ecd@cs.umn.edu@ncs-med.UUCP (Elwood C. Downey) (03/11/90)
Posting-number: Volume 11, Issue 8
Submitted-by: ecd@cs.umn.edu@ncs-med.UUCP (Elwood C. Downey)
Archive-name: ephem4.12/part07
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X follows the absolute magnitude and luminosity index coefficients.
X
X 7.1.4. On or Off
X
X The last selection on the right toggles the calculations for the object On
X and Off. It toggles when selected with RETURN and then immediately exits
X the quick-choice menu back to the main menu. If calculations become On,
X then they will be performed for the current type of object; if they become
X Off the object-X row of information will be erased.
X
X 8. Plotting
X
X Each time a field is drawn on the screen during a full screen update cycle
X (that as, during automatic looping or a manual "q" command character from
X the main menu but not from a screen redraw from control-l or when an
X individual planet is turned on or a single time field is changed) its
X full-precision value may be written to a file. This implies you may not
X plot a field from other than the current menu at the time plotting is on.
X You can append several plot runs together, however, if necessary.
X
X Each line in the file consists of a tag character followed by two or three
X floating point variables, all separated by commas. If there are two
X values, they should be interpreted to be x and y (or perhaps r and theta).
X If there is a third, it is a z or trace value.
X
X For efficiency on systems that can compute a screen full faster than they
X can display it, screen updates are suppressed while plotting is on and
X NStep is greater than 1. This can greatly reduce the time to generate a
X long plot file. Fields are still logged for plotting; they just are not
X drawn on the screen.
X
X The Plot field controls plotting. Whether plotting is currently active is
X indicated by "on" or "off" immediately to its right.
X
X Picking "Plot" brings up a quick-choice menu, as follows:
X
X Select: Select fields, Display a plot file, Cartesian coords, Begin plotting
X
X
X 8.1. Defining plot fields
X
X Select the "Select fields" option. You will be asked to move the cursor
X to the field you want to use as the x coordinate (abscissa), then asked to
X choose the y coordinate (ordinate), then asked to choose an optional z
X trace variable and finally a tag character. (X and Y may be for other
X coordinate systems too but ephem's quicky plotter can only plot in
X Cartesian coordinates.) If you type q for either x or y then no more
X fields will be defined. If you type q for the z field there will be no z
X field. You can not label a plot line with the letter "q" at this time.
X
X This then repeats so you may choose up to ten of these sets for any given
X plot run. Each set defines what will become a line on the final plot.
X
X
X
X
X
X
X
X
X
X - 14 -
X
X
X Note that you may select the "Search" field to indicate use of the current
X search function; that function must be defined by the time plotting is
X turned on.
X
X If you turn plotting off and back on the fields selected for plotting are
X reactivated the same as they were last time. You may change them if
X desired, of course, but there is no need to redefine them if you do not
X wish to change them.
X
X 8.2. Displaying a plot file
X
X Select the "Display a plot file" option to generate a crude plot on the
X screen of an existing plot file previously created by ephem. The entries
X in the file will be drawn on the screen using their tag characters; the
X plot remains on the screen until you type any character.
X
X The plot may be made in polar or Cartesian coordinates, depending on the
X setting of the plotting mode in the quick-choice (see next section).
X
X 8.3. Cartesian or Polar coords
X
X This toggles the plotting mode coordinate system. The mode remains until
X changed. Polar coordinates assume the first numeric field in the plot
X file is the radius, and the second is the angle counterclockwise from
X right, in degrees.
X
X 8.4. Begin Plotting
X
X If plot field lines are defined then the third option, "Begin plotting"
X will be available. You will be asked for the name of the file to use and,
X if it already exists, whether to overwrite it or append to it. Once you
X have chosen a file, plotting is on and the top menu plotting status field
X changes to "on". The default plot file name is ephem.plt. The values are
X written to the plot file each time they are updated on the screen until
X you select "Plot" again and select the "Stop" option to turn plotting back
X off.
X
X 8.5. Stopping Plotting
X
X If plotting is on, then selecting the Plot field in the top section will
X turn plotting off. You may pick Plot again and resume with the same fields
X by selecting "Begin plotting" again.
X
X Note that due to internal buffering the plot file will not be completely
X written to disk until plotting is turned off.
