 |
INGRID was mostly designed and
built in-house at the Isaac Newton Group of Telescopes, with help,
primarily at the early stages, from the now defunct RGO, the ATC and
the IAC. It has been commissioned in March 2000.
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Overview of INGRID
| Array | 1024x1024 HAWAII array, HgCdTe, sensitive from 0.?? - 2.5 microns |
| Quantum Efficiency | J = 40%, H = 55%, K = 55% (approx. figures) |
| Read noise | 10-15 e- per frame |
| Limiting Magnitude (1) | See SIGNAL |
| Optics | Optimized for 0.8 - 2.5 microns |
| Throughput | Net ~ 24%, similar to WHIRCAM (estimated) |
| Focal Station (2) | WHT Cassegrain IR port (AUX port B) |
| Plate scale | 0.242 arcsec/pixel giving a 4.13 x 4.13 arcminute field of view |
| Integration Times | 0.6 seconds minimum, 3600 seconds maximum |
| Broad Band Filters | Z, J,
H, K and K_s currently available
(more information here) |
| Narrow Band Filters | 11 narrow
band filters on order
(more information here) |
| Background | Dominated by sky OH emission (estimated) |
| Pupil Stops | Selectable - one optimized for >2 microns, second optimized for shorter wavelengths |
| (1) | Based on a 9000 second exposure of a stellar source, 1" seeing and a detection representing a S/N of 3 |
| (2) | INGRID is also the NAOMI imager at the Nasmyth focus |