1 ACCUMULATE LAS\ACCUMULATE ACCUMULATE is used to integrate step by step an ensemble of spectra. The T spectrum is added to the spectrum in R with the current weights. R thus contains the current sum, and T the last sum. As command SUM, ACCUMULATE checks for the positional coincidence and calibration homogeneity according to SET MATCH and SET CALIBRATION respectively. Alignement of spectra is checked according to SET ALIGN command. For EQUAL weights, ACCUMULATE computes the SUM of the two spectra, allowing addition of an ensemble of spectra after division by the total number of spectra. ACCUMULATE also works on Continuum drift. The alignement may be Channel or Position in this case. 1 BASE LAS\BASE [Deg] [/PLOT] [/CONTINUUM [flux]] LAS\BASE SINUS Amplitude Period Phase [/PLOT] LAS\BASE LAST [/PLOT] BASE copies R into T, then subtracts from R a polynomial baseline of degree Deg, or a sinusoidal baseline if the first argument is SINUS. In the latter case, SINUS must be followed by the Amplitude, Period and Phase (in the same unit as the period, usually km/s or MHz) of a trial sinusoid. Minimization will be done including also a linear baseline in addition to the sinusoid. Zones defined by the SET WINDOW command are not used to fit the baseline. BASE LAST will use the last determined baseline instead of computing a new one. It can be useful to find a baseline from one backend and apply it to another. This also applies for sinusoidal baselines. /PLOT plots this baseline after the minimization. BASE /CONTINUUM will divide the spectrum by the baseline rather than substracting it. This is useful to keep the continuum level, when continuum is present and variations of atmospheric emission are properly substracted out by fast enough switching. This is of course the case for correlation spectra (e.g. coming from an interferometer). The continuum level will be adjusted to the value of the argument `flux', if present; e.g. /CONTINUUM 1.0 will produce a spectrum of line-to- continuum ratio. BASE /CONTINUUM does not work with BASE LAST or BASE SINUS. For On-The-Fly scans, BASE subtracts a basline on all the individual spectra. 1 BOX LAS\BOX [Arg1] [Arg2] [Arg3] [Arg4] [/UNIT Type [UPPER]] BOX draws a frame for the spectra; the units and limits are determined according to the options of the SET command (SET MODE ; SET UNIT), and the box size governed by SET BOX. The first two arguments are used to modify the labelling of the lower and left axes respectively. They may take the values P for parallel labels (default for X axis), O for Orthogonal labels (default for Y axis) or N for No labels. A third argument is available to indicate that the ticks are to be In or Out of the box. The fourth argument, if present indicates for which axis labels should be plotted. Possible values are X, Y and None. If the option /UNIT is present, it modifies (with no permanent action) the units of the X axis, or only of the upper X axis if UPPER is specified. Type may be also IMAGE to get image-side-band frequency units. For Continuum data, the /UNIT command has no effect, but the unit is controlled by the SET ANGLE command. 1 CALIBRATE LAS\CALIBRATE [KEY val] [KEY val] ... This command show the calibration parameters if given without arguments. Called with a list of arguments in the form "KEY value", where KEY stands for BEAM_EFF, FORWARD_EFF, GAIN_IMAGE, H2O, P_AMB, T_AMB, T_CHOPPER or T_COLD, and value is the corresponding value for, respectively, a (new) Beam efficiency, Forward efficiency, Image/Signal gain ratio, mm of water vapor, ambient temperature, hot load (chopper) temperature, cold load temperature, will recompute the calibration, update the header and rescale the spectrum accordingly. 1 DROP LAS\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 LAS\DUMP [Argument] A debugging command no longer used very much. Without an argument, it lists a certain number of informations about the R Observation header (A CERTAIN number doesnot mean ALL, although it should...). With "D[ATA]" as argument, it lists in addition the data values. With "F[ILE]" as argument, it lists information about the input and output file, and finally with "I[NDEX]", it lists information about the current index. 