Thursday, April 25, 2024

Travel Through Data From Space in New 3D Instagram Experiences

Vela Pulsar - Tycho's Supernova Remnant - Helix Nebula - Cat's Eye Nebula
Credit: Vela Pulsar: X-ray: NASA/CXC/SAO; Optical: NASA/ESA/STScI; Image processing: NASA/CXC/SAO/J. Schmidt, K. Arcand; Tycho's Supernova Remnant: X-ray: NASA/CXC/SAO; Optical: DSS; Image Processing: NASA/CXC/SAO/N. Wolk; Helix Nebula: X-ray: NASA/CXC/SAO; UV: NASA/JPL-Caltech/SSC; Optical: NASA/ STScI/M. Meixner, ESA/NRAO/T.A. Rector; Infrared:NASA/JPL-Caltech/K. Su; Image Processing: NASA/CXC/SAO/N. Wolk and K. Arcand; Cat's Eye Nebula: X-ray: NASA/CXC/SAO; Optical: NASA/ESA/STScI; Image Processing: NASA/CXC/SAO/J. Major, L. Frattare, K. Arcand





These images represent new special 3D “experiences” available on Instagram made with data from NASA’s Chandra X-ray Observatory and other telescopes. By using augmented reality (AR), these experiences allow people to travel virtually through objects in space.

These Chandra Instagram experiences join a space-themed collection in Instagram from recent years, that includes NASA mission control, the International Space Station, and the Perseverance Rover on Mars. The objects in the new Chandra Instagram collection include the Tycho supernova remnant, the Vela Pulsar, the Helix Nebula, the Cat’s Eye, and the Chandra spacecraft.

The new Instagram experiences are created from 3D models based on data collected by Chandra and other telescopes along with computer models. Traditionally, it has been very difficult to gather 3D data of objects in space due to their two-dimensional projection on the sky. New instruments and techniques, however, have allowed astronomers in recent years to construct data-driven models of what these distant objects look like in three dimensions.

These advancements in astronomy have paralleled the explosion of opportunities in virtual, extended, and augmented reality. Such technologies provide virtual digital experiences, which now extend beyond Earth and into the cosmos.


Tycho's Supernova Remnant Effect [More Effects]
Video Credit: Smithsonian/NASA/SAO/CXC;
Sonification: NASA/CXC/SAO/K.Arcand, SYSTEM Sounds (M. Russo, A. Santaguida)

This new set of Chandra Instagram experiences was made possible by a collaboration including NASA and the Smithsonian Institution, as well as students and researchers at Brown University. The 3D models of Tycho, Vela and Helix were done in conjunction with Sal Orlando, an astrophysicist at Italy’s National Institute for Astrophysics in Palermo. The Cat’s Eye Nebula was created with data from Ryan Clairmont, physics researcher and undergraduate at Stanford University. Kim Arcand from SAO oversaw the project and worked with Brown University’s Tom Sgouros and his team, research assistant Alexander Dupuis and undergraduate Healey Koch, on the Chandra Instagram filters.




Vela Pulsar

Vela Pulsar: The Vela Pulsar is the aftermath of a star that collapsed, followed by an explosion that sent a remarkable storm of particles and energy into space. The Chandra X-ray Observatory and other telescopes captured this storm, seen here as a 3D model. At the center of Vela is a pulsar, a rapidly spinning dense star that sends beams of light out into space like a cosmic lighthouse.

Tycho's Supernova Remnant

Tycho's Supernova Remnant: Massive stars die in giant explosions called supernovas that can outshine an entire galaxy. After a supernova explosion, the remains of the star can become a spectacular and evolving cosmic monument to the now-deceased star. These remnants glow in X-ray light, which NASA’s Chandra X-ray Observatory can detect such as in this image of Tycho’s Supernova Remnant.

Helix Nebula

Helix Nebula:In about 5 billion years, our Sun will run out of fuel and expand, possibly engulfing Earth. These end stages of a star’s life can be utterly beautiful as is the case with this planetary nebula called the Helix Nebula. Astronomers study these objects by looking at all kinds of light, including X-rays that the Chandra X-ray Observatory sees.

Cat's Eye Nebula

Cat's Eye Nebula:Eventually, our Sun will run out of fuel and die (though not for about another 5 billion years). As it does, it will become like the object seen here, the Cat’s Eye Nebula, which is a planetary nebula. A fast wind from the remaining stellar core rams into the ejected atmosphere and pushes it outward, creating wispy structures seen in X-rays by Chandra and optical light by the Hubble Space Telescope.

Chandra Spacecraft

Chandra Spacecraft: A quarter of a century ago, scientists began a quest to answer some of the biggest questions in the Universe. They have discovered many truths — and uncovered even more mysteries. Since it was launched into space in July 1999, NASA’s Chandra X-ray Observatory has changed our view of the Universe. With this telescope, we continue to see what is otherwise invisible. We are still learning, exploring, and expanding humanity’s grasp of what the Universe has to offer. Our X-ray legacy continues.



Visual Description:

This image contains four separate images presented in a 2 by 2 grid. Top left, Vela pulsar. Top right, Tycho's Supernova Remnant. Bottom left, Helix Nebula. Bottom right, Cat's Eye Nebula.

The Vela Pulsar, the aftermath of a collapsed and exploded star sending a jet of particles into space. The pulsar resembles a soft, pillowy, lavender bean in a pocket of blue gas. A faint stream of gas, the X-ray jet, appears to shoot from the pocket, heading into the distance at our upper right. Purple markings in the lavender bean shape strongly resemble narrow eyes and an open mouth, giving the pulsar a squinting happy face. In this image, X-ray light detected by Chandra is shown in blues and purples.

The Tycho supernova remnant is a spherical cloud of reds, greens, and blues set against a starry sky. The cloud is ejected material still propagating from a star that exploded in 1572, as seen from Earth. Here, the supernova resembles a fluffy pink cotton ball. The dense, translucent cloud is streaked with hazy veins, and mottled with red and blue. The edges of the cloud appear to be highlighted in soft white. Upon close inspection, a thin red-violet line can be discerned around the outer edge of the multicolored cloud. The red-violet line shows where electrons have been accelerated to high energies, producing X-rays detected by Chandra. This provides evidence that supernova remnants are a major source of energetic particles, including electrons and protons, which continually hit Earth's atmosphere.

The Helix Nebula is a planetary nebula, the end phases of the life of a Sun-like star. Helix resembles a creature's eye, both in shape and in detail. At the center of the nebula, where the pupil would reside, an orb shaped cloud glows in dark pink. Surrounding the orb, where the colored iris of an eye would be, is a dramatic mix of color in blues, browns, and golds that appear somewhat striated, very similar to a human eye. These striations extend to the left and right of the otherwise circular iris structure, as though they had been gently pulled from the two o'clock and seven o'clock positions until the material formed faint wisps. Surrounding the iris structure are roughly spherical puffs of blue haze. The entire canvas is dotted with stars in red, green, and blue.

