1 Language CLIC\ Command Language Summary Continuum and Line Interferometric Calibration INFO : (HELP CLIC\ INFO) gives a list of recent modifications ATMOSPHERE : Perform atmospheric calibration. CHECK : Check the data for amplitude gain instabilities COMPRESS : Compress data COPY : Copy data CURSOR : Call the interactive graphic cursor DROP num [ver] : Take a scan out of the current index. DUMP : List some informations on the R spectrum. FILE type name : Define the input/output files. FIND : Search the input file for observations. GET [N] : Read a scan in the input file. HEADER : Display some header information on the R spectrum. IGNORE list : Ignore scans from the Input file. MARK : Force data to be treated as if flagged. MONITOR : process calibrations for phase correction parameters. LIST [name] : List header information about an ensemble of scans. MASK : Cause some flags to be ignored. MINMAX : compute extremal amplitudes in data MODIFY : Edit and change the scan header (and data). NEW_DATA : Wait until new data present in input file. RESIDUALS : Plot residuals from last SOLVE operation PLOT : Plot data according to display options PRINT : produces an output text file (PRINT BASELINE). SET : Enter a value for a parameter. SOLVE : Solve for calibration functions. STORE : Store calibration functions. TABLE : Create a UV data Table for mapping purposes. TAG qual list : Change the quality of scans in the output file. VARIABLES : enable/disable CLIC variables 2 INFO Main modifications to CLIC since the MAR99 version: [24-sep-1999] FIND /RECEIVER is now available [24-sep-1999] FIND will not be case sensitive for Source names and Line names. Main modifications to CLIC since the JUL98 version: [29-jan-1999] SET X TCHOP, TCOLD, TCABIN, TDEWAR1, ..., TDEWAR3: Plot some temperatures recorded in the receiver cabin. [13-jan-1999] SET PHASE ATM /ANT i j : The phase correction can be validated independently for the different antennas. [24-Nov-1998] SET X GROUNDEMIS, EMISSION, AIRMASS: new items to plot. [16-oct-1998] SET SCAN, FIND/SCAN: now accept a more general scan list s1 s2 s3 s4 ... Main modifications to CLIC since the APR98 version: [19-may-1998] MODIFY FOCUS: to correct the phases according to the actual focus position used (should be used only on data prior to November 1996, or April 1998 for the few projects using HIGH lock). [28-apr-1998] SET SELECTION CONT /WINDOW * is now allowed to reset frequency windows in the building of continuum tables from line subbands. [28-apr-1998] LIST/SHORT will now log the scan numbers is an array S_GROUP[2,N_GROUP] [25-apr-1998] LIST /OFFSET will give the list of position offsets in the current index (useful for a mosaic session). Main modifications to CLIC since the NOV97 version: [16-feb-1998] STORE CORRECTION AUTO [tmin] : tmin is now accessible (in minutes) [30-jan-1998] SOLVE FLUX now gives the decorrelation factor relative to the efficiencies logged in the scan headers. [24-nov-1997] SOLVE FIVE [/PLOT] now possible for five point pointing scans. SOLVE TOTAL/PRINT available. Main modifications to CLIC since the APR97 version: [08-oct-1997] FILE /DIRECTORY: Open a window to edit interactively the raw data file directories. [03-sep-1997] SET AMPLITUDE UNSCALED: to reset the SET AMPLITUDE SCALED state (if needed). [26-aug-1997] SET Y ATMVALIDITY: plots the validity of the phase correction (values 0 or 1) as stored by STORE CORRECTION [26-aug-1997] SOLVE GAIN SCAN to solve gain scan by scan (instead of averaging all scans) [21-aug-1997] SET Y WINDAVERAGE, WINDDIRAV, WINDTOP, WINDDIRTOP: plots the wind variables (average, direction of average, maximum, direction of maximum) [17-aug-1997] After a FIND the scans are now time ordered even across the 9999/0001 scan numbering boundary. [17-aug-1997] STORE CORRECTION SELF works like AUTO, but the phase correction valitity is based on the amplitude of each scan, whether or not it is a phase calibrator. [27-jul-1997] GET n /HEADER to access the header vatiables of a given observation without acessing the data itself (i.e. the header file only is needed). [25-jul-1997] SET OBSERVED n1 n2 : use integer representation of dates made possible [22-jul-1997] variable SHORTFILE available after FILE IN : contains the file name without directory or extension. [04-jun-1997] TABLE /RESAMPLE nchan rchan value inc V|F The syntax of /RESAMPLE has been changed for compatibility with CLASS: One may now enter the velocity or frequency offset at the reference channel. [22-may-1997] FILE /WINDOW Open data files via a file browser of the windowing system. [20-may-1997] SET PHASE ATMOSPHERE NOFILE bypasses the effect of STORE CORRECTION. [20-may-1997] It is now HIGHLY RECOMMENDED to use the extension ".hpb" when creating header files for calibration. [20-may-1997] FILE RAW [project] [date] [/WINDOW] This command may be used to open raw data files residing in the directories IPB_DATA:, IPB_DATA1:, IPB_DATA2:, ... assuming they have kept teir original names jj-mmm-yyy-pppp.ipb, (with date and project name), and to create header files for calibration. Main modifications to CLIC since the DEC96 version: [07-apr-1997] FITS [name] FITS will now create a fits file (named name- l0i) with each selected line subband. [04-apr-1997] SET SELECTION LINE DSB This is now allowed in LINE mode, and means that the side band will be automatically selected when the TABLE command is issued, to match the desired frequency range. [03-mar-1997] SOLVE FLUX [NOREFERENCE] Use the default efficiencies rather than a reference source to set the flux scale. [03-mar-1997] SOLVE FLUX [BEST n] Average the results of the n antennas giving the highest fluxes to compute the source flux. [12-feb-1997] COPY HEADERS|DATA [[NO]BASE] [[NO]]ANTENNA 1st argument is now mandatory; second and/or third select which calibration section is created. [08-jan-1997] STORE CORRECTION GOOD|BAD|AUTO Store, in the header of each scan, whether the atmospheric phase correction will be applied when SET PHASE ATMOSPHERE is used. Main modifications to CLIC since the NOV95 version: [29-nov-1996] SET WRITE DATA|NODATA now renamed to SET COPY DATA|NODATA. [12-nov-1996] STORE QUALITY qual ; change the data quality in the current index (equivalent to a loop of TAG commands). [12-nov-1996] LIST /VARIABLE variables /FORMAT formats : lists the header variables for scans in the current index; may also be used with /SHORT. [04-nov-1996] SOLVE POINT, SOLVE FOCUS, SOLVE GAIN, SOLVE DELAY now have an option /PRINT to write an OBS procedure in directory INTEROBS: [17-oct-1996] SOLVE HOLOGRAPHY [FREE r1 r2..] : some panel rings may be released from the paraboloid fit. SET Y AZ_ERR and ELERR ; AZ_PH and EL_PH : plot pointing errors, and horizontal coordinates of the phase tracking center. [04-jun-1996] SET Y AZ_ERR and ELERR ; AZ_PH and EL_PH : plot pointing errors, and horizontal coordinates of the phase tracking center. [27-may-1996] MODIFY ANTENNA|BASELINE /OFFSET 89|96 The argument to /OFFSET is mandatory, and selects either the old (89) or the new (96) standard station coordinates. [14-may-1996] ATMOSPHERE now checks the efficiencies on phase calibrators, assuming the flux in the header is correct. [10-may-1996] - FIND /SOURCE s1 s2 .. sn is now supported. - FIND /SCAN n1 n2 will now loop across 9999/0000 if n1 > n2. [29-apr-1996] - CLIC is now dimensioned for FIVE antennas. [29-apr-1996] - SET X|Y PARAL_ANGLE: The parallactic angle can be plotted. [14-apr-1996] - SET COPY DATA|NODATA: A new data access mode. See HELP SET COPY. - SET BASELINES ALL, SET ANTENNAS ALL: Use all the baselines, in the data by default. See HELP SET BASELINES, - SET SUBBANDS ALL, SET SUBBANDS LINE, SET SUBBANDS CONT: Use all the subbands in the data, switch between line and continuum subbands. - SET PHASE EXTERNAL|INTERNAL and STORE PHASE /RECEIVER: A new mode to use the other receiver as a phase reference for phase calibration. See HELP SET PHASE, HELP SOLVE PHASE. See also STORE PHASE. [07-mar-1996] - Command PHASE CONTINUOUS: to recover from a real time problem due to jumps of the LO2. [07-feb-1996] - Command MODIFY AXES: to correct for non intersection of the azimut and elevation axes. See HELP MODIFY AXES. SOLVE BASELINE has also been modified to solve for this parameter using elevation as an X axis. [17-jan-1996] - Command MODIFY BUG 1: to correct for a calibration bug affecting data between 11-nov-1995 and 09-jan-1996. [20-dec-1995] - Command PLOT /NOFRAME pen used to overlay a plot with the previous one, using a different color. [28-nov-1995] - SET PROJECT resets the RF mode to OFF. Main modifications to CLIC since the JAN95 version: [09-nov-1995] - Implementation of the atmospheric correction. See command MONITOR, and SET PHASE ATMOSPHERE. [08-sep-1995] - Command SET SORT RECEIVER|SCAN [25-jun-1995] - Command SET TIME_ORIGIN [08-jun-1995] - command SET UV_RANGE: data will not be plotted ouside of this range. 1 ATMOSPHERE [CLIC\]ATMOSPHERE [DETECTOR|CORRELATOR] [/NOWRITE] Recompute the atmospheric (transparency) calibration from the data and the informations provided by the SET ATMOSPHERE command. The operations are: - Compute atmospheric models from calibration scans, using either the continuum DETECTORs or the continuum CORRELATOR to measure the atmospheric emission. The data on the atmospheric monitor (the 1.3 mm) receiver will also be used to compute the phase correction coefficients. - Apply the new model to the observations and write (update) the recalibrated data if option /NOWRITE is not present. 1 CHECK CLIC\CHECK Threshold The continuum correlator had occasional instabilities in some of the 30 subbands. This command attempts to find out possible misfunctions of some subbands by comparing the amplitude of a subband to the mean amplitude of the 10 subbands of the same baseline. Threshold is the detection threshold (expressed in standard deviations from mean value). This command process only the current record. An example of use is VARIABLE DESCRIPTOR ON ! Turn on Descriptor variables. SET TYPE PHASE ! Use only on continuum sources, ! otherwise no signal... FIND FOR I 1 TO FOUND GET NEXT FOR J 1 TO R_NDUMPS ! Process record by record GET/RECORD J CHECK 2.0 ! 2 sigma is severe limit. 3.0 is a normal value. NEXT NEXT While these instabilities tend to smear out with time, a strong misfunction may influence the result. Data should be flagged accordingly, specially before bandpass calibration. Checking the source data itself is more difficult, since the signal may be too weak. 1 COMPRESS CLIC\COMPRESS timemax uvmax Compress data in the current index by averaging successive records in individual scans. 'timemax' is the maximum averaging time in seconds. Data with baseline orientation differing by more 'uvmax' in meters in the UV plane are not averaged, as well as data flagged differently. Defaults for timemax and uvmax are 60 seconds and 7.5 meters respectively. An output file must have been opened to receive the compressed data. Use command COPY rather than COMPRESS to copy the whole current index to a new file. For data taken after September 1992 (new correlator), the command will only compress the temporal data (data header and continuum subbands), since the spectral data is already compressed to 1 record per scan. 1 COPY CLIC\COPY HEADERS|[NO]DATA [[NO]BASE] [[NO]ANTENNA] Copy contents of the current index to the ouput file. The first argument is mandatory and controls whether the data section is actually written in the output file. COPY DATA selects the old mode which has been used so far. COPY HEADERS selects a new mode in which the data file, originally written at Plateau de Bure is later only used in a read-only mode. Further modifications are written in an output file that contains only the header sections, with e.g. calibration sections. In that output file the data sections are not written but replaced by pointers to the original file, which can now reside on a CD-ROM. When this file is later opened for input, CLIC will look for the data sections in the original (read-only) data file. The original data file may be kept locally (then it must have one of the extensions ".ipb", ".IPB;1" or ".IPB") or reside in any directory, which is pointed to by one of the logical names "IPB_DATA:", "IPB_DATA1:" to "IPB_DATA9:". The original file name MUST BE UNCHANGED, apart from the extension. It is HIGHLY RECOMMENDED to use the extension ".hpb" for the new file containing the headers. Example: Assume the original file is "14-apr-1996-f081.ipb", retrieved from the DAT tapes. Create a header file: clic\file in 14-apr-1996-f081.ipb clic\find clic\file out f081-b2.hpb new clic\copy headers Assume the file was on CDROM. Create a header file: sic\log ipb_data: "/CDROM" clic\file in "!ipb_data:F404F081.IPB" clic\find clic\file out f081-b2.hpb new clic\copy headers ! ! open f081-b2 for input/output, but do not write the data any more: file both f081-b2 find solve phase /plot store phase ! ... and so on as usual, except that the new file "f081-b2.ipb" contains only the headers and is much smaller than "14-apr-1996-f081.ipb-data". - Most commands are available in this new mode, even commands that affect data amplitudes phases such as ATMOSPHERE, MODIFY BASELINE or MODIFY DELAY. The phase factors are kept in the headers and applied only when the data will be later read again. - There need not be a one to one correspondence between the original ".ipb-data" file contents and the ".ipb" header file. That is the header file may refer to only part of the scans in the .ipb-data file (e.g. omit the IFPB or POINT scans), and it may refer to several Now arguments [NO]BASE and [NO]ANTENNA control whether respectively the baseline antenna-based calibration sections are written in the headers. Antenna-based cal is now the default and omitting the baseline-based sections saves a lot of space only the antenna-based sections will be created; do not forget to use COPY HEADE if you foresee you will need baselined-based calibration; or use COPY HEADERS for not so recent Bure data in which the baselined-based sections have been cre (otherwise those seldom used sections will use half the header space). 1 CURSOR CLIC\CURSOR mode Call the interactive cursor, if available on your graphic terminal. This enables you to measure point coordinates, and perform some data editing. One of the data points is selected according to the argument `mode'. In mode D the closest data point from the cursor is selected; in mode X (the default) the data point with closest X coordinate is selected; in mode Y the data point with closest Y coordinate is selected. - Press any key to get the coordinates of the selected point. - Press 'K' to delete the selected point from the current plot buffers (type PLOT SAME to replot the buffers). - Press 'N' to initiate a new range for Ignore, Tag, and Flag (see below) - Press 'I' to ignore all scans in the current range (initiated by scans. This works only with time-like plots, and is to be used preferrably for coordinates that are monotonous functions of time (scan number, observation number, time, ... - Press 'T' to tag all scans in the current range (initiated by 'N'). This is equivalent to typing the TAG command for the same scans. You will be prompted for a quality in the range 0 to 9. Same comments as with 'I'. The input and output files must be equal. - Press 'F' to flag all records in the current range (initiated by affect the baseline or antenna corresponding to the box you are pointing at. Same comments as with 'I'. The input and output files must be equal. - Press 'E' to exit the cursor mode. 1 DROP CLIC\DROP Obs [Ver] Remove an Observation from the current index. The version number must be specified if it is not the last in the input file, even if it is the last version in the current index. 