chem cryst
CRYSTALS manual
University of Oxford

Crystals User Guide

Chapter 2: Getting Started

2.1: INITIALISATION file

2.2: The basic data file

2.3: Migration from other program systems

2.4: The SCRIPT 'NEWSTRUCTURE'

2.5: Data reduction

2.6: EXAMPLE 1

2.7: EXAMPLE 2

2.8: EXAMPLE 3

2.9: EXAMPLE 4

The CRYSTALS system contains no routines for initial processing of the user's raw diffractometer data. Some other program must be used to prepare a file containing at least h,k,l and I for each reflection. If there is a serial number or X-ray exposure time associated with each reflection, the reflections need not be on a common scale, and a list of scale factors can be input to CRYSTALS (LIST 27) to perform the scaling as a function of serial or time. If reflections fall into a number of distinct batches each on its own absolute scale (from two crystals for example) a batch serial number may be associated with each reflection, and batch scale factors refined later during least-squares. There is no mechanism provided for extracting scale factors from intersecting data sets (Hamilton, Rollet, Sparks, Acta Cryst (1965) 18, 129). If absorption corrections are going to be applied, the user can either let CRYSTALS compute the reflection setting angles, or if a non-standard geometry was used he can input the actual observed angles. If the user wishes to use the standard deviations of his reflection in some future calculation, they should be provided in the input data and keys set to store them on the DISK.

If Patterson methods are not the most suitable for solving the structure, the user must use some other program (for example SIR, SHELXS, MULTAN). The instructions \PUNCH 6 and \FOREIGN enable structure factors to be output from CRYSTALS after data reduction in a variety of fixed and variable formats, some suitable for direct input to other programs.
The compressed format provides a suitable method for economical archiving of the reflections. This file could perhaps be appended to a file containing the other basic data for the structure, thus providing a source for rebuilding the DISK file should that be necessary. From time to time the user could append his latest coordinates to this file .

On program startup, CRYSTALS tries to obey an initialisation file, CRYSINIT.DAT, if it exists. This file may contain any valid CRYSTALS commands. Typically it contains 'system' commands like \SET <parameters>. It may also contain instructions to perform disk house keeping, or pass control to other files. In particular, the command \USE CRDIR:CRYSINIT.DAT will pass control to a CRYSINIT file in the current subdirectory, so that different subdirectories can have different initialisation files. The commands \USE CONTROL passes control to the terminal or batch control file without obeying futher CRYSINIT commands, and can be used to terminate the SCRIPT mode of working. A command like \USE CRDIR:INITIAL.DAT causes the file INITIAL to be processed, and so provides a mechanism for loading the disk file on systems where it cannot be preserved between jobs.

The basic data file contains those data which are unlikely to change during the course of the refinement. If subsequent events indicate that the original data were in error (for example, space group ambiguity) the new data could be appended to this file so that a record is kept of the initial tries. Details of most of the LISTS are found in VOL2, INITIAL.

The basic data file should contain:-

  TITLE   A line giving the compound name, source, formula, 
           date etc.
  LIST 1  The cell parameters. 
  LIST 2  The space group information. This is more 
           conveniently input with the SPACEGROUP command.
  LIST 3  The scattering factors. This list may contain 
           coefficients for atom types not in the current 
           structure, but since every atom type entry occupies 
           space in the users DISK, it would be unwise to use
           a single LIST 3 containing more than a dozen atom 
           types, unless the structure contained about that 
           many different atom types.
  LIST 4  The weighting scheme. The default is unit weights.
           Statistical weights are also available, but they
           are rarely suitable for the least-squares refinement 
           without extensive modification (Huml, Computing in 
           Crystallography, (1980), 12.15,  Indian Academy of 
           Sciences, Bangalore). 
  LIST 13 Details of the data collection procedure.
  LIST 14 The Fourier map limits. Remember the unique volume for
           a Patterson synthesis may be different to that for a 
           Fourier. Both are usually set with the SPACEGROUP 
           command.
  LIST 23 Mainly concerned with details for structure factors 
           and least-squares, but worth setting up here in case 
           it's forgotten later.
  LIST 29 Elemental properties, such as radii, weight.
 

The command \SPACEGROUP can be used to generate operators for most spacegroups in most settings and will also generate the Fourier limits, and \COMPOSITION will generate LISTS 3 and 29 from standard data files provided with the program.

If the basic data processing has been done in some other program system, the command \QUICKSTART provides a convenient way to transfer the data to CRYSTALS. If intensity data, i.e. I not F or F**2, are given, data reduction for four circle geometry is automatically performed. This is an example taken from VOL2 of the manual.