The Cat's Eye Nebula is an image of an ethereal shape surrounded by concentric circles. The shape is a huge cloud of gas and dust blown off of a dying star. The concentric circles are bubbles expelled by the star over time. The dust cloud resembles a translucent pastry pulled to golden yellow points near our upper right and lower left, with a blob of bright purple jelly inside the bulbous pale blue core. The jelly-like center represents X-ray data from Chandra. The outer cloud and translucent circles represent visible light data from the Hubble Space Telescope.



Fast Facts for Vela Pulsar:

Credit: X-ray: NASA/CXC/SAO; Optical: NASA/ESA/STScI; Image processing: NASA/CXC/SAO/J. Schmidt, K. Arcand
Scale: Image is about 4.8 arcmin (1.4 light-years) across
Category: Neutron Stars & X-ray Binaries
Coordinates (J2000): RA 08h 35m 20.60s | -45° 10' 35.00"
Constellation: Vela
Observation Date(s): 8 pointings between June and September 2010
Observation Time: 89 hours (3 days 17 hours)
Obs. IDs: 10135-10139, 12073-12075
Instrument: ACIS
Color Code: X-ray: purple (Chandra), light blue (IXPE); Optical: yellow (Hubble)
Distance Estimate: About 1,000 light-years



Fast Facts for Tycho's Supernova Remnant:

Credit: X-ray: NASA/CXC/SAO; Optical: DSS; Image Processing: NASA/CXC/SAO/N. Wolk
Scale: Image is about 12 arcmin (45 light-years) across
Category: Supernovas & Supernova Remnants
Coordinates (J2000): RA 00h 25m 17s | Dec 64° 08' 37"
Constellation: Cassiopeia
Observation Date(s): 14 pointings between Oct 1, 2001 and April 22, 2016
Observation Time: 336 hours (14 days 0 hours 2 min)
Obs. IDs: 115, 3837, 7539, 8551, 10093-10097, 10902-10904, 10906, 15998
Instrument: ACIS
Color Code: X-ray Broadband: red: 0.3-1.2 keV, yellow: 1.2-1.6 keV, cyan: 1.6-2.26 keV, navy: 2.2-4.1 keV, purple: 4.4-6.1 keV; X-ray Motion Shift: orange: 1.7666-1.7812 keV, blue: 1.9564-1.971 keV; Optical: red and blue
Distance Estimate: About 13,000 light-years



Facts for Helix Nebula:

Credit: X-ray: NASA/CXC/SAO; UV: NASA/JPL-Caltech/SSC; Optical: NASA/ STScI/M. Meixner, ESA/NRAO/T.A. Rector; Infrared:NASA/JPL-Caltech/K. Su; Image Processing: NASA/CXC/SAO/N. Wolk and K. Arcand
Scale: Image is about 30 arcmin (5.6 light-years) across
Category: White Dwarfs & Planetary Nebulas
Coordinates (J2000): RA 22h 29m 38.55s | Dec -20° 50' 13.6"
Constellation: Aquarius
Observation Date(s): 2 pointings Nov 17 & 18, 1999
Observation Time: 13 hours and 26 minutes
Obs. IDs: 631, 1480
Instrument: ACIS
Color Code: X-ray: purple; UV: light blue; Optical: red, green, and blue; IR: aqua and red
Distance Estimate: About 650 light-years



Facts for Cat's Eye Nebula:

Credit: X-ray: NASA/CXC/SAO; Optical: NASA/ESA/STScI; Image Processing: NASA/CXC/SAO/J. Major, L. Frattare, K. Arcand
Scale: Image is about 1.7 arcmin (1.5 light-years) across
Category: White Dwarfs & Planetary Nebulas
Coordinates (J2000): RA 17h 58m 33.5s | Dec +66° 37' 59.5"
Constellation: Draco
Observation Date(s): May 10, 2000
Observation Time: 12 hours 48 minutes
Obs. IDs: 630
Instrument: ACIS
Color Code: X-ray: magenta; Optical: red, green, and blue;
Distance Estimate: About 3,000 light-years


Wednesday, April 24, 2024

Hubble Celebrates 34th Anniversary with a Look at the Little Dumbbell Nebula

Little Dumbbell Nebula (WFC3 Image)
Credits: Image: NASA, ESA, STScI




In celebration of the 34th anniversary of the launch of NASA's legendary Hubble Space Telescope on April 24, astronomers took a snapshot of the Little Dumbbell Nebula (also known as Messier 76, M76, or NGC 650/651) located 3,400 light-years away in the northern circumpolar constellation Perseus. The photogenic nebula is a favorite target of amateur astronomers.

M76 is classified as a planetary nebula, an expanding shell of glowing gases that were ejected from a dying red giant star. The star eventually collapses to an ultra-dense and hot white dwarf. A planetary nebula is unrelated to planets, but have that name because astronomers in the 1700s using low-power telescopes thought this type of object resembled a planet.

M76 is composed of a ring, seen edge-on as the central bar structure, and two lobes on either opening of the ring. Before the star burned out, it ejected the ring of gas and dust. The ring was probably sculpted by the effects of the star that once had a binary companion star. This sloughed off material created a thick disk of dust and gas along the plane of the companion's orbit. The hypothetical companion star isn't seen in the Hubble image, and so it could have been later swallowed by the central star. The disk would be forensic evidence for that stellar cannibalism.

The primary star is collapsing to form a white dwarf. It is one of the hottest stellar remnants known at a scorching 250,000 degrees Fahrenheit, 24 times our Sun's surface temperature. The sizzling white dwarf can be seen as a pinpoint in the center of the nebula. A star visible in projection beneath it is not part of the nebula.

Pinched off by the disk, two lobes of hot gas are escaping from the top and bottom of the "belt," along the star's rotation axis that is perpendicular to the disk. They are being propelled by the hurricane-like outflow of material from the dying star, tearing across space at two million miles per hour. That's fast enough to travel from Earth to the Moon in a little over seven minutes! This torrential "stellar wind" is plowing into cooler, slower-moving gas that was ejected at an earlier stage in the star's life, when it was a red giant. Ferocious ultraviolet radiation from the super-hot star is causing the gases to glow. The red color is from nitrogen, and blue is from oxygen.

Given our solar system is 4.6 billion years old, the entire nebula is a flash in the pan by cosmological timekeeping. It will vanish in about 15,000 years.