1 FILE LAS\FILE Type Name [NEW] 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. The default extension can be specified using command SET EXTENSION (.BUR is recommended). 1 FIND LAS\FIND [Append] [New_Data] [/ALL] [/LINE Lname] [/NUMBER n1 n2] [/OFFSET o1 o2] [/SCAN s1 s2] [QUALITY q] [/RANGE w e s n] [/SOURCE Sname] [/TELESCOPE Tname] 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: /ALL all versions of each scan are searched for (if not present: only the last version) /LINE Lname search by line name /NUMBER n1 n2 search for the specified range of observation numbers /SCAN s1 s2 search for the specified range of scan numbers /OFFSET a1 a2 search for these offsets /QUALITY q search for the data of quality better than Q /RANGE w e s n search for the specified range of offsets /SOURCE Sname search by source name /TELESCOPE Tname search for the telescope used 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 CLASS format (Pico Veleta, Plateau de Bure) to use CLASS 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 FOLD LAS\FOLD Folds frequency-switched spectra. 1 GET LAS\GET [N] 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. 1 HEADER LAS\HEADER Displays some header information on the R 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) - General information line: Scan number and version Source name Line name Telescope name Date of observation Date of last reduction - 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, Az) - Quality information line: Quality of calibration (as defined by a SET QUALITY) Tau: opacity at zenith Tsys: system temperature (outside atmosphere). Time: total integration time on source (minutes) El: elevation of source - Spectral information lines (2): N: number of channel I0: reference channel (real) V0: velocity at reference channel Dv: velocity resolution (signed) F0: rest frequency at reference channel Df: frequency resolution (signed) Fi: image frequency at reference channel - Calibration information line: B_ef : Beam efficiency of telescope F_ef : Forward efficiency of telescope G_im : Gain in image band - 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 - Continuum Drift information lines (2) : N: Number of points I0: Reference point A0: Angle offset at reference point Da: Angular spacing between points (signed). F0: Observing frequency Df: Band pass Pos. Ang. : Position angle of the drift. followed by the list of Scan numbers added in the observation. 1 IGNORE LAS\IGNORE List_of_Observations This command can be used to declared the specified list of Observations (from the INPUT file) to be ignored in all FIND operations. They effectively become invisible to CLASS (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 Language LAS\ Command Language Summary ACCUMULATE : Add R and T observation. BASE [arg] : Subtract a baseline. BOX : Draw a frame for data. CALIBRATE : [Re-]Calibrates a spectrum. 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. FOLD : Folds a Frequency Switched spectrum. 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. LIST [name] : List header information about an ensemble of scans. MODIFY : Edit and change the scan header. MULTIPLY fact : Multiply the R spectrum by fact. NEW_DATA : Wait until new data present in input file. PLOT : Plot the observation in R, with box and title. SAVE [name] : Save the current parameters. SET : Enter a value for a parameter. SHOW Arg : Display some parameter. SPECTRUM [Yoff] : Plot the R observation. SUM : Add up all the observations of the current index. SWAP : Exchange the contents of the R and T buffers. TAG Qual List : Change the quality of scans in the Output file. TITLE : Write a header above the plotted frame. UPDATE : Update R in the output file. WRITE [Scan] : Write R in the output file. 2 NEWS - Exit LAS, welcome CLASS: support for continuum data. - Quality flag for scans: new commands IGNORE and TAG, command DELETE has been deleted. 