PoS(MeerKAT2016)009 http://pos.sissa.it/ for up to date www.trapum.org , supernova remnants and other high energy sources, globular clus- Fermi ∗ [email protected] [email protected] Speaker. TRansients and PUlsars with MeerKAT (TRAPUM)will is utilise a MeerKAT MeerKAT to Large greatly Survey expand Project ourat which knowledge radio of wavelengths the on populations timescales of rangingtivity sources from of which MeerKAT microseconds will emit to allow us seconds. toincluding The discover many excellent FRBs, new sensi- radio (millisecond) pulsars, emitting fast magnetars, radioto RRATs, transients name giant just pulses, a flare few. stars,radio It and will transients active also have binaries allow been us discovered. tosources significantly through MeerKAT the expand will combination the also of parameter be the spaceTRAPUM excellent relatively over will long for which achieve baselines localising this and and through the new use aemitters of combination identified transient of by buffers. targeted searches: directed at gamma-ray ters – reservoirs of pulsars, andplane. the Galactic It centre, will and also blind perform searchesto a of find wide regions at area of least Fly’s the 30 Eye of Galactic style thewith brightest search a FRBs. for These 400-beam fast searches transients beamformer are that enabled andthe will by real-time Max-Planck-Institut be MeerKAT in für and able combination Radioastronomie offline and processing theTRAP capabilities European project. funded Research through Council-funded This Meer- contributionconsists is of more completed than on 40 behalf members of from the across entire the TRAPUM world. team See which team membership and other information. ∗ Copyright owned by the author(s) under the terms of the Creative Commons c Attribution-NonCommercial-NoDerivatives 4.0 International License (CC BY-NC-ND 4.0). MeerKAT Science: On the Pathway to25-27 the May, SKA 2016 Stellenbosch, South Africa Michael Kramer Max-Planck-Institut für Radioastronomie, Auf dem HügelJodrell 69, Bank D-53121 Centre Bonn, for Germany Astrophysics, SchoolManchester of Physics and Astronomy, University of E-mail: Ben Stappers Jodrell Bank Centre for Astrophysics, SchoolManchester of Physics and Astronomy, University of E-mail: An Update on TRAPUM PoS(MeerKAT2016)009 Ben Stappers in this area. Over gamma-ray sources: gamma-ray sources host, Fermi ]. Radio pulsar timing and 1 Fermi Fermi gamma-ray sources. Excitingly, this Fermi 1 has revolutionised our view of the gamma-ray sky. Over 200 ). Fermi ◦ 39 − < δ ∼ gamma-ray sources provide a treasure map for deep pulsar searches and, for example, the Discover exotic systems containing pulsarspulsars and to compact enable improved companions tests and of new general millisecond relativity andDiscover the pulsars search in for the gravitational Galactic waves. centre anddark use matter them and to stellar probe gravitational populations. effects of Sgr A* , Expand number of transient radio sources: RRATs, giant pulses,Greatly flare stars, expand active the binaries. parameter space:fast sensitivity; radio search transients volume; to time resolution, studypossible search the use for them highest for energy cosmology, or density gravitational events wave in emission studies. theIncrease Universe; the and populations where ofdistributions, all to understand neutron the number stars of to neutron stars, constrain types birthStudy and formation rates, the rates. properties, spatial dynamics, andpulsars, and velocity including exotic evolution systems of which can globular be clusters used to (GCs)Investigate determine the by neutron dependence star finding of masses. the new pulsarmetallicity and and fast star transient formation populations history, on by properties searching such for them as in external galaxies The scientific aims of the TRAPUM project are to greatly expand our knowledge of the radio We now describe the motivation and goals of the TRAPUM project in more detail. Supernova remnants (SNRs), pulsar wind nebulae (PWNe) and Since its launch in 2008, • • • • • • • deep radio pulsation searches have70 been MSPs indispensable have to been the discovered in success targeted of searches of sky on timescales ranging from microseconds to seconds and thereby achieve the following goals. 1.1 Targeted pulsar searches of SNRs, PWNe, and unidentified An Update on TRAPUM 1. Science goals of TRAPUM arguably, some of the most interesting radio pulsars.a SNR/PWN/gamma-ray The source discovery of is a crucial radio for pulsar understanding coincidentvice-versa, the with multi-wavelength energy counterparts budget provide of substantially such more systems context and, fornature understanding of the the radioimportant pulsar for itself. understanding the Discovering Galacticexplosion, young neutron and pulsars star the formation associated rate, injection withFermi the of SNRs nature high-energy or of particles PWNe the into supernova is MSPs the found can interstellar probe medium. accretion physicsfor (e.g. Unidentified the “transitional” International MSPs), provide Pulsar newgravity Timing precision and/or Array, timers constraining as well themode, as neutron MeerKAT is identify star poised exotic to equation revolutionise binariesthe of pulsar Southern capable searches state. sky of of ( SNRs/PWNe/gamma-ray testing With sources in a 400-beam pulsar search gamma-ray pulsars are now known, roughly half of which are MSPs [ PoS(MeerKAT2016)009 Jy µ Fermi Ben Stappers Jy, being equivalent µ Jy). µ gamma-ray sources, a large . Targeting these sources as ]). Moreover, the Cherenkov ◦ 3 100 39 14 arcmin), thus requiring only a < − Fermi ∼ = In this case only two passes would be δ deeper than the Parkes radio telescope 2 × 10 − 2 1000 unidentified . ∼ ]. Through TRAPUM, MeerKAT can play a major role ◦ 2 39 ] provides us with a new list of 334 potential pulsar targets 25 new pulsars). In total, 338 hours for searching would be − 2 ], who used three passes per source, multiple visits are critical gamma-ray sources will require 54 min integrations to reach a 4 ∼ = δ ) promote collisions and exchange interactions that create binaries 3 ] for a recent review). This is because the dense stellar environments Fermi − 5 430h. pc =

