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Ferrario & Wickramasinghe (2006) explored the hypothesis that the magneticfields of neutron stars are of fossil origin. In this context, they predictedthe field distribution of the progenitor OB stars, finding that 5 per cent ofmain sequence massive stars should have fields in excess of 1kG. We havecarried out sensitive ESPaDOnS spectropolarimetric observations to search fordirect evidence of such fields in all massive B- and O-type stars in the OrionNebula Cluster star-forming region. We have detected unambiguous Stokes VZeeman signatures in spectra of three out of the eight stars observed (38%).Using a new state-of-the-art Bayesian analysis, we infer the presence of strong(kG), organised magnetic fields in their photospheres. For the remaining fivestars, we constrain any dipolar fields in the photosphere to be weaker thanabout 200G. Statistically, the chance of finding three ~kG fields in a sampleof eight OB stars is quite low (less than 1%) if the predictions of Ferrario &Wickramasinghe are correct. This implies that either the magnetic fields ofneutron stars are not of fossil origin, that the flux-evolution model ofFerrario & Wickramasinghe is incomplete, or that the ONC has unusual magneticproperties. We are undertaking a study of other young star clusters, in orderto better explore these possibilities.

Exploring the origin of neutron star magnetic field: magnetic properties of the progenitor OB stars