Observatory [Observatoire européen austral][Europäische Südsternwarte] (EU)/National Radio Astronomy Observatory(US)/National Astronomical Observatory of Japan(JP) ALMA Array in Chile in the Atacama at Chajnantor plateau, at 5,000 metres.

The map shows unusual structures that form in the ram pressure “wind” — long filaments of heavy gas connected to newly-forming stars. This dense, heavy gas is thought to be more resistant to ram pressure stripping, perhaps due to magnetic fields holding it more firmly in place.

“When an external force like ram pressure disturbs a galaxy, it offers an opportunity to learn about the internal forces that operate in galaxies,” said co-author Jeffrey Kenney, a professor of astronomy in Yale’s Faculty of Arts and Sciences. “The unusual filaments would not form without magnetic fields, so we also learn about the importance of magnetic fields in galaxies from this ram pressure interaction.”

The ALMA data clearly show filaments of molecular gas connected to galaxy NGC 4921 — the filaments are, indeed, resisting. But then the researchers saw something else: Some of the previously-stripped gas comes back.

“Instead of being thrown out never to return, some of this gas is moving like a boomerang, being ejected but then circling and falling back to its source,” Cramer said. If this gas is recaptured into the galaxy, it can form new stars.

The boomerang effect is significant for several reasons, according to the researchers. It provides hard evidence about the evolution of galaxies; it confirms a long-held theory about galaxy development; and it aids astronomers trying to predict the birthrate of new stars.

“The interstellar medium of galaxies is complex, with many variables that are hard to model,” Cramer said. “This observation is important because it shows that fallback of gas can be detected and allows us to search more broadly to help characterize it.”

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About Yale University (US)

Yale University is a private Ivy League research university in New Haven, Connecticut. Founded in 1701 as the Collegiate School, it is the third-oldest institution of higher education in the United States and one of the nine Colonial Colleges chartered before the American Revolution. The Collegiate School was renamed Yale College in 1718 to honor the school’s largest private benefactor for the first century of its existence, Elihu Yale. Yale University is consistently ranked as one of the top universities and is considered one of the most prestigious in the nation.

Chartered by Connecticut Colony, the Collegiate School was established in 1701 by clergy to educate Congregational ministers before moving to New Haven in 1716. Originally restricted to theology and sacred languages, the curriculum began to incorporate humanities and sciences by the time of the American Revolution. In the 19th century, the college expanded into graduate and professional instruction, awarding the first PhD in the United States in 1861 and organizing as a university in 1887. Yale’s faculty and student populations grew after 1890 with rapid expansion of the physical campus and scientific research.

Yale is organized into fourteen constituent schools: the original undergraduate college, the Yale Graduate School of Arts and Sciences and twelve professional schools. While the university is governed by the Yale Corporation, each school’s faculty oversees its curriculum and degree programs. In addition to a central campus in downtown New Haven, the university owns athletic facilities in western New Haven, a campus in West Haven, Connecticut, and forests and nature preserves throughout New England. As of June 2020, the university’s endowment was valued at $31.1 billion, the second largest of any educational institution. The Yale University Library, serving all constituent schools, holds more than 15 million volumes and is the third-largest academic library in the United States. Students compete in intercollegiate sports as the Yale Bulldogs in the NCAA Division I – Ivy League.

As of October 2020, 65 Nobel laureates, five Fields Medalists, four Abel Prize laureates, and three Turing award winners have been affiliated with Yale University. In addition, Yale has graduated many notable alumni, including five U.S. Presidents, 19 U.S. Supreme Court Justices, 31 living billionaires, and many heads of state. Hundreds of members of Congress and many U.S. diplomats, 78 MacArthur Fellows, 252 Rhodes Scholars, 123 Marshall Scholars, and nine Mitchell Scholars have been affiliated with the university.

Research

Yale is a member of the Association of American Universities (AAU) (US) and is classified among “R1: Doctoral Universities – Very high research activity”. According to the National Science Foundation (US), Yale spent $990 million on research and development in 2018, ranking it 15th in the nation.

