Status of MUSIC, the MUltiwavelength Sub/millimeter Inductance Camera

Sunil R. Golwala; Clint Bockstiegel; Spencer Brugger; Nicole G. Czakon; Peter K. Day; Thomas P. Downes; Ran Duan; Jiansong Gao; Amandeep K. Gill; Jason Glenn; Matthew I. Hollister; Henry G. LeDuc; Philip R. Maloney; Benjamin A. Mazin; Sean G. McHugh; David Miller; Omid Noroozian; Hien T. Nguyen; Jack Sayers; James A. Schlaerth; Seth Siegel; Anastasios K. Vayonakis; Philip R Wilson; Jonas Zmuidzinas

doi:10.1117/12.926055

27 September 2012 Status of MUSIC, the MUltiwavelength Sub/millimeter Inductance Camera

Sunil R. Golwala, Clint Bockstiegel, Spencer Brugger, Nicole G. Czakon, Peter K. Day, Thomas P. Downes, Ran Duan, Jiansong Gao, Amandeep K. Gill, Jason Glenn, Matthew I. Hollister, Henry G. LeDuc, Philip R. Maloney, Benjamin A. Mazin, Sean G. McHugh, David Miller, Omid Noroozian, Hien T. Nguyen, Jack Sayers, James A. Schlaerth, Seth Siegel, Anastasios K. Vayonakis, Philip R Wilson, Jonas Zmuidzinas

Author Affiliations +

Proceedings Volume 8452, Millimeter, Submillimeter, and Far-Infrared Detectors and Instrumentation for Astronomy VI; 845205 (2012) https://doi.org/10.1117/12.926055
Event: SPIE Astronomical Telescopes + Instrumentation, 2012, Amsterdam, Netherlands

Abstract

We present the status of MUSIC, the MUltiwavelength Sub/millimeter Inductance Camera, a new instrument for the Caltech Submillimeter Observatory. MUSIC is designed to have a 14', diffraction-limited field-of-view instrumented with 2304 detectors in 576 spatial pixels and four spectral bands at 0.87, 1.04, 1.33, and 1.98 mm. MUSIC will be used to study dusty star-forming galaxies, galaxy clusters via the Sunyaev-Zeldovich effect, and star formation in our own and nearby galaxies. MUSIC uses broadband superconducting phased-array slot-dipole antennas to form beams, lumpedelement on-chip bandpass filters to define spectral bands, and microwave kinetic inductance detectors to sense incoming light. The focal plane is fabricated in 8 tiles consisting of 72 spatial pixels each. It is coupled to the telescope via an ambient-temperature ellipsoidal mirror and a cold reimaging lens. A cold Lyot stop sits at the image of the primary mirror formed by the ellipsoidal mirror. Dielectric and metal-mesh filters are used to block thermal infrared and out-ofband radiation. The instrument uses a pulse tube cooler and³He/³He/⁴He closed-cycle cooler to cool the focal plane to below 250 mK. A multilayer shield attenuates Earth's magnetic field. Each focal plane tile is read out by a single pair of coaxes and a HEMT amplifier. The readout system consists of 16 copies of custom-designed ADC/DAC and IF boards coupled to the CASPER ROACH platform. We focus on recent updates on the instrument design and results from the commissioning of the full camera in 2012.

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Sunil R. Golwala, Clint Bockstiegel, Spencer Brugger, Nicole G. Czakon, Peter K. Day, Thomas P. Downes, Ran Duan, Jiansong Gao, Amandeep K. Gill, Jason Glenn, Matthew I. Hollister, Henry G. LeDuc, Philip R. Maloney, Benjamin A. Mazin, Sean G. McHugh, David Miller, Omid Noroozian, Hien T. Nguyen, Jack Sayers, James A. Schlaerth, Seth Siegel, Anastasios K. Vayonakis, Philip R Wilson, and Jonas Zmuidzinas "Status of MUSIC, the MUltiwavelength Sub/millimeter Inductance Camera", Proc. SPIE 8452, Millimeter, Submillimeter, and Far-Infrared Detectors and Instrumentation for Astronomy VI, 845205 (27 September 2012); https://doi.org/10.1117/12.926055

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