TABLE OF CONTENTS


1.  INTRODUCTION

2.  FIT
	2.1  Introduction
	2.2  Compiling and linking
	2.3  Input files
	2.4  Program FIT
	2.5  FIT - More Notes
	2.6  References

3.  TAB
	3.1  Generating Data Tables with TAB
	3.2  TAB Instruction List

4.  PLOT-NIT
	4.1  Looking at Night to Night Tables  (- Night Table -)

5.  PLOT-CLR
	5.1  Looking at Within Night Tables  (-Color Table-)

6.  PLOTTING
	6.1  Batch Printing of Graphs
	6.2  CLR File
	6.3  NIT File
	

7.  PERIOD
	7.1  Program
	7.2  Synopsis
	7.3  Purpose
	7.4  Description
	7.5  Computer Requirements
	7.6.0  Instructions/User Manual
		7.6.1  Preparing a data file
		7.6.2  Files required to run
		7.6.3  Description of a Sample Run
		7.6.4  The report
		7.6.5.0 Important Definitions
			7.6.5.1 Minimum Frequency
			7.6.5.2 Nyquist Frequency
	7.7  Compiling
	7.8  Algorithm
	7.9  Program Flow
	7.10  Bugs
	7.11  Suggestion for future work
	7.12 References




1.0  Introduction

	These programs were written to analyze robotic telescope data from the Fairborn Observatory in 
Arizona.  The programs were developed for William J. Borucki at NASA Ames Research Center by Bob 
Hogan and Kurt D. Schwehr.  Bod Hogan wrote FIT and TAB.  Kurt D. Schwehr wrote PLOT-NIT, 
PLOT-CLR, and PERIOD.  This manual was written by Kurt D. Schwehr, except for section 2.0 FIT.  
Direct all questions and comments to:

 				William Borucki
				MS 245-3
				NASA Ames Research
				Moffett Field, CA.
				(415)604-6492

	The process of data analysis is taken car of by five programs.  The data is transferred from the 
observatory's computer every couple of days.  Each ATIS file contains data for one night and is 
compressed into an archive (ARC).  Once the files are on the local computer, the program FIT does some 
initial data reduction and creates a very large binary data file.  The program TAB is used to extract data 
for each star.  The data is stored in ASCII tables that can be inspected, graphed and analyzed.  PLOT-NIT 
and PLOT-CLR will plot up the data for viewing and printing.  Finally, PERIOD is used to determine if 
any of the stars observed are likely to be variable. The next sections describe each of the five programs.