and/or highly accelerated MSPs. In fact, pulsars have undoubtedly been M 92 3 1 + ). As shown in [ 10 − 1400 4 S We expect many of these sourcesFor will sources be redbacks with and less black background widow temperature, systems. it would be useful to aim deeper to reach 20 SNR/PWN searches for young pulsars will require typically 9 min per target for a 40 Globular clusters (GCs) harbor a very large number of MSPs per unit stellar mass compared Searches of unidentified Considering SNRs and PWNe, we note that many still have no associated young pulsar, which Jy pulsar ( 1 2 µ in the cores (10 with the flux of the weakest youngest pulsar known. The small MeerKAT beam is an advantage here. needed for the 125 targets below with the Galactic plane (see [ in solving the lingering mysterydiscoveries of the to nature address of the these3FGL sources scientific catalog and goals produce unassociated mentioned a sources large [ here. yield of A pulsar recent classification of the for finding eclipsing missed in previous searches forand all based on of previous the search aforementioned results,gamma-ray we reasons. sources estimate we that Following search we the (i.e. will same discover strategy, a pulsar in one-fifth of the pulsar assuming a 10 Kthe excess flux of density sky contribution temperature fromrequired the in in background each order nebula. of to automatically the confirm individualephemeris weak for pencil candidate the pulsars beams discoveries. and Again due assuming to to a startand one-fifth building the success a rate time rotational this required results in to 50searches search new is pulsars the thus 338 250 targets is 92 h. The total1.2 time Globular required Cluster for Searches such targeted inferred from GeV measurements, of which 125 are below An Update on TRAPUM is just the tip offraction the of iceberg: which are there likely remain to be pulsars [ part of TRAPUM, which can reach a sensitivity 5 Telescope Array (CTA) will goSNRs, PWNe an and order gamma-ray of binariesmore magnitude than in deeper 250 the SNRs and TeV and domain. unveil PWNe(from a without the To any large Green our known 2014 population current associated catalog pulsar of knowledge,sky and and extensions there HESS visible comparable are Galactic from to the plane the Karoo survey),single TRAPUM pointing. the 400-beam vast We FOV aim ( majority to of deeply which search all have of these. 10 remains a mystery and greatlyand limits the our statistics ability to of understandour the their population. view energetics, of formation TeV PWNe history, gamma-rayand - observations are in sometimes with associated fact, HESS with PWNe have young, transformed are faint radio the pulsars predominant (e.g., [ Galactic source class of TeV emitters - the next best optionbecause for it searching is such likely that southern many sources. of these MeerKAT’s sensitivity sources will will be be very crucial faint ( PoS(MeerKAT2016)009 ]). ]) remains 7 6 Ben Stappers ]) As a consequence 8 . This emission is very likely due Fermi and references therein. 3 ]. We also plan to observe the following core-collapsed clus- 11 , the majority of them MSPs. Some clusters are spectacularly prolific: 3 ] and NGC 6652 [ 10 ]) are well-known secondary exchange binaries produced in two core-collapsed clusters. 9 http://www.naic.edu/%7pfreire/GCpsr.html See Two long observing tracks on each of these 16 clusters taken at different times to compensate MeerKAT has a similar discovery potential. Its Southern location and large collecting area will These GCs span a range of dynamical states, from low-density cores like Omega Centauri to GCs are typically very distant objects and combined with the intrinsic faintness of most MSPs, 3 for sensitivity losses due toreveal eclipses, the majority high of orbital the accelerations, pulsarswould and in correspond unfortunate these to clusters. scintillation an average will For of all 10-h the per clusters cluster, full giving tracks us (from the rise maximum to sensitivity set) that can be Two other clusters with these typesNGC of 1851 exotic [ binaries that weters propose that to are observe more too deeplyas far are they south have for high the potentialpulsar-black for GBT, hole finding namely system, new, which NGC exotic would 6397, binaries be and superb NGC for might 6752, testing include NGC gravity a theories. 362, double MSP NGC or 5946, a undetected, despite the depth ofis current not surveys. practical, Increasing because the any depthonly objects through be found longer made would integrations with be more too sensitivepulsars telescopes faint known as for coinciding illustrated follow with by up the the availability studies. step of change Progress the in GBT, can the finding number 71 of new GC MSPs (e.g., [ binaries can be disrupted andGCs we will get be partially crucial recycled to test pulsars.exchange this products: The hypothesis. normal pulsars The recycled we core pulsars will collapsechanged where clusters find for the also another in low-mass star, have these forming white many an "secondary" dwarfdwarf “exotic” companion or system. was another Sometimes neutron ex- this star, invariably other in starfor highly is which eccentric we a orbits. have massive Until multiple white now, post-Keplerian the effects only6544B, that two [ allow systems precise NS mass measurements (NGC provide a leap in sensitivity into a the large Parkes area of telescope. thesurveys sky of MeerKAT inaccessible is GCs to and about the similarly 6 GBTrich sensitive and return times to only as more the the accessible GBT. GBT, sensitive We and prioritise thanMSPs therefore GCs the with should has high most form the masses recent potential and (47 large for Parkes TucThe