Investigation of radiation from pulsar PSR 0329 + 54 using Mark III VLBI observations

Details Investigation of radiation from pulsar PSR 0329 + 54 using Mark III VLBI observations Investigation of radiation from pulsar PSR 0329 + 54 using Mark III VLBI observations

Dec 1985

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985aj.....90.2532b&link_type=abstract

Astronomical Journal (ISSN 0004-6256), vol. 90, Dec. 1985, p. 2532-2539. DFG-supported research.

Astronomy and Astrophysics

Astronomy

10

Emission Spectra, Interstellar Matter, Pulsars, Stellar Radiation, Very Long Base Interferometry, Data Correlation, Scattering, Signal To Noise Ratios, Space Observations (From Earth)

Scientific paper

The pulsar PSR 0329+54 was observed with the Mark III VLBI system at 2.3 GHz. All the data were correlated with the Haystack processor in the "gated" mode to improve the signal-to-noise ratio and to compute visibility as a function of pulsar longitude. The authors determined an upper limit for the diameter of the scattering disk of the pulsar of 1 mas (FWHM of a Gaussian). Any continuum emission from the pulsar at "off-pulse" longitudes has flux density less than 2.5 mJy or 0.08% (3σ) of the peak of the pulsed emission. The upper bounds on the differences in visibility phases between portions of the pulse profile correspond to upper bounds on the separation of the corresponding emission regions of ≡25 μas (3σ) in right ascension and ≡80 μas (3σ) in declination. The authors discuss the prospects for a 30-fold improvement in the precision of measurement of the difference in visibility phases, necessary to resolve the angular radius of the light cylinder of at least one pulsar. They further show that pulsars are useful for determining polarization characteristics of antenna feeds, which may be needed for precision astrometry and for mapping celestial sources.

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