Volume 577, May 2015
|Number of page(s)||10|
|Section||Celestial mechanics and astrometry|
|Published online||13 May 2015|
Revisiting the birth locations of pulsars B1929+10, B2020+28, and B2021+51
1 International Centre for Radio Astronomy Research (ICRAR), Curtin University, GPO Box U1987, Perth, WA 6845, Australia
2 Max Planck Institut für Radioastronomie (MPIfR), Auf dem Hügel 69, 53121 Bonn, Germany
3 Argelander Institut für Astronomie (AIfA), Universität Bonn, Auf dem Hügel 71, 53121 Bonn, Germany
4 Department of Earth and Space Sciences, Chalmers University of Technology, Onsala Space Observatory, 439 92 Onsala, Sweden
5 Joint Institute for VLBI in Europe, Oude Hoogeveensedijk 4, 7991 PD Dwingeloo, The Netherlands
6 Department of Astronomy, Cornell University, Ithaca, NY 14853, USA
Received: 20 December 2014
Accepted: 27 March 2015
We present new proper motion and parallax measurements obtained with the European VLBI Network (EVN) at 5GHz for the three isolated pulsars B1929+10, B2020+28, and B2021+51. For B1929+10 we combined our data with earlier VLBI measurements and confirm the robustness of the astrometric parameters of this pulsar. For pulsars B2020+28 and B2021+51 our observations indicate that both stars are almost a factor of two closer to the solar system than previously thought, placing them at a distance of 1.39-0.06+0.05 and 1.25-0.17+ 0.14kpc. Using our new astrometry, we simulated the orbits of all three pulsars in the Galactic potential with the aim to confirm or reject previously proposed birth locations. Our observations ultimately rule out a claimed binary origin of B1929+10 and the runaway star ζ Ophiuchi in Upper Scorpius. A putative common binary origin of B2020+28 and B2021+51 in the Cygnus Superbubble is also very unlikely.
Key words: pulsars: individual: B1929+10 / pulsars: individual: B2020+28 / pulsars: individual: B2021+51 / parallaxes / techniques: interferometric / proper motions
© ESO, 2015
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