SCUBA-2: a 10,000-pixel submillimeter camera for the James Clerk Maxwell Telescope

Holland, W. S.; MacIntosh, Michael J.; Fairley, Alasdair; Kelly, Dennis; Montgomery, David; Gostick, David C.; Atad-Ettedgui, Eli; Ellis, Maureen A.; Robson, Ian; Hollister, Matthew I.; Woodcraft, A.; Ade, Peter A. R.; Walker, I. K.; Irwin, K. D.; Hilton, G. C.; Duncan, William; Reintsema, C. D.; Walton, A.J.; Parkes, W.; Dunare, Camelia; Fich, M.; Kycia, J. B.; Halpern, M.; Scott, D.; Gibb, A. G.; Molnar, J.; Chapin, E. L.; Bintley, Dan; Craig, Simon C.; Chylek, Tomas; Jenness, Tim; Economou, Frossie; Davis, G. R.

doi:10.1117/12.671186

Cited by 80 publications

(36 citation statements)

References 6 publications

(8 reference statements)

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“…On the other hand, MAMBO with its 11 resolution was successful in separating sub-structures on a scale of 0.1 pc; further progress should be possible with Herschel. To determine the role of surface density and more generally which cold high-mass clumps will evolve to produce high-mass protostars, even higher resolution observations will be required, and so there appears to be a rich future in uncovering the unseen story using SCUBA2 (8 resolution at 450 μm, Holland et al 2006), CCAT (3. 5 at 350 μm, Sebring 2010), and ALMA 18 (down to subarcsecond resolution at submillimeter wavelengths).…”

Section: Discussionmentioning

confidence: 99%

THE BALLOON-BORNE LARGE APERTURE SUBMILLIMETER TELESCOPE (BLAST) 2005: A 10 deg²SURVEY OF STAR FORMATION IN CYGNUS X

Roy

Ade

Bock

et al. 2011

ApJ

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We present Cygnus X in a new multi-wavelength perspective based on an unbiased BLAST survey at 250, 350, and 500 μm, combined with rich data sets for this well-studied region. Our primary goal is to investigate the early stages of high-mass star formation. We have detected 184 compact sources in various stages of evolution across all three BLAST bands. From their well-constrained spectral energy distributions, we obtain the physical properties mass, surface density, bolometric luminosity, and dust temperature. Some of the bright sources reaching 40 K contain well-known compact H ii regions. We relate these to other sources at earlier stages of evolution via the energetics as deduced from their position in the luminosity-mass (L-M) diagram. The BLAST spectral coverage, near the peak of the spectral energy distribution of the dust, reveals fainter sources too cool (∼10 K) to be seen by earlier shorter-wavelength surveys like IRAS. We detect thermal emission from infrared dark clouds and investigate the phenomenon of cold "starless cores" more generally. Spitzer images of these cold sources often show stellar nurseries, but these potential sites for massive star formation are "starless" in the sense that to date there is no massive protostar in a vigorous accretion phase. We discuss evolution in the context of the L-M diagram. Theory raises some interesting possibilities: some cold massive compact sources might never form a cluster containing massive stars, and clusters with massive stars might not have an identifiable compact cold massive precursor.

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Section: Discussionmentioning

confidence: 99%

THE BALLOON-BORNE LARGE APERTURE SUBMILLIMETER TELESCOPE (BLAST) 2005: A 10 deg²SURVEY OF STAR FORMATION IN CYGNUS X

Roy

Ade

Bock

et al. 2011

ApJ

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“…The third and fourth stages of the instrument are cooled by a two stage 3 He adsorption refrigerator. The cooling capacities of the intercooler (IC) and ultracooler (UC) stills of the refrigerator are shown in Figs.…”

Section: Sub-kelvin Stagesmentioning

confidence: 99%

The cryomechanical design of MUSIC: a novel imaging instrument for millimeter-wave astrophysics at the Caltech Submillimeter Observatory

et al. 2010

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MUSIC (Multicolor Submillimeter kinetic Inductance Camera) is a new facility instrument for the Caltech Submillimeter Observatory (Mauna Kea, Hawaii) developed as a collaborative effect of Caltech, JPL, the University of Colorado at Boulder and UC Santa Barbara, and is due for initial commissioning in early 2011. MUSIC utilizes a new class of superconducting photon detectors known as microwave kinetic inductance detectors (MKIDs), an emergent technology that offers considerable advantages over current types of detectors for submillimeter and millimeter direct detection. MUSIC will operate a focal plane of 576 spatial pixels, where each pixel is a slot line antenna coupled to multiple detectors through on-chip, lumped-element filters, allowing simultaneously imaging in four bands at 0.86, 1.02, 1.33 and 2.00 mm.The MUSIC instrument is designed for closed-cycle operation, combining a pulse tube cooler with a two-stage Helium-3 adsorption refrigerator, providing a focal plane temperature of 0.25 K with intermediate temperature stages at approximately 50, 4 and 0.4 K for buffering heat loads and heat sinking of optical filters. Detector readout is achieved using semi-rigid coaxial cables from room temperature to the focal plane, with cryogenic HEMT amplifiers operating at 4 K. Several hundred detectors may be multiplexed in frequency space through one signal line and amplifier. This paper discusses the design of the instrument cryogenic hardware, including a number of features unique to the implementation of superconducting detectors. Predicted performance data for the instrument system will also be presented and discussed.

