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A Calibration System for Compton Polarimetry at $e^+e^-$ Linear Colliders

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arxiv 1509.03178 v1 pith:TGCUWHRS submitted 2015-09-10 physics.ins-det

classification physics.ins-det
keywords calibrationcomptoncollidersdetectorlinearsystemfuturemethod
verification ladder T0 review T1 audit T2 compute T3 formal
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abstract

Polarimetry with permille-level precision is essential for future electron-positron linear colliders. Compton polarimeters can reach negligible statistical uncertainties within seconds of measurement time. The dominating systematic uncertainties originate from the response and alignment of the detector which records the Compton scattered electrons. The robust baseline technology for the Compton polarimeters foreseen at future linear colliders is based on an array of gas Cherenkov detectors read out by photomultipliers. In this paper, we will present a calibration method which promises to monitor nonlinearities in the response of such a detector at the level of a few permille. This method has been implemented in an LED-based calibration system which matches the existing prototype detector. The performance of this calibration system is sufficient to control the corresponding contribution to the total uncertainty on the extracted polarisation to better than $0.1\%$.

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Cited by 2 Pith papers

Reviewed papers in the Pith corpus that reference this work. Sorted by Pith novelty score. Full citation record

  1. Tests of the Standard Model at the International Linear Collider

    hep-ex 2019-08 conditional novelty 5.0 of 10

    The paper projects that a polarized e+e- collider at 250 GeV to 1 TeV would measure most Higgs couplings to sub-percent precision and improve many electroweak observables by an order of magnitude.

  2. Letter of Intent for the LUXE Experiment

    physics.ins-det 2019-09 unverdicted novelty 4.0 of 10

    LUXE is a proposed experiment to collide XFEL electrons or bremsstrahlung photons with a 30-300 TW laser, reaching laser intensity parameter ξ up to 16 and quantum parameter χ up to 3.3.

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