The Herschel/PACS 2560 bolometers imaging camera

Billot, N.; Agnèse, P.; Auguères, J.-L.; Beguin, A.; Bouere, A.; Boulade, O.; Cara, C.; Cloué, Christelle; Doumayrou, E.; Duband, L.; Horeau, B.; Mer, I. Le; Lepennec, Jean; Martignac, J.; Okumura, K.; Revéret, V.; Sauvage, M.; Simoens, F.; Vigroux, L.

doi:10.1117/12.671154

Cited by 18 publications

(19 citation statements)

References 4 publications

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“…Performance is currently limited by the noise in the MOSFET amplifiers to the NEP » 10 -16 W/Hz 1/2 regime, but this technology allows for the construction of very large arrays suitable for higher background applications. Further details are in Billot et al [67].…”

Section: Semiconductor Bolometersmentioning

confidence: 99%

“…For example, the Herschel/PACS instrument uses a 2048−pixel array of bolom− eters [67] and is an alternative to JFET amplifiers. The archi− tecture of this array is vaguely similar to the direct hybrid mid−infrared arrays, where one silicon wafer is patterned with bolometers, each in the form of a silicon mesh, as shown in Fig.…”

Section: Semiconductor Bolometersmentioning

confidence: 99%

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Semiconductor detectors and focal plane arrays for far-infrared imaging

Rogalski

2013

Opto-Electronics Review

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The detection of far-infrared (far-IR) and sub-mm-wave radiation is resistant to the commonly employed techniques in the neighbouring microwave and IR frequency bands. In this wavelength detection range the use of solid state detectors has been hampered for the reasons of transit time of charge carriers being larger than the time of one oscillation period of radiation. Also the energy of radiation quanta is substantially smaller than the thermal energy at room temperature and even liquid nitrogen temperature. The realization of terahertz (THz) emitters and receivers is a challenge because the frequencies are too high for conventional electronics and the photon energies are too small for classical optics.Development of semiconductor focal plane arrays started in seventies last century and has revolutionized imaging systems in the next decades. This paper presents progress in far-IR and sub-mm-wave semiconductor detector technology of focal plane arrays during the past twenty years. Special attention is given on recent progress in the detector technologies for real-time uncooled THz focal plane arrays such as Schottky barrier arrays, field-effect transistor detectors, and microbolometers. Also cryogenically cooled silicon and germanium extrinsic photoconductor arrays, and semiconductor bolometer arrays are considered.

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Section: Semiconductor Bolometersmentioning

confidence: 99%

Section: Semiconductor Bolometersmentioning

confidence: 99%

Semiconductor detectors and focal plane arrays for far-infrared imaging

Rogalski

2013

Opto-Electronics Review

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“…A 3 He sorption cooler provides a base temperature of 285 mK to the focal plane for the whole duration of a PACS Photometer observation campaign. A more detailed description of the cryo-cooler is given in Billot et al 2006 8 and in Duband et al 2008 12 . Each instrument campaign starts with a cryo-cooler recycling that lasts 3 hours.…”

Section: Cryo-coolermentioning

confidence: 99%

“…The Blue BFP contains 8 16 × 16 bolometer arrays butted together, and the Red BFP contains 2 bolometer arrays. A detailed description of the PACS Photometer can be found in Billot et al 2006 8 . The native sampling frequency of the arrays is 40 Hz, however due to the limited downlink bandwidth of the Herschel spacecraft, the signal has to be processed on-board leading to an effective sampling frequency of 10 Hz.…”

Section: The Pacs Photometer Focal Plane Unitmentioning

confidence: 99%

CEA bolometer arrays: the first year in space

Billot¹,

Sauvage

Rodriguez

et al. 2010

SPIE Proceedings

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The CEA/LETI and CEA/SAp started the development of far-infrared filled bolometer arrays for space applications over a decade ago. The unique design of these detectors makes possible the assembling of large focal planes comprising thousands of bolometers running at 300 mK with very low power dissipation. Ten arrays of 16x16 pixels were thoroughly tested on the ground, and integrated in the Herschel/PACS instrument before launch in May 2009. These detectors have been successfully commissioned and are now operating in their nominal environment at the second Lagrangian point of the Earth-Sun system. In this paper we briefly explain the functioning of CEA bolometer arrays, and we present the properties of the detectors focusing on their noise characteristics, the effect of cosmic rays on the signal, the repeatability of the measurements, and the stability of the system.

