True Color Image Gallery: Galactic SNR | ... Position of Central Source (J2000) : ( 05 40 11.1, -69 19 55.2 ) . ... Radio Images Page . ... Exposure uf . ... Trailed Image of the central source is significant. ... 0.3 - 10.0 . ... central source . ... nH was derived by fitting the trail of central source which is believed not to be piled-up. see fit detail page for more about the fit. see chandra spectrum page for region used. ... 2001 , ApJ, 560, 742 : Chandra ACIS imaging and spectroscopy . ...

Next: Catalog Construction Up: Observations and Analysis Previous: Source Detections . ... It was assumed that the highest signal gives the most likely position of the source. ... Comparing the summed map with the maps from the individual energy ranges, the one which produced the smallest error box was chosen to represent the source position, as long as was greater than 4, a level chosen to reflect a reasonable degree of confidence in the detection. ...

... This is followed by astrometric columns - ie columns for the Right Ascension, declination, position error, galactic longitude and galactic latitude. There then follows columns for the computed significance (signal-to-noise) of each source for each of the filters present. Columns for the instrumental magnitudes and colours for each filter, follow. ... Columns for the standard magnitudes and errors, for each filter, follow. ... Standard colours and errors then follow. ...

... We now consider estimation of count rates for objects with stellar, power law, and emission line spectra. To estimate the number of electrons collected from a point source of apparent visual magnitude V, one can use the equation: . ... If one knows the spectral index a (which is zero for a source with a flat continuum), V + AB_nu can also be calculated as the monochromatic Oke system magnitude at the corrected mean wavelength of the filter: . ... 6.3.3 - Count Rates for Emission Line Sources . ...

... Up: Science Data Pipelines . ... We designed and developed a package which simulates extragalactic point source data within a given field of view and SIRTF band. ... The simulator is modular and extensible to enable multi-wavelength simulations, has been optimized by utilizing parallel processing capabilities, and will be used to test pipeline software. ... The extragalactic simulator is capable of generating large numbers of galaxies within a given patch of sky for SIRTF pipeline testing. ...

... comparison of the system performance for alfa and lbw at OH (.ps) ( .pdf ) (no amps in) . comparison of the system performance for alfa and lbw at OH (.ps) ( .pdf ) (with amps in) . ... On 01apr05 the system performance was measured using the continuum source CTA21 (B0316+162. ... The plots show the comparison of the system performance for alfa and lbw at OH (.ps) ( .pdf ) (no amps installed). ... Black is polA, red is polB. ... G/T alfa)/(G/T lbw) . ... The polB/polA performance ratios are: . ...