From 0049ba787e55d5c0794a57d8ad551389eb0e136f Mon Sep 17 00:00:00 2001 From: "Malcolm J. Currie" Date: Sun, 16 Sep 2012 19:45:07 -1000 Subject: [PATCH] docs: SC/21---Use ~ over \, as it looks better in the hypertext. (cherry picked from commit a4edcc41f8557fea13d6bb4529f803bc8de9edd8) --- docs/sc/021/sc21.tex | 5 ++--- 1 file changed, 2 insertions(+), 3 deletions(-) diff --git a/docs/sc/021/sc21.tex b/docs/sc/021/sc21.tex index 24b14942ee3..70626786291 100644 --- a/docs/sc/021/sc21.tex +++ b/docs/sc/021/sc21.tex @@ -741,7 +741,7 @@ \subsection{\xlabel{obs_modes}Observing modes} \end{minipage} \begin{minipage}[t]{0.85\linewidth} \textsc{daisy} maps are the option for point-like or compact sources -($<$3\,arcmin) by maximising the exposure time on the centre of the +($<$3~arcmin) by maximising the exposure time on the centre of the image. The telescope moves at a constant velocity in a `spirograph' pattern that has the advantage of keeping the source on the array throughout the observation. This is shown in the top panel of @@ -3280,7 +3280,7 @@ \subsection{\xlabel{fcf}Flux conversion factors (FCF)} flux density and the FWHM. The integrated flux density within a given aperture (30-arcsec radius default) is calculated using \photom\ \autophotom. Flux densities for calibrators such as Uranus, - Mars, CRL\,618, CRL\,2688 and HL\,Tau are already known to + Mars, CRL~618, CRL~2688 and HL~Tau are already known to \picard. To derive an FCF for other sources of known flux densities, the fluxes can be added to the parameter file with the source name (in upper case, spaces removed): \texttt{FLUX\_450.MYSRC = 0.050} @@ -4684,4 +4684,3 @@ \section{\xlabel{acronyms}List of Acronyms} \end{document} -