
Map_BSC h dDD[.MM[.YY]] { tHH[.MM[.SS]] | t{e|m|b}[#] } UT# 
 l<longitude> f<latitude>
 b# m# tr# [{wT[-] | wH | wP}<OuFile>] p[-] pl[-] ip im[<name>] ie
 {ib|nib} b<char>[-] nb nd ne np#[:#] ls# s:<char> s[#[:#[:#]]] sd[-]
 r# k<string>[:<string>] hor o[<name>][:<string>]
 e[#] g[#] x# xs# y# ys# z# ro# r- TS# RA# De# c hc mo gr gr#
 @<par-file> $@<orb.el.file> $<one_element>

plots a star map using the Bright Star Catalogue and auxiliary catalogs
               (Hipparcos or Tycho catalogues are a slow alternative).

H   writes this information into Map_BSC.hlp
HI[path] demands input from Hipparcos catalogue instead of the BSC
  (default path is d:\cats\hip_main.dat),
 path like e: means \cats\hip_main.dat is on drive e,
 path ending by \ is appended by hip_main.dat
TI[path] demands input from Tycho catalogue instead of BSC
  (default path is d:\cats\tyc_main.dat); if there is just one character
  (any) instead of path,   tyc_main.sel   file is assumed,
D and T have the current values as default
F{G|J} forces Gregorian (Julian) dating even outside the standard interval
TT#[unit] forces the Terrestric Time - UT difference, default unit is s
TE[#] is the moment when Sun is at # (default 12) degrees below horizon
     in the evening (TM for morning, TB for both evening and morning)
UT is the t-UTC difference / 1 h (default 1 from Nov. to March, else 2)
L and F (longitude and latitude / 1 degree) are those of Brno
B#  base for the faintness scale / 1 cmag (default -200, more for small fields)
B{R|C|M|F[#]}[-] plot [no] (default yes) border
   Rectangle (default) | Circle | Mask to cut | mask to cut and Fold
    (an outward shift (/ 1 mm) of lines to cut may be given then)
BG# per cent of white for background (default 0)
M#[:#]  faintness liMit / 1 cmag (default 800), the other number concerns
   just the solar system particles, mainly in cometary tails
Tr# transformation coefficient from cmag to dmag for star images (default 10)
wT[-] (wH, wP) precedes the output LaTeX (HPGL, eps) file name
    (default Screen.{ltx|hpg|eps})
 wT- implies creating just the picture part, not a complete LaTeX file
LA  for a PostScript output: prepend it with a prologue for landscape
   printing (the file will not be a true eps format any more)
P[{N|S}[{N|S}]] map center at north (south) pole instead of zenith
   with label tops toward north (south) (default is north)
Pl[-] include [not include] planets
Pl{N|B}#[:#[:#]]  number of planetary positions next or before (default 0)
   [:<time step>] for each new position / 1 day (default 1,
    #h  for # / 1 hour, #m for time step in minutes)
   [:<module>] for other bodies than Moon (default 1)
PlT#[:#] <module> for displaying times by planets
    (default 1, 0 means no times)
   [:<module>] for displaying times for Moon (default as for planets)
IP  include north poles of planets and their orbital planes
IM[<name>] include map outlines and descriptions from <name>.dbf (def. Maps)
IE  include perpendicular marks at each 30 degrees of ecliptics
IB  include stars below horizon
NI[B] do not include stars below horizon
NB  do not draw picture borders (see above, switch b<char>[-])
NE  do not draw equator
ND[P]  do not print date [print parameters instead]
NG  do not show geocentric Moon over horizon (just the topocentric one)
NR  do not refract, neither consider extinction
LS# labels of stars 0: nothing (default),1: HR numbers,..., 5: Names,... 
 (#:# for Hipparcos/Tycho input: starting column and length of label)
LL# length of line segments / 1 degree (default 2)
CS# comment stars - like LS, but just for the output file, default 5 (Name)
 (#:# for Hipparcos/Tycho input: starting column and length, default none).
 Record numbers are always present in the output file.
CW# compose stars within # minutes into one fixed star (default 6,
    for field radius below 12 degrees scaled down as 6*<radius of field>/12)
CR[-] plot a central cross (default; do not when -)
S:<char>[#] asks for marking stars having <char> as the beginning
    of the field # (default field 9, named A) (for text input, # is column)
S[#[!#[!#]][:#[:#]] Stereo view
    screen parallax (/ some 1 mm) for 1000 mas stellar parallax
    distance  (default 20)
    ! screen parallax for planets at 0.1 AU distance (default the same)
       ! and for the Moon at 30 Earth radii distance (default the same)
           : % of standard shift of some 70 mm (default 100)
              : nearer viewpoint then from the Earth / 1 AU (default 0,
   just for Solar system bodies other than Moon, useful for cometary heads)
SD[-] Show [do not show: default] distances of Solar system bodies
SC[#|-|B|G|R#] Stereo view in colour, full width. Sets standard shift to 0.
   # is green relative luminance / 1 % (default 75)
   R# the same for red, - means gray stereo again,
   B demands blue stars for the right eye, G resets them to green
SM Stereo view -- Mirror reversed image left. Sets % of standard shift to 190.
   (put the mirror between the images, put your right eye just a bit right
   from the mirror plane, look right to the mirror by your left eye)
HF hide faint stars within the bright ones (to preserve the bright ones)
R#  vertical radius of the field / 1 degree (default 95 for plane or conus,
   67 for cylinder as a projection surface, see below);
   it is measured in the units which hold in the center
   (away from center they hold just for the equidistant projection)
K<string>[:<string>]  kind of geometry and surface:
  E or 0     Equidistant from projection pole (default),
  Conf or 1  Conformal (non-distorted angles),
  G or 2     Gnomonic (central perspective)
  P or A     to a Plane (Azimuthal, default)
  Cyl or R or 3  to a Cylinder (the base grid will be Rectangular)
  Cone[#]    to a Conus, normal to a line of sight at # degrees
       of angular height (or absolute value of declination, default 60)
  S          Stereographic: short for to a Plane, Conformal
  U#         Undistorted parallel # degrees far from the central one
       (for cylinders and cones using equidistant projection,
       default half the R value)
Ho[r] like K3 NIB; then default R33 and Y24 and undistorted height 28.5
AA#  central astronomical azimuth / 1 degree (just for K=3, default 0)
A#  central (geographical) azimuth / 1 degree (just for K=3, default 180)
O[<name>][:<string>]  include objects from a database <name>.dbf (default obj)
    containing <string> (default A) in field MAPS
E[#] centers the map at this longitude of the ecliptic (default 90)
    (sets also "kR r67 ys50 m500 b-200")
G[#] centers the map at this galactic longitude (default 0)
    (sets also "kR r67 ys50 b-300")
X[P]# shift of X coordinate  / 1 degree [or % of vertical radius] (default 0)
Y[P]#     (the same for Y coordinate)
XS# side along X coordinate / 1 % of the screen (default 100)
YS#       (the same for Y coordinate)
Z#  is zenith extinction / 1 cmag (default 20) 
RO# rotate anticlockwise / 1 degree (default 0)
R-  do not turn descriptions with tops toward the map centre
TS# sidereal time / 1 h (sets "pl-": do not show planets)
RA# right ascension of the map pole (same as TS, but in degrees)
De# declination of the map pole (same as F)
C[{-|#}] Colurs and parallels will be [not: default] plotted
   each # degrees (default 90; 5, 10 or 30 are good values)
HC[{-|#}] Height circles      -         "          - 