HUBBLE'S STAR TREKKING

Since its launch in 1990 Hubble has made 1.6 million observations of over 53,000 astronomical objects. To date, the Mikulski Archive for Space Telescopes at the Space Telescope Science Institute in Baltimore, Maryland holds 184 terabytes of processed data that is science-ready for astronomers around the world to use for research and analysis. Since 1990, 44,000 science papers have been published from Hubble observations. The space telescope is the most scientifically productive space astrophysics mission in NASA history. The demand for using Hubble is so high it is currently oversubscribed by a factor of six-to-one.

Most of Hubble's discoveries were not anticipated before launch, such as supermassive black holes, the atmospheres of exoplanets, gravitational lensing by dark matter, the presence of dark energy, and the abundance of planet formation among stars.

Hubble will continue research in those domains and capitalize on its unique ultraviolet-light capability on such topics as solar system phenomena, supernovae outbursts, composition of exoplanet atmospheres, and dynamic emission from galaxies. And Hubble investigations continue to benefit from its long baseline of observations of solar system objects, stellar variable phenomena and other exotic astrophysics of the cosmos.

NASA's James Webb Space Telescope was designed to be meant to be complementary to Hubble, and not a substitute. Future Hubble research also will take advantage of the opportunity for synergies with Webb, which observes the universe in infrared light. The combined wavelength coverage of the two space telescopes expands on groundbreaking research in such areas as protostellar disks, exoplanet composition, unusual supernovae, cores of galaxies and chemistry of the distant universe.

The Hubble Space Telescope has been operating for over three decades and continues to make ground-breaking discoveries that shape our fundamental understanding of the universe. Hubble is a project of international cooperation between NASA and ESA (European Space Agency). NASA's Goddard Space Flight Center in Greenbelt, Maryland, manages the telescope and mission operations. Lockheed Martin Space, based in Denver, Colorado, also supports mission operations at Goddard. The Space Telescope Science Institute in Baltimore, Maryland, which is operated by the Association of Universities for Research in Astronomy, conducts Hubble science operations for NASA.




About This Release

Credits:

Release: NASA, ESA, STScI

Media Contact:

Ray Villard
Space Telescope Science Institute, Baltimore, Maryland

Permissions: Content Use Policy

Contact Us: Direct inquiries to the News Team.

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Tuesday, April 23, 2024

Hubble Goes Hunting for Small Main Belt Asteroids

Wayward Asteroid Photobombs Hubble Snapshot of Galaxy UGC 12158
Credits: Image: NASA, ESA, Pablo García Martín (UAM)
Image Processing: Joseph DePasquale (STScI)
Acknowledgment: Alex Filippenko (UC Berkeley)

Size Distribution for Unknown Asteroids in Hubble Asteroid Hunter Survey
Credits: Illustration: Pablo García Martín (UAM), Elizabeth Wheatley (STScI)




Like boulders, rocks, and pebbles scattered across a landscape, asteroids come in a wide range of sizes. Cataloging asteroids in space is tricky because they are faint and they don't stop to be photographed as they zip along their orbits around the Sun.

Astronomers recently used a trove of archived images taken by NASA's Hubble Space Telescope to visually snag a largely unseen population of smaller asteroids in their tracks. The treasure hunt required perusing 37,000 Hubble images spanning 19 years. The payoff was finding 1,701 asteroid trails, with 1,031 of the asteroids previously uncatalogued. About 400 of these uncatalogued asteroids are below 1 kilometer in size.

Volunteers from around the world known as "citizen scientists" contributed to the identification of this asteroid bounty. Professional scientists combined the volunteers' efforts with machine learning algorithm to identify the asteroids. It represents a new approach to finding asteroids in astronomical archives spanning decades, which may be effectively applied to other datasets, say the researchers.

"We are getting deeper into seeing the smaller population of main belt asteroids. We were surprised with seeing such a large number of candidate objects," said lead author Pablo García Martín of the Autonomous University of Madrid, Spain. "There was some hint of this population existing, but now we are confirming it with a random asteroid population sample obtained using the whole Hubble archive. This is important for providing insights into the evolutionary models of our solar system."

The large, random sample offers new insights into the formation and evolution of the asteroid belt. Finding a lot of small asteroids favors the idea that they are fragments of larger asteroids that have collided and broken apart, like smashed pottery. This is a grinding-down process spanning billions of years.

An alternative theory for the existence of smaller fragments is that they formed that way billions of years ago. But there is no conceivable mechanism that would keep them from snowballing up to larger sizes as they agglomerated dust from the planet-forming circumstellar disk around our Sun. "Collisions would have a certain signature that we can use to test the current main belt population," said co-author Bruno Merín of the European Space Astronomy Centre, in Madrid, Spain.

Amateur Astronomers Teach AI to Find Asteroids

Because of Hubble's fast orbit around the Earth, it can capture wandering asteroids through their telltale trails in the Hubble exposures. As viewed from an Earth-based telescope, an asteroid leaves a streak across the picture. Asteroids "photobomb" Hubble exposures by appearing as unmistakable, curved trails in Hubble photographs.

As Hubble moves around the Earth, it changes its point of view while observing an asteroid, which also moves along its own orbit. By knowing the position of Hubble during the observation and measuring the curvature of the streaks, scientists can determine the distances to the asteroids and estimate the shapes of their orbits.

The asteroids snagged mostly dwell in the main belt, which lies between the orbits of Mars and Jupiter. Their brightness is measured by Hubble's sensitive cameras. And comparing their brightness to their distance allows for a size estimate. The faintest asteroids in the survey are roughly one forty-millionth the brightness of the faintest star that can be seen by the human eye.

"Asteroid positions change with time, and therefore you cannot find them just by entering coordinates, because at different times, they might not be there," said Merín. "As astronomers we don't have time to go looking through all the asteroid images. So we got the idea to collaborate with over 10,000 citizen-science volunteers to peruse the huge Hubble archives."

In 2019 an international group of astronomers launched the Hubble Asteroid Hunter, a citizen-science project to identify asteroids in archival Hubble data. The initiative was developed by researchers and engineers at the European Science and Technology Centre (ESTEC) and the European Space Astronomy Centre's science data center (ESDC), in collaboration with the Zooniverse platform, the world's largest and most popular citizen-science platform, and Google.

A total of 11,482 citizen-science volunteers, who provided nearly 2 million identifications, were then given a training set for an automated algorithm to identify asteroids based on artificial intelligence. This pioneering approach may be effectively applied to other datasets.

The project will next explore the streaks of previously unknown asteroids to characterize their orbits and study their properties, such as rotation periods. Because most of these asteroid streaks were captured by Hubble many years ago, it is not possible to follow them up now to determine their orbits.

The findings are are published in the journal Astronomy and Astrophysics.

To learn how you can participate in citizen science projects related to NASA, visit https://science.nasa.gov/citizen-science/. Participation is open to everyone around the world, not limited to U.S. citizens or residents.

