\documentstyle [adc,11pt]{article}
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\newcommand{\dmv}{Documentation for the Computer-Readable Version}
\newcommand{\cat}{Lick Northern Proper Motion Program: NPM1 Reference Galaxies} 
\newcommand{\abbr}{NPM1}
\newcommand{\catref}{Klemola, et al. (1993)}
\newcommand{\pcatref}{Arnold R. Klemola, Robert B. Hanson, and Burton F. Jones}
\newcommand{\docnum}{NSSDC/WDC-A-R\&S 93-35}
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\begin{document}
%
\title{\cat}
\author{(\pcatref)}
\docauthor{Robert B. Hanson \linebreak{\it (UCO/Lick Observatory, University of 
California, Santa Cruz)}}
\docno{\docnum}
\date{}
\date{September 1993}
\maketitle

\begin{abstract} 

The Lick Northern Proper Motion (NPM) program measured proper motions,
positions, and photographic photometry for some 149,000 stars (NPM1 Catalog)
covering the sky outside the Milky Way north of declination $-23^\circ$. The
NPM1 proper motions were measured with respect to an absolute reference frame
defined by some 50,000 faint galaxies (mostly $16 < B < 18$).  The rms position
errors for the NPM1 reference galaxies average $\sim 0\secdot2$. The rms errors
for the $B$ magnitudes average $\sim 0.25$ mag. 

\end{abstract}

\section{Introduction and Source Reference}

{\bf A copy of this document should accompany any further distribution of this
file}. 

\subsection{Introduction} 

The Lick Northern Proper Motion (NPM) program is a mammoth photographic survey
of the northern sky, whose goal is to measure absolute proper motions on an
inertial system defined by some 50,000 faint galaxies for some 300,000 stars
over a blue apparent magnitude range from 8 to 18, covering the northern
two-thirds of the sky.  A full description of the NPM program is given by
Klemola, Jones, and Hanson (1987). 

The NPM survey is based on photographs taken with the Lick 51~cm (20~in)
Carnegie double astrograph.  There are 1,246 $6^\circ \times 6^\circ$ fields in
the NPM survey (from $+90^\circ$ to $-23^\circ$).  First-epoch photography began
in 1947; second-epoch photography was completed in 1988. Measurements and
reductions for proper motions, positions, and photometry in the sky outside the
Milky Way began in 1975 and were completed in 1992. 

The NPM program falls into two parts:  Part I covers the 72\% of the northern
sky lying outside the Milky Way.  Here, faint galaxies define the inertial
reference frame for absolute proper motions.  Part II covers the remaining 28\%
of the northern sky -- the Milky Way. 

Part I of the NPM program has now been completed (Klemola, Hanson, and Jones
1993).  The resulting catalog {\it (NPM1 Catalog)} contains some 149,000 stars
from measures in 899 of the 1,246 NPM fields.  The 50,000 NPM1 reference
galaxies comprise a separate list, for which positions and blue magnitudes are
given here. 

\subsection {Source Reference}

\begin{references}

\item ``Lick Northern Proper Motion Program. III:  The NPM1 Catalog'' 1993,
Klemola, A.R., Hanson, R.B., and Jones, B.F., AJ (in preparation). 

\end {references}

\section {Structure and Content of the NPM1 Reference Galaxy List}

\subsection{File Structure}

The {\em Lick NPM1 Reference Galaxy List} as distributed here is in a single
fixed block file.  It contains 50,517 records, each 46 bytes long. This list
concatenates 114 NPM1 zones, each covering $1^\circ$ of declination.  The zones
are ordered from North to South ($+89^\circ$ through $+00^\circ$, then
$-00^\circ$ through $-23^\circ$).  For identification, each galaxy is assigned a
running number within its zone, in right ascension order. Multiple measures from
overlapping fields have been averaged to give one entry (one record) per galaxy.

This information is sufficient for a user to describe the indigenous
characteristics of the machine-readable version of the Lick NPM1 Reference
Galaxy List to a computer. 

\subsection{Content} 

The NPM1 reference galaxies were selected at the Lick Gaertner survey machine
for the fundamental purpose of providing the absolute zero point of proper
motion in each NPM1 field (Klemola, Jones, and Hanson 1987).  The galaxies
selected for measurement lie in the magnitude range $14 < B < 18$, with most in
the fainter half of this range, i.e., $ 16 < B < 18$.  Ideally, a reference
galaxy should show little or no structure and have a small, generally round
shape with a well-exposed core.  In practice, to obtain an adequate number of
galaxies, most NPM fields rely on a wider range of galaxy types, including many
weak, patch-like objects.  Typically, from 50 up to a limit of 100 galaxies were
selected in each $6^\circ \times 6^\circ$ NPM1 field. Thus, the distribution on
the sky of the NPM1 reference galaxies is as nearly uniform as possible. 

