% Documentation for An Atlas of Ultraviolet Spectra of
%   Starforming Galaxies  (Kinney, et al 1993).
%
% Document Number:
% Written: June 93 by N. A. Oliversen
% TeX Ver: June 93 by N. A. Oliversen
%
\documentstyle [adc,11pt]{article}
%
\newcommand{\cat}{An Atlas of Ultraviolet Spectra of Starforming
 Galaxies}
\newcommand{\abbr}{{\it AUVSSG}}
\newcommand{\prefp}{Kinney, Bohlin, Calzetti, Panagia, and Wyse (1993)}
\newcommand{\docnum}{ADC }
%
\begin{document}
%
\title{\cat}
\author{\prefp}
\docauthor{N. A. Oliversen}
\date{October 1993}
\docno{NSSDC/WDC-A-R\&S 93-28}
\maketitle
\date{}

\begin{abstract}

This atlas contains the ultraviolet spectra of the central regions of
143 spiral, irregular, blue compact, Seyfert 2, and starburst galaxies,
which were produced by combining 387 low resolution spectra from the
International Ultraviolet Explorer (IUE) data archive.  The spectra
have been extracted with an optimal algorithm and co-added to produce
spectra with the best possible signal-to-noise ratio.  The holdings
for this catalog include three files: One file contains the atlas
spectral data in ASCII format, and two files (ASCII and TEX format)
contain Table~1 from \prefp.  Table 1 lists summary information
about each galaxy including the figure number, galaxy name,
morphological type, activity class, recession velocity, apparent
magnitude, absolute magnitude, E(B-V), galactic longitude and
latitude, right ascension, declination and other names.
For each galaxy the atlas spectral data file contains the following
columns: wavelength, IUE quality flag (Epsilon), gross flux,
background flux, net flux divided by exposure time, absolute
calibrated net flux, exposure time, and sigma.
The atlas spectral data file consists of 177600 78-byte records and
the ASCII version of Table 1 consists of 143 146-byte records.
\end{abstract}

\section{Introduction}

{\bf A copy of this document should be distributed with every
copy of the machine-readable catalog.}

\subsection {Description}

This catalog contains the co-added spectra from  {\em \cat}
(\abbr).  Data for this atlas were obtained from the IUE archives and
include spectra from the short wavelength prime (SWP, camera 3), long
wavelength prime (LWP, camera 1), and long wavelength redundant (LWR,
camera 2) cameras.  Only large aperture (10 arcsec x 20 arcsec
rectangular slit) spectra were used.

An optimal extraction technique was used to extract the spectra from
the spatially resolved IUE data.  See Kinney et al. (1991a) for a
discussion of the optimal extraction technique and \abbr\ for a
discussion of the extraction and calibrations used in this atlas.  A
previous atlas of Kinney et al. 1991b was also generated using
similar techniques.  Note that the archival data for this catalog were
processed with the IUE Spectral Image Processing System (IUESIPS)
(Turnrose and Thompson 1984).

\subsection{Reference}
\begin{references}
\item Kinney, A. L., Bohlin, R. C., Calzetti, D., Panagia, N., and
Wyse, R. F. G. 1993, ApJS, 86, 5-93

\end {references}

\section {Structure}
\subsection{The Files as a Whole}

The holdings for {\em \cat} consist of three files.  Two versions of Table
1 from \abbr\ are available.  One version is in TEX format.
A second ASCII format version of Table 1 is contained in a single fixed-block
file of 143 146-byte records.  The atlas spectral data are contained in a
single fixed-block file of 177600 78-byte records.   Detailed
descriptions of some of the fields in the files are given in the
following sections.

\subsection{Atlas Galaxies (Table 1)}

The file format information given in this section refers to
the ASCII file version of Table 1.

