Tagged: FRBs-fast radio bursts-one of today’s big mysteries in astronomy Toggle Comment Threads | Keyboard Shortcuts

  • richardmitnick 1:51 pm on January 10, 2019 Permalink | Reply
    Tags: , , , , , FRBs-fast radio bursts-one of today’s big mysteries in astronomy, , , Radio magnetars, The team looked at the magnetar named PSR J1745-2900 located in the Milky Way's galactic center using the largest of NASA's Deep Space Network radio dishes in Australia   

    From Caltech: “Magnetar Mysteries in our Galaxy and Beyond” 

    Caltech Logo

    From Caltech


    Whitney Clavin
    (626) 395-1856

    Illustration of a magnetar—a rotating neutron star with incredibly powerful magnetic fields.
    Credit: NASA/CXC/M.Weiss

    The 70-meter radio dish (DSS-43) in Canberra, Australia, part of NASA’s Deep Space Network.
    Credit: NASA/DSN

    New research looks at possible links between magnetars and extragalactic radio bursts.

    In a new Caltech-led study, researchers from campus and the Jet Propulsion Laboratory (JPL) have analyzed pulses of radio waves coming from a magnetar—a rotating, dense, dead star with a strong magnetic field—that is located near the supermassive black hole at the heart of the Milky Way galaxy. The new research provides clues that magnetars like this one, lying in close proximity to a black hole, could perhaps be linked to the source of “fast radio bursts,” or FRBs. FRBs are high-energy blasts that originate beyond our galaxy but whose exact nature is unknown.

    “Our observations show that a radio magnetar can emit pulses with many of the same characteristics as those seen in some FRBs,” says Caltech graduate student Aaron Pearlman, who presented the results today at the 233rd meeting of the American Astronomical Society in Seattle. “Other astronomers have also proposed that magnetars near black holes could be behind FRBs, but more research is needed to confirm these suspicions.”

    The research team was led by Walid Majid, a visiting associate at Caltech and principal research scientist at JPL, which is managed by Caltech for NASA, and Tom Prince, the Ira S. Bowen Professor of Physics at Caltech. The team looked at the magnetar named PSR J1745-2900, located in the Milky Way’s galactic center, using the largest of NASA’s Deep Space Network radio dishes in Australia. PSR J1745-2900 was initially spotted by NASA’s Swift X-ray telescope, and later determined to be a magnetar by NASA’s Nuclear Spectroscopic Telescope Array (NuSTAR), in 2013.

    NASA Neil Gehrels Swift Observatory

    NASA NuSTAR X-ray telescope

    “PSR J1745-2900 is an amazing object. It’s a fascinating magnetar, but it also has been used as a probe of the conditions near the Milky Way’s supermassive black hole,” says Fiona Harrison, the Benjamin M. Rosen Professor of Physics at Caltech and the principal investigator of NuSTAR. “It’s interesting that there could be a connection between PSR J1745-2900 and the enigmatic FRBs.”

    Magnetars are a rare subtype of a group of objects called pulsars; pulsars, in turn, belong to a class of rotating dead stars known as neutron stars. Magnetars are thought to be young pulsars that spin more slowly than ordinary pulsars and have much stronger magnetic fields, which suggests that perhaps all pulsars go through a magnetar-like phase in their lifetime.

    Women in STEM – Dame Susan Jocelyn Bell Burnell

    Dame Susan Jocelyn Bell Burnell, discovered pulsars with radio astronomy. Jocelyn Bell at the Mullard Radio Astronomy Observatory, Cambridge University, taken for the Daily Herald newspaper in 1968. Denied the Nobel.

    The magnetar PSR J1745-2900 is the closest-known pulsar to the supermassive black hole at the center of the galaxy, separated by a distance of only 0.3 light-years, and it is the only pulsar known to be gravitationally bound to the black hole and the environment around it.