1 DUMP CLIC\DUMP [Argument] A debugging command. - DUMP HEADER argument : lists a certain number of informations about the Observation header. Argument may be HEAD, GENERAL, POSITION, INTERFEROMETER, FREQUENCY, ATMOSPHERE, MONITOR, CONTINNUM, LINE, SCANNING, IC (Instrumental calibration), AIC (Antenna-based Instrumental calibration), PC (RF Passband calibration), APC (Antenna-based RF Passband calibration), DD (Data Descriptor) ... - DUMP DATA : lists the data associated parameters. - DUMP FILE : lists information about the input and output file - DUMP INDEX : lists information about the current index. - DUMP CONTINUUM : dumps the continuum data. - DUMP LINE c1 c2 : dumps the spectral data from channel c1 to c2. DUMP LINE c1 c2 /PLOT will plot the spectral data amplitude as a function of channel number. - DUMP VIRTUAL : gives the virtual memory and paging file quotas. DUMP DATA, DUMP LINE and DUMP CONTINUUM will give the phase-corrected or uncorrected data, depending on the last SET PHASE ATM or SET PHASE NOATM command issued. 1 FILE CLIC\FILE [Type] [Name] [NEW] [SHARED] [/WINDOW] [/DIRECTORY] Selects the input and output files. FILE IN name defines the input file FILE OUT name [NEW] defines the output file ; initializes a file if NEW is precised. FILE BOTH name selects the same file for input and output. FILE RAW [proj] [date] open a raw data file The default extension can be specified using command SET EXTENSION (.ipb is recommended for files containing data, .hpb for files containing only headers). If the 'Type' is not RAW, with option /WINDOW (if the windowing system is active), a panel window is created and the file name may be selected via a file browser ('name' is then used as a filter). Pressing GO will then open the file. FILE RAW [proj] [date] will select the first file residing in the directories IPB_DATA:, IPB_DATA1:, IPB_DATA2:, ... following the standard name convention used at Plateau de Bure (jj-mmm-yyyy-proj.ipb, or YMJJPROJ.IPB for CDROMs), which matches the optionally given project name and date. The names of all the NFILE files matching the project name and date are put in character array DATAFILE[NFILE] (the integer variable NFILE is also defined). With RAW and option /WINDOW (if the windowing system is active), a panel window is created with a menu to select one of the available files, and two action buttons, one for opening the file, the other for creating a header file for calibration. With RAW and options /WINDOW and /DIRECTORY (if the windowing system is active), a panel window is created with a menu to edit the list raw data file directories (logical names IPB_DATA:, IPB_DATA1:, ...) The character variable SHORT_FILE is available after FILE IN : it contains the file name without directory or extension. On VAX-VMS, FILE IN Name PATCHED will convert the file to VMS format (if it was created under another operating system). 1 FIND CLIC\FIND [Append] [New_Data] [/LINE Lname] [/NUMBER n1 n2] [/SCAN s1 s2 [s3 s4 ...]] [/QUALITY q] [/TELESCOPE Tname] [/PROCEDURE Proc1 Proc2 ...] [/TYPE Type] [/SOURCE s1 s2 ... sn] [/OFFSET o1 o2] FIND performs a search in the input file to build a new index, according to selection criteria defined by the SET command. These criteria may be temporarily modified by the following options : /LINE Lname search by line name /NUMBER n1 n2 search for the specified range of observation numbers /SCAN s1 s2 [s3 s4] search for the specified range(s) of scan numbers /OFFSET a1 a2 search for these offsets /PROCEDURE p1 pn search by procedure name(s) /QUALITY q search for the data of quality better than Q. /SOURCE s1 ... sn search by source name /TELESCOPE Tname search for the specified telescope name /TYPE Type search by source type (OBJECT, PHASE, or BANDPASS) /RECEIVER number search by receiver number FIND /SCAN s1 s2 [s3 s4 ..] will loop across the 9999/0001 border if s1 (s3) is larger than s2 (s4). Using several source names in FIND/SOURCE is now supported. Source name and Line name matching is not case sensitive. The current index is ordered by scan number or receiver number depending on the last command SET SORT. However the scan ordering is done modulo 9999 (i.e. the time order is respected if the 9999/0001 transition occurs in the current index). FIND by default overwrites the current index. Found observations may be appended to the current index by specifying the argument APPEND ; an index compression occurs to avoid duplication of scans in the index. FIND does not return an error if the index is empty, but the variable FOUND is set to 0. FOUND is always set to the number of observations in the index. Argument NEW_DATA can be used to wait until new data is present in the input file. This possibility is intended for sites where data acquisition is done in CLIC format (Plateau de Bure) to use CLIC as an automated quick look facility. The behaviour is similar to that of command NEW_DATA, but all selection criteria are considered and no switching to a new observation type occurs. 1 FITS CLIC\FITS name Create for each selected line subband, a FITS file containing the spectral data. For autocorrelation data the data from all antennas are averaged. For correlation data, the complex data form all baselines are averaged and the real part of the resulting visibility is used. The fits file names are e.g. name-l01.fits, name-l02.fits, name-l03.fits (one fits file is created for each subband), if one has specified SET SUBBAND l01 l02 l03. 1 FLAG CLIC\FLAG f1 f2 ... /ANTENNA i1 [...] [/BASELINE b1 [...]] [/RESET] Flag the current record (obtained by GET /RECORD) with flags f1 ... Flags may be relative to antennas or baselines. /ANTENNA or /BASELINE must be given, with lists of antenna numbers or baseline names as arguments. /ANTENNA ALL will flag all antennas, /BASELINE ALL will flag all baselines. These are the default. Supported flag names are: - C01 to C10 for bad individual continuum correlator subbands - L01 to L06 for bad individual spectral correlator subbands - DATA for bad data - TSYS for too high system temperature (antenna based only) - LOCK for out of lock local oscillator (antenna based only) - POINTING for poor pointing (antenna based only) - SHADOW for antenna being shadowed by another antenna (antenna based only) - SATURATION for too high total power on a particular antenna. Use option /RESET to suppress flags that were accidentally set. Give FLAG with no argument (but with options) to list the flags of the current record. Use command UPDATE to write the flagged data to disk. If more than one record is to be flagged, command STORE FLAG should be preferred. 1 GET CLIC\GET [N] [/RECORD r] [/HEADER] GET copies R into T, and loads the Observation number N in R. The current index initialized by FIND is first explored, then, if needed, the whole input file. If N is absent, the previous (last read) Observation is recovered. If N is FIRST, the first Observation of the current index is loaded. If N is NEXT, the next Observation in the current index is loaded. If option /RECORD is present, only record r is loaded. Otherwise, the average record is loaded; it will contain the phase-corrected or uncorrected data depending on the last SET PHASE [ATM]|[NOATM] command. If option /HEADER is present, only the scan header is read. No data record is accessed. This command does not access the data file if only the header file is available. 1 HEADER CLIC\HEADER Displays some header information on current observation. The FULL format is used, with the informations selected in command SET FORMAT written. The lines written contain (in output order, but not all lines are necessarily present) 1. General information line : Observation number and version Scan number Procedure name Source name and type Line name Telescope name Date of observation Date of last reduction 2. Interferometer Configuration line : Number of antennas Station numbers Number of baselines 3. Position information line RA or L : right ascension or longitude (or azimuth) DEC or B : declination or latitude (or elevation) Epoch if equatorial coordinates are used Offsets in current units Type of coordinate (Eq, Ga, Ho) 4. Quality information line : Tau: opacity at zenith Tsys: system temperature (outside atmosphere). Number of records Time: total integration time on source (minutes) El: elevation of source 5. Spectral information lines : N: number of subbands N: number of channels I0: reference channel (real) F0: rest frequency at reference channel Df: frequency resolution (signed) 6. Calibration information line : B_ef: Beam efficiency of telescope F_ef: Forward efficiency of telescope G_im: Gain in image band 7. Calibration status line : Atmospheric calibration done Instrumental calibration done Passband calibration done 8. Pointing corrections line : 9. Atmospheric information lines (2) : H2O_: millimeter of precipitable water vapor Pamb: ambient pressure Tamb: ambient (receiver cabin) temperature Tchop: Chopper temperature Tcold: Cold load temperature Tatm: Atmospheric temperature in the signal band Tau: Zenith opacity in the signal band Tatm_I: Atmospheric temperature in the image band Tau_I: Zenith opacity in the signal band 1 IGNORE CLIC\IGNORE List_of_Observations This command can be used to declare the specified list of Observations (from the INPUT file) to be ignored in all FIND operations. They effectively become invisible to CLIC (except in a LIST IN command), until a FILE IN command is typed again. The input file is not physically modified however. The list of observation may have the same format as the index list of a FOR command. 1 LIST CLIC\LIST [Name] [/SHORT] [/BRIEF] [/LONG] [/FLAG] [/OUTPUT File] [/PROJECT] [/SOURCE] [/VARIABLE var-list [/FORMAT format-list]] [/OFFSET] List header information about an ensemble of observations. LIST is used for a quick look to observation headers, in a more or less detailed format. Name specifies the file to be listed : IN or OUT ; if Name is not present, the current index is listed. A medium-sized format is used by default. /SHORT : Gives only one line for a set of scans with same parameters; IFPB and CALI are not listed. the first and last scan of each group are logged in array S_GROUP[2,N_GROUP], N_GROUP is the number of groups. /BRIEF : Brief format (Observation numbers and version numbers) /LONG : Long format (not allowed for the output file) /OUTPUT File : Send the list to a disk file instead of the terminal /FLAG : list data flags for current index. /PROJECT : list the observing projects in the current index. the number of differents offset positions is in variable N_OFFPOS the offsets are in array OFFPOS[2,N_OFFPOS] /SOURCE : list the observed sources in the current index. the number of differents source is in variable N_SOURCE the source names in character array C_SOURCE[N_SOURCE] /OFFSET : list the observed position offsets for the current index. /VARIABLE varst the content of the header variables in the list. These variables must have been defined by command VARIABLE. If /FORMAT format_list is also given, each variable in the list is printed according to the associated format item. The format items must match the variable types. With option /SHORT, a line is printed only if at least one of the variables has changed, and is preceded by the corresponding scan number range. example: LIST /VARIABLE FREQUENCY LFCEN[2] /FORMAT f10.3 f6.3 /SHORT gives the sky rest frequency and the central IF frequency of subband L02, as a function of scan numbers. To define these variables: use VARIABLE RF and VARIABLE LINE. The list will be ordered by scan numbers or by receiver number, depending on the command SET SORT [SCAN]|[RECEIVER]. 1 MARK CLIC\MARK f1 f2 ... [/ANTENNA i ][/BASELINE ij] [/RESET] Set the antenna or baseline mark words. To decide whether data should be used, CLIC uses the logical OR of the data flag words with the corresponding mark words. Thus data from some subbands may be [temporarily] ignored even if unflagged. Flags may be relative to antennas or baselines. /ANTENNA or /BASELINE must be given, with antenna numbers or baseline names as arguments. Several antennas and baselines may be given simultaneously. Use /ANTENNA ALL or /BASELINE ALL for all antennas or all baselines. Flag names f1 f2 ... are alphanumeric codes. Valid codes are subband names (C01 to C10, L01 to L06), DATA, POINTING, SHADOW, TSYS, SATURATION and LOCK. Use option /RESET to reset flags that were accidentally set in the mark words. MARK with no arguments (just options) will list the MARK words currently in use. 1 MASK CLIC\MASK f1 f2 ... [/ANTENNA i][/BASELINE ij] [/RESET] Set the antenna or baseline mask words Data flagged will normally not be processed by calibration commands. However flags set in the corresponding mask word will be ignored, causing data to be processed anyway. Flags may be relative to antennas or baselines. /ANTENNA or /BASELINE must be given, with antenna numbers or baseline names as arguments. Flag names f1 f2 ... are alphanumeric codes. Valid codes are subband names (C01 to C10, L01 to L04), DATA, POINTING, SHADOW, TSYS and LOCK. Use option /RESET to reset flags that were accidentally set in the mask words. MASK with no arguments (just options) will list the mask words currently in use. 1 MINMAX CLIC\MINMAX This command is used to compute extremal amplitudes in all continuum, line data, USB and LSB. Results are stored in variables C_MAXAMP_U, C_MINAMP_U and variables with similar names. This command may be used in a MODIFY DATA loop, to search for bad data. 1 MONITOR CLIC\MONITOR delta_time This command is used to prepare the atmospheric radiometric phase correction. It processes the calibration scans to compute the correction factors (i.e. the change of path length for a given change in emission temperature of the atmosphere at the atmospheric monitor frequency (normally 1.3 mm). The scans in the current index are grouped in intervals of maximum duration `delta_time' (in seconds); source changes will also be used to separate intervals. In each interval a straight line is fitted in the variation of atmospheric emission as a function of time; this line will be the reference value for the atmospheric correction, i.e. the correction at time t is proportional to the difference between the atmospheric emission at time t and the reference at time t. This scheme is used to avoid contaminating the correction with total power drifts of non-atmospheric origin (changes in receiver noise and gain, and changes in ground noise). MONITOR 0 will use for each scan the average of the atmospheric emission as the reference value. This will cause the correction to average to zero in one scan: the average phase is not changed, only the coherence is restored leading to an improved amplitude. 1 MODIFY CLIC\MODIFY Item [Values...] This is a command to change some parameters relevant to data acquisition, such as baseline values, time, position of phase center, are equal. 