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Scientific paper
Jul 1996
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996hst..prop.6526c&link_type=abstract
HST Proposal ID #6526
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Hst Proposal Id #6526 Hot Stars
Scientific paper
PSR0833-45 is, with the Crab pulsar and PSR0540-69, one of the few Isolated Neutron Stars {INSs} associated with a SNR. Moreover, these are, so far, the only INSs known to pulsate in the optical domain. Although the optical counterpart of the Vela Pulsar has been identified since 1977, nothing is known about its UV emission beyond a limited, ground based point in the U band. Blueward of it, the FOC could easily measure, for the first time, the presumably non-thermal radiation of the pulsar. On the other hand, recent results in X and Gamma-ray domains have challenged the commonly accepted value of 500 pc for the source distance, suggesting the need for a significant downward revision. The distance to the Vela Pulsar is a quite important piece of information, since this object is used as a calibrator for SNRs. Thus, it seems worthwhile to address this point with a set of three high accuracy WFPC2 observations aimed at measuring {or set limit on} the parallactic displacem. ent of the Vela Pulsar optical cou nterpart. At 250 pc, for instance, Vela should show a parallactic displacement of 0.004", equivalent to 0.09 PC pixels, a value which, according to our experience, is certainly within the instrument capabality. These high accuracy observations would also yield a precise measure of the pulsar's proper motion. This is yet another open point in the complex Vela Pulsar phenomenology, since, although proper motion is certainly present, existing radio and optical observations yield conflicting results.
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