On Saturday 02 August 2003 04:32 pm, Ian Drake wrote:
At this time, my particular interest is in attempting to identify clearly next-nearest neighbors in the RSF before attempting to do fitting. It is my hope that a positive identification of the next-nearest neighbor by means of IM analysis/ and or k-weighting will add validity to my final fitting results.
Well... I don't know what an "RSF" is or what "IM analysis" is, but I think I can suggest a way to isolate the scattering atom phase shift in a way that requires only a small amount of work and can be used with either ifeffit or artemis as they exist today. The second column of the feffNNNN.dat file is the central atom phase shift. The third and fourth are the scattering atoms magnitude and phase. Copy your feffNNNN.dat file of interest to another name, say feff_next_neighbor_no_caps.dat. Edit the new file, replacing the second column with zeros. Read this into ifeffit or artemis and use it as the path for phase correction. In artemis, this is done in the data view using the pull down menu labeled "Path to use for phase correction". Obviously, you should choose your edited path. In artemis, you may need to set the amplitude for this path to zero so that it doesn't really get used in a fit. That said, it's not clear to me how phase correction will really do what you seem to want. It seem unlikely to me that the signal beyond the first shell will magically become clear simply by doing phase correction. If the signal is a superposition of various scatterers before phase correction, it will still be a superposition of various scatterers afterwards. Removing the scattering atom phase shift does not affect the terms in the EXAFS equation that make peaks in a Fourier transform broad, nor does it magically separate signals which contribute similar Fourier components. Understanding how various paths contribute similar Fourier components is the reason that Artemis allows you to easily overplot data with the Fourier transforms of various paths. Then you can inspect the contributions from each path before setting up your fitting model. But if playing tricks with phase correction helps *you*, then great! That is why Artemis allows you to do this. B -- Bruce Ravel ----------------------------------- ravel@phys.washington.edu Code 6134, Building 3, Room 222 Naval Research Laboratory phone: (1) 202 767 5947 Washington DC 20375, USA fax: (1) 202 767 1697 NRL Synchrotron Radiation Consortium (NRL-SRC) Beamlines X11a, X11b, X23b, X24c, U4b National Synchrotron Light Source Brookhaven National Laboratory, Upton, NY 11973 My homepage: http://feff.phys.washington.edu/~ravel EXAFS software: http://feff.phys.washington.edu/~ravel/software/exafs/