X
X 9. Watching
X
X You may generate a simple drawing on the screen of the night sky or the
X solar system by selecting "Watch". It will bring up a quick-choice menu
X as follows:
X
X Select: Night sky, Solar system, No trails
X
X
X
X
X
X
X
X
X
X
X - 15 -
X
X
X 9.1. Trails
X
X You may either erase after each iteration or leave the tags up, referred
X to as "trails". Picking the right-most choice will toggle between "No
X trails" and "Leave trails"; you should set it as desired before you select
X the style of sky plot you wish. Ephem will remember your selection.
X
X 9.2. Night sky
X
X This selection draws the currently active planets as they would appear in
X the sky at the current time and date. The coordinate system is such that
X 0 degrees azimuth (north) through 360 degrees (north, once around) is
X mapped to the horizontal screen dimension, and 0 degrees altitude (level)
X through 90 degrees (the zenith) is mapped to the vertical dimension. Thus,
X the bottom row is the horizon and all across the top is the zenith.
X
X 9.3. Solar System
X
X This selection draws the currently active planets as they would appear
X looking "down from the top" of the ecliptic, with the sun at the center
X and zero hours right ascension towards the right. The scale is adjusted
X to roughly fill the screen according to the outter most active planet.
X The screen transformation assumes a screen aspect width/height ratio of
X 4/3. Down the left column of the screen is the heliocentric altitude of
X the planet above or below the ecliptic, drawn to the same scale as the
X circular display.
X
X In either style of display, pressing RETURN advances the time by whatever
X amount StpSz is set to. Pressing "h" advances the time by one hour, "d"
X advances by one day, and "w" advances by one week (seven days). Pressing
X "q" returns to the tabular main screen. Pressing any other key starts an
X automatic loop with each step advancing by StpSz; pressing any key stops
X the looping.
X
X As symbols are placed, collisions (overstrikes) are avoided by moving
X characters in such a way as to maintain increasing sorted order towards
X the right. In the case of the heliocentric altitude display, for example,
X greater height is indicated towards the right on the same row; the S and E
X symbols are always at 0.
X
X When you return to the main menu, the last watched time will be maintained
X as the current time. The StpSz is not changed.
X
X 10. Searching
X
X Ephem can search for arbitrary conditions to exist among most displayed
X fields. You first enter a function, then select from among three forms of
X equation solvers to iteratively solve for the next time when the function
X meets the requirements of the solver. The solver selects the next time for
X which it wants the function evaluated and sets StpSz so that the next
X iteration will occur at that time. The solvers continue to iterate until
X either they achieve their goal or NStep reaches 0.
X
X You may set NStep to be quite large and let ephem search unattended or set
X
X
X
X
X
X
X
X
X
X - 16 -
X
X
X it to 1 and watch it converge one step at a time. You may also plot at the
X same time as search to record the exact steps ephem took to converge.
X (But recall that screen updates are suppressed if plotting is also on).
X
X The "Search" selection in the top half of the screen controls all
X searching. Picking it brings up a quick-choice menu as follows:
X
X Select: Find extreme, Find 0, Binary, New function, Accuracy
X
X
X 10.1. Find extreme
X
X This search algorithm searches for a local maximum or a minimum in the
X search function, whichever it finds first. It begins by evaluating the
X search function at the current time then for two more times each separated
X by StpSz. It then fits these three points to a parabola and solves it for
X the time of its maximum (or minimum). StpSz is set so that the next
X iteration will evaluate at this point. This parabolic fit solution keeps
X repeating until StpSz changes by less than the desired accuracy or until
X the curve becomes so flat that an extrema appears too broad to find.
X
X 10.2. Find 0
X
X This search algorithm uses the secant method to solve for the time at
X which the search function is zero. The function is evaluated at the
X current time and then again StpSz later to establish a slope for which the
X x-intercept is found as the next zero guess. This is used to set StpSz for
X the next desired time value and the slope hunting process repeats until
X StpSz changes by less than the desired accuracy.
X
X 10.3. Binary
X
X This search algorithm must be used with a search function that yields a
X boolean result, ie, a true or false value. The idea is that the function
X is assumed to be one truth value when evaluated at the present time, and
X the opposite truth value when it is evaluated StpSz later. The algorithm
X will then do a binary search for the time when the truth value changes.
X
X The binary algorithm does not begin until the state change is bounded in
X time. Initially, as long as the truth value at StpSz is the same as the
X previous value the algorithm will just keep moving in time by StpSz
X looking for when the state changes. That is, a linear search is initiated
X to bound the state change, then the binary search proceeds.