1 LIST LAS\LIST [Name] [/BRIEF] [/LONG] [/OUTPUT File] 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. /BRIEF : Brief format (Observation numbers and version numbers) /LONG : Long format /OUTPUT File : Send the list to a disk file instead of the terminal 1 MODIFY LAS\MODIFY Item [Values...] This is a general purpose command to edit and change the current observation header. Some actions are merely presentation "details", others do affect the information in the observation. Among these, RECENTER, WIDTH, IMAGE and SWITCH_MODE are typically used only when the software did not agree with the hardware when the spectra was taken (i.e. when the information in the observation header is wrong). They should be used with caution. MODIFY actions are limited. You should use the SIC\ command LET to modify header variables which are not available within the MODIFY command (Caution: this is the rope to hang you). 2 FREQUENCY LAS\MODIFY FREQUENCY Rfreq Compute the velocity scale corresponding to a new rest frequency Rfreq. The sky frequency scale is not modified. 2 OFFSETS LAS\MODIFY OFFSETS O1 O2 Change the offsets. This may be required when you average spectra from different offsets, because the resulting "position" is meaningless (usually the position of the first observation added). 2 BLANKING LAS\MODIFY BLANKING NewBlank Change the blanking value in both header and data. This may be required before you can build a consistent strip or cube, specially if the spectra were initially loaded from a FITS tape. 2 RECENTER LAS\MODIFY RECENTER Rrchan Change the reference channel in order to change the velocity, frequency and image frequency scales. The sky frequency scale is also altered in this command. 2 BANDS LAS\MODIFY BANDS Exchange signal and image bands. This allows line fitting on image band for example. Currently, the spectrum is not rescaled even if the band ratio is not 1. 2 LINENAME LAS\MODIFY LINENAME "New Name" Modify the line name (for bookeeping). 2 VELOCITY LAS\MODIFY VELOCITY Rvoff Compute the image and rest frequencies corresponding to a new velocity (in km/s). The sky frequency scale is unchanged by this command. 2 WIDTH LAS\MODIFY WIDTH Rfres Change the frequency resolution (in MHz). 2 IMAGE LAS\MODIFY IMAGE Rimage Change the image frequency (in MHz). 2 BEAM_EFF LAS\MODIFY BEAM_EFF Value Change the beam efficiency. If the beam efficiency previously had a non zero value, the spectrum is rescaled according to the new value. Otherwise, only the beam efficiency is set to the new value. 2 TELESCOPE LAS\MODIFY TELESCOPE Name Change the telescope name, for instance from IRAM-30M to 30M-MRT. 2 POSITION LAS\MODIFY POSITION Lambda Beta Change the central position for the source. The offsets are also modified, as to be consistent with the new central position. This command is usefull when different parts of one source are mapped relative to several reference positions. 2 SYSTEM LAS\MODIFY SYSTEM System Change the System in which the center of projection (central position of the source) has been defined. Valid systems are GALACTIC, EQUATORIAL, HORIZONTAL and UNKNOWN. This command is typically used for "foreign" data when the SYSTEM information has not been decoded correctly by the conversion package. 2 SWITCH_MODE LAS\MODIFY SWITCH_MODE Switching_mode Nphase Off_1 Time_1 Weight_1 Change the description of the switching mode. This command is typically used for "foreign" data when this information has not been decoded correctly by the conversion package. For each phase, one should specify: - the offset for the phase (in MHz for frequency switching, in current angular unit otherwise). - the duration of the phase (in seconds) - the weight given to phase (arbitrary units) 1 MULTIPLY LAS\MULTIPLY Fact Multiply the R Observation by Fact. MULTIPLY leaves the T Observation unaffected. Note that Tsys is also multiplied by the same (absolute) factor to keep proper weights. If only the data is to be multiplied, use the SIC\LET command on array RY: 1 NEW_DATA [LAS\]NEW_DATA 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. 