this is for holding javascript data
Nick Konidaris added wave.tex
about 9 years ago
Commit id: a8dee43fd176a1c28b96b3bdb125b0a7b25c926c
deletions | additions
diff --git a/wave.tex b/wave.tex
new file mode 100644
index 0000000..0fe963a
--- /dev/null
+++ b/wave.tex
...
\subsection{Wavelength solution}
This step produces a set of coefficients for each trace. These coefficients return a wavelength solution as a function of pixel position along the trace.
\subsubsection{Input}
\begin{itemize}
\item \verb{\$arcname.fits} -- Arclamp image where a \$arcname is something like Hg, Cd, Zn, Xe, etc...
\item \verb{cat_Hg.fits.txt} -- Is the result of SexTractor on finding the locations of the Mercury lines.
\item \verb{dome.fits_segments.npy} -- Trace locations from trace finding module.
\end{itemize}
\subsubsection{Output}
dome.fits\_segments.npy contains a list (length the number of segments) of dictionaries. Each dictionary contains information about the location of each segment.
\begin{itemize}
\item ok (boolean) -- The segment has more than 50 illuminated pixels
\item mean\_ys ([float]) -- The mean Y location of each pixel in the trace. It's length is usually between 200 to 270 pixels long.
\item xs ([float]) -- The X location of each pixel. It's length is the same as means. The ridgeline of the trace is constructed from the points in (xs, means).
\item trace\_sigma (float) -- The 1 $\sigma$ width of the trace. An in focus image should have a FWHM of about 2.5 pixels and thus sigma should be about 1.06.
\item coeffs_y ([float]) -- A list of polynomial coefficients of order len(poly)-1 that is the best fit line to (xs, means). The bulk of this step's work is to derive poly.
\end{itemize}
