Slide 1

Harald Schuh (Chair of the IVS Directing Board) Dirk Behrend (Director of the IVS Coordinating Center) The International VLBI Service for Geodesy and Astrometry and VLBI2010 Korea, August 2007 Slide 2 Evolvement of Space Geodetic Techniques (1) Progress in accuracy of space geodetic techniques -1960 Satellite Triangulation (first global network)~10 m -1970 Satellite Laser Ranging 1. Gen.~1 m TRANSIT (Doppler)~ 0.5 1 m -1980 Satellite Laser Ranging 3. Gen.~3-10 cm Very Long Baseline Interferometry (Mark III)~3-10 cm -1990 SLR/VLBI/GPS progress~1 cm -2000 Combination space geodetic techniques~3 mm -2010 Goal Evolvement of Space Geodetic Techniques (2) Progress is based on technology developments of the last decades -Laser technology -Signal processing -IT developments (VLBI: data recording, ) -T&F (atomic clocks, frequency generator, time transfer) -... => High accuracy opens new fields for research and multidisciplinary applications Slide 4 Changing Earth Mantle convections -Plate motion -Volcanism Sea level rise Ice melting Tides (Moon, sun, planets) -Ocean tides -Earth tides Ocean -Mass transport -Loading Atmosphere/Wind -Mass transport -Loading -Friction Groundwater changes Variations in Geometry (Kinematic), Gravity Field, Earth Rotation Slide 5 Continuous geodetic observations required Monitor the variations on the Earth Improve the models (predictions) Understand geophysical phenomena Maintain global reference frames for positioning on Earth and navigation in space -Quasars, stars, planets, Moon... -Spacecrafts, satellites,... -Geodesy -Geo-Information -Navigation -... => IAG: GGOS (Global Geodetic Observing System) -one global reference frame, precision 10 -9 -consistent in geometrical and physical parameters Slide 6 http://www.ggos.org/ Slide 7 EOP: Earth Orientation Parameters Precession/Nutation Polar motion UT1 - UTC ICRF: International Celestial Reference Frame Quasar positions ITRF: International Terrestrial Reference Frame Positions Velocities Time series Reference Frames Slide 8 VLBI (Very Long Baseline Interferometry) SLR/LLR (Satellite/Lunar Laser Ranging) GNSS (GPS, GLONASS, future: Galileo) DORIS (Doppler Orbitography and Radio Positioning Integrated by Satellite) VLBI SLR/LLR GNSS/GPS DORIS Space Geodetic Techniques Slide 9 May 2, 20074th IVS Technical Operations Workshop 9 Unique technique for CRF Celestial pole UT1-UTC Primary technique for EOP (complete set of parameters) TRF (most precise technique for long baselines, scale) Very Long Baseline Interferometry Slide 10 Very Long Baseline Interferometry (VLBI) plays a fundamental role for the realization and maintenance of the global reference frames and for the determination of the EOP: Strengths of VLBI VLBI allows observation of quasars which realize the CRF VLBI provides complete set of EOP and is unique for the determination of DUT1 and long-term nutation VLBI provides precisely the length of intercontinental baselines, which strongly support the realization and maintenance of the TRF with a stable scale Slide 11 May 2, 20074th IVS Technical Operations Workshop 11 IVS is a Service of IAG - International Association of Geodesy IAU - International Astronomical Union FAGS - Federation of Astronomical and Geophysical Data Analysis Services IVS goals: To provide a service to support geodetic, geophysical and astrometric research and operational activities To promote research and development in the VLBI technique To interact with the community of users of VLBI products and to integrate VLBI into a global Earth observing system Main tasks of the IVS are: coordinate VLBI components, guarantee provision of products for CRF, TRF and the set of EOP IVS inauguration was on March 1 st, 1999 ~80 permanent components supported by ~40 institutions in ~20 countries ~280 Associate Members I V S - International VLBI Service for Geodesy and Astrometry Slide 12 May 2, 20074th IVS Technical Operations Workshop 12 IVS Organization Slide 13 May 2, 20074th IVS Technical Operations Workshop 13 IVS