W
W. F. Brisken
Researcher at Max Planck Society
Publications - 10
Citations - 683
W. F. Brisken is an academic researcher from Max Planck Society. The author has contributed to research in topics: Pulsar & Very-long-baseline interferometry. The author has an hindex of 6, co-authored 10 publications receiving 585 citations. Previous affiliations of W. F. Brisken include University of Minnesota & National Radio Astronomy Observatory.
Papers
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Journal ArticleDOI
DiFX-2: A More Flexible, Efficient, Robust, and Powerful Software Correlator
Adam Deller,Adam Deller,W. F. Brisken,Chris Phillips,John Morgan,Walter Alef,Roger J. Cappallo,Enno Middelberg,Jonathan D. Romney,Helge Rottmann,Steven Tingay,Randall B. Wayth +11 more
TL;DR: The DiFX correlator as discussed by the authors is a C++-based software correlation algorithm written in a high-level language such as C++ that is run on commodity computer hardware and has become increasingly attractive for small-to medium-sized and/or bandwidth-constrained radio interferometers.
Journal ArticleDOI
Microarcsecond VLBI Pulsar Astrometry with PSRπ II. Parallax Distances for 57 Pulsars
Journal ArticleDOI
Microarcsecond VLBI pulsar astrometry with PSR$\pi$ II. parallax distances for 57 pulsars
Adam Deller,W. M. Goss,W. F. Brisken,Sourav Chatterjee,J. M. Cordes,Gemma H. Janssen,Yuri Y. Kovalev,T. J. W. Lazio,Leonid Petrov,Benjamin Stappers,A. G. Lyne +10 more
TL;DR: In this article, the authors present the results of PSR$\pi, a large astrometric project targeting radio pulsars using the Very Long Baseline Array (VLBA).
Journal ArticleDOI
50 picoarcsec astrometry of pulsar emission
TL;DR: In this article, the authors used VLBI imaging of the interstellar scattering speckle pattern associated with the pulsar PSR 0834+06 to measure the astrometric motion of its emission.
Posted Content
Proper Motions of PSRs B1747-24 and B1951+32: Implications for Ages and Associations
TL;DR: In this paper, the radio-bright arc of emission along the pulsar proper motion vector shows time-variable structure, but moves with a pulsar at an approximately constant separation ~2.5'', lending weight to its interpretation as a shock structure driven by the PSR.