X
X 10.4. Define a New function
X
X Select "New function" to display the current search function. If you type
X "q" it will be left unchanged. If you type RETURN it will be erased. If
X you type anything else it will be compiled and, if there are no errors, it
X will become the new search function. Once a valid function has been
X stored, it will remain unless changed. If a search function is selected
X and there is as yet no valid search function defined, you will
X automatically be asked to enter one as though you had selected "New
X function."
X
X
X
X
X
X
X
X
X
X - 17 -
X
X
X A search function consists of intrinsic functions, field-specifiers,
X constants and operators, and precedence may be overridden with
X parentheses.
X
X
X 10.4.1. Intrinsic functions
X
X In this release, the only intrinsic function available is abs(), which
X returns the absolute value of its argument.
X
X 10.4.2. Field Specifiers
X
X A field in the bottom half of the menu is specified in the form of
X "object_name.column_name". The object_name is enough of the planet name to
X be unique; use "x" for the user-specified object X. The column_name is
X from the following table, depending on which menu is up. In all cases
X additional characters may be entered but are ignored.
X
X Planet Data Menu Rise/Set Menu Separation Menu
X ------------------ -------------------- ---------------
X al Alt hr Hrs Up, or j Jup
X az Az hu Hrs Up ma Mars
X d Dec raz Rise Az me Merc
X ed Ea Dst rt Rise Time mo Moon
X el Elong saz Set Az n Nep
X hla Helio Lat st Set Time pl Pluto
X hlo Helio Long ta Transit Alt sa Saturn
X ph Phs tt Transit Time su Sun
X ra R.A. u Uranus
X sd Sn Dst ve Venus
X si Size
X vm VMag
X
X
X In addition, the following top-half fields may be used:
X
X da Dawn
X du Dusk
X n NiteLn
X
X
X
X Remember, searching may only involve fields being calculated for display
X at the time the solver is active. While you can syntactically include any
X field in a search function it is useless to define a search that uses
X fields from other than the menu that is selected at the time the search is
X running.
X
X 10.4.3. Constants
X
X Constants may be integers or floating point numbers. The latter may be
X expressed in scientific notation if desired. Examples include 100, .9,
X 1.234, 1e10 and 1.2e-4. Any number may be preceded by - to make it
X negative.
X
X
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X - 18 -
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X 10.4.4. Operators
X
X The collection of arithmetic, relational and boolean operators provided
X mimics those of C language as listed in the following table, in decreasing
X order of precedence. Operators grouped together have the same precedence
X and all have left-to-right associativity. Parentheses may be used as
X desired.
X
X Symbol Meaning Resulting type
X ------ -------------------- --------------
X * multiply arithmetic
X / divide arithmetic
X
X + add arithmetic
X - subtract arithmetic
X
X > greater than boolean
X >= greater than or equal boolean
X < less than boolean
X <= less than or equal boolean
X
X == equality boolean
X != inequality boolean
X
X && logical and boolean
X
X || logical or boolean
X
X
X 10.5. Specifying Search Accuracy
X
X Selecting "Accuracy" allows you to specify when the search will stop. The
X search algorithms will stop when StpSz becomes equal to or less than this
X value. The default is one minute. If ephem has not yet converged to the
X specified accuracy but NStep has decremented to 1, the searching will stop
X but the search status field will still indicate which search procedure is
X in effect. To try more iterations you may increase NStep and resume
X searching. If the accuracy was achieved, the search status field will
X switch to "off" with the number of "unused" steps remaining in NStep and
X the last step size in the StpSz fields.
X
X 10.6. Stop
X
X If searching is on, this option will also appear on the quick-choice menu
X and may be selected to turn off the search.
X
X 10.7. Example Searches
X
X As an example, let's find when Pluto again becomes the furthest planet
X from Sol. You may find when the difference in their sun distance is zero,
X or you might use a binary search on the condition that Pluto's sun
X distance is larger then Neptune's.
X
X To try the former approach select Search, select "Find 0", specify the
X
X
X
X
X
X
X
X
X
X - 19 -
X
X
X search function to be:
X
X pl.sd - nep.sd
X
X set StpSz to something large like 10d, NStep to allow several iterations
X like 20, and then type "q" to start the search and watch ephem do the
X hunt. Ephem will settle on about 21:02 1/10/1999 UT.
X
X To try a binary search, you first need to have some idea of when the event
X will occur so you can eliminate the initial linear search for the state
X change. We can start at, say, 1/1/1999, set StpSz to 30d, select Binary
X search, specify the search function to be:
X
X pl.sd > nep.sd
X
X and go. Once it brackets the state change note how StpSz keeps being cut
X in half but can go in either direction (sign) as it divides each interval
X in half. Ephem will converge on the same answer.
