Paper

{
  "raw_xml": "<entry>\n    <id>http://arxiv.org/abs/2603.12970v1</id>\n    <title>Tied-array beam flatfielding</title>\n    <updated>2026-03-13T13:10:42Z</updated>\n    <link href='https://arxiv.org/abs/2603.12970v1' rel='alternate' type='text/html'/>\n    <link href='https://arxiv.org/pdf/2603.12970v1' rel='related' title='pdf' type='application/pdf'/>\n    <summary>Context. Multi-element phased-array radio telescopes use digital beamforming to widen their field-of-view with numerous tied-array beams (TABs). These beams share bandpass variations and radio frequency interference (RFI). Yet, most pulsar and transient pipelines process each beam independently, ignoring shared spatial information. This leads to many RFI-dominated false positives that require extensive later sifting. Aims. We exploit multi-beam spatial information to stabilize bandpasses, suppress red noise and broad-band RFI, and drastically reduce false positives without degrading genuine astrophysical signals. Methods. We derive tied-array gain against residual phase dispersion, showing off-beam sources converge to the incoherent limit. Using chi-squared statistics, we analyze dividing a TAB by a beam-averaged reference and quantify the necessary smoothing. We test these predictions using LOFAR high-band antenna voltages (PSR B0329+54), simulations, and LOTAAS survey data (PSR J0250+5854). Results. Off-beam sources contribute nearly uniform power across beams once primary-beam effects are handled. Dividing by a smoothed multi-beam reference yields flatter dynamic spectra and equal or higher pulse signal-to-noise ratios compared to incoherent subtraction. Applied to LOTAAS data, this \"beam flatfielding\" cuts single-pulse false triggers by a factor of ~200 while preserving profile morphology and peak S/N. Conclusions. Beam flatfielding is a computationally cheap, simple post-beamforming step. For current and future multi-beam facilities, it provides stable bandpasses, closer-to-Gaussian noise statistics, and drastically fewer false positives, easing downstream classification without sacrificing sensitivity.</summary>\n    <category scheme='http://arxiv.org/schemas/atom' term='astro-ph.IM'/>\n    <category scheme='http://arxiv.org/schemas/atom' term='astro-ph.HE'/>\n    <published>2026-03-13T13:10:42Z</published>\n    <arxiv:primary_category term='astro-ph.IM'/>\n    <author>\n      <name>Dirk Kuiper</name>\n    </author>\n    <author>\n      <name>Cees Bassa</name>\n    </author>\n    <author>\n      <name>Ziggy Pleunis</name>\n    </author>\n    <author>\n      <name>Jason Hessels</name>\n    </author>\n  </entry>"
}