Nançay Pulsars instrumentations. Nançay observations
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1 Nançay Pulsars instrumentations and observations Ismaël Cognard, CR Gilles Theureau, AA Grégory Desvignes, PhD Rob Ferdman, PostDoc Alessandro Corongiu, PostDoc Workshop PULSARS Theory and Observations, Paris Obs., Nov 24-26th 2008 Nançay observations
2 A brief pulsar history with the Nançay Radio Telescope EPTA GLAST HESS Scientists and Collaborations Lestrade, Bourgois Cognard Instrumentations and evolution of the number of pulsars observed at Nançay Lestrade Cognard Maitia Cognard Theureau Desvignes Cognard Cognard (Smith) Ferdman (Lestrade) Theureau (Dumora) Corongiu (Guillemot) (Hamidouche) Cognard UCBerkeley NRL Washington NBPP sweptlo telescope UPGRADE BON
3 Instrumentations No way to get data without instrumentations
4 Pulsar timing instrumentations at Nançay NBPP SWEPT LO BON
5 old BON instrumentation from 2004 to 2008 a coherent pulsar dedispersor called BON (Berkeley-Orléans-Nançay) a 128MHz spectrometer SerendipV 2 complex polars digitized at 128Ms/s a dedispersion computer 4 dataservers for data distribution cluster a 64-nodes Linux cluster of bi-proc Athlon 1.2GHz a bandwidth of 64MHz was processed installed in 2001!
6 How to get more computing power per Watt, per cm3,... per?
7 More computing power Use of GPU (Graphics Processing Unit) Nvidia GeForce 8800GTX Stream processors Memory Memory bandwidth Memory interface Core clock Shader clock Memory clock MB 86.4GB/s 384bits 575MHz 1350MHz 900MHz Use of CUDA SDK (Compute Unified Device Architecture - Software Development Kit)
8 March 2008 : a prototype (one CPU) Built with great help from P.Lespagnol, Nançay Gigabyte N680SLI-DQ6 + 2x 8800GTX + watercooling ~2k
9 April 2008 : an evolving prototype (dual-cpu + PCI-X 133/100MHz) Supermicro X7DWA-N + 2x EDT-PCICDa + 2x 8800GTX (+ watercooling) ~2.5k
10 May 2008 : data path is validated IN from spectrometer 2Gb/s OUT on disk 200kb/s
11 June 2008 : an operational system for 128MHz SerendipV (with only 2 units!) Supermicro X7DWA-N + EDT-PCI-CDa + 2x 8800GTX + watercooling
12
13 Next large bandwidth coherent pulsar dedispersor direct sampling of the Nançay MHz IF 400MHz usefull bandwidth ~ 1 MHz channels based on iadc and IBOB (or ROACH) provided by CASPER, Berkeley IBOB : Virtex2, 2x Z-DOK connectors, 2x 10GB ethernet links FPGA code being developped by Peter MacMahon, KAT IBOB
14 Next large bandwidth coherent pulsar dedispersor ROACH : Virtex5, PowerPC, 2x Z-DOK connectors, 4x 10GB ethernet links presently in final integration at Berkeley ROACH
15 Next large bandwidth coherent pulsar dedispersor Tests already started with IBOB (in Sept 2008) the final ROACH version should be operational mid GbE Gore cable 800MHz clock ibob PC + 10GbE card (+ GPU)
16 Observations Such a strong effort to design and build a very dedicated instrumentation would probably make a heavy use of the Nançay telescope
17 Nançay Pulsars observations schedule
18 pl us de ob se rv a tio ns su r pl us de 20 0 pu lsa rs en 4 an s
19 Nançay Scientific programs (2008B allocation) Multi-scale Gravitational Waves detection (1040hr) EPTA MoU Very low frequency GW (background) via a set of highly stable millisecond pulsars with the EPTA author list includes all the EPTA members! Low frequency GW emitted by relativistic binary systems via Double Neutron Star monitoring usually Gravitational Theories tests High 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) GLAST MoU radio monitoring of young and noisy pulsars to ensure a good folding of the very few high energy photons crashing 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 MHz(0.25MHz) 30min 80<l<170 deg -1<b<+1 deg 2009 : 4000h, 400MHz(0.25MHz), 32 s, 30min) Total ~ 1600 hours/semester ~ 50% of available telescope time
