% Solar Active Region EUV Spectrum from SERTS, Roger J. Thomas & W.M. Neupert
% Published in Ap.J.Suppl. 91, 461-482, 1994  (Final Version with corrections)
% ----------------------------------------------------------------------------
%	Notes to Table 3

\documentstyle[apjpt]{article}

\begin{document}
\setcounter{page}{8}
\begin{center}
\noindent Notes to Table 3:\\
\begin{enumerate}
\item Blend with first-order line (Fe~XI 349.035~\AA);~~listed values are 
	based on second-order response.
\item Blend with first-order line (Mn~XV 384.745~\AA);~~listed values are 
	based on second-order response.
\item Intensity relative to other Fe~XII lines is significantly lower than 
	predicted by Monsignori-Fossi 1992.
\item Intensity may be affected by possible vignetting at extreme edge of 
	wavelength range.
\item Identified as Ar~XIII by Dere 1978, but our wavelength and intensity 
	match better with Ni~XVIII.
\item Identified as blend with Ar~XIV by Dere 1978, but our wavelength and
	intensity match better with Fe~XV alone. 
\item Identified as Si~X by Behring et al. 1976.  Their Table~1 lists 
	256.38~\AA, but the accompanying note makes clear that this is a 
	calculated value for Si~X whereas the wavelength they actually 
	measured was 256.42~\AA.
\item Identified as blend with Ar~XIV by Dere 1978, but our wavelength and
	intensity match better with Fe~XIV alone. 
\item Identified as blend with Fe~XXI by Dere 1978 in his study of flare 
	spectra.
\item Identified as S XIII by Dere 1978, probably a typographical error.
\item Gaussian fit only to unsaturated portion of line profile;~~thus, 
	measurements are very uncertain.  Listed values for $\sigma_{\lambda}$, 
	$\sigma_I$, and $\sigma_W$ have been increased by a factor of~2 over 
	those resulting from the fit itself.
\item Lower level is given as $^1$S$_1$ by Kelly 1987;~~it should be 
	$^1$S$_0$.
\item Identified as N~IV by Feldman et al. 1987.
\item Measurements very uncertain due to plate flaw.  Listed values for 
	$\sigma_{\lambda}$, $\sigma_I$, and $\sigma_W$ have been increased by a 
	factor of~2 over those resulting from the fit itself.
\item Blend with second-order line (Fe~X 2x174.517~\AA);~~listed values are 
	based on first-order response.
\item Identified as blend with second-order Fe~X by Feldman et al. 1987, 
	but much stronger Fe~X at 2x175.47~\AA\ is not seen in our spectrum.
\item Identified as blend with Ar~XVI by Dere 1978;~~we resolve these two 
	lines.
\item Blend with second-order line (Fe~XII 2x192.373~\AA);~~listed values are 
	based on first-order response.
\item Identified as Ca~X by Behring et al. 1976 and by Dere 1978, and as 
	blend with Ca~X by Feldman et al. 1987.  See Keenan et al. 1993b 
	for our analysis of this line.
\item Intensity relative to other Mg~IX lines is significantly lower than that 
	predicted by Keenan et al. 1993a;~~may be due to instrumental 
	vignetting at extreme edge of wavelength range.
\end{enumerate}

\vspace*{.1in}
~~~i.~~Fit from data smoothed with a 5 pixel ``boxcar'' routine;
  listed values for $\sigma_{\lambda}$, $\sigma_I$, and $\sigma_W$ have 
  been increased by a \\ factor of $\sqrt{2}$ over those resulting from the 
  fit itself.
  ~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~

\vspace*{.1in}
~~~ii.~~Partially saturated at a few spatial locations along the slit, 
  with slight effect on the averaged 
  profile.  Listed values \\ for $\sigma_{\lambda}$, $\sigma_I$, and 
  $\sigma_W$ have been increased by a factor of $\sqrt{2}$ over those 
  resulting from the fit itself.~~~~~~~~~~~~~~~~

\end{center}
\vspace*{.1in}
$^s$Second-order line; b = Blend.
~~~Wavelengths in \AA\ ($\sigma_{\lambda}$ in m\AA);
	Intensities in ergs~cm$^{-2}$s$^{-1}$sr$^{-1}$; FWHM in m\AA.
\vspace*{.1in} 

\noindent ``Behr'' is Behring et al. 1976;~~``Dere'' is Dere
1978 plus Feldman et al. 1987;~~``Kelly'' is Kelly 1987. 
\vspace*{.1in} 

\noindent ID Code is: \\
\hspace*{.2in}	0 = Unidentified;
		1 = Behring et al. 1976;
		2 = Dere 1978;
		3 = Feldman et al. 1987;
		4 = This work using Kelly 1987; \\
\hspace*{.2in}	5 = Keenan et al. 1991;
		6 = Mason \& Bhatia 1978;
		7 = Kastner 1991;
		8 = Behring 1992;
		9 = Monsignori-Fossi 1992.
\end{document}
