\expandafter\ifx\csname doTocEntry\endcsname\relax \expandafter\endinput\fi 
\doTocEntry\toclikesection{}{\csname a:TocLink\endcsname{1}{Q1-1-1}{}{Abstract}}{2}\relax 
\doTocEntry\toclikesection{}{\csname a:TocLink\endcsname{1}{x1-1000}{QQ2-1-2}{Abstract}}{2}\relax 
\doTocEntry\toclikesection{}{\csname a:TocLink\endcsname{1}{Q1-1-3}{}{Contents}}{2}\relax 
\doTocEntry\toclikesection{}{\csname a:TocLink\endcsname{1}{x1-2000}{QQ2-1-4}{Contents}}{2}\relax 
\doTocEntry\tocsection{1}{\csname a:TocLink\endcsname{2}{x2-30001}{QQ2-2-5}{\hbox {}Introduction}}{3}\relax 
\doTocEntry\tocsection{2}{\csname a:TocLink\endcsname{3}{x3-40002}{QQ2-3-6}{\hbox {}SCUBA-2 Data Files}}{5}\relax 
\doTocEntry\tocsection{3}{\csname a:TocLink\endcsname{4}{x4-50003}{QQ2-4-7}{\hbox {}Visualising data}}{7}\relax 
\doTocEntry\tocsubsection{3.1}{\csname a:TocLink\endcsname{4}{x4-60001}{QQ2-4-8}{\hbox {}Concatenating data}}{7}\relax 
\doTocEntry\tocsubsection{3.2}{\csname a:TocLink\endcsname{4}{x4-70002}{QQ2-4-9}{\hbox {}Displaying scan patterns}}{8}\relax 
\doTocEntry\toclof{1}{\csname a:TocLink\endcsname{4}{x4-70031}{}{\ignorespaces The telescope positions during observation number 7 on 20090107. The plot is created by \href  {http://www.starlink.ac.uk/topcat}{Topcat\hbox {}} from the output from \href  {http://www.starlink.ac.uk/cgi-bin/htxserver/sun258.htx/sun258.html?xref_JCMTSTATE2CAT}{jcmtstate2cat\hbox {}} plotting the DRA column (right ascension offset from the map centre in arcsec) against the DDEC column (declination offset from the map centre in arcsec). The PONG scan pattern is clearly visible (see Scott \& Engelen 2008\cite  {sc2ana005}).}}{figure}\relax 
\doTocEntry\tocsubsection{3.3}{\csname a:TocLink\endcsname{4}{x4-80003}{QQ2-4-11}{\hbox {}Displaying data cubes}}{11}\relax 
\doTocEntry\toclof{2}{\csname a:TocLink\endcsname{4}{x4-80012}{}{\ignorespaces Initial \href  {http://www.starlink.ac.uk/cgi-bin/htxserver/sun214.htx/sun214.html?xref_}{Gaia\hbox {}} windows displayed upon loading a data cube (with slight modifications to the colour table using options under the `File' and then `Startup options'). \textbf  {Left:} The main window, after clicking the `Z' button a number of times to zoom-in, shows a map of bolometer values at a fixed sample in time. Note that these data came from an array with a number of broken columns and broken isolated bolometers, all indicated in grey. \textbf  {Right:} The `Display image sections of a cube' dialogue enables the user to navigate the time dimension. The `Index of plane' slider near the top can be used to select different time slices, and the main window will automatically update.}}{figure}\relax 
