There is an sm macro for plotting up the residuals, and a histogram of the residuals. chisq.pro also outputs files that are useful for examining the residuals (the difference between the predictions of the model and the data). The most important program in the package, written in the IDL language, is called chisq.pro and calculates $chi^2$, for an input power spectrum, according to the offset log-normal form of Bond, Jaffe and Knox (astro-ph/9808264). A unique aspect of this compilation is that the non-Gaussianity of the uncertainties has been characterized. The data are the constraints on the cosmic microwave background (CMB) angular power spectrum from all published data as of 9/99. The RADPACK package, written in IDL, contains both data and software. The SPEMD consists of a softened power-law radial distribution with elliptical isodensity contours.
#Saoimage ds9 position fitting code
FASTELL is a code to calculate quickly and accurately the lensing deflection and magnification matrix for the softened power-law elliptical mass distribution (SPEMD) lens galaxy model. This makes it easier to use these distributions for modeling individual lenses as well as for applications requiring larger computing times, such as statistical lensing studies. We present a family of lens models for which the deflection can be calculated to high relative accuracy (10-5) with a greatly reduced numerical effort, for small and large ellipticity alike. They are difficult to use, however, since previous studies have shown that the deflection angle (and magnification) in this case can only be obtained by rather expensive numerical integrations. Since galaxies are usually observed to have elliptical light distributions, mass distributions with elliptical density contours offer more general and realistic lens models. In the default mode, SPECTRUM computes the stellar-disk-integrated normalized-intensity spectrum, but in addition, SPECTRUM will compute the absolute monochromatic flux from the stellar atmosphere or the specific intensity from any point on the stellar surface.īecause of their simplicity, axisymmetric mass distributions are often used to model gravitational lenses.
SPECTRUM can be programmed with "command-line switches" to give a number of different outputs. SPECTRUM can use as input the fully blanketed stellar atmosphere models of Robert Kurucz including the new models of Castelli and Kurucz, but any other stellar atmosphere model which can be cast into the format of Kurucz's models can be used as well. SPECTRUM computes the LTE synthetic spectrum given a stellar atmosphere model.
The code for SPECTRUM has been written in the "C" language.
#Saoimage ds9 position fitting windows
It will also run under Windwos 9x/ME/NT/2000/XP using the Cygwin tools or the distributed Windows binaries. Gray, 1992-2008) is a stellar spectral synthesis program which runs on a number of platforms, including most flavors of UNIX and LINUX.
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