interaction a (NGC latter rates, similarly where two 104), more systems Omega have Centauriin been (NGC searched sensitivity with 5139), by the utilising NGC6388, GBT, a andclusters but longer is MeerKAT Liller1). that can integration they go time. have two been times detected Another in deeper reason gamma-rays with to target the aforementioned core collapsed systems and this affectswith the very pulsar dense populations cores to have much be higher found rates in of each interaction cluster. per Clusters binary (e.g. [ An Update on TRAPUM capable of recycling old neutron stars toin become MSPs. globular A clusters total to of date 146 pulsars have been discovered to the integrated gamma-ray emissionsearch from that their have MSP strong gamma-ray populations. emissionNGC2808, Other (and NGC a clusters 6093 likely we (M80), large NGC6361, propose number NGC6541, to of NGC6652 MSPs) and are NGC6717. 2MS-GC01, Terzan 5 and 47 Tuc host 34has and the 25 potential pulsars for respectively. rich Surveying and them rapid with reward. MeerKAT therefore implies that the vast majority of the pulsar population in GCs (between 600 to 3700; [ PoS(MeerKAT2016)009 Ben Stappers 50 mJy for 1-ms duration ∼ ] we find that TRAPUM will be able to 16 4 ] or the HTRU survey [ 15 ]. We have identified many regions of interest in the LMC/SMC based on 13 Jy in 2 hours for periodic sources, and a limit of µ 7 ∼ ]), this should result in a factor of 6 improvement in the number of pulsars detected. 12 ]. We have chosen 10 sources at the edge of, and beyond, the local group, where we are 14 Current models for large-scale structure formation predict that matter in the current epoch MeerKAT has the sensitivity to reveal new pulsars and fast transients beyond the Milky Way. go at least a factor of 6 deeper, and have up to an order of magnitude more observing time, greatly sensitive to any Crab-like giant7793 pulses. (3 These Mpc); hosts while range Fornax,number from of at galaxies, e.g. a and distance IC a of chance 1613best limits, to 17 (0.7 either probe from Mpc) Mpc, a Arecibo to allows [ significant NGC us fraction of to the simultaneously IGM. view Comparison a with large the the location of known pulsars, X-rayanalysis binaries, star shows formation that regions and their supernovalimited remnants. distribution number Our is of such pointings that ofthe the we bulk 400 of can both tied-array observe galaxies beams. can the8 also Using majority and be the tiled 26 of incoherent out pointings them beams simultaneously. forcoverage. in using Our the parallel calculations a A show SMC that total and we of LMC, need twice 136 so respectively, that hours in the for order above 34 flux to limit pointings, achieve and the each possible variability required of can spatial two beforms hours probed a will duration “cosmic be and required. web”. eachform observed Most the of “strands” the of baryonsof the in filaments. web, the with Detecting Universe groups pulsars residemuch and and in their signal fast clusters large-scale was transients filaments of dispersed outside by that galaxiesneeded the the intergalactic located to local medium at will probe group, begin the this and to intersections provideradio-emitting structure. determining us magnetars, how with Understanding has the tools gained the even nearbyfor more population at importance least of given some giant that of they pulse theFRB are FRBs emitting, [ and proposed or this models is further highlighted by the recent discovery of a repeating Using these systems we canstar determine formation the relationship and between their metallicity,the formation. most SMC recent and epoch Only 23 of in 29flux the pulsars density LMC). are of Using known MeerKAT it in will the be possible Magellanic to Clouds reach (6 a minimum in detectable An Update on TRAPUM realised with MeerKAT compared to previous surveys.results Compared in to the the improvement recent in Parkes the surveys, sensitivityGCs this by a (e.g., factor [ of 6. Given theFor luminosity 47 law Tuc, for this pulsars in implies thehave discovery been of discovered more already than there 100 (becausealready new of made), pulsars; scintillation so however, and the many number the faint of sheerin pulsars new number the pulsars of Parkes-only will observations sky, be the of numberfactor the of of order known 6 of pulsars improvement 10. is implies 6 For aboutpulsars, (5 the these 30 remaining in will new clusters NGC enable pulsars. 6752 the and first For 1are discoveries. the in For harder remaining NGC clusters to clusters 6397). visible calculate without with A known because theits GBT, each the declination. cluster improvements has The been Southern-most surveyedtwo to GC hours. a targeted Here, different by a depth, 10-hour the dependingset-time, track GBT and on results was the in two NGC almost tracks, 6388, twice a the total observed sensitivity. of only 320 Using h for 1.3 the would average be Extragalactic rise- required. pulsar to and transient searches individual pulses. This would result in aParkes flux limit observations about [ a factor of 7 more sensitive than the deepest PoS(MeerKAT2016)009 3 ∼ 10 thou- × ]. ) 9 22 . 0 Ben Stappers ]. MSPs that ± 7 . 