... As a result of BTA observations of 23 chemically peculiar stars with strong magnetic fields, it was found that in 22 of them the longitudinal magnetic field, measured from the hydrogen line cores are considerably lower (by about 1/3) than the value measured from metal lines in the same spectra. ... New approaches need to be developed in order to interpret the data. ... The Zeeman spectrum of a star with a strong magnetic field, 53 Cam. ...

This lesson introduces you to the different types of uncertainty, and how you can estimate them from the scatter in your measurements, or from knowledge of your experimental set-up. It also outlines how to quote uncertainties. Back Main Uncertainties Page .

ATM Forum Message . Forums: . ... Post . ... Measuring Resolution . ... Post Message | ... Posted by Amanda on April 20, 2007 22:08:30 UTC . ... resolution - rick_crockett - April 25, 2007 - 08:46 UTC . resolution - aschilli - April 30, 2007 - 00:08 UTC . Indoor resolution - rick_crockett - June 2, 2007 - 07:04 UTC . ... www.astronomy.net . ... Forum posts are Copyright their authors as specified in the heading above the post. "dbHTML," "AstroGuide," "ASTRONOMY.NET" & "VA.NET" . ...

The HyperNews Linux KHG Discussion Pages . ... Keywords: scheduler overhead . ... From: Jasleen Kaur < jks@cs.utexas.edu > . Hi, I am implementing a different scheduling policy in the scheduler of Linux 2.0.0. I need to measure the time taken for choosing the next task to be scheduled, i.e., the actual time spent in the schedule() function, without the actual context switch having taken place. Since I clear interrupts in schedule(), how do I measure the time? ... Thanks, Jasleen Kaur . ...

. Comedi Documentation . Prev . Next . comedi_sv_measure -- slowly-varying inputs . #include <comedilib.h> . int comedi_sv_measure (comedi_sv_t * sv, double * data); . The function comedi_sv_measure() uses the slowly varying Comedi structure sv to measure a slowly varying signal. If sucessful, the result (in physical units) is stored in the location pointed to by data, and the number of samples is returned. On error, -1 is returned. Prev . Home . Next . comedi_sv_update . Up . comedi_get_cmd_src_mask

. Overview . Package . Class . Use . Tree . Deprecated . Index . Help . PREV NEXT . FRAMES NO FRAMES All Classes . Package Hierarchies: . All Packages . java.lang.Object . ij.measure. Calibration (implements java.lang.Cloneable) . ij.measure. CurveFitter . ij.measure. ResultsTable (implements java.lang.Cloneable) . ij.measure. SplineFitter . ij.measure. Measurements . Overview . Package . Class . Use . Tree . Deprecated . Index . Help . PREV NEXT . FRAMES NO FRAMES All Classes .

... Previous: Background Fluctuation Analysis from the Multiscale Entropy . ... A new measure of information is defined which is based on noise modeling and incorporates resolution scale. Properties of this measure are discussed. ... Additionally it allows for image noise modeling, and subsequent noise removal. ... Hence information- and entropy-based processing technologies will be necessary for the effective design and implementation of large, future generation, image databases. ...

This page provides explanatory text for the dials shown on the Rice Current Solar Wind Conditions and Current Solar Wind Conditions (Dials Only) webpage. These dials use the last good received set of measurements from the Real Time Solar Wind package on the Advanced Composition Explorer (ACE) spacecraft. ... Measured) This quantity is the number of solar wind protons per unit volume as measured by the ACE Solar Wind Electron Proton Alpha Monitor (SWEPAM) . ... It is measured by ACE/SWEPAM. ...

. I measured my limiting magnitude on this picture at about Mag 18.9. I also did some photometry near for the SN positon, and I found a star liked object at about Mag 17.6. I think this object is 1999br. This image is deconvoluted, but I measured the magnitude pre-deconvulution. Kereszty Zsolt . Hungary, Miskolc . Back to Bright Supernovae . David Bishop Last modified: Thu Apr 15 11:44:03 EDT 1999

... Polarizer efficiency is defined as , where and are the respective measured signals for a polarizer oriented parallel and perpendicular to the axis of a fully polarized beam... angle 12.2 . Polarizer position angle as measured from the NICMOS Aperture Offset Angle of , about the aperture center toward the +U3 axis.. IDL 14.1 . IDL (Interactive Data Language) is an interactive analysis and visualization program written by Research Systems, Inc.... resolution. ...