Member Organizations Australia Austria Brazil Canada Chile China France Germany Italy Japan Norway Russia South Africa Spain Sweden Ukraine USA Geoscience Australia University of Tasmania Vienna University of Technology Centro de Radio Astronomia e Aplicacoes Espaciais Space Geodynamics Laboratory Geodetic Survey Division, Natural Resources Canada Dominion Radio Astrophysical Observatory Canadian Space Agency Universidad de Concepcion Universidad del Bio Bio Universidad Catolica de la Santisima Concepcion Instituto Geografico Militar Chinese Academy of Sciences Observatoire de Paris Observatoire de Bordeaux Deutsches Geodtisches Forschungsinstitut Bundesamt fr Kartographie und Geodsie Forschungseinrichtung Satellitengeodsie, TU-Munich Geodetic Institute of the University of Bonn Germany Istituto di Radioastronomia INAF Agenzia Spaziale Italiana Geographical Survey Institute National Institute of Information and Communications Technology National Astronomical Observatory of Japan National Institute of Polar Research Norwegian Defence Research Establishment Norwegian Mapping Authority Astronomical Institute of St.-Petersburg University Central (Pulkovo) Astronomical Observatory Institute of Applied Astronomy Hartebeesthoek Radio Astronomy Observatory Instituto Geografico Nacional Chalmers University of Technology Main Astronomical Observatory, National Academy of Sciences, Kiev Laboratory of Radioastronomy of Crimean Astrophysical Observatory NASA Goddard Space Flight Center U. S. Naval Observatory Jet Propulsion Laboratory Australia Canada Germany Hungary Korea Netherlands USA Affiliated Member Orgnaizations: Australian National University University of New Brunswick Max-Planck-Institut fr Radioastronomie Satellite Geodetic Observatory Korea Astronomy Observatory Joint Institute for VLBI in Europe (JIVE) Westerbork Observatory National Radio Astronomy Observatory Slide 14 IVS Component Map Slide 15 WETTZELL Slide 16 Effelsberg - 100 mWettzell - 20 m Slide 17 OHiggins - 9 m TIGO - 6 m Slide 18 Kashima - 34 m Shanghai - 26 m Slide 19 mobile antennas MV3 - 5 m Slide 20 IVS products Earth Orientation Parameters (EOP): 24-hour sessions (all EOP) 1-hour Intensives (UT1UTC) Terrestrial Reference Frame (TRF) Celestial Reference Frame (CRF) Daily EOP+station coordinates (SINEX-files) Tropospheric Parameters (TROPO) Baseline Lengths (BL) -VLBI Terrestrial Reference Frame (VTRF) Slide 21 ICRF CRF (Ma, et al., 1998) 212 defining sources 294 candidate sources 102 other sources ICRF-Extension 1 (IERS, 1999) completed 1999 adding 59 sources ICRF-Extension 2 (Fey et al., 2004) completed 2002 adding 50 sources IVS products for the CRF Slide 22 DUT1 from R1 and R4 Combined EOP are regular IVS products Analysis Coordinator: Axel Nothnagel, Univ. Bonn Complete set of EOP d d x p,y p UT1-UTC Combined solution from 6 Analysis Centers 20-30% improvement accuracy robustness R1 & R4 since 2002 Slide 23 WRMSY- Bias WRMSX- Bias AC 58,7-3,470,90,8USN 83,1-2,387,50,9IAA 44,2-1,952,12,0GSF 56,16,368,4-2,1BKG 217,41,1196,0-13,5AUS Y-Pol [as]X-Pol [as] IVS combined product: Polar motion Slide 24 2,4-0,2USN 2,4-0,4IAA 2,10,1GSF 2,80,3BKG 10,8O,9AUS WRMSX- Bias AC UT1-UTC [s] IVS combined product: UT1-UTC Slide 25 82,26,8219,7-8,0USN 59,714,6140,822,9IAA 76,6-10,1196,4-53,1GSF 80,50,4209,2-23,9BKG 89,4-18,9188,17,7AUS WRMSY- Bias WRMSX- Bias AC deps [as]dpsi [as] IVS combined product: precession/nutation Slide 26 average delay in 2002: 17 days Improved delay from observation to product availability (1) 2 time series per week IVS R1 (Bo, Ha, Wa) IVS R4 (Wash) Results available approximately after two weeks Potential for improvements Acceleration of transportation e-VLBI Correlator processing (employing MK5) Slide 27 average delay in 2006: 11 days Improved delay from observation to product availability (2) Slide 28 UT1-UTC from INTENSIVES with reference to CO4 MK5: Wettzell - Kokee Park (blue) and K5: Wettzell Tsukuba (green) Tsukuba Kokee Park Ny Alesund Wettzell Slide 29 With compliments from