26 pointing allows 2 ( / ) and varies both across the 4 − ν ∝ ]. Previous GalC surveys were in- 226h. ]. Remarkably, pulsars in the Galac- ]. Such a “laboratory” for precision τ 27 = 24 20 , 136 19 [ + 3 × 5 Survey of the GalC with the MPIfR S-band system, (i) ]. ]. One explanation has been annihilating Dark Matter in the no hair theorem ]), each pulsar allows us to probe the turbulent magnetized 29 25 23 and the GeV excess. We would search a region with diameter of 1 deg ( ], it would also enable the space-time around a rotating black hole to be Jy) MSPs [ 18 µ , ] and were focused on the very inner few degrees. However, supported by 2 the luminosity function for the longest period objects where scattering is 10 Fermi have revealed an “excess” in the diffuse emission at GeV energies (1-3 GeV) 17 / 28 > , would not only supersede all previous tests of General Relativity (GR) in the ? ]. Furthermore, mass-segregation in the central parsec may also lead to the presence 1400 Fermi ], which causes pulse broadening that reduces the sensitivity to both pulsars and S 21 30 ) of unresolved MSPs, perhaps originating from disrupted Globular Clusters [ In line with the goals defined in 2010, the aim is (a) to find pulsars in close proximity of The discovery of a pulsar closely orbiting the super-massive black hole at the centre of our In addition to using pulsar orbits about Sgr A* for high precision measurements of the cen- radio-bright ( transients. Pulse broadening is highly frequency dependent ( sensitive to MSPs [ GalC region and asbetter a to function search of at radial different frequencies. depth through the region. For this reason it would be the diffuse gamma-ray emission, we expecthigh the latitudes of bulge 5 MSP to population 10 to degrees. extend We to estimate comparatively that the bulge population contains Sgr A* to probeclearly the identifying black and characterising hole the properties,a central and and robust bulge (b) link population to to of MSPs, understand the also both establishing the GalC population by where about 7 pointings are needed to cover the region. A dwell time of 6 hr on degree scales towards the GalC [ interstellar medium in the extrememeasurements environment of around pulse the dispersion, black scatteringdiscovery of and hole. a Faraday radio-loud This rotation magnetar within is as 0.1tic demonstrated possible pc centre of by through (GalC) Sgr the also A* recent [ offer thedata possibility from of the tests of physics beyond the standard model: recently, Galactic nucleus, however, the observedsands spectrum is also fitted wellemit by in a gamma-rays large have populationveys also ( of been the shown Galactic to bulgeblack be are hole radio a can emitters, hence tantalising and be prospect as used to such to test limit targeted this Dark radio hypothesis. Matter sur- models Pulsars [ close to the 150 pc) centered onOur Sgr observing A* strategies with accommodate updated special knowledgevariations emphasis about [ on scattering from the electron-density inner arcminute centered on Sgr A*. sampling of about 1 probed with high precision and incosmic a censorship model conjecture independent fashion; for example, allowing tests of the strong-field regime [ of additional gravitational testbeds in the form of stellar-mass pulsar black hole binaries [ Galaxy, Sgr A tral black hole’s properties (e.g. [ An Update on TRAPUM enhancing the chance of detecting giant pulses.Fornax, We NGC therefore 6300, request time NGC for 7793, NGCintegrations 253, Sextans using NGC both A, 300, the Sextans coherent B, andOverall NGC incoherent this 3109, beams, results IC repeated in a thrice 1613 total to and observing allow IC time for 342, of variability. 10 1.4 of 3-hr Using pulsars to probe gravity, dark matter & stellar populations in the Galactic Centre tests of GR and black holethe physics S-Stars would [ be unrivalled by any future astrometric measurements of PoS(MeerKAT2016)009 3 ]. < 31 | b | We are 80 deg to − Ben Stappers = l regions, that can 30 deg and 2 + ≤ l ≤ 20%, this requires the detection 60 deg ∼ . We find that the difference in the − ◦ 9 | ≤ b ≤ | ◦ 6 ] covered a longitude range from 16 and 5 ◦ 5deg. We have conducted simulations to gauge the most , is the most promising. In contrast to the deepest survey 3 2 | ≤ | ≤ b | ` 18 disk MSPs). This is possible with 300 h of survey time in ∼ ≤ | ], which employed an integration of 4320 s, the greater sensitivity ◦ 3 32 − 5 bulge sources suffices to establish the detection of the bulge population ∼ Deep survey around Sgr A* at multiple frequencies with multiple passes to Galactic Bulge survey at L-band to test GalC Dark Matter hypothesis. Using ] where we assume that the spatial distribution of bulge MSPs traces the Fermi We will conduct this part of the survey within the time dedicated to the MPIfR 29 25 bulge MSPs (and level. However, in order to fully establish whether the Fermi GeV excess is caused by ∼ σ 30 deg with a latitude range of Since the first plans for TRAPUM proposed in 2010, the known pulsar population has in- The most successful survey to date, the Parkes Multibeam Survey (PMPS), combined with = + Based on these, we find that a Galactic plane survey covering of MeerKAT allows us to reduce this to 900 s. With the larger bandwidth available and somewhat be found in 30 minuteoptimal observations search with regions TRAPUM, to around extract thethe the Galactic GalC, bulge centre. at MSP approximately We population find are that a the few degrees north and south of l deg, resulting in a survey area of 540 deg creased by about 400 sources,niques or and about methods 20%. on existing This telescopes, and increasescience new has is telescopes been like enabled, LOFAR. achieved resulting With from by new pulsars, the improving new bulkthe tech- properties number of pulsars the that discovered are population, from probesratories increasing for of testing the theories surrounding of medium, gravity. orprevious As those largest MeerKAT that is dish are many used times exceptional for more labo- plane pulsar sensitive - than searches the Parkes, in birth the the placeexploring South, of the the pulsars dynamic radio search - sky. for provides The a 400 pulsarssignificant beams significant increase in combined in and the with search much rare Galactic capability, increased sharp making sensitivitysible, increase mean a but a in large-scale in survey sensitivity fact with for mandatory. MeerKAT notof A only the TRAPUM pos- inner Galactic Plane Galactic survey planeSKA will ever surveys. be conducted the and most would sensitive be survey the benchmark and testbedits for follow-up the surveys later HTRU and SUPERB [ LAT GeV excess we determined the number of bulge and disk MSPs in 4 deg our optimally