\begin{table}[h]
\centering
\begin{tabular}{ c c c l }
\hline\hline
         &         &Suggested &                \\
Bytes    & Units   &  Format  & \multicolumn{1}{c}{Item}     \\
\hline
 1- 7    &         & A7     & Figure number or activity class reference     \\
 9-10    &        & I2    & Number of SWP spectra  \\
 13-14    &        & I2  & Number of LWP or LWR spectra  \\
19-29    &        & A11    & Galaxy name \\
33-45    &      & A13    & Morphological type \\
47-57    &      & A11    & Activity class \\
59-63    & km ~sec$^{-1}$  & I5  & $v_{H}$\\
64      &        & A1  &  Note 1 \\
68-72   &        & F5.2 & $B_{T}$ \\
73      &        & A1   & Note 2 \\
74      &        & A1   & Note 3    \\
77-82   &  mag   & F6.2 & $M_{B}$ \\
83      &        & A1   & Note 4  \\
84      &        & A1   & Note 5  \\
86-89   &  mag   & F4.2 & E(B-V) \\
94-98   &  deg   & F5.1 & Galactic longitude \\
100-104 &  deg   & F5.1 & Galactic latitude \\
107-108 &  hr    & I2   & Right ascension (1950) \\
110-111 &  min   & I2   & Right ascension (1950) \\
113-116 &  sec   & F4.1 & Right ascension (1950) \\
119-121 &  deg   & I3   & Declination (1950) \\
123-124 &  $'$     & I2   & Declination (1950)  \\
126-127 &  $''$    & I2   & Declination (1950)  \\
130-145 &        & A16  & Other names   \\
\hline\hline
\end{tabular}
\caption{Atlas Galaxies}
\end{table}

{\bf Notes to Table 1}

The names, cross-identifications, coordinates, and some of the
morphological types are taken first from RSA or from the literature,
and otherwise come from the NASA Extragalactic Database (NED). The
morphological type follows, where possible, the classical Hubble
classification. Specific symbols are Am. = amorphous, Comp. = compact,
Cl. Irr. = clumpy irregular, 2-nuc. = presence of two nuclei. The
reddening E(B-V) from our Galaxy is from Burstein, D. and  Heiles, C.
1984, ApJ Supp., 54, 33. The activity classification is as follows:
BCG and BCDG are, respectively, blue compact galaxies and blue compact
dwarf galaxies (where a blue compact galaxy is considered to be a
dwarf if it has $M_{B}$ fainter than -20); Sy2 are Seyfert 2
galaxies; SB nuc. are galaxies experiencing a starburst in their
nuclei; Hs are hotspot galaxies; Lin are LINERs; HII are galaxies with
spectra typical of an HII region.

The criterion for defining the class is not based on physical
considerations but comes from the literature, where the most widely
accepted classification has been used for each galaxy. The first
column gives the figure number for galaxies treated individually in
this paper. If no figure is given, a reference for the activity
classification is given as listed below:

(r1) Thuan, T. X. and Martin, G. E. 1981, ApJ, 247, 823, (BCDG).
(r2) Gordon, D. and Gottesman, S. T. 1981, AJ, 86, 161, (BCG).
(r3) Mazzarella, J. M. and Balzano, V. A. 1986, ApJ Suppl., 62, 751, (Mrk).
(r4) Kollatschny, W. and Fricke, K. J. 1986, IAU Symp. no. 121, p. 377.
(r5) Phillips, M. M., Charles, P. A., and Baldwin, J. A. 1983, ApJ, 266, 485.
(r6) Lamb, S. A., Gallagher III, J. S., Hjellming, M. S., and Hunter, D. A.
1985,  ApJ, 291, 63.
(r7) Zamorano, J. and Rego, M. 1986, A\&A, 170, 31.
(r8) Joseph, R. D., Meikle, W. P. S., Robertson, N. A., and Wright, G. S. 1984, 
MNRAS, 209, 111.
(r9) Keel, W. C. 1983, ApJ Suppl., 52, 229.
(r10) De Robertis, M. M. and Osterbrock, D. E. 1986, ApJ, 301, 727.
(r11) Huchra, J. P., Wyatt, W. F., and Davis, M. 1982, AJ, 87, 1628.
(r12) Heckman, T. M., Van Breugel, W., Miley, G. K., and Butcher, H. R. 1983,
AJ, 88, 1077.
(r13) Moorwood, A. F. M. and Oliva, E. 1988, A\&A, 203, 278.
(r14) Heckman, T. M. 1980, A\&A, 87, 152.
(r15) Osterbrock, D. E. and Cohen, R. D. 1982, ApJ, 261, 64.
(r16) Veron-Cetty, M.-P. and Veron, P. 1986, A\&A Suppl., 65, 241.
(r17) Lamb, S. A., Bushouse, H. A., and Towns, J. W. 1989, BAAS, 21, 1163.
(r18) Keel, W. C., Kennicut, R. C. Jr., Hummel, E., and Van der Hulst 1985,
AJ, 90, 708.
(r19) Netzer, H., Kollatschny, W., and Fricke, K. J. 1987, A\&A, 171, 41.

