In radio astronomy, a fast radio burst (FRB) is a transient radio pulse of length ranging from a fraction of a millisecond to a few milliseconds, caused by some high-energy astrophysical process not yet understood. While extremely energetic at their source, the strength of the signal reaching Earth has been described as 1,000 times less than from a mobile phone on the Moon. The first FRB was discovered by Duncan Lorimer and his student David Narkevic in 2007 when they were looking through archival pulsar survey data, and it is therefore commonly referred to as the Lorimer Burst. Many FRBs have since been recorded, including three that repeat. Although the exact origin and cause is uncertain, they are almost definitely extragalactic.
When the FRBs are polarized, it indicates that they are emitted from a source contained within an extremely powerful magnetic field. The origin of the FRBs has yet to be identified; proposals for their origin range from a rapidly rotating neutron star and a black hole, to extraterrestrial intelligence.
The localization and characterization in 2012 of FRB 121102, one of the three repeating sources, has improved the understanding of the source class. FRB 121102 is identified with a galaxy at a distance of approximately 3 billion light-years, well outside the Milky Way, and is embedded in an extreme environment. The first host galaxy identified for a non-repeating burst, FRB 180924, was identified in 2019 and is a much larger and more ordinary galaxy, nearly the size of the Milky Way.
The first fast radio burst to be described, the Lorimer Burst FRB 010724, was detected in 2007 in archived data recorded by the Parkes Observatory on 24 July 2001. Since then, most known FRBs have been found in previously recorded data. On 19 January 2015, astronomers at Australia's national science agency (CSIRO) reported that a fast radio burst had been observed for the first time live, by the Parkes Observatory.
Fast radio bursts are bright, unresolved (pointsource-like), broadband (spanning a large range of radio frequencies), millisecond flashes found in parts of the sky outside the Milky Way. Unlike many radio sources, the signal from a burst is detected in a short period of time with enough strength to stand out from the noise floor. The burst usually appears as a single spike of energy without any change in its strength over time. The bursts last for several milliseconds (thousandths of a second). The bursts come from all over the sky, and are not concentrated on the plane of the Milky Way. Known FRB locations are biased by the parts of the sky that the observatories can image.
Many have radio frequencies detected around 1400 MHz; a few have been detected at lower frequencies in the range of 400–800 MHz. The component frequencies of each burst are delayed by different amounts of time depending on the wavelength. This delay is described by a value referred to as a dispersion measure (DM). This results in a received signal that sweeps rapidly down in frequency, as longer wavelengths are delayed more.
The interferometer UTMOST has put a lower limit of 10,000 kilometers for the distance to the FRBs it has detected, supporting the case for an astronomical, rather than terrestrial, origin (because signal sources on Earth are ruled out as being closer than this limit). This limit can be determined from the fact that closer sources would have a curved wave front that could be detected by the multiple antennas of the interferometer.
Fast radio bursts have pulse dispersion measurements > 100 pc cm−3, much larger than expected for a source inside the Milky Way galaxy and consistent with propagation through an ionized plasma. Furthermore, their distribution is isotropic (not especially coming from the galactic plane);:fig 3 consequently they are conjectured to be of extragalactic origin.
Fast radio bursts are named by the date the signal was recorded, as "FRB YYMMDD".
The first FRB detected, the Lorimer Burst FRB 010724, was discovered in 2007 when Duncan Lorimer assigned his student David Narkevic to look through archival data taken in 2001 by the Parkes radio dish in Australia. Analysis of the survey data found a 30-jansky dispersed burst which occurred on 24 July 2001, less than 5 milliseconds in duration, located 3° from the Small Magellanic Cloud. The reported burst properties argue against a physical association with the Milky Way galaxy or the Small Magellanic Cloud. The burst became known as the Lorimer Burst. The discoverers argue that current models for the free electron content in the Universe imply that the burst is less than 1 gigaparsec distant. The fact that no further bursts were seen in 90 hours of additional observations implies that it was a singular event such as a supernova or merger of relativistic objects. It is suggested that hundreds of similar events could occur every day and, if detected, could serve as cosmological probes.