Dorothee Fischer, Univ.Bonn UT1-UTC from INTENSIVES with reference to CO4 MK5: Wettzell - Kokee Park (black) and K5: Wettzell Tsukuba (red) Slide 30 Wet Zenith Delay for each R1 or R4 hourly resolution Solution of 5 Analysis Centers Combined by TU- Vienna Combined IVS product officially accepted at the 9 th DB- meeting 2-3mm precision comparable to GPS (or better?) Tropospheric parameters WZD as IVS product Slide 31 IVS Pilot Project: Time Series of Baseline Lengths Slide 32 In the last decade, international services were established by the individual techniques, in order to coordinate the observations, the data flow, the analysis and the development of technology. International Cooperation: IAG-, IAU- Services International Earth Rotation and Reference Systems Service (IERS) International GNSS Service (IGS) The International Laser Ranging Service (ILRS) International VLBI Service for Geodesy and Astrometry (IVS) International Doris Service (IDS) International Gravity Field Service (IGFS) Bureau International des Poids et Mesures (BIPM) - Time Section The Permanent Service for Mean Sea Level (PSMSL) IAG Bibliographic Service (IBS) -International Geoid Service (IGeS) -International Gravimetric Bureau (BGI) -International Centre for Global Earth Models (ICGEM) -International Center for Earth Tides (ICET) Slide 33 (From a global TRF solution derived by DGFI, Munich) RMS of Space Geodetic Techniques Slide 34 http://ivscc.gsfc.nasa.gov/about/wg/wg2/index.html Slide 35 ProductsSpecificationStatus 2002Status 2006Goals (2010) Polar Motion (x p, y p) accuracy product delivery resolution frequency of solution x p ~ 100, y p ~ 200 as 1 4 weeks 4 months 1 day 3 days/week x p, y p : 50 80 as 8 12 days 1 day 25 as 1 day 10 min 1 h 7 days/week UT1-UTC (DUT1) accuracy product delivery resolution 5 20 s 1 week 1 day 3 s 3 4 days 1 day 2 s 1 day 10 min Celestial Pole (d ; d accuracy product delivery resolution frequency of solution 100 400 as 1 4 weeks 4 months 1 day ~ 3 days/week 50 as 3 4 days 1 day 25 as 1 day 7 days/week TRF (x, y, z) accuracy5 20 mm5 mm2 mm CRF ( ; ) accuracy frequency of solution product delivery 0.25 3 mas 1 year 3 6 months 0.25mas (improv. distribution) 1 year 3 months 0.25 mas improve. for more freq. Bands 1 month Summary of current IVS main products status and goals (WG2) Slide 36 => Geodetic VLBI observations increased year by year => about 30% in 2002 compared to 2001 => about 15% in 2003 compared to 2002 => about 15% in 2004 compared to 2003 => 2005 similar to 2004 => 2006 similar to 2005 => about 5% in 2007 compared to 2006 Based on WG2 report: IVS observing programs started in 2002 Slide 37 Change from institution-driven observing to IVS- determined program in 2002 about 180 sessions per year, 3.5 sessions per week Complete EOP in two weekly 24-hr sessions: - R1 on Mondays, R4 on Thursdays DUT1 in daily 1-hr Intensive sessions (since 2004 also weekends) CRF sessions R&D sessions Change of IVS Observing Plan Slide 38 Session purpose Session codes Total # sessions (24 hr) Total station days Total TB per year Rapid EOP R1, R4104721604 TRF T2, E3, OHIG, EURO, APSG, JADE 44304147 CRF CRF, CRD164217 R&D R&D, RDV16174294 Intensives (318 days) INT1, INT2270.9 Total:18012681062.9 IVS Observing Plan Summary (Example 2006) Slide 39 Session purpose Session code Total # sessions (24 hr) Avg # particip. stations Total station days Average GB recor- ded per station Total TB per session Total TB per year Rapid turnaround EOP (Monday) IVS-R1526.734812008.0418 TRF, all stations 3-4 times / yr IVS-T2615.0904006.036 EOP, TRF using S2 IVS-E3125.5666003.340 Rapid turnaround EOP (Thurs) IVS-R4527.23735003.6186 CRF IVS-CRF63.0184001.27 CRF, emphasis on south IVS-CRD102.4244001.010 20-station EOP/TRF/CRF RDV619.0114100019.0114 R&D Gigabit/s investigations IVS-R&D106.060300018.0180 Regional Antarctica IVS-OHIG66.7403002.012 Regional Europe EURO68.8533002.616 Regional Asia/Pacific APSG26.0123001.84 Regional Asia/Pacific JADE123.6439003.239 1-hour EOP (232 days) INT12.020350.00.7 