X
X 10.8. Another Example
X
X To find the time of last quarter moon during December, 1989, use the "Find
X 0" search algorithm to solve "moon.el + 90". (At last quarter, the moon
X is 90 degrees west of the sun, or -90 east in ephem's elongation display.)
X Set the initial time to mid-month, 12/15/1989, StpSz to 1 day and NStep to
X 10. Ephem takes only a few iterations to settle on 23:57 12/19 UT.
X
X 10.9. Caution
X
X Beware that most celestial phenomena are generally pseudo-periodic in
X nature. In early search steps ephem can easily skip over a local maxima
X and find a later one, which, while correct, may not be what was desired.
X In general, the closer you can be when you start the search the better
X ephem can refine it; it is not as good with very broad searches that can
X go "wild". Set StpSz large enough to offer significant change in the
X function value, but small enough not to skip too far.
X
X For example, Saturn and Neptune had three close approaches during 1989.
X If you did not know this then just asking ephem to find a minimum would
X have produced different results depending on the starting conditions.
X When starting a search for a certain class of event it is a good idea to
X first use the plotting or watching facility of ephem to get a broad
X picture of the general circumstances then use ephem's search facility to
X refine a given region (or create and inspect a plot file and do your own
X interpolation directly from it separately).
X
X Similarly, ephem's searching techniques are not good for eclipses because
X the moon and sun are close every month; the trick is sorting through the
X frequent conjunctions for ones that are particularly close. One needs a
X way of establishing an envelope fit to the local extrema of a cyclic
X function in order to find a more global extreme.
X
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X - 20 -
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X
X 11. Implementation Notes
X
X Remember that everything is for the current local time. So, for example,
X the calendar marks moon events in local time; commercial calendars usually
X mark the UT date. Similarly, the rise/set times are for the current local
X day.
X
X The program uses a horizontal plane tangent to the earth as the horizon
X for all altitude calculations, rise/set events, etc. This is not the same
X as the angle up from the local horizon unless the observer is directly on
X the ground due to earth's curvature. The effect can be found from:
X
X sin(a)**2 = (h**2 + 2Rh) / (R+h)**2
X where:
X R = radius of earth
X h = height above ground (same units as R)
X a = increase in altitude
X
X For example, the effect is more than two arc minutes at a height of 5
X feet.
X
X Visual magnitudes are not very accurate at all... I haven't bother to fix.
X
X The accuracy of ephem can not be specifically stated since the Duffett-
X Smith book does not warrant its planet position polynomials to any given
X degree. I know for sure that better accuracy could be achieved if ephem
X used ephemeris time but I have not yet decided on a suitable UT-ET
X algorithm.
X
X The program uses double precision throughout. While this precision might
X seem a little ridiculous, it is actually more efficient for most
X traditional K&R C compilers, the search functions are far more stable, it
X improves small angles (conjunctions) calculated using acos(), etc.
X
X Searching and plotting always use full precision but if neither of these
X are turned on pure display and watching only recompute a given planets new
X location if the time has changed enough to effect the required display
X precision, based on the planets mean apparent orbital motion.
X
X The sun-moon distance is the solution for the third side of a planar
X triangle whose two other sides are the earth-moon distance and earth-sun
X distance separated by the angle of elongation.
X
X 11.1. Program limits
X
X The search function is limited to a maximum of 32 instructions (each
X constant, field spec, and operation is one instruction), with no more than
X a total of 16 constants and field specs. At run time, the function can not
X require more than 16 stacked values (due to operator precedence or
X explicit parenthetical expressions) to evaluate.
X
X No more than 32 different fields can be tracked simultaneously for
X plotting and/or searching.
X
X
X
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X - 21 -
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X
X No more than 10 lines may be plotted at once.
X
X The maximum file name length is 14 characters.
X
X 12. DOS Installation Procedure
X
X Summary:
X
X You must be running DOS V2.0 or later, though somewhere between V2.0 and
X V3.21 the behavior of control-c to terminate the program was fixed. A
X 8087 floating point chip will be used if present.
X
X The distribution floppy contains two files, ephem.exe and ephem.cfg.
X Ephem.exe is the executable program; ephem.cfg is a sample configuration
X file. To run the program, make working copies of these two files in a
X directory and run "ephem" from that directory. The program uses the
X environment variable TZ to establish the local timezone.