In 2010 there was a report of 16 similar pulses, clearly of terrestrial origin, detected by the Parkes radio telescope and given the name perytons. In 2015 perytons were shown to be generated when microwave oven doors were opened during a heating cycle, with detected emission being generated by the microwave oven's magnetron tube as it was being powered off.
In 2015, FRB 110523 was discovered in archival data from the Green Bank Telescope. It was the first FRB for which linear polarization was detected (allowing a measurement of Faraday rotation). Measurement of the signal's dispersion delay suggested that this burst was of extragalactic origin, possibly up to 6 billion light-years away.
An observation in 2012 of a fast radio burst (FRB 121102) in the direction of Auriga in the northern hemisphere using the Arecibo radio telescope confirmed the extragalactic origin of fast radio pulses by an effect known as plasma dispersion.
In November 2015, astronomer Paul Scholz at McGill University in Canada, found ten non-periodically repeated fast radio pulses in archival data gathered in May and June 2015 by the Arecibo radio telescope. The ten bursts have dispersion measures and sky positions consistent with the original burst FRB 121102, detected in 2012. Like the 2012 burst, the 10 bursts have a plasma dispersion measure that is three times larger than possible for a source in the Milky Way Galaxy. The team thinks that this finding rules out self-destructive, cataclysmic events that could only occur once, such as the explosion of a black hole or the collision between two neutron stars. According to the scientists, the data support an origin in a young rotating neutron star (pulsar), or in a highly magnetized neutron star (magnetar), or from highly magnetized pulsars travelling through asteroid belts, or from an intermittent Roche lobe overflow in a neutron star-white dwarf binary.
On 16 December 2016 six new FRBs were reported in the same direction (one having been received on 13 November 2015, four on 19 November 2015, and one on 8 December 2015).:Table 2 As of January 2019 this is one of only two instances in which these signals have been found twice in the same location in space. FRB 121102 is located at least 1150 AU from Earth, excluding the possibility of a human-made source, and is almost certainly extragalactic in nature.
As of April 2018, FRB 121102 is thought to be co-located in a dwarf galaxy about three billion light-years from Earth with a low-luminosity active galactic nucleus, or a previously unknown type of extragalactic source, or a young neutron star energising a supernova remnant.
On 26 August 2017, astronomers using data from the Green Bank Telescope detected 15 additional repeating FRBs coming from FRB 121102 at 5 to 8 GHz. The researchers also noted that FRB 121102 is presently in a "heightened activity state, and follow-on observations are encouraged, particularly at higher radio frequencies". The waves are highly polarized, meaning "twisting" transverse waves, that could only have formed when passing through hot plasma with an extremely strong magnetic field. FRB 121102's radio bursts are about 500 times more twisted (polarized) than those from any other FRB to date. Since it is a repeating FRB source, it suggests that it does not come from some one-time cataclysmic event, so one hypothesis, first advanced in January 2018, proposes that these particular repeating bursts may come from a dense stellar core called a neutron star near an extremely powerful magnetic field, such as one near a massive black hole, or one embedded in a nebula.
In April 2018, it was reported that FRB 121102 consisted of 21 bursts spanning one hour. In September 2018, an additional 72 bursts spanning five hours had been detected using a convolutional neural network.
In 2013, four bursts were identified that supported the likelihood of extragalactic sources.
Fast radio bursts discovered up until 2015 had dispersion measures that were close to multiples of 187.5 pc cm−3. However subsequent observations do not fit this pattern.
On 18 April 2015, FRB 150418 was detected by the Parkes observatory and within hours, several telescopes including the Australia Telescope Compact Array caught an apparent radio "afterglow" of the flash, which took six days to fade. The Subaru telescope was used to find what was thought to be the host galaxy and determine its redshift and the implied distance to the burst.