Yale’s faculty include 61 members of the National Academy of Sciences (US), 7 members of the National Academy of Engineering (US) and 49 members of the American Academy of Arts and Sciences (US). The college is, after normalization for institution size, the tenth-largest baccalaureate source of doctoral degree recipients in the United States, and the largest such source within the Ivy League.

Yale’s English and Comparative Literature departments were part of the New Criticism movement. Of the New Critics, Robert Penn Warren, W.K. Wimsatt, and Cleanth Brooks were all Yale faculty. Later, the Yale Comparative literature department became a center of American deconstruction. Jacques Derrida, the father of deconstruction, taught at the Department of Comparative Literature from the late seventies to mid-1980s. Several other Yale faculty members were also associated with deconstruction, forming the so-called “Yale School”. These included Paul de Man who taught in the Departments of Comparative Literature and French, J. Hillis Miller, Geoffrey Hartman (both taught in the Departments of English and Comparative Literature), and Harold Bloom (English), whose theoretical position was always somewhat specific, and who ultimately took a very different path from the rest of this group. Yale’s history department has also originated important intellectual trends. Historians C. Vann Woodward and David Brion Davis are credited with beginning in the 1960s and 1970s an important stream of southern historians; likewise, David Montgomery, a labor historian, advised many of the current generation of labor historians in the country. Yale’s Music School and Department fostered the growth of Music Theory in the latter half of the 20th century. The Journal of Music Theory was founded there in 1957; Allen Forte and David Lewin were influential teachers and scholars.

In addition to eminent faculty members, Yale research relies heavily on the presence of roughly 1200 Postdocs from various national and international origin working in the multiple laboratories in the sciences, social sciences, humanities, and professional schools of the university. The university progressively recognized this working force with the recent creation of the Office for Postdoctoral Affairs and the Yale Postdoctoral Association.

Notable alumni

Over its history, Yale has produced many distinguished alumni in a variety of fields, ranging from the public to private sector. According to 2020 data, around 71% of undergraduates join the workforce, while the next largest majority of 16.6% go on to attend graduate or professional schools. Yale graduates have been recipients of 252 Rhodes Scholarships, 123 Marshall Scholarships, 67 Truman Scholarships, 21 Churchill Scholarships, and 9 Mitchell Scholarships. The university is also the second largest producer of Fulbright Scholars, with a total of 1,199 in its history and has produced 89 MacArthur Fellows. The U.S. Department of State Bureau of Educational and Cultural Affairs ranked Yale fifth among research institutions producing the most 2020–2021 Fulbright Scholars. Additionally, 31 living billionaires are Yale alumni.

At Yale, one of the most popular undergraduate majors among Juniors and Seniors is political science, with many students going on to serve careers in government and politics. Former presidents who attended Yale for undergrad include William Howard Taft, George H. W. Bush, and George W. Bush while former presidents Gerald Ford and Bill Clinton attended Yale Law School. Former vice-president and influential antebellum era politician John C. Calhoun also graduated from Yale. Former world leaders include Italian prime minister Mario Monti, Turkish prime minister Tansu Çiller, Mexican president Ernesto Zedillo, German president Karl Carstens, Philippine president José Paciano Laurel, Latvian president Valdis Zatlers, Taiwanese premier Jiang Yi-huah, and Malawian president Peter Mutharika, among others. Prominent royals who graduated are Crown Princess Victoria of Sweden, and Olympia Bonaparte, Princess Napoléon.

Yale alumni have had considerable presence in U.S. government in all three branches. On the U.S. Supreme Court, 19 justices have been Yale alumni, including current Associate Justices Sonia Sotomayor, Samuel Alito, Clarence Thomas, and Brett Kavanaugh. Numerous Yale alumni have been U.S. Senators, including current Senators Michael Bennet, Richard Blumenthal, Cory Booker, Sherrod Brown, Chris Coons, Amy Klobuchar, Ben Sasse, and Sheldon Whitehouse. Current and former cabinet members include Secretaries of State John Kerry, Hillary Clinton, Cyrus Vance, and Dean Acheson; U.S. Secretaries of the Treasury Oliver Wolcott, Robert Rubin, Nicholas F. Brady, Steven Mnuchin, and Janet Yellen; U.S. Attorneys General Nicholas Katzenbach, John Ashcroft, and Edward H. Levi; and many others. Peace Corps founder and American diplomat Sargent Shriver and public official and urban planner Robert Moses are Yale alumni.

