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  • Workshop PULSARS Theory and Observations, Paris Obs., Nov 24-26th 2008 Nanay observations

    Nanay Pulsars instrumentationsand observations

    Ismal Cognard, CRGilles Theureau, AAGrgory Desvignes, PhDRob Ferdman, PostDocAlessandro Corongiu, PostDoc

  • Lestrade, BourgoisCognard








    A brief pulsar history with the Nanay Radio Telescope


    NRL Washington

    UCBerkeleyInstrumentations andevolution ofthe number of pulsarsobserved at Nanay


    Scientists and Collaborations

    telescope UPGRADE


  • Instrumentations

    No way to get data without instrumentations

  • Pulsar timinginstrumentationsat Nanay

    NBPP 1998-2003

    BON 2004-...

    SWEPT LO1988-2005

  • old BON instrumentationfrom 2004 to 2008

    a coherent pulsar dedispersor calledBON (Berkeley-Orlans-Nanay)

    a 128MHz spectrometerSerendipV 2 complex polars digitized at 128Ms/s

    a dedispersion computer4 dataservers for data distributioncluster a 64-nodes Linux cluster of bi-proc Athlon 1.2GHz

    a bandwidth of 64MHz was processedinstalled in 2001 !

  • How to get more computing powerper Watt, per cm3,... per ?

  • More computing power

    Use of GPU (Graphics Processing Unit)Nvidia GeForce 8800GTX

    Stream processors 128Memory 768MBMemory bandwidth 86.4GB/sMemory interface 384bitsCore clock 575MHzShader clock 1350MHzMemory clock 900MHz

    Use of CUDA SDK (Compute Unified Device Architecture - Software Development Kit)

  • March 2008 : a prototype (one CPU)Built with great help from P.Lespagnol, Nanay

    Gigabyte N680SLI-DQ6 + 2x 8800GTX + watercooling ~2k

  • April 2008 : an evolving prototype (dual-CPU + PCI-X 133/100MHz)Supermicro X7DWA-N + 2x EDT-PCICDa

    + 2x 8800GTX (+ watercooling) ~2.5k

  • IN from spectrometer2Gb/s

    May 2008 : data path is validated

    OUTon disk


  • June 2008 :an operational system

    for 128MHz SerendipV(with only 2 units!)

    Supermicro X7DWA-N+ EDT-PCI-CDa+ 2x 8800GTX + watercooling

  • Next large bandwidth coherent pulsar dedispersor

    direct sampling of the Nanay 100-500MHz IF400MHz usefull bandwidth ~ 1 MHz channelsbased on iADC and IBOB (or ROACH) provided by CASPER, Berkeley

    IBOB : Virtex2, 2x Z-DOK connectors, 2x 10GB ethernet linksFPGA code being developped by Peter MacMahon, KAT



    ROACH : Virtex5, PowerPC, 2x Z-DOK connectors,4x 10GB ethernet links

    presently in final integration at Berkeley

    Next large bandwidth coherent pulsar dedispersor

  • iBOB

    800MHz clock

    PC + 10GbE card (+ GPU)

    10GbE Gore cable

    Next large bandwidth coherent pulsar dedispersorTests already started with IBOB (in Sept 2008)

    the final ROACH version should be operational mid-2009

  • Such a strong effort to design and builda very dedicated instrumentation

    would probably make a heavy use of the Nanay telescope


  • Nanay Pulsars observations schedule

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  • Multi-scale Gravitational Waves detection (1040hr)Very low frequency GW (background)

    via a set of highly stable millisecond pulsars with the EPTAauthor list includes all the EPTA members !

    Low frequency GW emitted by relativistic binary systemsvia Double Neutron Star monitoring usually

    Gravitational Theories testsHigh frequency GW emitted by the neutron star oscillations triggered by glitches

    via monitoring young pulsars and alert sent to VIRGO/LIGO

    Multi-wavelength study (390hr)radio monitoring of young and noisy pulsars to ensure

    a good folding of the very few high energy photonscrashing from time to time on LAT/GLAST detectors during years...