The Hubble Space Telescope has been operating for over three decades and continues to make ground-breaking discoveries that shape our fundamental understanding of the universe. Hubble is a project of international cooperation between NASA and ESA (European Space Agency). NASA's Goddard Space Flight Center in Greenbelt, Maryland, manages the telescope and mission operations. Lockheed Martin Space, based in Denver, Colorado, also supports mission operations at Goddard. The Space Telescope Science Institute (STScI) in Baltimore, Maryland, which is operated by the Association of Universities for Research in Astronomy, conducts Hubble science operations for NASA.




About This Release:

Credits:

Media Contact:

Ray Villard
Space Telescope Science Institute, Baltimore, Maryland

Science Contact

Pablo García Martín
Autonomous University of Madrid, Madrid, Spain

Permissions: Content Use Policy

Contact Us: Direct inquiries to the team.

Related Links and Documents


Monday, April 22, 2024

Twinkle Twinkle Baby Star, ‘Sneezes’ Tell us How You Are

Artist’s conception of a ‘sneeze’ of magnetic field lines, dust, and gas ejected from a baby star.
Credit: ALMA (ESO/NAOJ/NRAO)).
Download image (1.6MB)



Astronomers have discovered the remnants of powerful ‘sneezes’ expelling gas, dust, and electromagnetic energy around stars in the process of forming. The team believes these sneezes help the baby star expel excess magnetic flux, and as such may play a vital role in enabling the star to form.

A star forms from a cloud of gas and dust. Interstellar magnetic field lines pass through these clouds. As the cloud contracts to form the star, the magnetic field lines get pulled along. But observations of young stars show that most of this magnetic energy is lost during the formation process. The question is, where does it go?

Looking for the answer to this question, a team led by Kazuki Tokuda, an astronomer affiliated with NAOJ and Kyushu University, used ALMA (Atacama Large Millimeter/submillimeter Array) to study one of the clouds with a baby star, known as Taurus Dense Core MC 27. This stellar nursery is located approximately 450 light-years from Earth in the direction of the constellation Taurus.

One of the leading theories was that the magnetic field gradually weakened over time as the baby star grew. But as Tokuda explains, “As we analyzed our data, we found something quite unexpected. There were these ‘spike-like’ structures extending a few astronomical units from the protostellar disk. As we dug in deeper, we found that these were spikes of expelled magnetic flux, dust, and gas.”

Tokuda continues, “This is a phenomenon called ‘interchange instability’ where instabilities in the magnetic field react with the different densities of the gases in the protostellar disk, resulting in an outward expelling of magnetic flux. We dubbed this a baby star’s ‘sneeze’ as it reminded us of when we expel dust and air at high speeds.”

Additionally, other spikes were observed several thousands of astronomical units away from the protostellar disk. The team hypothesizes that these were indications of past ‘sneezes.’ And similar spike-like structures have been observed in other young stars, indicating that they may be ubiquitous. These sneezes could help explain how baby stars shed excess magnetic energy and might be a vital part of the star formation process.




Detailed Article(s)


Kyushu University



Release Information

Researcher(s) Involved in this Release

Kazuki Tokuda (Department of Earth and Planetary Science, Faculty of Science, Kyushu University / National Astronomical Observatory of Japan)


Coordinated Release Organization(s)

Kyushu University
National Astronomical Observatory of Japan


Paper(s)

Kazuki Tokuda et al. “Discovery of Asymmetric Spike-like Structures of the 10 au Disk around the Very Low-luminosity Protostar Embedded in the Taurus Dense Core MC 27/L1521F with ALMA”, in The Astrophysical Journal, DOI: 10.3847/1538-4357/ad2f9a



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Sunday, April 21, 2024

Unusually Lightweight Black Hole Candidate Spotted by LIGO

The image shows the coalescence and merger of a lower mass-gap black hole (dark gray surface) with a neutron star (greatly tidally deformed by the black hole's gravity). This still image from a simulation of the merger highlights just the neutron star's lower density components, ranging from 60 grams per cubic centimeter (dark blue) to 600 kilograms per cubic centimeter (white). Its shape highlights the strong deformations of the low-density material of the neutron star Credit: Ivan Markin, Tim Dietrich (University of Potsdam), Harald Paul Pfeiffer, Alessandra Buonanno (Max Planck Institute for Gravitational Physics)

In May 2023, shortly after LIGO (Laser Interferometer Gravitational-wave Observatory) turned back on for its fourth run of observations, it detected a gravitational-wave signal from the collision of an object, most likely a neutron star, with a suspected black hole possessing a mass that is 2.5 to 4.5 times more than that of our Sun. This signal, called GW230529, is intriguing to researchers because the candidate black hole's mass falls within a so-called mass gap between the heaviest known neutron stars, which are slightly more than two solar masses, and the lightest known black holes, which are about five solar masses. While the gravitational-wave signal alone cannot reveal the true nature of this object, future detections of similar events, especially those accompanied by bursts of light, could hold the key to answering the question of how lightweight black holes can be.

"The latest finding demonstrates the impressive science capability of the gravitational-wave detector network, which is significantly more sensitive than it was in the third observing run," says Jenne Driggers (PhD '15), detection lead scientist at LIGO Hanford in Washington, one of two facilities, along with LIGO Livingston in Louisiana, that make up the LIGO Observatory.

LIGO made history in 2015 after carrying out the first direct detection of gravitational waves in space. Since then, LIGO and its partner detector in Europe, Virgo, have detected nearly 100 mergers between black holes, a handful between neutron stars, as well as mergers between neutron stars and black holes. The Japanese detector KAGRA joined the gravitational-wave network in 2019, and the team of scientists who collectively analyze data from all three detectors is known as the LIGO–Virgo–KAGRA (LVK) collaboration. The LIGO observatories are funded by the National Science Foundation (NSF), and were conceived, built, and are operated by Caltech and MIT.<

The latest finding also indicates that collisions involving lightweight black holes may be more common than previously believed.

"This detection, the first of our exciting results from the fourth LIGO–Virgo–KAGRA observing run, reveals that there may be a higher rate of similar collisions between neutron stars and low mass black holes than we previously thought," says Jess McIver, an assistant professor at the University of British Columbia, deputy spokesperson of the LIGO Scientific Collaboration, and a former postdoctoral fellow at Caltech.

Prior to the GW230529 event, one other intriguing mass-gap candidate object had been identified. In that event, which took place in August 2019 and is known as GW190814, a compact object of 2.6 solar masses was found as part of a cosmic collision, but scientists are not sure if it was a neutron star or black hole.

After a break for maintenance and upgrades, the detectors' fourth observing run will resume on April 10, 2024, and will continue until February 2025.

The preprint GW230529 study titled, "Observation of Gravitational Waves from the Coalescence of a 2.5-4.5 M_\odot Compact Object and a Neutron Star," has been posted online.