However, the association of the burst with the afterglow was soon disputed, and by April 2016 it was established that the "afterglow" originates from an active galactic nucleus that is powered by a supermassive black hole with dual jets blasting outward from the black hole. It was also noted that what was thought to be an "afterglow", did not fade away as would be expected, meaning that the variable AGN is unlikely to be associated with the actual fast radio burst.
The upgraded Molonglo Observatory Synthesis Telescope (UTMOST), near Canberra (Australia), reported finding three more FRBs. A 180-day three-part survey in 2015 and 2016 found three FRBs at 843 MHz. Each FRB located with a narrow elliptical 'beam'; the relatively narrow band 828–858 MHz gives a less precise dispersion measure (DM).
According to Anastasia Fialkov and Abraham Loeb, FRB's could be occurring as often as once per second. Earlier research could not identify the occurrence of FRB's to this degree.
The unusual CHIME (Canadian Hydrogen Intensity Mapping Experiment) radio telescope, operational from September 2018, will be used to detect "hundreds" of fast radio bursts as a secondary objective to its cosmological observations. FRB 180725A was reported by CHIME as the first detection of a FRB under 700 MHz – as low as 580 MHz.
In October 2018, astronomers reported 19 more new non-repeating FRB bursts detected by the Australian Square Kilometre Array Pathfinder (ASKAP). These included three with dispersion measure (DM) smaller than seen before.
On 9 January 2019, astronomers announced the discovery of a second repeating FRB source, named FRB 180814, by CHIME. Six bursts were detected between August and October 2018, "consistent with originating from a single position on the sky". The detection was made during CHIME's pre-commissioning phase, during which it operated intermittently, suggesting a "substantial population of repeating FRBs", and that the new telescope would make more detections.
Some news media reporting of the discovery speculated that the repeating FRB could be evidence of extraterrestrial intelligence, a possibility explored in relation to previous FRBs by some scientists, but not raised by the discoverers of FRB 180814.
FRB 180924 is the first non-repeating FRB to be traced to its source. The source is a galaxy 3.6 billion light-years away. The galaxy is nearly as large as the Milky Way and about 1000 times larger than the source of FRB 121102. While the latter is an active site of star formation and a likely place for magnetars, the source of FRB 180924 is an older and less active galaxy.
Because the source was nonrepeating, the astronomers had to scan large areas with the 36 telescopes of ASKAP. Once a signal was found, they used the Very Large Telescope, the Gemini Observatory in Chile, and the W. M. Keck Observatory in Hawaii to identify its host galaxy and determine its distance. Knowing the distance and source galaxy properties, enables a study of the composition of the intergalactic medium.
On 28 June 2019, Russian astronomers reported the discovery of nine FRB events (FRB 121029, FRB 131030, FRB 140212, FRB 141216, FRB 151125.1, FRB 151125.2, FRB 160206, FRB 161202, FRB 180321), which include FRB 151125, the third repeating one ever detected, from the direction of the M 31 (Andromeda Galaxy) and M 33 (Triangulum Galaxy) galaxies during the analysis of archive data (July 2012 to December 2018) produced by the BSA/LPI large phased array radio telescope at the Pushchino Radio Astronomy Observatory.
On 2 July 2019, astronomers reported that FRB 190523, a non-repeating FRB, has been discovered and, notably, localized to a few-arcsecond region containing a single massive galaxy at a redshift of 0.66, nearly 8 billion light-years away from Earth.
Because of the isolated nature of the observed phenomenon, the nature of the source remains speculative. As of 2019, there is no generally accepted explanation. The sources are thought to be a few hundred kilometers or less in size, as the bursts last for only a few milliseconds, and if the bursts come from cosmological distances, their sources must be very energetic, generating as much energy in a millisecond burst as the Sun does in 80 years.