X
X 12.1. Setting TZ
X
X Set a DOS environment variable, TZ, in the following form:
X
X set TZ=SSSnDDD
X
X
X This environment variable is used to establish the timezone name and hours
X offset whenever the "NOW" shorthand is used from ephem, either from the
X configuration startup file or whenever any time field is changed manually.
X
X SSS the 3-letter abbreviation for the local standard timezone;
X
X n a number between -23 to 24 indicating the number of hours that are
X subtracted from GMT to obtain local standard time;
X
X DDD is an optional 3-letter abbreviation for the local daylight savings
X time zone name. Leave it off if you do not have savings time in your
X area or it is not currently in effect. If the changeover dates differ
X from the internal algorithm, just use SSS and n directly.
X
X For example, in the midwestern United States with savings times set
X TZ=CST6CDT
X
X If for some reason your system does not change to savings time at the
X right time, then omit the DDD parameter and just set the SSS and n to
X exactly what you want.
X
X You can put this in your AUTOEXEC.BAT file so it gets set each time you
X boot DOS.
X
X 13. Wish List
X
X incorporate Terrestrial Dynamical Time (known as Ephemeris Time prior to
X 1984). TDT is about 57 seconds ahead of UT1 in 1990.
X
X
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X - 22 -
X
X
X add explicit searching for eclipses and occultations.
X
X work on a better precession algorithm. current one exhibits some
X hysteresis.
X
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X - 23 -
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X
X 14. Sample Screens
X
X Here are sample ephem screens. They are generated using the first sample
X ephem.cfg file (listed in the section describing the configuration file).
X There is one for each of the three possible screen formats. The rise/set
X screen was done using the Adaptive option. The separations screen was
X done using the Geocentric option.
X
X
X
XMove to another field, RETURN to change this field, ? for help, or q to run
X
XCST 19:45:00 4/04/1990 | LST 8:22:37 | Lat 44:50:37 | April 1990
XUTC 1:45:00 4/05/1990 | | Long 93:42:08 | Su Mo Tu We Th Fr Sa
XJulianDat 2447986.57292 | Dawn 4:10 | Elev 800 ft | 1 2 3 4 5 6 7
X | Dusk 20:27 | Temp 40 F | 8 FM 10 11 12 13 14
XWatch | NiteLn 7:43 | AtmPr 29.50 in | 15 16 17 18 19 20 21
XSearch off | | TZ 6:00:00 | 22 23 NM 25 26 27 28
XPlot off | NStep 1 | Epoch (OfDate) | 29 30
XMenu Planet Data | StpSz RT CLOCK | |
X--------------------------------------------------------------------------------
XOb R.A. Dec Az Alt Helio Helio Ea Dst Sn Dst Elong Size VMag Phs
X Hr:Mn.d Deg:Mn Deg E Deg Up Long Lat AU(mi) AU Deg E ArcS %
XSu 0:55.3 5:55 289:53 -10:56 195:01 1.0004 1919 -27
XMo 9:18.7 15:26 153:36 57:49 241151 1.0018 122.3 1847 -12 68
XMe 1:54.5 13:19 284:22 4:39 96:23 5:14 1.0909 0.3105 16.3 6.2 -2.4 71
XVe 22:02.0 -11:07 320:00 -50:07 241:32 0:53 0.7267 0.7250 -46.4 23.3 -5.1 53
XMa 21:23.9 -16:34 330:36 -58:56 282:18 -1:28 1.7066 1.4309 -56.9 5.5 0.5 91
XJu 6:14.0 23:29 241:30 56:16 104:06 0:05 5.2961 5.1847 78.2 37.1 -2.2 99
XSa 19:46.0 -21:00 20:34 -65:00 288:58 0:12 10.137 10.019 -80.4 16.3 1.2 100
XUr 18:41.7 -23:24 52:10 -60:18 276:37 -0:18 19.276 19.397 -95.5 3.4 5.7 100
XNe 19:02.8 -21:48 42:00 -61:43 282:39 0:52 30.183 30.208 -90.5 2.1 7.9 100