Read the full story from the LVK collaboration.

Source: Caltech/News



Contact:

>Whitney Clavin
(626) 395‑1944

wclavin@caltech.edu


Saturday, April 20, 2024

‘Swallowed’, torn up or live on: How Earth will fare when the Sun dies

Clumps of debris from a disrupted planetesimal are irregularly spaced on a long and eccentric orbit around the white dwarf. Individual clouds of rubble intermittently pass in front of the white dwarf, blocking some of its light. Because of the various sizes of the fragments in these clumps, the brightness of the white dwarf flickers in a chaotic way.Credit:Dr Mark Garlick/The University of Warwick

Licence type: Attribution (CC BY 4.0)

Our solar system and everything within it - including the Earth - will look very different when the Sun dies.

But whether the planet we call home is “swallowed” up by our dying star or manages to escape its clutches, only time will tell.

The inner planets Mercury and Venus will almost certainly be crushed and engulfed by the Sun, according to a new paper published today in the Monthly Notices of the Royal Astronomical Society (MNRAS).

But even if Earth does outlive its star, unfortunately it still wouldn’t be habitable. On the plus side, it would at least fare better than some of Jupiter’s moons, which an international team of astrophysicists say could be dislodged and shredded as the Sun runs out of energy.

They came up with the terrifying prophecy of what our solar system may look like five billion years from now after studying what happens to planetary systems like our own when their host stars become white dwarfs.

“Whether or not the Earth can just move out fast enough before the Sun can catch up and burn it is not clear, but [if it does] the Earth would [still] lose its atmosphere and ocean and not be a very nice place to live,” explained Professor Boris Gaensicke, of the University of Warwick.

If our planet was engulfed by the Sun, along with Venus and Mercury, this would leave Mars and the four gas giants - Jupiter, Saturn, Uranus and Neptune - orbiting what would ultimately be a white dwarf.

Surviving asteroids and smaller moons would then likely be ripped apart and ground to dust before falling into the dead star, the team of researchers said. Currently the Sun is burning hydrogen at its core, but once this is used up it will expand and become a red giant, before ending up as a white dwarf – the end state of stars when they have burned all their fuel.

Studying white dwarfs is useful because it offers an insight into different aspects of star formation and evolution.

SUMMARY: 'Long-term variability in debris transiting white dwarfs'

Researchers in this study wanted to know what happens to asteroids, moons and planets that pass close to white dwarfs.

What they found is that the fate of these bodies is likely to be extremely violent and catastrophic. They came to this conclusion after analysing the bodies’ transits – dips in the brightness of stars caused by objects passing in front of them.

Unlike the predictable transits caused by orbiting planets around stars, transits caused by debris are oddly shaped, chaotic and disorderly

Lead researcher Dr Amornrat Aungwerojwit, of Naresuan University in Thailand, said: “Previous research had shown that when asteroids, moons and planets get close to white dwarfs, the huge gravity of these stars rips these small planetary bodies into smaller and smaller pieces.”

Collisions between these pieces eventually grind them to dust, which then falls into the white dwarf, enabling researchers to determine what type of material the original planetary bodies were made from.

In this new research, scientists analysed changes in the brightness of stars for 17 years, shedding insight into how these bodies are disrupted. They focused on three different white dwarfs which all behaved very differently.

Professor Gaensicke said: “The simple fact that we can detect the debris of asteroids, maybe moons or even planets whizzing around a white dwarf every couple of hours is quite mind-blowing, but our study shows that the behaviour of these systems can evolve rapidly, in a matter of a few years.

“While we think we are on the right path in our studies, the fate of these systems is far more complex than we could have ever imagined.”

The first white dwarf (ZTF J0328−1219) studied appeared steady and “well behaved” over the last few years, but the authors found evidence for a major catastrophic event around 2010. Another star (ZTF J0923+4236) was shown to dim irregularly every couple of months, and shows chaotic variability on time scales of minutes during these fainter states, before brightening again.

The third white dwarf analysed (WD 1145+017), had been shown by Massachusetts Institute of Technology (MIT) in 2015 to behave close to theoretical predictions, with vast variations in numbers, shapes and depths of transits.

Surprisingly, the transits studied in this research are now gone.

“The system is, overall, very gently getting brighter, as the dust produced by catastrophic collisions around 2015 disperses”, said Professor Gaensicke.

“The unpredictable nature of these transits can drive astronomers crazy – one minute they are there, the next they are gone. And this points to the chaotic environment they are in.”

When asked about the fate of our own solar system, Professor Gaensicke, said: “The sad news is that the Earth will probably just be swallowed up by an expanding Sun, before it becomes a white dwarf.

“For the rest of the solar system, some of the asteroids located between Mars and Jupiter, and maybe some of the moons of Jupiter may get dislodged and travel close enough to the eventual white dwarf to undergo the shredding process we have investigated.”

The paper 'Long-term variability in debris transiting white dwarfs' has been published today in MNRAS.




Media contacts

Sam Tonkin
Royal Astronomical Society
Mob: +44 (0)7802 877700

press@ras.ac.uk

Robert Massey
Royal Astronomical Society
Mob: +44 (0)7802 877699

press@ras.ac.uk

Annie Slinn
University of Warwick
Mob: +44 (0)7392 125 605

annie.slinn@warwick.ac.uk



Science contacts

Professor Boris Gaensicke
University of Warwick
Tel: +60 18 204 3100

boris.gaensicke@warwick.ac.uk

Dr Sukuny Ross
Naresuan University

sukunyaj@nu.ac.th



Further information

The new study 'Long-term variability in debris transiting white dwarfs', Amornrat Aungwerojwit et al., has been published in Monthly Notices of the Royal Astronomical Society.




Notes for editors

About the Royal Astronomical Society

The Royal Astronomical Society (RAS), founded in 1820, encourages and promotes the study of astronomy, solar-system science, geophysics and closely related branches of science. The RAS organises scientific meetings, publishes international research and review journals, recognises outstanding achievements by the award of medals and prizes, maintains an extensive library, supports education through grants and outreach activities and represents UK astronomy nationally and internationally. Its more than 4,000 members (Fellows), a third based overseas, include scientific researchers in universities, observatories and laboratories as well as historians of astronomy and others.

