A 5-18 micron array camera for high-background astronomical imaging

Gezari, D. Y.; Folz, W. C.; Woods, Lawrence A.; Városi, F.

doi:10.1086/132978

Cited by 20 publications

(3 citation statements)

References 7 publications

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“…The Celeste instrument (McCabe et al , 2003 ) currently represents the only cooled-grating instrument dedicated to solar use at these wavelengths, though other instruments may have abilities here. For use on warm spectrographs, a camera system which functions at these wavelengths is the Si:Ga array detector used by Gezari et al ( 1992 ) and employed for solar observations by Gezari et al ( 1999 ). This array is nominally sensitive from 5000 to 18000 nm.…”

Section: Future Prospects For Infrared Solar Observationsmentioning

confidence: 99%

Infrared Solar Physics

Penn

2014

Living Rev. Solar Phys.

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The infrared solar spectrum contains a wealth of physical data about our Sun, and is explored using modern detectors and technology with new ground-based solar telescopes. The scientific motivation behind exploring these wavelengths is presented, along with a brief look at the rich history of observations here. Several avenues of solar physics research exploiting and benefiting from observations at infrared wavelengths from roughly 1000 nm to 12 400 nm are discussed, and the instrument and detector technology driving this research is briefly summarized. Finally, goals for future work at infrared wavelengths are presented in conjunction with ground and space-based observations.

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Section: Future Prospects For Infrared Solar Observationsmentioning

confidence: 99%

Infrared Solar Physics

Penn

2014

Living Rev. Solar Phys.

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“…During the interval 22 to 29 September 1992, the NASA 5-18μπι camera was set up on the main image of the McMath-Pierce Telescope for continuum imaging of solar disk features. See Gezari et al (1992) for technical details of the camera. Telescope image scale is 2.39 arc-sec/mm.…”

Section: Array Datamentioning

confidence: 99%

Observations of Seeing at 0.5 and 12.4 μm

Livingston

Kopp

Gezari

et al. 1994

Symp. - Int. Astron. Union

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A variety of observations have been made of solar features (sunspots, faculae, the limb) using both array and single element scanning techniques. The telescope was the 1.6 m McMath-Pierce on Kitt Peak. Array data were acquired with a 58×62 pixel Si:Ga detector at 4.8, 7.8, 12.4, and 18 μm, while a CCD camera recorded the same image position at 0.5 μm. In a separate experiment, a nutating mirror device was used to generate a raster scan of solar disk areas, the output being fed to a Si PIN diode (0.5 μm filter) and a As:Si diode (12.4 μm filter). The scanner data yield simultaneous images at the two wavelengths and was essentially a repeat of the 1970 Turon-Léna experiment with updated equipment. Examples of images at the various wavelengths are given in the poster. Analysis of the data is incomplete at this time. We can report that the effects of seeing were encountered at all wavelengths, including 18μm, even though conditions were deemed good at times (for example, penumbral filaments were resolved in sunspots). We have thus been unable to verify, as yet, the conditions reported by Bester et al, in which exceptional seeing is realized in the infrared.

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“…Other arrays are much more limited. An extreme example is the 10/rni camera described by Gezari et al (1992), based on a 58 x 62 SBRC Ga:Si hybrid chip with i 0.25 arcsec square pixels, which requires to be read out 30 times per second and the frames co-added. This requires high-speed electronics and data processing.…”

Section: Well Capacitymentioning

confidence: 99%