The recession velocity ($v_{H}$) and the apparent magnitude ($B_{T}$)
are from {\it The Revised Shapley-Ames Catalogue} when no marks are shown;
$v_{H}$ is the heliocentric velocity; $B_{T}$ is the apparent
magnitude in the $B_{T}$ system of the RC2 ({\it Second Reference Catalogue
of Bright Galaxies}); $M_{B}$ is the absolute magnitude calculated from
an apparent magnitude corrected for galactic and internal absorption
and from a recession velocity reduced to the centroid  of the Local
Group (cfr. RSA).

{\bf Note 1, Note 3, and/or Note 4:}  An asterisk following a value of
$v_{H}$, $B_{T}$, or $M_{B}$ means the following: $v_{H}$ and $B_{T}$
correspond to the heliocentric velocity and to the uncorrected
apparent magnitude from {\it The Third Reference Catalogue of Bright
Galaxies} (RC3); $v_{H}$  is the $V_{21}$ or the $V_{opt}$ when the
first is not available (the difference between the two is in general
small). The absolute magnitude $M_{B}$ is obtained from RC3 using the
velocity reduced with respect to the Galactic Standard of Rest,
$v_{GSR}$, the apparent magnitude corrected for galactic and internal
absorption, $B^{o}_{T}$, and assuming $H_{0} = 50$ km/s/Mpc. For
recession velocities between 500 and 3000 km/s $M_{B}$ has been
calculated with the usual formula after checking that it is not near a
cluster. For v $>$ 3000 km/s the formula has been applied without
problem. Redshift corrections were applied for v $>$ 10,000 km/s. For
galaxies belonging to a cluster $M_{B}$ has been obtained from
$B^{o}_{T}$ (RC3) and with the assumed distance being the distance of the
cluster.

{\bf Note 2 and/or Note 5:} Other notation is as follows:
p--When $B_{T}$ is not
available from RC3, the photographic magnitude has been reported;
o--This marks galaxies with redshift in the range 500-3000 km/s, but not
belonging to a cluster; m--This marks the distances calculated through
the distance modulus;  a--$B_{T}$ or corrections to derive $B^{o}_{T}$
have been taken from r1;  b--$B^{o}_{T}$ have been taken from r2;
c--Galaxies for
which $B_{T}$ or $v_{H}$  or both have been taken from NED
since they are not reported in RSA or in RC3;
the same values have been used to calculate an approximate value for
$M_{B}$. The symbol indicates also an approximate $M_{B}$ for galaxies
with both $v_{H}$ and $B_{T}$ from RC3 but without the extinction
corrected $B^{o}_{T}$.

\subsection{Spectral Atlas File}

The information for each galaxy consists of a header plus the co-added
spectra and is separated from the next object by a blank line (record)
of 78 bytes.  Each co-added spectrum is preceeded by a header
containing the object number, object name, IUE camera(s), and image
number(s) that were used to form the co-added spectrum.  A sample
header is given below.  The first line contains the target number and
the object name.  The next line gives the total number of
individual spectra that were used to form the co-added spectrum from
the SWP (camera 3) camera.  The next four lines give the individual
image number(s) of the spectra, used to form the co-added SWP
spectrum. Note that the S-AP nomenclature indicates the spectra are
normalized in flux to the L-AP set of spectra and does {\it NOT} mean
that the spectra were obtained in the small aperture.   A second group
of five lines may also be given in the header for the long wavelength
camera (either the LWP [camera 1] or LWR [camera 2]).  The first byte
in each line (record) in the header is blank.  In the example below
only one large aperture SWP and one large aperture LWP image were used
to form the spectrum of 1050+04.

