The first CMOS LNA on a radio telescope

Belostotski, Leonid; Haslett, J.W.; Veidt, B.; Landecker, T. L.; Gray, A. D.; Hovey, Gary; Sheehan, Ev; Messing, Rob

doi:10.1109/antem.2014.6887719

Cited by 9 publications

(4 citation statements)

References 11 publications

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“…The theoretical and experimental work on dielectric rod antennas was conducted by many researchers, some earlier works were reported in [3][4][5]. Later, Hamid [6] and Yaghjian [7] experimentally studied the performance of short dielectric rods, fed by a waveguide.…”

Section: Introductionmentioning

confidence: 99%

“…As signals received by a radio telescope are adjusted in its receivers to an optimum level for digitization by an analog‐to‐digital converter (ADC) , the PD is used to preserve the power level of the incoming signal for subsequent data processing. Ahead of the PD, an ultra‐low‐noise amplifier (LNA) followed by additional gain stages is used to amplify low power radio‐frequency input signals, which are dominated by the receiver noise and leakage from ground radiation noise . Due to very stringent requirements for the LNA noise temperature, the LNA inevitably consumes a significant amount of power.…”

Section: Introductionmentioning

confidence: 99%

“…A high‐sensitivity PD can partially relieve the gain requirement for the LNA and gain stages thus reducing the power consumption of those blocks. As described in , depending on the final configuration of the SKA, there may be millions of receivers required. Because of this, receiver power consumption is important as highlighted by an estimate that every additional 0.1 W/receiver will add an additional €1M/year operating cost to the SKA .…”

Section: Introductionmentioning

confidence: 99%

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A broadband self-calibrated RMS power detector embedded in a square kilometre array receiver

Beaulieu

Belostotski

et al. 2015

Microw. Opt. Technol. Lett.

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The black quads in Figure 5 explicit the optimum interval for the referred matrix dimensions. Applying the least square method in these optimum values a linear correlation is obtained. It allows optimum interval predetermination to achieve best computational performance with different size of the matrix dimensions in the interval from 3 3 10 3 to 7 3 10 4 . Scalability AnalysisThe scalability is the runtime simulation performance over the analysis with different matrix dimensions. In this approach, the performance can be expressed by the coefficients in (1). It was chosen the traditional iterative method was chosen with the option of fixed wavelength interval to analyze the scalability.In (1), x is the matrix dimension, a and b are the unknown coefficients. Figure 6 presents the linearization of these results, which make possible to predict the behavior of this method. The results presented in this section were obtained in a computer with Athlon X2 4400, 2GB RAM, with Linux operating system under the Ubuntu distribution, and gfortran compiler for Fortran 90. Figure 6 and Table 6 emphasize the differences in linear coefficients in these two codes, which are counterbalanced by the angular coefficient. These results show that the best performance is achieved when the linear coefficients are decreased. CONCLUSIONSThis work presents a successful computational performance version of the FEM, called fFEM. It integrates preconditioned Bi-CGSTAB and two important approaches to eliminate many ILUT decompositions. These FEM improvements has, consequently, decreased the runtime simulations and improved the numerical scalability performance successfully demonstrated in some computational performance tests of these strategies in fix wavelength intervals and smallest linear coefficients problems.In addition, the best computational performance results were obtained using the iterative method, applying local assembling/ disassembling matrix and with the integration of some strategies to process a ILUT preconditioner, achieving performance improvements up to 70% when compared with the FEM reference runtime. The contribution of this sequential FEM solution provides significant impact when applied to electromagnetic device iterative optimizations, such as the Metaheuristics based. Some of these optimizations have been under study by this work team group. ACKNOWLEDGMENTThe authors wish to thank CAPES and FAPESP, for the partial financial. Key words: power detector; radio frequency integrated circuits; receiver INTRODUCTIONA power detector (PD) circuit is an important building block in the square kilometre array (SKA), the next-generation high-sensitivity radio telescope [1,2]. As signals received by a radio telescope are adjusted in its receivers to an optimum level for digitization by an analog-to-digital converter (ADC) [3], the PD is used to preserve the power level of the incoming signal for subsequent data processing. Ahead of the PD, an ultra-low-noise amplifier (LNA) [4,5] followed by additional gain stages [6] is used to amp...

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Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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A broadband self-calibrated RMS power detector embedded in a square kilometre array receiver

Beaulieu

Belostotski

et al. 2015

Microw. Opt. Technol. Lett.

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“…In some applications, such as the Square Kilometre Array (SKA) radio telescope initiative [1], the bandwidth requirement is more demanding and involves an operating frequency range of an octave or more. Recent research has demonstrated LNAs with noise figures below 0.4 dB from 0.7 GHz to 1.4 GHz using CMOS technology [2][3][4][5]. This paper examines a wideband LNA design that uses off-theshelf Gallium Arsenide (GaAs) transistors.…”

Section: Introductionmentioning

confidence: 99%

Wide-Band Two-Stage Gaas Lna for Radio Astronomy

Kulyk¹,

Ge²,

Belostotski³

et al. 2015

PIER C

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Abstract-This paper presents the design, simulation and measurements of wideband two-stage LNAs using commercially available discrete components and targeting Square Kilometre Array (SKA) focalplane-array verification studies. The design optimization was implemented through simulations based on theoretical work that shows that low wide-band noise figures and power match are achievable by inner-stage component selection and device bias. In contrast to the conventional practice of having each stage of a discrete LNA matched to 50 Ω, the inner stage was designed with a mismatching capacitor between the two stages. The measured results are presented for 0.7-1.4 GHz and achieve noise figures below 0.4 dB, gain of at least 28 dB, mid-band input return loss of 7 dB, output P1 dB of 18.3 dBm, input-referred IP3 of −15.47 dBm, and power consumption of 500 mW with a supply voltage of 5 V.

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Highly Sensitive Broadband SiGe HBT LNA: Genetic Algorithm based Optimization and Design Methodology

Bimana

Sinha

2022

2022 IEEE 41st International Conference on Electronics and Nanotechnology (ELNANO)

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The first CMOS LNA on a radio telescope

Cited by 9 publications

References 11 publications

A broadband self-calibrated RMS power detector embedded in a square kilometre array receiver

A broadband self-calibrated RMS power detector embedded in a square kilometre array receiver

Wide-Band Two-Stage Gaas Lna for Radio Astronomy

Highly Sensitive Broadband SiGe HBT LNA: Genetic Algorithm based Optimization and Design Methodology

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