One possible explanation would be a collision between very dense objects like merging black holes or neutron stars. It has been suggested that there is a connection to gamma-ray bursts. Some have speculated that these signals might be artificial in origin, that they may be signs of extraterrestrial intelligence. Analogously, when the first pulsar was discovered, it was thought that the fast, regular pulses could possibly originate from a distant civilization, and the source nicknamed "LGM-1" (for "little green men").
In 2007, just after the publication of the e-print with the first discovery, it was proposed that fast radio bursts could be related to hyperflares of magnetars. In 2015 three studies supported the magnetar hypothesis.
Especially energetic supernovae could be the source of these bursts. Blitzars were proposed in 2013 as an explanation. In 2014 it was suggested that following dark matter-induced collapse of pulsars, the resulting expulsion of the pulsar magnetospheres could be the source of fast radio bursts. In 2015 it was suggested that FRBs are caused by explosive decays of axion miniclusters. Another exotic possible source are cosmic strings that produced these bursts as they interacted with the plasma that permeated the early Universe. In 2016 the collapse of the magnetospheres of Kerr–Newman black holes were proposed to explain the origin of the FRBs' "afterglow" and the weak gamma-ray transient 0.4 s after GW 150914. It has also been proposed that if fast radio bursts originate in black hole explosions, FRBs would be the first detection of quantum gravity effects. In early 2017, it was proposed that the strong magnetic field near a supermassive black hole could destabilize the current sheets within a pulsar's magnetosphere, releasing trapped energy to power the FRBs.
Repeated bursts of FRB 121102 have initiated multiple origin hypotheses. A coherent emission phenomenon known as superradiance, which involves large-scale entangled quantum mechanical states possibly arising in environments such as active galactic nuclei, has been proposed to explain these and other associated observations with FRBs (e.g. high event rate, variable intensity profiles).
Nonetheless, in July 2019, astronomers reported that non-repeating Fast Radio Bursts (FRB)s may not be one-off events, but actually FRB repeaters with repeat events that have gone undetected and, further, that FRBs may be formed by events that have not yet been seen or considered.
|Name||Date and time (UTC) for 1581.804688 MHz||RA
|FRB 010621||2001-06-21 13:02:10.795||18h 52m||−08° 29′||746||7.8||0.4|
|FRB 010724||2001-07-24 19:50:01.63||01h 18m||−75° 12′||375||4.6||30||"Lorimer Burst"|
|FRB 011025||2001-10-25 00:29:13.23||19h 07m||−40° 37′||790||9.4||0.3|
|FRB 090625||2009-06-25 21:53:52.85||03h 07m||−29° 55′||899.6||<1.9||>2.2|
|FRB 110220||2011-02-20 01:55:48.957||22h 34m||−12° 24′||944.38||5.6||1.3|
|FRB 110523 ||2011-05-23||21h 45m||−00° 12′||623.30||1.73||0.6||700–900 MHz at Green Bank radio telescope, detection of both circular and linear polarization.|
|FRB 110627||2011-06-27 21:33:17.474||21h 03m||−44° 44′||723.0||<1.4||0.4|
|FRB 110703||2011-07-03 18:59:40.591||23h 30m||−02° 52′||1103.6||<4.3||0.5|
|FRB 120127||2012-01-27 08:11:21.723||23h 15m||−18° 25′||553.3||<1.1||0.5|
|FRB 121002||2012-10-02 13:09:18.402||18h 14m||−85° 11′||1628.76||2.1; 3.7||0.35||double pulse 5.1 ms apart|
