The characteristics of millisecond pulsar emission: III.From low to high frequencies

Abstract

In this paper we present the first observations of a large sample of millisecond pulsars at frequencies of 2.7 GHz and 4.9 GHz. Our new flux measurements extend the known spectra for millisecond pulsars to the highest frequencies to date. The coverage of more than a decade of radio spectrum allows us for the first time to search for spectral breaks as so often observed for normal pulsars around 1 GHz. We align the observed millisecond pulsar profiles with data from lower frequencies. Deviations from a dipolar magnetic field structure are not evident and absolute timing across the wide frequency range with a single dispersion measure is possible. We seem to observe mainly unfilled emission beams, which must originate from a very compact region. A compact emission region is also suggested by a remarkably constant profile width or component separation over a very wide frequency range. For a few sources, polarization data at 2.7 and 4.9 GHz could also be obtained which indicate that millisecond pulsars are weakly polarized or even unpolarized at frequencies above 3 GHz. The simultaneous decrease in degree of polarization and the constant profile width thus question proposals which link de-polarization and decreasing profile width for normal pulsars to the same propagation effect (i.e. birefringence). Comparing the properties of core and conal like profile components to those of normal pulsars, we find less significant patterns in their spectral evolution for the population of millisecond pulsars. Hence, we suggest that core and conal emission may be created by the same emission process. In general, MSP emission properties tend to resemble those of normal pulsars only shifted towards higher frequencies.