1-hour EOP (86 days) INT22.07350.00.2 Total:18012681062.9 2006 Observing Plan Summary Slide 40 8 th IVS Analysis Workshop Vienna, Austria 14 April 2007 http://vlbi.geod.uni-bonn.de/IVS-AC/workshops/ workshop2007/workshop2007.html 2 nd IVS VBLI2010 Working Meeting Vienna, Austria 15 April 2007 http://mars.hg.tuwien.ac.at/~evga/Agenda_2010.pdf 4 th IVS Technical Operations Workshop Haystack Observatory, Westford, MA, USA 30 April 2007 3 May 2007 http://ivscc.gsfc.nasa.gov/meetings/tow2007/ Recent IVS Activities Meetings Slide 41 Directing Board: elections in December 2006, January 2007 17 th Board meeting on 24 February 2007 in Wettzell, Germany new Chair: Prof. Harald Schuh Working Groups Joint IERS/IVS WG on the Second Realization of the ICRF (ICRF-2), foreseen milestones: April 12, 2007: WG meeting in Vienna Fall 2007: generation and comparison of time series Spring 2008: analysis of time series Mid 2008: defining source criteria Fall 2008: selection of defining sources, analysis configuration Spring 2009: generation of ICRF-2 catalogue, presentation to IVS, IERS, and IAU working group Recent IVS Activities Organizational Items (1) Slide 42 Working Groups IVS WG on New Data Structures for VLBI purpose: to design next generation VLBI data structure general establishment approved by Directing Board (DB) final charter and membership to be approved by DB at 15 September 2007 meeting Recent IVS Activities Organizational Items (2) Slide 43 Additional Intensive session (Int3) every Monday @ 6 UT Stations: Ny- lesund, Tsukuba, Wettzell correlation at MPIfR Bonn data transfer via high-speed network (e-transfer) product availability, turnaround time: 24-hours first test successful operational start: end of August 2007 Ultra-rapid Intensive sessions irregular, initially August 2007 through March 2008 Stations: Onsala, Mets hovi, Kashima, Tsukuba correlation in Japan (NICT, GSI) on software correlator data transfer via high-speed network (e-VLBI) product availability, turnaround time: near-real time successful test on Onsala-Kashima baseline Recent IVS Activities Additional observation sessions Slide 44 Digital recorder MK5A MK5B K5 VSI (VLBI Standard Interface) e-VLBI near real time (data stored at correlator) real time (correlation done in real time) Recent IVS Activities Operational Improvements Slide 45 Developments Haystack- USA (MK5) CRL Japan (K5) Replacing MKIV by MK5 Combination of various developments via VSI (VLBI Standard Interface) 2007: MK5A to MK5B VSI included Station unit replacement at correlator MK5A Digital Recorders Slide 46 Motivation Most of VLBI equipment developed in 70s and 80s pushed to its limits, costly to maintain Radio interference at S-Band increased, making observations problematic Old slow moving antennas make it difficult to provide agile whole sky coverage Location of antennas is not ideal, unbalanced in global distribution Operation costs remain high Processing time to final results is too long Charter Examine current and future requirements including all components provide a report with recommendations for a new generation system IVS Working Group on VLBI 2010 (WG3) (1) Slide 47 Subgroups for special studies Observing strategies (Bill Petrachenko) RF/IF, frequency and time (Hayo Hase) Backend systems (Gino Tuccari) Data acquisition and transport (Alan Whitney) Correlation and fringe finding (Yasuhiro Koyama) Data analysis (Harald Schuh) Data archiving and management (Chopo Ma) IVS Working Group on VLBI 2010 (WG3) (2) Slide 48 VLBI 2010: Current and Future Requirements for Geodetic VLBI A. Niell, A. Whithney, W. Petrachenko, W. Schlter, N. Vandenberg, H. Hase, Y. Koyama, C. Ma, H. Schuh, G. Tuccari released September 2005 Supports coordination of VLBI developments at various institutions Provides arguments for supporting IVS and for getting funds http://ivscc.gsfc.nasa.gov/about/wg/wg3/index.html WG 3 Report Slide 49 Criteria 1mm measurement accuracy on global baselines Continuous measurement for time series of station positions