The Photon Counting Camera CP40

Foy, R.

doi:10.1007/978-1-4612-3880-5_58

Cited by 10 publications

(2 citation statements)

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“…After years of struggling with custom-built photon-counting cameras for visible-light interferometry work, such as the PAPA camera (Papaliolios et al 1985, Lawson 1994) and intensified CCDs (e.g. Blazit (1987), Foy (1988)), commercial devices are being sold aimed at the adaptive optics market which have high quantum efficiencies (>50%), kilohertz frame times, and read noise of only a few electrons (fast readout CCDs). For beam combination schemes where single pixel detectors are suitable, Avalanche photo-diodes (APDs) have as high quantum efficiency as CCDs but can photon-count at rates up to 10 MHz, although the best commercial devices seem to have an expensive tendency to stop working.…”

Section: Beam Combination and Fringe Modulationmentioning

confidence: 99%

Optical interferometry in astronomy

2003

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Abstract. Here I review the current state of the field of optical stellar interferometry, concentrating on ground-based work although a brief report of space interferometry missions is included. We pause both to reflect on decades of immense progress in the field as well as to prepare for a new generation of large interferometers just now being commissioned (most notably, the CHARA, Keck and VLT Interferometers). First, this review summarizes the basic principles behind stellar interferometry needed by the lay-physicist and general astronomer to understand the scientific potential as well as technical challenges of interferometry. Next, the basic design principles of practical interferometers are discussed, using the experience of past and existing facilities to illustrate important points. Here there is significant discussion of current trends in the field, including the new facilities under construction and advanced technologies being debuted. This decade has seen the influence of stellar interferometry extend beyond classical regimes of stellar diameters and binary orbits to new areas such as mapping the accretion disks around young stars, novel calibration of the Cepheid Period-Luminosity relation, and imaging of stellar surfaces. The third section is devoted to the major scientific results from interferometry, grouped into natural categories reflecting these current developments. Lastly, I consider the future of interferometry, highlighting the kinds of new science promised by the interferometers coming on-line in the next few years. I also discuss the longer-term future of optical interferometry, including the prospects for space interferometry and the possibilities of large-scale ground-based projects. Critical technological developments are still needed to make these projects attractive and affordable. †

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Section: Beam Combination and Fringe Modulationmentioning

confidence: 99%

Optical interferometry in astronomy

2003

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“…The CP40 (Blazit, 1987;Foy, 1988b) is an ICCD photon-counting detector. The intensified image is divided into 4 quadrants by a fiber optics splitter.…”

Section: The Cp40 Photon-counting Detectormentioning

confidence: 99%

The Extended Hα Component of T Tau

Thiébaut

Devaney

Foy

et al. 1994

Symp. - Int. Astron. Union

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We report the observation of T Tau by visible speckle interferometry at the CFHT. The observations were carried out at two wavelengths simultaneously. Each image was split into two, allowing improved data processing. The 4-channel photon-counting detector CP40 was used. We have discovered that 30% of the total energy at Hα is emitted by an extended elliptical component, with a FWHM of 70 marcsec. In the neighbouring continuum, T Tau is not resolved by the 3.60 m CFHT. We briefly discuss the astrophysical consequences of this new result.

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