\doTocEntry\toclof{3}{\csname a:TocLink\endcsname{4}{x4-80033}{}{\ignorespaces The `Spectral Plot' window is spawned automatically once a bolometer is clicked in the main window, such as (13,23) in this example, displaying its time-varying signal. The vertical red line indicates the time slice that is currently selected in the `Display image sections of a cube' dialogue. The regular pattern, with a period of about 30 seconds in this particular case, is slow baseline drift correlated with variations in the SCUBA-2 fridge temperature. The green-circled narrow spike is produced by the bolometer crossing Uranus. Usually astronomical signals are not readily visible in raw time series plots such as these, since they are relatively much fainter. Note that on some systems `gaps' may appear, such as those at the start of the time series, and at $\sim 34$\tmspace  +\thinmuskip {.1667em}s in this example. These are simply rendering artefacts due to re-sampling the data to the resolution of the display (zooming-in to these regions using the `Lower index' and `Upper index' sliders in the `Display image sections of a cube' dialogue followed by a click on `Re-extract' to update the plot demonstrates this).}}{figure}\relax 
\doTocEntry\tocsubsection{3.4}{\csname a:TocLink\endcsname{4}{x4-90004}{QQ2-4-14}{\hbox {}Regridding data into a map}}{17}\relax 
\doTocEntry\toclof{4}{\csname a:TocLink\endcsname{4}{x4-90044}{}{\ignorespaces Map produced from raw data of a scan across Uranus. The image is completely dominated by noise in the relative signal offsets of each bolometer, and no astronomical signal can be seen. The scan (a Curvy PONG) can clearly be seen as a repetitive `waffle' pattern in the image.}}{figure}\relax 
\doTocEntry\tocsubsection{3.5}{\csname a:TocLink\endcsname{4}{x4-100005}{QQ2-4-16}{\hbox {}Cleaning data}}{20}\relax 
\doTocEntry\tocsubsubsection{3.5.1}{\csname a:TocLink\endcsname{4}{x4-110001}{QQ2-4-17}{\hbox {}Removing bolometer averages and DC Steps}}{20}\relax 
\doTocEntry\toclof{5}{\csname a:TocLink\endcsname{4}{x4-110055}{}{\ignorespaces \textbf  {Top:} \href  {http://www.starlink.ac.uk/cgi-bin/htxserver/sun214.htx/sun214.html?xref_}{Gaia\hbox {}} plot of the array signal at time slice 1 after using \href  {http://www.starlink.ac.uk/cgi-bin/htxserver/sun258.htx/sun258.html?xref_SC2CLEAN}{sc2clean\hbox {}} to remove the mean of each bolometer signal (clean.sdf). The LOW and HIGH data values for this intensity plot are $-1.7171$\tmspace  +\thinmuskip {.1667em}pW and $+5.50352$\tmspace  +\thinmuskip {.1667em}pW, respectively. Most of the working bolometers (not grey) now have approximately the same signal range (approximately $\pm 0.1$\tmspace  +\thinmuskip {.1667em}pW), and therefore have nearly the same colour (brown). However, there are several outliers, for example, the orange pixel with an `x' at (10,17). \textbf  {Bottom:} The time series for bolometer (10,17) showing the presence of a large level change, or `DC Step' near 30\tmspace  +\thinmuskip {.1667em}s.}}{figure}\relax 
\doTocEntry\toclof{6}{\csname a:TocLink\endcsname{4}{x4-110106}{}{\ignorespaces Map produced from `clean2.sdf' in which DC steps have been repaired and the bolometer means have been subtracted. There are still many artefacts in the data, but now Uranus is visible.}}{figure}\relax 
\doTocEntry\tocsubsubsection{3.5.2}{\csname a:TocLink\endcsname{4}{x4-120002}{QQ2-4-20}{\hbox {}Watching a movie}}{26}\relax 
\doTocEntry\tocsubsubsection{3.5.3}{\csname a:TocLink\endcsname{4}{x4-130003}{QQ2-4-21}{\hbox {}Frequency-domain filtering}}{26}\relax 