    In addition to discovering similarities between the galactic-center magnetar and FRBs, the researchers also gleaned new details about the magnetar’s radio pulses. Using one of the Deep Space Network’s largest radio antennas, the scientists were able to analyze individual pulses emitted by the star every time it rotated, a feat that is very rare in radio studies of pulsars. They found that some pulses were stretched, or broadened, by a larger amount than predicted when compared to previous measurements of the magnetar’s average pulse behavior. Moreover, this behavior varied from pulse to pulse.

    “We are seeing these changes in the individual components of each pulse on a very fast time scale. This behavior is very unusual for a magnetar,” says Pearlman. The radio components, he notes, are separated by only 30 milliseconds on average.

    One theory to explain the signal variability involves clumps of plasma moving at high speeds near the magnetar. Other scientists have proposed that such clumps might exist but, in the new study, the researchers propose that the movement of these clumps may be a possible cause of the observed signal variability. Another theory proposes that the variability is intrinsic to the magnetar itself.

    “Understanding this signal variability will help in future studies of both magnetars and pulsars at the center of our galaxy,” says Pearlman.

    In the future, Pearlman and his colleagues hope to use the Deep Space Network radio dish to solve another outstanding pulsar mystery: Why are there so few pulsars near the galactic center? Their goal is to find a non-magnetar pulsar near the galactic-center black hole.

    “Finding a stable pulsar in a close, gravitationally bound orbit with the supermassive black hole at the galactic center could prove to be the Holy Grail for testing theories of gravity,” says Pearlman. “If we find one, we can do all sorts of new, unprecedented tests of Albert Einstein’s general theory of relativity.”

    The new study, titled, “Pulse Morphology of the Galactic Center Magnetar PSR J1745-2900,” appeared in the October 20, 2018, issue of The Astrophysical Journal and was funded by a Research and Technology Development grant through a contract with NASA; JPL and Caltech’s President’s and Director’s Fund; the Department of Defense; and the National Science Foundation. Other authors include Jonathon Kocz of Caltech and Shinji Horiuchi of the CSIRO (Commonwealth Scientific and Industrial Research Organization) Astronomy & Space Science, Canberra Deep Space Communication Complex.

    See the full article here .

    Please help promote STEM in your local schools.

    Stem Education Coalition

    The California Institute of Technology (commonly referred to as Caltech) is a private research university located in Pasadena, California, United States. Caltech has six academic divisions with strong emphases on science and engineering. Its 124-acre (50 ha) primary campus is located approximately 11 mi (18 km) northeast of downtown Los Angeles. “The mission of the California Institute of Technology is to expand human knowledge and benefit society through research integrated with education. We investigate the most challenging, fundamental problems in science and technology in a singularly collegial, interdisciplinary atmosphere, while educating outstanding students to become creative members of society.”

    Caltech campus

    Caltech campus

  • richardmitnick 8:54 pm on November 9, 2018 Permalink | Reply
    Tags: ASKAP- CSIRO's Australian Square Kilometre Array Pathfinder telescope in remote Western Australia, , , , , , , , FRBs-fast radio bursts-one of today’s big mysteries in astronomy, If we can identify host galaxies of FRBs with ASKAP then we can use a telescope like ESO’s VLT to get optical spectra of those galaxies which can tell us their distances very precisely   

    From ESOblog: “Pinpointing the Hosts of Fast Radio Bursts” 

    ESO 50 Large

    From ESOblog


    9 November 2018

    Interview with Elizabeth Mahony and Stuart Ryder

    First detected barely a decade ago, fast radio bursts (FRBs) are one of today’s big mysteries in astronomy, and Australia’s ASKAP telescope is the best facility in the world for detecting them.

    Australian Square Kilometre Array Pathfinder (ASKAP) is a radio telescope array located at Murchison Radio-astronomy Observatory (MRO) in the Australian Mid West. ASKAP consists of 36 identical parabolic antennas, each 12 metres in diameter, working together as a single instrument with a total collecting area of approximately 4,000 square metres.

    A team of scientists recently used ESO’s Very Large Telescope to follow up on an ASKAP detection, to search for an FRB host galaxy to find out more about how, where and why they form. This investigation was possible thanks to a long-term partnership between ESO and Australia, and is an elegant example of the complementary nature of Australia’s radio telescopes and ESO’s optical telescopes. Project members Elizabeth Mahony and Stuart Ryder tell us more.