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

Keep up with the RAS on
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Friday, April 19, 2024

Rubin Observatory Will Reveal Dark Matter’s Ghostly Disruptions of Stellar Streams

PR Image noirlab2409a
Artist’s Impression: Stellar streams in and around the Milky Way

PR Image noirlab2409b
Rubin Observatory Under the Milky Way



Videos

Nora Shipp discusses how Rubin Observatory will contribute to the study of stellar streams
PR Video noirlab2409a
Nora Shipp discusses how Rubin Observatory will contribute to the study of stellar streams

Nora Shipp comenta sobre la forma en que Rubin contribuirá al estudio de las corrientes estelares
PR Video noirlab2409b
Nora Shipp comenta sobre la forma en que Rubin contribuirá al estudio de las corrientes estelares



Vera C. Rubin Observatory’s stunningly detailed images will illuminate distant stellar streams and their past encounters with dark matter

Glittering threads of stars around the Milky Way may hold answers to one of our biggest questions about the Universe: what is dark matter? With images taken through six different color filters mounted to the largest camera ever built for astronomy and astrophysics, Vera C. Rubin Observatory’s upcoming Legacy Survey of Space and Time will reveal never-before-seen stellar streams around the Milky Way — and the telltale effects of their interactions with dark matter.

As mesmerizing as rivers that glitter in sunlight, stellar streams trace sparkling arcs through and around our home galaxy — the Milky Way. Stellar streams are composed of stars that were originally bound in globular clusters or dwarf galaxies, but have been disrupted by gravitational interactions with our galaxy and drawn into long, trailing lines. These slender trails of stars often show signs of disturbance, and scientists suspect that in many cases dark matter is the culprit. Vera C. Rubin Observatory, jointly funded by the U.S. National Science Foundation (NSF) and the U.S. Department of Energy (DOE), will soon provide a wealth of data to illuminate stellar streams, dark matter, and their complex interactions.

Dark matter makes up 27% of the Universe, but it can’t be observed directly, and scientists currently don’t know exactly what it is. To learn more, they use a variety of indirect methods to investigate its nature. Some methods, like weak gravitational lensing, map the distribution of dark matter on large scales across the Universe. Observing stellar streams allows scientists to probe a different aspect of dark matter because they showcase the fingerprint of dark matter’s gravitational effects at small scales.

Vera C. Rubin Observatory, located in Chile, will use an 8.4-meter telescope equipped with the largest digital camera in the world to conduct a 10-year survey of the entire southern hemisphere sky beginning in late 2025. The resulting data, with images taken through six different color filters, will make it easier than ever for scientists to isolate stellar streams among and beyond the Milky Way and examine them for signs of dark matter disruption. “I'm really excited about using stellar streams to learn about dark matter,” said Nora Shipp, a postdoctoral fellow at Carnegie Mellon University and co-convener of the Dark Matter Working Group in the Rubin Observatory/LSST Dark Energy Science Collaboration. “With Rubin Observatory we’ll be able to use stellar streams to figure out how dark matter is distributed in our galaxy from the largest scales down to very small scales.

Rubin Observatory will begin science operations in late 2025. Rubin Observatory is a Program of NSF NOIRLab, which, along with SLAC National Accelerator Laboratory, will jointly operate Rubin.

Evidence suggests that a spherical halo of dark matter surrounds the Milky Way, made up of smaller dark matter clumps. These clumps interact with other structures, disrupting their gravitational dynamics and changing their observed appearance. In the case of stellar streams, the results of dark matter interactions appear as kinks or gaps in the starry trails.

Rubin Observatory’s incredibly detailed images will make it possible for scientists to identify and examine very subtle irregularities in stellar streams, and thus infer the properties of the low-mass dark matter clumps that caused them — even narrowing down what types of particles these clumps are made of. “By observing stellar streams, we’ll be able to take indirect measurements of the Milky Way's dark matter clumps down to masses lower than ever before, giving us really good constraints on the particle properties of dark matter,” said Shipp.

Stellar streams in the outer regions of the Milky Way are especially good candidates for observing the effects of dark matter because they’re less likely to have been affected by interactions with other parts of the Milky Way, which can confuse the picture. Rubin Observatory will be able to detect stellar streams at a distance of about five times farther than we can see now, allowing scientists to discover and observe an entirely new population of stellar streams in the Milky Way’s outer regions.

Stellar streams are challenging to distinguish from the many other stars of the Milky Way. To isolate stellar streams scientists search for stars with specific properties that indicate they likely belonged together as globular clusters or dwarf galaxies. They then analyze the motion or other properties of these stars to identify those connected as a stream.

“Stellar streams are like strings of pearls, whose stars trace the path of the system’s orbit and have a shared history,” said Jaclyn Jensen, a PhD candidate at the University of Victoria who plans to use Rubin/LSST data for her research on the progenitors of stellar streams and their role in the formation of the Milky Way. “Using properties of these stars, we can determine information about their origins and what kind of interactions the stream may have experienced. If we find a pearl necklace with a few scattered pearls nearby, we can deduce that something may have come along and broken the string.”

Rubin Observatory’s 3200-megapixel LSST Camera is equipped with six color filters — including, notably for stellar stream scientists like Shipp and Jensen, an ultraviolet filter. Rubin’s ultraviolet filter will provide critical information on the blue-ultraviolet end of the light spectrum that will enable scientists to distinguish the subtle differences and untangle the stars in a stream from look-alike stars in the Milky Way. Overall, Rubin will provide scientists with thousands of deep images taken through all six filters, giving them a clearer view of stellar streams than ever before.

The avalanche of data that Rubin will provide will also inspire new tools and methods for isolating stellar streams. As Shipp notes, “Right now it’s a labor-intensive process to pick out potential streams by eye — Rubin’s large volume of data presents an exciting opportunity to think of new, more automated ways to identify streams.




More information

Rubin Observatory is a joint initiative of the U.S. National Science Foundation (NSF) and the Department of Energy (DOE). Its primary mission is to carry out the Legacy Survey of Space and Time, providing an unprecedented data set for scientific research supported by both agencies. Rubin is operated jointly by NSF NOIRLab and SLAC National Accelerator Laboratory (SLAC). NOIRLab is managed for NSF by the Association of Universities for Research in Astronomy (AURA) and SLAC is operated for DOE by Stanford University. France provides key support to the construction and operations of Rubin Observatory through contributions from CNRS/IN2P3. Additional contributions from a number of international organizations and teams are acknowledged.

The U.S. National Science Foundation (NSF) is an independent federal agency created by Congress in 1950 to promote the progress of science. NSF supports basic research and people to create knowledge that transforms the future.

NSF NOIRLab (U.S. National Science Foundation National Optical-Infrared Astronomy Research Laboratory), the U.S. center for ground-based optical-infrared astronomy, operates the International Gemini Observatory (a facility of NSF, NRC–Canada, ANID–Chile, MCTIC–Brazil, MINCyT–Argentina, and KASI–Republic of Korea), Kitt Peak National Observatory (KPNO), Cerro Tololo Inter-American Observatory (CTIO), the Community Science and Data Center (CSDC), and Vera C. Rubin Observatory (in cooperation with DOE’s SLAC National Accelerator Laboratory). It is managed by the Association of Universities for Research in Astronomy (AURA) under a cooperative agreement with NSF and is headquartered in Tucson, Arizona. The astronomical community is honored to have the opportunity to conduct astronomical research on I’oligam Du’ag (Kitt Peak) in Arizona, on Maunakea in Hawai‘i, and on Cerro Tololo and Cerro Pachón in Chile. We recognize and acknowledge the very significant cultural role and reverence that these sites have to the Tohono O’odham Nation, to the Native Hawaiian community, and to the local communities in Chile, respectively.