    Globular Clusters pulsars (32hr)Proper motions of GC pulsars

    Survey of the Galactic Plane (160hr)Pilot during 2008 128MHz(0.25MHz) 30min


  • Very low frequency GWUse a set of highly stable pulsars

    to probe the cosmological background of gravitational waves

  • University of Manchester, JBO, UK


    Max-Planck Institut fur Radioastronomie, GERINAF Osservatorio Astronomico di Cagliari, IT

    Paris-Nanay Observatory, FR

    The EPTA is based on a unique feature in Europe :the availability of 4 (and soon 5) 100-m class radiotelescopes

  • Members of the European Pulsar Timing Array (EPTA)

    I.Cognard1, G.Desvignes1, M.Burgay2, A.Corongiu1,N.D'Amico2, R.Ferdman1, R.vanHaasteren3, J.Hessels3,

    G.Janssen3, A.Jessner4, C.Jordan5, M.Kramer5,L.Kuo5, K.Lazarides4, A.Lyne5, M.Pilia2,

    A.Possenti2, M.Purver5, B.Stappers5, G.Theureau1 1 LPCE-CNRS, Orlans, France

    2 Osservatorio Astronomico di Cagliari, Italy3 Astronomical Institut 'Anton Pannekoek', Netherlands

    4 MPI fur Radioastronomie, Germany5 University of Manchester, United Kingdom

  • Why the EPTA ?to achieve a better combined sensitivity to Gravitational Waves and

    take advantage of this concentration of large telescopes and experts,a Memorandum of Understanding (MoU)

    was signed in Januay 2006 and Nanay joined in October 2006

    How works the EPTA ?regular workshops at the different telescopes :

    Nanay (Oct 2006), Cagliari (May 2007),Bad Honnef (Jan 2008)... next is Manchester (Sept 2008)

    monthly video-conferences (EVO) since Feb 2008actions

    Coordinated source lists and partly-coordinated observing sessionsTime Of Arrivals (TOAs) and templates (and later raw data) shared among partnersLibrary of common synthetic multi-frequency templates

    (based on excellent experience with double pulsar timing)Open to international collaboration (sharing TOAs for joint goals)MoU with australian PPTA in preparation ;

    hope to reach similar agreement with US NANOGrav

  • Westerbork

    WSRT 96 m14 25-m dishes Summed in phase to form Tied-Array

    PUMA II8x20 MHz sub-bands splitted in 16/32/64 channels,two complex polarisations, 8 bitscoherent dedispersion

    32x 2.0GHz dual-Opteron + 8x4 TB disk space

    15% pulsar

  • Jodrell Bank

    JB 76 mrecently resurfaced dish

    incoherent filterbank64x1MHz

    COBRA IISerendip5 based : expect 64MHz for DM

  • Effelsberg

    dish 100mEBPP coherent dedispersor

    112MHz 32x3.5MHzdual polarisation, 4bits

    future instrumentationbased on ATNF DBF3

    New 7 beam receiver1290-1430 MHz

    15% pulsar

  • Cagliari

    MANGUSTA280 AMD Opteron 2.6GHz CPUs

    a 64m antenna still in constructionactive primary mirror0.3-100GHz

    future instrumentationbased on ATNF DFB3 summer 2008

  • Nanay

    NRT 94 mcollecting area 35x200mKraus design1.1-3.5GHz

    BON (Berkeley-Orlans-Nanay)128 MHz from Serendip5 spectrometer,two complex polarisations 8 bitscoherent dedispersion on GPUs

    44% pulsar

  • To achieve even better sensitivity to GWs we are planning on combining all the telescopes coherently

    That gives a telescope with a sensitivity equivalent to Arecibo, but able to see much more of the skyIt will test limits of sensitivity and pulse jitter

    LEAP : Large European Array for Pulsars

    It also provides excellent tests of SKA-like pulsar observing

  • Multi-wavelength study

    A large number of high energy instrumentsare now available


    A need for accurate and up-to-date radio ephemerison young and noisy pulsarsis emerging more than ever

  • Smith et al, 2008, A&A in press

    Giant Pulses from the Crab pulsarwere used to test the FERMI-LAT pulsar timing sofware

  • The four bestmilliseconds pulsars observed at Nanay

    J1909-3744 410ns

    J1600-3053 542ns

    B1937+21 203ns

    B1713+07 496ns

    no DM correction

  • A recent result from EPTA ondouble neutron star system PSR J1518+4904






    the different datasets

    constrains on masses and inclination angle of the orbit

    Janssen et al., A&A 490, 753

  • Simultaneous observationsof the Crab Pulsarin radio and optical

    Oosterbroek, Cognard et al. A&A 488, 271

    optical-radio lag 25521s

  • Double neutron star PSR J1906+0746



    Desvignes et al., 2008, in prep

  • PSR B1855+09


  • PSR B1257+12 the pulsar with planets

    3 planets : A, B and Cdue to 3:2 resonnance,B and C show time variable orbital parameters

    no perturbed planetary motionsin 'tempo' yet !

    residuals obtained without perturbation

  • Conclusion

    The large Nanay radiotelescope has now one of the bestpulsar coherent instrumentation in the world

    It's diffinitively possible to observe many pulsarsof different kind

    So... as in January 2006,that's a call for collaborations/ideas/help/...


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