  \QUICKSTART
  SPACEGROUP P 21 21 2
  FORMULA C 6 H 4 N O 2 CL
  FILE CRDIR:REFLECT.DAT
  FORMAT (3F3.0, 2X, 2F8.2)
  DATA 1.5418
  CELL 10.2 12.56 4.1
  END
 

At sites where some on-line working is permitted, the SCRIPT NEWSTRUCTURE (which call the scripts STARTUP and DATRED, and hence many other sub-scripts) will guide the user into getting his initial data into the CRYSTALS data base.

Intensity data can be introduced to CRYSTALS either by embedding it in a control file, or from an auxilliary file read by the instruction \LIST 6 or \HKLI. This is the only time in CRYSTALS that users data are read in from an auxilliary device. If the data are in a compact form, say lines with four reflections per line, and there are not too many reflections, it would be best to enter them directly into the command line. If the reflections are in an extended form with, say, setting angles and other information for each reflection, it is probably more efficient to read them from the auxilliary file. The user has the option of FIXED or FREE format reads. With the exception of CRYSTALS compressed data, FIXED format reads are always more efficient. Remember that a figure of -512 or less for the first value on a reflection line terminates reflection input.

The section REFLECTIONS in the manual describes the options available and explains why work files are used at this stage. The user has already been cautioned (above) about the work files, he should also remember that sorting many thousand records can be time consuming. At the end of data reduction the user must copy his data from the work file onto his DISK (using READ TYPE=COPY in LIST 6) otherwise all it will contain is information pointing to the (possibly deleted!) work file. Some installations may provide means to preserve the work files, but this should only be necessary when processing large data sets. The reflection handling procedures in CRYSTALS are powerful but for many purposes a simple strategy will suffice. If multi-batch data is being processed, e.g. from several crystals, the user will need to change the data keys. REFLECTIONS bears reading several times.

The instruction \SYSTEMATIC should always be used, since it may provide confirmation of the space group, and moves reflections, by the permitted symmetry operators, into a standard segment of reciprocal space. This is a prerequisite for \SORT and \MERGE, which should also usually be applied since the computation of Fourier maps and structure factors is speeded up if the reflections are in a standard order. The user should not MERGE his reflections or apply Friedel's law if subsequent computations are geometry (e.g. analytic absorption) or polarity (e.g. anomalous scattering) dependent, or if he has multi-batch data and intends to refine batch scale factors.

A user doing many crystals structures might prepare himself a standard data reduction file which he could USE for all structures.

Intensity data are available on a common scale, 4 reflections per line, having been collected on a Weissenberg diffractometer, and are to be embedded in the input stream. The INSTRUCTONS, DIRECTIVES and keywords are written out more or less in full, though the experienced user might wish to omit or abreviate them.

 
  \LIST 13
  DIFFRACTION GEOMETRY=EQIUINCLINATION
  CONDITIONS WAVELENGTH=1.5418
  AXIS 1 0 0
  \LIST 6
  READ NCOEF=4 TYPE=FIXED F'S=NO NGROUP=4 UNIT=DATAFILE
  FORMAT (4(3F4.0,F8.0))
  END
  1   0   0    1234   2   0   0   24600   
  4   0   0    5000   6   0   0    100
  (etc)
  -512 
  \ a dummy reflection to end the list
  \LP
  \SYST
  \SORT
  \MERGE
  \LIST 6
  READ TYPE=COPY
  \FINISH
 

The reflection data output from a CAD4 are in a separate file produced by a pre-processor and in a format defined in the manual. No geometry dependent calculations are being done, so the default null orientation matrix can be used.

  \LIST 13
  DIFF GEOM=CAD4
  MATRIX
  COND
  \ the standard conditions on this site are 
  \ monochromatic Mo radiation
  \HKLI
  \LP
  \SYST
  \SORT
  \MERGE
  WEIGHT SCHEME=2 NPARAM=6
  \ this scheme filters out outliers
  PARAM .05 3.0 1.0 2.0 .01 .0001
  REFLECTIONS LIST=MEDIUM
  \ contributors more than 3 sigma from the 
  \ mean are listed with a *
  \LIST 6
  READ TYPE=COPY
  \FINISH
 

The keyword RATIO should be used in LIST 28 to limit the minimum ratio of I/sigma(I) used in calculations.

The data are in a free format, and the user wishes to carry weights based on sigma(Fo) through into least-squares. The reflections are embedded in the control data.

