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EVN2015: Pulsars and VLBI

EVN2015: Pulsars and VLBI. Find them! Time them! VLBI Them! Ben Stappers (ASTRON/UvA). Three Main Goals. Astrometry Pulsar Emission Pulsar Environments. PSR J0218+4232. All best achieved with Pulsar Binning. Astrometry. Parallaxes and proper motions essential for:

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EVN2015: Pulsars and VLBI

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  1. EVN2015: Pulsars and VLBI Find them! Time them! VLBI Them! Ben Stappers (ASTRON/UvA)

  2. Three Main Goals • Astrometry • Pulsar Emission • Pulsar Environments PSR J0218+4232 All best achieved with Pulsar Binning

  3. Astrometry • Parallaxes and proper motions essential for: • Pulsar velocities: SNe physics, Pulsar birth places, SNR assoc. VLBA: B1508+55 Requires: High Sensitivity & binning with high time resoln. regular scheduling.

  4. Astrometry • Parallaxes and proper motions essential for: • Understanding ISM properties, especially locally Requires: High Sensitivity & binning with high time resoln. regular scheduling.

  5. Astrometry • Parallaxes and proper motions essential for: • Precise tests of GR require accurate distances and velocities • e.g. PSR B1913+16 & B1534+12 • More accurate measures of Pdot and timing noise. Requires: High Sensitivity & binning with high time resoln. regular scheduling.

  6. Pulsar Emission Physics What lies beneath? • Off pulse emission in wide cones and the very wide pulse profiles • The particle acceleration mechanism • Structure of the magnetosphere Requires: High Sensitivity & binning with high time resoln.

  7. Pulsar Environments: PWNe What lies nearby and beneath? • Majority Lspin in wind • Only obs. In ISM shocks • Small in radio • Resolve inner shocks • combine with other wavelengths • as radio gives unique information Mouse. Gaensler et al Requires: High Sensitivity & binning with high time resoln.

  8. Pulsar Environments: Disks & Jets • Fallback disks possibly seen in • high B magnetars • Models of pulsar emission propose • infalling bodies from disk • Study the compact form of jets in • the radio. • Relationship with larger structures • Energetics cf. shocks/winds Requires: High Sensitivity & binning with high time resoln.

  9. A big telescope! Using the EVN telescopes as a tied array If we assume that we had something like 9 telescopes with an average size of 64m then we basically have a sensitivity equivalent to a >200m dish! With the proposed very wide bandwidths this would be close to the best PSR telescope Excellent step in the direction of the SKA EPTA High precision timing, stability, new parameters Timing, and studies of unique v. weak sources Requires Tied-Array, high time resoln/freq output, Mbeam?

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