chosen regions. Wesurvey note described that below. this area is highly complementary to1.5 that of Towards the a plane Galactic census efficient yield in terms of new discoveries per covered area, based on the PSRPOPpy package [ in this area, HTRU-LowLat [ at the 3 the bulge MSP population, itMSPs to will high be enough necessary accuracy. to Aiming estimate at a the statistical density error and of distribution of bulge An Update on TRAPUM less of an issue. S-band survey. (ii) aware that the required receivers areuntil not they available are. yet and (iii) that this project would not be possible expected Dark Matter distribution of detectable bulgethe and detections thick-disk MSPs of is just rather large, such that of about contend with spin-axis (geodetic) precession,S-Band eclipses, it would and be intrinsic desirable to intermittency. observecomparable 10 In luminosity. epochs addition each This to at X-band would (three result pointings each) in to an sample additional 120h and 180h, respectively. our simulations [ PoS(MeerKAT2016)009 ] ]. 39 23 ] for , Using 28 20 4 ], evapo- 40 Ben Stappers ] and the GBT [ 38 ]. It was located out of the 37 7 ]. These detections are consistent with cataclysmic 35 800 new pulsar discoveries. These numbers are naturally − ]. 36 ]). RRATs were shown to most likely be spinning neutron stars 34 ] which are exciting in themselves but also highlighted that the dynamic 33 ]. For this object, it rules out cataclysmic events: coalescing neutron stars [ 14 Note that a complementary survey of the inner Galaxy will be conducted as part of the “MPIfR S-Band Project". The confirmation of FRBs as a class has led to many models of their progenitor (see [ The fast transient landscape has changed dramatically since 2010 with the discovery of the The field of fast radio transient detection was reignited with the discovery of 11 Rotating The fast transient parameter space was further expanded with the discovery of a highly dis- )and so compared to HTRU-LowLat is reduced by factors of 100 and 20, respectively. 4 3 obs t confirmed that these were not terrestrialParkes and 1.4 provided GHz the bandpass. first detections at frequencies outside the somewhat uncertain, but in particular the improvedthis sensitivity survey to highly tremendously accelerated systems promising makes “holy for grail” of finding a pulsar-black extreme hole compact system, which binary will be systems, a superb including probe of the gravity theories [ events or a mechanismmagnetosphere. which generates Understanding rare the conditionsneutron number star in of manifestations an these is otherwise objectsGalactic crucial quiescent neutron and for star neutron their population determining star [ relationship if to there the is other a problem with the size of the population of FRBs [ radio sky is still largelycombination unexplored of and wide with FoV, high potentiallyper sensitivity, more unit and rich time wide rewards. and bandwidth frequency willsome MeerKAT’s unique making provide of it supreme the a sensitivity possible primeexciting instrument sources discoveries to are of the study transient unexpected the ones. emission transient sky. below, but We discuss history hasRadio Transients shown (RRATs, that [ the most persed millisecond transient in a 1.4 GHz Parkes pulsar survey [ our simulations, we predict about 600 In order to cover the area requested, this part of the1.6 project would Fast require transients 1350 – hours. discovering and understanding source populations with periods of 0.1–8 s.that As there more is RRATs are strong discoveredclose diversity the in to diversity the in the emission class. death patternsdetected line. argues Some and the appear RRAT While to is in be never seen extreme others, again nullers a [ and/or single old pulse pulsars or a single short sequence of pulses is Galactic plane with aGalactic dispersion ionised gas measure along significantly theand exceeding line references the of therein), sight. estimated it became With contributionsource clear similar of that that Parkes highly-dispersed are detections transients now (see were called the a FRB Fast new catalog Radio class Bursts. of radio FRBs detected at Arecibo [ summary) and ideas for their potentialRecently utility FRBs as have probes been of detected therepeat ISM at [ of frequencies other from galaxies 0.8 and the – IGM. 2 GHz and one has been shown to An Update on TRAPUM lower centre frequency (1250 MHz),up the to survey 3.5 will be times twice morefor as sensitive searches sensitive than as of PMPS. HTRU-LowLat, much At and massive the more companions. same highly This time, accelerated is the systems, because shorter( the i.e. integration computational time load allows those scales strongly in with tighter observing orbits time and/or more PoS(MeerKAT2016)009 ]. 43 . If prompt 1 Ben Stappers − -ray emission is γ 600 yr ∼ ]). However, there may ] are responsible. 42 45 -ray emission, MeerKAT will γ FRBs the dispersion measure distri- We will carry out commensal observ- + ]. The Fly’s Eye search (Alan Telescope 100 47 ∼ 8 ] or atmospheric phenomena [ ]. Constraints on scattering and scintillation have countered 44 ]. 