2 BASELINE CLIC\MODIFY BASELINE b1 x1 y1 z1 [b2 x2 y2 z2 ...] [/OFFSET 89|96] CLIC\MODIFY BASELINE FITTED Modify the vector coordinates for baseline b1 to be: x1, y1, z1 (meters), and the phases accordingly. Keyword FITTED will load the baseline coordinates the most recenty found by the SOLVE BASELINE command. Use option /OFFSET 96 to enter baseline coordinates offsets instead (i.e. offsets from the new (1996) standard antenna positions in STATION.DAT). For old procedures, referring to the old (1989) station values, use /OFFSET 89 instead. Apply to the current index; an output file must be open (may be equal to the input file). 2 ANTENNA CLIC\MODIFY ANTENNA a1 x1 y1 z1 [a2 x2 y2 z2 ...] [/OFFSET 89|96] CLIC\MODIFY ANTENNA FITTED Modify the vector coordinates for antenna a1 to be: x, y, z (meters), and the phases accordingly. Keyword FITTED will load the antenna coordinates the most recenty found by the SOLVE BASELINE command. Use option /OFFSET 96 to enter antenna coordinates offsets instead (i.e. offsets from the new (1996) standard antenna positions in STATION.DAT). For the old procedures use /OFFSET 89. Apply to the current index; an output file must be open (may be equal to the input file). 2 DELAY CLIC\MODIFY DELAY a1 d1 [a2 d2 ...] [/OFFSET] Modify the delay for antenna a1 to be: d1 (nanoseconds), and recompute the phases accordingly. Use option /OFFSET to enter delay changes with respect to the precious values. Applies to the current index; an output file must be open (may be equal to the input file). 2 FLUX CLIC\MODIFY FLUX value Modify the flux of the calibrator as stored in the header. In case the calibrator is to be used to calibrate amplitudes, the calibrator amplitude will be divided by this number before plotting. (use SET AMPLITUDE SCALED to do this). Apply to the current index; an output file must be open (may be equal to the input file). 2 FOCUS CLIC\MODIFY FOCUS antenna1 value1 antenna2 value2 ... Correct the phases for the offsets in focus, introduced to optimize efficiency. A1 is the antenna number, value1 the focus offset in mm, and so on. The phases are normally corrected in real time since 29- nov-1996. Between 29-may-1996 and 29-nov-1996, the focus corrections were logged in the data files. Before 29-may-1996 they are only in the log-obs files. However between 29-nov-1996 and 02-apr-1998, the correction had wrong sign for the few projects using HIGH LOCK. So use MODIFY FOCUS with NO arguments for data more recent that 29-nov- 1996: this should correct the HIGH LOCK problem. Between 29-may-1996 and 29-nov-1996, MODIFY FOCUS with no arguments will use the focus offsets in the header and apply the corresponding phase offsets. For older data you may now search for the focus changes in the log files to apply the phase corrections before calibration; or use jumps in the phase calibration just as you had done before. This command applies to the current index; an output file must be open (may be equal to the input file). 2 SCALE CLIC\MODIFY SCALE amplitude phase Multiply all data in the current index by this (complex) scale factor (in case of emergency only!). Apply to the current index; an output file must be open (may be equal to the input file). 2 DOPPLER CLIC\MODIFY DOPPLER Computes the Doppler velocity correction, in case it was not taken into account at the time of observing. The LO2 frequency in the header is assumed to be the frequency actually used. A warning is issued if the LO1 frequency in the header is not coherent with the LO2 frequency (which means the phase tracking might be in error, since it uses that LO1 frequency). The frequencies and line names introduced by SET FREQUENCY are used to define the velocity scales for each subband/sideband. A related command is MODIFY OBJECT wich change the type of observations from PHASE to OBJECT, before computing the Doppler velocity correction, as in MODIFY DOPPLER. 2 FREQUENCIES CLIC\MODIFY FREQUENCIES The frequencies and line names introduced by SET FREQUENCY are used to re-define the velocity scales for each subband/sideband. By default, the frequency and line name entered in OBS for at data aquisition on the Plateau de Bure is used for all sidebands and subbands. 2 OBJECT CLIC\MODIFY OBJECT This command changes the type of PHASE observations (Phase and Passband calibrations) to tho OBJECT type, then computes the Doppler velocity correction, as for MODIFY DOPPLER. The LO2 frequency in the header is assumed to be the frequency actually used. A warning is issued if the LO1 frequency in the header is not coherent with the LO2 frequency (which means the phase tracking might be in error, since it uses that LO1 frequency). The frequencies and line names introduced by SET FREQUENCY are used to define the velocity scales for each subband/sideband. 2 POSITION CLIC\MODIFY POSITION EQ epoch R.A. Dec. Modify the source (phase center) position. This precesses the phase accordingly. Note that this cannot change the antenna pointing center. Typical use of this command is to correct positions of inaccurate phase calibrators. 2 TIME CLIC\MODIFY TIME DUT1 Modify the time constant DUT1 (in seconds) . For very high accuracy astrometry, DUT1 may need to be adjusted afterwards to correct for irregularities for the earth rotation. The "a priori" estimates may be wrong. Another case is the leap second, if they are introduced asynchronously with the DUT1 constant... 2 REFERENCE CLIC\MODIFY REFERENCE UPPER|LOWER r1 r2 r3 r4 The reference channels in the available line subbands are changed to the new values. Use with caution: this command is actually changing the frequency and velocity scale of your data. 2 VELOCITY CLIC\MODIFY VELOCITY UPPER|LOWER v1 v2 v3 v4 The reference velocities in the available line subbands are changed to the new values. Use with caution: this command is actually changing the frequency and velocity scale of your data. 2 HEADER CLIC\MODIFY HEADER procedure This is a general command to edit the header of the scans in the current index.. CLIC enters a loop in which all the headers are read successively. For each header the procedure 'procedure' (default extension ".CLIC") is executed. This procedure may only contain the following commands : DUMP, HEADER, GO, or any SIC command that acts on variables. The command GO [WRITE] must end the procedure. With GO WRITE, the scan header will be updated; with only GO, the scan header is not updated and CLIC loads the next scan header in the current index. If no GO command in excountered in the procedure, the loop is aborted. If a PAUSE command is found in the procedure, the PAUSE is executed, but the prompt changes to "MODIFY>". The same commands as above may then be executed from the keyboard; "QUIT ALL" may be used to abort the loop. 2 DATA CLIC\MODIFY DATA procedure This is a general command to edit the data headers of the scans in the current index. CLIC enters a loop in which all the data header of all records of all scans in the current index are read successively. For each record the procedure 'procedure' (default extension ".CLIC") is executed. This procedure may only contain the following commands : DUMP, HEADER, FLAG, MINMAX, GO, or any SIC command that acts on variables. The command GO [WRITE] must end the procedure. With GO WRITE, the data record will be updated; with only GO, the data record is not updated and CLIC loads the next record from the current index. If no GO command in excountered in the procedure, the loop is aborted. If a PAUSE command is found in the procedure, the PAUSE is executed, but the prompt changes to "MODIFY>". The same commands as above may then be executed from the keyboard; "QUIT ALL" may be used to abort the loop. 2 PHASE_SIGN CLIC\MODIFY PHASE_SIGN Change the sign of all phases of the data in the current index. This command is intended for recovering data taken in a preliminary status of the new correlator software. 2 AXES CLIC\MODIFY AXES a1 x1 [a2 x2 ...] Correct the phases for the offset of the elevation axis with respect to the azimuth axis. This effect, if different for differnt antennas, causes a phase offset proportional to frequency and to the cosine of elevation. a1 is the antenna number, x1 the offset between axes in meters. The actual values should be at most 1 mm, and may be measured using the command SOLVE BASELINE, using SET X ELEVATION in addition to Hour angle and declination. 2 BUG CLIC\MODIFY BUG number This command is reserved for the correction of nasty bugs in the data acquisition, and worthwhile. The number is used for identification. Current accepted values: - 1 Affecting data taken between 11-nov-1995 and 09-jan-1996. Bug in RDI found by S. Guilloteau. The continuum data was erroneously calibrated in the real-time aquisition. As result, the continuum data did not agree with the average of the spectral data. For instance plotting data with "set sub C02 L02" as a function of time gives different results for C02 and L02. The result would affect line intensities if, as is usually the case, the amplitude calibration is done with the continuum subbands. Correction: the current index should contain both atmosphere calibrations and correlation data; the data file should be open for both input and output. This command should not affect data taken before 11-nov-1995 and after 09-jan-1996; be careful for the last day since the hour is not checked, and RDI was corrected at 3pm. 1 NEW_DATA [CLIC\]NEW_DATA [time] [tries] Waits until new data has been written to the input file, then makes a new index from all new data. The type of observation can be changed by this command, but the index will contain only observations of one type. Selection criteria defined by command SET are ignored. This command can be used to make a quick look or analysis of data produced by a real time acquisition system. Caution : only two programs should access the input file simultaneously, one for writing the other for reading. The first argument is the time interval between two consecutive inspections of the file index; the second is the allowed number of unsuccessful attempts to find new data in the file. The defaults are 10 seconds and 12 tries (two-minute timeout). 1 PLOT CLIC\PLOT keyword [/NOFRAME [pen]] [/RECORD list] [/APPEND] [/IDENTIFY] [/RESET] Plot data according to options selected by CLIC\SET command. PLOT will clear the screen before plotting (the default with PLOT ALL and PLOT FIRST), while PLOT /NOFRAME will only plot the data itself, in the same boxes, optionally using a different pen (useful to overlay plots). Parameters: CLIC\PLOT [ALL] Erases the screen and plots all data in the current index (default). CLIC\PLOT FIRST Plots data from the first observation in the current index. CLIC\PLOT NEXT Plots data from the next observation in the current index. CLIC\PLOT number Plots data from the observation of the given number (must be in the current index). CLIC\PLOT SAME Plots again the last plotted buffers (with possibly new options, such as line type, limits, ...). CLIC\PLOT /NOFRAME [pen] Do not erase the screen, and plots data in the present boxes, optionally with a new pen. This may be used for comparing data or in conjunction with PLOT /APPEND. CLIC\PLOT /RECORD list will plot only some records for the observation(s). "list" is of the format n1 to n2 n3 n4 to n5, as with SIC\FOR command. CLIC\PLOT /IDENTIFY [COLOUR] will plot a different GREG symbol for each source (if SET PLOT POINT is currently active). Using optional argument COLOUR will produce points differing by colour rather than by symbol shape. CLIC\PLOT /RESET Reset the time origin (and, by consequence, the time-dependent amplitude and phase calibration curves) before plotting. CLIC\PLOT /APPEND will not reset the previous buffers before reading data and plotting. This may be used at the Plateau de Bure for incrementally plotting new data just after it is written on disk. 1 PRINT CLIC\PRINT parameter Prepares a procedure for further use. CLIC\PRINT BASELINE Prepares a procedure to be used in OBS to enter the most recently fitted baseline parameters. This procedure also contains (but commented out) the CLIC\MODIFY command to edit previous data to the same fitted baseline parameters. CLIC\PRINT DELAY Prepares a procedure to be used in OBS to enter the most recently fitted delay parameters. CLIC\PRINT FLUXES Prepares a procedure to be used in CLIC to re-enter the most recently determined source fluxes. 1 RESIDUALS CLIC\RESIDUALS Item Clear the graphic screen and plot the residuals from last SOLVE command. Item can only be "BASELINE" up to now. 1 SAVE CLIC\SAVE Name [STILL UNIMPLEMENTED] SAVE creates a procedure file of name "Name.clic", containing all the current parameters of the program. This file may be executed at any time using the @ command : just type "@@ name" after the CLIC> prompt, or pass "@ name" as a parameter when invoking CLIC (by typing "CLIC @ name"). This file is composed of standard CLIC commands, and may be edited with any text editor. 1 SET CLIC\SET something [value1 [value2 [...]]] This command is used to set a value for a CLIC parameter. If no value argument is given, the default will be restored. 2 AMPLITUDE CLIC\SET AMPLITUDE ABSOLUTE|RELATIVE|SCALED [KELVIN|JANSKY] [BASELINE|ANTENNA] This command decides which scaling factor is applied to the data for plotting and writing the final Table, in subsequent PLOT and TABLE commands: - ABSOLUTE means that the relative amplitude calibration is not applied; - RELATIVE means that the relative amplitude calibration, as determined with SOLVE AMPLITUDE, and stored with STORE AMPLITUDE, is applied; - SCALED means that the absolute amplitude is divided by the source flux - ANTENNA|BASELINE switches between Antenna-based and Baseline-based amplitude calibrations. This switch will be active for SOLVE AMPLITUDE (calibration curve determination), STORE AMPLITUDE (calibration curve store operation), and SET AMPLITUDE RELATIVE (for application). Both baseline-based and antenna-based calibration curves may be stored alongside in the data header, independently of each other. SCALED is only used for the command SOLVE AMPLITUDE (this command actually forces SET AMPLITUDE SCALED KELVIN). The second keyword indicates if conversion between Janskys and Kelvins is to be done. With SET AMPLITUDE ABSOLUTE, the amplitudes are normally in Kelvins of main-beam brightness temperature, so the default is KELVIN. With SET AMPLITUDE RELATIVE, the amplitudes are in Janskys, since a calibrator of known flux has been used for reference. The default is then JANSKY. If the default is overridden (SET AMPLITUDE ABSOLUTE JANSKY or SET AMPLITUDE RELATIVE KELVIN), conversion factors are taken from the scan headers; these factors may be determined by SOLVE FLUX, and stored by STORE FLUX. 2 ANGLE CLIC\SET ANGLE Unit Specify the angle unit for offsets. May be R[adian], D[egree], M[inute of arc], S[econd of arc]. Default is MINUTE. The ANGLE unit is also used to display Continuum drifts. 