
                New features of "Astrometrica" Version 3.0
               


  This is a brief description of the new features of "Astrometrica 3.0".


  CAUTION:  If you have been using version 2.x of "Astrometrica",  start the
    program  UPDATE.EXE  before you run  "Astrometrica 3.0"  for the
            first time.  It will modify your ASTROMET.INI file so that it is
            compatible with version 3.0.
            The updated ASTROMET.INI file will no  longer  work  with  older
            versions of "Astrometrica"!
            After you have updated ASTROMET.INI  with  UPDATE.EXE, or if you
            are  installing  "Astrometrica"  for the first time,  delete the
            file UPDATE.EXE!


  The most important change is that, while earlier versions were common  DOS
  real mode applications,  version 3.0  is a DOS protected mode application.
  This means that it can address larger amounts of  XMS memory  while memory
  for common DOS applications is limited to 640 kB.

  "Astrometrica 3.0" will run on computers having a 80286 or better CPU, and
  at least 1 MB XMS memory.  The  files  DPMI16BI.OVL  (16 Bit DOS Protected
  Mode Interface)  and  RTM.EXE (Run Time Manager)  must  reside in the same
  directory as the application (ASTROMET.EXE).


  The following new features are available:

* Support of larger CCD Images:
  
  Version 3.0 is able to read images up to  2056 x 1032  pixels in size, and
  store them in your computers main memory.  For display only, images larger
  than  514 x 258  pixels  will  be  binned  (2 by 2 pixels for images up to
  1028 x 516,  3 by 3 pixels for images up to 1542 x 774,  and 4 by 4 pixels
  for images up to 2056 x 1032 pixels).

  The cross hairs/cursor box will move in units of one pixel on the  screen,
  that is,  for example,  by 3 image pixels for images binned 3 by 3.  Press
  the Shift key to move the cross hairs/cursor box in units of single  image
  pixels (or use the Zoom function to see individual pixels).  Both the data
  reduction and the Zoom-function will work on the original  (that  is,  not
  binned) image data.


* Expanded File Interface:
  
  The file interface has been expanded, and it is now able to read all kinds
  of SBIG type 3 images  (generated by either the SBIG ST-4X, ST-5, ST-6, or
  the new ST-7 or ST-8 model), and both 8 and 16 bit TIFF grey scale images.


* Saving Text Windows:
  
  Text files,  as loaded  with  the  'File - View Text-File'  command, or as
  generated by the ephemeris calculation of "Astrometrica", can now be saved
  using file names selected by the user.  The  ephemeris  will  therefore no
  longer be saved to the default file EPHEM.TXT.


* Deleting Files:
  
  There is a 'File - Delete' command that may be used to delete all kinds of
  DOS files. The history list always shows the path to the  image files  and
  to the files holding the orbital elements,  so  the user  can access these
  files quickly.


* Edit Parameters sets Name and Designation of the Object:
  
  The dialog box for editing the image parameters  (displayed after  loading
  an image or by the command 'Utility - Edit Parameters') can now be used to
  set the name and designation of the  objet,  too.  If  there  are  orbital
  elements loaded, the default for the name and designation  of  the  object
  will be set according to the elements file.

  The name and designation of the object will appear in the file REPORT.TXT,
  AREPORT.TXT, and CREPORT.TXT, respectively.


* Support of the new IAU comet designations:
  
  The file CREPORT.TXT now supports the new IAU  cometary  designations,  as
  described in the February, 1995 issue Minor Planet Circulars.


* Correction for local Time Zone:
  
  You can now set your local time  zone  using  the  'Options - Observatory'
  command.  Enter the value that the computer will add to the times given in
  in the image file header to convert local time to Universal Time UT. Enter
  0 if the times given in the image file headers are already UT (that is, if
  the clock of the computer that is used to take the CCD images runs on UT).
  Otherwise, note that this value is negative in the eastern hemisphere, and
  positive in the western.


* Tool for calculating the Mid-Exposure of added Images:
  
  There is now a button labelled  "Mid-Ex"  in the dialog window for editing
  the image parameters.  Pressing this button starts a dialog  that  can  be
  used to calculate the time of mid-exposure  for  added  images  or  images
  taken using SBIG's Track & Accumulate mode.

  When an image covers the time around midnight  (local time,  according  to
  the time zone setting),  use 24 for the hour of those images started after
  midnight (23:58:17 and 24:02:19, for example).  As  this dialog  sets  the
  time, but not the date, be sure to check the date in these cases,  or when
  crossing midnight UT.

  Remember always to check the date and time of mid exposure of  the  image,
  no matter weather you are using this feature or not!


* Set Background & Range for Display:
  
  The  'Utility - Set Background & Range'  command  may  be  used to set the
  Background and Range parameters for the display of an image. Those working
  with SBIG cameras will be familiar with these values.


* Expanded Zoom Functions:
  
  Use the 'Options - Settings' command to select one of three magnifications
  3x, 7x or 11x) to be used for the Zoom function.

  The Zoom function is now not only available  when  measuring  images,  but
  also for images displayed with the 'Display - Image' command.

  When measuring an image, you can now move and size the  cursor  box  while
  the zoomed image is displayed.  Also, you can change the contrast  of  the
  zoomed image using the F5, F6 and F7 keys,  just  as  with  the  un-zoomed
  image.