and EOP Turn around time to initial geodetic results less than 24 h Low cost construction and operation Strategies Reduce random and systematic errors of delay observables (clocks, atmosphere,...) Improve geographic distribution of antennas Increase number of observations Develop new observing strategies VLBI 2010 (1) Slide 50 Recommendations Design a new observing system based on small antennas (10-12m), fast moving, operate unattended, mechanically reliable, economically replicable Broad continuous frequency range (e.g. 2-18 GHz) which includes S- and X-band Upgrade of large antenna to preserve continuity, maintaining CRF Transfer data with combination of high speed networks and high rate disk systems Examine the possibilities for a new correlator system (software correlator ?) Automate and streamline the complete data analysis pipeline VLBI 2010 (2) Slide 51 WG3 report rises questions and identifies steps that need to be taken: System studies and simulations Error budget developments Decision on observing frequencies Optimal distribution of new sites Number of antennas per site New observing strategies Transition plan VLBI 2010 (3) Slide 52 WG3 report rises questions and identifies steps that need to be taken: Development of projects and prototyping Small antenna systems Feed and receiver Higher data-rate system Correlator development Backend development Data management Analysis software => VLBI2010 Committee (V2C) is tasked to coordinate the efforts VLBI 2010 (4) Slide 53 Established September 2005 Members: W. Petrachenko (chair), D. Behrend, J. Bhm, B. Corey, R. Haas, Y. Koyama, D. MacMillan, Z. Malkin, A. Niell, G. Tuccari Charter: Promote and guide research into the improvement of the "technique" of geodetic VLBI Take an integrated view of VLBI, evaluate effectiveness of proposed system changes with respect to final products Take responsibility for encouraging the implementation of the recommendations of WG3 VLBI2010 Committee (V2C) (1) Slide 54 Actions documented in Memos (available at the IVS-web page) Error budget, Arthur Niell A Monte Carlo Simulator for Geodetic VLBI, Bill Petrachenko Simulations of Weth zenith Delays and Clocks, Johannes Bhm, Jrk Wresnik Multiband Delay Error, Arthur Niel, Brian Corey, Bill Petrachenko Some Notes on Broad-band Dual Polarization Feeds, Rdiger Haas, Per-Simon Kildal Simulation Studies at Goddard, Dan McMillan V2C Simulations at IGG Vienna, Jrg Wresnik, Johannes Bhm Performance Comparison between Traditional S/X and X/KA Systems and a Braodband S_KU System, Bill Petrachenko Source Structure Simulation, Arthur Niell First VLBI2010 Working Meeting, Haystack, September 15, 2006 VLBI2010 Committee (V2C) (2) Slide 55 Vienna VLBI Simulations Slide 56 Working Group 3 of the International VLBI Service (IVS) 2004-2005 Tasks: Current and Future Requirements for Geodetic VLBI Systems Design a new VLBI observing system based on small antennas with 1mm accuracy - number, location and configuration of antennas At IGG: System studies and simulations accuracy of 1mm site position & of 0.1mm/year velocity continuous measurements for EOP rapid generation & distribution of IVS products Goals: Slide 57 Test Networks for VLBI2010 Slide 58 Creating a VLBI observing schedule catalogue files stations radio sources position structure models flux density position diameter slew rate axis limits surface accuracy pointing accuracy create new catalogue files for simulation frequencies observing S & X to be determined mainly done by John Gipson NVI@GSFC Slide 59 Monte Carlo simulation atmosphere clocks wzd & clocks are stochastic processes simulate for station 1 and 2 90-e 2 1 Slide 60 Simulation of wzd and clock parameters random walk variances of: 0.1 psec/s 0.7 psec/s turbulence model (Tobias Nilsson, Onsala Space Observatory (OSO), Sweden) Simulate the wet zenith delay Slide 61 Simulation of wzd and clock parameters Simulate the clocks random walk + integrated random walk Allan standard deviation of: 210 -15 @15min 110 -14 @50min Slide 62 