2 ANTENNAS CLIC\SET ANTENNAS [a1 a2 ...] CLIC\SET ANTENNAS ALL Selects the antennas for which data will be displayed by command PLOT. Valid antennas are currently 1, 2, and 3. This command is exclusive with commands SET BASELINES and SET TRIANGLES. Parameters which may be displayed in this antenna-mode are obvious antenna based parameters such as cable phase, LO-phase and rate, ... with SET Y AMPLITUDE and when more than 3 antennas are available in the data, antenna amplitude is computed by averaging all possible "triangular ratios" of baseline amplitudes. with SET Y PHASE a phase is attributed to each antenna by setting the phase of antenna 1 to zero, and making use of closure relations for other antennas (least square fit). This is useful for fitting baselines for instance (it enables one to determine directly antenna position offsets). SET ANTENNA with no other antenna selects all antennas used for the baselines previously in use. SET ANTENNA ALL will select all the antennas available in the first scan of the current index, for each command accessing the data (e.g. PLOT). This is now the default. 2 AVERAGING CLIC\SET AVERAGING mode Selects averaging of data plotted (the data in the file is unaffected). 1. NONE : all data points are plotted 2. SCAN : data is averaged within each scan; on point is plotted per scan. 3. TIME dt : data is averaged in time intervals of length dt (seconds). Data of consecutive scans is NOT averaged together. 4. METHOD VECTOR : complex visibilities are averaged as complex numbers. 5. METHOD SCALAR : amplitude and phases of visibilities are averaged separately. See also SET BINNING for another way of averaging data. 2 ASPECT_RATIO CLIC\SET ASPECT_RATIO value [AUTO|EXACT] Choose a default aspect ratio (x_size/y_size) for boxes plotted by command PLOT. If several boxes must be plotted (depending on subbands, baselines, or side bands selected), the plot page will be partitioned in order to: i) in AUTO mode: approach this aspect ratio for each box while filling the whole page ; ii) in EXACT mode: use this aspect ratio for each box (part of the plot page will be left blank). The default is 2.0 AUTO. 2 ATMOSPHERE CLIC\SET ATMOSPHERE argument value [/RECEIVER i] Selects the way atmospheric calibration is done by command ATMOSPHERE. Argument may be FILE, AUTO, TREC, or MANUAL. - In FILE mode the actual mode is taken from the data header, as given in the OBS program. - In TREC mode the receiver temperature is assumed known, to set the scale of measured sky temperature and optical depth, and determine the system noise temperature. The receiver temperature is taken from the data header, as given in OBS. It may be forced to a different value by giving it as second argument 'value', or by the SET TREC command. - In AUTO mode the water wapor content is assumed known; it is determined from the antennas in TREC mode, if any, or taken from the data header, or forced to the value given in the second argument 'value', or by the SET WATER command. These parameters, together with the wheather station data, are used to compute the system noise temperature for each antenna. In MANUAL mode, no model atmosphere is used, but the values of optical depths and atmospheric temperatures stored in the data. 2 BANDS CLIC\SET BANDS b1 b2 ... Selects the sidebands for which data will be displayed by command PLOT. Valid codes are currently "UPPER", "LOWER", "AVERAGE", "DIFFERENCE", and "RATIO". In "AVERAGE", "DIFFERENCE" or "RATIO" modes, the sidebands visibilities are combined after correction for their relative phases, as determined by the RF bandpass calibration. If no RF bandpass calibration is available (i.e. stored with the data), the relative phases are obtained by averaging the continuum subbands (which is useless if no continuum emission is detected). 2 BASELINES CLIC\SET BASELINES [b1 b2 ...] CLIC\SET BASELINES ALL Selects the baselines for which data will be displayed by command PLOT. Valid codes are currently "12", "13", "23". This command is exclusive with commands SET ANTENNAS and SET TRIANGLES. SET BASELINE with no other antenna selects all baselines connecting the antennas previously in use. SET BASELINE ALL will select all the baselines available in the first scan of the current index, for each command accessing the data (e.g. PLOT). This is now the default. 2 BINNING CLIC\SET BINNING size position CLIC\SET BINNING OFF Selects data averaging in bins of the parameter in the X coordinate array. Bins are defined by the size of intervals, and the position of one of the intervals (in units of the X coordinate). SET BINNING OFF will turn this mode off. Note that this averaging in bins occurs AFTER the averaging selected by SET AVERAGE (normally use SET AVERAGING NONE). SET BINNING is particularly useful for plotting data as a function of UV coordinates. A command SET X used to change the X units will automatically reset the binning OFF. 2 CLOSURE CLIC\SET CLOSURE b1 w1 b2 w2 ... Select weights to be used for each baseline in using the closure relations. (this is done by a least squares resolution of an overdetermined system, in antenna mode). You may wish to give more weight to the shorter baselines. Default weights are equal. 2 CRITERIA CLIC\SET CRITERIA /DEFAULT Reset all the search criteria for command FIND to their default values. All the observations in the file will be found. 2 /DEFAULT CLIC\SET [CRITERIA|ALL] /DEFAULT Select the default values for all the parameters, or for selection criteria only. 2 DATA CLIC\SET DATA np nb Extend the size of the plot buffers to contain nb boxes of np points each. 2 DEFAULT CLIC\SET DEFAULT (or SET /DEFAULT) Reset all the SET parameters to their default values. 2 DROP CLIC\SET DROP low high Give the fraction of the passband to be left out at the low-frequency and at the high frequency ends of each spectral correlator subband. This is used by further PLOT and TABLE commands. The default is 5% of the bandwidth at both ends. 2 ERRORS CLIC\SET ERROR NOISE|ATMOSPHERE Controls the way the error bars for phase plots in time mode are computed. - with NOISE the errors are computed according to the system noise only. - with ATMOSPHERE the rms phase fluctuations as measured when compressing the data, are included in the error bars. 2 EXTENSION CLIC\SET EXTENSION string Use 'string' as the default extension for the FILE command. The default is ".ipb". Other possible values are ".ipb-raw", ".ipb-comp", ".ipb-cal", and ".ipb". 2 FLUX CLIC\SET FLUX name value [frequency] [date] [/RESET] Enters `value' as the flux of source `name' (in janskys). The flux of reference sources must be entered in CLIC, as an input to command SOLVE FLUX. If the flux of a source is entered by SET FLUX, this source will be a reference source for determining the antenna efficiencies, and the fluxes of other objects. After CLIC\SET FLUX name *, source `name' will not be a reference source any more. Its flux may then be re-determined by a subsequent SOLVE FLUX command. Use command SHOW FLUX to list the fluxes known to the current CLIC session. One may optionally enter a frequency (in GHz) and a date (jj-mmm-yyyy). The frequencies and dates are checked in that case by STORE FLUX and SOLVE FLUX. Matching is within 1 GHz for frequencies and 1 week for dates. If /RESET is given, all entries with the given source name are deleted from the flux list. SET FLUX ALL /RESET will empty the flux list. 2 FORMAT CLIC\SET FORMAT type Set the format of the title of observations plotted. The same format is used by the LIST command. The format may be BRIEF (Observation number and version, Source name, Line name, Telescope name and position offsets), LONG or FULL which is similar to the long format, but also displays the list of original Scans. The default is BRIEF. FULL format is always used for command HEADER. Other keywords can be specified to indicate which type of information should be written for the LONG and FULL formats. This is done by command CLIC\SET FORMAT Keyword [ON] [OFF] (ON to write the information corresponding to the specified keyword, OFF to ignore it). The keywords are - INTERFEROMETER for the number of antennas, baselines, .. - POSITION for position of the source, offsets, type of coordinates and Epoch - QUALITY for the Opacity, System temperature, Elevation, Integration time. - SPECTRAL for the number of subbands, channels, reference channel, rest frequency, frequency resolution. - CALIBRATION for the beam and forward efficiencies and the gain image ratio. - STATUS for the status of different possible calibration operations. - ATMOSPHERE for the water vapor content, pressure, temperatures and opacities in signal and image bands. A line of general information is always written in any case. 2 FREQUENCY CLIC\SET FREQUENCY subband sideband name freq CLIC\SET FREQUENCY ALL name freq Select the line name and frequency to be used to define the velocity scale, in spectral-mode plots, for the given sub-band and sideband. 'subband' may be C for continuum or L01 to L04 for spectral correlator subbands; 'sideband' must be either USB or LSB; 'name' is a (max. 12 character) mnemonic for the line name; 'freq' is the rest frequency in MHz. If the line name is '*', then the default frequency entered prior to the observation will be used to compute the velocity scale for the corresponding sub-band. This information will be used by all subsequent SPECTRUM and MODIFY DOPPLER commands. SET FREQUENCY ALL will fill in the given frequency for all subbands. 2 GAIN_IMAGE CLIC\SET GAIN_IMAGE value /ANTENNA i Give the value of the relative gain for the receiver image side band, to be used by the command ATMOSPHERE. Use * instead of the value to force the use of the numbers stored in the file. 2 GIBBS CLIC\SET GIBBS number Give the number of channels to be masked on each side of the central frequency, for the correlator subbands which are obtained by juxtaposition of both sidebands of a common (third) local oscillator. Due to the Gibbs effect, a few channels are corrupted by a contribution of the image sideband of the first local oscillator, which may contain signal if the source has continuum emission. This is used by further PLOT and TABLE commands. The default is 0, which is relevant for line sources with no continuum emission. 2 HOUR_ANGLE CLIC\SET HOUR_ANGLE first last FIND will select all observations with hour angles in the specified range (in hours). Default is * * (no selection by Hour Angle). 2 IC CLIC\SET IC status FIND will select observations according to the status of Instrumental (Phase) Calibration (IC). 'status' may be YES to select observations already calibrated, NO to select still uncalibrated observations, * to disregard this selection criterion. 2 LEVEL CLIC\SET LEVEL number Set the threshold severity level for messages to be output on the terminal. A reasonable value is 4. 2 LINE CLIC\SET LINE NAME FIND will select all observations according to the specified line name. Default is *. A syntax like NAM* can be used to find observations with line names beginning by NAM. 2 MODE CLIC\SET MODE type Selects which kind of data are displayed. "type" stands for TIME or SPEC. In TIME mode, the underlying parameter is time, i.e. two time-dependent parameters are plotted one against each other, for instance phase versus time, or amplitude versus hour-angle. In SPECtral mode, the underlying parameter is frequency, for instance amplitude versus velocity. 2 NUMBER CLIC\SET NUMBER n1 n2 FIND will select all Observations with numbers between n1 and n2. Default is * *. 2 OBSERVED CLIC\SET OBSERVED d1 d2 FIND will select all Observations with observing dates between d1 and d2. Default is * *. d1 and d2 are normally in explicit form (jj-mmm- yyyy) but internal day numbers are also accepted (i.e. something like SET OBSERVED DOBS-1 DOBS+1 is possible). 2 OFFSETS CLIC\SET OFFSETS o1 o2 FIND will select all observations with offsets between o1 and o2. Default is * *. 2 PC CLIC\SET PC status FIND will select observations according to the status of RF Passband Calibration (PC). 'status' may be YES to select observations already calibrated, NO to select still uncalibrated observations, * to disregard this selection criterion. 2 PHASE CLIC\SET PHASE [ABSOLUTE|RELATIVE] [ANTENNA|BASELINE] [DEGREES|RADIANS] [JUMPY|CONTINUOUS] [ATMOSPHERE|NOATMOSPHERE] [FILE|NOFILE] [INTERNAL|EXTERNAL] CLIC\SET PHASE [ABSOLUTE|RELATIVE] This command decides which phase correction is applied to the data for plotting and writing the final Table, in subsequent PLOT and TABLE. ABSOLUTE means do not use the phase calibration determined by the SOLVE PHASE command, RELATIVE means apply it. CLIC\SET PHASE ANTENNA|BASELINE Switch between Antenna-based and Baseline-based phase calibrations. This switch will be active for SOLVE PHASE (calibration curve determination), STORE PHASE (calibration curve store operation), and SET PHASE RELATIVE (for application). Both baseline-based and antenna-based calibration curves may be stored alongside in the data header, independently of each other. CLIC\SET PHASE [ATMOSPHERE|NOATMOSPHERE] Switch ON and OFF the atmospheric phase correction. The atmospheric phase correction is based on monitoring the atmosphere water vapor emission using the 1.3 mm receivers. The correction parameters are in the atmospheric monitor header section, and are computed by commands MONITOR or ATMOSPHERE (this is normally done in real time for data taken since November 1995). However the command MONITOR should still be used to precise the reference for the correction (see command MONITOR). With SET PHASE ATMOSPHERE the phase-corrected spectral data, if available, will be used. Note that the phase correction will NOT be applied if it has been declared invalid for a given scan, using the command STORE CORRECTION BAD or AUTO, except if SET PHASE NOFILE is in effect. See these commands. CLIC\SET PHASE [FILE|NOFILE] Turn ON of OFF the effect of the STORE CORRECTION command. - If SET PHASE ATMOSPHERE FILE, the information on the validity of the phase correction declared by STORE CORRECTION BAD or AUTO, will be used, and the phase correction will be done only on scans validated by STORE CORRECTION. - If SET PHASE ATMOSPHERE NOFILE, this information will be bypassed, and the phase correction will be done for all scans. CLIC\SET PHASE [INTERNAL|EXTERNAL] Switch between two modes of phase calibration. INTERNAL is the standard mode (default). In EXTERNAL mode the calibration curve from another receiver may be used (as stored by STORE PHASE /RECEIVER r). On the top of this a second order calibration curve may be determined (using SOLVE PHASE) and stored as usual. This does not erase any INTERNAL calibration curve previously stored. for example, using receiver 2: SET PHASE INTERNAL RELATIVE: use the phase curve determined from rec. 2 only SET PHASE EXTERNAL ABSOLUTE: use the phase curve from rec 1 only, as stored with STORE PHASE /RECEIVER 1 SET PHASE EXTERNAL RELATIVE: use the phase curve from rec 2, determined on top of the phase curve from receiver 1, by using SOLVE PHASE and STORE PHASE with SET PHASE EXTERNAL in effect. CLIC\SET PHASE arguments ... Selects the way phases are determined. With arguments DEGREES the phases are expressed in degrees of angle, with RADIANS in radians ; with argument JUMPY no attempt is made to suppress 2pi jumps : the determination is always [-pi,pi] ; while with argument "CONTINUOUS n", the phase jumps are limited to +/- pi, that is the phase is always chosen in the range [previous-pi,previous+pi]; n being the number of points averaged together to estimate the 'previous' phase (default is 1, higher values are to be used in noisy cases). 