<!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>Column label: MOONW</TITLE> <META NAME="description" CONTENT="Column label: MOONW"> <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="previous" HREF="node588.html"> <LINK REL="up" HREF="node584.html"> <LINK REL="next" HREF="node590.html"> </HEAD> <BODY > <!--Navigation Panel--> <A NAME="tex2html8880" HREF="node590.html"> <IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="icons.gif/next_motif.gif"></A> <A NAME="tex2html8877" HREF="node584.html"> <IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="icons.gif/up_motif.gif"></A> <A NAME="tex2html8873" HREF="node588.html"> <IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="icons.gif/previous_motif.gif"></A> <A NAME="tex2html8879" 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="tex2html8881" HREF="node590.html">MOUNTING='GERMAN'</A> <B> Up:</B> <A NAME="tex2html8878" HREF="node584.html">MOUNTING='FORK'</A> <B> Previous:</B> <A NAME="tex2html8874" HREF="node588.html">Column label: OBSW</A> <BR> <BR> <!--End of Navigation Panel--> <H3><A NAME="SECTION003243500000000000000"> Column label: MOONW</A> </H3> The values in this column are the corresponding hour angles of the western ``moonlight'' limits, in decimal degrees. <P> A simple sanity check on the tabular data is that the ``moonlight'' limits should always be closer to the horizon (i.e., farther from the meridian) than the ``observing'' limits, at every declination. The difference is approximately the angular size of the telescope entrance pupil, as seen from the object that obscures the horizon. If the obscuration is nearby, the difference may be many degrees; if distant, it may be a fraction of a degree. <P> <BR><HR> <ADDRESS> <I>Petra Nass</I> <BR><I>1999-06-15</I> </ADDRESS> </BODY> </HTML>