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“…They are cooled down to 300 mK to optimise the sensitivity down to the physical limit imposed by the photon background noise. The PACS bolometer arrays have passed all the qualification tests (Billot et al 2006). The newly started ArTéMiS project at CEA Saclay capitalises on this achievement by developing submm (200 -450 µm) bolometer arrays with ∼ 4,000 pixels for ground-based telescopes.…”

mentioning

confidence: 99%

CAMISTIC: THz/submm astronomy at Dome C in Antarctica

et al. 2006

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Submillimetre (submm) astronomy is the prime technique to unveil the birth and early evolution of a broad range of astrophysical objects. It is a relatively new branch of observational astrophysics which focuses on studies of the cold Universe, i.e., objects radiating a significant − if not dominant − fraction of their energy at wavelengths ranging from ∼ 100 µm to ∼ 1 mm. Submm continuum observations are particularly powerful to measure the luminosities, temperatures and masses of cold dust emitting objects. Examples of such objects include star-forming clouds in our Galaxy, prestellar cores and deeply embedded protostars, protoplanetary disks around young stars, as well as nearby starburst galaxies and dust-enshrouded high-redshift galaxies in the early Universe.A major obstacle to carry out submm observations from ground is the atmosphere. Astronomical observations in the submm spectral bands can only be achieved from extremely cold, dry and stable sites (e.g., high altitude plateau, Antarctica) or from space (e.g., the Herschel Space Observatory) to overcome the atmosphere opacity and instability that are mainly due to water vapour absorption and fluctuation in the low atmosphere. Chile currently offers the best accessible (all-year long) sites on Earth, where the precipitable water vapour (PWV) content is often less than 1 mm. Chile hosts the best astronomical facilities such as ESO VLT, APEX and Chajnantor plateau will be the ALMA site.At longer term, and particularly if global warming severely restricts the 200 -350 -450 µm windows on ESO sites, Antarctica conditions with less than 0.2 mm PWV, could offer an exciting alternative for THz/submm astronomy (Fig. 1). This is an attractive opportunity for the 200 µm windows, especially, which are normally explored with space telescopes (e.g., Herschel).Observations of submm continuum emission are usually carried out with bolometer detectors. Recently, two Research Departments at CEA (DSM/DAPNIA/SAp and DRT/LETI/LIR) developped filled bolometer arrays for the PACS submm/far-infrared imager on the Herschel Space Observatory, to be launched by ESA in 2007. The R&D was based on a unique and innovating technology that combines all silicon technology (resistive thermometers, absorbing grids, multiplexing) and monolithic fabrication. The bolometers are assembled on a mosaic 'CCD-like' array that provides full sampling of the focal plane with ∼ 2,000 pixels that are arranged in units of 256 pixels. They are cooled down to 300 mK to optimise the sensitivity down to the physical limit imposed by the photon background noise. The PACS bolometer arrays have passed all the qualification tests (Billot et al. 2006). The newly started ArTéMiS project at CEA Saclay capitalises on this achievement by developing submm (200 -450 µm) bolometer arrays with ∼ 4,000 pixels for ground-based telescopes. A prototype camera operating in the 450 µm 709 available at https://www.cambridge.org/core/terms. https://doi

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The Herschel/PACS 2560 bolometers imaging camera

Cited by 18 publications

References 4 publications

Semiconductor detectors and focal plane arrays for far-infrared imaging

Semiconductor detectors and focal plane arrays for far-infrared imaging

CEA bolometer arrays: the first year in space

CAMISTIC: THz/submm astronomy at Dome C in Antarctica

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