\doTocEntry\toclof{7}{\csname a:TocLink\endcsname{4}{x4-130017}{}{\ignorespaces High-pass filtered data (clean3.sdf). \textbf  {Top:} The time series for a single bolometer (13,23). Comparing with the un-filtered data in Fig.\nobreakspace  {}\o:ref {fig:gaia_spec}, the positive spikes produced by Uranus are now much more apparent. \textbf  {Bottom:} a map produced from these cleaned and filtered data. The brightness of Uranus compared to the noise is now much more significant than in Fig.\nobreakspace  {}\o:ref {fig:map_dc_mean}, but the filtering has caused ringing around the source-crossing in the time series, which appears as negative dips in the map along the scan directions (i.e. a negative cross around the source).}}{figure}\relax 
\doTocEntry\tocsubsection{3.6}{\csname a:TocLink\endcsname{4}{x4-140006}{QQ2-4-23}{\hbox {}Bolometer power-spectra}}{29}\relax 
\doTocEntry\toclof{8}{\csname a:TocLink\endcsname{4}{x4-140378}{}{\ignorespaces The power spectrum of bolometer (13,23) produced by the \href  {http://www.starlink.ac.uk/cgi-bin/htxserver/sun258.htx/sun258.html?xref_}{Smurf\hbox {}} task \href  {http://www.starlink.ac.uk/cgi-bin/htxserver/sun258.htx/sun258.html?xref_SC2FFT}{sc2fft\hbox {}}. In this particular case the noise looks flat above a $1/f$ knee of about 1\tmspace  +\thinmuskip {.1667em}Hz. The red line simply indicates the frequency slice currently being displayed in the main \href  {http://www.starlink.ac.uk/cgi-bin/htxserver/sun214.htx/sun214.html?xref_}{Gaia\hbox {}} window (not shown).}}{figure}\relax 
\doTocEntry\tocsubsection{3.7}{\csname a:TocLink\endcsname{4}{x4-150007}{QQ2-4-25}{\hbox {}Data quality flagging}}{33}\relax 
\doTocEntry\tocsection{4}{\csname a:TocLink\endcsname{5}{x5-160004}{QQ2-5-26}{\hbox {}Dynamic Iterative Map-Making}}{35}\relax 
\doTocEntry\toclof{9}{\csname a:TocLink\endcsname{5}{x5-161629}{}{\ignorespaces Map of Uranus produced with the \href  {http://www.starlink.ac.uk/cgi-bin/htxserver/sun258.htx/sun258.html?xref_}{Smurf\hbox {}} task \href  {http://www.starlink.ac.uk/cgi-bin/htxserver/sun258.htx/sun258.html?xref_MAKEMAP}{makemap\hbox {}} using the iterative algorithm with default parameters. The S/N of the source is now greatly improved compared to the simplistic reduction in Fig.\nobreakspace  {}\o:ref {fig:highpass}, and the negative ringing has been removed.}}{figure}\relax 
\doTocEntry\toclof{10}{\csname a:TocLink\endcsname{5}{x5-1622510}{}{\ignorespaces Time-domain components of the iterative solution for bolometer (13,23). From top to bottom: ASTronomical signal (clearly showing Uranus as positive spikes); COMmon mode (dominated by 30\tmspace  +\thinmuskip {.1667em}s fridge variations); FiLTered (residual low-frequency noise missed by COM); RESidual (looking flat, except for a small residual around the location of a repaired DC step); and QUAlity (indicating the location of the DC step -- the numerical value 8; this region of the data is not used in the final map). All of the plots were produced with \href  {http://www.starlink.ac.uk/cgi-bin/htxserver/sun214.htx/sun214.html?xref_}{Gaia\hbox {}}, restricting the range of the $x$-axis to samples 2840--11500.}}{figure}\relax 
