... Data Analysis SAS News What is SAS? ... Back to Calibration Homepage The most recent Canned Response Matrices can be downloaded here (please refer to Update 2014-11-24 ) and can be used to estimate EPIC count rates in AO15. ... PN response files . ... MOS response files . Since SAS 6.5 the full set of ready-made MOS response files is not provided (see "Update 2005-12-15" ). ... Note: MOS response files before SAS 6.5 had a different nomenclature as the one listed above (see "Update 2005-12-15" ). ...

IBIS Data Analysis . ... IBIS . ... Flat Fielding - Introduction . The images obtained by IBIS will have intensity variations across the field of view that are not due to the solar image, but rather caused by instrumental effects that alter the observed intensity in each point of the field of view. ... IBIS Flat Fielding Techniques . ... Therefore, it is desirable to obtain the flat field measurements center on a point along the equator near the heliographic center of the solar disk. ...

... NICMOS Data Handbook > Chapter 4: Anomalies and Error Sources > 4.6 Flat Fielding . 4.6 Flat Fielding . ... NICMOS flat fields show response variation on both large and small scales. ... The flat-field variations are due also to a strong function of wavelength. ... That paper describes methods for constructing color-dependent flat-field reference files, and provides IRAF scripts for doing so (currently applicable to Cycle 7 and 7N data, but see the NICMOS Web page for updates on this script). ...

Monte Carlo Methods for Including Calibration Uncertainties in Model Fitting Analyses Jeremy J. Drakea , Peter Ratzlaffa , Vinay Kashyapa , Richard Edgara , Rima Izemb , Diab Jeriusa , Herman ... University, Cambridge, MA 02138 MIT Kavli Institute for Astrophysics and Space Research, Cambridge, MA 02139 b c SUMMARY · Instrument response uncertainties almost universally ignored in astrophysical X-ray ... Limiting accuracy of Chandra ACIS reached in spectra with 10 4 counts. ...

... The improvement will be more pronounced in our crowded Wide Field Camera (WFC) images, and may be increased further through use of a more sophisticated method of combining the individual dithered images. Our analysis allows us to check for point spread function shape variations in the HST Planetary Camera (PC) field. ... In crowded field images, we are deriving information about the faint end of the luminosity function (LF) from the texture of the image background. ...

Next: Fitting the Blaze Up: Instrument Response Correction Previous: Instrument Response Correction . ... This flux has to be corrected for two effects in order to get absolute fluxes: first, for the echelle blaze effect, and second, for the chromatic response of the instrument. ... The solution adopted in the reduction, using the standard star љ , is to correct for both the blaze effect and the instrument response simultaneously. ...

Jeff mock supplied 6 different types of filters to use with the high resolution mode of the mock spectrometer. ... Plots were made of the time domain voltage response as well as the frequency domain power response. A decimation of 10 was used for the filter decimation. this gave a filter length of 80 coeff. The plots compare the filter shapes for these filter types (.ps) ( .pdf ) . ... Each color is a different filter type . middle: spectral density reponse for each filter . ...

... Primordial theory review : Dick Bond . Defects and the CMB review : Andy Albrecht . ... Gravitational wave contribution to CMB anisotropies : V.B. Lukash and E.V. Mikheeva . C_l from cosmic strings : Lloyd Knox . Some aspects of CMB anisotropies induced from topological defects : Mairi Sakellariadou . ... CMB anisotropies from scaling sources : Ruth Durrer . ... SZ observations I : Sarah Church . ... Holes in the microwave sky? ... Detecting cosmic strings in the CMB : James Robinson . ...

. Note: This material is from a 1994(!) Talk about CCDs - the physics remains the same, only the detector size has increased since then. ___________________________________________________________________ The Electronic Universe Project e-mail: nuts@moo.uoregon.edu

... In order to compare the number of different evolutionary stages obtained and X-ray luminosity of the chosen X-ray sources with the observed galactic values we use the sum of C/O+O/C , where C and O are the calculated and observed values of a given binary type, respectively. If we make comparison for a number of different binary species (for example, we compare the number of CV, number of X-ray pulsars,   total X-ray luminosity of LMXB, etc.), we write this criterion in the form: . ...

Next: J.E. Chambers, Research Astronomer Up: Research Previous: Research Contents . ... Solar Variability and Climate . Other Activities . ... Applied to data of flares on Gliese866 he was able to estimate the area of hydrogen emitting flare regions as 1-13% of the stellar surface. ... As partners in the project, Armagh Observatory has been asked to contribute to the selection process in exchange for priority access to the data which will eventually flow from the satellite. ...

... This type of analysis requires careful intensity calibration of the Mopra observations. ... Figure 1: Comparison of SEST and Mopra data before and after calibration of the Mopra data. (a) SEST corrected antenna temperature (T A *) plotted with Mopra peak antenna temperature before calibration (Q T ). ... The calibrated Mopra observations can then be placed on the SEST antenna temperature scale using the linear fit from Figure 1b. This relationship is . T A *(SEST) = (1.62 ? 0.06)T A '(Mopra). ...