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 | PSR J1023+0038 transforming between a radio pulsar and an accreting system | Anne Archibald | [NOTE: the paper appears in print July 20th, possibly accompanied by a press release and video, so this might be a good time to post the image.] PSR J1023+0038 is a neutron star spinning 592 times per second, orbited by a small Sun-like star. We think all such fast-spinning neutron stars were spun up by accreting material spiraling in from a companion. We have actually seen this system switch back and forth between a radio pulsar (left) and an X-ray bright system with a disc of accreting material (right). Right now, in fact, the system is in this mysterious accreting state. When the accretion switches off, will the neutron star have spun up, slowed down, or stayed the same? (c) Anne Archibald, Joeri van Leeuwen | {{:propaganda:appp2014:archibald-poster-j1023.pdf|}} {{ :propaganda:appp2014:archibald-poster-j1023.png?150 }} |  |
 | PSR J0337+1715: a millisecond pulsar in a stellar triple system | Anne Archibald | Radio telescopes, including the Westerbork Synthesis Radio Telescope operated by ASTRON, allow us to measure how early or late the pulses from this radio pulsar are as it moves around its orbit. We can then compute the delays - shown above - due to the interaction of the inner and outer orbit. These measurements, and the tremendous density of the pulsar, let us test one of the foundations of Einstein's theory of gravity, the Strong Equivalence Principle. (c) Jason Hessels, Anne Archibald | {{:propaganda:appp2014:archibald-poster-0337-portrait.pdf|}} {{ :propaganda:appp2014:archibald-poster-0337-portrait.png?150 }} |  |
-| Global VLBI imaging of the gravitational lens JVAS B1938+666 | John McKean | [Not ready for AJDI release] Gravitational lensing is the deflection of light from a distant background object (the source) by an intervening mass distribution (the lens). If the surface mass density of the lens is sufficiently high, then multiple images of the background source, which are often highly magnified and distorted, are produced. The gravitational lensing phenomena is beautifully illustrated in this global very long baseline interferometry image of JVAS B1938+666 at redshift 2.0. Here, the extended background radio source is highly distorted into several images, some of which are stretched to form large gravitational arcs. Never before has such high angular resolution of extended arcs been seen before, which highlights the excellent sensitivity that can be achieved with VLBI arrays today (a collecting area that is about 10 per cent of the SKA). | {{:propaganda:appp2014:mckean_poster2.pdf|}} {{ :propaganda:appp2014:mckean_poster2.png?150 }} |  |
+| Global VLBI imaging of the gravitational lens JVAS B1938+666 | John McKean | [Not ready for AJDI release] Gravitational lensing is the deflection of light from a distant background object (the source) by an intervening mass distribution (the lens). If the surface mass density of the lens is sufficiently high, then multiple images of the background source, which are often highly magnified and distorted, are produced. The gravitational lensing phenomena is beautifully illustrated in this global very long baseline interferometry image of JVAS B1938+666 at redshift 2.0. Here, the extended background radio source is highly distorted into several images, some of which are stretched to form large gravitational arcs. Never before has such high angular resolution of extended arcs been seen before, which highlights the excellent sensitivity that can be achieved with VLBI arrays today (a collecting area that is about 10 per cent of the SKA). | {{:propaganda:appp2014:mckean_poster2_new.pdf|}} {{ :propaganda:appp2014:mckean_poster2_new.png?150 }} RAW: {{:propaganda:appp2014:mckean_poster2.key.tar}} |  |
 |Apertif | Tom Oosterloo| The sky as Apertif will see it. The blue objects show the radio continuum emission from star forming galaxies and from galaxies with an Active Galactic Nucleus. The orange objects illustrate the cold, atomic Hydrogen in galaxies. Apertif will detect the Hydrogen in more than 100,000 galaxies, and the continuum emission from about 10,000,000 objects | {{:propaganda:appp2014:apertif.pdf|}} {{:propaganda:appp2014:apertif.png?150| }}|  |
 |Dwingeloo 1 & 2 | Tom Oosterloo| Dwingeloo 1 and 2 were discovered with the Dwingeloo dish in 1994 as part of a search for galaxies that are hidden by dust clouds in the plane of the Milky Way. Such dust clouds block the optical light of galaxies, but are transparent for their radio emission. Therefore, surveying the plane of the Milky Way with radio telescopes can reveal galaxies that are otherwise hard to see. In optical light, Dwingeloo 1 and 2 are almost invisible, but they have bright radio emission. The picture shows the radio image of Dwingeloo 1 and 2 made with the Westerbork Synthesis Radio Telescope| {{:propaganda:appp2014:dwloo12poster-2.pdf|}}{{:propaganda:appp2014:dwloo12poster-2.png?150|}}|
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 Pulsar presentation, high-shool and general audience, includes movies, sounds, etc. {{http://www.astron.nl/pulsars/presentations/Pulsar%20Presentation%202010.zip|Zipped powerpoint file, 100MB}}