|FRB 121002||2012-10-02 13:09:18.50||18h 14m||−85° 11′||1629.18||<0.3||>2.3|
|FRB 121102||2012-11-02 06:35:53.244||05h 32m||+33° 05′||557||3.0||0.4||by Arecibo radio telescope|
|FRB 130626||2013-06-26 14:56:00.06||16h 27m||−07° 27′||952.4||<0.12||>1.5|
|FRB 130628||2013-06-28 03:58:00.02||09h 03m||+03° 26′||469.88||<0.05||>1.2|
|FRB 130729||2013-07-29 09:01:52.64||13h 41m||−05° 59′||861||<4||>3.5|
|FRB 131104||2013-11-04 18:04:01.2||06h 44m||−51° 17′||779.0||<0.64||1.12||'near' Carina Dwarf Spheroidal Galaxy|
|FRB 140514||2014-05-14 17:14:11.06||22h 34m||−12° 18′||562.7||2.8||0.47||21 ± 7 per cent (3σ) circular polarization|
|FRB 150215||2015-02-15 20:41:41.714||18h 17m 27s||−04° 54′ 15″||1105.6||2.8||0.7||43% linear, 3% circular polarized. Low galactic latitude. Low/zero rotation measure. Detected in real time. Not detected in follow up observations of gamma rays, X-rays, neutrinos, IR etc.|
|FRB 150418||2015-04-18 04:29||07h 16m||−19° 00′||776.2||0.8||2.4||Detection of linear polarization. The origin of the burst is disputed.|
|05h 31m 58s (average)||+33° 08′ 04″ (average)||559 (average)||0.02–0.31||2.8–8.7||10 repeat bursts at FRB 121102 location: 2 bursts on May 17 and 8 bursts on June 2 |
and 1 on 13 Nov 2015, 4 on 19 Nov 2015, and 1 on 8 Dec 2015
|FRB 150610||2015-06-10 05:26:59.396||10:44:26||−40:05:23||1593.9(±0.6)||2(±1)||0.7(±0.2)|
|FRB 150807||2015-08-07 17:53:55.7799||22:40:23||– 55:16||266.5||0.35±0.05||120±30||80% linearly polarised, Galactic latitude −54.4°, Decl ±4 arcmin, RA ±1.5 arcmin, highest peak flux|
|FRB 151206||2015-12-06 06:17:52.778||19:21:25||−04:07:54||1909.8(±0.6)||3.0(±0.6)||0.3(±0.04)|
|FRB 151230||2015-12-30 16:15:46.525||09:40:50||−03:27:05||960.4(±0.5)||4.4(±0.5)||0.42(±0.03)|
|FRB 160102||2016-01-02 08:28:39.374||22:38:49||−30:10:50||2596.1(±0.3)||3.4(±0.8)||0.5(±0.1)|
|FRB 160317||2016-03-17 09:00:36.530||07:53:47||−29:36:31||1165(±11)||21||>3.0||UTMOST, Decl ± 1.5°:Table A1|
|FRB 160410||2016-04-10 08:33:39.680||08:41:25||+06:05:05||278(±3)||4||>7.0||UTMOST, Decl ± 1.5°:Table A1|
|FRB 160608||2016-06-08 03:53:01.088||07:36:42||−40:47:52||682(±7)||9||>4.3||UTMOST, Decl ± 1.5°:Table A1|
|FRB 170107||2017-01-07 20:05:45.1397||11:23||– 05:01||609.5(±0.5)||2.6||27±4||first by ASKAP, high fluence ~58 Jy ms. In Leo. Galactic latitude 51°, Distance 3.1 Gpc, isotropic energy ~3 x 1034 J|
|unnamed||2017-08-26 13:51:44||05h 32m||+33° 08′||558(approx)||?||?||15 more bursts at the location of FRB 121102 detected by Green Bank Telescope over a 24-minute interval, bringing the total received bursts from this location to 34.|
|FRB 170827||2017-08-27 16:20:18||00h 49m 18.66s||−65° 33′ 02.3″||176.4||0.395||low DM|
|FRB 170922||2017-09-22 11:23:33.4||21h 29m 50.61s||−07° 59′ 40.49″||1111||26||extreme scattering (long pulse)|
|FRB 171020||2017-10-20 10:27:58.598||22:15||– 19:40||114.1±0.2||3.2||ASKAP s/n=19.5 G-Long'=29.3 G-lat'=-51.3 Lowest DM so far.|
|FRB 171209||2017-12-09 20:34:23.5||15h 50m 25s||−46° 10′ 20″||1458||2.5||2.3|
|FRB 180301||2018-03-01 07:34:19.76||06h 12m 43.4s||+04° 33′ 44.8″||520||3||0.5||positive spectrum, from Breakthrough Listen|
|FRB 180309||2018-03-09 02:49:32.99||21h 24m 43.8s||−33° 58′ 44.5″||263.47||0.576||12|
|FRB 180311||2018-03-11 04:11:54.80||21h 31m 33.42s||−57° 44′ 26.7″||1575.6||12||2.4|
|FRB 180725A||2018-07-25 17:59:43.115||06h 13m 54.7s||+67° 04′ 00.1″||716.6||2||first detection of an FRB at radio frequencies below 700 MHz|
Realtime detection by CHIME.
