131 research outputs found
Asset Price Shocks, Financial Constraints, and Investment: Evidence from Japan
10.1086/379866Journal of Business771175-19
Effect of Composition on Optical and Thermoelectric Properties of Microstructured p-type (Bi2Te3)x(Sb2Te3)1 â x Alloys
Semiconducting (Bi2Te3)x(Sb2Te3)1 â x alloys are among the best thermoelectric materials available today near room temperature. This property is largely attributed to compositional variations, resulting in improved figure of merit. Considering this, present study aimed at characterizing the optical and thermoelectric properties of microstructured p-type (Bi2Te3)x(Sb2Te3)1 â x alloys for enhanced thermoelectric efficiency. High performance microstructured p-type (Bi2Te3)x(Sb2Te3)1 â x alloys were prepared by melting technique. The phase, optical band gap, microstructure, carrier type concentration and thermoelectric properties of the prepared alloys were systematically investigated by X-ray diffraction, Fourier transform infrared spectroscopy, scanning electron microscopy, hot probe p-n type tester, four-probe method, Îș-probe method and Seebeck coefficient measurement system. The electrical conductivity and Seebeck coefficient were measured in the temperature range 298-473 K to elucidate the Sb content effect on the thermoelectric properties of the p-type (Bi2Te3)x(Sb2Te3)1 â x alloys. The optical band gap decreased with increasing Sb content. Also, with the increase of Sb content, the electrical conductivity increased substantially, the thermal conductivity increased significantly and the Seebeck coefficient decreased marginally, which lead to a great improvement in the thermoelectric figure of merit. The maximum power factor of 3.2 Ă 10 â 3 Wm â 1K â 2 and figure of merit of 0.72 were obtained at 300 K for the composition of 15 %Bi2Te3-85 %Sb2Te3.
When you are citing the document, use the following link http://essuir.sumdu.edu.ua/handle/123456789/3582
Observations of TeV gamma-rays from Mrk 421 during Dec. 2005 to Apr. 2006 with the TACTIC telescope
The TACTIC -ray telescope has observed Mrk 421 on 66 clear nights
from Dec. 07, 2005 to Apr. 30, 2006, totalling 202 hours of on-source
observations. Here, we report the detection of flaring activity from the source
at 1 TeV energy and the time-averaged differential -ray spectrum
in the energy range 1-11 TeV for the data taken between Dec. 27, 2005 to Feb.
07, 2006 when the source was in a relatively higher state as compared to the
rest of the observation period. Analysis of this data spell, comprising about
97h reveals the presence of a -ray signal with
daily flux of 1 Crab unit on several days. A pure power law spectrum with
exponent as well as a power law spectrum with an exponential
cutoff and are found to provide
reasonable fits to the inferred differential spectrum within statistical
uncertainties. We believe that the TeV light curve presented here, for nearly 5
months of extensive coverage, as well as the spectral information at
-ray energies of 5 TeV provide a useful input for other groups
working in the field of -ray astronomy.Comment: 13pages,4figures; Accepted for publication in Astroparticle Physic
Quantization and Compressive Sensing
Quantization is an essential step in digitizing signals, and, therefore, an
indispensable component of any modern acquisition system. This book chapter
explores the interaction of quantization and compressive sensing and examines
practical quantization strategies for compressive acquisition systems.
Specifically, we first provide a brief overview of quantization and examine
fundamental performance bounds applicable to any quantization approach. Next,
we consider several forms of scalar quantizers, namely uniform, non-uniform,
and 1-bit. We provide performance bounds and fundamental analysis, as well as
practical quantizer designs and reconstruction algorithms that account for
quantization. Furthermore, we provide an overview of Sigma-Delta
() quantization in the compressed sensing context, and also
discuss implementation issues, recovery algorithms and performance bounds. As
we demonstrate, proper accounting for quantization and careful quantizer design
has significant impact in the performance of a compressive acquisition system.Comment: 35 pages, 20 figures, to appear in Springer book "Compressed Sensing
and Its Applications", 201
Open data from the third observing run of LIGO, Virgo, KAGRA, and GEO
The global network of gravitational-wave observatories now includes five detectors, namely LIGO Hanford, LIGO Livingston, Virgo, KAGRA, and GEO 600. These detectors collected data during their third observing run, O3, composed of three phases: O3a starting in 2019 April and lasting six months, O3b starting in 2019 November and lasting five months, and O3GK starting in 2020 April and lasting two weeks. In this paper we describe these data and various other science products that can be freely accessed through the Gravitational Wave Open Science Center at https://gwosc.org. The main data set, consisting of the gravitational-wave strain time series that contains the astrophysical signals, is released together with supporting data useful for their analysis and documentation, tutorials, as well as analysis software packages
Constraints on the cosmic expansion history from GWTCâ3
We use 47 gravitational wave sources from the Third LIGOâVirgoâKamioka Gravitational Wave Detector Gravitational Wave Transient Catalog (GWTCâ3) to estimate the Hubble parameter H(z), including its current value, the Hubble constant H0. Each gravitational wave (GW) signal provides the luminosity distance to the source, and we estimate the corresponding redshift using two methods: the redshifted masses and a galaxy catalog. Using the binary black hole (BBH) redshifted masses, we simultaneously infer the source mass distribution and H(z). The source mass distribution displays a peak around 34 Mâ, followed by a drop-off. Assuming this mass scale does not evolve with the redshift results in a H(z) measurement, yielding (68% credible interval) when combined with the H0 measurement from GW170817 and its electromagnetic counterpart. This represents an improvement of 17% with respect to the H0 estimate from GWTCâ1. The second method associates each GW event with its probable host galaxy in the catalog GLADE+, statistically marginalizing over the redshifts of each event's potential hosts. Assuming a fixed BBH population, we estimate a value of with the galaxy catalog method, an improvement of 42% with respect to our GWTCâ1 result and 20% with respect to recent H0 studies using GWTCâ2 events. However, we show that this result is strongly impacted by assumptions about the BBH source mass distribution; the only event which is not strongly impacted by such assumptions (and is thus informative about H0) is the well-localized event GW190814
- âŠ