    Q. What are fast radio bursts and why should we be interested in them?

    Stuart (S): Fast radio bursts (FRBs) are bright bursts of radio emission that last for just a few milliseconds. Their energetic nature tells us that they must be caused by extreme events, but being so short-lived they are extremely difficult to detect. Pinpointing exactly where they come from is even more challenging, so we still know very little about the environments they form in and the triggers that cause them.

    Elizabeth (E): About 50 FRBs have been detected in the past, but just one has been pinpointed to a host galaxy, and that is the only one that has had repeated bursts. For all other detected FRBs we don’t know precisely where they came from, which makes it hard to understand them and their host galaxies.

    Q. Tell us more about your investigation.

    E: An FRB was spotted a year ago by CSIRO’s Australian Square Kilometre Array Pathfinder (ASKAP) telescope in remote Western Australia. This particular object, denoted FRB 171020, has the lowest “dispersion measure” detected to date — this measure tells us how much matter the radio emission has travelled through. The value suggests that the FRB must have taken place less than one billion light-years away, meaning that its light took one billion years to reach us. This sounds extremely distant but actually, it’s the closest FRB ever detected, making it easier for us to narrow down its location and search for its host galaxy. The ASKAP detection gave us a rough idea of the position of this FRB, so we could then search for its host galaxy.

    Q. How does ASKAP detect FRBs when they last just a few milliseconds?

    S: ASKAP is a radio telescope made up of 36 antennas that can each see 30 square degrees of sky — as a reference, the full Moon covers just 0.2 square degrees of sky! To search for FRBs we use ASKAP in an unusual configuration called “fly’s-eye mode” where each antenna points in a different direction. This maximises the amount of sky that is observed at once, drastically increasing the chances of catching an FRB when it happens.

    Q. Why is it interesting to identify the host galaxies of FRBs?

    S: All we know currently is that FRBs are the result of some sort of astronomical object undergoing a dramatic, though not necessarily destructive, outburst. If it emerges that FRBs originate only in certain types of galaxies, then this will offer us clues about what objects and environments can spark FRBs.

    E: In addition to this, if we can identify host galaxies of FRBs, we can use a telescope like ESO’s Very Large Telescope (VLT) to get optical spectra of those galaxies, which can tell us their distances very precisely. By comparing these physical distances with the measured dispersion values, we will be able to trace the distribution of matter between galaxies far more accurately than is currently possible. Once the distances to thousands of FRB host galaxies are known, we will be able to conduct 3D “tomography” of the intergalactic medium, that will help us understand more about how galaxies expel and accrete gas.

    Q. Why did you use the VLT to follow-up on this FRB?

    E: FRBs are so bright that they can be detected even if they are very far from Earth, coming from potentially quite dim host galaxies. This, combined with the fact that we don’t know what kind of galaxies host FRBs, means that we need to use the largest optical telescopes in the world to identify the correct host galaxy.

    Q. …and what did you find?

    E: With ASKAP we located FRB171020 to an area of sky measuring 50 arcminutes by 34 arcminutes (roughly two full Moons across), but this area contains hundreds of galaxies. The dispersion measure helped us narrow down this number to just 16 potential host galaxies. We then used the VLT’s X-shooter instrument to determine the distances to these 16 galaxies, and identified the closest one — nearby spiral ESO 601-G036 — as the most likely to be the host galaxy.

    ESO X-shooter on VLT on UT2 at Cerro Paranal, Chile

    ESO 601-G036 is 120 million light-years away, which is within the distance limit set by the dispersion measure. This is the first time that a host galaxy has been singled out for a non-repeating FRB. With this knowledge, we will be able to further investigate what kind of environments FRBs are formed in, and shed light on what causes these very energetic outbursts.

    S: We also saw a dim “smudge” next to ESO 601-G036, at the same distance. We expect that this is the remains of another galaxy merging with the larger ESO 601-G036 — a process that can be extremely violent and could potentially spark FRBs. It will be interesting to see if other FRB host galaxies show such signs of merger activity.