  \HKLI
  READ 5 FREE UNIT=DATAFILE F'S=YES
  INPUT H K L /FO/ SIGMA(/FO/)
  STORE 7
  OUTPUT INDICES /FO/ WEIGHT /FC/ BATCH/PHASE 
  CONT   SIGMA(/FO/) RATIO
  \ note that a slot is left for the weight later
  END
  1 0 0 123 10
  2  0 0 24600 130
  3  1 0 15420  70
  -512 0 0 0 0
  \LP
  \SYST
  \SORT
  \MERGE
  \LIST 4
  SCHEME 7
  \ to generate weights from sigma
  \WEIGHT
  \ this generates the weights from sigma, and stores 
  \ them in the weight slot. NOTE  that after the COPY, 
  \ the sigma slot does not exist by default, so that a 
  \ reWEIGHTing with scheme 7 will loose the weights.
  \LIST 6
  READ TYPE=COPY
  END
  \LIST 4
  SCHEME 5
  \ this ensures that we dont loose the weights by an 
  \ accidental reweight.
  END
  \USE LAST
 

In this example the weights are calculated and applied while the data is on the scratch files. The LIST 4 could equally well have been applied after the LIST 6, i.e. at some much later stage of the process, if we had preserved the sigmas.

The instruction \HKLI enables the user to apply some simple absorption corrections. All are only approximate, but do prove to be cost effective for routine work. The PHI and THETA corrections involve interpolation. The interval between the points should reflect the rate at which the curve is changing. This is particularly important for the PHI correction (NORTH, PHILLIPS, MATHEWS, Acta Cryst (1968) A24, 351) when the sample is plate-like. A plan for preparing a phi curve is to observe the intensity of a reflection whose scattering vector is close to the diffractometer phi axis at a number of phi values (say, at 10 degree intervals). For the calculation to be even approximately valid, the I vs phi curve should have two-fold symmetry, so that the two halves of the curve (0-180 and 180-360) can be superimposed and a smooth curve drawn through them. Values of I and phi are taken from this curve for a range rather less than 180 degrees and input to CRYSTALS. The user should note that he must give PHI Eulerian values, and not psi or phi-Kappa values.

The 'tube' correction, originally devised for cases where the sample was in a capilliary tube inclined at a substantial angle to the phi axis, (Watkin, J. Appl. Cryst. (1975) 8, 491), can be used to provide an approximate correction for needle-like crystals inclined to the phi axis. In this case the parameter 'MU' should be something like 0.8*mu*r, where r is the needle diameter. A[max] in this case would be the correction for a ray passing along the axis of needle. The 'plate' correction is similar, with 'MU' being mu*t, where t is the plate thickness. A[max] is rather less than the correction for a ray passing along a diameter of the plate.

The theta correction is suitable for any correction which is a smooth function of theta only, for example the spherical or cylindrical corrections tabulated in International Tables. Expect to see your temperature factors increase if you apply this correction!

If the user has measured standard reflections from time to time, he can compute decay or stability corrections. These are introduced to CRYSTALS as a LIST 27. Each reflection must have an associated sequence number. This can either be a serial number or a figure derived from, say, the X-ray exposure time. The scale factors in LIST 27 are associated with the the sequence number of the first of each batch of standard reflections. The scale factor for general reflections is then obtained by interpolation in this table. To avoid interpolation across scale discontinuities, two different scale factors may be given with the same sequence number. If the reflection sequence numbers do not rise continuously, (for example data from two experiments) interpolation will continue safely if scale factors are present in LIST 27 for the two reflections at the discontinuity. The scale factor scalenumbers are not used by CRYSTALS. Remember that there is a maximum value for the sequence numbers (try (X-ray time in secs)*0.1).

  \LIST 27
  READ NSCALE=10
  SCALE 1 1.00 1.00 2
  SCALE 2 1.01 1.00 30
  SCALE 3 1.00 1.00 60
  \ reflection sequence 60 is the first with 
  \ the larger scale factor
  SCALE 4 3.00 3.00 60
  SCALE 5 3.01 3.01 90
  SCALE 6 3.02 3.02 120
  SCALE 7 3.03 3.03 147 
  \ reflection sequence 147 is the last in 
  \ the old experiment
  \ reflection sequence 3 is the first in the new
  SCALE 8 3.03 3.03 3
  SCALE 9 3.02 3.03 50
  SCALE 10 3.03 3.03 100
  END
 

[The Crystals User Guide | Getting Started | Atoms And Peaks, Parameters, And Parameter Values. | Fourier And Patterson Functions | Generalised Fourier Sections | Regularisation | Hydrogen Placing | Refinement | Results | Conclusion ]