1 PLOT LAS\PLOT [/SCAN] Display the Observation in R. PLOT is equivalent to the following sequence of commands: CLEAR BOX SPECTRUM TITLE PLOT /SCAN will plot an on-the fly scan as a 2-dimensional image with velocity/frequency in the X axis, record number in the Y axis, intensity being rendered as grey/color scale. Entering command POPUP after PLOT/SCAN enables displaying a single spectrum, selected by clicking with the middle button of the mouse. 1 SAVE LAS\SAVE Name SAVE creates a procedure file of name "Name.CLASS", containing all the current parameters of the program. This file may be executed at any time using the @ command: just type "@ name" after the LAS> prompt, or pass "@ name" as a parameter when invoking CLASS (by typing "CLASS @ name"). This file is composed of standard CLASS commands, and may be edited with any text editor. 1 SET LAS\SET something [value1 [value2 [...]]] [/NOCURSOR] This command is used to set a value for a CLASS parameter. If no argument is given, the default value for the parameter will be restored. 2 DEFAULT LAS\SET DEFAULT Restore most (hopefully all) parameters to their default value. The default values for individual parameters are documented under the corresponding subtopic. 2 PROCESSING The following SET Parameter commands control data processing options: LAS\SET ALIGN Type Range LAS\SET BAD Check LAS\SET BASE arg LAS\SET CALIBRATION [Beam_Tol [Gain_Tol]] or OFF LAS\SET CURSOR Arg LAS\SET MASK [ml1 ml2 [...]] LAS\SET MATCH Tol LAS\SET NOMATCH LAS\SET TYPE CONTINUUM or LINE or SKYDIP LAS\SET VARIABLE Section_Name [Keyword] LAS\SET VELOCITY L[sr]H[eliocentric]A[utomatic] LAS\SET WEIGHT type LAS\SET WINDOW [wl1 wu1 [wl2 wu2 [...]]] 2 DISPLAY The following SET Parameter commands affect data display: LAS\SET CURSOR Arg LAS\SET FORMAT Type LAS\SET LEVEL interactive_min_value logfile_min_value LAS\SET MODE A [Type] LAS\SET PLOT type LAS\SET SYSTEM Type [Equinox] LAS\SET UNIT Lower [Upper] LAS\SET VARIABLE Section_Name [Keyword] LAS\SET VELOCITY L[sr]H[eliocentric]A[utomatic] 2 SELECTION The following SET Parameter commands affect data selection in FIND: LAS\SET ANGLE Unit LAS\SET LINE NAME LAS\SET MATCH Tol LAS\SET NOMATCH LAS\SET NUMBER n1 n2 LAS\SET OBSERVED d1 d2 LAS\SET OFFSETS o1 o2 LAS\SET POSANGLE amin amax LAS\SET QUALITY q LAS\SET RANGE West East South North LAS\SET REDUCED d1 d2 LAS\SET SCAN s1 s2 LAS\SET SOURCE name LAS\SET SYSTEM Type [Equinox] LAS\SET TELESCOPE Name LAS\SET TYPE CONTINUUM or LINE or SKYDIP 2 ALIGN LAS\SET ALIGN Type Range Defines the way the spectra are aligned to be added together. Type may be C[hannel], V[elocity] or F[requency] for spectra, C[hannel] or P[osition] for drifts. The range may be I[ntersect] or C[omposite]. The default is CHANNEL INTERSECT. This means that continuum drifts in opposite directions are not properly added: ALIGN Position must be specified for that. 2 ANGLE LAS\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 BAD LAS\SET BAD Check Specify the way ACCUMULATE and SUM behaves in the case of bad channels. Check may be OR or AND. Default is OR, i.e. the output channel is bad if any of the input channels is bad. 2 BASELINE LAS\SET BASELINE arg Specify the degree of polynomial baselines to be subtracted. Default is 1. 2 CALIBRATION LAS\SET CALIBRATION [Beam_Tol [Gain_Tol]] or OFF Specify the tolerance on the Beam efficiency (Beam_Tol) and gain image ratio (Gain_Tol), on turn or calibration checking. A value of 0 means no check. The default values are 0.02 and 0 respectively. These values are used by command SUM to verify that the calibration is coherent, and by command WRITE which writes the corresponding information in the output file only if Beam_Tol is non zero. Note that because the beam efficiency is less than 1, you could use Beam_Tol=1 to suppress the calibration checking but still write the information. 2 COORDINATES LAS\SET COORDINATES [Automatic|Galactic|Equatorial] Specify the system used when displaying the absolute coordinates of the source. 