
1 CATALOG
        [ASTRO\]CATALOG name [/VELETA] [/ALTERNATE]

    Open  the  catalog  file  specified by ’name’. Default file extension is
    .SOU.  Some standard catalogs are available  in  the  directory  GAG_AS‐
    TRO_DATA: and may be used as examples:
        SIO.SOU contains SiO masers used for pointing.
        CONTINUUM_1.SOU contains "strong" continuum sources (Flux > 8 Jy)
        CONTINUUM_2.SOU  contains weaker sources, still useable for pointing
        (Flux > 3 Jy).
        PHASE‐2000.SOU contains the phase calibrators  of  Plateau  de  Bure
        (Flux > 0.1 Jy)
    The  catalog  format  is described in the ASTRO manual and summarized in
    the subtopic FORMAT.

    CATALOG with no arguments will display the catalogs currently opened.

2 /VELETA
        This option will open the catalog file ’name’.CAT, assuming it  fol‐
    lows  the  format of OBSINP catalogs in use on the 30m Radiotelescope of
    IRAM.  A file ´name’.SOU will be created in the current directory in the
    Plateau  de  Bure format, so that this option needs to be specified ONLY
    ONCE for each catalog. Fancy options such as SL0P, SB0P ... are not sup‐
    ported.

2 /ALTERNATE
        This option will open the specified catalog as a second catalog, on‐
    ly accessible through the "/ALTERNATE" options of commands SOURCE, HORI‐
    ZON,  and  CONVERT.  For  instance,  a catalog containing calibration or
    pointing sources may be opened as an Alternate catalog,  while  the  ob‐
    jects  to study are kept in the Current catalog, enabling easy switching
    between the two kinds of objects.

2 FORMAT
        In the Plateau de Bure format each source uses one line of the cata‐
    log  file.   Each line should contain the following consecutive keywords
    (some may be omitted):
     1) Source name field:
       The source name field is a composite item which can accomodate several
       names for a single source. Names should be separated by a vertical bar
       ( | ) with no embedded spaces, e.g.: B0415+379|3C111
       Each name must have at most 12 characters.
     2) Coordinate system: 2 characters, optional, may be:
          EQ for equatorial coordinates. If "EQ" is given explicitely,
                                 then the Epoch  keyword is mandatory.
          GA for Galactic II coordinates.
          EC for J2000 Ecliptic coordinates
          HO for horizontal coordinates
          DA for equatorial, present‐day coordinates.
     3) Epoch:  needed for equatorial coordinates after "EQ" keyword.
     4) Longitude‐like coordinate: in degrees, except for EQ and DA where it
        should be in hours. Format is
              hh:mm:ss.sss[,first[,second]]
        where
              "hh:mm:ss.sss" is a generalized sexagesimal format
                (hh:mm:ss.sss or dd.ddd or hh:mm.mmm)
              "first" is an (optional) first order time derivative
              "second" is an (optional) second order time derivative
     5) Latitude‐like coordinate: in degrees, same format as above.

     the following OPTIONAL KEYWORD Value(s) series, which may be listed in
     any order:

     A) a "Velocity" keyword
         Velocity Value
            where "Velocity" is an alphabetic code, equal to "LSR", "HELIO"
            or "EARTH". HELIO actually means: referred to the Solar System
            barycenter. Value is the velocity in km/second, in the corresponding
            reference frame. Default is zero.
     B) an "Intensity" keyword
         FLUX  Value [Index]
             Value is the flux in Jy. Index is an optional spectral index
         Mx  Value
             Value is the magnitude, Unknown values can be coded 99.99
             Mx can be MAGNITUDE, or x is one of V,R,I,J,H,K,L,M,N to indicate
             the visual band
     C) a "Project" keyword
         PROJECT ProjectID
            to specify a project identification (a string without spaces)
     D) an "hour" keyword to indicate the validation hour for the coordinates
        (which is useful when time  derivatives are given), specified by
         HOUR Value
     E) A "Parallax" keyword
         PARALLAX Value
              Value is in arcsec.