SLAC National Accelerator Laboratory is a vibrant multiprogram laboratory that explores how the Universe works at the biggest, smallest, and fastest scales and invents powerful tools used by scientists around the globe. With research spanning particle physics, astrophysics and cosmology, materials, chemistry, bio- and energy sciences and scientific computing, SLAC helps solve real-world problems and advance the interests of the nation.

SLAC is operated by Stanford University for the U.S. Department of Energy’s Office of Science. The Office of Science is the single largest supporter of basic research in the physical sciences in the United States and is working to address some of the most pressing challenges of our time.




Links



Contacts

Nora Shipp
Postdoctoral fellow at Carnegie Mellon University
Co-convener of the Dark Matter Working Group in the Rubin/LSST Dark Energy Science Collaboration.
Email:
nshipp@uw.edu

Kristen Metzger
Communications Manager for Education and Public Outreach, Rubin Observatory
Email:
kristen.metzger@noirlab.edu

Bob Blum
Director for Operations, Vera C. Rubin Observatory, NSF NOIRLab
Tel: +1 520-318-8233
Email:
bob.blum@noirlab.edu

Željko Ivezić
Director of Rubin Construction
Professor of Astronomy, University of Washington/AURA
Tel: +1-206-403-6132
Email:
ivezic@uw.edu

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

Manuel Gnida
Media Relations Manager, SLAC National Accelerator Laboratory
Tel: +1 650-926-2632 (office)
Cell: +1 415-308-7832 (cell)
Email:
mgnida@slac.stanford.edu


The eponymous NGC 3783

A spiral galaxy, seen face-on to the viewer. The bright centre of the galaxy is crossed by a glowing bar, and it is surrounded by tightly-wound spiral arms, forming a circular shape with relatively clear edges. Faraway galaxies can be seen around it, along with a few bright stars, on a dark background. One star to the right of the galaxy is very large and extremely bright with long diffraction spikes around it. Credit:  ESA/Hubble & NASA, M. C. Bentz, D. J. V. Rosario

This image features NGC 3783, a bright barred spiral galaxy about 130 million light-years from Earth, that also lends its name to the eponymous NGC 3783 galaxy group. Like galaxy clusters, galaxy groups are aggregates of gravitationally bound galaxies. Galaxy groups, however, are less massive and contain fewer members than galaxy clusters do: where galaxy clusters can contain hundreds or even thousands of constituent galaxies, galaxy groups do not typically include more than 50. The Milky Way is actually part of a galaxy group, known as the Local Group, which contains two other large galaxies (Andromeda and the Triangulum galaxy), as well as several dozen satellite and dwarf galaxies. The NGC 3783 galaxy group, meanwhile, contains 47 galaxies. It also seems to be at a fairly early stage of its evolution, making it an interesting object of study.

Whilst the focus of this image is the spiral galaxy NGC 3783, the eye is equally drawn to the very bright object in the lower right part of this image. This is the star HD 101274. The perspective in this image makes the star and the galaxy look like close companions, but this is an illusion. HD 101274 lies only about 1530 light-years from Earth, meaning it is about 85 thousand times closer than NGC 3783. This explains how a single star can appear to outshine an entire galaxy!

NGC 3783 is a type-1 Seyfert galaxy, which is a galaxy with a bright central region — so it’s particularly bright itself, as far as galaxies go. In this image it is recorded by Hubble in incredible detail, from its glowing central bar to its narrow, winding arms and the dust threaded through them, thanks to five separate images taken in different wavelengths of light. In fact, the galactic centre is bright enough to Hubble that it exhibits diffraction spikes, normally only seen on stars such as HD 101274.



Thursday, April 18, 2024

Most massive stellar black hole in our galaxy found

PR Image eso2408a
Artist’s impression of the system with the most massive stellar black hole in our galaxy

PR Image eso2408b
Comparison of several stellar black holes in our galaxy

PR Image eso2408c
Wide-field view around the BH3 black hole 



Videos

Record-breaking stellar black hole found nearby | ESO News
PR Video eso2408a
Record-breaking stellar black hole found nearby | ESO News

Artist’s animation of the system with the most massive stellar black hole in our galaxy
PR Video eso2408b
Artist’s animation of the system with the most massive stellar black hole in our galaxy

Zooming into the BH3 black hole system
Zooming into the BH3 black hole system

Comparison of several stellar black holes in our galaxy
Comparison of several stellar black holes in our galaxy

Animation showing the locations and distances to some of our galaxy’s black holes
PR Video eso2408e
Animation showing the locations and distances to some of our galaxy’s black holes



Astronomers have identified the most massive stellar black hole yet discovered in the Milky Way galaxy. This black hole was spotted in data from the European Space Agency’s Gaia mission because it imposes an odd ‘wobbling’ motion on the companion star orbiting it. Data from the European Southern Observatory’s Very Large Telescope (ESO’s VLT) and other ground-based observatories were used to verify the mass of the black hole, putting it at an impressive 33 times that of the Sun.

Stellar black holes are formed from the collapse of massive stars and the ones previously identified in the Milky Way are on average about 10 times as massive as the Sun. Even the next most massive stellar black hole known in our galaxy, Cygnus X-1, only reaches 21 solar masses, making this new 33-solar-mass observation exceptional [1].

Remarkably, this black hole is also extremely close to us — at a mere 2000 light-years away in the constellation Aquila, it is the second-closest known black hole to Earth. Dubbed Gaia BH3 or BH3 for short, it was found while the team were reviewing Gaia observations in preparation for an upcoming data release. “No one was expecting to find a high-mass black hole lurking nearby, undetected so far,” says Gaia collaboration member Pasquale Panuzzo, an astronomer from the National Centre for Scientific Research (CNRS) at the Observatoire de Paris - PSL, France. "This is the kind of discovery you make once in your research life."

To confirm their discovery, the Gaia collaboration used data from ground-based observatories, including from the Ultraviolet and Visual Echelle Spectrograph (UVES) instrument on ESO’s VLT, located in Chile’s Atacama Desert [2]. These observations revealed key properties of the companion star, which, together with Gaia data, allowed astronomers to precisely measure the mass of BH3.

Astronomers have found similarly massive black holes outside our galaxy (using a different detection method), and have theorised that they may form from the collapse of stars with very few elements heavier than hydrogen and helium in their chemical composition. These so-called metal-poor stars are thought to lose less mass over their lifetimes and hence have more material left over to produce high-mass black holes after their death. But evidence directly linking metal-poor stars to high-mass black holes has been lacking until now.