  For charts turnable or shiftable under a mask, two more options:
Mo[-] [don't] display Months along the ecliptics marking midnight culmination
Gr[-] [don't] make a Grid (an overlay or mask) for a map made with Mo option
Gr{I|O}- don't display a inner/outer hour scale in that grid

  A (S)VGA screen options:
Gr# 2:Use just black and white for stars (instead of 16 degrees of gray)
    5 to 100: % of the maximum white (default 60) for lines and texts
SVGA#    or
SVGA256:# Try SVGA 256-color mode # (default 4 for the 1024x768 resolution
                                3 would set the 800x600 mode)
SVGA16:# is a 16 color alternative for 0.5 MB cards
SVGA:#   is another 256-color alternative, if you have svga.bgi
  Caution, some cards lock up the computer so that just RESET helps.
  (For the Free Pascal Compiler, the SVGA option is obsolete
   as the executable uses some VESA mode in any case.)

  A large catalogue speed-up option:
Q#[:#[:#]] Size of whole queueue, size of its part for compounding stars,
  limit over the limiting faintness (parameter M) for the components / 1 cmag.
  Default is 150:100:500 for the BSC (150:100:200 for HI or TY),
          or 850:100:200 for PostScript output,
  q0 gives quick draft processing, unsuitable for the final output.
  (HF option, see above, reduces the queue to its second part, 100 by default)

If needed, three parameters for computing refraction can be added:
 PR  pressure / 1013.25 kPa (default 0.97)
 CT  Celsius air temperature / 1 K (default 10)
 RH  Relative humidity of the air / 1 % (default 70)
Q  quit after making the map (batch mode, for generating PostScript output)

@   file with any default parameters (other than further @);
    default suffix is .cnf; on each line, text after %, & or # is a comment.
    % or & can be also used to disable the rest of the command line.
$   prefix for elements concering comets etc.
 ($? to see help, $h to append it to file Map_BSC.hlp)
$@  file with orbital elements; default suffix is .elm

