... The fitting package in STSDAS (Space Telescope Science Data Analysis System) relies on two basic techniques (one linear and one non-linear) for fitting functions to data. ... Results show that both methods may generate biased coefficients (at the ~few percent level), and over or under-estimate error bars (at the ~10 percent level), in particular from low signal-to-noise data. ... Function coefficient errors are computed directly from the covariance matrix. ... Abscissa is signal-to-noise. ...

... Tags: biased , breakdown point , chi-square , confidence interval , coverage , delta chi-square , estimator , LAD , mean , median , plug-in , rmse . ... Thanks to L. Lyons? work discussed in [ArXiv] Particle Physics , I found this paper, titled Systematic Errors describing the concept and statistical inference related to systematic errors in the field of particle physics. ... Tags: bias , confidence interval , confidence region , coverage , Errors , Estimation , inference , Model Selection . ...

... Computing the pointing error . ... The platform can be rotated by pulling on the tie downs or redistributing weight on the platform. ... The horn rotates through the same angle as the platform. ... The plots show the computed pointing error for different platform rotation angles (.ps) ( .pdf ): . This shows the pointing error in as you tilt the platform. ... B2209+080 has the pointing errors with no tilt. ... The computed pointing error for a platform tilt track the measured errors pretty well. ...

... Using the central limit theorem, the total noise can be approximated by a Gaussian or normal distribution which has the frequency function : . ... where is the mean intensity of the source. ... In the statistical analysis of the probability distribution of data several estimators based on moments are used. ... For a normal distribution, these moments are and while for a Poisson distribution are and . Besides these moments other estimators are used to describe a distribution e.g. median and mode . ...

... The absolute photometric accuracy of FOC observations depends on several factors. ... The remaining errors most likely arise from: 1) errors in the published fluxes or variations in fluxes of the spectrophotometric stars used to calibrate the absolute DQE, 2) errors in the assumed PSFs, 3) errors in the assumed filter transmission curves, 4) format dependence effects, 5) temporal variability in the FOC detectors, and 6) the spectrum of the source. ... Errors in the assumed filter transmission curves...

... Keyword TIMEDEL missing in Input File . error . The TIMEDEL keyword is missing in the timeseries FITS file, which is necessary to determine the binning factor of the data . ... Hence it is impossible to carry out the variability test. corrective action: Use a different input file . ... The keyword is missing in the input timeseries FITS file which could indicate that there is a problem with the input timeseries FITS file. corrective action: Verify that this is a valid fits file . ...

... Calculations of at least two runs with different values of a parameter are required in order to discover to what extent the results depend on the , if at all. ... In order to study how the final statistical distributions depend on the initial functions, the method of Green functions is used. ... Then we can restore any distribution on this parameter (with a certain accuracy) by summing the results for each interval with the appropriate weight. ...

... Bojan Nikolic web pages (r. 329) . ... This page describes the software and some pointers for using beam cuts through the Moon or Sun for determining the approximate correlation length-scales of errors of a telescope surface. ... At the moment the software can generate a synthetic beam shape at any frequency with a surface errors which are a sum of distributions with Gaussian-spectrum fluctuations. ... Analysis of surface error distributions through Moon (or Sun) beam cuts . ...

... Files in red?history) . ... Trapped Motion . ... 10a. Particle Drift . ... Fast Particles . ... The fact charged particles circle around field lines was well known to J.J. Thomson when he experimented with electron and ion beams in a magnetic field. ... The notion of adiabatic invariance is tied with the early years of quantum theory. ... By about1910, physicists realized that these patterns indicated changes in the laws of physics as one approached atomic dimensions. ...

Sloan Digital Sky Survey Telescope Technical Note 19970527 Walter Siegmund . ... Pointing Error Budget . ... The interleaved strips and adjacent stripes overlap about 1 arc minute. ... However, a 2-D pointing accuracy of 3 arc seconds RMS leads to acceptibly uniform overlap and minimises the number of cases that require special handling (Table 3). ... A guide fiber bundle diameter of 16.5 arc seconds and a pointing accuracy of 3 arc sec RMS results in 99% initial success in acquiring guide stars. ...