ON-LINE STATIC EIT RECONSTRUCTION SERVER . ... Static image reconstruction from the data measured in vivo is still intriguing problem in EIT. ... dipole (adjacent) current injection and voltage measurements on pairs of adjacent electrodes (like in Sheffield systems) . ... You can view examples of the text files for polar , dipole and trigonometric injection, use them for testing the server and find more details on HOW TO PREPARE INPUT FILE FOR THE ON-LINE EIT RECONSTRUCTION SERVER page. ...

... Parameter Spec Measurement Technique: Wavelength = 355nm (Visual confirmation) Energy = 30 uJ, 160-180 mJ (4025 pulses), 40 uJ (micropulse) Pulse Duration = 10 ms (Measured at 10 ms on an oscilloscope) Micropulse Width = 70ps IR, = 50 ps UV (Autocorrelator to measure IR pulse waveform Temporal Profile - flat envelope) Measured at 10 ms on an oscilloscope. ... Burn Paper measurement) Repetition Rate = 10 Hz/402.5 MHz Oscilloscope Shot to Shot Stability = 3% RMS for pulse envelope. ...

The wave complex KEM-3 is designed to measure the parameters of electromagnetic waves in the VLF and ULF ranges. ... The electric antenna is a 1.6 m long dipole made up by two spherical carbon EDS detectors each with a preamplifier. ... The same detector is also used for the VLF device. ... 1. component Ex: 0.1 Hz - 400 kHz; 5*10E(-8)HzE(-1/2) (2 kHz). 2. component Bx: 1.0 kHz - 50 kHz; 10E(-5) nT*HzE(-1/2) (2 kHz). 3. components Bx,y,z: 1.0 Hz - 2 kHz; 3*10E(-5) nT*HzE(-1/2) (100 Hz). ...

... Observations of GRB afterglows with Russian-Turkish 1.5-m Telescope (RTT150) . ... The afterglow light curve was measured in detail starting from about 5 h after the GRB and over five ensuing nights. In addition, upper limits were obtained on the rapid variability of the afterglow on the first night of observations and the history of afterglow color variations was measured in detail. ... 2007) : . ... Astronomy Letters, 33, 797 (2007) , arXiv:0802.1635 , The original text in Rissian . ...

Sheepdog standing in the rain, Bullfrog doing it again Some think that happinness is measured out in years You don't know what it's like to listen to your fears Child-like No one understands, Jack knife In your sweaty hands, Some think that happiness is measured out in miles What makes you think you're something special when you smile You can talk to me, if you're lonely you can talk to me ...

... 1 Institute of Solid State Physics, Russian Academy of Sciences, Chernogolovka, Moscow oblast, 142432 Russia . 2 Laboratoire de Physique de la Mati re Condens e, Ecole Normale Sup rieure, 75231 Paris, France . ... The c -axis penetration depth c in Bi 2 Sr 2 CaCu 2 O 8 + (BSCCO) single crystals as a function of temperature has been determined using two techniques, namely, measurements of the ac -susceptibility at a frequency of 100 kHz and the surface impedance at 9.4 GHz. ...

We have designed the laboratory model of static Fourier spectrometer for onboard usage for spectral study of atmosphere and ionosphere. The gain of model is to simulate onboard FS which will not have any moving elements (all its optical elements will be mounted at fused quartz monolithic construction), to compare experimental results with theoretical estimations and to measure MTF of CCD array. ... This fact connected with low frequency response of CCD array due to small format of it. ...

... Total expanded uncertainty at E = 8.35 eV is ? ... 0.21 7.54 -0.14 ? ...

The deflection of light induced by the Sun gravity field and measured with geodetic VLBI (1) Titov O., (2)Girdiuk A. (1) Geoscience Australia, Australia; (2) Institute of Applied Astronomy RAS, Russia The Sun's gravitational field deflects positions of close objects in accordance with the formulae of general relativity. ... The geodetic VLBI technique is capable to measure the deflection of the light from distant radio sources anytime and around the whole sky. ...

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