The NPM1 galaxies were measured for astrometry and photometry in the same manner
as the NPM1 stars.  However, the galaxy data have two major differences from the
stellar data in the {\it NPM1 Catalog}.  First, the proper motions measured for
the galaxies simply reflect measurement errors, and contain no information about
the galaxies' actual motions, which are vanishingly small.  Hence, proper
motions are not given in the NPM1 Reference Galaxy List. Second, $B-V$ colors
for the NPM1 galaxies are not given, since the NPM1 faint star color reductions
(Klemola, Jones, and Hanson 1987) do not apply to galaxies. 

\begin{table} [htbp]
\begin{center}
\begin{tabular}{ c l l l }
\hline
      &          &       &                                              \\
Bytes & Item     &Format & Description                                  \\
\hline
      &          &       &                                              \\
 1- 8 &          &       & NPM1 galaxy ``name''                         \\
 1    &  zsign   & a1    & Sign of declination for this zone (+ or $-$) \\
 2- 3 &  npmzone & i2  & Declination zone (degrees)                     \\
 4- 8 &  znum    & f5.4  & Running number in this declination zone      \\
 9-21 &          &       & Right ascension (B1950 Epoch and Equinox)    \\
10-11 &  irah    & i2  & \phantom{xxxxx}Hours                           \\
13-14 &  iram    & i2  & \phantom{xxxxx}Minutes                         \\
16-17 &  iras    & i2  & \phantom{xxxxx}Seconds (integer part)          \\
18-21 &  rasec   & f4.3  & \phantom{xxxxx}Seconds (fractional part)     \\
22    &          & 1x    & Blank                                        \\
23-34 &          &       & Declination (B1950 Epoch and Equinox)        \\
23    &  dsign   & a1    & \phantom{xxxxx}Sign of declination for this galaxy (+
or $-$) \\ 
24-25 &  idd     & i2  & \phantom{xxxxx}Degrees                         \\ 
27-28 &  idm     & i2  & \phantom{xxxxx}Arc minutes                     \\
30-31 &  ids     & i2  & \phantom{xxxxx}Arc seconds (integer part)      \\
32-34 &  dsec    & f3.2  & \phantom{xxxxx}Arc seconds (fractional part) \\
35-40 &  bmag    & f6.2  & Photographic photometry ($B$ magnitude)      \\
41-42 &  nfields & i2    & Number of NPM fields on which                \\
      &          &       & \phantom{xxxxx}this galaxy was measured      \\
43    &          & 1x    & Blank                                        \\
44-46 &          &       & Discrepancy flags (see Table 2)              \\
44    &  ips     & i1    & \phantom{xxxxx}Position                      \\
45    &  ipm     & i1    & \phantom{xxxxx}Proper motion                 \\
46    &  ibv     & i1    & \phantom{xxxxx}Photometry                    \\
      &          &       &                                              \\
\hline
\end{tabular}
\caption{Data Format for NPM1 Galaxy List }
\end{center}
\label{T:form}
\end{table}

Each galaxy's entry begins with its NPM1 ``name,'' containing the NPM1
declination zone and the galaxy's running number within its zone (e.g.,
+89.0001).  Any galaxy in the list can then be specified by prefixing ``NPM1G''
to the ``name'' (e.g., NPM1G+89.0001). 

Positions are given for equinox B1950.  Each galaxy's entry includes the blue
magnitude $(\sim B )$, the number of NPM fields measured, and discrepancy flags
for position, proper motion, and photometry.  (Even though proper motions are
not listed here, the discrepancy flag has been retained as in the {\it NPM1
Catalog}, so that all cases with suspect astrometry are flagged.) 

The rms errors of the NPM1 galaxy positions average about $0\secdot2$ in each
coordinate for declinations from $0^\circ$ to $+70^\circ$. North of $+70^\circ$
and south of the Equator, the positional errors approach $0\secdot3$. The rms
errors for the NPM photographic photometry ($B$ magnitudes) average about 0.25
mag. 

\begin{table} [htbp]
\begin{center}
\begin{tabular}{ l l l l }
\hline
       &          &               &                \\
Flags  & Position & Proper Motion & Photometry     \\
\hline
       &          &               &                \\
  0    &    O.K.  &    O.K.       &O.K.            \\
       &          &               &                \\
  1    &    R.A.  &    R.A.       & $B$            \\
       &          &               &                \\
  2    &    Dec.  &    Dec.       & $B-V$          \\
       &          &               &                \\
  3    &    Both  &    Both       & Both           \\
       &          &               &                \\
  9    &    Error &    Error      & Error          \\
       &          &               &                \\
\hline
       &          &               &                \\
Limits & $1.0^{\prime\prime}$ & $3.0^{\prime\prime}~{\rm cent}^{-1}$ 
& 1.0 mag \\ 
       &          &               &                \\
\hline
\end{tabular}
\caption{NPM Discrepancy Flags (Galaxies)}
\end{center}
\label{T:form}
\end{table}

\subsection{File Format}

Table 1 gives a byte-by-byte description of the contents of the data file.

Table 2 gives a description of the discrepancy flags for proper motion,
position, and photometry.  (NOTE:  Error code [9] may appear in the NPM1
Reference Galaxy List as any serious errors are identified.  These objects will
be retained to preserve the numbering system.  However, their data should not be
used.) 

\section{Notes to the Catalog} 

As of September 1993 there are no Notes to the NPM1 Reference Galaxy List.
Detailed documentation and an updated description of the NPM reductions and
catalog preparation will be published separately (Klemola, Hanson, and Jones
1993). 

\section{Acknowledgments} 

We thank the National Science Foundation for its continued support of the Lick
NPM program.  Current work is supported by grant AST 92-18084. 

\section{References}
\begin{references}

\item Klemola, A. R., Jones, B. F., and Hanson, R. B. 1987, AJ 94, 501 

\item Klemola, A. R., Hanson, R. B., and Jones, B. F. 1993, AJ (in preparation) 

\end{references}

\end{document}