    Any other keyword will be ignored

1 CONSTELL
        [ASTRO\]CONSTELL [/DRAW [m] [l] [s]] [/NAME] [/BOUNDARIES]

    Plots in the current FRAME with the current FONT, MARKER  and  PEN,  the
    constellations,  i.e.,  the  main stars of all the constellations with a
    marker size adequately depending on the magnitude.  The options are:
     /DRAW [m] [l] [s]
     "m" will cause markers at the star’s positions to be plotted
     "l" will cause the constellations outlines to be plotted
     "s" will cause the star’s names to be plotted (using current centering and
         character size)
     /NAME will draw the constellation’s names
     /BOUNDARIES will draw the constellation boundaries (originally constant RA
         and DEC at 1875 epoch, they are precessed to the current epoch).
         The current code is quite slow.
    This command makes use of the logical name GAG_CONSTELL which points  to
    a  GILDAS  Table  containing  the stars positions and drawing codes, and
    GAG_CONST_BOUND which defines the constellation boundaries.

1 CONVERT
        [ASTRO\]CONVERT  [Catalog_Name]  [/ALTERNATE]  [/J2000  [Obs_epoch]]
    [/PRECESS  [New_epoch]]  [/GALACTIC] [/FLUX fmin] [/NAME ncname [iname]]
    [/INPUT POS|FLUX filename pos]

    Change catalog format or epoch.

    Without any option (or with option  /ALTERNATE)  and  without  argument,
    this command creates an OBSINP‐compatible copy of the ’name’.SOU catalog
    (or Alternate  catalog  if  /ALTERNATE  is  specified)  under  the  name
    ’name’.CAT.

    With  the  /J2000  and/or  /PRECESS option, the command will precess the
    current SOU catalog to J2000 system, using the specified epochs for  ob‐
    servation (Obs_epoch, default 1950) and final result (New_epoch, default
    2000). The output catalog is ’Catalog_name’.SOU, and  has  the  standard
    format.

    /FLUX  create  a  copy  of the current catalog with only sources of flux
    larger than fmin

    /NAME ncname [iname]: reserve ncname characters for names  field.   With
    iname.gt.0, a standard name (Jhhmmmsddmmm) is created and put in inameth
    positions in the list of names.

    /INPUT FLUX filename : will take fluxes from filename, which has  itself
    the format of a catalog (both input catalog and filename are assumed al‐
    phabetically sorted)

    /INPUT POSITION filename dpos : will take positions  from  filename,  if
    different  by more than dpos arc seconds. Filename has itself the format
    of a catalog (both input catalog and filename are assumed alphabetically
    sorted)

    /ALTERNATE option : do the same operation with the Alternate catalog.

1 FRAME
        [ASTRO\]FRAME System [...]

    This command specifies the reference frame to be used for plots.  System
    may be HORIZONTAL or EQUATORIAL (at epoch defined by TIME command) If no
    other  argument  is  given,  plotting is done in rectangular coordinates
    representing Azimuth Elevation or Right Ascension Declination.  If other
    arguments are given, a Stereographic projection is used.
      ‐ FRAME EQUATORIAL Ra Dec Size
        the  projection  will  be  centered on Ra and Dec (hours ‐ degrees);
        Size in degrees specify the plotting range (e.g.  180  for  a  whole
        hemisphere: the default)
      ‐ FRAME HORIZONTAL Az El Size
        same thing, but Az and El are in degrees.
      ‐ FRAME HORIZONTAL Center
        will  plot  a  hemisphere  in horizontal system, where Center may be
        ZENITH, NORTH, EAST, SOUTH or WEST.

1 HEADER
        [ASTRO\]HEADER

    Write the UTC and LST times on top of plot, as well as  the  observatory
    coordinates.  Lists more information on the alphanumeric screen, in par‐
    ticular the Start and End of Twilights and some moon phase information.

1 HORIZON
        [ASTRO\]HORIZON h1 h2 ... [/SOURCE ... ] [/PLANET ...  ]  [/AIRMASS]
    [/FLUX    Fmin    Fmax]   [/PROJECT]   [/NIGHT_MARKS]   [STATIONS   ...]
    [/TIME_STAMP\ [ut|lst]] [/DELAY_LINE ...]