2 CURSOR LAS\SET CURSOR Arg Activates or deactivates the use of cursor for the commands SET WINDOW, SET MASK, SET MODE and LINES, according to the value of Arg: ON or OFF. Default is OFF. 2 EXTENSION LAS\SET EXTENSION Ext Defines the default extension for input and output files. Default is .BUR. 2 FIND LAS\SET FIND UPDATE|NOUPDATE FIND will check (or not) for new scans in the input file (see FIND New_Data). 2 FORMAT LAS\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 LAS\SET FORMAT Keyword [ON] [OFF] (ON to write the information corresponding to the specified keyword, OFF to ignore it). The keywords are - 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 channel, reference channel, velocity and resolution, signal and image frequency and resolution. - CALIBRATION for the beam and forward efficiencies and the gain image ratio. - ATMOSPHERE for the water vapor content, pressure, temperatures and opacities in signal and image bands. - CONTINUUM for continuum drift information - ORIGIN for the list of added scans. The default is Position - Quality - Spectral for spectra, Position - Quality - Continuum for drifts. A line of general information is always written in any case. 2 LEVEL LAS\SET LEVEL interactive_min_value logfile_min_value Sets the level (0 to 10) of informational messages returned to the user in interactive mode and in the message file (CLASS.MES). The level attributed to a message (i.e., a warning message, an error message, a severe-error message) is somewhat dependent of the good humor of the programmer, but typically aknowledgement messages range 0-2, warnings 3-5, errors 6-8, severe-errors 9-10. To prevent printing of message milder than 7 at interactive level and 4 in CLASS.MES, type LAS\SET LEVEL 7 4 2 LINE LAS\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 MASK LAS\SET MASK [ml1 ml2 [...]] Defines a mask for the Gaussian fits by its boundaries. The cursor will be used to specify missing arguments if SET CURSOR is ON, unless option /NOCURSOR is present. When using the cursor, enter: N to enter a value, C to cancel the last entry, H for help, E for exit. Default is no mask. The boundaries are in current unit. 2 MAP LAS\SET MAP [Clear|Normal] Will Clear (or Not) the screen before processing a MAP command. However, a "MAP Where" command does not clear the screen even in a "LAS\SET MAP Clear" mode. 2 MATCH LAS\SET MATCH Tol Turn on the checking of position-matching in ACCUMULATE. Tol is the position tolerance in current units. The default is SET MATCH 2 (arcsec). The tolerance is also used in FIND, MAP and a few other commands such as CUBE. 2 MODE LAS\SET MODE A [Type] Select the scale mode for axis A (X or Y). The mode can be TOTAL (all data plotted), AUTO (limits as found in the input file), or Amin, Amax for fixed limits. If no Type argument is given, the graphic cursor will be invoked to define the limits if SET CURSOR ON is selected. The default is AUTO. 2 NOMATCH LAS\SET NOMATCH Turn off checking of position-matching in ACCUMULATE and SUM. This does not change the tolerance for the other functions like FIND and MAP. 2 NUMBER LAS\SET NUMBER n1 n2 FIND will select all Observations with numbers between n1 and n2. Default is * *. 2 OBSERVED LAS\SET OBSERVED d1 d2 FIND will select all Observations with observing dates between d1 and d2. Dates are specified as DD-MMM-YYYY (i.e. 14-JUL-1789). Default is * *. 2 OFFSETS LAS\SET OFFSETS o1 o2 FIND will select all observations with offsets within the specified tolerance (SET MATCH) of o1 and o2. See also SET RANGE. Default is * * (select all offsets). 2 PLOT LAS\SET PLOT type Set the plotting type for the spectra: N[ormal] for broken lines, or H[istogram]. Default is normal (50% faster plot). 2 POSANGLE LAS\SET POSANGLE amin amax Specify the position angle range (continnum drifts only) for subsequent searches. 2 QUALITY LAS\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 LAS\SET RANGE West East South North FIND will select all observations with offsets in the specified range. Default is * * * *. 2 REDUCED LAS\SET REDUCED d1 d2 FIND will select all observations with reduction dates between d1 and d2. Dates are specified as DD-MMM-YYYY (i.e. 14-JUL-1789). Default is * *. 