|FRB 180814||Detected by CHIME. Second repeating FRB to be discovered and first since 2012.|
|FRB 180924||2018-09-24 16:23:12.6265||21h 44m 25.26s||−40° 54′ 0.1″||361.42||1.3||16||first non-repeating FRB whose source has been localized|
FRBs are also cataloged at frbcat.
A number of significant scientific events have occurred or are scheduled to occur in 2019.Alien Planet
Alien Planet is a 94-minute docufiction, originally airing on the Discovery Channel, about two internationally built robot probes searching for alien life on the fictional planet Darwin IV. It was based on the book Expedition, by sci-fi/fantasy artist and writer Wayne Douglas Barlowe, who was also executive producer on the special. It premiered on May 14, 2005.
The show uses computer-generated imagery, which is interspersed with interviews from such notables as Stephen Hawking, George Lucas, Michio Kaku and Jack Horner. The show was filmed in Iceland and Mono Lake in California.Andrew Siemion
Andrew Patrick Vincent Siemion is an astrophysicist and director of the Berkeley SETI Research Center. His research interests include high energy time-variable celestial phenomena, astronomical instrumentation and the search for extraterrestrial intelligence (SETI).. Andrew Siemion is the Principal Investigator for the Breakthrough Listen program.Siemion received his B.A. (2008) M.A. (2010) and Ph.D. (2012) in astrophysics from the University of California, Berkeley. In 2018, Siemion was named the Bernard M. Oliver Chair for SETI at the SETI Institute. Siemion is jointly affiliated with Radboud University Nijmegen and the University of Malta. Also in 2018, he was elected to the International Academy of Astronautics as a Corresponding Member for Basic Sciences. In September 2015, Siemion testified on the current status of astrobiology to the House Committee on Science, Space, and Technology of the United States Congress.Canadian Hydrogen Intensity Mapping Experiment
The Canadian Hydrogen Intensity Mapping Experiment (CHIME) is an interferometric radio telescope at the Dominion Radio Astrophysical Observatory in British Columbia, Canada which consists of four 100 x 20 metre semi-cylinders (roughly the size and shape of snowboarding half-pipes) populated with 1024 dual-polarization radio receivers sensitive at 400–800 MHz. The telescope's low-noise amplifiers are built with components adapted from the cellphone industry and its data are processed using a custom-built FPGA electronic system and 1000-processor high-performance GPGPU cluster. The telescope has no moving parts and observes half of the sky each day as the Earth turns.
CHIME is a partnership between the University of British Columbia, McGill University, the University of Toronto and the Canadian National Research Council's Dominion Radio Astrophysical Observatory. A first light ceremony was held on 7 September 2017 to inaugurate the commissioning phase.Canadian Institute for Theoretical Astrophysics
The Canadian Institute for Theoretical Astrophysics (CITA) is a national research institute funded by the Natural Sciences and Engineering Research Council, located at the University of Toronto in Toronto, Ontario, Canada. CITA's mission is "to foster interaction within the Canadian theoretical Astrophysics community and to serve as an international center of excellence for theoretical studies in astrophysics." CITA was incorporated in 1984.CITA has close administrative and academic relations with the Canadian Institute for Advanced Research (CIFAR); several CITA faculty also serve as members of CIFAR.Dispersion (optics)
In optics, dispersion is the phenomenon in which the phase velocity of a wave depends on its frequency.Media having this common property may be termed dispersive media. Sometimes the term chromatic dispersion is used for specificity.
