... Figure 1: Data from selected high latitude pointings overlaid in detector co-ordinates. 132ksec total low proton flare conditions, and bright point sources excised . Figure 2: Same data set from selected high latitude pointings but in 0.2-2keV only. ... Figure 3: Same data set from selected high latitude pointings but in 2-10keV only. ... Figure: EPIC MOS data set from selected high latitude pointings plotted as spectra (PATTERNS 12&&#XMMEA_EM), and normalised for approx 1 arcmin square. ...

Next: Examples and Photometric Up: Image Restorations of High Previous: Introduction . ... where is the intensity of the point sources (mainly zero apart from -functions at the positions of designated sources) and is the intensity of the background. ... When is zero the objective function becomes the same as that of the standard Lucy-Richardson technique. takes the form of an entropy expression which may be calculated in two ways, relative to a flat background: . ...

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Next: The Clark CLEAN Up: Image Deconvolution Previous: Introduction . The CLEAN algorithm (H?gbom 1974) (A&AS 15, 417) represents the image as a number of point sources in an otherwise empty field of view. ... The H?gbom CLEAN algorithm looks for the brightest (in an absolute sense) pixel (called a CLEAN component) in a specified region in the image (called the CLEAN window which must include all the real emission in the image). ... This subtracted image is called the residual image. ...

... 1Haynes+ A catalogue at 5 GHz of 915 sources in the Galactic plane is presented. Sources with a peak beam brightness temperature of at least 0.2 K above the surrounding background are included, except in confused regions; a point source of 0.2 K corresconds to 0.26 Jy. ... It was assumed that Hydra A was a point source with a peak flux density of 13 Jy at 5 GHz; this is equivalent to a mean beam brightness temperature of 10.0 K for a beamwidth of 4.1x4.4'. ...

... A technique allowing automatic representation by a relatively small number of independent parameters based on the principal component analysis of data sequences is presented. ... In recent years the spectrum of observed astronomical data can be characterized as greatly varied. ... In this instance, the problem of initial description and classification of newly-observed data becomes most urgent, especially if there is a lack of preliminary observational material and theoretical expectations. ...

Subject: Some useful data about gains, NFs compression points of Eddies box components . ... Gain: ~ 21 dB . ... 1 dB compression: + 6 dBm . ... 1dB compression point for this system is ~ +15 dBm. For a clean(i.e., very linear) signal, we recommend staying 10 dB or more below the 1dB compression point, putting the "peak linear power" at +5 dBm. ... Assuming an LNA + Mixer gain of ~ 35 dB and with + 8 dBm mixer compression point, any input - 27dBm will begin to saturate the mixer. ...

... Galaxies 99 Cosmic background with model of cloudy interstellar medium Yu. ... Figure 1: Averaged spectrum of the cosmic background I f in frequency range 0.25 200 MHz for the Galactic poles. ... First interpretation of the cosmic noise background spectrum at broad band frequency range 0.25 200 MHz with a model of the cloudy interstellar medium ISM is presented here. ... Synthesized background spectra I f for regions of the Galactic poles at the frequency range 0.25 200 MHz is presented in Fig. ...

Next: Average Up: Quick Guide Previous: Reduce the background data Contents . ... Load all data if you have sufficient memory (this may take a few moments). ... Use R EDUCE P OINT D ATA I MAGING PLOT to plot and edit the point data data in much the same way as you did with the background data. ... Use plots vs channel if you have to flag several entire channels. Use the PLOT A UTO option to automatically edit outliers in PhotonRate and VisSq (select all channels for speed). ...