Weaving together Astronomy+Statistics+Computer Science+Engineering+Intrumentation, far beyond the growing borders . ... Posts tagged ?Frequentist? ... Continue reading ?[ ... Tags: Bayesian , Frequentist , Ping Zhao , question for statisticians , weighted mean . Category: Bad AstroStat , Fitting , Frequentist , Stat , Uncertainty | 18 Comments . ... Category: arXiv , Quotes | Comment . ... Category: arXiv | ... Category: Bayesian , Fitting , Frequentist , Jargon , Stat , Uncertainty | ...

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• The AstroStat Slog Ping Zhao
• The AstroStat Slog weighted mean
• The AstroStat Slog Fisher information

... Avg: the average value of the spectra (maybe throwing out some channels at the edges). <>:average over the spectra (throwing out points at the edges if you want). gCal(f) :- frequency dependence of the tabulated cal values. ... calInK(Avg): Scaler cal value averaged over the band. calOffSpc(Avg): cal off value averaged over the band (in spectrometer counts) . ... cntsToK(avg) = calInK(Avg) / (calDif_cnts(Avg)) . To convert a spectrum b_cnts in spectrometer counts to b_K in Kelvins using cntsToK: . ...

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• gps L3 nov13
• a2186
• pdev_birdies_25jun07

Time Standard and Ensemble Pulsar Time Scale Ding Chen, George & Dick, Bill 20100928, Orange National Time Service Center. ... Ensemble Pulsar Time Scale(EPT) : (TAI - EPT ) = k = ( 2 k k =1 N ^ k (TAI - PTk ) + 2 z ,k ( T )) -2 PPTA is the best project to establish the new independent ensemble time scale which will take contribution to both GW detection and BIPM. ... Ensemble Pulsar Time Scale is more stable than the AT of some clock laboratory on long term scale. ...

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• cflag (Flagging Utility) CentralProcessor 0.11 documentation
• difx:verification:bd148a [ATNF VLBI Wiki]
• Image Statistics and Histograms

ACS Insturment Handbook for Cycle 24 . ... Advanced Camera for Surveys Instrument Handbook for Cycle 24 > Chapter 9: Exposure-Time Calculations > 9.3 Computing Exposure Times . ... The detector background ( B det ) or dark count in units of counts/second/pixel and the read noise ( R) in counts of the CCD. ... As a consequence, in order to obtain correct estimated count rates for red targets, observers are advised to use the synphot package in IRAF /STSDAS (or Pyraf), or the pysynphot package in Pyraf. ...

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• Space Telescope Imaging Spectrograph Instrument Handbook
• ACS Instrument Handbook for Cycle 20
• Roelof's Citation Statistics

A computer controlled low light photometer for nightglow observations. Hardware units of portable photometer for low light measurements, especially night glow emission is described. ... Interface card contain three channels of 24 bit counter, 4 channels of 12 bit ADC and the buffer bus for the controlled motors of the altazimuthal fork mounting and filters wheel, the position encoders. ... Where N( ) is output signal photometer generated input light flux F( l ) . ... PMT # . 599 . ...

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• Second order reduction quantities. Explanations for Computer Ephemeris.
• Ephemeris of Saturnian rings. Explanations for Computer Ephemeris (DE200...
• Lunar equatorial positions. Explanations for Computer Ephemeris.

... The question which method of the detection of features in the test statistic is the most sensitive, is of considerable importance for all practical TSA applications. ... A power of the test statistic is the probability that is accepted for the given Y : . ... Then, all statistics based on models with 3 parameters have similar values of the test power: power spectrum, Scargle statistics, fit of a sinusoid, AOV(3) statistic and PDM(3) statistic with corrected probability distribution. ...

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• Time series analysis in the frequency domain
• Corrections to the probability distribution
• Averaging and Merging Frames

... Chapter 14. ... Data consist of numbers, of course. ... In the following sections, you will repeatedly encounter the following paradigm: § apply some formula to the data to compute a statistic § compute where the value of that statistic falls in a probability distribution that is computed on the basis of some null hypothesis § if it falls in a very unlikely spot, way out on a tail of the distribution , conclude that the null hypothesis is false for your ... 603 604 Chapter 14. ...

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• http://www.arcetri.astro.it/irlab/doc/library/recipes/bookcpdf/c14-0.pdf
• http://www.arcetri.astro.it/irlab/instr/spectralgpu/doc/spegpu_summary.pdf
• Saturn's Moon Titan

... flspec computes the spectrum of the background fluctuations in EPIC Imaging data in different offaxis annular regions. ... Once the 'flatfielded' image is free from detected sources, its pixels are binned according to the input parameter binsize and classified as 'positive' (if they have more counts than the median in the image) and 'negative' pixels (less counts than the median). ... The positive and negative spectra are extracted with an spectral binning of 15 eV (MOS) and 5 eV (PN). ...

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... 2009 July 30 . 6 Minutes 42 Seconds . ... Explanation: The July 22nd total solar eclipse was the longest of the 21st century . From the point of maximum eclipse along the Moon's shadow track across the Pacific Ocean, the Moon completely blocked the Sun for a total of 6 minutes and 39 seconds. But from the deck of this cruise ship the duration of the total eclipse phase was extended to a whopping 6 minutes and 42 seconds by the ship's motion along the shadow track. ... About APOD | ...

