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Eastwood, Michael W.

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  <identifier identifierType="DOI">10.5281/zenodo.1049160</identifier>
      <creatorName>Eastwood, Michael W.</creatorName>
      <nameIdentifier nameIdentifierScheme="ORCID" schemeURI="">0000-0002-4731-6083</nameIdentifier>
      <affiliation>Department of Astronomy, California Institute of Technology</affiliation>
    <date dateType="Issued">2016-10-27</date>
  <resourceType resourceTypeGeneral="Software"/>
    <alternateIdentifier alternateIdentifierType="url"></alternateIdentifier>
    <relatedIdentifier relatedIdentifierType="URL" relationType="IsSupplementTo"></relatedIdentifier>
    <relatedIdentifier relatedIdentifierType="DOI" relationType="IsPartOf">10.5281/zenodo.1049159</relatedIdentifier>
    <rights rightsURI="">GNU General Public License 3.0</rights>
    <rights rightsURI="info:eu-repo/semantics/openAccess">Open Access</rights>
    <description descriptionType="Abstract">&lt;p&gt;TTCal is a calibration routine developed for the OVRO-LWA.&lt;/p&gt;

&lt;p&gt;The standard procedure for phase calibrating a radio interferometer usually involves slewing a small number of large dishes to stare at a known point source. A point source at the phase center of the interferometer has zero phase on all baselines, so phase calibration essentially amounts to zeroing the phase on all baselines.&lt;/p&gt;

&lt;p&gt;Low frequency telescopes (&amp;lt;300 MHz) tend to occupy an entirely different region of phase space. That is they are usually composed of numerous cheap dipole antennas with very broad beams (LOFAR, MWA). Furthermore, the low frequency sky is corrupted by propagation through the ionosphere. Until the field matures, the demand for a new and effective calibration technique is best met by a simple, adaptable, and relatively fast software package. This is why I wrote TTCal.&lt;/p&gt;</description>
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