    This command is used to produce plots of LST  ranges  of  observability,
    above  specified elevations, of sources and planets. A line is drawn for
    all hours when the object is visible above elevation h1; tick marks  and
    labels  are  provided for elevations h1, h2, ... (in degrees), or corre‐
    sponding air masses values (with /AIRMASS option). Elevation values must
    be  in  increasing  order, or airmasses in decreasing order. UTC axis is
    drawn on top of the plot. A label with date and observatory  coordinates
    is plotted.
      /SOURCE                  will plot on one page all sources
                               of the Current (by default) or Alternate
                               (optionally) catalog.
      /SOURCE name1 name2 ...  will be restricted to the specified sources
      /SOURCE NEXT n           will plot the next n sources in the current
                               catalog; (repeat this command to avoid over‐
                               crowded pages)
      /ALTERNATE               with /SOURCE, will use the Alternate catalog.
      /FLUX Fmin Fmax          restrict the search to sources with flux in
                               the specified range.

      /PLANET                  will plot on one page all solar‐system bodies
      /PLANET name1 name2 ...  will be restricted to the specified bodies

      /NIGHT_MARKS             Plots also the beginning and end of Astronomical,
                               Nautical and Civil Twilights, and an estimate of
                               The moon phase and the moon bolometric magnitude.
           ‐‐‐‐‐‐Options related to interferometers with delay lines ‐‐‐‐
      The use of these option create a second ’observability line; in the plot
      that correspond to the limits permitted by the stroke of the various
      delay lines.
      /STATIONS station1 station2 [station3 [...]]
       or
      /STATIONS E00‐W34‐N56‐N64‐E32 define the name of the Stations used (see
                                HELP UV_TRACK). Stations names can be
                                entered separated by blanks or in the form of
                                ONE configuration (names separated by ’‐’).

      /DELAY_LINE dl1 dl2 dl3 ...
       or
      /DELAY_LINE dl1‐dl6‐dl4   defines which delayline (see HELP UV_TRACK) is
                                affected to the corresponding station in the
                                station list or configuration.
      /TIME_STAMP [UT|LST]      plots the entry and exit LST (default) or UT
                                time in the delay lines and above minimum elevation.

1 DELAY_LINE
        [ASTRO\]DELAY_LINE Station1 Station2  ... [/NIGHT_MARKS]
     [/THROW ...] [/TIME_STAMP [ut|lst]]  [/DELAY_LINE dl1 dl2 ...]

    This  command  is  used  for interferometers with optical delay lines to
    produce plots of LST/UT ranges of observability of ONE source, for  each
    delay  line associated with the telescopes (here we mostly deal with op‐
    tical  interferometers!)  listed  by  Station1,  Station2...  See   HELP
    UV_TRACK  for  more  information about the list of Stations.  The top of
    plot is the observability limit of the  source  above  horizon.  Follows
    then,  for  each  delay line used by the array of telescopes listed, the
    periods of compatibility with the delay line’s total OPD.  UTC  axis  is
    drawn  on top of the plot. A label with date and observatory coordinates
    is plotted.
      /NIGHT_MARKS             Plots also the beginning and end of Astronomical,
                               Nautical and Civil Twilights, and an estimate of
                               The moon phase and the moon bolometric magnitude.
      /DELAY_LINE dl1 dl2 dl3 ...
       or
      /DELAY_LINE dl1‐dl6‐dl4  defines which delayline (see HELP UV_TRACK) is
                               affected to the corresponding station in the
                               station list or configuration.
      /TIME_STAMP [UT|LST]     plots the entry and exit UT or LST (default)
                               time in the delay lines.

1 Language
                        ASTRO\ Language summary

    The ASTRO\ language contains commands to compute apparent  source  posi‐
    tions on the sky at any time(*) for any place on earth.
    CATALOG name        : opens a standard source catalog
    CONVERT             : convert .SOU catalogs to .CAT or J2000 system
    FRAME               : define plotting reference system
    HORIZON             : plot observability hours of sources and planets
    HEADER              : write time parameters on top of plot
    OBSERVATORY [name]  : load observatory coordinates
    PLANET [name]       : compute planet coordinates
    SOURCE [name]       : compute source coordinates
    SET parameter value : enter some parameter value
    TIME [time [date]]  : set computation time
    UV_TRACKS           : plot interferometer UV tracks
    DELAY_LINE          : deals with delay lines (optical interferometers)
    * Ephemerides must be available for the planets at this time.