... First, we computed the mean errors of orbit parameters on the assumption of the linear connection of them with observation errors and then we compared obtained estimates with those resulting from the assumption of the nonlinearity of this connection. Secondly, we correlate orbital parameters and their errors obtained by the method of the least modulus with those obtained by the least-squares method. ...

... It is found that the metallisity distribution of disk stars has a gap which subdivide the disk population into two groups. The distribution may be described by the sum of two normal curves which are centered at [Fe/H]=-0.22 and +0.08. The curves can be interpreted as distributions of random errors in metallisity of sample stars. This leads to the conclusion that all stars in each group have actually the same value of [Fe/H]. ... Рассмотрен вопрос о происхождении подсистем Галактики. ...

... St Petersburg 23, September 2014 1 Motivation · Origin of Martian moons? ... Considered error sources: ­ Phobos a priori ephemerides; ­ Phobos a priori GM value; ­ measurements noise; ­ different strategies; · Methods: ­ real data analysis; ­ simulations. ... St Petersburg 23, September 2014 8 Simulations: sensitivity of the measurements to the a priori GM value Simulations: zero noise+ IMCCE a priori ephemerides +GMPH = 7.16 * 105 m3/sec2. ... St Petersburg 23, September 2014 14 Thank you! ...

Karas V.I., Moiseev S.S., Novikov V.E. Nonequilibrium stationary distributions of charged particles in solid state plasma. ... In russian . ... Karas V.I., Moiseev S.S. About conversions of nuclear energy to electric one based on the nonequilibrium particle distributions. ... Altaiskii M.V., Balebanov V.M., Erokhin N.S., Zolnikova N.N., Mikhailovskaya L.A., Moiseev S.S. Analytic approximations for description of charged particles interaction with the emitter of radioisotope source of current. ...

... This appendix describes how to use the JavaScript console to evaluate expressions and display error messages to the user. ... Displaying Error Messages with the Console JavaScript 1.2 and earlier versions. ... You can specify whether to automatically open the console when a JavaScript error occurs or to display a dialog box for each JavaScript error. ... To open a dialog box each time an error occurs, add the following line to prefs.js : user_pref("javascript.classic.error_alerts", true); . ...

For a sample of 16 people, the error would be 4/16 = 25%. This a large error since the range of YES vs NO is from 0-100% if 12 people answered yes and 4 people answered no then your result would be: . Percentage yes = 75 +/- 25% . ... For a sample fo 1000 people, the error would be SQRT(1000)/1000 = 33/1000 = 3%. If 750 answered yes and 250 answered no then your result would be: . ... Conclusion: Always ask what the measuring errors are!! Previous Lecture Next Lecture Course Page ...

Next: Polarization efficiency: size/shape/orientation effects Up: Optical properties of cosmic Previous: The 2175? feature . To model the interstellar polarization one needs to calculate the forward-transmitted radiation for an ensemble of non-spherical aligned dust grains. ... Let non-polarized stellar radiation passes through a dusty cloud with a homogeneous magnetic field. ... The angle between the line of sight and the magnetic field is ( ). ... where the angle is connected with and ( ). ...

... In brief: the frequency-dependent radiative transfer equation is solved for a dust under assumption of spherically-symmetric geometry for its distribution taking into account particle size distribution and quantum heating effects for the very small dust particles. ... Table: Model parameters for IRAS04296+3429. ... parameter . ... hot dust shell) . ... The best fit to the spectral energy distribution of IRAS04296 is shown by heavy solid line (see Table2 for details concerning parameters of the model...

polimplot -- Plot a polarization vector map . ... inpol = "" [name] . Input linear polarization image (in %) to plot. inpopa = "" [name] . Input image for position angle of linear polarization vectors (degrees). poi_err = "" [boolean] . ... Name of corresponding polarization position angle error image (degrees). ... This task is a flexible tool for plotting a polarization vector map from two images of the polarization and the position angle of the polarization vector. ...

polimplot -- Plot a polarization vector map . ... inpol = "" [name] . Input linear polarization image (in %) to plot. inpopa = "" [name] . Input image for position angle of linear polarization vectors (degrees). poi_err = "" [boolean] . ... Name of corresponding polarization position angle error image (degrees). ... This task is a flexible tool for plotting a polarization vector map from two images of the polarization and the position angle of the polarization vector. ...