Stars in pairs tend to have similar compositions, meaning that BH3’s companion holds important clues about the star that collapsed to form this exceptional black hole. UVES data showed that the companion was a very metal-poor star, indicating that the star that collapsed to form BH3 was also metal-poor — just as predicted.

The research study, led by Panuzzo, is published today in Astronomy & Astrophysics. “We took the exceptional step of publishing this paper based on preliminary data ahead of the forthcoming Gaia release because of the unique nature of the discovery,” says co-author Elisabetta Caffau, also a Gaia collaboration member and CNRS scientist from the Observatoire de Paris - PSL. Making the data available early will let other astronomers start studying this black hole right now, without waiting for the full data release, planned for late 2025 at the earliest.

Further observations of this system could reveal more about its history and about the black hole itself. The GRAVITY instrument on ESO’s VLT Interferometer, for example, could help astronomers find out whether this black hole is pulling in matter from its surroundings and better understand this exciting object.

Source: ESO/News



Notes

[1] This is not the most massive black hole in our galaxy — that title belongs to Sagittarius A*, the supermassive black hole at the Milky Way’s centre, which has about four million times the mass of the Sun. But Gaia BH3 is the most massive black hole known in the Milky Way that formed from the collapse of a star.

[2] Aside from UVES on ESO’s VLT, the study relied on data from: the HERMES spectrograph at the Mercator Telescope operated at La Palma (Spain) by Leuven University, Belgium, in collaboration with the Observatory of the University of Geneva, Switzerland; and the SOPHIE high-precision spectrograph at the Observatoire de Haute-Provence – OSU Institut Pythéas.




More information

This research was presented in a paper entitled “Discovery of a dormant 33 solar-mass black hole in pre-release Gaia astrometry” to appear in Astronomy & Astrophysics (https://aanda.org/10.1051/0004-6361/202449763).

The paper, by P. Panuzzo et al., is authored by the Gaia collaboration, which involves over 300 authors from around the world, including Austria, Belgium, Czechia, Finland, France, Germany, Italy, Netherlands, Poland, Portugal, Spain, Sweden, Switzerland, United Kingdom, Chile and Australia.

The European Southern Observatory (ESO) enables scientists worldwide to discover the secrets of the Universe for the benefit of all. We design, build and operate world-class observatories on the ground — which astronomers use to tackle exciting questions and spread the fascination of astronomy — and promote international collaboration for astronomy. Established as an intergovernmental organisation in 1962, today ESO is supported by 16 Member States (Austria, Belgium, Czechia, Denmark, France, Finland, Germany, Ireland, Italy, the Netherlands, Poland, Portugal, Spain, Sweden, Switzerland and the United Kingdom), along with the host state of Chile and with Australia as a Strategic Partner. ESO’s headquarters and its visitor centre and planetarium, the ESO Supernova, are located close to Munich in Germany, while the Chilean Atacama Desert, a marvellous place with unique conditions to observe the sky, hosts our telescopes. ESO operates three observing sites: La Silla, Paranal and Chajnantor. At Paranal, ESO operates the Very Large Telescope and its Very Large Telescope Interferometer, as well as survey telescopes such as VISTA. Also at Paranal ESO will host and operate the Cherenkov Telescope Array South, the world’s largest and most sensitive gamma-ray observatory. Together with international partners, ESO operates ALMA on Chajnantor, a facility that observes the skies in the millimetre and submillimetre range. At Cerro Armazones, near Paranal, we are building “the world’s biggest eye on the sky” — ESO’s Extremely Large Telescope. From our offices in Santiago, Chile we support our operations in the country and engage with Chilean partners and society.




Links



Contacts

Pasquale Panuzzo
Observatoire de Paris - PSL/CNRS
Paris, France
Tel: +33 1 45 07 78 42
Email:
pasquale.panuzzo@observatoiredeparis.psl.eu

Elisabetta Caffau
Observatoire de Paris - PSL/CNRS
Paris, France
Tel: +33 1 45 07 78 73
Email:
elisabetta.caffau@observatoiredeparis.psl.eu

Bárbara Ferreira
ESO Media Manager
Garching bei München, Germany
Tel: +49 89 3200 6670
Cell: +49 151 241 664 00
Email:
press@eso.org


Wednesday, April 17, 2024

Inexplicable Flying Fox found in Hydra Galaxy Cluster

GMRT radio image of the central region of the Hydra Cluster. The “head” of the Flying Fox discovered this time points to the south-west (lower right). The Flying Fox has a “wingspan” of 220,000 light years. The white contours in the background show the X-ray surface brightness as observed by ESA’s XMM-Newton satellite.(Credit: Kohei Kurahara). Download image (631KB

High sensitivity radio observations have discovered a cloud of magnetized plasma in the Hydra galaxy cluster. The odd location and shape of this plasma defy all conventional explanations. Dubbed the Flying Fox based on its silhouette, this plasma will remain a mystery until additional observations can provide more insight.

A team led by Kohei Kurahara at the National Astronomical Observatory of Japan analyzed observations from the Giant Metrewave Radio Telescope (GMRT) targeting the Hydra galaxy cluster, located over 100 million light years away in the direction of the constellation Hyrda. By applying recent analysis techniques to the GMRT (Giant Metrewave Radio Telescope) data archive, the team was able to discover a cloud of magnetized plasma shaped like a flying fox which has never been reported before.

Radio/optical/IR/X-ray images failed to find a host galaxy at the center of the Flying Fox. This combined with its elongated shape, has left astronomers scratching their heads; the Flying Fox does not fit the model for any known class of objects. New observing facilities, like the Square Kilometre Array currently under construction, are expected to study the Flying Fox and provide new insights into the nature and history of this unusual object.




Detailed Article(s)

Inexplicable Flying Fox found in Hydra Galaxy Cluster
NAOJ Mizusawa



Release Information

Researcher(s) Involved in this Release
Kohei Kurahara (Mizusawa VLBI Observatory, National Astronomical Observatory of Japan)
Takuya Akahori (Mizusawa VLBI Observatory, National Astronomical Observatory of Japan)Yuki Omiya (Department of Physics, Nagoya University)
Kazuhiro Nakazawa (Department of Physics, Nagoya University / Kobayashi-Maskawa Institute for the Origin of Particles and the Universe)




Coordinated Release Organization(s)

National Astronomical Observatory of Japan
Kobayashi-Maskawa Institute for the Origin of Particles and the Universe, Nagoya University




Paper(s)

Kohei Kurahara et al. “Discovery of Diffuse Radio Source in Abell
1060”, in Publications of the Astronomical Society of Japan,
DOI: 10.1093/pasj/psae011



Related Link(s)