20 Very low frequency GW Use a set of highly stable pulsars to probe the cosmological background of gravitational waves
21 The EPTA is based on a unique feature in Europe : the availability of 4 (and soon 5) 100-m class radiotelescopes INAF Osservatorio Astronomico di Cagliari, IT Max-Planck Institut fur Radioastronomie, GER University of Manchester, JBO, UK Paris-Nançay Observatory, FR ASTRON, NL
22 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, Orléans, France 2 Osservatorio Astronomico di Cagliari, Italy 3 Astronomical Institut 'Anton Pannekoek', Netherlands 4 MPI fur Radioastronomie, Germany 5 University of Manchester, United Kingdom
23 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 Nançay joined in October 2006 How works the EPTA? regular workshops at the different telescopes : Nançay (Oct 2006), Cagliari (May 2007), Bad Honnef (Jan 2008)... next is Manchester (Sept 2008) monthly video-conferences (EVO) since Feb 2008 actions Coordinated source lists and partly-coordinated observing sessions Time Of Arrivals (TOAs) and templates (and later raw data) shared among partners Library 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
24 Westerbork PUMA II 8x20 MHz sub-bands splitted in 16/32/64 channels, two complex polarisations, 8 bits coherent dedispersion 32x 2.0GHz dual-opteron + 8x4 TB disk space WSRT 96 m m dishes Summed in phase to form Tied-Array 15% pulsar
25 Jodrell Bank incoherent filterbank 64x1MHz JB 76 m recently resurfaced dish 70% pulsar COBRA II Serendip5 based : expect 64MHz for DM<230 dual quad-core computers future instrumentation based on ATNF DFB3 may use HYDRA (144-nodes dual quad-core) Digital Filterbank DFB3 from ATNF (BW=1GHz, fully programmable FPGA system)
26 Effelsberg dish 100m EBPP coherent dedispersor 112MHz 32x3.5MHz dual polarisation, 4bits future instrumentation based on ATNF DBF3 New 7 beam receiver MHz 15% pulsar
27 Cagliari a 64m antenna still in construction active primary mirror GHz future instrumentation based on ATNF DFB3 MANGUSTA 280 AMD Opteron 2.6GHz CPUs summer 2008
28 44% pulsar Nançay NRT 94 m collecting area 35x200m Kraus design GHz BON (Berkeley-Orléans-Nançay) 128 MHz from Serendip5 spectrometer, two complex polarisations 8 bits coherent dedispersion on GPUs
29 LEAP : Large European Array for Pulsars 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 sky It will test limits of sensitivity and pulse jitter It also provides excellent tests of SKA-like pulsar observing
30 Multi-wavelength study A large number of high energy instruments are now available HESS (HESS-II) FERMI-GLAST A need for accurate and up-to-date radio ephemeris on young and noisy pulsars is emerging more than ever
31
32 Giant Pulses from the Crab pulsar were used to test the FERMI-LAT pulsar timing sofware Smith et al, 2008, A&A in press
33 The four best milliseconds pulsars observed at Nançay J ns B ns J ns B ns no DM correction
34 A recent result from EPTA on double neutron star system PSR J the different datasets NRT Eff WSRT constrains on masses and inclination angle of the orbit JB GB Janssen et al., A&A 490, 753
35 Simultaneous observations of the Crab Pulsar in radio and optical optical-radio lag 255±21μs Oosterbroek, Cognard et al. A&A 488, 271
36 Double neutron star PSR J U PPA= arctan 2 Q Desvignes et al., 2008, in prep
37 PSR B P=5.362ms DM=13.305pc.cm-3
38 PSR B the pulsar with planets 3 planets : A, B and C due to 3:2 resonnance, B and C show time variable orbital parameters no perturbed planetary motions in 'tempo' yet! residuals obtained without perturbation
39 Conclusion The large Nançay radiotelescope has now one of the best pulsar coherent instrumentation in the world It's diffinitively possible to observe many pulsars of different kind So... as in January 2006, that's a call for collaborations/ideas/help/...
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