TY - GEN
T1 - SCUBA. Submillimetre common-user bolometer array for the James Clerk Maxwell Telescope
AU - Cunningham, Colin R.
AU - Gear, Walter K.
PY - 1990
Y1 - 1990
N2 - We describe a submillimetre continuum array instrument being built by the Royal Observatory, Edinburgh (ROE) for the 15m James Clerk Maxwell Telescope (JCMT) on Mauna Kea, Hawaii. The instrument contains 2 arrays, one of 91 pixels optimised for 438 μm and the second of 37 pixels optimised for 855 μm. Both are hexagonally close-packed, with each pixel having diffraction-limited angular resolution. Conical horns and single-moded waveguides are used to couple to the submillimetre beams, minimising the bolometer background loading. A filter changing mechanism allows operation of the arrays at 350 and 750 μm. Single 'photometric' pixels are provided optimised for operation at 350, 600, 750, 1100, 1400 and 2000 μm. The instrument will have bolometers sensitive enough to reach the photon-noise sensitivity limit at both wavelengths, corresponding to an optical noise equivalent power (NEP) of 1.6×10-16 W.Hz- 1/2 . This is achieved by cooling to 0.1 K, using a dilution refrigerator.
AB - We describe a submillimetre continuum array instrument being built by the Royal Observatory, Edinburgh (ROE) for the 15m James Clerk Maxwell Telescope (JCMT) on Mauna Kea, Hawaii. The instrument contains 2 arrays, one of 91 pixels optimised for 438 μm and the second of 37 pixels optimised for 855 μm. Both are hexagonally close-packed, with each pixel having diffraction-limited angular resolution. Conical horns and single-moded waveguides are used to couple to the submillimetre beams, minimising the bolometer background loading. A filter changing mechanism allows operation of the arrays at 350 and 750 μm. Single 'photometric' pixels are provided optimised for operation at 350, 600, 750, 1100, 1400 and 2000 μm. The instrument will have bolometers sensitive enough to reach the photon-noise sensitivity limit at both wavelengths, corresponding to an optical noise equivalent power (NEP) of 1.6×10-16 W.Hz- 1/2 . This is achieved by cooling to 0.1 K, using a dilution refrigerator.
UR - http://www.scopus.com/inward/record.url?scp=0025641982&partnerID=8YFLogxK
U2 - 10.1117/12.19115
DO - 10.1117/12.19115
M3 - Conference Publication
AN - SCOPUS:0025641982
SN - 0819402796
SN - 9780819402790
T3 - Proceedings of SPIE - The International Society for Optical Engineering
SP - 515
EP - 523
BT - Proceedings of SPIE - The International Society for Optical Engineering
PB - Publ by Int Soc for Optical Engineering
T2 - Instrumentation in Astronomy VII
Y2 - 13 February 1990 through 17 February 1990
ER -