Determination of the multiplier gain of a photomultiplier

Wright, A. G.

doi:10.1088/0022-3735/14/7/017

Cited by 11 publications

(3 citation statements)

References 15 publications

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“…Scope of this paper is the determination of the first of these two coefficients; methods to determine the second are discussed e.g. in [6,7,8].…”

Section: Response and Energy Calibration Of Iactsmentioning

confidence: 99%

“…One can, e.g., combine data-sheet specifications, educated guesses, and measurements for the individual factors entering K IACT . In particular, the crucial factor G P M G el can be determined by either directly observing the singlephotoelectron peak in the digitized spectrum (see, e.g., [6]), or by determining the mean number of photoelectrons generated by a test light pulse on the basis of the relative width of distribution of digitized signals, which is proportional to 1/ √ n pe , modulo corrections for the width of the single-photoelectron peak, intensity fluctations of the test light pulse, and electronics and digitizer noise; see, e.g., [7,8]. A problem with this technique is that data-sheet specifications are not always reliable (mirror reflectivity will e.g.…”

Section: Response and Energy Calibration Of Iactsmentioning

confidence: 99%

See 1 more Smart Citation

Calibration of the sensitivity of imaging atmospheric Cherenkov telescopes using a reference light source

Fraß¹,

Köhler²,

Hermann³

et al. 1997

Astroparticle Physics

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The sensitivity of an Imaging Atmospheric Cherenkov telescope is calibrated by shining, from a distant pulsed monochromatic light source, a defined photon flux onto the mirror. The light pulse is captured and reconstructed by the telescope in an identical fashion as real Cherenkov light. The intensity of the calibration light pulse is monitored via a calibrated sensor at the telescope; in order to account for the lower sensitivity of this sensor compared to the Cherenkov telescope, an attenuator is inserted in the light source between the measurements with the calibrated sensor, and with the telescope. The resulting telescope sensitivities have errors of 10%, and compare well with other estimates of the sensitivity.Imaging Atmospheric Cherenkov Telescopes (IACTs) have evolved into the most powerful tool for the study of galactic and extragalactic γ-ray sources in the TeV energy range [1]. In IACTs, a (frequently tesselated) reflector with areas between a few m 2 and almost 100 m 2 is used to image the Cherenkov photons emitted by an air shower onto a camera consisting of photomultiplier (PM) pixels. The elliptical shower image traces the longitudinal development of an air shower. The long axis of the image points to the image of the source. The shape of the image allows to distinguish, to a certain degree, compact γ-ray induced showers from the more diffuse cosmic-ray showers [2]. The power of IACTs can be improved significantly by operating multiple IACTs in a stereo mode, observing the same shower with several IACTs in coincidence. Stereo imaging allows the unambiguous spatial reconstruction of the direction of individual air showers with a precision of 0.1• and better [3,4,5], and therefore provides the best angular resolution of all tools in γ-ray astronomy.As the field matures, emphasis is shifting from the simple detection of TeV γ-ray sources to the precise determination of source fluxes and their spectra. The spectra contain important clues both concerning the acceleration mechanisms

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“…Scope of this paper is the determination of the first of these two coefficients; methods to determine the second are discussed e.g. in [6,7,8].…”

Section: Response and Energy Calibration Of Iactsmentioning

confidence: 99%

Section: Response and Energy Calibration Of Iactsmentioning

confidence: 99%

Calibration of the sensitivity of imaging atmospheric Cherenkov telescopes using a reference light source

Fraß¹,

Köhler²,

Hermann³

et al. 1997

Astroparticle Physics

View full text Add to dashboard Cite

show abstract

“…For the HV tuning it is necessary to provide a robust method of the gain measurement. The method of a multiplier gain measurement with multichannel analyzer in the self-triggering mode has a precision worse than 10% [3]. The fundamental limit comes from the inability of a multichannel analyzer used in the measurements to access all the contributions from the low amplitude region.…”

Section: Electron Multiplier Gain Measurementsmentioning

confidence: 99%

Setting of the predefined multiplier gain of a photomultiplier

Smirnov

2019

Preprint

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A method to set the predefined PMT gain with high precision is described. The method supposes minimal participation of the operator. After the rough initial setting of the gain, the automated system adjusts the PMT gain within a predefined precision (up to 2%). The method has been successfully applied at the Borexino PMT test facility at LNGS for the gain adjustment of the 2000 photomultipliers for the Borexino detector

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Optimal use of photomultipliers for chemiluminescence and bioluminescence applications

Ellis¹,

Wright²

1999

Luminescence

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Determination of the multiplier gain of a photomultiplier

Cited by 11 publications

References 15 publications

Calibration of the sensitivity of imaging atmospheric Cherenkov telescopes using a reference light source

Calibration of the sensitivity of imaging atmospheric Cherenkov telescopes using a reference light source

Setting of the predefined multiplier gain of a photomultiplier

Optimal use of photomultipliers for chemiluminescence and bioluminescence applications

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