Simulation of wzd and clock parameters Simulate observation errors white noise: 4 psec 8 psec 16 psec Slide 63 simulation of 25 identical 24 hour sessions What are the effects of wzd and clocks? Does a 4psec antenna improve the results? simulate wzd 25 times for each station simulate clocks 25 times for each station random walk + integrated rw 4 psec 8 psec 16 psec turbulence model random walk generate white noise 25 times for each baseline Simulation of wzd and clock parameters Slide 64 Baseline lengths repeatability 2737 scans 57595 observations 5760 scans 116308 observations 9386 scans 226639 observations Three types of schedules Slide 65 Baseline lengths repeatability 60 000 wet zenith delay 2e-15@15min (ASD) 0.0036 psec**2/sec (PSD) 0.1 psec**2/sec clocks 120 000 220 000 observations => clear improvement with dense schedules baselines with few obs. show worse baseline repeatability isolated stations 4 psec white noise effect of schedules Slide 66 Baseline lengths repeatability if the PSD of wet zenith delay is 0.7 psec**2/sec, 4 psec antennas give the same result as 16 psec antennas and PSD of wet zenith delay of 0.1psec**2/s => the wet zenith delay is the limiting factor effect of wet zenith delay 4 psec wet zenith delay 2e-15@15min (ASD) 0.0036 psec**2/sec (PSD) 0.1 psec**2/sec clocks 16 psec white noise 0.7 psec**2/sec Slide 67 Baseline lengths repeatability at 16 psec noise level very small differences of the baseline length repeatability can be seen for different clocks at 4 psec noise level the influence of the clocks can be seen effect of clocks 4 psec wet zenith delay 2e-15@15min (ASD) 0.0036 psec**2/sec (PSD) 0.1 psec**2/sec clocks 16 psec white noise 1e-14@50min (ASD) 0.3 psec**2/sec (PSD) Slide 68 Baseline lengths repeatability 4 psec wet zenith delay clocks white noise the turbulence model is between the two values for wzd, simulated with random walk 0.1 psec**2/sec 0.7 psec**2/sec turb. model 2e-15@15min (ASD) 0.0036 psec**2/sec (PSD) effect of turbulance Slide 69 CONT05 real data vs Monte Carlo simulator the use of the turbulence model gives a more realistic Monte Carlo simulation wet zenith delay clocks white noise turb. model 1e-14@50min (ASD) obs. error Slide 70 CONT05 real data vs Monte Carlo simulator wet zenith delay clocks white noise turb. model 1e-14@50min (ASD) obs. error 4 psec turb. model 2e-15@15min (ASD) improvement of the VLBI2010 system can be seen clearly Slide 71 VLBI System Characteristics CurrentVLBI2010 antenna size5100 m dish~ 12 m dish slew speed~20200 deg/min 360 deg/min sensitivity20015,000 SEFD 2,500 SEFD frequency rangeS/X band~215 (18) GHz recording rate128, 256 Mbps816 Gbps data transfer usually ship disks, some e-transfer e-transfer, e-VLBI, ship disks when required Slide 72 Next steps Advantage: higher observation density continuous observations better determination of systematic effects one frequency standard (change the code in OCCAM for one clock) one more local tie Twin antennas Simulation for multiple antennas twin antennas at the sites Slide 73 (Can WVR be used for VLBI2010 and improve the results?) Summary of Simulations schedule dependent improvement Schedules have to be improved w.r.t. observation density 120 000 220 000 observations seems to be sufficient only slight improvement of the baseline length repeatability by using clocks with an ASD of 2e-15@15min Baseline length repeatability PSD of wet zenith delays dominates the baseline length repeatability Clocks with an ASD of 2e-15@15min are sufficient the turbulence model is between the values for wzd 0.1 & 0.7 psec**2/sec simulated with random walk Good agreement compared to real data of CONT05 Slide 74 e-VLBI Alan Whitney (MIT Haystack Observatory) Slide 75 e-VLBI Alan Whitney (MIT Haystack Observatory) Slide 76 e-VLBI Alan Whitney (MIT Haystack Observatory) Slide 77 April 2005 Start routine e-VLBI transfer from Kashima and Tsukuba (>200Mbps) Starting ~June 2005 Automated regular e-VLBI UT1 Intensive data transfers from Wettzell to ISI-E (disks