S-Cam 3: Optical astronomy with a STJ-based imaging spectrophotometer

Verhoeve, P.; Martin, D.; Hijmering, R. A.; Verveer, J.; Dordrecht, A. van; Sirbi, G.; Oosterbroek, T.; Peacock, A.

doi:10.1016/j.nima.2005.12.198

Cited by 20 publications

(14 citation statements)

References 8 publications

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“…MKIDs use frequency domain multiplexing [15] that allows thousands of pixels to be read out over a single microwave cable. While the largest STJ array is 120 pixels [16] and the largest optical TES array is 36 pixels [10], the MKID arrays described below are 1024 pixels, with a clear path to Megapixel arrays. The ability to easily reach large formats is the primary advantage of MKID arrays.…”

Section: Introductionmentioning

confidence: 99%

A superconducting focal plane array for ultraviolet, optical, and near-infrared astrophysics

Mazin¹,

Bumble²,

Meeker³

et al. 2012

Opt. Express

142

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Abstract:Microwave Kinetic Inductance Detectors, or MKIDs, have proven to be a powerful cryogenic detector technology due to their sensitivity and the ease with which they can be multiplexed into large arrays. A MKID is an energy sensor based on a photon-variable superconducting inductance in a lithographed microresonator, and is capable of functioning as a photon detector across the electromagnetic spectrum as well as a particle detector. Here we describe the first successful effort to create a photon-counting, energy-resolving ultraviolet, optical, and near infrared MKID focal plane array. These new Optical Lumped Element (OLE) MKID arrays have significant advantages over semiconductor detectors like charge coupled devices (CCDs). They can count individual photons with essentially no false counts and determine the energy and arrival time of every photon with good quantum efficiency. Their physical pixel size and maximum count rate is well matched with large telescopes. These capabilities enable powerful new astrophysical instruments usable from the ground and space. MKIDs could eventually supplant semiconductor detectors for most astronomical instrumentation, and will be useful for other disciplines such as quantum optics and biological imaging.

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Section: Introductionmentioning

confidence: 99%

A superconducting focal plane array for ultraviolet, optical, and near-infrared astrophysics

Mazin¹,

Bumble²,

Meeker³

et al. 2012

Opt. Express

142

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“…with homogeneous boundary conditions of third kind: for x = 0 and x = a Du x (a, y, t) = − β 1 u(a, y, t) , Du x (0, y, t) = β 1 u(0, y, t) (2) for y = 0 and y = b…”

Section: Statement Of the Problemmentioning

confidence: 99%

“…In our model, quasiparticles reaching the boundaries x = 0 and x = a leave the strip and enter the trap, where they tunnel producing detector signals Q l and Q r . The capture efficiency of quasiparticles in the trap is determined by the coefficient β 1 and the boundary conditions (2). The signal at the left endpoint of the strip is calculated from the formula…”

Section: Statement Of the Problemmentioning

confidence: 99%

“…For X rays the energy resolution of STJ-detectors is more than an order of magnitude higher than the resolution of traditional semiconductor detectors [1]. In the optical spectrum STJ-detectors are capable of registering single light quanta [2]. However, a whole range of physical processes negatively affect the detector characteristics and primarily the energy resolution [3].…”

Section: Introductionmentioning

confidence: 99%

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Two-dimensional model of a strip detector with two tunnel junctions

Gorkov

Andrianov

2012

Comput Math Model

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The article describes a two-dimensional model of a strip X-ray detector with a superconducting absorbing strip and two tunnel junctions at its ends, The motion of nonequilibrium current carriers (quasiparticles) is considered in the framework of a diffusion equation with boundary conditions of third kind. The detector signals Q l and Q r and the spectral line shape are computed as a function of the strip size, quasiparticle capture efficiency in the tunnel junction, the quasiparticle loss parameter on the absorber lateral boundaries, and the quasiparticle recombination parameter R . Analytical solutions for the detector signals Q l and Q r are derived for the case R = 0 . Numerical calculations are generally used. When boundary and recombination losses are allowed for, the detector signals turn out to depend on the photon absorption coordinate in the transverse direction. This broadens and distorts the spectral line shape.

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“…While both of these technologies produced functional detectors, they have had difficulties with large array size due to the challenge of wiring and multiplexing large numbers of detectors. Currently the largest STJ array is 120 pixels 6 and the largest optical TES array is 36 pixels 5 , although recently there have been proposals for larger TES multiplexers 7 .…”

Section: Introductionmentioning

confidence: 99%

Optical lumped element microwave kinetic inductance detectors

Marsden

Mazin

Bumble

et al. 2012

High Energy, Optical, and Infrared Detectors for Astronomy V

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Microwave Kinetic Inductance Detectors, or MKIDs, have proven to be a powerful cryogenic detector technology due to their sensitivity and the ease with which they can be multiplexed into large arrays. An MKID is an energy sensor based on a photon-variable superconducting inductance in a lithographed microresonator. It is capable of functioning as both a photon detector across the electromagnetic spectrum and a particle detector. We have recently demonstrated the world's first photon-counting, energy-resolving, ultraviolet, optical, and near infrared MKID focal plane array in the ARCONS camera at the Palomar 200" telescope. Optical Lumped Element (OLE) MKID arrays have significant advantages over semiconductor detectors such as charge coupled devices (CCDs). They can count individual photons with essentially no false counts and determine the energy (to a few percent) and arrival time (to ≈ 1µs) of every photon, with good quantum efficiency. Initial devices were degraded by substrate events from photons passing through the Titanium Nitride (TiN) material of the resonator and being absorbed in the substrate. Recent work has eliminated this issue, with a solution found to be increasing the thickness of the TiN resonator from 20 to 60 nm.

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S-Cam 3: Optical astronomy with a STJ-based imaging spectrophotometer

Cited by 20 publications

References 8 publications

A superconducting focal plane array for ultraviolet, optical, and near-infrared astrophysics

A superconducting focal plane array for ultraviolet, optical, and near-infrared astrophysics

Two-dimensional model of a strip detector with two tunnel junctions

Optical lumped element microwave kinetic inductance detectors

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