2 SCAN LAS\SET SCAN s1 s2 FIND will select all observations with Scan numbers between s1 and s2. The Scan number, attributed by the on-line acquisition system may be different from the observation number which is used by CLASS to refer to the observations. Default is * *. 2 SOURCE LAS\SET SOURCE name FIND will select all scans according to the specified source name. Default is *. Syntax like NAM* can be used to find all observations with source name beginning by NAM. 2 SYSTEM LAS\SET SYSTEM Type [Equinox] Specify the coordinate system to be used. Type may be E[quatorial] followed by an epoch, G[alactic], or A[utomatic]. Default is Auto, i.e. uses the type found in the data file. If the equinox of Equatorial coordinates is not specified, the previous value is used. The initial default is 1950.00. Coordinates and offsets are automatically converted to the specified coordinate system and precessed to the specified epoch if needed. 2 TELESCOPE LAS\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 TYPE LAS\SET TYPE CONTINUUM or LINE or SKYDIP Defines on which type of data the program is working. - LINE (or SPECTROSCOPY) (the default when entering LAS) selects Spectral Line data only, and the program prompt is LAS> (Line Analysis System). - CONTINUUM selects continuum drifts results only, and the program prompt changes to CAS> (Continuum Analysis System). - SKYDIP selects only skydips, and the prompt changes to SAS> In CONTINUUM mode, a continuum drift is treated as a spectrum would be in LINE mode. You can add drifts, subtract baseline, make gauss fits, change plotting scales etc... The current angular units is used in plots. SKYDIP mode has very limited capabiblities: only command REDUCE may be used to analyse the SKYDIP results. 2 UNIT LAS\SET UNIT Lower [Upper] Specify the unit to be used for the lower and upper X axis. Allowed units are C[hannel], F[requency], [Image] and V[elocity]. Default is Velocity. For Continuum drifts, this unit is ignored, but the angular unit specified by SET ANGLE is used. 2 VARIABLE LAS\SET VARIABLE Section_Name [Keyword] Declare SIC variables corresponding to section of the header of the R observation. The header sections are POSITION, SPECTRO, BASE, HISTORY, PLOT, FSWITCH, CALIBRATION, SKYDIP, GAUSS, SHELL, NH3 (or HFS), DRIFT, BEAM, and CONTINUUM. Defining these SIC variables allows to access the header for mathematical computations using SIC facilities. All variables are declared as readonly, unless Keyword WRITE is specified as third argument. If Keyword OFF is specified, the corresponding SIC variables are deleted (to save space since the total number of SIC variables is limited). The SIC variables have the name of the corresponding FORTRAN variables stripped from the first character (always R in the FORTRAN code). They are defined below GENERAL General parameters, always present: INTEGER MGEN INTEGER MGEN2 PARAMETER (MGEN=9,MGEN2=11) INTEGER RNUM ! Observation number INTEGER RVER ! Version number INTEGER RTELES(3) ! Telescope name INTEGER RDOBS ! Date of observation (code) INTEGER RDRED ! Date of reduction (code) CHARACTER RCDOBS ! Date of observation (in clear) CHARACTER RCDRED ! Date of reduction (in clear) INTEGER RTYPEC ! Type of coordinates INTEGER RKIND ! Type of data INTEGER RQUAL ! Quality of data INTEGER RSCAN ! Scan number REAL*8 RUT ! UT of observation REAL*8 RST ! LST of observation REAL*4 RAZ ! Azimuth REAL*4 REL ! Elevation REAL*4 RTAU ! Opacity REAL*4 RTSYS ! System temperature REAL*4 RTIME ! Integration time POSITION Position information: INTEGER MPOS PARAMETER (MPOS=11) INTEGER RSOURC(3) ! Source name REAL*4 REPOCH ! Epoch of coordinates REAL*8 RLAM ! Lambda REAL*8 RBET ! Beta REAL*4 RLAMOF ! Offset in Lambda REAL*4 RBETOF ! Offset in Beta INTEGER RPROJ ! Projection system SPECTRO Spectroscopic information (for spectra) INTEGER MSPEC PARAMETER (MSPEC=18) INTEGER RLINE(3) ! Line name REAL*8 RRESTF ! Rest frequency INTEGER RNCHAN ! Number of channels REAL*4 RRCHAN ! Reference channels REAL*4 RFRES ! Frequency resolution REAL*4 