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TOFSANSResolutionByPixel v1¶
Summary¶
Calculate the Q resolution for TOF SANS data for each pixel.
See Also¶
Properties¶
Name 
Direction 
Type 
Default 
Description 

InputWorkspace 
Input 
Mandatory 
Name the workspace to calculate the resolution for, for each pixel and wavelength 

OutputWorkspace 
Output 
Mandatory 
Name of the newly created workspace which contains the Q resolution. 

DeltaR 
Input 
number 
0 
Virtual ring width on the detector (mm). 
SampleApertureRadius 
Input 
number 
0 
Sample aperture radius, R2 (mm). 
SourceApertureRadius 
Input 
number 
0 
Source aperture radius, R1 (mm). 
SigmaModerator 
Input 
Mandatory 
Moderator time spread (microseconds) as afunction of wavelength (Angstroms). 

CollimationLength 
Input 
number 
0 
Collimation length (m) 
AccountForGravity 
Input 
boolean 
False 
Whether to correct for the effects of gravity 
ExtraLength 
Input 
number 
0 
Additional length for gravity correction. 
Description¶
Calculates the Qresolution per pixel according to Mildner and Carpenter equation
where \(L1\) and \(L2\) are the collimation length and sampletodetector distance respectively and
and
where \(\sigma_{\lambda}\) is the overall effective standard deviation in wavelength. \(\Delta \lambda\) values are found from the wavelength binning of the InputWorkspace, \(\sigma_{moderator}\) is the moderator time spread (the variation in time for the moderator to emit neutrons of a given wavelength). Note that \(\Delta \lambda\) may be imposed by wavelength steps set elsewhere in Mantid which should be at least as large as the equivalent time bins used in the original histogram data collection. For event mode data \(\Delta \lambda\) is in theory very small, but in practice a histogram in time has to be generated (perhaps using monitor time bins or specifically set eventtimebins), before a rebinning into user provided wavelength steps in InputWorkspace. Again the latter steps should be the largest.
Q values needed here are calculated in the same way as for Q1D, including correction for gravity for which detector coordinates are assumed centred at zero wavelength.
\(\sigma_Q\) is returned as the yvalues of the InputWorkspace, and the remaining variables in the main equation above are related to parameters of this algorithm as follows:
\(R_1\) equals SourceApertureRadius
\(R_2\) equals SampleApertureRadius
\(\Delta R\) equals DeltaR
\(\sigma_{moderator}\) equals SigmaModerator
\(\L_1\) equals CollimationLength
\(\lambda\) in the equation is the midpoint of wavelength histogram bin values of InputWorkspace.
Collimation length \(L_1\) in metres in the equation here is the distance between the first beam defining pinhole (Radius \(R_1\)) and the sample aperture (radius \(R_2\)). (Beware that \(L_1\) is more often the moderator to sample distance.)
For rectangular collimation apertures, size H x W, Mildner & Carpenter say to use \(R = \sqrt{( H^2 +W^2)/6 }\). Note that we are assuming isotropically averaged, scalar \(Q\), and making some small angle approximations. Results on higher angle detectors may not be accurate. For data reduction sliced in different directions on the detector (e.g. GISANS) adjust the calling parameters to suit the collimation in that direction.
Note that \(\Delta\) is the full width of a rectangular distribution in radius or wavelength, for which the standard deviation is \(\sigma=\Delta/\sqrt{12}\). For a Gaussian distribution the FWHM (full width at half maximum) is \(\sqrt{8\ln{2}}\sigma=2.35482\sigma\). For an exponential decay \(e^{t/\tau}\), the standard deviation (and the mean) is \(\tau\). For nonrectangular distributions these equations allow the equivalent \(\Delta\) to be entered as \(\Delta=\sqrt{12}\sigma\).
This version of the algorithm neglects wavelengthdependent detector detection depth effects.
Categories: AlgorithmIndex  SANS
Source¶
C++ header: TOFSANSResolutionByPixel.h
C++ source: TOFSANSResolutionByPixel.cpp