... Meta Index / Home Page . ... Description . Errors . ... Keyword TIMEDEL missing in Input File . ... Negative background values in Input File . ... Negative count rates in Input File . ... Null or negative Bin Width in Input File . ... CONTENT parameter for input file is .. ... Keyword CONTENT missing in Input File . ... Keyword EXPOSURE missing in Input File . ... Keyword HDUCLASS missing in Input File . ... Keyword TSTART missing in Input . ... Null or negative exposure time in Input File . ...

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• Description

... 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. ...

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• Comments on: chi-square distribution [Eqn] By: Alex By: vlk By: aneta By: aneta
• The AstroStat Slog gaussian
• The AstroStat Slog PDF

... FTP access the basic models is here . ... Below, we put short descriptions of the used SED models for the photometric redshifts providing by the current server . ... The uniqueness of this model consists in expanding to the near IR (NIR) of Rocca-Volmerange and Guiderdoni's (1988) atlas of synthetic spectra with a revised stellar library, which includes parameters of cool stars. ... Homepage of the GISSEL model). ... Another model used earlier is the model of synthetic spectra of Poggianti (1997). ...

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... 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. ...

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• Synthetic Images of the Solar Corona from Octree Representation of 3-D Electron
• ADASS 2003 Conference Proceedings
• A Computer-Based Technique for Automatic Description and Classification of

Next: Simulations Up: Maximum Likelihood Estimation of Previous: Introduction . The properties of an ensemble of faint galaxies can be defined by the distribution of the parameters of the models that best fit each individual object. ... The model also includes instrumental parameters, such as the sky background (estimated locally) and amplitude of the noise. ... The probability of the observed value is then computed for each pixel using the adopted error distribution. ...

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• A New Database of Observed Spectral Energy Distributions of Nearby Starburst
• CSPICE Routines: SETMSG_C
• Rate for NICMOS time conversion in error

Tired light models invoke a gradual energy loss by photons as they travel through the cosmos to produce the redshift-distance law. ... The tired light model can not produce a blackbody spectrum for the Cosmic Microwave Background without some incredible coincidences. ... So the CMB must have come from a far away part of the Universe, and its photons will thus lose energy by the tired light effect. ... Assume that the CMB starts out as a T = (1+z)*T_o = 2.998 K blackbody, which is the blue curve. ...

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• Errors in the Steady State and Quasi-SS Models
• Noise distributions
• Culgoora catalog

Next: The derived luminosity and Up: The galactic population of Previous: The galactic population of . Figure 16: The observed distribution of pulsar dispersion measures. Dotted curve is the total known population, solid curve is the Parkes survey. Figure 17: The observed distribution of pulsar distances above the galactic plane. ... Figure 18: The observed distribution of pulsar flux densities. ...

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• casacore: casa::CountedPtr_global_functions_dereference_error Struct Reference
• casacore: casa::ObsInfo Class Reference
• casacore: casa::MSSelectionKeywords Class Reference

... 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. ...

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• Keywords_120
• Keywords_60

... Bojan Nikolic web pages (r. 329) . Zernike Polynomials . ... Example of an OOF analysis for the GBT . Observed data and analysis . ... Sample data . ... Out-Of-Focus (OOF), or phase-retrieval, holography is a technique to measure the shape of surfaces of radio telescopes (i.e., to do antenna metrology). ... There are two recent papers describing OOF holography; see the publications page . ... The OOF wiki pages . ... My old OOF holography pages at the MRAO. ... Out-Of-Focus (OOF) Holography . ...

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• DUST: boseint.h File Reference
• Astrophysics Group MADCOW
• Simulating Atmospheric Phase Errors, Phase Correction and the Impact on ALMA

... DevHlp_Security This devhlp allows to open a file for read access in the Init routine of a BASEDEV . ... returned: size of file SYIOpenFile ends Valid at INIT time only. ... This routine uses the corresponding function of the miniFSD , not normal file I/O, thus access is restricted. ... Although the size argument of the data structure implies, I'd recommend to better not read more than 32K at a time. ... DL = 044h This function will return the table of security helper functions for file access. ...

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• Bugs found so far in XFree86/OS2 3.2/3.2A
• Appendix B: Changes from CSS1
• Bugs found so far in XFree86/OS2 3.3.5

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. ...

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• MILT Description
• TUI:Telescope:User Catalogs
• Astrophysical Research Consortium - Apache Point Observatory