2 PLANET CLIC\SET PLANET *|P|S [Limited help available] Planet model to be used by SOLVE FLUX * = default (elliptical disc) P = same with primary beam attenuation S filename : use data in file filename 2 PLOT CLIC\SET PLOT type Selects the way the data are displayed. "type" stands for LINE, POINTS, HISTOGRAM, or BARS. In POINTS type, the current GreG marker is used. In BARS type (valid only for the visibility data), 1-sigma error bars are drawn. 2 PROCEDURE CLIC\SET PROCEDURE p FIND will select observations done under procedure 'p'. This may be: CORRELATION, AUTOCORR, ONOFF, CALIBRATE, POINTING, FOCUSSING, IF_PASSBAND, DELAY, or GAIN_RATIO. SET PROCEDURE * will disable procedure as a selection criterion. 2 PROJECT CLIC\SET PROJECT n FIND will select observations done fro Observing Project number n. Project numbers are positive integers. SET PROJECT * will disable project number as a selection criterion. 2 QUALITY CLIC\SET QUALITY q FIND will select only observations of quality better than Q (i.e. less than Q). When originally written, unless the real time acquisition system detected a severe problem, all observations have quality 0, a priori the best. The quality flag of an observation can be changed using the TAG command. See HELP TAG for the recommended quality scale. 2 RANGE CLIC\SET RANGE West East South North FIND will select all observations with offsets in the specified range. Default is * * * *. 2 RECEIVER CLIC\SET RECEIVER number|* Use the receiver number as a selection criterion. The default is SET RECEIVER * : observations with both receivers will be selected. 2 RECORD CLIC\SET RECORD list Will force all further PLOT commands to use only the records as given in the list (e.g. r1 r2 r3 to r4 by r5 ...). Very seldom needed. Use SET RECORD 1 to 1000000 to reset it. 2 REDUCED CLIC\SET REDUCED d1 d2 FIND will select all observations with reduction dates between d1 and d2. Default is * *. 2 REFERENCE CLIC\SET REFERENCE antenna_number Enter the logical number of the antenna used as reference for antenna- based calibrations (both RF passband and phase calibrations). Default is 1. 2 RF_PASSBAND CLIC\SET RF_PASSBAND [ON|OFF] [CHANNEL|FREQUENCY] [FILE|MEMORY] [ANTENNA|BASELINE] ON|OFF : switch on or off the application of RF passband calibration curve in plotting the data. The RF passband calibration curve is solved for by SOLVE RF_PASSBAND and stored with the data by STORE RF_PASSBAND. Subsequent PLOT commands will use or not this curve according to the status of SET RF_PASSBAND, which is displayed with the plot. CHANNEL|FREQUENCY : use either the channel dependent passband curves or the frequency dependent passband curve. The channel- dependent passband curves must be determined separately for each subband (continuum and spectral), while the frequency- dependent passband curve is determined by using SOLVE RF_PASSBAND on the continuum correlator, and is used for both the continuum and spectral correlators (this will not work for data taken before July 14th 1990). MEMORY|FILE : use either the passband curves just determined by SOLVE RF_PASSBAND, and still [resent in the program memory, or the passband curves previously stored in the data headers of the input file by a previous command STORE RF_PASSBAND. ANTENNA|BASELINE : Switch between Antenna-based and Baseline-based RF passband calibrations. This switch will be active for SOLVE RF (passband determination), STORE RF (passband store operation), and SET RF ON (for passband application). Both baseline-based and antenna-based calibration curves may be stored alongside in the data header, independently of each other. 2 SCAN CLIC\SET SCAN s1 s2 [s3 s4 ...] FIND will select all observations with Scan numbers between s1 and s2, or s3 and s4 .... The Scan number, attributed by the on-line acquisition system may be different from the observation number which is used by CLIC to refer to the observations. Default is * *. 2 SELECTION CLIC\SET SELECTION mode band subband-range [FREQ freqout] /WINDOW fmin fmax [fmin2 fmax2 ...] Choose the type of data selection to be done by command TABLE, which creates a UV data Table for mapping software. - The first argument 'mode' may be CONTINUUM or LINE, to prepare single channel or multiple channel maps. - The second argument is the sideband to be used, UPPER or LOWER, or DSB. DSB may be used in conjunction with CONTINUUM: in this case, two separate visibility points are written, one for each sideband. DSB used in conjunction with LINE means that the side band will be selected to match the desired frequency range (as given in the command TABLE), thus allowing to mix in the same table data from USB and LSB, if different frequency setups have been used in different configurations. - The third argument is a subband range as for SET SUBBANDS command. In Continuum mode subbands are averaged, in spectral mode they are combined to produce a single spectrum. The syntax is, e.g. SET SELECTION n1 TO n3 to include subbands from n1 to n3; or SET SELECTION n1 TO n3 and n4 to include subbands from n1 to n3 and subband n4. The default is : SET SELECTION CONTINUUM, DSB, L01 TO L06 Arguments "FREQ freqout" are used only for CONTINUUM tables. They define the frequency (in MHz) used for mapping purposes. U and V (for each side band in DSB mode) will be scaled to this frequency. This is intended to combine maps obtained in continuum at slightly different frequencies. The default for freqout will be the actual observing frequency, or the frequency used for previous data if data is appended to a previously existing table by the TABLE command. Option /WINDOW is used to avoid spectral lines when producing a continuum table from spectral correlator data. The first two rest frequencies (in MHz) give the first frequency window in which data is to be used, the next two give the second frequency window, ... etc. 2 SPECTRUM CLIC\SET SPECTRUM ON|OFF Switch on or off the automatic processing of data by command PLOT. If SPECTRUM is ON, all quasi real time processing that is normally done by SPECTRUM command will be done by command PLOT while reading the data. Note that, like in command SPECTRUM the result will depend on the order at which the data is read; ideally the data should be read in the natural time order. 2 SOURCE CLIC\SET SOURCE name1 name2 ... namen FIND will select all scans according to the specified source names. Default is *. Syntax like NAM* can be used to find all observations with source name beginning by NAM. 2 SORT CLIC\SET SORT RECEIVER|SCAN The output of LIST and LIST/SHORT may be sorted primarily be receiver number or scan number. Use SET SORT to switch between the two modes. 2 STEP CLIC\SET STEP t_step Select the time interval parameter to be used by the SOLVE PHASE and SOLVE AMPLITUDE command (time interval between knots of the cubic spline functions). Value is in hours (default 3 hours). 2 SUBBANDS CLIC\SET SUBBANDS n1 n2 ... [/WINDOW f1 l1 f2 l2 ...] CLIC\SET SUBBANDS ALL CLIC\SET SUBBANDS EACH CLIC\SET SUBBANDS LINE|CONT Selects the subbands for which data will be displayed by command PLOT. Valid codes are continuum subbands numbers (C01, C02, ... C10) or line subbands numbers (conventionnaly named L01, L02, L03, and L04 : use L01 if only one subband is present in the data, L01 and L02 if two subbands are present in the data, L01, L02, L03 and L04 if 4 subbands are present in the data). Subbands may be grouped by typing: SET SUBBANDS n1 to n2 and n3 n4 ... where two quantities will be plotted, the first being either the average of actual subbands n1 to n2 and n3 (in Time Mode), or the concatenation of spectral data from subbands n1 to n2 and n3 (in Spectral Mode); the second being subband n4. the first scan of the current index, for each command accessing the data. The subband are concatenated (equivalent to e.g. SET SUBBANDS l01 to l06). the first scan of the current index, for each command accessing the data. The subband are NOT concatenated (equivalent to e.g. SET SUBBANDS l01 l02 l03 l04 l05 l06). SET SUBBANDS LINE|CONT will switch all subbands to their line/continuum counterpart, e.g. L01 to L04 will be changed to C01 to C04 by SET SUBBBANDS CONT (note that this is also automatically done by switching from spectral mode to time mode). Use /WINDOW to give first and last channels to be used for line subbands in TIME mode. In this case line data will be integrated in the given window. For example SET SUBBANDS L01 L02 /WINDOW 1 10 1 10 will plot data from the first ten of the first line subband, as a first quantity, and data from the first 10 channels of the second line subband, as a second quantity. In spectral mode the window limits may be used to restrict the plot to a certain range, e.g. SET SUBBANDS L01 TO L02 /WINDOW 2 64 will avoid plotting channels 1 and 61 to 64 of each of the two subbands L01 and L02, since these channels are usually meaningless (these subbands are combined here to a single spectrum; in the mode in which the spectral correlator is split in two subbands of 64 channels). Note: if you want to use both continuum and line subbands, in the same plot page, you should include dummy arguments in the /WINDOW option for the continuum spectra: SET SUBBANDS C01 to C10 L01 to L02 /WINDOW 0 0 2 64 (two arguments are needed for each resulting spectrum). 2 TELESCOPE CLIC\SET TELESCOPE NAME FIND will select all scans according to the specified telescope name. Default is *. Syntax like NAM* can be used to find all observations with telescope name beginning by NAM. 2 TREC CLIC\SET TIME_ORIGIN *|date Specify the time origin for the abscissa in time plots. This is normally the day for which the first data is plotted, and time is displayed in hours since that day. This day is reset by using PLOT/RESET. SET TIME_ORIGIN date forces the time origin to the specified day (e.g. 23-NOV-1995). SET TIME_ORIGIN * reset the default (automatic) behaviour. 2 TREC CLIC\SET TREC value /ANTENNA i Give the value of the receiver temperature, to be used by the command ATMOSPHERE. Use * instead of the value to force the use of the numbers stored in the file. 2 TRIANGLE CLIC\SET TRIANGLE t1 t2 ... Selects the triangle products for which data will be displayed by command PLOT. Valid triangles : currently only "123" (for three antennas). This command is exclusive with commands SET BASELINES and SET ANTENNAS. This command will be effective only if the triangle products have been computed and stored in the data by commands SPECTRUM/TRIANGLE or COMPRESS/TRIANGLE. In that case the triangle products will have been averaged by these commands; since the phase of the triangle products are closure quantities, the amplitude of the average should not be affected by atmospheric decorrelation. 2 TYPE CLIC\SET TYPE par FIND will select observations of specified type 'par'. This may be OBJECT, PHASE (CALIBRATOR), or RF_PASSBAND (CALIBRATOR). Use argument "*" to disable selection by Source Type. 2 X CLIC\SET X parameter [/LIMITS] Choose the parameter to be plotted along x-axes by command PLOT. Valid parameters are : Parameters valid in both TIME mode and SPECTRAL mode: AMPLITUDE, PHASE, REAL, or IMAGINARY: referring to the visibility in the subband(s), sideband(s), baseline(s) (or antenna(s)) selected by SET SUBBANDS, SET BANDS, SET BASELINES or SET ANTENNAS commands. Only correlation scans will be plotted, not autocorrelations. AUTOCORR. : the autocorrelation power measured in the subband(s), antenna(s) selected by SET SUBBANDS, and SET ANTENNAS commands. Only autocorrelation scans will be plotted, (including calibration scans), not correlations. Parameters valid in SPECTRAL mode only: CHANNEL : channel number in the correlator (use ony this one if Fourier Transform has not been made). VELOCITY : normally with respect to LSR. I_FREQUENCY : the frequency in the second IF (around 350 MHz). SKY_FREQUENCY : the sky frequency. This should be the line rest frequency if the velocity is correct. Parameters valid in TIME mode only: U_COORD, V_COORD, RADIUS, ANGLE: referring to cartesian, or polar coordinates, in the (U,V) plane, of the baseline(s) selected by command SET BASELINES. TIME: universal time (in hours, origin determined by the first plot made, may be reset by PLOT /RESET). SCAN: the scan number NUMBER: the observation number. RECORD: the record number (1 to the number of plotted points). HOUR_ANGLE DECLINATION RMS_PHASE: the r.m.s. of the phase of the average of the non- flagged subbands of the continuum correlator, in current phase units (degrees or radians). This r.m.s. phase is computed during the data compression. RMS_AMPLITUDE: the r.m.s. of the amplitude of the average of the non-flagged subbands of the continuum correlator, in current amplitude units (kelvins or janskys). This r.m.s. amplitude is computed during the data compression. DELAY: as specified for specified baseline (differential, A1-A2 for baseline 12), or for the specified antenna(s). LO_RATE: as specified for specified baseline (differential, as DELAY), or for the specified antenna(s). LO_PHASE: as used for specified baseline (differential, as DELAY), or for the specified antenna(s). CABLE_PHASE: as measured for specified baseline (differential, as DELAY), or for the specified antenna(s). GAMME: the current range (1 or 2) of the cable phasemeter. TOTAL_POWER: the total power measured for the given antenna(s), as measured by the connected detectors. LAMBDA, BETA, or FOCUS: the scanning coordinates for pointing and focussing scans (arc seconds, or millimeters), for the specified antenna, or the moving antenna if the given baseline (if only one is moving). AZ_CORR: the azimuth collimation correction in arc seconds. EL_CORR: the elevation collimation correction in arc seconds. FOC_CORR: the Z focus correction in millimeters. T00 ... T04 : general test parameters (in data headers) T10 ... T14 : test parameters (antenna based) (in data headers) TREC: receiver temperature for the given antenna(s). TSYS : Equivalent system temperature for the given baseline (Geometrical mean of Tsys for both antennas), or for the given antenna(s). PAMB, TAMB, HUMIDITY: measured atmospheric parameters. WIND_AVERAGE, WIND_DIRAV, WIND_TOP, WIND_DIR_TOP: The wind in m/s and the wind direction in degrees, for 5 min. averages and maxima.. QUALITY: The observation quality as set with commands TAG or CURSOR. AZIMUTH, ELEVATION: Start azimuth and elevation for each scan. AZ_ERR, EL_ERR: The tracking errors in arc seconds. AZ_PH, EL_PH: The azimuth and elevation for each record (as used for phase tracking). PARAL_ANGLE: Parallactic angle (angle between the vertical direction and the meridian plane) WATER: Water content of atmosphere (as set by the programmer, or measured with given antenna). ATM_EMISSION: From the output of the atmospheric monitor (normally the 1.3mm receiver). This is the measured radiation temperature of the atmosphere, in Kelvins of Rayleigh-Jeans equivalent radiation temperature. ATM_POWER: This is the output of the atmospheric monitor (normally the 1.3mm receiver). It is the actual counts that appear on the monitors during observations. ATM_REFERENCE: The atmospheric emission used as a reference for the phase correction. This is computed by the command MONITOR. The phase correction will be proportional to the difference between the output of the atmospheric monitor and this reference value. ATM_PHASE: The computed atmospheric phase correction. ATM_UNCORRPH: The phase uncorrected from atmosphere. ATM_CORRPH: The phase corrected from atmosphere. ATM_VALIDITY: 0 or 1 whether the phase correction has been declared valid or not. CAL_PHASE: The phase instrumental calibration curve. CAL_AMPLI: The amplitude instrumental calibration curve. AIR_MASS: The number of air masses (1/sin(elev)) GROUND_EMIS: The ground emission in K (calibrated total power, with sky emission subtracted). EMISSION: The total power detected in emission in K (ground + sky) TDEWAR1, TDEWAR2, TDEWAR3: The temperatures in the 3-stage cryogenerators. TCABIN, TCHOP, TCOLD: The temperatures of the receiver cabin, of the ambient load, and the equivalent temperature of the cold load. Default are : SET Y AMPLITUDE PHASE. The /LIMITS option is used to specify fixed limits: CLIC\SET X TIME /LIMITS t1 t2 where t1 and t2 are the time limits to be used in this example. The codes "*" and "=" may be used. "*" means that the limits are automatically adjusted to the data, separately in each box; "=" means that common limits to all boxes are computed. For time-like plots, the defaults are "/LIMITS * * ". For frequency- like plots, the defaults are "/LIMITS = =". 