1 OBSERVATORY
        [ASTRO\]OBSERVATORY Name
                 or
        [ASTRO\]OBSERVATORY [Name longitude latitude altitude radius]
                 or
        [ASTRO\]OBSERVATORY [longitude latitude altitude radius]

    Specify  an observatory whose coordinates are known, or Enter the obser‐
    vatory geographic coordinates in degrees, and elevation in km above  sea
    level.  CAUTION: East longitudes are positive.  The fourth (fifth) argu‐
    ment is the radius of the Sun avoidance circle, in degrees.

    Without argument, the observatory name is translated  from  the  GAG_AS‐
    TRO_OBS logical name.

    Known  observatories  are  BURE,  CSO, VLA, VLT, IOTA, PTI, GI2T, CHARA,
    COAST, SMA, ALMA.

    Example:  OBSERVATORY MYOBS 44:23:12.0  +45:09:57.9 3.987 30.

    A reasonable system default should be introduced in command file set  as
    the  logical variable ASTRO_LOCAL_INIT. Files describing the observatory
    are expected in the ASTRO_DIR: directory. The presence of  a  file  ’MY‐
    OBS.stations’  means that MYOBS is an interferometer, and this file con‐
    tains the Name, X Y and Z equatorial local positions  of  all  the  sta‐
    tions,  and optionally the optical path in m from the station to a pupil
    plane common to all interferometer beams (where the delay will  be  com‐
    pensated by the delay lines).

    A  file  MYOBS.delayline  could be present giving the name and stroke of
    all the delay lines (even fixed ones, i.e., with a stroke of 0.  A  two‐
    telescope  interferometer  with  only one delayline should define a null
    delayline of stroke 0 to be affected to ). Absence of this file  implies
    that all delays can be compensated.

    Additional  information  on  the fixed OPD setup is searched in the file
    columns, giving for each couple station/dl the fixed opd between the fo‐
    cus  of the primary of the telescope and a reference plane common to all
    beams when the delayline (or pops) is set at DL 0. If a  combination  is
    invalid,  it  suffices  to  indicate  a negative fixed opd such as ‐1E6.
    Some of these OPDS line may in fact be a list of fixed delays  ("pops"),
    the instrument switches when handy. Support for this is contemplated.

    Finally,  each  station  XXX  may be associated with a file named closed
    contour encompassing all the sky visible from the telescope situated  at
    this station. (see the VLT stations files for an example).

    The  variable  FREQUENCY  is  also changed by this command to reasonable
    values for the known observatories (0.6 to 2.5 microns  typically).  Use
    the command "LET FREQUENCY" to tailor the frequency to your needs or de‐
    fine it for unknown observatories. The BEAM variable  used  to  override
    the frequency‐dependent default is reset to zero (value meaning that the
    program should use the default).

1 PLANET
        [ASTRO\]PLANET [name] [/DRAW [...]]

    Compute the coordinates of a Solar System  object.  Known  objects  are:
    SUN,  MOON,  MERCURY,  VENUS, MARS, JUPITER, SATURN, URANUS, NEPTUNE. By
    default, all known objects are plotted if visible.  The Option /DRAW  is
    used  to  plot  the object symbol on the screen.  The planet coordinates
    (apparent RA, apparent DEC, Azimuth and Elevation at  time  of  computa‐
    tion) are typed on the screen.

    PLANET  outputs also the geocentric (DE) and heliocentric (DS) distances
    of the object (in A.U.), the apparent minor and major diameters (Min and
    Maj  in  arcsec.),  the position angle of the central meridian (PA, east
    from north, in degrees), the brightness temperature (TB in K),  and  the
    flux  (S  in Jy) at the current frequency. It also outputs the frequency
    (in GHz), the beam (in arcsec), the main beam temperature  (Tmb  in  K),
    the associated flux (in Jy) and the planet size convolved with the tele‐
    scope beam (size in arcsec).

