<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2 Final//EN"> <!--Converted with LaTeX2HTML 98.1p1 release (March 2nd, 1998) originally by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds * revised and updated by: Marcus Hennecke, Ross Moore, Herb Swan * with significant contributions from: Jens Lippmann, Marek Rouchal, Martin Wilck and others --> <HTML> <HEAD> <TITLE>How to get it</TITLE> <META NAME="description" CONTENT="How to get it"> <META NAME="keywords" CONTENT="vol2"> <META NAME="resource-type" CONTENT="document"> <META NAME="distribution" CONTENT="global"> <META HTTP-EQUIV="Content-Type" CONTENT="text/html; charset=iso-8859-1"> <LINK REL="STYLESHEET" HREF="vol2.css"> <LINK REL="next" HREF="node252.html"> <LINK REL="previous" HREF="node250.html"> <LINK REL="up" HREF="node249.html"> <LINK REL="next" HREF="node252.html"> </HEAD> <BODY > <!--Navigation Panel--> <A NAME="tex2html4576" HREF="node252.html"> <IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="icons.gif/next_motif.gif"></A> <A NAME="tex2html4573" HREF="node249.html"> <IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="icons.gif/up_motif.gif"></A> <A NAME="tex2html4567" HREF="node250.html"> <IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="icons.gif/previous_motif.gif"></A> <A NAME="tex2html4575" HREF="node1.html"> <IMG WIDTH="65" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="contents" SRC="icons.gif/contents_motif.gif"></A> <BR> <B> Next:</B> <A NAME="tex2html4577" HREF="node252.html">What to do with</A> <B> Up:</B> <A NAME="tex2html4574" HREF="node249.html">Introduction</A> <B> Previous:</B> <A NAME="tex2html4568" HREF="node250.html">What is needed</A> <BR> <BR> <!--End of Navigation Panel--> <H2><A NAME="SECTION001812000000000000000"> How to get it</A> </H2> <P> To help you get the necessary calibration data in the least observing time, the planning program generates a schedule of required observations. A considerable amount of photometric expertise is built into this program, so that observers without much photometric experience can confidently adopt its recommended defaults, and obtain a plan that should be satisfactory for most photometric observing programs. At the same time, the program is flexible enough to let experienced observers design special-purpose programs. <P> This flexibility requires considerable interaction between the user and the planning program. The program needs information about the program stars, the calibration stars, the peculiarities of the instrument, and the requirements of the observer. This input information is described in detail below, and in the appendix on data-file formats. <P> <BR><HR> <ADDRESS> <I>Petra Nass</I> <BR><I>1999-06-15</I> </ADDRESS> </BODY> </HTML>