2 Y CLIC\SET Y parameter [/LIMITS] Choose the parameter to be plotted along y-axes by command PLOT. The available parameters are the same as with SET X parameter. Parameters valid in both TIME mode and SPECTRAL mode: AMPLITUDE, PHASE, REAL, or IMAGINARY: referring to the visibility in the subband(s), sideband(s), baseline(s) (or antenna(s)) selected by SET SUBBANDS, SET BANDS, SET BASELINES or SET ANTENNAS commands. Only correlation scans will be plotted, not autocorrelations. AUTOCORR. : the autocorrelation power measured in the subband(s), antenna(s) selected by SET SUBBANDS, and SET ANTENNAS commands. Only autocorrelation scans will be plotted, (including calibration scans), not correlations. Parameters valid in SPECTRAL mode only: CHANNEL : channel number in the correlator (use ony this one if Fourier Transform has not been made). VELOCITY : normally with respect to LSR. I_FREQUENCY : the frequency in the second IF (around 350 MHz). SKY_FREQUENCY : the sky frequency. This should be the line rest frequency if the velocity is correct. Parameters valid in TIME mode only: U_COORD, V_COORD, RADIUS, ANGLE: referring to cartesian, or polar coordinates, in the (U,V) plane, of the baseline(s) selected by command SET BASELINES. TIME: universal time (in hours, origin determined by the first plot made, may be reset by PLOT /RESET). SCAN: the scan number NUMBER: the observation number. RECORD: the record number (1 to the number of plotted points). HOUR_ANGLE DECLINATION RMS_PHASE: the r.m.s. of the phase of the average of the non- flagged subbands of the continuum correlator, in current phase units (degrees or radians). This r.m.s. phase is computed during the data compression. RMS_AMPLITUDE: the r.m.s. of the amplitude of the average of the non-flagged subbands of the continuum correlator, in current amplitude units (kelvins or janskys). This r.m.s. amplitude is computed during the data compression. DELAY: as specified for specified baseline (differential, A1-A2 for baseline 12), or for the specified antenna(s). LO_RATE: as specified for specified baseline (differential, as DELAY), or for the specified antenna(s). LO_PHASE: as used for specified baseline (differential, as DELAY), or for the specified antenna(s). CABLE_PHASE: as measured for specified baseline (differential, as DELAY), or for the specified antenna(s). GAMME: the current range (1 or 2) of the cable phasemeter. TOTAL_POWER: the total power measured for the given antenna(s), as measured by the connected detectors. LAMBDA, BETA, or FOCUS: the scanning coordinates for pointing and focussing scans (arc seconds, or millimeters), for the specified antenna, or the moving antenna if the given baseline (if only one is moving). AZ_CORR: the azimuth collimation correction in arc seconds. EL_CORR: the elevation collimation correction in arc seconds. FOC_CORR: the Z focus correction in millimeters. T00 ... T04 : general test parameters (in data headers) T10 ... T14 : test parameters (antenna based) (in data headers) TREC: receiver temperature for the given antenna(s). TSYS : Equivalent system temperature for the given baseline (Geometrical mean of Tsys for both antennas), or for the given antenna(s). PAMB, TAMB, HUMIDITY: measured atmospheric parameters. WIND_AVERAGE, WIND_DIRAV, WIND_TOP, WIND_DIR_TOP: The wind in m/s and the wind direction in degrees, for 5 min. averages and maxima.. QUALITY: The observation quality as set with commands TAG or CURSOR. AZIMUTH, ELEVATION: Start azimuth and elevation for each scan. AZ_ERR, EL_ERR: The tracking errors in arc seconds. AZ_PH, EL_PH: The azimuth and elevation for each record (as used for phase tracking). PARAL_ANGLE: Parallactic angle (angle between the vertical direction and the meridian plane) WATER: Water content of atmosphere (as set by the programmer, or measured with given antenna). ATM_EMISSION: From the output of the atmospheric monitor (normally the 1.3mm receiver). This is the measured radiation temperature of the atmosphere, in Kelvins of Rayleigh-Jeans equivalent radiation temperature. ATM_POWER: This is the output of the atmospheric monitor (normally the 1.3mm receiver). It is the actual counts that appear on the monitors during observations. ATM_REFERENCE: The atmospheric emission used as a reference for the phase correction. This is computed by the command MONITOR. The phase correction will be proportional to the difference between the output of the atmospheric monitor and this reference value. ATM_PHASE: The computed atmospheric phase correction. ATM_UNCORRPH: The phase uncorrected from atmosphere. ATM_CORRPH: The phase corrected from atmosphere. ATM_VALIDITY: 0 or 1 whether the phase correction has been declared valid or not. CAL_PHASE: The phase instrumental calibration curve. CAL_AMPLI: The amplitude instrumental calibration curve. AIR_MASS: The number of air masses (1/sin(elev)) GROUND_EMIS: The ground emission in K (calibrated total power, with sky emission subtracted). EMISSION: The total power detected in emission in K (ground + sky) TDEWAR1, TDEWAR2, TDEWAR3: The temperatures in the 3-stage cryogenerators. TCABIN, TCHOP, TCOLD: The temperatures of the receiver cabin, of the ambient load, and the equivalent temperature of the cold load. Default are : SET Y AMPLITUDE PHASE. The /LIMITS option is used to specify fixed limits: CLIC\SET Y AMPLITUDE /LIMITS a1 a2 where a1 and a2 are the amplitude limits to be used in this example. The codes "*" and "=" may be used. "*" means that the limits are automatically adjusted to the data, separately in each box; "=" means that common limits to all boxes are computed. Default limits are provided for AMPLITUDE and PHASE only (0 * -180 180 if SET PHASE JUMPY is effective, and 0 * * * if SET PHASE DEGREES CONTINUOUS ; with corresponding values if SET PHASE RADIANS). 2 WATER CLIC\SET WATER value /ANTENNA i Give the value of the water vapor content (in mm), to be used by the command ATMOSPHERE. Use * instead of the value to force the use of the numbers stored in the file. 2 WEIGHTS CLIC\SET WEIGHTS [TSYS ON|OFF] [CALIBRATION ON|OFF] Selects the way the data is weighted in command TABLE. With TSYS ON, data is weighted by 1/TSYS**2, where TSYS is the equivalent system temperature (the geometrical mean of system temperature of both antennas, for a given baseline). With TSYS OFF, this weight factor is turned off. With CALIBRATION ON, data is also weighted by 1/CAL**2, where CAL is the amplitude instrumental calibration factor (if any). If no amplitude instrumental calibration function is applied (absolute amplitude), this weighting should have no effect. With CALIBRATION OFF, weights are not affected by amplitude instrumental calibration. With both TSYS OFF and CALIBRATION OFF, data is weighted proportionally to observing time. 2 COPY CLIC\SET COPY DATA|NODATA This command is used to select the default data access mode on COPY commands. See the help for COPY. 1 SHOW CLIC\SHOW Arg Display some parameter defined by SET. "SHOW ALL" will display all parameters specified by SET (See SET command). "SHOW CRITERIA" will display only selection criteria, "SHOW DISPLAY" will give only the parameters relevant to command PLOT, and "SHOW GENERAL" will give the rest of the parameters. 1 SOLVE CLIC\SOLVE Item This is a command to determine interferometer parameters from measured data. such as baseline values, or calibration curves. 2 AMPLITUDE CLIC\SOLVE AMPLITUDE [/PLOT] [/BREAK ...] [/POLYNOMIAL...] [/WEIGHT] This will fit a mathematical function into the measured amplitude of the sources in the current index (presumably calibrators). This data must have been selected and plotted in axes : SET X TIME and SET Y AMPLITUDE for the baselines and bands of interest, specified by the corresponding SET commands. The calibration function is kept in memory. Command STORE should be used next to store this function in the header of source observations, after a change in the index to select the appropriate scans. In antenna mode the averaged phase and amplitude closures are computed, as well as their standard deviations. The phase closures should be close to zero, while the amplitude closures should be close to 100%. Strong deviations of amplitude closures from 100% are an indication of amplitude loss on long baselines, due to phase decorrelation during the time averaging. The fit then shows strong systematic errors; if this occurs, baseline based calibration of the amplitudes might be preferred. Option /PLOT will plot the fitted curve over the data. Fitted curves may be of two kinds: - Cubic splines (the default). By default knots are regularly spaced with an interval between knots set by the SET STEP command. Additional knots may be introduced with the option: /BREAK kind time [kind time ...] a break introduced at abscissa 'time' ; 'kind' is an integer in the range 0-3; 0 means that a discontinuity will be present, 1 that the first derivative will be discontinuous, and so on. Several breaks may be introduced; the program will detect an error if too many breaks are introduced, compared to the density of data points. - Polynomial curves may be used instead. For this the option is: /POLYNOMIAL [degree] indicating the degree of the polynomial (default 0). Normally the data points are all assigned the same weight for the fit. With option /WEIGHT, the data points are weighted according to their errors. Errors are set to the statistical errors for the amplitudes. 2 HOLOGRAPHY CLIC\SOLVE HOLOGRAPHY [MO nmodes] [NP npix] [IT niter gain] [FREE r1 r2 ...] [/OFFSET x y z] [/PLOT [AMP amin amax astep] [PHA pmin pmax pstep] [ERRORS emin emax estep] [NUMBER] (Keywords like MO, NP, IT, FREE may be given in any order, each must be followed by its arguments; they are all optional) This command computes an antenna surface map from a set of holography measurements. The set of scans (procedure HOLO) should have first been calibrated in phase, amplitude and RF passband relative to interspaced correlation scans in the direction of the source. The map will be computed from the first band and subband sets chosen with commands SET BAND and SET SUBBAND. SET BAND AVERAGE is recommended for continuum measurements; only continuum subbands should be used. For line measurements, the continuum width of one of the correlator units should match the actual line width for better sensitivity. The antenna to be studied should be selected by command SET ANTENNA i. Data from the baselines linking this antenna (scanned) to other (fixed) available antennas are averaged. The amplitude and phase maps are obtained by Fast Fourier Transform of the observed beam map. The maps will be square (npix by npix pixels). The default for npix is 64, it should be greater than the number of observed holography scans (usually 16 or 32). After FFT a gaussian illumination function is fitted in the amplitudes, giving the offset from the center (in meters) and the edge taper (in dB). If /PLOT is given, the amplitude map will be shown (in decibels), from -15 to 0 dB, with contours in steps of 3db (these may be changed using amin, amax and astep). A lest square fit is used to correct the phases from a remaining phase offset, pointing errors, and focus offsets. The panel rings following FREE are not used for this fit. If /PLOT is given, the antenna normal surface errors will be shown, in micrometers, from -500 to 500 mum, with contours in steps of 100 mum (these may be changed using keyword ERRORS followed by emin, emax and estep). If /PLOT PHASE is given, the residual phase map will be plotted instead of surface errors, in radians from -pi to pi, with contours in steps of 0.2 radian. If this map shows remaining 2*pi discontinuities, or if focus offsets larger that 1mm are found, you should try using option /OFFSET to correct the phases for an offset (x,y,z in meters) in the focus coordinates, before fitting. This should lead to better rms values. /PLOT gives also the amplitude illumination pattern, in dB; default plot limits are -15dB to 0dB by step of 3dB; use /PLOT AMP amin amax astep to change these settings. If NUMBER is given as a /PLOT argument, the panels numbers are drawn. The rms values for the phase and the normal surface errors (in radians and micrometers) are given, both with and without amplitude weighting. The contribution of the illumination amplitude distribution and of the observed phase errors to the antenna efficiency are given. Finally, if nmodes is larger than 0, a listing of panels displacements is computed, and written in a file like "panels-an1.dat". This uses the parameter nmodes which is the number of modes used for each panel: 1 is only the translation mode (normal to the antenna surface); 3 (the usual setting), adds both tilt modes, radial and tangential, but no panel deformation; 4 adds a torsion mode and 5 a motion of the panel center relative to its edges (there are only 5 screws for each panel, thus only 5 possible modes). In the file "panels-an1.dat" a line for each panel is printed. The first two numbers are the panel numbers, followed by up to five screw settings (three only for the inner ring). All screw settings are equal if nmodes was set to 1, only one number is then printed. If niter is not forced to zero, the fit is obtained iteratively: the panel orthogonal deformation modes are computed from the aperture phase, then the phase change that these deformations would have caused is computed (by doing a FFT to the beam map, doing a cut-off at the observed map size, followed by a FFT back to the aperture plane), and subtracted from the aperture phase; second order panel deformations are computed from these residuals, and so on. The number of iterations niter and a gain to this iterative procedure may be specified ([IT niter gain]); their default values are 5 and 1.0 . Use IT 0 for no iterative procedure at all. At each step the phase residual rms and the rms of panel deformations fitted are given (weighted by the fitted amplitude illumination and counted perpendicularly to the surface). A gildas image file of the results is kept (e.g. "jj-mmm-yyyy-an1.map"), in which plane 3 in the amplitude in dB, plane 4 the raw phases and plane 2 the residual phase in radians (plane 1 contains the fitted amplitude, i.e. a Gaussian). 