RFOFF ! Frequency offset REAL*4 RVRES ! Velocity resolution REAL*4 RVOFF ! Velocity at reference channel REAL*4 RBAD ! Blanking value REAL*8 RIMAGE ! Image frequency INTEGER RVTYPE ! Type of velocity REAL*8 RSKYFR ! Sky frequency REAL*4 RVTELES ! Velocity of telescope /reference frame BASE Baseline information (for spectra of drifts) INTEGER MWIND INTEGER MBASE PARAMETER (MWIND=20,MBASE=4+2*MWIND) INTEGER RDEG ! Degree of last baseline REAL*4 RSIGFI ! Sigma REAL*4 RAIRE ! Area under windows INTEGER RNWIND ! Number of line windows REAL*4 RW1(MWIND) ! Lower limits of windows REAL*4 RW2(MWIND) ! Upper limits of windows HISTORY Scan numbers of initial observations INTEGER MSEQ INTEGER MORIG PARAMETER (MSEQ=100,MORIG=2*MSEQ+1) INTEGER RNSEQ ! Number of sequences INTEGER RSTART(MSEQ) ! Start can number of seq. INTEGER REND(MSEQ) ! End scan number of seq. PLOT Default plotting limits. INTEGER MPLOT PARAMETER (MPLOT=4) REAL*4 RAMIN ! Min Y value plotted REAL*4 RAMAX ! Max Y value plotted REAL*4 RVMIN ! Min X value plotted REAL*4 RVMAX ! Max X value plotted FSWITCH Frequency switching information (for spectra) INTEGER MXPHAS INTEGER MFSW PARAMETER (MXPHAS=8,MFSW=2+6*MXPHAS) INTEGER RNPHAS ! Number of phases REAL*8 RDECAL(MXPHAS) ! Frequency offsets REAL*4 RDUREE(MXPHAS) ! Time per phase REAL*4 RPOIDS(MXPHAS) ! Weight of each phase INTEGER RSWMOD ! Switching mode (frequency, position...) REAL*4 RLDECAL(MXPHAS) ! Lambda offsets REAL*4 RBDECAL(MXPHAS) ! Beta offsets of each phase CALIBRATION Calibration parameters INTEGER MCALIB PARAMETER (MCALIB=21) REAL*4 RBEEFF ! Beam efficiency REAL*4 RFOEFF ! Forward efficiency REAL*4 RGAINI ! Image/Signal gain ratio REAL*4 RH2OMM ! MM of water vapor REAL*4 RPAMB ! Ambient pressure (hPa) REAL*4 RTAMB ! Ambient temperature (K) REAL*4 RTATMS ! Atmosphere temp. signal band REAL*4 RTCHOP ! Chopper temperature REAL*4 RTCOLD ! Cold load temperature REAL*4 RTAUS ! Opacity signal band REAL*4 RTAUI ! Opacity image band REAL*4 RTATMI ! Atmosphere temp. image band REAL*4 RTREC ! Receiver temperature INTEGER RCMODE ! Calibration mode REAL*4 RATFAC ! Applied calibration factor REAL*4 RALTI ! Site elevation REAL*4 RCOUNT(3) ! Power of Atm., Chopp., Cold REAL*4 RLCALOF ! Longitude offset for sky measurement REAL*4 RBCALOF ! Latitude offset for sky measurement SKYDIP For Skydips observations. No associated data. INTEGER MSKY INTEGER MSKYDIP PARAMETER (MSKY=10,MSKYDIP=10+4*MSKY) INTEGER RSLINE(3) ! Line name REAL*8 RSREST ! Rest frequency REAL*8 RSIMAG ! Image frequency INTEGER RNSKY ! Number of points on sky INTEGER RNCHOP ! - - - - chopper INTEGER RNCOLD ! - - - - cold load REAL*4 RELEV(MSKY) ! Elevations REAL*4 REMISS(MSKY) ! Power on sky REAL*4 RCHOPP(MSKY) ! Power on chopper REAL*4 RCOLD(MSKY) ! Power on cold load GAUSS Gauss fit results (for spectra or drifts) INTEGER MXGAUS INTEGER MFIT PARAMETER (MXGAUS=5,MFIT=3+6*MXGAUS) INTEGER RNLINE ! Number of components REAL*4 RSIGBA ! Sigma on base REAL*4 RSIGRA ! Sigma on line REAL*4 RNFIT(3*MXGAUS) ! Fit results REAL*4 RNERR(3*MXGAUS) ! Errors SHELL "Stellar shell" profile fit results (for spectra) INTEGER MSHELL PARAMETER (MSHELL=43) INTEGER RLSHEL ! Number of components REAL*4 RBSHEL ! Sigma on base REAL*4 RRSHEL ! Sigma on line REAL*4 RNSHEL(20) ! Fit results REAL*4 RESHEL(20) ! Errors HFS "Hyperfine Structure" profile fit results (for spectra, ex: NH3, HCN) INTEGER MNH3 PARAMETER (MNH3=27) INTEGER RLNH3 ! Number of components REAL*4 RBNH3 ! Sigma on base REAL*4 RRNH3 ! Sigma on line REAL*4 RNNH3(12) ! Fit results REAL*4 RENH3(12) ! Errors ABS "Hyperfine Structure" ABSORPTION profile fit results (for spectra, ex: NH3, HCN) INTEGER MABS PARAMETER (MABS=35) INTEGER RLABS ! Number of components REAL*4 RBABS ! Sigma on base REAL*4 RRABS ! Sigma on line REAL*4 RNABS(16) ! Fit results REAL*4 REABS(16) ! Errors DRIFT Continuum drift description (for drifts) INTEGER MCONT PARAMETER (MCONT=16) REAL*8 RFREQ ! Rest frequency REAL*4 RWIDTH ! Bandwidth INTEGER RNPOIN ! Number of data points REAL*4 RRPOIN ! Reference point REAL*4 RTREF ! Time at reference REAL*4 