\doTocEntry\tocsubsection{4.1}{\csname a:TocLink\endcsname{5}{x5-170001}{QQ2-5-29}{\hbox {}Configuration Files}}{44}\relax 
\doTocEntry\tocsection{5}{\csname a:TocLink\endcsname{6}{x6-180005}{QQ2-6-30}{\hbox {}Calibrating SCUBA-2 Data}}{46}\relax 
\doTocEntry\tocsubsection{5.1}{\csname a:TocLink\endcsname{6}{x6-190001}{QQ2-6-31}{\hbox {}Extinction Correction}}{46}\relax 
\doTocEntry\tocsubsection{5.2}{\csname a:TocLink\endcsname{6}{x6-200002}{QQ2-6-32}{\hbox {}Flux conversion factors}}{48}\relax 
\doTocEntry\tocsection{6}{\csname a:TocLink\endcsname{7}{x7-210006}{QQ2-7-33}{\hbox {}Examples of different reductions}}{53}\relax 
\doTocEntry\tocsubsection{6.1}{\csname a:TocLink\endcsname{7}{x7-220001}{QQ2-7-34}{\hbox {}Deep point source maps}}{53}\relax 
\doTocEntry\toclof{11}{\csname a:TocLink\endcsname{7}{x7-2201111}{}{\ignorespaces Maps of a deep cosmology field towards the cluster MS0451, at 450\relax \c:def \A:mbox {\A:mbox }\c:def \B:mbox {\B:mbox }\unhbox \voidb@x \hbox {\tmspace  +\thinmuskip {.1667em}${\umu }$m}. \textbf  {Left:} map using the specialized \texttt  {dimmconfig_blank_field.lis} which gives a significantly flatter result than \textbf  {Right:} map using the default \texttt  {dimmconfig.lis}.}}{figure}\relax 
\doTocEntry\toclof{12}{\csname a:TocLink\endcsname{7}{x7-2202012}{}{\ignorespaces 450\relax \c:def \A:mbox {\A:mbox }\c:def \B:mbox {\B:mbox }\unhbox \voidb@x \hbox {\tmspace  +\thinmuskip {.1667em}${\umu }$m} maps processed with the \href  {http://www.starlink.ac.uk/cgi-bin/htxserver/sun265.htx/sun265.html?xref_}{Picard\hbox {}} recipe \texttt  {SCUBA2_MATCHED_FILTER}, suppressing scales larger than 15\tmspace  +\thinmuskip {.1667em}arcsec. \textbf  {Left:} filtered map of Uranus from Fig.\nobreakspace  {}\o:ref {fig:itermap}. \textbf  {Right:} filtered version of deep cosmology map from left-hand panel of Fig.\nobreakspace  {}\o:ref {fig:cosmomap}.}}{figure}\relax 
\doTocEntry\toclof{13}{\csname a:TocLink\endcsname{7}{x7-2202513}{}{\ignorespaces S/N map produced from the match-filtered image of the cluster MS0451 in Fig.\nobreakspace  {}\o:ref {fig:cosmo_filt}, scaled from $-4\sigma $ (black) to $+4\sigma $ (white).}}{figure}\relax 
\doTocEntry\toclof{14}{\csname a:TocLink\endcsname{7}{x7-2202614}{}{\ignorespaces The distribution of S/N for the central $100 \times 100$ pixels of Fig.\nobreakspace  {}\o:ref {fig:cosmo_filt} (histogram), compared with an ideal Gaussian distribution with mean zero and $\sigma =1$ (dashed line). The fact that the real distribution is narrower demonstrates that in this region of the map the noise is probably slightly over-estimated.}}{figure}\relax 
\doTocEntry\tocsubsection{6.2}{\csname a:TocLink\endcsname{7}{x7-230002}{QQ2-7-39}{\hbox {}Extended Galactic Sources}}{67}\relax 
\doTocEntry\tocsubsubsection{6.2.1}{\csname a:TocLink\endcsname{7}{x7-240001}{QQ2-7-40}{\hbox {}Standard DIMM configuration + \href  {http://www.starlink.ac.uk/cgi-bin/htxserver/sun265.htx/sun265.html?xref_}{Picard\hbox {}}}}{68}\relax 