Yale has produced numerous award-winning authors and influential writers, like Nobel Prize in Literature laureate Sinclair Lewis and Pulitzer Prize winners Stephen Vincent Benét, Thornton Wilder, Doug Wright, and David McCullough. Academy Award winning actors, actresses, and directors include Jodie Foster, Paul Newman, Meryl Streep, Elia Kazan, George Roy Hill, Lupita Nyong’o, Oliver Stone, and Frances McDormand. Alumni from Yale have also made notable contributions to both music and the arts. Leading American composer from the 20th century Charles Ives, Broadway composer Cole Porter, Grammy award winner David Lang, and award-winning jazz pianist and composer Vijay Iyer all hail from Yale. Hugo Boss Prize winner Matthew Barney, famed American sculptor Richard Serra, President Barack Obama presidential portrait painter Kehinde Wiley, MacArthur Fellow and contemporary artist Sarah Sze, Pulitzer Prize winning cartoonist Garry Trudeau, and National Medal of Arts photorealist painter Chuck Close all graduated from Yale. Additional alumni include architect and Presidential Medal of Freedom winner Maya Lin, Pritzker Prize winner Norman Foster, and Gateway Arch designer Eero Saarinen. Journalists and pundits include Dick Cavett, Chris Cuomo, Anderson Cooper, William F. Buckley, Jr., and Fareed Zakaria.

In business, Yale has had numerous alumni and former students go on to become founders of influential business, like William Boeing (Boeing, United Airlines), Briton Hadden and Henry Luce (Time Magazine), Stephen A. Schwarzman (Blackstone Group), Frederick W. Smith (FedEx), Juan Trippe (Pan Am), Harold Stanley (Morgan Stanley), Bing Gordon (Electronic Arts), and Ben Silbermann (Pinterest). Other business people from Yale include former chairman and CEO of Sears Holdings Edward Lampert, former Time Warner president Jeffrey Bewkes, former PepsiCo chairperson and CEO Indra Nooyi, sports agent Donald Dell, and investor/philanthropist Sir John Templeton,

Yale alumni distinguished in academia include literary critic and historian Henry Louis Gates, economists Irving Fischer, Mahbub ul Haq, and Nobel Prize laureate Paul Krugman; Nobel Prize in Physics laureates Ernest Lawrence and Murray Gell-Mann; Fields Medalist John G. Thompson; Human Genome Project leader and National Institutes of Health (US) director Francis S. Collins; brain surgery pioneer Harvey Cushing; pioneering computer scientist Grace Hopper; influential mathematician and chemist Josiah Willard Gibbs; National Women’s Hall of Fame inductee and biochemist Florence B. Seibert; Turing Award recipient Ron Rivest; inventors Samuel F.B. Morse and Eli Whitney; Nobel Prize in Chemistry laureate John B. Goodenough; lexicographer Noah Webster; and theologians Jonathan Edwards and Reinhold Niebuhr.

In the sporting arena, Yale alumni include baseball players Ron Darling and Craig Breslow and baseball executives Theo Epstein and George Weiss; football players Calvin Hill, Gary Fenick, Amos Alonzo Stagg, and “the Father of American Football” Walter Camp; ice hockey players Chris Higgins and Olympian Helen Resor; Olympic figure skaters Sarah Hughes and Nathan Chen; nine-time U.S. Squash men’s champion Julian Illingworth; Olympic swimmer Don Schollander; Olympic rowers Josh West and Rusty Wailes; Olympic sailor Stuart McNay; Olympic runner Frank Shorter; and others.