Although the term is used in the field of optics to describe light and other electromagnetic waves, dispersion in the same sense can apply to any sort of wave motion such as acoustic dispersion in the case of sound and seismic waves, in gravity waves (ocean waves), and for telecommunication signals along transmission lines (such as coaxial cable) or optical fiber.
In optics, one important and familiar consequence of dispersion is the change in the angle of refraction of different colors of light, as seen in the spectrum produced by a dispersive prism and in chromatic aberration of lenses. Design of compound achromatic lenses, in which chromatic aberration is largely cancelled, uses a quantification of a glass's dispersion given by its Abbe number V, where lower Abbe numbers correspond to greater dispersion over the visible spectrum. In some applications such as telecommunications, the absolute phase of a wave is often not important but only the propagation of wave packets or "pulses"; in that case one is interested only in variations of group velocity with frequency, so-called group-velocity dispersion.FRB
FRB may refer to:
Fast radio burst in radio astronomy
Fairbourne railway station, in Wales, station code
Federal Reserve Board of Governors, in the United States
Federal Reserve Bank
Forbes Airport, New South Wales, Australia, IATA code
Team Frøy–Bianchi, a Norwegian cycling team, code
Full of rabid babies, a 2b1 group from JIC, code
FKBP12-Rapamycin Binding domain; see Mechanistic target of rapamycinList of fast radio bursts
This is a list of fast radio bursts. Items are listed here if information about the fast radio burst has been published. Although there could be thousands of detectable events per day, only detected ones are listed.Matthew Bailes
Professor Matthew Bailes is an astrophysicist at the Centre for Astrophysics and Supercomputing, Swinburne University of Technology and the Director of OzGrav, the ARC Centre of Excellence for Gravitational Wave Discovery. In 2015 he won an ARC Laureate Fellowship to work on Fast Radio Bursts. He is one of the most active researchers in pulsars and Fast Radio Bursts in the world. His research interests includes the birth, evolution of binary and millisecond pulsars, gravitational waves detection using an array of millisecond pulsars and radio astronomy data processing system design for Fast Radio Burst discovery. He is now leading his team to re-engineer the Molonglo Observatory Synthesis Telescope with a newly designed correlation system for observation of pulsars and Fast Radio (Lorimer) Bursts.
Bailes founded the organisation for development of the Virtual Room, an octagonal virtual reality system for displaying the planets, our sun, the stars, the milky way, the galaxies and the universe, etc. He made the 3D film "Realising Einstein's Universe".
Bailes is a committee member of the Australia Telescope Steering Committee and on advisory board of Collaboration for Astronomy Signal Processing and Electronics Research (CASPER).MeerKAT
MeerKAT, originally the Karoo Array Telescope, is a radio telescope consisting of 64 antennas in the Northern Cape of South Africa. In 2003, South Africa submitted an expression of interest to host the Square Kilometre Array (SKA) Radio Telescope in Africa, and the locally designed and built MeerKAT was incorporated into the first phase of the SKA.Molonglo Observatory Synthesis Telescope
The Molonglo Observatory Synthesis Telescope (MOST) is a radio telescope operating at 843 MHz. It is operated by the School of Physics of the University of Sydney. The telescope is located in Hoskinstown, near the Molonglo River and Canberra, and was constructed by modification of the East-West arm of the former Molonglo Cross Telescope, a larger version of the Mills Cross Telescope.PALFA Survey
PALFA is a large-scale survey for radio pulsars at 1.4 GHz using the Arecibo 305-meter telescope and the ALFA multibeam receivers. It is the largest and most sensitive survey of the Galactic plane to date.Peryton
The peryton is a mythological hybrid animal combining the physical features of a stag and a bird. The peryton was created and described by Jorge Luis Borges in his 1957 Book of Imaginary Beings, using a supposedly long-lost medieval manuscript as a source.Peryton (disambiguation)
The peryton is a mythical creature with features of a stag and a bird.