\doTocEntry\toclof{15}{\csname a:TocLink\endcsname{7}{x7-2401115}{}{\ignorespaces \textbf  {Top row:} Orion22.sdf (left) and Orion23.sdf (right) maps from the mapmaker with no post processing. A patchy background and negative bowling around the strong sources is apparent. \textbf  {Bottom row:} Orion22_back.sdf (left) and Orion23_back.sdf (right). The top row maps following processing with the \href  {http://www.starlink.ac.uk/cgi-bin/htxserver/sun265.htx/sun265.html?xref_}{Picard\hbox {}} recipe \texttt  {REMOVE_BACKGROUND} using \href  {http://www.starlink.ac.uk/cgi-bin/htxserver/sun255.htx/sun255.html?xref_FINDBACK}{findback\hbox {}} with a box size of 30 pixels (120\tmspace  +\thinmuskip {.1667em}arcsec).}}{figure}\relax 
\doTocEntry\toclof{16}{\csname a:TocLink\endcsname{7}{x7-2402816}{}{\ignorespaces Orion23_back_crop_mos.sdf. The final map following the post processing steps of background removal, cropping and coadding with wcsmosaic.}}{figure}\relax 
\doTocEntry\tocsubsubsection{6.2.2}{\csname a:TocLink\endcsname{7}{x7-250002}{QQ2-7-43}{\hbox {}Bright / extended DIMM configuration}}{74}\relax 
\doTocEntry\toclof{17}{\csname a:TocLink\endcsname{7}{x7-2500517}{}{\ignorespaces \textbf  {Top:} Map using all of the same data as in Fig.\nobreakspace  {}\o:ref {fig:orionmakemap}, but processed simultaneously using a single call to \href  {http://www.starlink.ac.uk/cgi-bin/htxserver/sun258.htx/sun258.html?xref_MAKEMAP}{makemap\hbox {}} with the specialized \texttt  {dimmconfig_bright_extended.lis}. \textbf  {Bottom:} The QUALITY component of the resulting map indicates (white) where the map has been constrained to zero after all but the final iteration. It is selected based on a S/N threshold.}}{figure}\relax 
\doTocEntry\tocsection{7}{\csname a:TocLink\endcsname{8}{x8-260007}{QQ2-8-45}{\hbox {}Cheat sheet for checking data quality}}{79}\relax 
\doTocEntry\tocsubsection{7.1}{\csname a:TocLink\endcsname{8}{x8-270001}{QQ2-8-46}{Using \href  {http://www.starlink.ac.uk/cgi-bin/htxserver/sun258.htx/sun258.html?xref_SC2CLEAN}{sc2clean\hbox {}} to help inspect time-series}}{79}\relax 
\doTocEntry\tocsubsection{7.2}{\csname a:TocLink\endcsname{8}{x8-280002}{QQ2-8-47}{Looking at calibration data}}{80}\relax 
\doTocEntry\toclikesection{}{\csname a:TocLink\endcsname{1}{Q1-1-48}{}{sstrefsectionReferences}}{82}\relax 
\doTocEntry\toclikesection{}{\csname a:TocLink\endcsname{1}{x1-290002}{QQ2-1-49}{References}}{82}\relax 
\doTocEntry\tocsection{}{\csname a:TocLink\endcsname{1}{Q1-1-50}{}{References}}{82}\relax 
\doTocEntry\tocsection{A}{\csname a:TocLink\endcsname{9}{x9-300001}{QQ2-9-51}{\hbox {}Data Characteristics and Issues}}{84}\relax 
\doTocEntry\tocsubsection{A.1}{\csname a:TocLink\endcsname{9}{x9-310001}{QQ2-9-52}{\hbox {}Introduction data issues}}{84}\relax 
\doTocEntry\tocsubsection{A.2}{\csname a:TocLink\endcsname{9}{x9-320002}{QQ2-9-53}{\hbox {}Telescope tracking}}{85}\relax 
\doTocEntry\toclof{18}{\csname a:TocLink\endcsname{9}{x9-3200518}{}{\ignorespaces \textsl  {left:} Actual tracking; \textsl  {Right:} Demanded tracking }}{figure}\relax 
\doTocEntry\tocsubsection{A.3}{\csname a:TocLink\endcsname{9}{x9-330003}{QQ2-9-55}{\hbox {}Flat field}}{88}\relax 