43 28 ]. GW progenitors have potential electromagnetic counterparts 46 -ray quiet detections of these orphaned GRBs would allow the deduction γ ], or collapsing supra-massive neutron stars (e.g. [ 41 1 second) time scales, radio transient studies have long focused on the rich science > ]) points each antenna in a different direction to incoherently search a large area of sky. 48 The recent discovery of gravitational waves (GW) with LIGO provides radio astronomers with Accurately localising FRBs on the sky with the TRAPUM multi-beam searches enables their On slow ( Crucially compared to most other transient surveys, MeerKAT transient surveys using multiple another incredible opportunity [ not detected. Radio-loud/ of the true underlying rate. Array; [ We describe below three modes ofCommensal-Transient-Searches-on-Pulsar-Searches operation. Mode: ing for fast transients on all of the TRAPUM observations proposed here: Galactic plane and host galaxies to be unambiguouslywhich, identified. in The tandem redshift with can theformed. then precisely measured be The dispersion determined first means in of new the(including these cosmology optical, the is tests so-called "missing can to baryons") be ‘weigh’ is per- what the causes baryons the FRB’s in characteristic the dispersion [ IGM; the ionised component of these achievable with follow up of SNe and GRBs. GRBs are detected at rates of tied-array beam modes will haveously resolution associate of events a with sources few in arcseconds differentthan or wavebands. some better, Arguably, MeerKAT other sufficient has suitable a to smaller pathfinders unambigu- FoV butand as as the MeerKAT full has FoV a is significantlymodes, computationally higher it challenging sensitivity is to and an explore, outstanding can instrument berare for used bright the in survey events coherent for (such and transient as sources. incoherent Lorimerwith Furthermore, bursts fast to or imaging, find the sub-arraying, the and prompt forming emissionalso incoherent of already sums begun GRBs) commissioning and there a Fly’s are modest Eye "fast possibilities modes.ing imaging" searches Our correlator for mode team transients that has can over perform the imag- entire field of view [ As the sample of FRBsthe detected strands of in the this cosmic waymap web grows for which one will each should be redshift be traced value. able on With the to a sky ‘see’ large in sample clustering the of due FRB to dispersion measure sky radio emission is associated with thesedetect GRBs, approximately and beamed one like per the beamed, year. allowing the The detection of expectation rapid is, transients however, associated that with GRBs the whose radio emission is not with both fast coherent radiocorrelation pulses with and events slow from synchrotron GW afterglows.events, detectors will but Their not detection is only and likely shed cross- galaxies. the light Some on only models the of way nature FRBs to of predictwould that such localize truly coordinating extreme revolutionise GW with our GW events understanding and of optical in GWs, afterglow order networks FRBs, the to IGM, locate and much any more. associated host An Update on TRAPUM rating black holes [ indeed be multiple classes of FRBssuggestions [ that Galactic flaring stars [ bution as a function ofthe dark redshift energy can equation be of state made.in parameter. other This The wavelength gives shape regimes) a for unique of method measuringany. this (and More this distribution orthogonal details parameter, depends to can and efforts be directly its found on redshift-dependent in variation [ if PoS(MeerKAT2016)009 , ) 5 2 σ ± rela- 13 S 2 deg . ∼ log 51 − Ben Stappers = ], to be 10 N 49 64 × 8 . Alongside the sheer increase in the number of 9 ] to get positions to a few arcminutes. Compared with 50 30 new detections in 720h. Discovering these bright bursts ∼ ) FRBs with a MeerKAT Fly’s Eye experiment. Comparing the dif- σ . Based on the first discovery a rate of bright events of 225/sky/day σ 5, we estimate a total detectable FRB rate (above a conservative 9 Lorimer-bursts. Making the simplest assumption of a log . 400- 1 ∼ > − and bandwidth of the single MeerKAT dish and Parkes we very conservatively We consider here the exciting possibility of the detectability of Lorimer-burst sys 0384 . 0 × 10 bursts in the incoherent and tied-array modes respectively. This is a significant increase ± 1 FRB/day, and a total yield of ∼ and 20 on the current known population andhave using our positions transient of buffer a and few imagingover capability arcseconds the they or present will better situation. all based onFly’e-Eye the Mode: burst alone, anbrightness enormous (30 improvement Jy and ferences in gain, T the ATA Fly’s Eye experiment, our proposedmore sensitive experiment while will also be covering more a thanDeep-Searches-of-Known-FRB-Locations significant an Mode: fraction order of of the magnitude sky. assume that it is 15 timesLorimer-burst less at sensitive. above Thus 27 a single MeerKAT antenna would have detected the was calculated, which agrees withthe new the detections. current In FRB Fly’s Eye rates mode, and MeerKAT will the instantaneously rarity cover 0 of Lorimer-bursts among An Update on TRAPUM Centre, High energy point sourcesrich and and SNRs, varied globular locations clusters to and searchsum external for of galaxies. all all sorts These of 64 offer transients. dishes to Insources, all in achieve cases parallel a we we wide will will field use use ofThis the the view, combination incoherent 400 but allows tied-array for lower beams effective sensitivity, determination to to of do lookthere luminosity narrower may for relations but be with rare much an one brighter deeper survey. apparent searches. While orsar real search dearth provides of an FRBs excellent and detected uniform throughsufficient way the sensitivity to Galactic to determine plane, be whether the this able is deep todearth. true. pul- detect It a The will few Galactic also FRBs plane have which pulsar helptransients search such clarify will as if, also RRATs, and radio provide why, emitting a there magnetars,classes is rich flare of such region stars, transients. a to active The binaries, search searches novae for away andnities from Galactic any the to fast new plane find discussed transients above in provide excellent those(see opportu- regions below) or has in already the been Universeon-sky successful beyond. time in The and revealing follow sensitivity a up will new ofwill reveal FRB known add more FRBs to and sources. on-sky here time Similarly too at the a thefollow-up range follow combination timing of up Galactic of will timing latitudes. allow observations The the multipleare visits opportunity discovered, planned to but for also searches