Difference: SpireCalibrationWeb (52 vs. 53)

Revision 532012-03-09 - LucaConversi

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META TOPICPARENT name="WebHome"

SPIRE instrument and calibration web pages

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Example use
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This example is based on fitting the peak of Gamma Dra in ObsID 0x50005984 in the PSW band.
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This example is based on fitting the peak of Gamma Dra in ObsID 0x50005984 in the PSW band. The fitter requires a SpireListContext with PointedPhotTimelines: these data should be processed through a baseline removal or destriper tool before this class is used.
 
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fitter=bendoSourceFit(inputContext)
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obs = getObservation(obsid=0x50005984, useHsa=1) l1_nobase = baselineRemovalMedian(obs.level1)

fitter=bendoSourceFit(l1_nobase)

 param=fitter.fit("PSW", 269.1515617, 51.488894, 200) param=fitter.fit("PSW", 269.1515617, 51.488894, 22, 300, 350)
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The first line defines an instance of the fitter object.
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The first line load the observation from the Herschel archive, while in the second a median baseline is removed from the observation's level 1. The third line defines an instance of the fitter object.
 
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The second line calls a method in which the data within a 200 arcsec circle centered on RA=269.1515617 and Dec=51.488894 is fit with a Gaussian function. The default is to fit an elliptical Gaussian function with a variable background. The first parameter will be the peak flux density.
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The forth line calls a method in which the data within a 200 arcsec circle centered on RA=269.1515617 and Dec=51.488894 is fit with a Gaussian function. The default is to fit an elliptical Gaussian function with a variable background. The first parameter will be the peak flux density.
 
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The third line calls a methods in which a background is measured within an annulus between radii of 300 and 350 arcsec and then a Gaussian function is fit to both the central 22 arcsec and the background annulus. The default function, an elliptical Gaussian function with a variable background, is still used in this case.
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The fifth line calls a methods in which a background is measured within an annulus between radii of 300 and 350 arcsec and then a Gaussian function is fit to both the central 22 arcsec and the background annulus. The default function, an elliptical Gaussian function with a variable background, is still used in this case.
  See the comments at the beginning of the code to learn how to select optional functions, set parameters for the fits, or get additional data based on the resulting fits (e.g. uncertainties in the best fitting parameters).
 
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