This is a list of most of the commands and the syntax required. For a fuller description type help at the prompt in psrprof or look at /psr/help/psrprof.

ABCD E FG H I J K LMNOP Q RS T U V W X Y Z

Command

Syntax

Description

 If only channel_A is specified, this is averaged into channel 1.

 If no channels are given, AVCH averages all the channels of each polarisation into sequential channels starting at 1. The polarisation of the resulting channels is preserved and the number of channels reset to the number of pols. (Function assumes all channels of each polarisation are grouped together eg llllrrrr)

 If channel_A is set to -1 then all channels are averaged and the average is placed in the next available channel (pol set to 'i'). The number of channels is incremented by 1.

 If channel_A is set to -2 then all channels of the same frequency are averaged and the average is placed in first (lowest) channel of each set.

 The number of channels is reset according to to number of frequency sets and the pol changed to i.

 A check is made that the channels specified are contained in the data.

 Examples:

• AVCH IN 2 1 averages channel 2 and 1 in IN array, result in 1 
• AVCH IN 3 averages channel 3 and 1 in IN array, result in 1 
• AVCH IN avs all chans by pol in IN array eg llrr --> lr 
• AVCH IN -1 avs all chans result in nch+1 
• AVCH IN -2 avs all chans by freq in IN array eg llllrrrr --> iiii
• AVCH IN 2 1 SCALE scale channels before averaging 2 and 1, result in 1

 If ch1 and optionally ch2 are given, COPY copies ch1 in IN array to ch2 in the OUT array. (Omitting ch2 will give a copy of ch1 from IN to OUT). See also COPYCH for copying channels within an array

 Examples:

• COPY INAV copies IN array to AV array 
• COPY INAV 1 copies IN array channel 1 to AV array channel 1 
• COPY INAV 1 2 copies IN array channel 1 to AV array channel 2

 Example:

• COPYCH IN 1 2 copies IN array channel 1 to channel 2

 The default behaviour of psrprof is to use the pulsar parameters given in an ephemeris file to correct the pulse arrival time. The ephemeris file to be used at any given MJD is found in a lookup file called ephindex.dat which has the following form:
 
 

! ephindex.dat file: Contains the name of an .eph 
! file, and the end date (mjd) for that file to be 
! applied. (Any text after the MJD will be ignored).
! END statement is optional, comment lines start 
! with a !
! An MJD of -1. means 'until the last syllabub
! of recorded time'
psrav 50934. 98/05/01
psr99 51452. 99/10/01
psrA0 51740. 00/07/15
psrA0b 51805. 00/09/18
psrA0c -1.
END

• C To change a single data point. Position the cursor over the point to be changed and vertically at the required new value. The option 'C' is now entered, followed by the channel number. A dashed line is then drawn between the old and new values. 
• I To interpolate between two data points. Position the cursor over the first point and vertically at the required level and enter the option 'I'.Place the cursor over the second point and enter the channel number. A dotted line will then be drawn showing the new data. 
• R To restore the last data point that has been changed. Will fault if no point has been restored, but after having restored a point, will not restore until a further point has been changed. 
• Z Similar operation as I but the data in the selected region is set to zero 
• D To display the latest data i.e after some operation without quitting. 
• Q This is the clean way to exit.

• fft data_block_a sum data_block_b

This will carry out an fft on data_block_a and add it to an fft that has previously been formed in data_block_b. The result is left in data_block_b
• fft data_block_a div data_block_b

This will carry out an fft on data_block_a and then divide it by the fft that has previously been formed in data_block_b. The result is left in data_block_a.
• fft data_block inv <opt>

This will carry out the inverse fft operation, multiplying the fft in data_block by a gausssian of width opt, where opt is the fraction of the datablock width. The result is left in data_block_a when finished.
The fourier transform is held with the amplitudes in channel 1 and the phases in channel 2.
 

Frequency ranges are:-
< 500MHz uses 408temps.bin or channel 1 of templates.bin
>= 500MHz AND < 750MHz 610temps.bin or channel 2 of templates.bin
>= 750MHz AND < 1100MHz 910temps.bin or channel 3 of templates.bin
>= 1100MHz AND < 1500MHz 1420temps.bin or channel 4 of templates.bin
>= 1500MHz 1600temps.bin or channel 5 of templates.bin

Checks whether the data looks like template data, and faults if the Header time is not less than one day. The template in A3 is then automatically operated on by CHANGETBIN using the value of TBIN found in the specified data block. (This command does not alter the value of INCHAN)
Specials..... pulsars 0531+21, 0329+54, 1828-10 and 0538+2817 are hard coded to use either a calculated template (0531+21) or a combination of 2 templates in tempa.bin and tempb.bin. To use a template combination for these pulsars the file templates.bin should not be found, and the templates.code file should read eg: (formatting must be exact).

  0538+2817 00000 M

    A,a - amplitude
    B,b - width
    C,c - position
    D,d - baseline
    E,e - slope

 If GETARRTIME alone is used, the template is convolved with the data block and an arrival time found by interpolation around the peak of the convolution.

