... Posts tagged ?background? ... Probability density functions are another way of summarizing the consequences of assuming a Gaussian error distribution when the true distribution is Poisson. We can compute the posterior probability of the intensity of a source , when some number of counts are observed in a source region, and the background is estimated using counts observed in a different region. ... In both cases a background of 200 counts collected in an area 40x the source area is used. ...

... ATNF Home . About ATNF . ... About ATNF overview . ... Australia Telescope Steering Committee . ... The Hб  I Column Density Distribution Function at z =0: the Connection to Damped Ly Statistics . ... We present a measurement of the Hб  I column density distribution function [ ] at the present epoch for column densities . These high column densities compare to those measured in damped Ly lines seen in absorption against background quasars. ... The Column Density Distribution Function . ...

... For many years, all email related to a given HST observing program has been stored in that program's "history" file on SOGS. ... Nevertheless, we continued to store HST observing program emails in text files. ... Beginning on December 19, 2011, Exchange Public Folders will be used to store all future HST observing program related email. ... One folder per HST observing program . ... Exchange public folders are visible only to Outlook and Outlook Web Application (OWA) and not to other mail clients. ...

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. ...

Next: Generation from Ground Calibration Up: EMOS_REDIST Previous: EMOS_REDIST Contents . The redistribution parameters for the MOS cameras. ... Attributes: . None. Columns: . ... The central CCD of each MOS detector has developed a patch where the energy resolution is worse than the average. ... The energy bounds of PHA channels. ... The energy bounds of the PI channels, used to determine the equivalent energies of spectral channels in the redistribution matrix construction. ...

... 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. ...

... Science Users Information > Libraries > telbib information . ... Observing with ESO Telescopes . ... ESO Annual Reports . ... Statistics derived from the ESO Telescope Bibliography include only papers based on data from telescopes and instruments for which observing time was recommended by the ESO OPC (Observing Programmes Committee). telbib is compiled by scanning the major astronomical journals for scientific papers that contain any of the ESO-defined keywords (e.g., telescope and instrument names...

If the calculated chi-squared statistic exceeds a tabled value for the appropriate number of degrees of freedom, then observed values are significantly different from expected values at the confidence level indicated by p. For one degree of freedom: . p=0.05, 3.84; p=0.025, 5.02; p=0.01, 6.64; p=0.005, 7.88 . For two degrees of freedom: . ... For three degrees of freedom: . ... For four degrees of freedom: . ... For five degrees of freedom: . ...

Magnetic Fields around Radio Galaxies Robert Laing (ESO) Laing et al. ... 2008) Negligible depolarization and 2 rotation Almost all Faraday effects must be due to foreground material How to fit depolarization caused by foreground Faraday rotation Complex polarization Rotation measure Integrate over a beam Observed RM for 0 2 rotation and depolarization Faraday rotation and depolarization 5.5 arcsec FWHM Faraday effects at high resolution FWHM = 1.5 ...