A miniature Q-band CMOS LNA with triple-cascode topology

Yeh, Han-Chih; Wang, Huei

doi:10.1109/mwsym.2009.5165787

Cited by 7 publications

(3 citation statements)

References 16 publications

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“…Therefore E+A galaxies have been explained as post-starburst galaxies, that is, a galaxy has experienced starburst recently, but truncated it suddenly. Some works have been performed on this type of galaxies ( Falkenberg et al 2009a, b;Huang & Gu 2009;Pracy et al 2009, and references therein).…”

Section: E+a Galaxiesmentioning

confidence: 99%

Comparing six evolutionary population synthesis models by performing spectral synthesis for galaxies

Chen

Liang

Hammer

et al. 2010

A&A

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Aims. We compare six popularly used evolutionary population synthesis (EPS) models by fitting the full optical spectra of six representative types of galaxies (star-forming and composite galaxies, Seyfert 2s, LINERs, E+A, and early-type galaxies) taken from the Sloan Digital Sky Survey (SDSS). We explore the dependence of stellar population synthesis results on the main ingredients of the EPS models and study whether there is an age sequence among these types of galaxies. Methods. We use the simple stellar populations (SSPs) of each EPS model and the software STARLIGHT to perform our fits. Firstly, we explore the dependence of stellar population synthesis on EPS models by fixing the age, metallicity, and initial mass function (IMF) to construct a standard SSP group. We then use the standard SSP group of each EPS model (BC03, CB07, Ma05, GALEV, GRASIL, and Vazdekis/Miles) to fit the spectra of star-forming and E+A galaxies. Secondly, we fix the IMF and alter the age and metallicity to construct eight additional SSP groups. We then use these SSP groups to fit the spectra of star-forming and E+A galaxies to verify the effects of age and metallicity on stellar populations. Finally, we study the effect of stellar evolution tracks and stellar spectral libraries on our results, and present a possible age sequence among these types of galaxies. Results. Using different EPS models, the numerical values of contributing light fractions obviously change, even though the dominant populations are unaltered. The stellar population synthesis does depend on the selection of age and metallicity, but does not depend significantly on the stellar evolution track. The importance of young populations decreases from star-forming, composite, Seyfert 2, LINER, to early-type galaxies, and the properties of E+A galaxies are between composite galaxies and Seyfert 2s in most cases. Conclusions. Different EPS models infer different stellar population parameters, so that it is not reasonable to directly compare stellar populations estimated from different EPS models. To obtain reliable results, we should use the same EPS model to derive the parameter values that we compare.

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Section: E+a Galaxiesmentioning

confidence: 99%

Comparing six evolutionary population synthesis models by performing spectral synthesis for galaxies

Chen

Liang

Hammer

et al. 2010

A&A

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“…Cascode configuration amplifiers feature high gain and good reverse isolation performances due to the combination of common source and common gate (CG) stages. [5, 6]. The proposed cascode configuration with two inductors, or L G and L S at the CG stage is shown in Figure 1.…”

Section: Circuit Design and Fabricationmentioning

confidence: 99%

“…Previous works related to CMOS LNAs utilize cascode‐based topology for high gain or low noise consideration at multi‐giga hertz [1–5]. These LNAs with cascode [1, 2], folded‐cascode [3], or triple‐cascode topology [5] achieve acceptable gain performances with low power consumptions. Moreover, the LNA using the parallel‐resonant technique achieve a minimum noise figure (NF) at X‐band [4].…”

Section: Introductionmentioning

confidence: 99%

Design of a 9 GHz CMOS low noise amplifier using gain‐enhanced technique

Wang

2011

Micro & Optical Tech Letters

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In this article, a 9 GHz low noise amplifier (LNA) using gain-enhanced technique is presented. The compact and high-gain LNA with cascode topology is implemented in a standard 0.18-lm CMOS process. The gain-enhanced technique consists of two inductors in the common gate (CG) stage of the cascode configuration. The first inductor at the source terminal in the CG stage eliminates the parasitic effects caused by the parasitic capacitances of transistors at high frequencies. Moreover, the second inductor at the gate terminal in the CG stage achieves a negative resistance making a high gain characteristic of the amplifier. Finally, the measured small signal gain, noise figure and input P 1dB at 9 GHz are 16.5 dB, 4.5 dB, and À15 dBm, respectively. The chip size of the compact LNA is 0.48 mm Â 0.8 mm including all testing pads.

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