* Improved Blink Comperator:
  
  The comparison image now will be scaled to match the contrast of the first
  image.  Further,  you may use the F5 key to boost the image contrast while
  blinking  (which will be helpful to detect faint asteroids or comets)  and
  the F6 to restore the original contrast.

  When  you  set  the  blinking  speed to 0, and the original image (not the
  comparison image) is visible, the mouse cursor appears,  so  you can click
  on the image and the respective coordinates will appear on the screen.


* Data Reduction Limits:
  
  The user can now set limits  for the reasiduals  in  both  photometric and
  astrometric data reduction,  using  the 'Options - Settings' command.  Any 
  reference star with residuals larger than that limit will be excluded from 
  the data reduction process,  and  it's  residuals  will  be  displayed  in 
  brackets.

  Note that,  after excluding a reference stars with  large  residuals,  the
  solution may be considerably  better,  and  the  final  residual  for  the
  excluded star may be somewhat lower than the limit specified by the  user,
  finally.


* More Reference Stars:
  
  "Astrometrica" now accepts up to 12 reference stars.


* Turn Sound On or Off:
  
  The 'Options - Settings' command can also be used to toggle the sound  you
  hear when measuring images or selecting  reference  stars  for  the  blink
  comperator on or off.


* Display Pixel Value instead of Saturation:
  
  The  Info-Box  below an image will no longer display a saturation value in
  percent, but rather the pixel value.

  While the saturation  (in percent)  may cause confusion  (for example,  it
  will never get larger than  6.25%  for  12 bit  images  saved to a  16 bit
  file),  users are usually familiar with the pixel values of the images  of
  their various CCD cameras.


* Reading Reference Star Data from Sources other than the GSC:
  
  For some purposes  (e. g. last minute predictions for occulations of stars
  by minor planets,  preparation of spacecraft encounters with minor planets
  or comets),  special reference star sets have been compiled,  which should
  be used instead of the GSC.

  "Astrometrica"  can  now  read  reference star data from ASCII files built
  like that:
  Each line of the file starts with the name or designation of the reference
  stars in the first 13 columns, followed by at least one blank, and then by
  the  Right Ascension  (hours, minutes and seconds separated by one or more
  blanks),  the  Declination  (Sign,  followed by degree, arc minute and arc
  second,  separated by one or more blanks),  and  by the magnitude.  Proper
  motion data for both  Right Ascension  and  Declination may be  optionally
  inserted preceding the magnitude data.

  Here are some examples of valid entries:

  Column:  1         2         3         4         5         6
  123456789012345678901234567890123456789012345678901234567890
  ------------------------------------------------------------
  Star # 1      13 37 30.33 -00 13 17.3 9.3
  GSC 240601508 05 59 46.35 +31 04 39.9 12.34
  PPM 092899    03 47 29.073 +24 06 18.38 +0.0014 -0.046 2.8
  Sirius         6 45 08.871 -16 42 57.99 -0.0385 -1.205 -1.53

  Most of the Catalogues may not be in exactly that format, but it should be
  easy for someone, even with minimal programming skills, to write a program
  that converts the original data to  that  format.  For  small  numbers  of
  reference stars, manually entering the data is also possible using a text-
  editor.

  If you take data from large catalogues  (e. g., the PPM),  keep your files
  short (including only reference stars surrounding the region of the object
  of interest), as the complete catalogue file will be read each time a star
  chart is plotted.

  Use the  'Utility - Set Star Catalogue'  command to use a  star  catalogue
  other than the GSC in the format above,  and  use  the  'Utility - Default
  Catalogue' to use GSC data again.


* Calculation of the semimajor Axis from the mean daily Motion:
  
  Some sources (e.g., orbital elements for numbered minor planets printed in
  the MPCs) give the mean daily motion (n) instead of the semimajor axis (a)
  for minor planet orbits.  In these cases, enter the value given for  n  in
  the input line for the semimajor axis,  and press the new button  labelled
  "n -> a" near that input line. The computer will read the value of n, will
  calculate the corresponding value for  a,  and set the result in the input
  line.


* ELEMCONV.EXE Tool:
  
  The ELEMCONV.EXE tool, which is located in the /ELM directory on the disk,
  converts orbital elements from the Minor Planet Center's  Computer Service
  in the ELM files used by "Astrometrica".
  Start the program with the parameter /? for further information.


* AREPORT file:
  
  Besides REPORT.TXT, CREPORT.TXT and ASTROMET.LOG, "Astrometrica"  will now
  create another Report-File: AREPORT.TXT.  This file may be used  to report
  astrometric observations of minor planets to the  Minor  Planet Section of
  the Association of Lunar and Planetary Observers (ALPO).


* Windows Support:
  
  There is now also a Program Information File  and  two Icons for those who
  who want to rum "Astrometrica" from Windows.


* Corrected Bugs:
  
  There was a bug  (incorrect path)  accessing some a southern  GSC regions,
  which has been corrected.

  The functions using a second graphics page  (that is, the blink comperator
  and the Zoom) did not work properly when  "Astrometrica"  was started from
  Windows. There should be no more problems with the new version.


* Expanded README.TXT file:
  
  The new README file includes a section called 'Astrometrica interna' which
  describes the data reduction algorithms used by that software. The chapter
  'Tips and Suggestions'  holds  some information on how to get good results
  from  your images:  Above all,  how  to  get  precise  positions of bright
  comets is discussed in some details. Also, there is a section on how to
  report your astrometric observations to the IAU or ALPO.


  For further details, please refer to the file README.TXT!