RAREF ! Angular offset at ref. REAL*4 RAPOS ! Position angle of drift REAL*4 RTRES ! Time resolution REAL*4 RARES ! Angular resolution REAL*4 RCBAD ! Blanking value INTEGER RCTYPE ! Type of offsets REAL*8 RCIMAG ! Image frequency REAL*4 RCOLLA ! Collimation error Az REAL*4 RCOLLE ! Collimation error El BEAM Beam-switching parameters (for spectra or drifts) INTEGER MBEAM PARAMETER (MBEAM=5) REAL*4 RCAZIM ! Azimuth of observation REAL*4 RCELEV ! Elevation of observation REAL*4 RSPACE ! Beam spacing REAL*4 RBPOS ! Position angle of beams INTEGER RBTYPE ! System for angle CONTINUUM Double gaussian and baseline fit results (for drifts) INTEGER MFCONT PARAMETER (MFCONT=19) INTEGER RLCONT ! Number of components REAL*4 RBCONT ! Sigma on base REAL*4 RRCONT ! Sigma on line REAL*4 RNCONT(8) ! Results REAL*4 RECONT(8) ! Errors 2 VELOCITY LAS\SET VELOCITY L[sr]H[eliocentric]A[utomatic] Forces the velocity axis values to Lsr or Heliocentric values. Automatic reverts to the default mode, where the velocity type is taken from the header of the spectrum. 2 WEIGHT LAS\SET WEIGHT type Weighting to be used for summations: T[ime], E[qual] or S[igma] (for 1/sigma**2). The default is TIME. Sigma is not recommended unless you just made a baseline fit before. Equal behaves differently in SUM (produces the average) and ACCUMULATE (produces the SUM). 2 WINDOW LAS\SET WINDOW [wl1 wu1 [wl2 wu2 [...]]] Defines one or several line windows to be avoided by BASE when fitting a baseline. The cursor will be used to specify missing arguments if SET CURSOR is ON, unless option /NOCURSOR is present. When using the cursor, enter: N to enter a value, C to cancel the last entry, H for help, E for exit. The boundaries are in current unit. There is no default. 1 SHOW LAS\SHOW Arg Display some parameter defined by SET. Arg can be "ALL" to display all parameters specified by SET. See SET command. 1 SPECTRUM LAS\SPECTRUM [Yoff] Plots the spectrum in the R buffer in the units and scales defined by SET UNIT and SET MODE. Yoff (unit Kelvins, default 0) is a constant Y- offset added to the plotted values (useful to compare two spectra). 1 SUM LAS\SUM Adds all the spectra of the current index using the current weighting function (SET WEIGHT) and alignment mode (SET ALIGN). The position coincidence will be checked according to SET MATCH. The homogeneity of calibration is checked according to SET CALIBRATION. Bad channels are handled according to SET BAD. A sum may be interrupted by <^C>, but the results is then undefined. If the data are On-The-Fly scans, all the individual positions are averaged. 1 SWAP LAS\SWAP Exchange the contents of the R and T buffers. 1 TAG LAS\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 Should never exist 9 Reserved for deleted Observations 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 TITLE LAS\TITLE [/BRIEF] [/LONG] Writes the header of the Observation currently in R above the plotted data. The format used is the one selected by SET FORMAT, which may be temporarily overridden by the options. 1 UPDATE LAS\UPDATE Update the LAST version of the observation in the R buffer in the output file ; the update OVERWRITES the observation. If more space is needed (e.g., the new version has more header information), an error is returned. You MUST then WRITE the observation to avoid loss of information. You can update only last versions. This command MUST BE USED WITH CAUTION ; in case of complex manipulations of observations, you may get confused and erase precious data. The only typical case where it may be used is in the following sequence: GET Number GAUSS or MODIFY UPDATE 1 WRITE LAS\WRITE [observation] Writes the observation in the R buffer onto the output file ; if a version of this observation is already in the file, a new version of the observation is created. A new observation number can be specified as argument. The information written depends on the operations done on the observation. Existing fit results are written. The calibration information is written only if the calibration is checked (see SET CALIBRATION command). 1 END