GISMO: a 2-millimeter bolometer camera for the IRAM 30 m telescope

Staguhn, Johannes; Benford, Dominic J.; Allen, Christine A.; Moseley, S. H.; Sharp, Elmer H.; Ames, Troy; Brunswig, W.; Chuss, David T.; Dwek, Eli; Maher, Stephen F.; Marx, Catherine; Miller, Timothy M.; Vilanova, Santiago; Wollack, Edward J.

doi:10.1117/12.671970

Cited by 24 publications

(13 citation statements)

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“…The reason for this is predominantly of technical nature, in particular the very demanding requirements on the noise performance of a background-limited camera operating in this low opacity atmospheric window. In order to provide background-limited observations in the 2 mm window at a good mountain site such as the IRAM 30 m telescope on Pico Veleta, the required sensitivity, expressed in Noise Equivalent Power, for the detectors is ∼5 × 10 −17 W √ s (Staguhn et al 2006), a requirement that is met by our "high" temperature (T c = 450 mK) Transition Edge Sensor (TES) detectors. Consequently we have proposed and built a 2 mm wavelength bolometer camera, the GISMO , for astronomical observations at the IRAM 30 m telescope on Pico Veleta, Spain (Baars et al 1987).…”

Section: The Gismo 2 MM Cameramentioning

confidence: 99%

The Gismo Two-Millimeter Deep Field in Goods-N

Staguhn

Kovács

Arendt

et al. 2014

ApJ

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We present deep continuum observations using the GISMO camera at a wavelength of 2 mm centered on the Hubble Deep Field in the GOODS-N field. These are the first deep field observations ever obtained at this wavelength. The 1σ sensitivity in the innermost ∼4 of the 7 diameter map is ∼135 μJy beam −1 , a factor of three higher in flux/beam sensitivity than the deepest available SCUBA 850 μm observations, and almost a factor of four higher in flux/beam sensitivity than the combined MAMBO/AzTEC 1.2 mm observations of this region. Our source extraction algorithm identifies 12 sources directly, and another 3 through correlation with known sources at 1.2 mm and 850 μm. Five of the directly detected GISMO sources have counterparts in the MAMBO/AzTEC catalog, and four of those also have SCUBA counterparts. HDF850.1, one of the first blank-field detected submillimeter galaxies, is now detected at 2 mm. The median redshift of all sources with counterparts of known redshifts is z = 2.91 ± 0.94. Statistically, the detections are most likely real for five of the seven 2 mm sources without shorter wavelength counterparts, while the probability for none of them being real is negligible.

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Section: The Gismo 2 MM Cameramentioning

confidence: 99%

The Gismo Two-Millimeter Deep Field in Goods-N

Staguhn

Kovács

Arendt

et al. 2014

ApJ

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“…GISMO (actually named GISMO-2 after the earlier prototype, GISMO; Staguhn et al, 2006) is designed to detect the highest-redshift DSFGs by taking advantage of the dramatic K-correction at 2 mm (see Figure 3). The field of view is 1.8×3.7 arcmin and the beamsize 16.7 .…”

Section: Goddard-iram Superconducting 2-millimeter Observer [Gismo] mentioning

confidence: 99%

Dusty star-forming galaxies at high redshift

2014

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Far-infrared and submillimeter wavelength surveys have now established the important role of dusty, star-forming galaxies (DSFGs) in the assembly of stellar mass and the evolution of massive galaxies in the Universe. The brightest of these galaxies have infrared luminosities in excess of 10 13 L with implied star-formation rates of thousands of solar masses per year. They represent the most intense starbursts in the Universe, yet many are completely optically obscured. Their easy detection at submm wavelengths is due to dust heated by ultraviolet radiation of newly forming stars. When summed up, all of the dusty, star-forming galaxies in the Universe produce an infrared radiation field that has an equal energy density as the direct starlight emission from all galaxies visible at ultraviolet and optical wavelengths. The bulk of this infrared extragalactic background light emanates from galaxies as diverse as gas-rich disks to mergers of intense starbursting galaxies. Major advances in far-infrared instrumentation in recent years, both spacebased and ground-based, has led to the detection of nearly a million DSFGs, yet our understanding of the underlying astrophysics that govern the start and end of the dusty starburst phase is still in nascent stage. This review is aimed at summarizing the current status of DSFG studies, focusing especially on the detailed characterization of the bestunderstood subset (submillimeter galaxies, who were summarized in the last review of this field over a decade ago, Blain et al. 2002), but also the selection and characterization of more recently discovered DSFG populations. We review DSFG population statistics, their physical properties including dust, gas and stellar contents, their environments, and current theoretical models related to the formation and evolution of these galaxies.

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“…The near-term applicability of the BUG detector architecture is primarily for upgrades of existing ground-based and airborne instruments, and applicability to small, rapid development cycle instruments such as GISMO [15] . The GISMO focal plane was designed to accommodate a 32×40 array of 1.1 mm BUG detectors, equivalent to one quadrant of an array the size of the SCUBA-2 array, although it presently holds an 8×16 format array of 2 mm pixels.…”

Section: Applicability To Astronomical Instrumentsmentioning

confidence: 99%

Technology developments toward large format long wavelength bolometer arrays

et al. 2007

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We are developing a kilopixel, filled bolometer array for infrared astronomy. The array consists of three individual components, to be merged into a single, working unit; 1) a transition edge sensor (TES) bolometer array, operating in the milliKelvin regime, 2) quarter-wave resonance backshorts, and 3) superconducting quantum interference device (SQUID) multiplexer readout. The detector array is a filled, square-grid of suspended, silicon membrane bolometers with superconducting thermistors. The spacing of the backshort beneath the detector grid can be set from ~30-300 microns by adjusting two process parameters during fabrication. We have produced prototype, monolithic arrays having 1 mm and 2 mm pitch detectors. The key technologies required for kilopixel arrays of detectors to be hybridized to SQUID multiplexer readout circuits have been demonstrated. Mechanical models of large-format detector grids have been indium bump-bonded to dummy multiplexer readouts to study electrical continuity. A monolithic array of 1 mm pitch detectors has been mated to a backshort grid optimized for a 350 micron resonant wavelength. Through-wafer microvias, for electroplated, low-resistance electrical connection of detector elements, have been prototyped using deep reactive ion etching. The ultimate goal of this work is to develop large-format (thousands of pixels) bolometer array architecture with background-limited sensitivity, suitable for a wide range of long wavelengths and a wide range of astronomical applications such as imaging, spectroscopy, and polarimetry and applicable for ground-based, suborbital, and space-based instruments.

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GISMO: a 2-millimeter bolometer camera for the IRAM 30 m telescope

Cited by 24 publications

References 0 publications

The Gismo Two-Millimeter Deep Field in Goods-N

The Gismo Two-Millimeter Deep Field in Goods-N

Dusty star-forming galaxies at high redshift

Technology developments toward large format long wavelength bolometer arrays

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