... Archives . ... Reduced and Processed Data . ... 2 distribution plays an incredibly important role in astronomical data analysis, but it is pretty much a black box to most astronomers. ... Comment ( RSS ) | ... I guess in the typical analysis we call chi2 a ?random variable? that follows the chi2 distribution: . ... where D(i) is the observed data, M(i) is the model predicted data and we ?silently? assume that D(i) is normally distributed and each i measurement is independent. ... Chandra Blog . ...

Next: Code II: Unknown Up: Image Restorations of High Previous: Construction of Algorithms . ... The positions of the designated point sources ( ) must be given as well as initial amplitudes for and . ... The integrated flux of the point sources ( ) plus that of the distributed emission ( ) is constrained to equal that of the observed image ( ). ... This is investigated in Fig. 1 where all emission derives from point sources but only one - the brightest - is designated as such. ...

... 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 . ...

... We have assumed a constant in time star formation rate and the total number of stars in the Galaxy, , to be such that the total mass of the galaxy is ; assuming the Salpeter mass function   , we get . ... This number agrees with a standard estimation of the galactic star formation rate of order of per year. In each run of calculations, we trace the evolution of binaries with initial parameters randomly distributed according to the chosen initial laws. ...

... The next fragment computes the backscal and frac_exp statistics from the accumulated exposure, which is just the sum over all exposure map pixels that lie within the spatial selection region at the given channel. ... IF ( mode == HTR ) fg.backscal = background distribution integrated over EnergySourceRegion bg.backscal = background distribution integrated over EnergyBackgroundRegion normalizer = $rebin * extent( SpatialSourceRegion ) * fullExposure frac_exp = normalizer ? ...

... 1 What about: (t ) = exp - t 2 2 2 (13) (14) (15) The PDF that corresponds to this characteristic function : N (x ; ) = 1 2 2 exp - x2 2 2 (16) The Normal Distribution Results naturally where a large number of independent variables are additively combined (x - µ) 1 exp - N (x ; µ, ) = 2 2 2 2 N (t ; µ, ) = exp it µ - t 2 2 2 2 (17) (18) The Normal Distribution Plot 0.9 N ( x ; µ = 0 , = 1 ) 0 .3 9 9 x N (x ; µ = 0, = 1)d x 0.7 0.5 0.3 ...

Hide Zen home . ... Extent is a shortest and non-nested sequence of words, which satisfy a query . ... We don't consider normalization of document weight to 1, since we have no global information about document collection. w{i}, len{i} - weight and length of i-th extent . ... Next - the number of unique extents. freq{i} - frequency of i-th extent . We could consider strict and soft uniqueness of an extent, depending on how do we consider the order of words in extent. ... 2 - document length . ...

... arXiv.org . ... Although great progress has been made in modelling the disk with radiative transfer models able to reproduce the spectral energy distribution (SED) of Herbig Ae stars, the constraints brought by images have not been yet fully exploited. Here, we are interested in checking if these new observational imaging constraints can be accounted for by predictions based on existing models of passive centrally irradiated hydrostatic disks made to fit the SEDs of the Herbig Ae stars. ...

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 -- . ...