\doTocEntry\toclof{19}{\csname a:TocLink\endcsname{9}{x9-3300119}{}{\ignorespaces Mean signal in time-series }}{figure}\relax 
\doTocEntry\toclof{20}{\csname a:TocLink\endcsname{9}{x9-3301420}{}{\ignorespaces \textsl  {left:} Mean signal in DC-removed time-series; \textsl  {Right:} Histogram of values in DC-removed time series }}{figure}\relax 
\doTocEntry\tocsubsection{A.4}{\csname a:TocLink\endcsname{9}{x9-340004}{QQ2-9-58}{\hbox {}Spikes and Steps}}{94}\relax 
\doTocEntry\toclof{21}{\csname a:TocLink\endcsname{9}{x9-3400121}{}{\ignorespaces Example time series in the DC-corrected data set showing spikes, steps, and noisy bolometers. The dominant common-mode signal is a variation due to a 30\nobreakspace  {}s temperature cycle in the dilution fridge. \textsl  {Top-left:} a bolometer with a typical time series. Variations due to the 30\nobreakspace  {}s fridge oscillation are obvious. Since all bolometers share this oscillation it is a `common-mode' signal, but the amplitude may vary for different bolometers. \textsl  {Top-right:} a bolometer with spikes in the time series. \textsl  {Middle-left:} a bolometer with a moderate `step'. Steps can be introduced by the bias for that bolometer `rolling-over' as it reaches its limit. During the S2SRO the instrument software that flags these events was not active. \textsl  {Middle-right:} a bolometer with a large step. \textsl  {Bottom-left:} a bolometer with multiple steps and spikes. \textsl  {Bottom-right:} a `noisy' bolometer. }}{figure}\relax 
\doTocEntry\toclof{22}{\csname a:TocLink\endcsname{9}{x9-3402922}{}{\ignorespaces Original (white) and sc2clean step-corrected (red) time series.}}{figure}\relax 
\doTocEntry\tocsubsection{A.5}{\csname a:TocLink\endcsname{9}{x9-350005}{QQ2-9-61}{\hbox {}Common Mode Signal}}{100}\relax 
\doTocEntry\tocsubsubsection{A.5.1}{\csname a:TocLink\endcsname{9}{x9-360001}{QQ2-9-62}{\hbox {}Method 1}}{100}\relax 
\doTocEntry\toclof{23}{\csname a:TocLink\endcsname{9}{x9-3601323}{}{\ignorespaces Example time series in the block-median common-mode subtracted data set high-lighting intrinsic noise issues that can be seen in bolometers. The top-left time series is the same as the top-left time series in figure Fig.\nobreakspace  {}\o:ref {fig:timeseries}}}{figure}\relax 
\doTocEntry\tocsubsubsection{A.5.2}{\csname a:TocLink\endcsname{9}{x9-370002}{QQ2-9-64}{\hbox {}Method 2}}{103}\relax 
\doTocEntry\toclof{24}{\csname a:TocLink\endcsname{9}{x9-3702124}{}{\ignorespaces Example time series (white) and the derived common-mode signal (red). This time series is the same as the top-left time serie in Figs.\nobreakspace  {}\o:ref {fig:timeseries} and \o:ref {fig:timeseries2}}}{figure}\relax 
\doTocEntry\toclof{25}{\csname a:TocLink\endcsname{9}{x9-3702225}{}{\ignorespaces Histogram of the bolometer gains as derived by the DIMM based on their response to the common-mode signal. Note that these gains are, by default, only used for the subtraction of the common mode and not for the subsequent gridding into a map.}}{figure}\relax 