    The frequency may be entered either through command LINE or by  updating
    variable  FREQUENCY  (in GHz). The beam used in computation is available
    through the READONLY variable PRIMBEAM (in arcsec).  User  may  override
    the  default  used  beam size by setting the BEAM variable to a non‐zero
    value (in arcsec).

    Arguments to /DRAW may be LINE, MARKER, SYMBOL, or FULL:
      LINE   will draw a line from the previously computed position
      MARKER will draw a marker (GreG style defined by GREG\SET MARKER)
              at the computed position
      SYMBOL will draw the planet’s symbol at the computed position
      FULL   will combine MARKER and SYMBOL (the symbol will be offset
             one marker size above the computed position).
    If several arguments are given they will be used in sequence.

1 SET
        [ASTRO\]SET parameter value

    Enter a value for a parameter. Valid parameters are :
      ‐ DUT1
        which is (UT1‐UTC) in seconds of time (from I.E.R.S.)
      ‐ DTDT
        which is (TDT‐UTC) in seconds of time (from I.E.R.S.)
      ‐ AZIMUTH_REFERENCE
        which is either NORTH or SOUTH, and defines the azimuth to  be  zero
        in the North or South direction (to conform to local conventions).
      ‐ FLUX Name Value
        Attribute  the  flux value Flux to the source Name (only for quasars
        or continuum sources which are not planets). This  command  is  used
        when  no  planet measurement is available and/or as a redundant flux
        check on strong and well known quasars or W3OH for example. A  *  as
        flux value frees the source as reference source.
      ‐ SET NAME Argument
        Define  the  naming convention for listing sources from the catalog.
        Sources in the catalog may have several names. This  command  define
        which  name should be printed in commands SOURCE and HORIZON.  Argu‐
        ment can be
            *   to print the name of the source which has been searched for
            ALL to print all the possible names of the source
            1,2,3 etc... to print the first, second, third,  etc..  possible
            names of the source

    Reasonable  system  defaults  may be introduced in the command procedure
    GAG_ASTRO_LOCAL.

1 SOURCE
        [ASTRO\]SOURCE [name [...]] [/DRAW [m]  [l]  [s]  [f]]  [/ALTERNATE]
    [/SUN] [/FLUX Fmin Fmax]

    Compute  the  coordinates  of  a Source from the Current catalog.  If no
    name is specified, all sources of the catalog are selected.  Source  co‐
    ordinates  may also be specified in the command line, in the same format
    as the catalog file.  The /DRAW option is used to draw the  source  name
    on  the  plot  at its current position (Azimuth, Elevation).  The source
    coordinates (RA, DEC, Azimuth and Elevation at time of computation)  are
    printed  on  the  screen, as well as the line‐of‐sight components of the
    following velocities:
      ‐ V(S/OBS)
        Source (S) relative to Observatory
      ‐ V(S/LSR)
        Source (S) relative to Local Standard of Rest. This is the  LSR  ve‐
        locity furnished by the observer as part of the source coordinates.
      ‐ V(LSR/G)
        Local Standard of Rest relative to Solar System Barycenter (G)
      ‐ V(G/OBS)
        Solar System Barycenter (G) relative to the Observatory
    All velocities are in km/s, positive if the distance is increasing. With
    the above convention, we have: V(S/OBS) = V(S/LSR)+V(LSR/G)+V(G/OBS).

    Arguments to /DRAW may be LINE, MARKER, SYMBOL, or FULL, as for  command
    PLANET:
      LINE   will draw a line from the previously computed position
             (SOURCE or PLANET)
      MARKER will draw a marker (GreG style defined by GREG\SET MARKER)
             at the computed position  SYMBOL will draw the source name in capitals at the computed position
      FULL   will combine MARKER and SYMBOL (the name will be offset
             one marker size above the computed position).
    If several arguments are given they will be used in sequence.

    /ALTERNATE will direct the search to the Alternate catalog.

    /SUN will also list the sun avoidance limits

    /FLUX  Fmin  Fmax  will  select  only sources with flux densities in the
    specified range. Marker sizes will be proportional to the (logarithm  of
    the) flux.

