... The ewavelet tasks detects sources using wavelet transforms. ... Figure: Solid line: The mexican hat wavelet function. Dashed line: a gaussian function with the same parameter . ... Since the image is convolved with the MH function the MH acts like a sort of sliding cell: the positive part being the source cell and the negative part being background area. From this it is clear that the wavelet scale should be smaller than the image itself in order to get a well defined image convolution. ...

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This diagram illustrates a floating image that overlaps the borders of two paragraphs in normal flow: the paragraph borders are clipped by the non-transparent parts of the image. ... A left-floating image causes the final three lines of the upper paragraph to float along its right side. It causes the first three lines of the following paragraph to do the same, and the remainder of that paragraph flows normally. The paragraph borders shine through the margin area of the image box. ...

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• Long description for normal flow example
• Long description for relative flow example
• Property index

... casa::Normal . ... Normal ( RNG *gen, Double mean=0.0, Double variance=1.0) . Construct a random number generator for a normal distribution. virtual . ... Returns a value from the normal distribution. virtual Double . ... These function allow you to manipulate the parameters (mean & variance) described above through the base class. virtual Vector < Double > . ... The second and third arguments define the parameters for this distribution as described in the synopsis. virtual casa::Normal::~Normal . ...

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• uvplanet
• uvfit
• casacore: casa::LogNormal Class Reference

... Posts tagged ?normal? ... Posted by hlee . ... Category: arXiv , Astro , Cross-Cultural , Frequentist , Methods , News , Quotes , Stat , Uncertainty | ... This paper might be an interest for those: Interval Estimation in Exponential Families by Brown, Cai,and DasGupta ; Statistica Sinica (2003), 13 , pp. ... The authors investigated issues in interval estimation of the mean in the exponential family, such as binomial, Poisson, negative binomial, normal, gamma, and a sixth distribution. ...

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• The AstroStat Slog PDF
• The AstroStat Slog Blog Archive my first AAS. VI. Normalization
• Model Spectra for Spectral-Fitting Program

Compilation of radio continuum . HyperLeda home | Documentation | ... e_mag = 1.08575 (e_Jy/F_Jy) 0: normal measurement; 1: upper limit; 3: uncertain log (F/Mhz) Source characteristics : log (diameter/ arcsec )+4 Source characteristics : log (diameter/ arcsec )+4 0: normal measurement; 1: upper limit; 3: uncertain Source characteristics : Position angle Beam characteristics : log (diameter/ arcsec )+4 Beam characteristics : log (diameter/ arcsec )+4 Beam HyperLeda . ...

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• General Description
• Order Definition
• Other Useful Commands

Next: Main-sequence stars (stage I) Up: Evolutionary Scenarios of Binary Previous: Evolutionary Scenarios of Binary . We begin with a description of normal star evolution. The evolutionary states of normal stars will be written using roman figures (I-IV), whereas those of compact stars will be denoted by capital letters (E, P, A, SA ...) (see Section  4 ). ... a main-sequence (MS) star inside its Roche lobe   (RL); . ... a post-MS star inside its RL; . ... Main-sequence stars (stage I) . ...

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• Why do Radiopulsars not Usually Form Pairs with Normal Stars?
• Star Formation Rate and Normalization of Stellar Populations
• Stellar Winds From Normal Stars

... Detailed_Input plane is a CSPICE plane. ... The CSPICE routines that produce CSPICE planes from data that define a plane are: nvc2pl_c ( Normal vector and constant to plane ) nvp2pl_c ( Normal vector and point to plane ) psv2pl_c ( Point and spanning vectors to plane ) The CSPICE routines that convert CSPICE planes to data that define a plane are: pl2nvc_c ( Plane to normal vector and constant ) pl2nvp_c ( Plane to normal vector and point ) pl2psv_c ( Plane to point and spanning vectors ) . ...

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• CSPICE Routines: PL2NVP_C
• CSPICE Routines: NEARPT_C
• CSPICE Routines: NVC2PL_C

... Using a simple 2-D Gaussian Point Spread Function (PSF) on a constant (flat) sky background, I derive a theoretical photometric and astrometric performance model for analytical and digital PSF-fitting stellar photometry. ... The photometric performance is maximized when either the effective background area or the effective-background-level measurement error is minimized. ... An important, but frequently ignored, noise source is the uncertainty of the measurement of the effective background level ( )...

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• Recreating Einstein Level One Processing Exposure Masks and Background Maps in
• The New JCMT Holographic Surface Mapping System - Implementation
• Starfinder: a Code for Crowded Stellar Fields Analysis

Posit ion switched data can be converted from spectrometer counts to kelvins using the cal values (see cnts to kelvins ). ... CalInK(avg) is the measured cal value averaged over the entire 172 Mhz band of the spectra. ... The mask was then applied to all averages. the 1200 Mhz polB is not on scale, but it is offset from the 1350 Mhz band . Bottom: Compute the rfi mask from the calon,off and well as the position on,off data. the 1200 Mhz band now has a smaller offset from the 1350 Band. ...

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• Slide 2
• Alfa Rcvr monitoring routines
• a2584

polimodel -- Produce model linear polarization and position angle images . ... Whether to apply random errors to output polarization and position angle values. seed = "" [integer] . ... This task produces a model linear polarization image and corresponding position angle image from an input image assumed to represent intensity (Stokes I parameter). ... A threshold for the input image can be defined such that polarization and position angle are not computed for input values less than this threshold. ...

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• ESO - I derived quantities related to the performance of an instrument. How do
• ESO - Science Announcements
• FORS1 Photometric System Characterization

polimodel -- Produce model linear polarization and position angle images . ... Whether to apply random errors to output polarization and position angle values. seed = "" [integer] . ... This task produces a model linear polarization image and corresponding position angle image from an input image assumed to represent intensity (Stokes I parameter). ... A threshold for the input image can be defined such that polarization and position angle are not computed for input values less than this threshold. ...

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