{"paper":{"title":"Model for a Noise Matched Phased Array Feed","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.IM","authors_text":"2), 2. National Radio Astronomy Observatory, Arecibo, Arecibo Observatory, Charlottesville), D. Anish Roshi (1, Ionosphere Center, J. Richard Fisher (2) (1. National Astronomy, W. Shillue (2)","submitted_at":"2019-02-05T01:51:11Z","abstract_excerpt":"We present a model for a Noise Matched Phased Array Feed (PAF) system and compare model predictions with the measurement results. The PAF system consists of an array feed, a receiver, a beamformer and a parabolic reflector. The novel aspect of our model is the characterization of the {\\em PAF system} by a single matrix. This characteristic matrix is constructed from the open-circuit voltage covariance at the output of the PAF due to signal from the observing source, ground spillover noise, sky background noise and (low-noise) amplifier (LNA) noise. The best signal-to-noise ratio on the source "},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1902.01515","kind":"arxiv","version":2},"verdict":{"id":null,"model_set":{},"created_at":null,"strongest_claim":"","one_line_summary":"","pipeline_version":null,"weakest_assumption":"","pith_extraction_headline":""},"references":{"count":0,"sample":[],"resolved_work":0,"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57","internal_anchors":0},"formal_canon":{"evidence_count":0,"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"author_claims":{"count":0,"strong_count":0,"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"builder_version":"pith-number-builder-2026-05-17-v1"}