    /PRINT  option  will  suppress  the printing of Az and El, and print the
    source characteristics as in catalog instead.

1 TIME
         [ASTRO\]TIME [time [date]] [/ZONE Z] [/UT1] [/TDT] [/NODRAW]

    Specify the time‐date of computation. Time  is  normally  understood  as
    UTC; options /UT1 and /TDT may be used to change this to UT1 or TDT. The
    time format is HH:MM:SS.SSS, and the date format  is  DD‐MMM‐YYYY.  Time
    and date may be absent or replaced by an asterisk (*), which defaults to
    current system time.  Local civil time may be input instead, in conjunc‐
    tion with the option /ZONE z, where z is the difference in hours between
    UT and local civil time (use /ZONE 2 on Plateau de Bure in summer, 1  in
    winter).

    By  default, if the sun is visible, a Sun Avoidance Circle (see HELP OB‐
    SERVATORY) is plotted. It can be suppressed using  the  /NODRAW  option.
    Use HEADER to examine the value of the Sun Avoidance Circle.

1 UV_TRACKS
        [ASTRO\]UV_TRACKS   station1   station2  [station3  [...]]   [/FRAME
    [size]] [/HOUR_ANGLE  Hmin  [Hmax]]  [/TABLE  [Name]]  [/HORIZON  Elmin]
    [/SIZE  size1  nsize1  size2 nsize2 ...] [/INTEGRATION t|now] [/STATIONS
    ALL|list] [/DELAY_LINE ...] [/BANDWIDTH band1start band1end  [band2start
    band2end...]]

    Plot interferometer UV tracks for the most recently called source.  Sta‐
    tions should be referred to by a mnemonic (e.g. E03, W00 ...) or a "con‐
    figuration"  (e.g.  E03‐W00‐N05)  given  as  arguments  of UV_TRACKS.  A
    sketch of the interferometer described by ASTRO_STATIONS is also drawn.
         /FRAME should be used to start a new UV  coverage.  It  clears  the
    plot, draws the box, and open a new table if /TABLE is present.
         /HORIZON specify a minimum elevation (in degrees) for the source.
         /HOUR_ANGLE  can be used to limit the hour angle coverage.  Default
    is from source rise (above the minimum elevation) to source setup.  Hmin
    and Hmax are in decimal hours.
         /TABLE  can be used to write the sampling function (UV coverage) on
    a UV table for further processing such as producing beams using the task
    UV_MAP. Name should be specified only if option /FRAME has been set.
         /INTEGRATION  t  is used to change the time interval between points
    in the u,v plane (currently there is a max of 3000 points between HA_MIN
    and  HA_MAX).  ’/INTEGRATION now’ is a special case and plot the current
    time positions only. Usually associated with option /VERBOSE
         /STATIONS enable to access stations by their rank number in the AS‐
    TRO_STATIONS file, not by their mnemonic. ALL means ’take all stations’.
         /SIZE  (mostly  used in conjunction with /STATIONS) permits to give
    the corresponding aperture size of the telescopes (or antennae).
         /VERBOSE gives a number of useful information about u,v radius  and
    angles  and  delay line positions as well as warnings about impossibili‐
    ties (such as telescope  shadowing  and  horizons,  delay  line  limited
    stroke,  etc...).  Use  with ’/INTEGRATION now’ to get the precise value
    for a precise moment (after having set the time ’no’ refers to with  the
    TIME command).
         /DELAY_LINE enable to give the list of delay lines corresponding to
    the stations.
         /BACKGROUND file [plane] gives aspro a  GDF  file  to  be  used  as
    beackground to the u,v box drawn by the command.
         /BANDWIDTH band1start band1end [band2start band2end...] will plot
     lines corresponding to the bandwidth of observations, given by the
     succession  of  start and end values (defining observation bands) given
    in the list, in MICRONS.

    The box labelling is in meters. A double labelling in  kilo  wavelengths
    is  drawn if variable FREQUENCY (observing frequency in GHz) is defined.
    Switching to the VLT by the command "OBSERVATORY VLT" defines  FREQUENCY
    to some 1 micron (300 THz). Some labellings are then in wavelengths (mi‐
    crons).

1 ENDOFHELP





































