\documentstyle [adc,11pt]{article}
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\newcommand{\dmv}{Documentation for the Computer-Readable Version}
\newcommand{\cat}{Atlas and Catalogue of Infrared Sources in the Magellanic
Clouds}
\newcommand{\abbr}{IRMC}
\newcommand{\catref}{Schwering and Israel (1990)}
\newcommand{\pcatref}{Schwering, P. B. W. and Israel, F. P.}
\newcommand{\docnum}{NSSDC/WDC-A-R\&S 93-10}
\parindent 0pt
\parskip 11pt
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\begin{document}
%
\title{\cat}
\author{(\pcatref)}
\docauthor{Nancy G. Roman}
\docno{NSSDC/WDC-A-R\&S 93-10}
\date{March 1993 }
\maketitle

\begin{abstract}
The authors have used the IRAS data to construct maps of the Magellanic Clouds
at wavelengths of 12, 25, 60, and 100 microns.  These are contained in the
published volume.  The position and characteristics of each source are included
in this compilation.  Also included are cross references to sources at other
wavelengths (H-alpha emission nebulae, dark clouds, and stars) when these could
be reasonably identified with the IR sources.
\end{abstract}

\section{Introduction}

The {\em \cat} as presented here contains a list of sources in the Large and
Small Magellanic Clouds as observed in the Additional Observations program of
the Deep Sky Mapping mode of the IRAS mission. Fluxes are given in the IRAS
wavelengths of 12, 25, 60, and 100 microns. Maps of these sources are presented
in the Source Reference. This version also provides cross identifications to
sources observed in other wavelengths.

\section {Source Reference}

\begin{references}

\item {\em Atlas and Catalogue of Infrared Sources in the Magellanic Clouds}
      Schwering, P.B.W. and Israel, F. P., 1990 Kluwer Academic Publishers,
      Dordrecht/Boston/London.
\end {references}


\section {Structure}

\subsection{File Structure}

The {\em Atlas and Catalogue of Infrared Sources in the Magellanic Clouds} as
distributed here is in two files. The first file contains the information on all
of the infrared sources. The second table contains the cross identifications
with sources in other wavelengths. Table 1 contains the characteristics of these
files. In the first file, the two tables in the published paper for the SMC and
LMC, respectively, have been concatenated. Each record has been prefixed by
``S'' or ``L'' to indicate in which cloud the source is located. In the second,
the individual tables in the printed volume have also been concatenated with the
addition of identifiers to distinguish the parts.

A copy of this document should be transmitted with any additional copy of this
catalog.


\begin{table}
\begin{center}
\begin{tabular}{ c l c c }
\hline
File      & Contents          & Logical Record  & Total Number of    \\
          &                   &  Length         & Logical Records    \\
\hline
1         & Source List       & 122             & 2140               \\
2         & Cross References  &  97             &  993               \\
\hline
\end{tabular}
\caption{File Content}
\end{center}
\label{T:files}
\end{table}


\subsection{File Format}

Table 2 gives a byte-by-byte description of the contents of File 1. File 2
should be read with an A97 format.

\begin{table}
\begin{center}
\begin{tabular}{ c c c l }
\hline
          &                     &        &                          \\
Bytes     & Unit                &Format  & Item                     \\  \hline
 1        &                     & A1     & Cloud                    \\
 2 - 5    &                     & I4     & Source Number            \\
 8 - 9    & h                   & I2     & Right Ascension (1950)   \\
11 - 12   & min                 & I2     & Right Ascension (1950)   \\
14 - 17   & s                   & F4.1   & Right Ascension (1950)   \\
19 - 21   & $^{\circ}$          & I3     & Declination (1950)       \\
23 - 24   & $'$                 & I2     & Declination (1950)       \\
26 - 27   & $''$                & I2     & Declination (1950)       \\
29 - 32   &$10^{-8}$w/m$^{2}/sr$& I4     & 12$\mu$ intensity        \\
33 - 35   &$10^{-8}$w/m$^{2}/sr$& I3     & 12$\mu$ background       \\
37 - 40   &$10^{-8}$w/m$^{2}/sr$& A4     & 25$\mu$ intensity        \\
42 - 44   &$10^{-8}$w/m$^{2}/sr$& A3     & 25$\mu$ background       \\
46 - 49   &$10^{-8}$w/m$^{2}/sr$& A4     & 60$\mu$ intensity        \\
51 - 53   &$10^{-8}$w/m$^{2}/sr$& A3     & 60$\mu$ background       \\
55 - 58   &$10^{-8}$w/m$^{2}/sr$& A4     &100$\mu$ intensity        \\
60 - 62   &$10^{-8}$w/m$^{2}/sr$& A3     &100$\mu$ background       \\
63 - 67   & $'$                 & A5     & Size (see note)          \\
71 - 76   & Jy                  & A6     & $12\mu$ flux             \\
78 - 85   & Jy                  & A6     & $25\mu$ flux             \\
86 - 91   & Jy                  & A6     & $60\mu$ flux             \\
93 - 98   & Jy                  & A6     & $100\mu$ flux            \\
112-113   &                     & A10    & IRAS id                  \\
114-118   &                     & A5     & DPM field                \\
121-122   &                     & A1     & Spectral type            \\
\hline
\end{tabular}
\caption{File Format }
\end{center}
\label{T:form}
\end{table}
\begin{center}
\Large{SPECTRAL CODE}
\end {center}
\normalsize
\begin {definition} {5em}
\item [CODE]     MEANING
\item [C] Cool dust
\item [W] Warm dust
\item [S] Stellar spectrum
\end {definition}

\begin {center}
Notes to Table 2
\end{center}

If the right ascension is given in $0.\!\!^{s}$1, it and the error are from the
{\em IRAS PSC}; otherwise, they are taken from the maps with an error of
$12^{s}$.