hand-carried to USNO for correlation) A few start-up problems, but now operating fairly smoothly Spring 2005 Commitment to connect Hobart via optical fiber (schedule unknown) September 2005 All CONT05 data from Tsukuba transferred to Haystack via e-VLBI (~15 TB!) Also all Syowa data now transferred via e-VLBI from Japan to Haystack Progress towards e-VLBI (1) Slide 78 November 2005 Project initiated to connect NyAlesund to Haystack through NASA/GSFC at up to 100Mbps Data now transmitted routinely from NyAlesund, but slow data rate of ~80Mbps does not allow all data to be transferred; decision by NMA is pending whether to continue, upgrade, etc. December 2005 Funds secured to connect Fortaleza at 2.5 Gbps; (expect connection RSH) February 2007 Efforts initiated to re-connect Kokee, at least on trial basis; (expect first testing soon) => 50 TB of data now transferred annually, increasing rapidly Progress towards e-VLBI (2) Slide 79 JIVE 17 x 1 Gbps + 10GigE (soon) Haystack (2.5 Gbps; expect to expand to 10Gbps RSN) Westford, MA (10 Gbps to Haystack; 1 Gbps to outside world) Kashima, Japan (2.5 Gbps) Usuda, Japan (2.5 Gbps) Nobeyama, Japan (2.5 Gbps) Koganei, Japan (2.5 Gbps) Metsahovi, Finland (10 Gbps) MPI, Germany (1 Gbps) Tsukuba, Japan (2.5 Gbps) GGAO, MD (1 Gbps) Onsala, Sweden (1 Gbps) Torun, Poland (1 Gbps) Westerbork, The Netherlands (1 Gbps) Medicina (1 Gbps) NyAlesund (~80 Mbps); expect to improve to ~300Mbps Jodrell Bank (1 Gbps) Arecibo, PR (155 Mbps) Wettzell, Germany (~30 Mbps; soon to be ~600Mbps) Kokee Park, HA (hope to re-connect soon at ~80Mbps) TIGO (~30-90Mbps) Svetloe (100 Mbps) Zelenchukskaya (100 Mbps) In progress: Hobart agreement reached to install high-speed fiber; details not known, but schedule delayed Forteleza funds secured for fiber connection at 2.5Gbps; contract has been signed; expect completion Feb 2007, but have not heard Badary expect 2008 Antenna/Correlator Connectivity (geodetic sites shown in red) Slide 80 Digital backends (DBEs) (1) Two design approaches have been pursued: 1. Polyphase filter - DBE (Haystack) Developed in collaboration with UC Berkeley Entire IF bandwidth partitioned into 2n adjacent channels (example: 16 32-MHz channels across 512 MHz IF) Not quite as flexible in exact placement of freq channels Largely eliminates need for phase-cal (but not delay cal) Allows natural expansion to multi-Gbps data rates with no additional DBE costs Successfully tested at 4Gbps Westford-GGAO using 2 500MHz Ifs Plan 8Gbps broadband tests summer 2007 Collaboration with NRAO to develop next-generation DBE 16Gbps; prototype expected Q4 2007 Slide 81 Digital backends (DBEs) (2) Two design approaches have been pursued: 2. Analog BBC replacement dBBC (EVN) Direct replacement of analog BBCs Full flexibility of channel placement Test experiments have been successful Deployment beginning 2007 => Compatibility testing between dBBC and DBE will begin soon, probably using Noto and Westford => Flexible LO/IF subsystem being designed for easy selection of IF sub-bands from broadband LO Slide 82 Haystack/Berkeley DBE Slide 83 Publications Journal of Geodesy special issue VLBI Volume 81, Numbers 6-8 June 2007 online version available at: http://www.springerlink.co m/content/v760312v657v/? p=cf1d0d1bf2c1471390db3 f07ca25a2a8&pi=0 17 articles including preface Slide 84 VLBI2010 is supporting some proposals: Korean Institutes (KASI, NGII, Ajou Univ.) Geoscience Australia: proposal for 3 fundamental stations Univ. Tasmania (Hobart): getting operation money University of Concepcion/Chile: developing a telescope ISRO, India: 32m telescope for lunar mission extended for geodetic VLBI NASA Haystack: support of VLBI 2010 telescope / Gilmore Creek BKG: twin-telescope 2008-2010 More? International VLBI plans wrt. VLBI2010 Slide 85 Thank you for your attention! see you all at the Slide 86 Slide 87 Thank you for your attention! http://ivscc.gsfc.nasa.gov/meetings/gm2008/ Fifth IVS General Meeting March 3-6, 2008 St. Petersburg, Russia see you all at the