2 BASELINE CLIC\SOLVE BASELINE [/OFFSET b1 dx1 dy1 dz1 b2 ...] [/SEARCH range] [/POLYNOMIAL degree] This uses a linear method to determine baselines separately and should work only if the starting values are within half a wavelength in any direction of the true values. The baselines to be determined must have been selected by the SET BASELINE command, and the data plotted; plot axes must have been previously selected by : SET X HOUR_ANGLE DECLINATION and SET Y PHASE. Use option /OFFSET to correct the phases for an offset (dx1,dy1,dz1) in baseline b1 before fitting. This is needed if the baseline was wrong by more than half a wavelength. Offsets are to be given in meters. The results are given as offsets in meters to be added to the baseline used for data acquisition (which may be read by SIC\EXAMINE BASELINE). The total fitted baseline is also given in meters, as well as the rms of the residuals in phase units. Two sets of offsets are given: the first set (dx, dy, dz) are the offsets with respect to the antenna positions actually used, while the secoond set (DX, DY, DZ) are with respect to the standard antenna coordinates (the default values in OBS). The /SEARCH option enables an automatic search with starting offsets scanning a 3-d box in dx, dy, dz, by steps of half a wavelength in the three directions. The argument range is in meters (scanning is from -range/2 to +range/2, default -0.005 to 0.005). Only the solution with the minimum rms is kept. Searching one baseline in a 0.01 meter range takes 4 seconds on the micro-vax 3400. Use command RESIDUALS BASELINE to display the fit residuals (phase should be constant). With SET ANTENNA in action the antenna position offsets are directly fitted to the antenna phases, ensuring baseline closure. Use later command PRINT BASELINE to create a procedure file (named CLIC-BASELINE.OBS) containing the antenna position offsets. This procedure file may be executed by the observing program OBS on the control computer BURE01. With option /POLYNOMIAL degree, and if SET X TIME is used in addition of HOUR_ANGLE and DECLINATION, a polynomial function of time is included in the phase function being fitted. The degree may range from 0 (the default) to 3. In that case command RESIDUALS will also plot the residuals as a function of time. In one specify elevation as an additional X variable (e.g. SET X HOUR_ANGLE DECLINATION TIME ELEVATION), then an additional parameter is fitted: the offsets between elevation and azimuth axes (or rather the differences between antennas). These differing offsets result in a phase effect proportional to the cosine of elevation. In antenna mode, these offsets are given for each antenna in meters. In baseline mode, only differences are computed. To further correct for this effect use the command MODIFY AXES. It is foreseen to correct for this effect in real time, when the values are well and unambiguously known. 2 DELAY CLIC\SOLVE DELAY [/SEARCH range interval] [/PLOT] This uses a linear method to determine delays. The baselines to be determined must have been selected by the SET BASELINE (or SET ANTENNA) command, and the data plotted; plot axes must have been previously selected by : SET X I_FREQUENCY and SET Y PHASE. The results are given in nanoseconds. The /SEARCH option enables an automatic search with starting offsets from -range|2 to +range|2 by steps of given interval. the default range is 200 nanoseconds, with interval of 1 nanosecond. With SET ANTENNA in action the antenna delays are directly fitted to the antenna phases, ensuring delay closure. Use later command PRINT DELAY to create a procedure file (named CLIC- DELAY.OBS) containing the fitted antenna delays. This procedure file may be executed by the observing program OBS on the control computer BURE01. With option /PLOT, the fitted phases pill be plotted over the data. 2 FLUX CLIC\SOLVE FLUX [NOREFERENCE] [BEST n] Calculate the fluxes of the sources in the current index or the antenna efficiencies (Jansky to Kelvin) if the source flux is known. The command can also be used to bootstrap source fluxes from a known source. It should be used before computing any amplitude calibration, on an index covering a reasonably short time interval to avoid possible efficiency variations. The commands should be used in the following way: - The command SET FLUX may be used to define the flux of one, or several of the sources in the current index for which the flux is known. Frequencies and dates may be specified in SET FLUX. Alternatively, the default efficiencies stored in the data header will be used, if NOREFERENCE is present. - Then the command SOLVE FLUX will use the sources of known flux (optionally with matching frequencies and dates) to determine the efficiencies for all antennas, and compute the fluxes of all other sources using those efficiencies. IF BEST n is present, the antennas giving the highest n fluxes will be used for averaging (n: 1 to the number of available antennas). SOLVE FLUX now gives the decorrelation factor relative to the efficiencies logged in the scan headers (assumed to be the standard single-dish efficiencies). - The command SHOW FLUX will give a list of fluxes either assumed or just determined. - The command PRINT FLUX will create a procedure that may be used later to reload these fluxes in CLIC, if needed. - The command STORE FLUX will store the fluxes and efficiencies in the headers of the observations in the current index. SOLVE FLUX includes a correction for decorrelation effect, using the rms phases computed from the 1-second integration dumps. Use SOLVE FLUX RAW to ignore this correction. SOLVE FLUX normally requires point sources to be meaningful. There two exceptions to this: - Planets, at least the smallest ones. - W3OH, a reasonably strong circumpolar HII region These sources can be used as flux calibrators. Size effects are corrected for by CLIC, using the ephemerides to determine the planet characteristics, and a simple (but accurate) source model for W3OH. 2 FOCUS CLIC\SOLVE FOCUS [/PLOT] [/COMPRESS] [/PRINT] Find focus corrections from a FOCUS scan. All focus scans in the current index are processed by a parabolic fit. All continuum subbands and both side bands are averaged. SET AVERAG METHOD SCALAR is recommended. The fits may be displayed with option /PLOT. The option /COMPRESS may be used to average data in a given time interval before processing, to improve the signal-to-noise ratio. Default is 4 seconds. The presence of option /PRINT produces a procedure file "focus.obs", to be used in OBS for introducing the fitted focus offset. 2 GAIN CLIC\SOLVE GAIN [SCAN] [/PRINT] Compute the receiver gain ratio (Image Side Band over Signal Side band) from correlation data on a continuum source. Compute also the LO1 and LO3 phases that should be used in real time to have zero phases in both side bands. The data from all the scans in the current index are averaged except if optional argument SCAN is given, in which case the gain ratios are computed for each scan. Option /PRINT : write a procedure INTER_OBS:gain.obs to set the gains (and phases) in OBS. 2 PHASE CLIC\SOLVE PHASE [/PLOT] [/BREAK ...] [/POLYNOMIAL...] [/WEIGHT] This will fit a mathematical function into the measured phases of the sources in the current index (presumably calibrators). This data must have been selected and plotted in axes : SET X TIME and SET Y PHASE for the baselines and bands of interest, specified by the corresponding SET commands. Phases should be continuous. The calibration function is kept in memory. Command STORE should be used next to store this function in the header of source observations, after a change in the index to select the appropriate scans. SOLVE PHASE internally and temporarily resets SET PHASE to ABSOLUTE. The INTERNAL|EXTERNAL mode is kept to allow determining a phase curve on top of an external receiver reference. Option /PLOT will plot the fitted phase curve over the data. Fitted curves may be of two kinds: - Cubic splines (the default). By default knots are regularly spaced with an interval between knots set by the SET STEP command. Additional knots may be introduced with the option: /BREAK kind time [kind time ...] a break introduced at abscissa 'time' ; 'kind' is an integer in the range 0-3; 0 means that a discontinuity will be present, 1 that the first derivative will be discontinuous, and so on. Several breaks may be introduced; the program will detect an error if too many breaks are introduced, compared to the density of data points. - Polynomial curves may be used instead. For this the option is: /POLYNOMIAL [degree] indicating the degree of the polynomial (default 0). Normally the data points are all assigned the same weight for the fit. With option /WEIGHT, the data points are weighted according to their errors. Errors computed from the phase rms determined in the data compression. 2 POINTING CLIC\SOLVE POINTING [beam] [/PLOT] [/OUTPUT filename [NEW|APPEND] [FLUX]] [/COMPRESS time] [/PRINT] Find pointing corrections from POINTING scans. All pointing scans in the current index are processed by a gaussian fit. All continuum subbands and both side bands are averaged. SET AVERAG METHOD SCALAR is recommended. The fits may be displayed with option /PLOT. The results may be written on a file if /OUTPUT is given. The file is given extension .LIS by default; a new file is opened except if APPEND is given as a second argument of option /OUTPUT. The file is by default in a format suitable for the determination of a pointing model (program POINT at BURE). The presence of optional argument FLUX changes the output format for the determination of relative fluxes (by ASTRO). The option /COMPRESS may be used to average data in a given time interval before processing, to improve the signal-to-noise ratio. Default is 4 seconds. Option /PRINT : write a procedure file INTEROBS:pointing.obs to update the pointing corrections in OBS. 2 FIVE CLIC\SOLVE FIVE [beam] [/PLOT] [/OUTPUT filename [NEW|APPEND] [FLUX]] [/PRINT] Find pointing corrections from FIVE point scans. All five-point scans in the current index are processed by a gaussian fit. All continuum subbands and both side bands are averaged. The fits may be displayed with option /PLOT. The results may be written on a file if /OUTPUT is given. The file is given extension .LIS by default; a new file is opened except if APPEND is given as a second argument of option /OUTPUT. The file is by default in a format suitable for the determination of a pointing model (program POINT at BURE). The presence of optional argument FLUX changes the output format for the determination of relative fluxes (by ASTRO). Option /PRINT : write a procedure file INTER_OBS:pointing.obs to update the pointing corrections in OBS. 2 TOTAL CLIC\SOLVE TOTAL [beam] [/PLOT] [/PRINT] [/OUTPUT filename [NEW|APPEND] [FLUX]] [/COMPRESS time] [/PRINT] Find pointing corrections from POINTING scans, but using the total power from each antenna. All pointing scans in the current index are processed by a gaussian fit. The fits may be displayed with option /PLOT. The results may be written on a file if /OUTPUT is given. The file is given extension .LIS by default; a new file is opened except if APPEND is given as a second argument of option /OUTPUT. The file is by default in a format suitable for the determination of a pointing model (program POINT at BURE). The presence of optional argument FLUX changes the output format for the determination of relative fluxes (by ASTRO). The option /COMPRESS may be used to average data in a given time interval before processing, to improve the signal-to-noise ratio. Default is 4 seconds. Option /PRINT : write a procedure file INTER_OBS:pointing.obs to update the pointing corrections in OBS. 2 RF_PASSBAND CLIC\SOLVE RF_PASSBAND [da] [dp][/PLOT] Solve for passband calibration curves, by fitting it to the amplitudes and phases measured on a strong continuum source (passband calibrator). The behaviour of this command depends on the current mode of rf passband calibration (Frequency or Channel). - for frequency-dependent rf passabnd calibration: the resolution is normally done using all the spectral subbands plotted together, as a function of intermediate frequency. It should be done separately for upper and lower side bands. A single frequency-dependent polynomial is fitted, a high degree might be necessary for the phase, if band edges are used (up to 20 is feasible). - for channel dependent rf passband calibration: (i) for continuum, the data itself is directly stored as calibration values (this gives a channel-dependent passband curve). In addition a polynomial is fitted and optionally plotted (this gives a frequency-dependent passband curve). (ii) for spectral subbands, polynomials are fitted and optionally plotted, as a channel-dependent passband curve. The degrees for polynomials are 'da' for amplitude, 'dp' for phase (defaults 0 and 1). X unit must be channel. Spectral subbands must be plotted separately. The current index should contain calibration observations of strong continuum sources. Command STORE should be used next to store this function in the header of source observations. Both channel dependent and frequency dependent curves will be stored; Use command SET RF_PASSBAND FREQUENCY|CHANNEL to apply one or the other. Option /PLOT will plot the polynomial fits over the data. 2 SKYDIP CLIC\SOLVE SKYDIP [TREC|EFF] [/PLOT] [/OUTPUT File [NEW]] Compute receiver temperature TREC or antenna forward efficiency EFF from skydip scan. All skydip scans in the current index a solved. A graphic display of the solution can be plotted using the /PLOT option, and data can be written to an output file using the /OUTPUT option. 1 STORE CLIC\STORE par Writes calibration (or edition) data in the output file. All scans in the current index are processed. Calibrated data may later be plotted with the PLOT command, after setting INSTRUMENTAL and/or RF_PASSBAND to ON. 2 AMPLITUDE CLIC\STORE AMPLITUDE [PHASE] [/BAND code] [/SELF] Store the amplitude (and optionally phase) calibration. Storing both calibrations together is more efficient. With option "/BAND code", one may use the calibration curve determined with one of the sidebands (`code' is UPPER, LOWER or AVERAGE), to calibrate both sidebands. With option "/SELF", the calibration stored will not be the calibration curve determined with the last SOLVE AMPLITUDE [or PHASE], but, for each scan, the visibility corresponding to the first subband set (eg., SET SUB L01 to L03 ...); data from each side band will be used to calibrate the same side band. This provide a simple, easy way to calibrate data taken on strong continuum sources (quasars). 2 CORRECTION CLIC\STORE CORRECTION GOOD|BAD|AUTO|SELF [tmin] Stores in the header of each scan (of the current index) the information whether the phase correction is or not declared valid, and should be actually applied when SET PHASE ATM is selected. If AUTO, that information is determined on the phase calibrators (type PHASE), by comparing the amplitudes with and without the correction. This information is then propagated to the neighbouring source observations (type OBJECT, in a +- tmin minutes time window). `tmin' interval (in time minutes) defaults to 15 minutes. If SELF, that information is determined on the source, whatever its type may be, by comparing its amplitude with and without the correction. 