The CFHT CCD Detector

Walker, G. A. H.; Johnson, R.; Christian, C. A.; Kormendy, John

doi:10.1117/12.944681

Cited by 3 publications

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“…because in recent years charge-coupled devices have become the instrument of choice for most electronic image detection at optical and near-infrared wavelengths, the remaining discussion will concentrate on them to the exclusion of other detector systems. For discussions of the properties of CCDs in astronomical applications, see, for example, G. A. H. Walker et al (1984), Massey (1985), and Jacoby (1985).…”

Section: Introductionmentioning

confidence: 99%

“…Flat-field patterns, which are variations in the intensity scale, manifest themselves both globally across the chip and locally from one pixel to the next, and usually depend significantly on the color temperature of the illumination. In addition, position-dependent variations are often found in the dark counts due, for instance, to certain P-N junctions in the chip acting as light-emitting diodes, or to the on-chip amplifier s keeping one part of the detector constantly warmer than the rest (see, e.g., G. A. H. Walker et al 1984). Finally, with some devices and in some photometric passbands strong spatial variations in the sky brightness are found, caused by interference within the detector of the light of night-sky emission lines.…”

Section: Introductionmentioning

confidence: 99%

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DAOPHOT - A computer program for crowded-field stellar photometry

Stetson¹

1987

PASP

4,535

4,065

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The difficult art of stellar photometry in crowded fields is currently undergoing a surge of popularity, and a number of different computer programs for deriving photometric information from two-dimensional digital images are currently in use. This paper describes one such program, DAOPHOT, which was written and continues to be developed at the Dominion Astrophysical Observatory. Emphasis is placed on the various types of philosophical and technical complications which arise when accurate photometry is sought for blended stellar images, and on the mathematical algorithms with which DAOPHOT attempts to deal with these complications, rather than on details of the coding. Some ways in which DAOPHOT resembles or differs from other similar programs are mentioned, and a discussion is presented of known shortcomings of the current program as well as possibilities for future improvement.

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Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

DAOPHOT - A computer program for crowded-field stellar photometry

Stetson¹

1987

PASP

4,535

4,065

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“…The 30 µm pixels currently in use at the CFHT have a read noise of approximately 75 a and a full -well capacity in excess of 400,000 e-. 1 The dewar that housed the double-density RCA2 CCD was constrained by a number of factors. First, it was necessary for the dewar to be mechanically and optically similar to the older RCA 1 dewar.…”

Section: The Ccd Cameramentioning

confidence: 99%

Evaluation Of The RCA 640 X1024 Charge-Coupled-Device Imager For Astronomical Use

Christian

1987

Opt. Eng

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A double-density (15 ,um X15 um pixels) RCA charge -coupled device has been tested and commissioned for astronomical imaging and spectroscopy at the Canada -France -Hawaii telescope (CFHT). This thinned device has had its support glass removed and has received a broadband antireflection coating to improve the UV and blue response. Presented here are characterization measurements resulting from 10 months of laboratory testing and use at the telescope. Although the read noise is not as low as with other CCDs available, the high pixel density and the permanent quantum efficiency enhancements provided by this RCA device give some advantages over other sensors when used at the CFHT.

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The Mass Distribution in the Elliptical Galaxy NGC 3377: Evidence for a 2 × 10[TSUP]8[/TSUP] [ITAL]M[/ITAL][TINF][sun][/TINF] Black Hole

Kormendy

Bender

Evans

et al. 1998

The Astronomical Journal

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This paper is a study of the mass distribution in the central 35 ′′ ≃ 1.7 kpc of the E5 galaxy NGC 3377. Stellar rotation velocity and velocity dispersion profiles (seeing σ * = 0. ′′ 20 -0. ′′ 56) and V -band surface photometry (σ * = 0. ′′ 20 -0. ′′ 26) have been obtained with the Canada-France-Hawaii Telescope. NGC 3377 is kinematically similar to M 32: the central kinematic gradients are steep. There is an unresolved central rise in rotation velocity to V = 110 ± 3 km s −1 (internal error) at r = 1. ′′ 0. The apparent velocity dispersion rises from 95 ± 2 km s −1 at 1. ′′ 0 ≤ r < 4 ′′ to 178 ± 10 km s −1 at the center.To search for a central black hole, we derive three-dimensional velocity and velocity dispersion fields that fit the above observations and Hubble Space Telescope surface photometry after projection and seeing convolution. Isotropic models imply that the mass-to-light ratio rises by a factor of ∼ 4 at r < 2 ′′ to M/L V > ∼ 10. If the mass-to-light ratio of the stars, M/L V = 2.4 ± 0.2, is constant with radius, then NGC 3377 contains a central massive dark object (MDO), probably a black hole, of mass M • ≃ (1.8 ± 0.8) × 10 8 M ⊙ . Several arguments suggest that NGC 3377 is likely to be nearly isotropic. However, flattened, anisotropic maximum entropy models can fit the present data without an MDO. Therefore the MDO detection in NGC 3377 is weaker than those in M 31, M 32, and NGC 3115.The above masses are corrected for the E5 shape of the galaxy and for the difference between velocity moments and velocities given by Gaussian fits to the line profiles. We show that the latter correction does not affect the strength of the MDO detection, but it slightly reduces MTherefore the inner parts of NGC 3377 are dominated by a normal old stellar population. In this elliptical, as in the bulge-dominated galaxies NGC 3115 and NGC 4594, halo dark matter is unimportant over a significant range in radius near the center.

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The CFHT CCD Detector

Cited by 3 publications

References 0 publications

DAOPHOT - A computer program for crowded-field stellar photometry

DAOPHOT - A computer program for crowded-field stellar photometry

Evaluation Of The RCA 640 X1024 Charge-Coupled-Device Imager For Astronomical Use

The Mass Distribution in the Elliptical Galaxy NGC 3377: Evidence for a 2 × 10[TSUP]8[/TSUP] [ITAL]M[/ITAL][TINF][sun][/TINF] Black Hole

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