Hypothesis Testing Mathematical Computations Numerical Computations Fur ther Reading Hypothesis Testing David A. van Dyk1 1 Depar tment of Statistics University of California, Irvine 2008 HEAD Meetings David A. van Dyk Statistics : Handle with Care Hypothesis Testing Mathematical Computations Numerical Computations Fur ther Reading Outline 1 Hypothesis ... H0 : No emission line. ... The test statistic must behavior differently under the alternative hypothesis. ...

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• The AstroStat Slog MCMC
• The AstroStat Slog Skilling
• The AstroStat Slog Blog Archive tests of fit for the Poisson distribution

... We demonstrate through numerical simulations that model parameters estimated with our technique are essentially bias-free, even when the average number of counts per bin is 1. ... The IW technique avoids such biases by estimating through successive iterations, where for each iteration, j, , and the best-fit parameters are determined by minimization of . ... In our sample, we find that the minimum values and best-fit parameters converge after about 6 iterations. ...

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• Recent Advances in Parameter Estimation in Astronomy with Poisson-Distributed
• Modern CCD Observations of Moving Celestial Objects: Algorithms and Software
• Heuristic Estimates of Weighted Binomial Statistics for Use in Detecting Rare

Next: Star Formation Rate and Up: No Title Previous: Calculation of Evolutionary Tracks . To start calculations, we choose the distributions of the initial binary parameters: the mass of the primary ZAMS component, , binary mass ratio, , orbital separation a . ... whereas the mass ratio distribution is not. ... The zero assumption often made is that the mass ratio distribution has a flat shape, that is binaries with a high mass ratio occur as frequently as those with equal masses. ...

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• Initial binary parameters
• Restrictions on the Scenario Parameters
• Dependence on the Scenario Parameters and Initial Distributions

Next: Reducing 12-mm ATCA observations Up: Combining Mosaics and Single Previous: The Non-Linear Method - . Here we describe two ad hoc methods of combining single-dish and mosaic images. ... where and are the beam volumes of the synthesised mosaic beam and the single-dish beam respectively). ... If both the interferometer primary beam and the single-dish beam are gaussian forms with widths and respectively, then you will want to add a gaussian to the mosaic beam dataset which has a width . ...

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• An alternative approach to calibration
• Alternative treatment of DSA with synchrotron losses
• Cosmological Parameter Survey Using the Gravitational Lensing Method

... The parameter pgdev allows the user to specify a pgplot device, but, in contrast to the pgplot standard, the file name should not be included, but instead supplied via the parameter plotfile . ... To write a colour postscript file called op.ps: pgdev=/cps plotfile=op.ps . However note that at present, if a colour postscript device ( pgdev = `/cps'), a fits file ( pgdev = `/fits') or a ppm file ( pgdev = `/ppm') are selected, the task in fact bypasses pgplot and writes the postscript file directly. ...

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• XSPEC session thread
• Description

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• Comparative Review of Alternative Energies
• Physics 162: Alternative Energy; Spring 1998
• Overview of Alternative Energy

Next: Analysis in the Up: MIDAS utilities for Previous: Fourier analysis . For the detection of smooth signals, e.g. sinusoids, use either SCARGLE/TSA or AOV/TSA with bins. ... SCARGLE/TSA -- . Scargle sine model: This command computes Scargle's (1982) periodogram for unevenly spaced observations x . ... In this way, the command can be used to perform a CLEAN-like analysis manually by removing individual oscillations one by one in the time domain (see Roberts et al. ... AOV/TSA -- . ...

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• Signal detection
• The main observational parameters
• Corrections to the probability distribution

The beam pattern and the polarization characteristics . of the radio telescope RATAN-600 . The Mueller matrix elements was computed via formulas [1]: . ... The BP were computed by the aperture method, proceeding from the fild distribution in the aperture of the primary mirror. The components of the main and cross-polarization components of the electric field in the vertical aperture of the primary mirror was computed in Frenel diffraction approximation. ...

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• Determination of atmospheric parameters and calculation of chemical composition
• Spectral energy distribution
• The peculiar post-AGB supergiant IRAS04296+3429: optical spectroscopy and its

... AMPLE (Adaptable Minor Planet Ephemerides) is integrated software package to deal with a number of problems concerning minor planets with the aid of IBM-type personal computer. ... compiling a list of all numbered minor planets which can be seen at certain moment within specified sky region and visualization of their mutual positions; . ... As AMPLE is able to reproduce virtually any table of "the Ephemerides of Minor Planets" , it may be considered as computer version of the EMP. ...

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• (Untitled)

The problem of solar wind data correlation for the observations onboard several spacecraft is very important for three points of view: . ... This problem is studied now in detail by systematic determination of ion flux and ion velocity data correlations by INTERBALL-1 (IKI group), WIND and IMP 8 (both - MIT group). ... Solar wind plasma correlation lengths from IMP 8, WIND and INTERBALL-1. ... Correlation of solar wind observations onboard several spacecraft: INTERBALL-1, IMP 8 and WIND data. ...

