... The models provided are: . abs - absorption of x-rays by neutral gas with solar abundances. parameter 1 = . ... parameter 2 = . ... normalization - logarithmic value of the flux density at 1 keV in units of keV cm -2 s -1 keV -1 . ... normalization - logarithmic value of the normalization of the gaussian in units of keV cm -2 s -1 . ... absorption ( params )* model ( params ) . ... A single value for the normalization (i.e., fixed normalization) will force the program to use that value. ...

... efftplot (efftplot-2.17) [xmmsas_20080701_1801-8.0.0] . ... The parameters of powspec are computed from the parameters of efftplot , such that for each energy band, only one time-averaged PDS is computed. Then for each energy band, efftplot reads the PDS into the FITS file produced by powspec , and plots it with the PGPLOT library. ... 1 : PDS is normalized such that the (white) noise level expected corresponds to a power value of 2. ... 2 : as =2, but the expected white noise level is subtracted. ...

... Avg: the average value of the spectra (maybe throwing out some channels at the edges). <>:average over the spectra (throwing out points at the edges if you want). gCal(f) :- frequency dependence of the tabulated cal values. ... calInK(Avg): Scaler cal value averaged over the band. calOffSpc(Avg): cal off value averaged over the band (in spectrometer counts) . ... cntsToK(avg) = calInK(Avg) / (calDif_cnts(Avg)) . To convert a spectrum b_cnts in spectrometer counts to b_K in Kelvins using cntsToK: . ...

... A frequently used procedure, alternative to the correction for the chromatic response, is to normalise the continuum to unity by dividing the observed spectrum by a smooth approximation of its continuum. This approximation can be obtained either interactively with the graphic cursor, or from a table (command NORMALIZE/SPECTRUM ) or by dividing the raw data by itself after filtering or smoothing. Median filtering and running average algorithms are well suited for this purpose (command FILTER ). ...

... The close proximity of the Magellanic Clouds allows us to probe the nature of these star forming regions at small spatial scales. ... We present the spatial analysis, via aperture/annulus photometry, of 16 Large Magellanic Cloud (LMC) and 16 Small Magellanic Cloud (SMC) H II region complexes using the Spitzer Space Telescope's IRAC (3.6, 4.5, 8 ЮМm) and MIPS (24, 70, 160 ЮМm) bands. ... The IRAC, MIPS, UV, and HЮБ spatial analysis are compared with the spatial analysis of the TIR. ...

... MIPT Solid State Physics Department . ... Interacting Electrons in Normal Metals . ... The course is an introduction to interacting Fermi-particle physics and intended for future experimentalists. ... Hartree-Fock approximation. ... Linear reaction function. Calculation of density-density reaction function. Relation of density-density reaction function to compressibility of Fermi liquid and thermodynamic state density. ... Density-density reaction function of free Fermi gas in long-wave limit. ...

We cannot observe the way the distant universe accelerates cosmic rays or produces energetic photons, but acceleration processes also occur on our Sun , though on a much more moderate scale. ... That is why such events are often missed by cosmic ray detectors near the equator, where the lowest energies are excluded by the Earth's magnetic field. The best detectors for observing solar particles are therefore those sensitive to the lowest energies of the cosmic radiation. ...

... Star Atlas . ... stars . ... If neutron stars don't produce energy from fusion, like normal stars, how can they shine in visible light? ... Although it is true that neutron stars have, for the most part, consumed all their internal thermonuclear fuel, they tap into other energy sources to produce light. Indeed, neutron stars are remarkably "resourceful" and employ a variety of physical mechanisms to make themselves visible.A newborn neutron star is incredibly hot ? ... Atlas of the Stars . ...

Next: Feature enhancement: local Up: No Title Previous: Feature enhancement: filtering . ... As a result, a common magnitude scale (contour lines on the maps above, or color scale on Fig.1) will poorly display the short-duration events in a signal. Normalizing each line of the map (fixed duration) so it has unit variance (in effect dividing the energy map by the mean energy spectrum) at each duration restores more details of small-scale activity (Fig. ...

... Next: The PROS Big Up: Software Systems Previous: Data Reduction Software . ... The srcinten task provides PROS users with a tool to compute count rates for point sources in the ROSAT High Resolution Imager (HRI). ... Corrected upper limits are cited at locations where the count rate falls below the source detection threshold. ... Srcinten is a new PROS task that computes and applies the above correction factors to the net counts in a user-specified aperture. ...

... The units of N(S) are counts/Jy/steradian. The user also specifies N0, which is a cosmological normalization, usually a power law of S. This function is input via a power law and/or polynomial. ... Key: out Confusion noise (sigma) image (1/2 size of beam image) in Jy Key: flux 3 numbers (Jy). flux(1) and flux(2) define the range of flux densities for which the confusion noise is calculated. flux(3) is the break point below which the power law is used, and above which the polynomial is used. ...