If the declination is given in $1''$, it and the error are from the IRAS PSC;
otherwise they are taken from the DPM or Co-Add maps and have an error of $1'$.

If the source is present in the {\em IRAS Point Source Catalog} (PSC; Beichman
et al., 1989b), its PSC/SSS designation is given. A colon indicates that the
associated PSC or SSS entry is at a large distance from the source. An asterisk
indicates that the association has been made for more than one source in the
catalog. A plus sign indicates that another designation is given in the printed
catalog.

\vspace {6mm}

As mentioned above, the six tables in the printed volume (two of which have
three and five parts, respectively) have been concatenated into a single file.
The first byte in each file is an S or an L to indicate the cloud in which the
source is found. This is followed by one or more letters that indicate the type
of source. Since the arrangement of the data is such that a character code is
normally required to read it properly, no attempt was made to make the data
arrangement in the various parts of the table correspond. However, \ref{T:data}
lists the bytes in which each type of data is found for each type of source.

\begin{center}
\Large{SOURCE CODE}
\end {center}
\normalsize
\begin {definition} {5em}

\item[CODE] MEANING
\vspace  {2mm}
\item[A] Infrared emission from emission nebulae, Davies et al. (1976)
\item[D] Infrared emission from Hodge (1974) dark clouds
\item[S] Infrared emission from stars in the SAO catalog
\item[K] Infrared emission from star clusters, Kron (1956), Lindsay (1958)
\item[NGC] Infrared emission from NGC clusters
\item[Sk] Infrared emission from planetary nebulae, Sanduleak et al. (1978), Sanduleak and Pesch (1981)
\item[R] Infrared emission from Radcliffe stars, Feast et al. (1960)
\item[N] Infrared emission from supernovae remnants, Mathewson et al.
\end{definition}

\vspace {2mm}

\begin {table} [h]
\begin {center}
\begin{tabular}{ l c c c c c c }
SOURCE       &         &        &        &        &      &         \\
CODE         &  A      &   D    &    S   & K,R,N  & NGC  &  Sk     \\ \hline
Type         &  1-2    &  1-2   & 1-2    &  1-2   &  1-4 &  1-3    \\
Running No.  &  3-8    &  3-7   &        &        &      &         \\
Source No.   &  9-20   &        &  3-8   &  6-7   &  6-9 &  6-7    \\
LI No.       & 26-38   & 11-18  & 14-18  & 15-18  &      & 15-18   \\
Detection    &  43     &  26    &  28    &  28    &   28 &  28     \\
Intensity    & 21-24   &        &        &        &      &         \\
Remarks      & 50-97   & 34-97  & 36-97  & 36-97  & 36-97& 36-97   \\ \hline
\end{tabular}
\caption{Location of Data in File 2}
\end{center}
\label{T:data}
\end{table}
\vspace {2mm}

\section{Additional Information}
In addition to the concatenation described above, File 1 was modified in
several ways. The file was reformatted to eliminate a number of blank columns.
Plus signs were added to the IRAS identification to indicate an additional
source in the printed catalog. Colons were added to the spectral types in the
SMC where they appeared in the printed catalog.


\section{Acknowledgments}

We thank Dr. Schwering for forwarding to us a machine-readable
version of the catalog.

\section{References}
\begin{references}
\item van den Bergh, S. 1981, A\&AS, 46, 79.
\item Bruck, M.T., 1976, Occ. Rep. Roy. Obs. Edinburgh 1.
\item Davies, R. D., Elliott, K. H., Meaburn, J., 1976, MN 81, 89.
\item Feast, M. W., Thackeray, A. D., Wesselink, A. J., MN 121, 337.
\item Hodge, P. W., 1972, PASP, 84, 365.
\item Hodge, P. W., 1974, PASP, 86, 263.
\item Kron, G. E., 1956, PASP 68, 125.
\item Lindsay, E. M., 1958, MN 118, 172.
\item Mathewson, D. S., Ford, V. L., Dopita, M. A., Tuohy, I. R., Long, K. S.,
      Helfand, D. J., 1983, ApJS 51, 345.
\item Sanduleak, S. N., MacDonnell, D. J., Davis Philip, A. G., 1978, PASP 90,
      621.
\item Sanduleak, N., Pesch, P., 1981, PASP, 93, 431.
\item {\em Smithsonian Astrophysical Observatory Star Catalog}, 1966, Washington
      D.C., Smithsonian Institution (version 1984) USA.
\item Schwering, P.B.W. and Israel, F. P., 1990, Kluwer Academic Publishers,
      Dordrecht/Boston/London.
\end {references}

\end{document}