  Further paths:
LB<directories with the Bright Star Catalogue>
   (default c:\d\j\d\stars;C:\D\BSC5\;c:\d\stars\bsc5;/home/jhollan/public_html/data;/home/guest/cats;g:\cats )
LE<directories with orbital elements and configuration files>
   (default c:\d\sol_syst;c:\d\j\d\sol_syst;c:\d\stars;c:\d\stars\atlas;/home/jhollan/public_html/data;/home/guest/cats;g:\cats)

no parameters are obligatory, ? gives this help

( (C) Jan Hollan, N.Copernicus Observatory and Planetarium in Brno, 1999;
 subject to the GNU General Public License, http://www.gnu.org/copyleft;
 source code available at http://astro.sci.muni.cz/pub/hollan/programmes)

$@<File with orbital elements of an object>
should contain (and parameters given elsewhere, preceded by $, can change):

{ {A|Q}# AN# I# E# P{D<yy.mm.dd.ddd>|M#} P{N|L}#
 | !<string>[:<filename>] }

 !<string>[:<filename>] will read elements from the line containing <string>
   using text(!) file <filename> (default xephem.dat, mpc format is,
   an alternative, in this case >mpc< should be contained in the file name

 A  is the large semiaxis
 AN longitude of ascending node
 I  inclination
 E  numerical excentricity (default 0)
 PD perihelion date
 PM perihelion Modified Julian Date
  (moment of perihelion passage can be replaced by:
  MA mean anomaly, AD that mean Anomaly Date and ev. DM daily mean motion)
 PN elongation of perihelion from ascending node
 PL perihelion longitude (= PN + AN)
 Q  perihelion distance from the Sun

It may contain also moments and way the object should be shown:
 dDD[.MM[.YY]] tHH[.MM[.SS]] UT# FA#[:#] CE[#] B# N# NT S{#|#h|#m} M<symbol>
 CD# ST#
 t{A#:#:... | B#     | D#[:#[...]]   | I[#]       | M#  |
   O[#]     | P#:#:# | T#[:#]~#:#~...| W#[:#[:#]] }
 { ? | h }

 D and T are initially taken from the main programme
 UT is the t-UTC difference / 1 h (November-March 1, then 2)
 FA Absolute Faintness / 1 cmag  (those at 1 AU from both Earth and Sun,
    at zero "phase angle" (in fact, Sun-object-Earth <> 0 at this position)
  [:<increment of faintness for generated particles / 1 cmag> (def. 400)]
 B  positions before the given moment (default 0)
 N  next positions to be computed (default 0)
 NT[-] do not (-: do) show times (and dates) by each position
 S  step to further/preceding time (default 1 day, S#h for time in hours)
 M  string to be shown at each place (default +)
 W  module for writing time (default as for planets)
  [:<module for age of dust particles> (default 10* the first one)
  [:<module for age of plasma particles> (default the preceding one /5)]]

The remaining parameters concern comets only:
 CE cometary exponent (amount of diffused sunlight is proportional to
   distance from Sun **CE, default 4, solid bodies have 2); phase angle
   dependence of faintness is neglected when the parameter is given
 CD Time of negligible solar acceleration of particles when blown by gas
   in coma (default 2 days)
 ST Split Time of large dust particles (default no splitting)

parameters beginning with T (Tail; finish its computation by pressing >S<):
 tA set of solar repulsion accelerations of cometary particles, as ratios
   to gravitational solar attraction, maximum 6 values separated by :
   (default 0.5:1:2:3:4:200), less then 6 values imply less particles;
   repulsion may be appended by a value differing from that given by CD
   (delimiter is ", i.e., last item may read 200"4 instead of just 200)
 tB number of parent body positions before the given moment for which
   cometary particles should be generated (default = B)
 tD ejection velocity of particles at 1 AU / (m/s) (default 400);
   more values (separated by :) apply to last tA values
 tI interrupt computation each # step (1 when no # is given, pressing >R<
   begins continuous run of programme without interruptions)
 tM show just tails mod # (default=tB, just the tail in the given moment
   is shown)
 tO show tail Only (do not mark position of the parent body); if time is
   to be written (see $W parameter), shift it # millimeters right
 tP (Prograde) pole of the rotation of the parent body and longitude of axis
   of ejection measured from the subsolar meridian (RA:decl:angle)/1 degree
 tT Tilts of ejection (from its axis) / 1 degree
   and number of sections of the cone given as tilt[:sect.]~tilt[:sect.]~...
   (default tilt 0, sections 6 for tilt>0)
 tW velocity of the solar wind / 1 km.s (default 400)
 ?  will display this help (i.e., $? from the command line)
 h  will append it to the Map_BSC.hlp file

Each $@<file> represents one body.
 The same holds for $!<string>:<file> -- an alternative for a $@<file>
 as far as the necessary ephemeris parameters are concerned.
If more than one is given in a @<file>
 or on the command line,
 only those parameters are valid for the current ${@|!}file,
 which are given before the following ${@|!}file.