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• Monitoring Options
• APOD: 2012 July 23 - Lightning Captured at 7207 Images per Second
• APOD: 2001 January 5 - Second Millennium, Last Eclipse

Next: Imaging by an Optimizing Method . ... A big advantage of this numerical integrator is its stability: the error in the semi-major axis and the eccentricity depends only on the step size and does not grow with an increasing number of time steps. ... As the integration time increases, the numerical results become more contaminated by various errors. ... A new symplectic integrator produces no secular truncation errors in the actions of a Hamiltonian system. ...

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• QuickLook Data Reduction Pipeline - Keck Adaptive Optics Real Time Data
• Heuristic Estimates of Weighted Binomial Statistics for Use in Detecting Rare
• Modelling Spectro-photometric Characteristics of Nonradially Pulsating Stars

The original files with the data were in different formats. ... Such files were named "standard data files" and linked to the database. They can be easily transformed to any desirable format by a code. Here we present two simple computer programs of this kind. ... When running the code, you can specify columns in the output file: wavelength, energy (eV) or wavenumber (cm -1 ) as the first column, and complex refractive index or dielectric function as the second and third columns. ...

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• Vladimir P. Reshetnikov's Home Page
• The Atomic data Guide

... We then updated to PVCam 2.7.4.2, but we still see corrupt images if we don't close and reopen the camera after every exposure sequence, and the camera sometimes fails to respond to a trigger pulse. ... Close and re-init the camera, as follows: ... pl_cam_close(0) pl_pvcam_uninit() pl_pvcam_init() . ... power off camera . ... Call pl_exp_start_cont (to start a continuous exposure sequence into a circular buffer) with a circular buffer that holds too many images and you will hang your computer. ...

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• Astrophysical Research Consortium - Apache Point Observatory

... 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)
• AY (preface)
• AY2006 (preface)

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• Astronomy 123 Spring 1996
• Potential Energy
• The Paperless Class

... The tracking system works in micro-step regime with a computer step of correction = 0.003 arcsec per second of time and a maximum speed of correction up to 4.6 arcsec per second of time. ... The APD module was constructed for performing experiments of receiving of 2 Mbps signals from “ARTEMIS” using the Cassegrain focus of 0.7m telescope. ... GaAs PIN photo diode. ... Laser module with thermoelectric stabilisation of laser diode. ... Electronic module for turbulence compensation system . ...

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• MAO NASU :: Forum Statistics
• Air Optical Communication Systems
• Traffic Analysis for ursa (UARNET)

... The procedure of radiometer signal integration can be considered as a sort of reducing dimension of the initial sampling space, where the samples are the result of analog-to-digital conversion. ... The probability distribution of the signal and spikes is completely known. ... The quality of the considered algorithm could be also illustrated by Figure 2 . ... One could see the considered adaptive algorithm is preferable even by low degree of compression, because all spikes have been depressed. ...

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• From Power Up To Bash Prompt: Lilo
• shmidt_e
• Writing programs that use comedi and comedilib

... Thomson's multiple window method of spectral estimationthomson provides a very good estimate of the power spectrum by measuring the energy contained within a collection of rectangular shaped frequency intervals. ... Often, much of the fine structure of a spectral estimate is due to noise. It should be stressed that while other methods of spectral estimation (such as the Welchoppenheim method) exist, the Thomson method is particularly noteworthy for its precisely defined rectangular frequency bins. ...

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• List of books on Statistics and thermodynamics
• Solar modeling input physics (thermodynamics, opacity, nuclear reactions)
• The pyramidal (multi-resolution) CCT

... Bojan Nikolic web pages (r. 329) . ... Atmospheric Modelling for ALMA . This is a short and simple illustration of how to use (A)ATM to calculate the dispersive path delay introduced by the atmosphere as well as the non-dispersive parts. ... Compute dispersive delay in the atmosphere This program is part of AATM version 0.06 GPL license -- you have the right to the source code. ... Computing dispersive atmospheric delay with AATM . ... Computing atmospheric absorption with AATM . ...

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• Computing dispersive atmospheric delay with AATM
• ALMA Phase Calibration Techniques at the Cavendish Astrophysics Group
• Statistics for astronomy graduate course Bojan Nikolic web pages (r. 329)

asncombine -- Process and combine images in one or two NICMOS associations asncombine association . ... set to yes to include error planes in co-added images error. background . ... This is useful to use different background subtractions for different images. fheader . set to yes in order to multiply the background by the value of keyword "factor" in the image header. ... Set to yes to use quadrants statistics save in the image header from previous runs of asncombine. regquad1 . ...

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• ST-ECF Grism Spectrum Software for NICMOS Grism Data
• The Photometric Performance of the NICMOS Grisms
• The Stellar Population in the NICMOS Parallel Fields

... The greater the distance, the smaller the parallax. ... That triangle has the same proportions as the much larger triangle ABC, and therefore, if the distance B'C to the thumb is 10 times the distance A'B' between the eyes, the distance AC to the far landmark is also 10 times the distance AB. ... The most distant objects our eyes can see are the stars, and they are very far indeed: light which moves at 300,000 kilometers (186,000 miles) per second, would take years, often many years, to reach them. ...

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• Kepler's Second Law
• Jupiter's Moon Adrastea
• Radar aurora [Oulu]