2 FLAG CLIC\STORE FLAG f1 f2 ... [/ANTENNA a1 a2 ... ] [/BASELINE b1 b2 ...] [/BAND b] [/RESET] Flag all data in the current index according to the parameters and option specified. This is equivalent to the following sequence of commands CLIC\MODIFY DATA with a DATA.CLIC procedure containing FLAG f1 f2 ... [/ANTENNA a1 a2 ...] [/BASELINE b1 b2 ...] [/RESET] GO WRITE but it is simpler and faster (however, all the data records will be flagged). 2 FLUX CLIC\STORE FLUX Store the source fluxes and antenna efficiencies determined from a previous SOLVE FLUX command. Source names, frequencies (within 1GHz) and dates (within a week) must match. 2 PHASE CLIC\STORE PHASE [AMPLITUDE] [/BAND code] [/RECEIVER irec] Store the phase (and optionally amplitude) calibration. Storing both calibrations together is more efficient. With option "/BAND code", one may use the calibration curve determined with one of the sidebands (`code' is UPPER, LOWER or AVERAGE), to calibrate both sidebands. With option "/SELF", the calibration stored will not be the calibration curve determined with the last SOLVE PHASE [or AMPLITUDE], but, for each scan, the visibility corresponding to the first subband set (eg., SET SUB L01 to L03 ...); data from each side band will be used to calibrate the same side band. This provide a simple, easy way to calibrate data taken on strong continuum sources (quasars). With option "/RECEIVER irec", the calibration curves solved using data from receiver "irec" will be stored in parallel with any other calibration curve. This phase curve will be selected by giving SET PHASE EXTERNAL. (see this command). This has no meaning for amplitudes. /BAND may be used in conjunction with /RECEIVER. 2 QUALITY CLIC\STORE QUALITY code Store the data quality to be used as a selection criterion. All the scans in the current index are tagged. Code may be an integer in the range 0-9, or drectly the corresponding quality word: 0 Unknown 1 Excellent 2 Good 3 Fair 4 Average 5 Poor 6 Bad 7 Awful 8 Worst 9 Deleted 2 RF_PASSBAND CLIC\STORE RF_PASSBAND Store the Continuum and/or Line RF passband calibration curves. Both channel dependent and frequency dependent curves will be simultaneously stored. Caution: Line RF passbands should be stored only for consistent spectral correlator configurations. 1 TABLE CLIC\TABLE Name Status [/RESAMPLE nc ref val inc code shape width] [/COMPRESS tmax uvmax] [/FREQUENCY name rest-freq] [/DROP n1 n2] [/FFT] This command will create a UV data Table from the current index. not given, the most recently created table will be extended. 'Status' may be OLD (default value if not specified) to extend and existing table, or NEW to create a new table. The bands and subbands used are given by command SET SELECTION (See HELP SET SELECTION). The weighting modes are given by command SET WEIGHTS. Option /RESAMPLE enables to resample data on a new spectral grid (for line data). 'nc' is the output number of channels, 'ref' the reference channel, 'val' the value of velocity or frequency offset (with respect to the rest frequency) at the reference channel, 'inc' the resolution, 'code' is "V" if the value 'val' and the resolution 'inc' are in velocity units, "F" for frequency units. The reference channel thus corresponds to the given 'val' velocity, or to the offset 'val' in MHz from the rest frequency present in the header or modified by option /FREQUENCY. Resampling is done by default through linear interpolation of input channel data. Resampling may also be done (using option /FFT) in Fourier space by cut-off or extrapolation (by zeroes) of the Fourier components, after deconvolution by the channel response of the correlator (due to on-line apodization), and followed by reconvolution to produce frequency channels of the given shape and width. Allowed shapes are: TBox = a box in delay space (unapodized correlator) Ppar = a parabola in delay space (apodized correlator) (the default) FBox = a box in frequency space (square filter) FTri = a triangle in frequency space (Hanning smoothed square filter) The width is the channel width in units of channel separation (default 1). Option /FFT is not recommended when joining together several subbands to produce a single spectrum, with a limited number of broad channels. In those cases using the FFT could produce a spectrum with "holes" at the points between subbands with limited overlap. Option /FREQUENCY is used to redefine the rest frequency (and line name) for the output table. The velocity scale is computed accordingly. This rest frequency will correspond to the reference channel in option RESAMPLE. Option /DROP enables to drop the first 'n1' and last 'n2' channels in each subband of the OLD spectral correlator. For the NEW spectral correlator (data taken since summer 1992), it is replaced by the commands SET GIBBS and SET DROP. Option /COMPRESS is used to compress the data before writing the table. This works like the COMPRESS command, but no intermediate file is written. A UV data Table is a file in the Gildas Data Format, of dimension 2. Each column corresponds to a visibility data point. Lines contain respectively: 1. U in meters 2. V in meters 3. W in meters 4. Observation date (integer CLASS Day Number) 5. Time in seconds since above date 6. Number of start antenna 7. Number of end antenna 8. First frequency point (real part) 9. First frequency point (imaginary part) 10. First frequency point (weight = integration time x frequency width in MHz divided by the product of system temperatures of both antennas); see SET WEIGHTS to select the weighting modes. 11. Same for second frequency point, and so on. The first dimension is then the 3 * nchan + 7, for nchan frequency channels; The second dimension is the number of UV points measured. For use with GreG COLUMN command, this UV Data Table must be transposed by Gildas Task TRANSPOSE. 1 TAG CLIC\TAG Quality_Code List_of_Observations Attributes a quality to a given list of Observations. Quality_Code is an integer in the range 0-9, and the recommended quality scale is 0 Unknown 1 Excellent 2 Good 3 Fair 4 Average 5 Poor 6 Bad 7 Awful 8 Worst 9 Deleted The operation is immediate and occurs in the OUTPUT file for all versions of all Observations specified in the list. If no list is given, the R memory is attributed the specified quality. A FIND operation will only select Observations of quality better than (i.e. less or equal to) the quality specified by the SET QUALITY command, or in the /QUALITY option. 1 VARIABLES CLIC\VARIABLES group state This command is used to enable/disable CLIC variables. 'state' may be ON or OFF; 12 groups of variables are available, corresponding to sections in the scan headers. READ_WRITE Input/Output file information (Global) GENERAL General information (Scan based) POSITION Source related information (Scan based) CONFIG Array configuration related information (Scan based) RF_SETUP Receiver related information (Scan based) CONTINUUM Continuum correlator related information (Scan based) LINE Spectral correlator related information (Scan based) SCANNING Special scan information (Record based) ATMOSPHERE Atmospheric calibration parameters and results (Scan based) DESCRIPTOR Data descriptor information (Scan based) DATA_HEADER Data header information (Record based) DATA_RECORD Data values (Record based) Scan or Record based variables variables refer to the last read scan or record (explicitely by GET/RECORD, or implicitely by PLOT or other commands). 2 READ_WRITE CLIC\VARIABLES READ_WRITE ON|OFF Input/Output file related variables IN_FILE Name if input file OUT_FILE Name of output file INBLOC Block of observation in input file IDATA Address od data section in input observation INSEC Number of sections in header INEXT Next available block in input file ONEXT Next available block in output file IXNUM Index number of current observation in input file ISEC [INSEC] Header sections ILEN [INSEC] Length of header section (words) IADD [INSEC] Addresses of header sections (words) IXNEXT Next available entry in input file index OXNEXT Next available entry in output file index CXNEXT Next available entry in current index INWORD Number of words in current observation IDATAL Length (words) of data section MODIFY (Logical) data is open for modify SHARE (Logical) Output file is shared FOUND Number of observations in current index IX_NUM [ ] Observation numbers in input file index IX_BLOC [ ] Blocks numbers of observations in input file OX_NUM [ ] Observation numbers in output file index OX_BLOC [ ] Blocks numbers of observations in output file CX_NUM [ ] Observation numbers in current index CX_BLOC [ ] Blocks numbers of observations in current index 2 GENERAL CLIC\VARIABLES GENERAL ON|OFF General information related variables TELESCOPE Telescope name NUMBER Observation number VERSION Observation version number DOBS Day of observation (internal format) DATE_OBSERVED Day of observation (in clear) DRED Day of last reduction (internal format) DATE_REDUCED Day of last reduction (in clear) DATATYPE Type of observation (4 for interferometer data) RQUAL Quality of observation (0-9) QUALITY Quality of observation (Excellent, ... Awful) SCAN Scan number UTOBS Time of observation (radians!) TIME_OBSERVED Time of observation (hh:mm:ss.ss) LSTOBS Sidereal time of observation (radians) AZIMUTH Azimuth of source direction (radians) ELEVATION Elevation of observation (radians) TIME Integration time (minutes) PROC Procedure used (internal format) PROCEDURE Procedure used (in clear) TYP_OFF Type of offsets 2 POSITION CLIC\VARIABLES POSITION ON|OFF Source related information SOURCE Source name LAMBDA Source longitude-like coordinate (radians) BETA Source latitude-like coordinate (radians) OFF_LAMBDA Offset in lambda (radians) OFF_BETA Offset in beta (radians) EPOCH Epoch of coordinates (if equatorial) PROJECTION Projection used for offsets FOCUS Focus position used FLUX Source flux (Jy) for calibrators 2 CONFIG CLIC\VARIABLES CONFIG ON|OFF Array configuration related information NANT Number of antennas NBAS Number of baselines HOUR_ANGLE Hour angle of observation (hours) STATION [NANT] Positions of antennas PHYS_ANT [NANT] Antenna physical numbers CORR_INPUT [NANT] Correlator input connected for each antenna START_ANTENNA [NBAS] First antenna of baseline END_ANTENNA [NBAS] Second antenna of baseline BASELINE [3,NBAS] Coordinates of baselines (meters) ANTENNA [3,NANT] Coordinates of antennas (meters) AXES_OFFSET [NANT] Offsets of El axis from Az axes (meters) 2 RF_SETUP CLIC\VARIABLES RF_SETUP ON|OFF Receiver related information LINE Line name (in OBS) FREQUENCY Rest Frequency (in OBS) (MHz) ISB Side band (1:upper, 2:lower) LOCK Lock FLO1 Frequency of First LO (MHz) FLO2 Frequency of Second LO (MHz) FIF1 First intermediate frequency (MHz) VELOCITY Velocity entered in OBS (km/s) TYPE_VEL Velocity type DOPPLER Doppler correction factor (v/c) 2 CONTINUUM CLIC\VARIABLES CONTINUUM ON|OFF Continuum correlator related variables N_SIDEBANDS Number of present sidebands N_SUB_BANDS Number of continuum sub-bands NCDAT Total number of channels (sidebands x subbands) CRCH [2] Reference channel for sideband CVOFF [2] Velocity for sideband CVRES [2] Velocity resolution CRFOFF [2] Rest frequency (MHz) CRFRES [2] Frequency resolution CNAM_U Line name for Upper side band CNAM_L Line name for lower side band CFLO3 [10] LO3 frequency for subband CFWID [10] Width of subband (MHz) 2 LINE CLIC\VARIABLES LINE ON|OFF Spectral correlator related information N_LINE_BANDS Number of line subbands FOURIER (Logical) FFT done, data in frequency space TOTAL_CHANNELS Total number of line channels N_CHANNELS [nsubband] Number of channels in subband FIRST_CHANNEL [nsubband] First channel in subband LFCEN [nsubband] LO3 frequency (channel 1) LFRES [nsubband] Frequency resolution (signed) REF_CHANNEL [2,nsubband] Reference channel for spectrum F_RESOLUTION [2,nsubband] Frequency resolution F_OFFSET [2,nsubband] Rest frequency in reference channel V_RESOLUTION [2,nsubband] Velocity resolution V_OFFSET [2,nsubband] Velocity in reference channel R_LILEVU [nsubband,nant] Sampling levels (USB) R_LILEVL [nsubband,nant] Sampling levels (LSB) 2 SCANNING CLIC\VARIABLES SCANNING ON|OFF Special scans (Pointing, Focus, Calibrate and Skydip) SCAN_TYPE Type of special scan (1 focus 2,3 point 4,5 calibr) MOBIL [NANT] Antennas in motion COLL_AZ [NANT] Collimation in azimuth (arc sec) COLL_EL [NANT] Collimation in elevation (arc sec) COR_FOC [NANT] The Z focus correction in mm. 2 ATMOSPHERE CLIC\VARIABLES ATMOSPHERE ON|OFF Atmospheric calibration PRESSURE Pressure in hectopascals (zero alt.) AMBIANT_T Outside temperature (K) ALTITUDE Altitude in kilometers HUMIDITY Humidity in % WATER [NANT] Water content (mm) TAU_S [NANT] Optical depth in signal side band TATM_S [NANT] Temperature of atmosphere in signal side band TAU_I [NANT] Optical depth in image side band TATM_I [NANT] Temperature of atmosphere in image side band BEAM_EFF [NANT] Beam efficiency FORWARD_EFF [NANT] Forward efficiency T_CHOPPER [NANT] Temperature of ambiant load (K) T_REC [NANT] Receiver temperature (K) GAIN_IMAGE [NANT] Gain ratio image/signal CHOPPER_COUNTS [NANT] Measured counts on ambiant load SKY_COUNTS [NANT] Measured counts on sky T_SYS_S [NANT] System temperature (signal band) T_SYS_I [NANT] System temperature (image band) CHOPPER_EFF [NANT] Chopper efficiency CAL_MODE [NANT] Calibration reduction mode 2 DESCRIPTOR CLIC\VARIABLES DESCRIPTOR ON|OFF Data descriptor information N_DUMPS Number of records HEADER_LENGTH Length of data header (words) CONT_LENGTH Length of continuum data (words) LINE_LENGTH Length of line data (words) 2 DATA_HEADER CLIC\VARIABLES DATA_HEADER ON|OFF Data header information DH_DUMP Record number DH_OBS Date of observation (in internal format) DH_DATE Date of observation (in clear) DH_INTEG Integration time in seconds DH_SVEC[3] EQ coordinates of source direction DH_AFLAG [NANT] Antenna flag word DH_TOTAL [NANT] Total power DH_DELCON [NANT] Delay used for continuum correlator (ns) DH_DELLIN [NANT] Delay used for line correlator (ns) DH_DELAYC [NANT] Computed delay (ns) DH_DELAY [NANT] Delay offset (ns) DH_PHASEC [NANT] Computed LO1 phase DH_PHASE [NANT] LO1 Phase offset DH_RATE [NANT] Computed fringe rate DH_CABLE [NANT] Phase of IF cable (at LO2 frequency) DH_OFFFOC [NANT] Focus offset (mm) DH_OFFLAM [NANT] Azimuth offset (arc sec) in pointing scans DH_OFFBET [NANT] Elevation offset (arc sec) in pointing scans DH_UVM [2,NBAS] U and V for baseline (meters) DH_RMSPE [2,NANT] AZ and EL pointing errors (rms, in arc sec.) DH_UTC UT Time (sec) DH_TIME UT Time (hh:mm:ss.ss) DH_ATFAC [2,NANT] Atmosphecic calibration factor (K) [sideband,ant] DH_BFLAG [NBAS] Baseline Flag word DH_INFAC [2,2,NBAS] Instrumental factor [real/imag,upp/lower,baseline] 2 DATA_RECORD CLIC\VARIABLES DATA_RECORD ON|OFF Data values DATA_C [CONT_LENGTH] Continuum data DATA_L [LINE_LENGTH] Line data The following additional variables are computed by command MINMAX: C_AMPMAX_U [NBAS] Maximum amplitude, continuum, USB L_AMPMAX_U [NBAS] Maximum amplitude, line, USB C_AMPMAX_L [NBAS] Maximum amplitude, continuum, LSB L_AMPMAX_L [NBAS] Maximum amplitude, line, LSB C_AMPMIN_U [NBAS] Minimum amplitude, continuum, USB L_AMPMIN_U [NBAS] Minimum amplitude, line, USB C_AMPMIN_L [NBAS] Minimum amplitude, continuum, LSB L_AMPMIN_L [NBAS] Minimum amplitude, line, LSB