Peryton may also refer to:
Peryton (Dungeons & Dragons), a creature in Dungeons & Dragons
Peryton (astronomy), a type of Fast Radio Burst that was found to originate in microwave ovensRotating radio transient
Rotating radio transients (RRATs) are sources of short, moderately bright, radio pulses, which were first discovered in 2006. RRATs are thought to be pulsars, i.e. rotating magnetised neutron stars which emit more sporadically and/or with higher pulse-to-pulse variability than the bulk of the known pulsars. The working definition of what a RRAT is, is a pulsar which is more easily discoverable in a search for bright single pulses, as opposed to in Fourier domain searches so that 'RRAT' is little more than a label (of how they are discovered) and does not represent a distinct class of objects from pulsars. As of March 2015 over 100 have been reported.VVV-WIT-07
VVV-WIT-07 is a unique variable star which presents a sequence of recurrent dimmings (v~14.35 – 16.164) with a possible deep eclipse in July 2012. The star, located in the Scorpius constellation about 23,000 ly (7,100 pc)(?) away, is not a binary star, which would eliminate such a system from explaining the various observed dimmings.The star was found by the "Vista Variables in the Via Lactea" (VVV) project, which is a survey of European Southern Observatory (ESO) variability of the innermost bulge of the Milky Way galaxy. The near-infrared spectra of VVV-WIT-07 appear without features, without prominent emission or absorption lines. The characteristics found in the light curve of VVV-WIT-07 (WIT refers to "What Is This?") are similar to those seen in J1407 (Mamajek's Object), a pre-MS K5 dwarf with a ring system that eclipses the star or, alternatively, to KIC 8462852 (or Tabby's star), a F3 IV/V star that shows irregular and aperiodic obscurations in its light curve.From 2010 to 2018, the star dimmed and brightened irregularly (v~14.35 – 16.164), and seemed similar to Tabby's star, except the light from VVV-WIT-07 dimmed by up to 80 percent, while Tabby’s star faded by only about 20 percent. Another star, J1407, however, has been found to have dimmed by up to 95%, which may be more similar to the light curve presented by VVV-WIT-07. Nonetheless, according to ESO astronomer Valentin Ivanov, "A key word that could be used to describe our finding [of VVV-WIT-07] is extreme. In every aspect ... We have identified a system that challenges the imagination even more than usual, because it is so unlike our own planetary system."Wow! signal
The Wow! signal was a strong narrowband radio signal received on August 15, 1977, by Ohio State University's Big Ear radio telescope in the United States, then used to support the search for extraterrestrial intelligence. The signal appeared to come from the direction of the constellation Sagittarius and bore the expected hallmarks of extraterrestrial origin.
Astronomer Jerry R. Ehman discovered the anomaly a few days later while reviewing the recorded data. He was so impressed by the result that he circled the reading on the computer printout and wrote the comment Wow! on its side, leading to the event's widely used name.The entire signal sequence lasted for the full 72-second window during which Big Ear was able to observe it, but has not been detected since, despite several subsequent attempts by Ehman and others. Many hypotheses have been advanced on the origin of the emission, including natural and human-made sources, but none of them adequately explains the signal. Although the Wow! signal was unmodulated and had no encoded information, it remains the strongest candidate for an alien radio transmission ever detected.Zero Gravity (Rebirth and Evolution)
Zero Gravity (Rebirth and Evolution) is the debut studio album by Italian symphonic power metal band Turilli / Lione Rhapsody. It was released on July 5, 2019 via Nuclear Blast.The album was funded by a crowdfunder that the band had started on Indiegogo.