XPl 15:16.7 -1:38 81:32 -10:43 226:07 15:30 28.837 29.657 -144.5 0.3 13.7 100
XX 1:47.7 20:05 290:19 8:13 93:07 26:03 1.1320 0.3759 19.0 -1.8 74
X
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X - 24 -
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X Move to another field, RETURN to change this field, ? for help, or q to run
X
X CST 19:45:00 4/04/1990 | LST 8:22:37 | Lat 44:50:37 | April 1990
X UTC 1:45:00 4/05/1990 | | Long 93:42:08 | Su Mo Tu We Th Fr Sa
X JulianDat 2447986.57292 | Dawn 4:10 | Elev 800 ft | 1 2 3 4 5 6 7
X | Dusk 20:27 | Temp 40 F | 8 FM 10 11 12 13 14
X Watch | NiteLn 7:43 | AtmPr 29.50 in | 15 16 17 18 19 20 21
X Search off | | TZ 6:00:00 | 22 23 NM 25 26 27 28
X Plot off | NStep 1 | Epoch (OfDate) | 29 30
X Menu Rise/Set Info | StpSz RT CLOCK | |
X --------------------------------------------------------------------------------
X Ob Rise Transit Set Hrs Up
X Time Az Time Alt Time Az
X Su 5:49 80:53 12:18 50:58 18:47 279:24 12:58
X Mo 13:17 65:36 20:43 59:56 3:30 297:14 14:14
X Me 6:18 70:50 13:16 58:17 20:16 289:49 13:58
X Ve 4:05 105:12 9:24 33:57 14:44 254:58 10:38
X Ma 3:52 113:04 8:47 28:31 13:42 247:04 9:51
X Ju 9:50 54:50 17:37 68:39 1:27 305:10 15:37
X Sa 2:36 119:28 7:10 24:11 11:45 240:32 9:09
X Ur 1:44 123:07 6:06 21:48 10:29 236:53 8:45
X Ne 1:57 120:39 6:27 23:24 10:58 239:21 9:01
X Pl 20:41 91:31 2:42 43:32 8:39 268:29 11:58
X X 5:46 61:23 13:11 64:52 20:40 299:57 14:54
X
X
X
X Move to another field, RETURN to change this field, ? for help, or q to run
X
X CST 19:45:00 4/04/1990 | LST 8:22:37 | Lat 44:50:37 | April 1990
X UTC 1:45:00 4/05/1990 | | Long 93:42:08 | Su Mo Tu We Th Fr Sa
X JulianDat 2447986.57292 | Dawn 4:10 | Elev 800 ft | 1 2 3 4 5 6 7
X | Dusk 20:27 | Temp 40 F | 8 FM 10 11 12 13 14
X Watch | NiteLn 7:43 | AtmPr 29.50 in | 15 16 17 18 19 20 21
X Search off | | TZ 6:00:00 | 22 23 NM 25 26 27 28
X Plot off | NStep 1 | Epoch (OfDate) | 29 30
X Menu Separations | StpSz RT CLOCK | |
X --------------------------------------------------------------------------------
X Ob Sun Moon Merc Venus Mars Jup Saturn Uranus Nep Pluto X
X
X Su 122:17 16:20 46:22 56:53 78:11 80:24 95:28 90:29 144:29 19:02
X Mo 122:17 106:01 168:37 178:19 44:06 157:19 142:15 147:14 89:57 104:59
X Me 16:20 106:01 62:37 73:11 61:56 96:40 111:44 106:43 156:32 6:57
X Ve 46:22 168:37 62:37 10:43 124:33 34:03 49:07 44:07 100:46 63:41
X Ma 56:53 178:19 73:11 10:43 135:03 23:35 38:36 33:40 91:16 74:24
X Ju 78:11 44:06 61:56 124:33 135:03 158:36 173:39 168:38 131:51 61:21
X Sa 80:24 157:19 96:40 34:03 23:35 158:36 15:04 10:06 68:17 97:27
X Ur 95:28 142:15 111:44 49:07 38:36 173:39 15:04 5:07 54:09 112:25
X Ne 90:29 147:14 106:43 44:07 33:40 168:38 10:06 5:07 58:29 107:19
X Pl 144:29 89:57 156:32 100:46 91:16 131:51 68:17 54:09 58:29 151:30
X X 19:02 104:59 6:57 63:41 74:24 61:21 97:27 112:25 107:19 151:30
X
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EOFxEOF
len=`wc -c < Man.txt.2`
if expr $len != 29650 > /dev/null
then echo Length of Man.txt.2 is $len but it should be 29650.
fi
# if Man.txt.1 exists, then the first part of the manual has already been
# extracted from its shar file, and we stick this one after it to form the
# complete manual, Man.txt.
if test -w Man.txt.1
then
echo catting Man.txt.2 to Man.txt.1 to form Man.txt
cat Man.txt.2 >> Man.txt.1
rm Man.txt.2
mv Man.txt.1 Man.txt
fi