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evn:evn_scince

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The European VLBI Network (EVN)

Recent science highlights from the EVN




Pulsars astrometry

Extending the time baseline from two years to more than ten years, Kirsten et al. 2015 (A&A, 577, 111, 2015) measured the parallax and the proper motion for the three isolated pulsars B1929+10, B2020+28, and B2021+51 in a global VLBI experiment. Combining their 5 GHz data with that from Brisken et al. 2002 (ApJ, 571, 906, 2002) and Chatterjee et al. 2004 (ApJ, 604, 339) their data on B1929+10 indicates a distance of 360 +/- 7 pc, Fig. 1. In combination with the measured proper and inferred transverse velocity the authors trace the pulsar's trajectory back in time through the Galactic potential. They conclude that the previously made claim that the pulsar once formed a binary system with the runaway O-star z-Ophiuchi is very unlikely. They also conclude that the putative common binary origin of B2020+28 and B2021+51 in the Cygnus Superbubble is very unlikely.

Figure 1. Relative measured positions of B1929+10 with the best fit proper motion removed. The solid line is the best fit parallax from all available data combined. Solid dots show the most recent measurements at 5 GHz, open stars are the data from Brisken et al. 2002 (ApJ, 571, 906, 2002), and squares are the data from Chatterjee et al. 2004 (ApJ, 604, 339).

Introduction

evn/evn_scince.1461304239.txt.gz · Last modified: 2016/04/22 05:50 by michael.lindqvist