 If GETARRTIME FREQ is used, the data is convolved with the template in the frequency domain

1. The number of arrival times to be used,(MAX=100) 
2. The span of the printout, and 
3. The limit for rejecting 'bad' points.

• 0= OK
• 1=no poln data in syscal.dat
• 2 = freq. inconsistency 
• -1 = Jycnt used instead of JYSCAL
•  -2 = unexpected poln. id.

 Other options in place of the name of a data block are:-

• 1828-10
• 0329+54
• 0538+2817
• 0531+21 or CRAB

 CRABTEMP type
CRABTEMP uses the parameters from the IN array and forms a template for the Crab pulsar in the A3 array. The command is followed by 1 or 2 to determine whether the main pulse or interpulse is first.

• MON <datablock> <ASCII>

If the quantity is a data block then the following options are available:- 
• MON <datablock> shows a full mon 
• MON <datablock> hdr only shows the header information 
• MON <datablock> ch only shows the channel information 
• MON <datablock> ch <channel no> shows the data in the required channel. 

• Default file type is binary (or use bin qualifier) the exact flavour is found from header information.
• epn, sigproc and mel files are recognised by the file extension or qualifier. These file types may contain multiple profiles with multiple channels. (except sigproc which is currently single channel)
• xray/asc/bak files are recognised ONLY by the qualifier. The code for these qualifiers probably hasn't been used in anger for many years, expects specific datafile formats and doesn't look too fault tolerant!)

• verbose - print debug information
• rms <threshold> [ignore <val> [periods]]

Calculates the rms of each subintegration. If ignore is specified then val seconds (or periods if stated) around the central bin are not included in the calculation of the rms (should be used for scintillating pulsars). Any subintegration with an rms greater than the smallest rms multiplied by the threshold is deleted
e.g. testreject a4 rms 3 ignore 0.1 periods verbose
• slope.

Applies fitslopes to the data before any other analysis
e.g. testreject a4 slope rms 10 verbose
• zap <val> 

Runs zap to remove a sinusoid of period val seconds (default = 0.02) from the data before any other analysis is carried out.
• save. Writes any deleted subintegrations to intreject.dat

• CAL:

If the option CAL is present, the data are scaled by the factor factor/(DCLON-DCLOFF), so that the factor is treated as being the flux density of the calibration signal. 
• NORM:

If the option NORM is present, the data are scaled by the factor factor/DCLEV.

• BLOCK <block_number>
• TIME <date_time>
• PSR <pulsar_name>
• NEWPSR <> 

1. The required data_block (i.e.IN,AV,A3,A4) 
2. The required channel 
3. The new_value for FOBS for that channel

1. The required data_block 
2. The frequency of channel 1 
3. The frequency difference between channels.

1. The required data_block (i.e. IN,AV,A3) 
2. The name of the quantity to be changed 

The quantities that can be changed are:- 
Pulsar parameters:- RA, DEC, EPOCH, PERIOD, PDOT, PDDOT, UTS, DUTS 
Binary parameters:- EPBIN, PBIN, ASINI, OMEGA, OMEGDOT, ECCBIN 
Observing values :- NCH, NBIN, ITELNO, DDUCHANS, DDUF, TBIN, DELAY NP, DM, CLOCK1, DDUDF 
Sundry items :- COMMENT, PSRNAME, JPSRNAM, POL,
JFLAG
3. and 3) The new_value(s). 

• SETVAR IN NCH 1 
• SETVAR IN POL 1 4 i l q u 

• PULSARS - the first block of a new pulsar is summarised 
• BLOCKS - every block is summarised. 

• WRITE COMMAND SEEK Write a seek command for the current pulsar
• WRITE COMMAND GATES <B|S> gatenumber Write out a SETGATES command for the currently set gates. If an optional gatenumber is supplied then only that gate is written out. The B option writes the line out in terms of bins, and the S option in terms of time. If the argument is negative then gates 1 to ABS(argument) are written out.
• WRITE COMMAND EDITS Write out the current edits to the file, in a form suitable to OBEY
• WRITE COMMAND FILE writes a SET INIFILE

IDENT, CLOCKS, FITTIME, FITERR, CORRTIME, SAT, PSRNAME, TEL, FOBS ,IDDU, CHAN, PULSEAMP, DCLEVEL, GATEAMP, NEWLINE, DATA, FLUX ,MA ,NBIN ,FITAMP, DCLOFF, AZEL, DDUF, DDUDF, SCINTAMP, STRING, SUMMARY, POL, WIDTH, TBIN, TEMPO, MJD, TRES, RADEC, OBSRADEC, RADEC2000, OBSRADEC2000, CALLEVEL, SIGMA, DCLON, TSKY, FITWIDTH, NP, SHORTMON, UTS, PARANGLE, POSDIFF, TOBS, MJDM, PARS