\doTocEntry\toclof{26}{\csname a:TocLink\endcsname{9}{x9-3703126}{}{\ignorespaces \textsl  {Left:} Gain image: black $<$ 0.75, white $>$ 1.25; \textsl  {Middle:} Common-mode subtracted median: black $< -$5e-04, white $>$ 5e-04 \textsl  {Right:} Common-mode subtracted rms: white $>$ 6e-03 (twice the median).}}{figure}\relax 
\doTocEntry\toclof{27}{\csname a:TocLink\endcsname{9}{x9-3705627}{}{\ignorespaces Sample time-series with a simple common-mode subtracted.}}{figure}\relax 
\doTocEntry\tocsubsection{A.6}{\csname a:TocLink\endcsname{9}{x9-380006}{QQ2-9-69}{\hbox {}Maps}}{117}\relax 
\doTocEntry\toclof{28}{\csname a:TocLink\endcsname{9}{x9-3800128}{}{\ignorespaces  \textsl  {Top left:} Map of the concatenated data; \textsl  {Top right:} After removing a linear baseline from the time series; \textsl  {Bottom left:} After linear baseline, steps, and spike removal; \textsl  {Bottom right:} Iterative map maker with \texttt  {dimmconfig_bright_compact.lis} }}{figure}\relax 
\doTocEntry\tocsubsection{A.7}{\csname a:TocLink\endcsname{9}{x9-390007}{QQ2-9-71}{\hbox {}Sample Common-mode script}}{121}\relax 
\doTocEntry\tocsection{B}{\csname a:TocLink\endcsname{10}{x10-400002}{QQ2-10-72}{Notes on Shared Risk Observing}}{123}\relax 
\doTocEntry\tocsubsection{B.1}{\csname a:TocLink\endcsname{10}{x10-410001}{QQ2-10-73}{S2SRO FCFs}}{123}\relax 
\doTocEntry\toclot{1}{\csname a:TocLink\endcsname{10}{x10-410011}{}{\ignorespaces Secondary calibrators used for flux calibration of SCUBA-2. The flux values are sourced from the references noted in the table. }}{table}\relax 
\doTocEntry\toclof{29}{\csname a:TocLink\endcsname{10}{x10-4100429}{}{\ignorespaces Histograms of the 450\relax \c:def \A:mbox {\A:mbox }\c:def \B:mbox {\B:mbox }\unhbox \voidb@x \hbox {\tmspace  +\thinmuskip {.1667em}${\umu }$m} (left) and 850\relax \c:def \A:mbox {\A:mbox }\c:def \B:mbox {\B:mbox }\unhbox \voidb@x \hbox {\tmspace  +\thinmuskip {.1667em}${\umu }$m} (right) \ensuremath  {\mathrm@@ {FCF\sb {beamequiv}}} values calculated for the secondary calibrators observed during the S2SRO period.}}{figure}\relax 
\doTocEntry\tocsubsection{B.2}{\csname a:TocLink\endcsname{10}{x10-420002}{QQ2-10-76}{Method for calibrating your data}}{129}\relax 
\doTocEntry\tocsubsection{B.3}{\csname a:TocLink\endcsname{10}{x10-430003}{QQ2-10-77}{\hbox {}Significant Events}}{130}\relax 
\doTocEntry\tocsubsubsection{B.3.1}{\csname a:TocLink\endcsname{10}{x10-440001}{QQ2-10-78}{Data Files}}{130}\relax 
\doTocEntry\tocsubsubsection{B.3.2}{\csname a:TocLink\endcsname{10}{x10-450002}{QQ2-10-79}{\hbox {}Flatfields}}{130}\relax 
\doTocEntry\tocsubsubsection{B.3.3}{\csname a:TocLink\endcsname{10}{x10-460003}{QQ2-10-80}{Setup}}{131}\relax 
\doTocEntry\tocsubsubsection{B.3.4}{\csname a:TocLink\endcsname{10}{x10-470004}{QQ2-10-81}{Electronics}}{131}\relax 
\doTocEntry\tocsubsubsection{B.3.5}{\csname a:TocLink\endcsname{10}{x10-480005}{QQ2-10-82}{Weather}}{132}\relax 
\doTocEntry\tocsubsubsection{B.3.6}{\csname a:TocLink\endcsname{10}{x10-490006}{QQ2-10-83}{Telescope}}{132}\relax 
\doTocEntry\tocsection{C}{\csname a:TocLink\endcsname{11}{x11-500003}{QQ2-11-84}{\hbox {}List of acronyms}}{133}\relax 
\par