not provide and only sensitivity tothe check sources repeating the which FRB variability show and longer of some timescale new RRATs.Parkes variability, sources like The and single that the pulse observing sensitivity times is willbe a be possible factor significantly to of longer more about than than 6FRBs the double better that GBT the than we and known will so RRAT detect population. we in these expect Our commensal it simulations observations, will for based on the the number rate of from [ or 0.00128 of the sky.becomes 225 An observing time oftion 720h with an corresponds index to of 0.0384of sky days and the yield provides crucial information on thethe luminosity local distribution IGM and and potentiallymode, the very by host useful choosing probes galaxy. the of appropriateour While pointing multi-beam the locations localisation for localisation techniques the will [ telescopes not it be will particularly be possible good to in use this PoS(MeerKAT2016)009 Ben Stappers ]. Our experience with LOFAR has 52 10 1000 pulsars discovered by TRAPUM, across all the − 800 ]. These bursts are characterised by a range of flux density and ∼ 51 After the initial discovery of a pulsar, most of the science can only be extracted by follow-up One of the crucial advantages of finding pulsars with an interferometer compared to single shown that even when the pulsarin is follow-up found observations in to an give incoherentfor an beam, binary accurate we pulsars, position can more use for frequent the observations subsequentTiming may tied-array of observations. the be beams MSPs needed We requires note to the determine that pulsarit the timing will beams binary be and parameters. possible hardware, to however for use thewe the slower are pulsar pulsars providing search and beams thus (that is allowingfind we us that don’t to need for potentially coherent time an dedispersion) a that estimatedsearches number proposed total of here, pulsars of of simultaneously. which We approximatelytotal 10% of are 500 expected hours to is be required in for binaries, initial we follow find up that timing a observations. timing. Therefore, it is an absolutelyget crucial a aspect timing of solution. characterising theperiod In new derivative TRAPUM its so pulsars that most to one basic canand form compare this in the means pulsar particular getting properties for an withknowing those the their accurate characteristic known position, sources ages pulsar period and that population, their and areenergy spin-down emission, energies found for to example. compare in with We our are the alsopotentially SNRs targeted interested high and in searches high precision determining timers we whether and or are sobinary not useful systems the interested for sources and in gravitational are so wave potentially searches, useful and/or for members mass of determinations or tests ofdishes, gravity. is the narrow beam ofstarts the with tied-array a beam it precise is position. discoveredtween This in, the removes which positional a means uncertainty large that and one degree the period-derivative already ofup and observations the so in ambiguity one order need that to not obtain usually have a exists as coherent be- many timing follow solution [ strongly varying spectral indices and athe wide detection range of of any modulation possible indices underlying that periodicity.from have The a so repeating cataclysmic far nature indicates prevented event that and they suggest arestar that not origins, at least like some magnetars FRBs or aremeans giant possibly pulses for associated from the with radio neutron FRB pulsars. populationmultiple Crucial as classes. to a It understanding is whole what also is this essentialthey determining to are if be associated able all with to FRBs galaxies, localise repeatUsing and these or where bursts 200 accurately possible whether hours to determine there of be where are observing ableallow in to time us the see to galaxies if to follow they place up occur. buffer known stronger data FRBs will limits allow at on us the to any MeerKAT getone sensitivity better repeat to would localisations follow bursts for up any while a repeat significant forming bursts.strong sample limits Two of images hundred on 20 any hours from sources underlying allows pulse each the energy forbe distribution. transient 10 an The hours, follow which hour up will observations in will providepossible. typically crucially duration Working and with distributed ThunderKAT would logarithmicallyto also in understand allow the time one radio to to properties use sample of the any as simultaneous host. many imaging data timescales as 1.7 Follow Up Timing: An Update on TRAPUM FRBs detected the other major developmentboth is at that Arecibo FRB and 121102 with has the GBT exhibited [ repeated bursts seen PoS(MeerKAT2016)009 Ben Stappers 11 Given the various observing modes, we have highlighted the observing strategy in detail for Funds obtained by the MPIfR internally and from the Max-Planck Society will enable the im- each individual science goal above. Intied-array general all beams observations and will the use the incoherentMoreover combination there beams of will the when be 400 undertaking a real-time pulsarthen search and more undertaken fast using detailed transient the searches, available searches. capability. processing offline, hardware using The and size the of temporaryand this storage then storage capacity require buffer 2-3 and will days extrathe allow to computing next about process pulsar and 24 search so hours observations thatof of can will day observation take place when to some place. pulsar be scheduling searchany stored In restrictions observations transients general on take there when that place, is are but nomode found to where restriction take some we on advantage night will the of use time time the opticalbeams. would 64 follow Thus dishes be up the independently useful. of processing and requirements sotime. The are they appear Also, reduced