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“…The success of tests to date has enabled the production of science grade arrays to start, with delivery of the instrument to the telescope (JCMT, Mauna Kea, Hawaii) expected in late 2006. Further information on the instrument and detectors, and the many groups involved in the design and construction, can be found in [1] & [2].…”

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Detectors for the 10000 Pixel SCUBA-2 Super-conducting Sub-mm Camera for Astronomy

Woodcraft

2006

2006 Joint 31st International Conference on Infrared Millimeter Waves and 14th International Conference on Teraherz Electronics

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-We describe the current status of the SCUBA-2 sub-mm camera for astronomy.Current continuum (broadband) instruments for submillimetre astronomy (wavelengths of a few hundred μm to a few mm) are severely limited by the small number of pixels. Instruments have moved from a single pixel to hundreds over the last decade, and further increases in pixel count are necessary to exploit existing and future telescopes. Another aim is to achieve background limited performance (BLIP), in which the noise limit is set by photon noise from background radiation. Bolometric detection is used, since this is the most sensitive method. Until recently instruments have generally used germanium semiconducting thermometers. However, despite having reached the fundamental noise limits, these detectors are not background limited for the best ground based telescopes. It is also difficult to make arrays because the germanium chips must be individually glued to each pixel, and because they cannot be multiplexed.Superconducting detectors (transition edge sensors) are therefore being used for the next generation of instruments. As well as being able to achieve better signal to noise than semiconducting bolometers, it is possible to fabricate an entire array without any operations being required at the level of a single pixel. Moreover, a multiplexed readout can be used.However, the amount of wiring required between a detector array and multiplexer chip has set a practical limit on the array size. For SCUBA-2, array sizes of over 1000 pixels ( Fig. 1) are achieved by using a new multiplexer configuration, in which the multiplexer wafer is bonded to the detector wafer, with indium bump bonds providing electrical connections between each pixel and the multiplexer. These arrays can be butted together on two sides, to form focal planes of over 5000 pixels. A time division multiplexing scheme (TDM) is used, with multiplexers supplied by NIST. The detectors themselves consist of Mo/Cu bi-layer thermistors, with weak thermal linking provided by a silicon nitride membrane. To obtain the required performance, the arrays must be operated from a heat sink at a temperature of approximately 0.06 K, with cooling to this temperature provided by a dilution refrigerator. This operates from a temperature of 4 K, which traditionally would be provided by a liquid helium bath. To avoid the running costs associated with liquid helium consumption, the instrument is instead mechanically cooled using pulse tube coolers.The size of the instrument (over 5 m 3 ; Fig. 2) is driven by the large mirrors required due to the large field of view. The last three mirrors must be cooled to below 10 K in order to reduce the thermal background on the arrays.SCUBA-2 will operate simultaneously at two wavelength ranges centred on 450 and 850 microns (670 and 350 GHz). So far, a prototype array designed for each wavelength range has been tested in a dedicated testbed, with results meeting the specifications. One array has also been tested in the instrument itself, demonstrat...

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SCUBA-2: a 10,000-pixel submillimeter camera for the James Clerk Maxwell Telescope

Cited by 80 publications

References 6 publications

THE BALLOON-BORNE LARGE APERTURE SUBMILLIMETER TELESCOPE (BLAST) 2005: A 10 deg²SURVEY OF STAR FORMATION IN CYGNUS X

THE BALLOON-BORNE LARGE APERTURE SUBMILLIMETER TELESCOPE (BLAST) 2005: A 10 deg²SURVEY OF STAR FORMATION IN CYGNUS X

The cryomechanical design of MUSIC: a novel imaging instrument for millimeter-wave astrophysics at the Caltech Submillimeter Observatory

Detectors for the 10000 Pixel SCUBA-2 Super-conducting Sub-mm Camera for Astronomy

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SCUBA-2: a 10,000-pixel submillimeter camera for the James Clerk Maxwell Telescope

Cited by 80 publications

References 6 publications

THE BALLOON-BORNE LARGE APERTURE SUBMILLIMETER TELESCOPE (BLAST) 2005: A 10 deg2SURVEY OF STAR FORMATION IN CYGNUS X

THE BALLOON-BORNE LARGE APERTURE SUBMILLIMETER TELESCOPE (BLAST) 2005: A 10 deg2SURVEY OF STAR FORMATION IN CYGNUS X

The cryomechanical design of MUSIC: a novel imaging instrument for millimeter-wave astrophysics at the Caltech Submillimeter Observatory

Detectors for the 10000 Pixel SCUBA-2 Super-conducting Sub-mm Camera for Astronomy

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THE BALLOON-BORNE LARGE APERTURE SUBMILLIMETER TELESCOPE (BLAST) 2005: A 10 deg²SURVEY OF STAR FORMATION IN CYGNUS X

THE BALLOON-BORNE LARGE APERTURE SUBMILLIMETER TELESCOPE (BLAST) 2005: A 10 deg²SURVEY OF STAR FORMATION IN CYGNUS X