\clearpage

{\tt~~~\\
~~\#\#\#~~~~1~~1050+04     \\
~~SUM OF~~1 L-AP \&~~0 S-AP IMAGES~~~~CAMERA 3      \\
~~L-AP:~~~~18807                                   \\
~~L-AP:                                            \\
~~S-AP:                                             \\
~~S-AP:                                             \\
~~SUM OF~~1 L-AP \&~~0 S-AP IMAGES~~~~CAMERA 1       \\
~~L-AP:     1769                                    \\
~~L-AP:                                             \\
~~S-AP:                                             \\
~~S-AP:                                              \\
~~~LAM~~~~~EPS~~~~GROSS~~~~~BKG~~~~~NET/TIME~~~ABNET~~~~TIME(sec)~~~SIGMA \\}

The header is immediately followed by the co-added spectral data.  Each
co-added spectrum consists of eight columns of ASCII numbers with the column
headings as described in Table 1.

\begin{table}[h]
\centering
\begin{tabular}{ c c c l }
\hline\hline
         &         &Suggested &                \\
Bytes    & Units   &  Format  & \multicolumn{1}{c}{Item}     \\
\hline
 2- 7    & \AA       & F6.1    & Wavelength     \\
 9- 14    &        & F6.0    & Epsilon \\
 16-23    & FN       & F8.0  & Gross flux  \\
25-32    & FN       & F8.0    & Background flux \\
36-42    & $FN~sec^{-1}$   & F7.2    & Net flux/time \\
44-53    & $erg~cm^{-2} sec^{-1} \AA^{-1}$   & E10.3    & ABNET \\
55-63    & sec     & F9.2  & Exposure time\\
67-73    &        & F7.4  & Sigma \\
\hline\hline
\end{tabular}
\caption{Catalog Record Format}
\end{table}

{\bf Notes to Table 2}

\begin{definition}{20ex}

\item[Epsilon] IUE data quality flag.   See Kinney at al. (1991a) for
discussion of how the epsilon values were determined for the optimal
extraction algorithm.

\item[Gross flux]  The gross flux is given in IUE Flux Number (FN)
units.

\item[Background flux] The background flux is given in IUE Flux Number
(FN) units.

\item[Net flux/time] The net flux (gross-background)/time.

\item[ABNET] Absolutely calibrated net flux.

\item [Sigma]  Sigma represents the error in the mean as estimated
from the IUE noise models constructed by the authors.  Sigma is
given in percent (i.e., 2.1 = 210\%).

\end{definition}

\clearpage
\section{History}

\subsection{Remarks and Modification}

{\em \cat } was received by the Astronomical Data Center (ADC), NASA
Goddard Space Flight Center, from Dr. Anne Kinney, Space Telescope
Science Institute, Baltimore, Maryland.

The spectral data for each of the objects were originally contained in 143
separate files.  These files were first concatenated into a single
file by the data center.  The headers for each of the objects were
then edited to remove information that was relevant only to the original
tape versions of the data (i.e., record and file numbers) and not
relevant to the ADC on-line version.  Some redundant information
was also removed from the headers to make them more readable.
The position of fields 6, 7 and 8 (absolute net flux,
exposure time, and sigma) varied by 1 byte from object-to-object
in the original data files.  The information in these three fields
were shifted by 1 byte to the right so that all entries were aligned
vertically.  The affected object numbers were 1, 4, 5, 11-13, 17, 21,
29-30, 32-36, 39-40, 42-44, 48-49, 51-56, 58-59, 61-64, 68-79, 81-86,
88-92, 94-108, 110-114, 116-117, 120-132, 134-135, 140-142.
The epsilon and net flux/time fields were edited
to align the sign bytes into the same column for each respective field.

Table 1 was received from Dr. Anne Kinney in TEX format and was
converted to ASCII format by the data center using "dvi2tty" and by
realigning the various columns.  Documentation within the TEX version
of Table 1 (i.e., Notes to Table 1) is included in this ADC
document.  The galactic longitude of NGC3125 was changed from 365.3
(as it was in the original paper) to 265.3 in the ASCII and TEX
versions of Table 1 by the ADC.

\section{Reference to the Documentation}
\begin{references}
\item {Kinney, A.L., Bohlin, R.C., Blades, J.C., and York, D.G.
1991a, ApJS, 75, 645}
\item {Kinney, A.L., Bohlin, R.C., and Neill, J. D. 1991b, PASP, 103,
665}
\item {Kinney, A.L., Bohlin, R.C., Calzetti, D., Panagia, N., and
Wyse, R.F.G. 1993, ApJS, 86, 5-93}
\item {Turnrose, B. E. and Thompson, R. W. 1984, International
Ultraviolet Explorer Image Processing Information Manual, Version
2.0}
\end{references}
\end{document}