exception as here for is if and the they the all Fly’sat are Eye processing Fly’s 64 night observations will Eye different the to be majority allow done of for inthe the real the observing observing possibility strategy, time the for would observing simultaneous preferably timearea. optical be request is detection. This discussed does in As not detail with include forour the calibration each integration discussion individual or times science of slewing are time, long, the andthe we latter WSRT and typically is the have small VLA many (much have nearby shown lessabout pointings. that than 30 to Our minutes 1%) phase experience of as up with observing the time arraythe for for calibration beam-forming a overhead typically 24 is requires h about run, 2-3%. so assuming scheduling blocks of that duration 2.2 Observing strategy and time request: 2.1 The 400-beam beamformer and real-time/offline processing resources plementation of S-band receivers (see elsewhere inother these things, proceedings enable for deep more pulsar details) searches to,funds in amongst the obtained Galactic by plane Stappers and through Galactic anTRAP centre. European project Combined Research with (see Council elsewhere Advanced in Granttied-array for these beamformer the proceedings), Meer- and also computing support resources thetargets for proposed development the here, of for storage a off-line of 400-beam acceleration long/deep,time processing. observations search The MeerTRAP of for funding the pulsars enables and awhich fast real- can transients store in thirty parallel seconds andtransients of the and data the implementation from better of each characterisation a of ofthe transient the the dispersion, transients. buffer MeerKAT dishes width The and to polarisation addition be characteristics of usedity of the for to localising 400-beam perform beamformer the and Galactic offlineacceleartion plane processing searches search that enables in will the reasonable be abil- observing used time for and the also plane and enables globular the cluster crucial searches. An Update on TRAPUM 2. Achieving the proposed science goals We outline below the details of the approach we will implement to achieve these science goals. PoS(MeerKAT2016)009 , leading s µ Ben Stappers ]) to filter out the most likely pulsars 53 12 The transient search processing will be undertaken at the same time as the real-time pulsar Triggering of the individual telescope transient buffers will result in data spanning the duration TRAPUM includes its own commensal observing, that is, it will undertake transient searches The data processing challenges associated with TRAPUM will build on the development of This pulsar search raw data product is too large to be archived (i.e. in total more than 250 2 PetaBytes of storage acquired through the MPIfR/MeerTRAP grants. Up to 24 h of data will be search. The added challengereal-time of and the output transient the pipeline contents is ofas the that quickly transient as we buffers possible. will and need trigger ThederKAT/4piSky. MeerKAT to mechanics and The generate of other output this triggers facilities data process in willstored products be for will built further consist on assessment mainly those with ofciently established improved candidates, interesting by algorithms. Thun- a which For piece will those of also detectionsepoch the will deemed be be time-frequency-polarisation to added data be to suffi- cube thevery surrounding similarly long the to term the transient archive. real The timeual Fly’s transient Eye detection telescope mode mode, inputs where observations and in will so this bethe case the processed tied-array there data searches. will rates The be and output 64 data individ- processing products requirements and will archiving be plans will lessof be than the the those same. dispersed for event, toimaged be in distributed near to real the timetransient pipelines data at like storage high those identified developed time for above. The resolution. LOFAR/ThunderKAT. formed image data These and The will tied-array data transient beam- be will will archived.they be be will Storing be identified the kept using for raw imaging a telescope few data months. long term will2.4 not Commensal be Observing: possible, but commensally on all its pulsarEye search mode and FRB observations follow require up adifferent observations very described directions specific above. and observing The so set Fly’s they up cannot with be the carried dishes out pointed in in a many commensal mode, but other projects, and fast transients. All candidates willcan be be stored, as re-analysed they with are new sufficientlyof small machine these volume, learning so data that algorithms. products they thatPetaBytes. We we have will a implement definition and and we description have funding for long term archive of 2.5 pulsar and fast transient search pipelinesand for surveys the like HTRU-N/S, SKA. SUPERB, In PALFA, LOTAAS allbeams observations each apart with from 4096 Fly’s frequency Eye channels, we digitised will to be 8-bits operating and with sampled 400 every 64 tied-array Petabytes), however we will keep athe data version volume) with for potential reduced reprocessing frequency and and confirmations.pulsar time candidates, The main resolution including data (100th folded product will of and beuse dedispersed sets our data of state-of-the cubes, art and machine associated learning metadata. algorithms We (e.g. will [ An Update on TRAPUM 2.3 Plan for creating and archiving the scientific data product: to a total datatime rate commensal searching of for 24 fast radio GByte/s.pulsars transients in and binary pulsars These and systems. data offline∼ processing will The to real-time be search and for analysed offline in analysisrecorded three will for offline use different processing the which ways: will hundreds take of Real- place GPUs while the and telescope is pursuing other projects. 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