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Next: Prior Models Up: Prior Models and the Previous: Bayesian Paradigm . The observed image differs from the true brightness distribution in having been blurred and encountering statistical noise in the recording process. ... Let us describe the noise models. ... This model can be approximated, at least for high brightness values, by the Gaussian distribution . ... The noise model we will use in this paper is Poissonian; see Molina and Ripley (1989) for the use of robust Gaussian noise models. ...

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• Figure of Merit
• Model Fitting
• Image and Spectrum Recovery

Some peculiarities of orbits of observed comets. ... Icarus, 2005 Simulation and reality Distribution of anti-perihelia of short-period comets with e 0.9 ( ecliptic coordinates ) Distribution of anti-perihelia of short-period comets with e 0.9 ( ecliptic coordinates ) Distribution of anti-perihelia of long-period comets with 0.9 e 1 ( ecliptic coordinates ) ­ ...

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• Pulkovo NEO Page: Ephemeris Support

... Fitting the observed dependence includes calculations of the polarization cross-sections averaged over particles orientation and size distribution, their normalization and the comparison of obtained dependencies with Serkowski's curve representing observational data for a chosen star. ... Variations of the polarization factors with wavelength are shown in Fig. 16 for homogeneous spheroidal particles with PF orientation. ... The distinction between prolate and oblate spheroids is also clearly seen. ...

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The radial distribution of metallicity of star-forming galaxies in a galaxy cluster can inform us about the mass assembly and enrichment history of the galaxy cluster. ... Both galaxy clusters are cool-core clusters at redshift z т?? ... The gas-phase metallicity of star- forming galaxies in MACS1115+01 exhibit anti-correlation with projected distance т??0.15 ТБ 0.08 dex/Mpc, whereas the radial metallicity distribution of RXJ1532+30 is statistically flat (т??0.09 ТБ 0.12 dex/Mpc). ...

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• COALA - Computational Astrophysics Laboratory
• The SMS Survey
• Other Infrared Instruments.

Next: The Evolution of Stars Up: NICMOS Science Previous: A Coronagraphic Search for . ... The NICMOS Parallel program . ... The Stellar Population . ... NICMOS Camera 3 is being used in parallel mode to observe galactic fields at both high and low galactic latitudes. ... Most of the fields are at high galactic latitude; as Figure 1 shows, only 8 pointings are within |b| = 10 o , i.e. the galactic disk. Figure 1: NICMOS parallel fields distribution in galactic latitude. ... Figure 6 ). ...

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• ASNCOMBINE (Nov98) --- nictools --- ASNCOMBINE (Nov98)

Before calibrating the visibility data, we need to plot it and flag the blue channels 21 to 32 because of their low signal-to-noise ratio. Select VisSq, the uncalibrated raw (squared) visibility amplitude, and plot it versus channel. ... The data selection defines which data is to be used to compute the correlation parameters, with the exception that if the Option|Loop parameter is selected in the calibration widget, the channels are calibrated independently, doing every selected channel. ...

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• OYSTER Lab
• KMOS Exposure Time Calculator
• SINFONI Exposure Time Calculator

... The <B> element specifies that the enclosed text should be displayed in a boldface. ... The <I> element specifies that the enclosed text should be displayed, if practical, in an italic font (or slanted). ... The <SMALL> element specifies that the enclosed text should be displayed, if practical, using a small font (compared with normal text). ... The <SUB> element specifies that the enclosed text should be displayed as a subscript, and if practical, using a smaller font (compared with normal text). ...

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N. Zhukavets Faculty of Electrical Engineering, Czech Technical University in Prague Prague, Czech Republic natalia@math.feld.cvut.cz Free Malcev and alternative sup eralgebras on one o dd generator (Joint work with I.Shestakov.) ... 5] I. Shestakov, N. Zhukavets: The Malcev Poisson superalgebra of the free Malcev superalgebra on one odd generator, J. Algebra and its Applications, 5(4) (2006), 521­535. ... 7] I. Shestakov, N. Zhukavets: The free alternative superalgebra on one odd generator, Internat. ...

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• Alternative transport (in Russian)

... The distribution of galactic RCB stars is controversial. Several authors have argued that they belong to a thick galactic disk, and are thus old Population I stars. ... However, their distribution and space velocities suggest they may alternatively belong to the even older galactic bulge (Population II, [ Drilling 1986 ]). ... These are the only RCB stars for which a distance is known and hence for which an absolute magnitude can be deduced. ...

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• ffit help file
• Irregular Satellite Research
• Refereed Journal Publications 2004

... One of the most widely used tools of Fourier analysis is the Parseval theorem. It enables the experimentalist to view how the `energy' in the signal is distributed among frequencies. The Fast Fourier Transform (FFT) algorithms have made power spectra one of the obvious diagnostics tools during data acquisition, and energy maps are a versatile alternative. ... The result is an energy map (Fig. 9), showing the distribution of energy corresponding to the wavelet map (Fig. ...

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• Conformance: requirements and recommendations
• XFree86/OS2 Available Ported Software
• Historical Notes