    The area of sky selected for follow-up observation by the VLT, with potential host galaxies circled in red and ESO 601-G036 at the centre. At the bottom left is a more detailed picture of ESO 601-G036 from the VST Atlas survey. Credit: Elizabeth Mahony

    Q. When did ESO sign a strategic partnership with Australia and what does this partnership mean for the astronomical community?

    S: The Strategic Partnership between ESO and Australia was signed on 11 July 2017 in Canberra, during the Annual Scientific Meeting of the Astronomical Society of Australia. It gives the Australian astronomy community access to ESO’s La Silla and Paranal Observatories, as well as the opportunity to bid for instrumentation and industry contracts. It also secured the immediate future operations of the Anglo-Australian Telescope.

    AAO Anglo Australian Telescope near Siding Spring, New South Wales, Australia, Altitude 1,100 m (3,600 ft)

    Siding Spring Mountain with Anglo-Australian Telescope dome visible near centre of image at an altitude of 1,165 m (3,822 ft)

    The ten-year agreement lays a pathway for full Australian membership to ESO, which would then include access to ALMA [below] and the ELT [below].

    Q. How did the partnership allow you to make this discovery?

    S: While ASKAP is the world’s best facility for detecting FRBs, we need access to other telescopes to carry out the optical and infrared follow-up of their candidate host galaxies. Through this Strategic Partnership, we now have long-term certainty of access to such telescopes. Australia has really dominated the search for FRBs in the past, and is well-placed to feed a steady stream of FRB detections to ESO for rapid follow-up.

    Q. Do you think that the European-Australian collaboration will lead to more astronomical discoveries than either partner could achieve alone?

    E: Absolutely! ASKAP is now operating in a mode that will potentially allow us to not only detect more FRBs, but to then pinpoint their positions with a really high accuracy. That means we could work out not only exactly which galaxy an FRB occurred in, but even where within the galaxy it occurred. Do FRBs occur at the centre of galaxies, perhaps pointing to black holes as their source? Or do they prefer the outskirts of galaxies? Once we know that, we can use the unparalleled capability of the VLT’s MUSE instrument with the Laser Guide Star Facility to home in on the sites of FRBs, as well as to reveal intervening galaxies that the FRB signal passed through.

    ESO MUSE on the VLT on Yepun (UT4),

    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.

    See the full article here .


    Please help promote STEM in your local schools.

    Stem Education Coalition

    Visit ESO in Social Media-




    ESO Bloc Icon

    ESO 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”.

    ESO LaSilla
    ESO/Cerro LaSilla 600 km north of Santiago de Chile at an altitude of 2400 metres.

    ESO VLT 4 lasers on Yepun

    ESO Vista Telescope
    ESO/Vista Telescope at Cerro Paranal, with an elevation of 2,635 metres (8,645 ft) above sea level.

    ESO/NTT at Cerro LaSilla 600 km north of Santiago de Chile at an altitude of 2400 metres.

    ESO VLT Survey telescope
    VLT Survey Telescope at Cerro Paranal with an elevation of 2,635 metres (8,645 ft) above sea level.

    ALMA Array
    ALMA on the Chajnantor plateau at 5,000 metres.

    ESO/E-ELT,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).

    APEX Atacama Pathfinder 5,100 meters above sea level, at the Llano de Chajnantor Observatory in the Atacama desert.

    Leiden MASCARA instrument, 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)

    Leiden MASCARA cabinet at ESO 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 at Cerro Paranel, 2,635 metres (8,645 ft) above sea level

    SPECULOOS four 1m-diameter robotic telescopes 2016 in the ESO Paranal Observatory, 2,635 metres (8,645 ft) above sea level

    ESO TAROT telescope at Paranal, 2,635 metres (8,645 ft) above sea level

    ESO ExTrA telescopes at Cerro LaSilla at an altitude of 2400 metres

Compose new post
Next post/Next comment
Previous post/Previous comment
Show/Hide comments
Go to top
Go to login
Show/Hide help
shift + esc
%d bloggers like this: