The Large Scale Distribution of Galaxies in the Shapley Supercluster
Michael J. Drinkwater$^{1}$
Quentin A. Parker$^{2}$
Dominique Proust$^{3}$
Eric Slezak$^{4}$
Hern\'an Quintana$^{5}$
We present new results of our wide-field redshift survey of galaxies in a 182 square degree region of the Shapley Supercluster (SSC) based on observations with the FLAIR-II spectrograph on the UK Schmidt Telescope (UKST). In this paper we present new measurements to give a total sample of redshifts for 710 bright ($R\leq 16.6 $) galaxies, of which 464 are members of the SSC ($8000<v<18000\kms $). Our data reveal that the main plane of the SSC ($v\approx 14500\kms $) extends further than previously realised, filling the whole extent of our survey region of 10 degrees by 20 degrees on the sky (35 Mpc by 70 Mpc, $H_0=75\kmsMpc$). There is also a significant structure associated with the slightly nearer Abell 3571 cluster complex ($v\approx12000\kms$) with a caustic structure evident out to a radius of 6 Mpc. These galaxies seem to link two previously identified sheets of galaxies and establish a connection with a third one at $\overline V$= 15000\kms near $R.A.= 13h$. They also tend to fill the gap of galaxies between the foreground Hydra-Centaurus region and the more distant SSC. We calculate galaxy overdensities of $5.0\pm0.1$ over the 182 square degree region surveyed and $3.3\pm0.1$ in a 159 square degree region excluding rich clusters. Over the large region of our survey the inter-cluster galaxies make up 46 per cent of all galaxies in the SSC region and may contribute a similar amount of mass to the cluster galaxies.
shapley3.tex
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\begin{document}
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% Title
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\title{The Large Scale Distribution of Galaxies in the Shapley Supercluster}
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% Authors
\author{Michael J. Drinkwater$^{1}$, 
 Quentin A. Parker$^{2}$, 
 Dominique Proust$^{3}$,\and
 Eric Slezak$^{4}$,  Hern\'an Quintana$^{5}$
} % IMPORTANT: leave this curly bracket as the first character of this line.

% Date - leave this blank.
\date{Submitted to PASA 2003 Sep 18}
\maketitle

% Institutions
{\center
$^1$ Department of Physics, University of Queensland, QLD 4072, Australia,
\\mjd@physics.uq.edu.au\\[3mm]
$^2$ Department of Physics, Macquarie University, NSW 2109, Australia,
and Anglo-Australian Observatory, PO Box 296, Epping NSW 1710,  Australia,
\\qap@ics.mq.edu.au\\[3mm]
$^3$ Observatoire de Paris-Meudon, F92195 Meudon CEDEX, France
\\Dominique.Proust@obspm.fr\\[3mm]
$^4$ Observatoire de Nice, 06304 Nice CEDEX4, France, 
Slezak@obs-nice.fr\\[3mm]
$^5$ Departamento de Astronomia y Astrofisica, Pontificia Universidad
Cat\'olica de Chile, Casilla 104, Santiago 22, Chile,
hquintan@astro.puc.cl\\
}

% Abstract
\begin{abstract}
We present new results of our wide-field redshift survey of galaxies
in a 182 square degree region of the Shapley Supercluster (SSC) based
on observations with the FLAIR-II spectrograph on the UK Schmidt
Telescope (UKST). In this paper we present new measurements to give a
total sample of redshifts for 710 bright ($R\leq 16.6 $) galaxies, of
which 464 are members of the SSC ($8000<v<18000\kms $). Our data
reveal that the main plane of the SSC ($v\approx 14500\kms $) extends
further than previously realised, filling the whole extent of our
survey region of 10 degrees by 20 degrees on the sky (35 Mpc by 70
Mpc, $H_0=75\kmsMpc$). There is also a significant structure
associated with the slightly nearer Abell 3571 cluster complex
($v\approx12000\kms$) with a caustic structure evident out to a radius
of 6 Mpc.  These galaxies seem to link two previously identified
sheets of galaxies and establish a connection with a third one at
$\overline V$= 15000\kms near $R.A.= 13h$. They also tend to fill the
gap of galaxies between the foreground Hydra-Centaurus region and the
more distant SSC. We calculate galaxy overdensities of $5.0\pm0.1$
over the 182 square degree region surveyed and $3.3\pm0.1$ in a 159
square degree region excluding rich clusters. Over the large region of
our survey the inter-cluster galaxies make up 46 per cent of all
galaxies in the SSC region and may contribute a similar amount of mass
to the cluster galaxies.
\end{abstract}

{\bf Keywords: Redshifts of galaxies - clusters of galaxies - subclustering}
% Place keywords here. Please write all keywords in lower case. PASA uses the
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% Body of paper
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\newpage
\section{Introduction}

In the past few decades, large galaxy redshift surveys have revealed
structures on ever-increasing scales. The largest structures found are
superclusters, collections of thousands of galaxies with sizes as
large as 100 Mpc. The mere existence of these structures places
important constraints on theories of the formation of galaxies and
clusters. The Shapley supercluster, the subject of this paper,
is one of the most massive concentrations of galaxies in the local
universe (Scaramella et al.\ 1989; Raychaudhury 1989), so it is also
of particular interest to consider its effect on the dynamics of the
Local Group.

The Shapley supercluster (SSC) is a remarkably rich concentration of
galaxies centred around R.A.$=13^h25^m$ Dec. $= -30^{\circ}$ which has
been investigated by numerous authors since its discovery in 1930 (see
Quintana et al. 1995). It consists of many clusters and groups of
galaxies in the redshift range $0.04<z<0.055$. The SSC lies in the
general direction of the dipole anisotropy of the Cosmic Microwave
Background (CMB), (Smoot et al. 1992), and is located 130\hMpc\ beyond
the Hydra-Centaurus supercluster (itself $\simeq 50$\hMpc\ away from
us).  Quintana et al.\ (1995) estimated that for $\Omega_{o}= 0.3$ and
$H_{o}$= 75\kmsMpc the gravitational pull of the supercluster may
account for up to 25\% of the peculiar velocity of the Local Group
required to explain the CMB dipole anisotropy in which case the mass
of the supercluster would be dominated by inter-cluster dark matter.
A major study of the SSC was made by Bardelli et al.\ (2000, 2001 and
references therein) who also studied inter-cluster galaxies in the
core region of the supercluster. They derived a total mean overdensity
of the SSC of $N/\overline N \sim 11.3$ on a scale of $10.1h^{-1}$ Mpc
and found that the central part of the supercluster contributes about
26\kms\ to the peculiar velocity of the Local Group.

%The central cluster A3558 has also been measured with
%a ROSAT PSPC observation by Bardelli et al. (1996) who derive a total
%mass of $M_{tot}=3.1\times10^{14}\mo$ within an Abell radius of
%2\hMpc. Several other x-ray clusters form part of the Shapley
%supercluster (Pierre et al.\ 1994).

The early studies of the Shapley supercluster were limited
(primarily by observational constraints) to the various rich Abell
galaxy clusters in the region, but this might give a very biased view
of the overall supercluster as they represent only the most
concentrated peaks in the luminous matter distribution. We have
commenced an investigation into the larger scale distributions of
galaxies throughout the entire SSC region and close environs using
data from wide-field multi-fibre spectrographs such as the FLAIR-II
system on the U.K. Schmidt Telescope (UKST) of the Anglo-Australian
Observatory (Parker \& Watson, 1995, Parker 1997). With such
multiplexed facilities we are able to measure many more galaxy
redshifts over large angular extents and obtain a more complete
picture of the composition and disposition of galaxies in the entire
supercluster. 

A preliminary analysis based on 301 new, bright ($R\leq 16$) galaxy
redshifts obtained with FLAIR-II in a 77~deg$^{2}$ region of the
supercluster has already been published by our group (Drinkwater et
al.\ 1999, hereafter D99). The measured galaxies were uniformly
distributed over the selected inter-cluster regions, and most ($230
\equiv 75\%$) were found to be members of the supercluster. The D99
sample traced out two previously unknown sheets of galaxies which
appeared to link various Abell clusters in the supercluster. We also
found that in a 44 deg$^{2}$ sub-area of the supercluster {\em
excluding} the Abell clusters, these sheets alone represent an
overdensity of a factor of $2.0\pm0.2$ compared to a uniform galaxy
distribution.  Within the initial survey area of D99 the new galaxies
contribute an additional 50\% to the known contents of the Shapley
supercluster in that region, implying a corresponding increase in
contribution to the motion of the Local Group. A much larger galaxy
sample over a similar area of sky was presented by Quintana et al.\
(2000). They measured nearly 3000 galaxy redshifts in an area of about
$12\deg \times 6\deg$. They estimated the upper bound on the mass of
the central region and found the overdensity to be substantial, but
still only able to contribute to a small fraction
($3\Omega_m^{-0.4}$\%) of the observed motion of the Local Group
(Reisenegger et al.\ 2000).

In this paper we present radial velocities for an additional 409
bright ($R\leq16.5$) galaxies spread over an extended region to the
East, West and South of the main SSC concentration. We analyse a
combined magnitude-limited sample from this paper and D99 of 710
galaxies with measured redshifts, of which 464 (65 per cent) are
members of the supercluster based on their redshift range ($8,000 <
cz < 18,000\kms$). They seem to link the two previously identified
galaxy sheets found in D99 and also establish a connection with a
third feature at $\overline V$= 15000\kms near R.A.=~13h. The new
sample also tends to fill a previous gap in the galaxy distribution
between the foreground Hydra-Centaurus region and the SSC. Future
study of the SSC will cover even larger regions using data from the
FLASH survey of Kaldare et al.\ (2003) (also with the UKST/FLAIR-II
system) and the 6dF survey of the southern sky currently in progress
(Watson et al.\ 2000).

The observed galaxy sample and observations are described in
Section~2, the results are presented in Section~3 and a brief
discussion of the significance of these new measurements is given in
Section~4.  A full and detailed analysis and interpretation of the new
redshifts from D99, this work and a compilation of all literature
redshifts in the SSC is the subject of a separate paper (Proust et
al., in preparation). Unless otherwise noted in this paper we use a
Hubble constant of $H_0=75\kmsMpc$ giving a distance of 200 Mpc to the
main supercluster ($cz=15,000\kms$) so 1 degree subtends a distance of
3.5 Mpc.

\section{Observations and Data Reductions}

In 1997 we began a concerted campaign to obtain complete samples of
galaxies down to the same magnitude below $L_*$ for constituent
clusters and inter-cluster regions of the SSC using the FLAIR-II
system at the UKST. During the period 1997-2000 we subsequently
observed more than 700 selected galaxies over 7 UKST standard fields
in the SSC region, namely in fields 382--384 and 443--446. The main
SSC core centred on A3558 at $13^h~25^m$, $-$31$^{\circ}$ is in field
444.  As each selected Abell cluster has a projected angular diameter
of 2.5 to 3.0 degrees, the wide-field UKST FLAIR-II system was an
ideal facility for this project whilst additionally permitting us to
probe the regions between the dominant clusters neglected in previous
studies. These combined fields covered an area of  182~deg$^2$
which allows us to investigate the outer limits of the SSC out to
radii of more than 10~deg (35\Mpc) from A3558.

\subsection{Input Galaxy Samples}

All target galaxies were originally obtained from the red ESO/SRC sky
survey plates of the above fields scanned by the Paris Observatory
MAMA plate-measuring machine (Guibert \& Moreau 1991; Moreau
1992). The images were classified using standard star/galaxy
separation techniques (e.g. Dickey et al. 1987, Heydon-Dumbleton et
al. 1989).  We defined a galaxy sample to a photometric limit of
$R\leq16$, corresponding (assuming a mean $B-R=1.5$) to $B<17.5$, the
nominal galaxy limiting magnitude of the FLAIR-II system (Parker \&
Watson 1995). This corresponds to an absolute magnitude of $M_B=-19$
at the Shapley distance of 200\Mpc.  This selection gave total galaxy
samples of 600--1000 per field.  All previously catalogued matches to
literature redshifts were then removed from the target samples prior
to observation.



\subsection{FLAIR-II observations}

Table~1 gives the journal of FLAIR-II observations reported here. An
interim magnetic-button fibre-ferrule system, implemented with the
71-fibre FLAIR-II plateholder, was commissioned during these
observations. This was as a proof of concept for the
recently-commissioned automated robotic fibre positioner that will
replace FLAIR-II at the UKST and known as 6dF - for 6-degree field
(e.g. Watson et al. 2000).  Note that typically 6~fibres were devoted
to the blank sky regions to facilitate sky-background subtraction. An
overall redshift success rate of 75\% was achieved from the FLAIR-II
data.

\begin{table}
\caption{Summary of FLAIR-II observations}
\label{tab_obs}
\vspace{0.2cm}
\begin{tabular}{lrrrrrrr}
\hline
Date    & Field  &  RA (J2000) Dec & time & seeing  & weather & N$_g$ & N$_r$ \\
\hline
1998 May  22 &F383B & 13:15:00 -35:15:00 &5400  & 1   &clear &58 & 43\\%+11*
1999 June 10 &F445A & 13:51:00 -30:15:00 &11000 & 2-3 &clear &65 & 53\\%+ 5*
1999 June 11 &F445B & 13:51:00 -30:15:00 &12000 & 3-4 &cloudy&65 & 54\\%+ 3*
1999 June 12 &F445C & 13:51:00 -30:15:00 &12000 & 3   &clear &65 & 52\\%+ 5*
1999 June 13 &F445D & 13:51:00 -30:15:00 &12000 & 2-3 &clear &65 & 41\\%+ 3*
1999 June 14 &F443A & 13:05:00 -30:15:00 &12000 & 1-2 &clear &73 & 21\\%+ 9*
1999 June 16 &F443B & 13:05:00 -30:16:00 &12000 & 1-2 &clear &73 & 32\\%+12*
1999 June 17 &F443C & 13:05:00 -30:16:00 &12000 & 2+  &cloudy&65 & 42\\%+13*
2000 June  2 &F446  & 14:14:00 -30:14:00 &15000 & 2-3 &clear &61 & 28\\%+ 1*
2000 June  3 &F384  & 14:03:00 -30:14:00 &15000 & 1-2 &clear &80 & 64\\%+4* 
\hline
\end{tabular}
\vspace{0.2cm}

{\small Notes: N$_g$ is the number of target galaxies observed while
N$_r$ is the number of galaxies actually yielding a redshift in a
particular field configuration, not counting the spectra dominated by
Galactic stars.
%The number of stellar dominant spectra is also quoted for each
%field. 
%All observations except those for %fields F443A, F443B amd F384 were
%made with the interim 71 fibre %magnetic button plateholder 14/6.
}
\end{table}

The data were reduced as in Drinkwater et al.\ (1996) using the
dofibers package in IRAF (Tody 1993). Redshifts were measured for
galaxy spectra using the cross-correlation task XCSAO in RVSAO (Kurtz
\& Mink 1998) using a mixture of a dozen stellar and galaxy
templates. The galaxy templates included a number of emission line
examples.  The IRAF EMSAO utility was also used to manually check
emission line redshifts where necessary.  For spectra showing both
absorption and emission features the result (either XCSAO/EMSAO) with
the lower error was used. Note that 61 spectra were contaminated by a
dominant foreground star although we tried to remove all galaxies with
a dominant star on the line-of-sight during the fibering procedure. No
redshift was measured for these galaxies.

The complete set of FLAIR-II measurements from both papers was
carefully checked for consistency, in particular by matching the
galaxy positions to the new SuperCOSMOS catalogue (Hambly et al.\
2001a, 2001b, 2001c). During this process several errors in the data
from D99 were identified: 5 galaxies had incorrect redshifts reported
and 12 had incorrect positions, all but two of which we have been able
to correct. The 17 galaxies from D99 with incorrect measurements are
listed in Table~\ref{tab-errata}.

\begin{table}
\caption{Galaxies with incorrect measurements in D99}
% checked: all in current N=710 flairdata
\label{tab-errata}
%\vspace{0.2cm}
\begin{center}
\begin{tabular}{ccrl}
\hline
Original Position$^1$ &New Position$^2$  & $cz {\pm {\Delta}cz}$ &
 Correction \\
RA (B1950) Dec &RA (J2000) Dec& (\kms)\\
\hline
 13:04:08.4 -37:06:37 & 13:06:56.1 -37:22:09 &-- & position  \\
 13:12:05.7 -33:29:36 & 13:14:52.8 -32:45:27 &-- & position  \\
 13:14:37.9 -33:39:08 & 13:17:26.2 -33:55:36 &-- & position  \\
 13:15:21.3 -31:45:59 & 13:18:08.7 -32:01:06 &-- & position  \\
 13:18:06.6 -27:47:20 & 13:20:52.8 -28:13:06 &-- & position  \\
 13:19:39.1 -33:06:29 & 13:22:28.0 -33:29:03 &-- & position  \\
 13:24:21.4 -37:00:34 & 13:27:13.1 -36:25:34 &-- & position  \\
 13:24:28.2 -36:49:27 & 13:27:10.4 -37:05:00 &-- & position  \\
 13:29:40.1 -33:54:18 & 13:32:31.3 -33:09:42 &-- & position  \\
 13:31:39.7 -36:33:12 & 13:34:33.1 -36:48:32 &   2398  17& velocity \\
 13:33:21.5 -36:38:27 & 13:36:15.3 -36:53:45 &   3897  79& velocity \\
 13:35:47.0 -34:17:07 & -- &-- & removed$^3$   \\
 13:37:15.1 -34:05:41 & 13:30:06.0 -34:21:10 &-- & position  \\
 13:40:52.6 -34:49:27 & 13:43:46.5 -35:04:30 &  14681  71& velocity \\
 13:42:33.6 -36:31:58 & 13:45:29.1 -36:46:59 &   7633  80& velocity \\
 13:43:08.2 -33:29:39 & 13:46:01.4 -33:44:39 &  24838  61& velocity \\
 13:43:32.6 -35:50:50 & -- &-- & removed$^3$   \\

\hline
\end{tabular}
\vspace{0.2cm}

{\small Notes. 1) the position given in D99; 2) the J2000
  position in this paper, corrected in some cases; 3) in two cases the
  original position was wrong, but the correct identification could not
  be determined.}
\end{center}
\end{table}


Table~\ref{tab-cat} lists our complete catalogue of 710 galaxies
measured in the work reported here and our previous FLAIR-II
observations from D99. The column descriptors are given at the
end of the table. In Fig.~\ref{fig-sky} we show the projected
distribution of the observed galaxies on the sky.  We also show
galaxies with previously published redshifts and the known Abell
clusters.

\begin{figure*}
\psfig{figure=fig_sky1.eps,width=15cm}
\caption[]{Sky distribution of galaxies with measured redshifts in the
  Shapley Region. The galaxies observed with FLAIR-II for this work
  are plotted as crosses and those previously published as dots. Known
  galaxy clusters with redshifts overlapping the Shapley range
  ($7500<cz<18500$\kms) are indicated by large labeled circles, and
  the 5 UKST fields by large overlapping squares. Note the
  concentration of previous measurements in the clusters.}
\label{fig-sky}
\end{figure*}

%\input shapley3_data

\subsection{Observed Galaxy Sample and Completeness}

For the purpose of our analysis below we wished to compare our sample
of observed galaxies to the total magnitude-limited galaxy
distribution in our survey region. We chose to use the new SuperCOSMOS
sky surveys (Hambly et al.\ 2001a,b,c) to construct the parent galaxy
catalogue for the region. This choice was motivated by the
availabililty of full image data online from the SuperCOSMOS survey as
well as some evidence that the MAMA photometry values used for the
final two fields (384 and 446) was different from the others. We
therefore quote and analyse the SuperCOSMOS R (the ``$R_1$'' value
from the U.K.\ Schmidt Telescope survey plates) magnitudes of all
galaxies in this paper. In this system the sample does not have a
sharp magnitude limit, as shown in Fig.~\ref{fig-mag1}. We compared
the magnitude distributions of the objects measured in the seven
fields: two-sample K-S tests showed that they were all consistent with
the same distribution (mean $R \approx 15.8$) except for the two final
fields---384 and 446---which were significantly fainter (mean
$R\approx 16.4$).

% Comparison of mag dists between fields compared to-
% field N    mean        sem        rms      erms  KS445 KS383
% 
% 445 197  15.720     0.037     0.514     0.026  --      0.09229
% 382 123  15.895     0.041     0.457     0.029  0.01091 0.29596
% 383 165  15.836     0.039     0.500     0.028  0.09229 --
% 384  60  16.252     0.065     0.506     0.047  0.00000 0.00000
% 443  93  15.721     0.054     0.517     0.038  0.99510 0.21389
% 446  26  16.480     0.107     0.545     0.077  0.00000 0.00000

We next used the SuperCOSMOS survey to define a parent galaxy sample
over the whole region covered by our seven fields observed. Allowing
for the boundaries of the survey fields and a circular region 1 degree
in diameter we excluded around the bright star HD 123139 (at 14 06
41.0 -36 22 12, J2000), the total survey region has an area of 182
square degrees.  As in D99 we also defined a restricted
inter-cluster region by excluding regions 1 degree in diameter around
any rich galaxy clusters in the Shapley velocity range, having an area
of 159 square degrees. The excised cluster regions are shown in
Fig.~\ref{fig-sky}.

We used the parent galaxy sample to determine the completeness of our
survey as a function of limiting magnitude. This is shown in
Table~\ref{tab-samples} for both the full region and the inter-cluster
region. As in D99 we have also compiled a larger list of galaxy
measurements in the survey region based on published data (NED
searched 2003 Aug 5) and other new observations by our group (Quintana
et al.\ in preparation). The table shows that the completeness is
highest for the brighter magnitude limits, peaking at 28 per cent for
the whole sample at $m_R<16$.


% AREAS
%  full              182
%  full RA<14:05     151
%  Shap vel clusters 159
%  all clusters  is  151 sq deg

\begin{table}
\caption{Galaxies observed}
\label{tab-samples}
\begin{center}
\begin{tabular}{lrrrl}
\hline
Field  & R Mag limit &  Catalogue  &  FLAIR-II  & FLAIR-II + Published \\
\hline
Full          & 16.0 &  6193 & 409 (7\%)& 1754 (28\%)\\
Full          & 16.5 & 14635 & 643 (4\%)& 2627 (18\%) [10\%]\\
Full          & 17.0 & 30949 & 701 (2\%)& 3279 (11\%) [4.0\%]\\
\hline
Full RA$<$14:50     & 16.0 &  5309 & 397 (7\%)& 1630 (31\%)\\
Full RA$<$14:50     & 16.5 & 12256 & 610 (5\%)& 2458 (20\%) \\
Full RA$<$14:50     & 17.0 & 25484 & 658 (3\%)& 3087 (12\%)\\
\hline
Inter-cluster & 16.0 &  4930 & 293 (6\%)& 1138 (23\%) \\
Inter-cluster & 16.5 & 11819 & 459 (4\%)& 1580 (13\%) [6.4\%]\\
Inter-cluster & 17.0 & 25511 & 508 (2\%)& 1911  (7\%) [2.4\%]\\
\hline
\end{tabular}
\end{center}
Notes: the completeness of each sample compared to the catalogue is
given in parentheses (integral) and brackets [differential].
\end{table}


\begin{figure}
\hbox{
\psfig{figure=fig_mag1.eps,width=8cm}\psfig{figure=fig_mag2.eps,width=8cm}}
\caption[]{Magnitude distributions of observed and catalogued galaxies
in the Shapley region. Left: full samples; Right: inter-cluster region
only. Note that in each case the catalogue histogram is on a
different scale, shown on the right.}
\label{fig-mag1}
\end{figure}

%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
\section{Discussion}

We have obtained a total of new 710 galaxy radial velocities from all
of our FLAIR-II observing runs. This represents a substantial
improvement in the available velocity catalogue in the SSC
particularly for the previously neglected inter-cluster regions.
In this section we use our sample to analyse the extent of the SSC and
the galaxy overdensity it represents.

\subsection{Extent of the SSC}


Fig.~\ref{fig-cone} shows the combined resulting distribution of
galaxies towards the Shapley supercluster as cone diagrams in right
ascension and declination for both available literature redshifts and
our new combined sample. The importance of the SSC in this region of
the sky is demonstrated by the fact that 65\% of galaxies in our new
combined sample belong to the SSC with velocities in the range
8000--18500~\kms.  In both plots the new data are indicated by
larger squares to emphasise their impact. It can be seen that by
probing large regions of the SSC away from the rich Abell clusters, we
have revealed significant additional structures which make complex
links with the main cluster locations.

\begin{figure*}
\vspace{-4.0cm}
\psfig{figure=fig_coner.eps,height=15cm}
\vspace{-4.0cm}
\psfig{figure=fig_coned.eps,height=15cm}
\caption[]{Cone velocity diagram in right ascension from R.A.$=
12^h15^m$ to R.A.$= 14^h30^m$ (upper panel), and declination from
$-26^{\circ}$ to $-38^{\circ}$ (lower panel) for the measured galaxies
in the Shapley Supercluster. Previously published galaxies are plotted
as points; the combined new measurements from our project are
plotted as squares. Also show as large circles are the locations of
the richest galaxy clusters in this region.}
\label{fig-cone}
\end{figure*}

Fig.~\ref{fig-redshift} shows the histogram of 2030 galaxy redshifts
in the direction of the Shapley supercluster with all currently
available published velocities (including our combined sample) in the
range 0~\kms $\leq$ V $\leq$ 40000~\kms with a step size of
500~\kms. The new velocities are also shown as the hatched region.

%\begin{figure*}
%\psfig{figure=shapley3f_caustic.eps,width=9cm}
%\caption[]{Projected distribution of galaxies around the cluster
%  A~3571 with the location of a caustic profile shown as a dashed
%  line.}
%\label{fig-redshift}
%\end{figure*}

\begin{figure}
\psfig{figure=fig_histo1.eps,width=9cm}
\caption[]{The redshift distribution of galaxies in the SSC survey
  region. The area of sky is 182 square degrees. The shaded histogram
  shows the 710 new measurements we present here and the upper
  histogram shows those combined with all know published redshifts, a
  total of 4215 galaxies. The bin size is 500~\kms.}
\label{fig-redshift}
\end{figure}

In agreement with previous works we note the presence of a prominent
foreground wall of galaxies (the Hydra-Centaurus region) at
$\overline{V}$= 4000~\kms. This distribution can be related to the
nearby cluster A3627 associated with the ``Great Attractor''
(Kraan-Korteweg et al. 1996).  Moreover, our newly measured galaxies
tend to establish a link between the Hydra-Centaurus region and the
SSC especially at the high Dec.\ end of the cone. A similar structure
was suggested by Tully et al.\ (1992).

Concerning the main SSC, our new data
revise our knowledge of its large-scale structure by measuring a large
number of galaxies away from the rich Abell clusters previously
studied.  The majority ($65\%$) of the galaxies we observed were found
to be part of the SSC, so our principal result is to show that the SSC
is bigger and more complex than previously thought. Looking at the
cone diagram in Right Ascension (Fig.~\ref{fig-cone}) we can see that
the SSC is separated into two main velocity components as previously
suggested (D99). The nearer concentration at about
$\overline{V}$=11240~\kms is located to the East of the main SSC
region at about $\overline{V}$=14850~\kms. However clumps of objects
seem to link these two main structures which were not observed
before. Care must be taken in the interpretation of the cone plots
because of the finger of God effect evident in the main SSC
concentrations due to the internal individual cluster velocity
dispersions which can lead the eye to spurious links.

A large concentration of objects at about R.A.$= 12^h54^m$ and around
$\overline{V}$= 16000-17000~\kms\  (the ``A3558'' complex; see Bardelli
et al.\ 2000) is connected to the main structure by a broad bridge of
galaxies. It can also be seen from the Declination cone diagram
(Fig.~\ref{fig-cone} lower panel) that the Southern part of the SSC
consists of two large sheets of galaxies, of which the previously
measured Abell Clusters represent the peaks of maximum density. The
more distant sheet, in particular, at $\overline{V}$= 15000~\kms is
present right across the observed region from $-27^{\circ}$ to
$-38^{\circ}$ so the true extent of this wall is currently
unknown. The Southern part of this wall may be an extension of the
plane of galaxies defined by Bardelli et al.\ (2000), although it has
the same offset of $-5$\hMpc as our earlier D99 sample when analysed
by Bardelli et al.\ in their Figure~4.

These new observations mean that we must re-appraise the conclusions
of previous papers about the overall shape of the SSC. Based on the
previously available velocity information on the main clusters it was
thought that the SSC was highly elongated and either inclined towards
us or rotating. We now reveal that the SSC extends as far as our
measurements do to the South via a broad inter-connected wall so we
find it is not elongated or flattened.  The actual situation so far
revealed is more complex, being composed of the known Abell clusters
embedded in at least two sheets of galaxies of much larger extent.

\subsection{Galaxy Overdensity}

% Numbers 7500<cz<1800 in FULL 182 deg2 from Metcalfe
% -with FULL completeness(mag) included
% Rlim  N/deg2  Nexpect  Nobs  Overdensity
% 16.0  4.2538  348.1    1185  3.4 0.10
% 16.5  5.5929  403.0    1783  4.4 0.10
% 17.0  6.5629  428.7    2144  5.0 0.10
%
%
% Numbers 7500<cz<1800 in INTER 159 deg2 from Metcalfe
% -with INTER completeness(mag) included
% Rlim  N/deg2  Nexpect  Nobs  Overdensity
% 16.0  3.4942  249.8     637  2.5 0.10
% 16.5  4.3512  280.5     863  3.1 0.10
% 17.0  4.9332  294.0     979  3.3 0.11
%
% So how much of the total overdensity is INTER?
% expect 428.7 obs 2144 = 979(inter)+1165(cluster)
%
% Surface density in full 182 deg2 expected from Metcalfe
% Rlim  N/deg2  Nexpect  Nobs  Overdensity
% 16.0  15.2    2766     6193  2.2
% 16.5  28.6    5205    14635  2.8
% 17.0  52.9    9628    30949  3.2

In D99 we estimated the galaxy overdensity in an inter-cluster
region of area 44 deg$^2$ at the centre of the SSC region. Our new
observations, combined with data from the literature, allow us to
calculate the overdensity over a much larger region. We shall consider
both our full survey region of 182 deg$^2$ and our new inter-cluster
region of 151 deg$^2$.  As we are most interested in galaxies at the
distance of the SSC, the overdensity is best seen as the peaks in the
redshift histograms. 

In Fig.~\ref{fig-histo2} we show the redshift distributions for both
the full survey and inter-cluster regions. Also shown on both
histograms are the expected distributions for a smooth, homogeneous
galaxy distribution based on the number count data of Metcalfe et al.\
(1991). These were calculated allowing for the differential
incompleteness of each sample as a function of $m_R$ as listed in the
final column of Table~\ref{tab-samples}.

We calculated the galaxy overdensity as the ratio of the number of
observed galaxies within the nominal velocity limits of the SSC
complex (8000--18500\kms) to the number expected from the Metcalfe
counts within the same velocity limits, all with the magnitude limit
of $m_R<17$. In the full region the overdensity was $5.0\pm0.1$ and in
the restricted inter-cluster region is was $3.3\pm0.1$. This can be
compared with our result in D99 where we found $2.0\pm0.2$ over an
area of 44 deg$^{2}$.  Our overdensity values are lower than those
found by Bardelli et al.\ (2000) in a study of the central part of the
SSC. They report an overdensity of $3.9\pm0.4$ for their inter-cluster
sample and $11.3\pm0.4$ for their total sample, on scales of
$10h^{-1}$Mpc. Our data probe the distribution on much larger scales
of around 10--15 degrees corresponding to $26-40h^{-1}$Mpc.  We have
confirmed that earlier detection of a very significant galaxy
overdensity in the inter-cluster space of the SSC region. In terms of
galaxy numbers, the inter-cluster galaxies make up 46 per cent of the
2144 galaxies in the SSC velocity range, so assuming a similar mass
function they contribute a similar amount of mass to the cluster
galaxies which were the focus of most previous work on the SSC.


\begin{figure*}
\hbox{\psfig{figure=fig_histo2.eps,width=7cm}
\psfig{figure=fig_histo3.eps,width=7cm}}
\caption[]{Redshift distributions of galaxies in the SSC region
  compared to that expected for a smooth, homogeneous galaxy
  distribution. The samples are drawn from (A) our full survey region
  and (B) the inter-cluster region. In each case the samples are
  limited to $m_R<17$. The expected distributions (Metcalfe et al.\
  1991) are scaled to the bin size, area and completeness of our
  samples. The dashed vertical lines indicate the nominal redshift
  range of the SSC, 7500--18000\kms.}
\label{fig-histo2}
\end{figure*}

\section{Conclusion}

Our new observations of galaxies towards the Shapley supercluster
have, by surveying a large contiguous region including areas away from
known clusters, revealed substantial new, large, inter-connected
structures. The original SSC region has now been shown to form part of
a much larger structure extending uniformly in at least two sheets
over the whole surveyed region principally to the South of the SSC
core. We have detected an additional 426 members of the SSC in our
combined (D99 and this paper) survey area, increasing very
significantly the number of known SSC galaxies. Our new data suggest
that the SSC is at least 50\% more massive than previously thought
with a significant part of the extra mass in the closer
sub-region. The SSC must therefore has a more important effect on the
Local Group that originally envisaged. We defer a detailed calculation
of the size of this effect and a fuller analysis and interpretation of
these new data, to a subsequent paper (Proust et al, in preparation)
where some additional data will also be included.

We now plan to investigate regions well away from the SSC center
between R.A. 12h30 to 14h30 and from $-23^{\circ}$ to $-42^{\circ}$ in
order to: i) define the complete topology of the SSC, ii) analyze the
individual Abell clusters contained in the SSC and iii) determine more
precisely its gravitational effect on the Local Group. We have already
obtained the necessary extended catalogue of galaxies for this larger
region from additional red ESO/SRC SSC plates scanned by the MAMA
machine. The new 6dF replacement for FLAIR-II at
the UKST with its automated robotic fibre positioner and 150~fibres in
a $6^{o}$ field will be an ideal facility to continue our study of the
Shapley Supercluster.



\section*{Acknowledgments}
We wish to thank the UKST and AAO staff, especially Paul Cass, Malcolm
Hartley and Ken Russell. DP acknowledges receipt of a France-Australie
PICS in support of visits to Siding-Spring Observatory. We are
particularly grateful to Mike Read (ROE) for guidance with the
SuperCOSMOS survey data. We also thank Maureen Younger (UQ) for help
with the galaxy identifications.

This research was partially supported by the cooperative programme
ECOS/CONICYT C96U04 and HC thanks the FONDAP Centre for Astrophysics
and the Guggenheim Foundation for partial support.

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\bigskip



\begin{table*}[h]
\caption[]{Heliocentric redshifts for observed galaxies.}
\label{tab-cat}
\begin{flushleft}
\begin{tabular}{llllll}
\hline
RA      &   Dec    & field & $m_R$ & $v_{hel}$ & $\Delta v_{hel}$ \\
(J2000) & (J2000)  &       & (mag) & (\kms)    & (\kms)   \\
\hline
12:52:07.1&  $-$32:50:44 & 443 & 15.68&  15056 &  81  \\
12:52:35.2&  $-$31:14:36 & 443 & 16.14&  15580 &  40  \\
12:52:55.8&  $-$32:06:30 & 443 & 14.69&   8739 & 126  \\
12:53:23.8&  $-$28:20:46 & 443 & 15.81&  16403 &  60  \\
12:53:24.3&  $-$28:28:47 & 443 & 14.82&   8140 &  31  \\
12:53:33.0&  $-$32:19:44 & 443 & 15.13&   9277 &  74  \\
12:53:40.6&  $-$28:48:58 & 443 & 16.21&  16633 & 132  \\
12:53:55.1&  $-$28:20:30 & 443 & 15.91&  15938 & 166  \\
12:54:11.2&  $-$29:36:38 & 443 & 16.22&  25584 & 100  \\
12:54:23.0&  $-$29:04:17 & 443 & 16.08&  16380 &  96  \\
\end{tabular}
\end{flushleft}
\end{table*}

{\em Here we only present the first 10 lines of our 710-line catalogue
of all galaxies observed. The complete table is provided in the
electronic \LaTeX\  input file of the paper and as a separate text file.}

\end{document}

%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
12 52 07.1  -32 50 44  443   15.68  15056  81   
12 52 35.2  -31 14 36  443   16.14  15580  40   
12 52 55.8  -32 06 30  443   14.69   8739 126   
12 53 23.8  -28 20 46  443   15.81  16403  60   
12 53 24.3  -28 28 47  443   14.82   8140  31   
12 53 33.0  -32 19 44  443   15.13   9277  74   
12 53 40.6  -28 48 58  443   16.21  16633 132   
12 53 55.1  -28 20 30  443   15.91  15938 166   
12 54 11.2  -29 36 38  443   16.22  25584 100   
12 54 23.0  -29 04 17  443   16.08  16380  96   
12 54 31.4  -28 31 05  443   16.72  20873  34   
12 54 39.9  -29 27 33  443   15.48  15132 127   
12 54 55.5  -29 30 12  443   15.97  16340  86   
12 55 09.0  -31 56 55  443   16.77   3439  71   
12 55 11.6  -30 26 20  443   15.83  30321  79   
12 55 40.1  -30 02 16  443   15.96  15571  96   
12 55 40.3  -28 34 34  443   15.87  17033  71   
12 55 43.6  -29 24 41  443   16.10  18479  94   
12 55 54.2  -31 19 26  443   15.62  16232  94   
12 56 25.0  -29 13 00  443   15.48  16993  68   
12 56 27.8  -29 08 55  443   15.98  17719  19   
12 56 43.5  -27 59 04  443   15.92  30909  96   
12 56 50.5  -32 24 35  443   16.27   9039  25   
12 56 57.9  -29 14 31  443   16.27  24623  39   
12 57 01.3  -30 14 34  443   15.88  16698 174   
12 57 16.2  -29 56 23  443   16.21  17550 107   
12 57 18.3  -32 37 42  443   16.08   4737 135   
12 57 19.0  -31 48 34  443   15.55   8289  97   
12 57 24.8  -29 03 44  443   15.73  17863 129   
12 57 28.0  -30 42 15  443   16.36  12097 109   
12 57 29.9  -27 52 23  443   16.09  17497 139   
12 57 34.9  -30 27 02  443   15.95  17241  64   
12 57 58.5  -30 08 04  443   15.45  15159 130   
12 58 05.7  -30 16 28  443   15.70  16662  52   
12 58 08.4  -29 25 12  443   15.36  25974  88   
12 58 26.8  -28 29 44  443   15.60  20571  92   
12 58 42.5  -32 24 26  443   14.72   9237  64   
12 59 03.3  -31 44 49  443   15.94  15520  86   
12 59 05.2  -32 07 21  443   14.87   8442  60   
12 59 19.5  -29 36 53  443   15.39   3025  29   
12 59 43.7  -32 37 17  443   15.46  22833  81   
13 00 21.0  -31 57 10  443   15.93  16317  61   
13 00 24.1  -32 00 51  443   15.03  12359  81   
13 00 30.6  -30 51 54  443   14.98  17057  93   
13 00 33.0  -31 35 32  443   15.91  16787  95   
13 00 56.2  -28 21 11  443   15.84   2485  53   
13 01 18.2  -32 16 02  443   15.18   4614  39   
13 01 31.8  -31 55 45  443   16.06  25297  64   
13 02 01.7  -32 36 47  443   15.64  10635  47   
13 02 26.3  -32 01 38  443   16.38  14294  91   
13 03 01.2  -36 37 40  382   16.30   3443  36   
13 03 21.2  -33 58 43  382   15.80  23713  68   
13 03 24.9  -31 19 21  443   15.37   4912  25   
13 03 43.4  -28 14 28  443   15.23  14523  82   
13 03 44.2  -28 04 09  443   15.64  14633 127   
13 03 54.2  -36 32 13  382   14.98  10298  56   
13 04 15.6  -36 28 02  382   16.12  27469  33   
13 04 15.9  -33 52 32  382   16.26  21437 126   
13 04 22.1  -37 30 56  382   15.91  15818 101   
13 04 22.6  -31 11 43  443   14.62  15752 109   
13 04 27.9  -29 33 54  443   16.02  15441  43   
13 04 30.3  -28 23 22  443   14.61   5280 124   
13 04 58.8  -36 50 18  382   16.28  17698  13   
13 05 07.9  -28 23 46  443   14.92   9471  93   
13 05 26.1  -36 31 53  382   15.40  37525  71   
13 05 36.9  -34 17 58  382   16.30  25647  42   
13 05 43.7  -31 31 39  443   15.61  16416  82   
13 05 49.4  -36 45 01  382   15.07  10092  72   
13 06 02.3  -37 36 03  382   15.80  14899  97   
13 06 03.2  -36 00 33  382   16.03  24066  96   
13 06 15.9  -37 00 20  382   16.10  14943  69   
13 06 20.1  -29 33 48  443   15.96  20080  71   
13 06 31.9  -35 56 25  382   16.26  14737  72   
13 06 34.4  -34 11 38  382   16.01  25475 184   
13 06 46.7  -28 12 14  443   15.54  23485  88   
13 06 51.1  -36 58 57  382   16.21  15011 215   
13 06 56.1  -37 22 09  382   16.11  14058  47   
13 07 10.0  -32 11 31  443   16.01   9342  17   
13 07 20.1  -36 07 36  382   16.15  15099  75   
13 07 32.9  -32 50 18  382   14.50  15419 132   
13 07 36.7  -34 25 58  382   16.31  18872  37   
13 07 44.6  -37 35 12  382   16.00  15024  60   
13 08 00.5  -37 22 25  382   15.90  13228 117   
13 08 05.0  -32 07 03  443   16.27  15372  33   
13 08 06.2  -33 16 31  382   16.07  10171 150   
13 08 07.5  -34 19 32  382   16.05  15174 163   
13 08 11.0  -36 12 30  382   16.73  15763 139   
13 08 11.1  -28 34 25  443   16.49  32243 105   
13 08 12.9  -30 10 04  443   15.55  15262  31   
13 08 18.7  -31 04 04  443   16.08   4478  62   
13 08 27.7  -34 25 29  382   15.75  15067  78   
13 08 58.9  -37 31 18  382   16.34  14312  81   
13 09 02.8  -29 13 33  443   16.12   4416  37   
13 09 20.1  -31 53 32  443   15.30   3965  72   
13 09 21.9  -34 45 37  382   15.80  13201  76   
13 09 34.5  -34 40 59  382   16.36  18578  77   
13 09 43.7  -35 36 33  382   15.78  28284  52   
13 09 47.6  -32 44 09  443   15.60  21832 130   
13 09 55.8  -37 08 18  382   16.35  14350  61   
13 10 05.3  -31 54 09  443   15.56  15013  75   
13 10 16.0  -32 52 40  443   15.06   9510 109   
13 10 22.2  -34 36 46  382   16.66  27522  60   
13 10 28.5  -30 48 56  443   15.15   9646  45   
13 10 37.1  -37 18 03  382   15.07  14555  42   
13 10 48.9  -33 57 59  382   16.65  15113  95   
13 10 49.6  -31 18 43  443   15.70   9349  80   
13 11 06.5  -32 59 32  382   16.33  43801  44   
13 11 07.2  -33 04 58  382   16.07  15899  84   
13 11 14.0  -36 40 33  382   15.79   3363  89   
13 11 14.5  -34 05 35  382   16.30  14837  25   
13 11 24.7  -32 19 21  443   15.39  14942  34   
13 11 31.6  -30 26 32  443   14.38   9563  63   
13 11 38.5  -31 55 47  443   16.19  15192  54   
13 11 49.4  -34 18 19  382   16.21  27235  66   
13 11 55.5  -36 03 48  382   16.25  10491  54   
13 12 04.6  -37 27 35  382   16.08  13069 119   
13 12 07.0  -34 35 45  382   15.76   3196  80   
13 12 22.4  -35 20 36  382   16.20  23360  77   
13 12 24.3  -37 20 52  382   16.48  10414  81   
13 12 26.5  -34 01 35  382   16.03  13063 141   
13 12 41.1  -33 22 17  382   16.06  23141  79   
13 12 43.8  -36 14 55  382   15.56  14386  63   
13 13 01.6  -34 46 48  382   16.19  15159 154   
13 13 18.5  -28 29 09  443   15.85   4306  23   
13 13 19.0  -32 56 44  382   16.51  29991  72   
13 13 35.2  -33 22 19  382   16.35  29645 117   
13 13 37.2  -31 20 43  443   16.58  14813  64   
13 13 39.8  -32 50 37  443   15.61  15443  22   
13 13 43.1  -35 26 01  382   15.51   7527  96   
13 13 51.2  -36 32 39  382   15.16  14367  76   
13 13 54.7  -30 38 42  443   14.96   4634  75   
13 13 57.5  -33 55 05  382   15.11  15299  49   
13 14 10.2  -34 05 42  382   15.20  15355  81   
13 14 13.0  -37 13 28  382   16.59  10229  83   
13 14 20.2  -37 11 45  382   14.96  10688  59   
13 14 29.8  -33 23 03  382   15.11   8889  69   
13 14 41.8  -33 21 38  382   16.04  14649 115   
13 14 52.8  -32 45 27  382   16.45  30594 115   
13 14 56.7  -32 39 50  443   15.65  14603  70   
13 14 58.5  -32 45 21  443   16.17  31197  68   
13 15 02.2  -29 45 56  443   15.68  14638  53   
13 15 05.2  -32 15 00  443   15.36  14433  72   
13 15 06.6  -32 53 08  443   16.23  14315  76   
13 15 11.7  -33 38 20  382   15.03  14531  79   
13 15 27.2  -32 42 38  444   14.76  13869  96   
13 15 27.3  -32 43 12  443   16.22  14202  81   
13 15 29.1  -37 11 20  382   16.00  10048  85   
13 15 30.6  -28 17 04  443   15.15   4310  96   
13 15 36.7  -29 30 18  443   15.40  16187  46   
13 15 42.4  -32 42 11  443   15.79  14561  90   
13 15 56.4  -28 29 07  443   15.96  14025  82   
13 16 03.1  -36 58 56  382   16.21  31971  88   
13 16 09.9  -32 53 13  382   15.55  15284  88   
13 16 11.2  -31 11 26  443   15.21  11997  78   
13 16 14.4  -31 23 14  443   16.64  40199  89   
13 16 23.5  -35 16 13  382   16.32  11473  98   
13 16 25.5  -32 51 45  382   16.42  14428  86   
13 16 27.8  -32 12 57  443   16.16  10900  52   
13 16 30.7  -37 28 30  382   15.99  14637  23   
13 16 39.3  -32 15 11  443   16.78  14649 127   
13 16 42.7  -33 15 46  382   15.66  14315  98   
13 16 49.1  -35 47 36  382   16.16  32384 102   
13 17 17.6  -31 48 55  444   16.14  14998 126   
13 17 23.8  -33 26 57  382   15.83  15334  48   
13 17 26.2  -33 55 36  382   15.43  15224  73   
13 17 31.5  -31 36 27  444   16.16  15632 176   
13 17 48.6  -33 13 32  382   16.45  25689  64   
13 17 59.2  -37 25 52  382   15.25   7330  66   
13 18 04.5  -30 09 18  444   15.69   9769  73   
13 18 06.5  -35 48 30  382   15.74   3265  94   
13 18 08.7  -32 01 06  444   14.74   4358 114   
13 18 08.8  -36 59 01  382   15.87  14921  28   
13 18 19.9  -37 18 41  382   15.81  15014  63   
13 18 26.7  -33 18 03  382   15.09   4342  51   
13 18 54.9  -33 25 31  382   16.12  13407  47   
13 18 55.3  -31 49 03  444   15.05  15641 103   
13 19 07.9  -37 14 05  382   15.34  14311  86   
13 19 19.8  -33 18 31  382   16.36  15047  69   
13 19 27.3  -33 21 16  382   16.37  14960  70   
13 19 28.9  -35 06 08  382   15.29   1247  28   
13 19 29.3  -33 31 03  382   14.84  14981  98   
13 19 29.9  -33 54 56  382   15.65   8432  37   
13 19 40.0  -36 58 19  382   16.16  11687  66   
13 19 57.1  -34 17 47  382   15.99  23525 110   
13 20 13.5  -35 06 17  382   16.12  13924 121   
13 20 19.5  -37 05 36  382   15.76   2359  47   
13 20 27.5  -34 19 44  382   16.12  15106 145   
13 20 36.5  -34 07 57  382   16.25  23532  69   
13 20 42.5  -34 55 57  382   16.19  15393  86   
13 20 52.8  -28 13 06  444   16.04  15326 122   
13 20 56.5  -37 16 17  382   16.32  15980  78   
13 21 04.1  -33 03 00  382   15.73  15768  64   
13 21 06.1  -35 35 59  382   15.95  15654  85   
13 21 16.5  -35 11 34  382   15.63  20402  58   
13 21 21.5  -35 48 47  382   16.02  15373 163   
13 21 24.7  -32 46 33  444   15.15  14469 110   
13 21 29.2  -36 10 04  382   15.61  15345  94   
13 21 40.4  -34 56 16  382   15.76  15222 196   
13 21 48.1  -35 32 18  382   15.09  13903 170   
13 21 50.7  -33 52 30  382   16.27  35049 132   
13 21 57.8  -35 45 17  382   15.89  16535  91   
13 22 01.2  -28 22 16  444   15.08  14030  85   
13 22 10.8  -34 47 52  382   15.96  15664 126   
13 22 16.4  -34 37 12  382   16.01  15667 127   
13 22 28.0  -33 29 03  382   16.40   3497  96   
13 22 38.4  -35 52 12  382   16.14  14747 142   
13 22 43.1  -33 26 07  382   14.93  14379  44   
13 22 54.8  -35 02 55  382   15.55   7237  96   
13 22 58.7  -32 42 47  382   15.28   8503  67   
13 23 03.1  -34 59 07  382   15.73  16498  84   
13 23 14.2  -35 19 36  382   16.16  14710  59   
13 23 43.1  -34 27 36  382   16.00  15426 126   
13 23 43.4  -35 53 43  382   15.30   3792  78   
13 23 44.7  -27 59 30  444   15.22  13674  69   
13 23 45.2  -31 42 27  444   16.58  15170  63   
13 23 54.1  -34 39 38  382   15.06  14472 103   
13 23 54.3  -32 10 56  444   14.83  15249 107   
13 23 55.4  -29 18 22  444   15.99  14096  98   
13 24 18.8  -31 38 41  444   15.29  14390 176   
13 24 22.4  -32 53 42  382   15.67  14251 135   
13 24 25.4  -30 15 03  444   15.20   3634  98   
13 24 29.5  -33 58 35  382   15.81  14827  87   
13 24 42.9  -36 17 50  382   15.68  10771  96   
13 24 48.5  -34 22 33  382   15.71   8371 106   
13 24 50.5  -31 33 38  444   16.35  14773  14   
13 25 10.1  -33 54 41  382   16.64  27194 132   
13 25 38.0  -36 35 20  382   15.69  15208  42   
13 25 48.5  -37 17 02  382   15.96  10225 123   
13 26 14.8  -37 02 44  382   16.40  19958 150   
13 26 46.1  -31 31 43  444   16.33  14660 117   
13 26 54.9  -34 10 39  382   16.14  14909  34   
13 26 57.5  -32 11 52  444   16.05  13839  84   
13 27 01.1  -30 04 34  444   15.69   1866  78   
13 27 03.5  -31 13 31  444   15.56  16332 122   
13 27 10.2  -37 05 00  382   15.77  14367  76   
13 27 13.1  -36 25 34  382   15.82  14520  36   
13 27 20.2  -36 29 38  383   15.47  14637  25   
13 27 24.5  -32 18 00  444   15.90  14176  82   
13 27 48.3  -32 37 16  383   15.94  11832  16   
13 28 02.1  -31 46 10  444   16.34  15590  96   
13 28 04.0  -32 45 43  383   15.51  11585  57   
13 28 09.0  -31 40 52  444   15.56  12200 135   
13 28 13.1  -30 14 32  444   15.57  12776  81   
13 28 32.2  -33 59 50  383   16.05  24960  71   
13 28 32.6  -34 12 23  383   15.96  14661 129   
13 29 01.1  -33 30 23  383   16.27  14540  52   
13 29 01.8  -28 50 22  444   15.15  12289  58   
13 29 17.0  -32 02 34  444   15.29  14060 114   
13 29 28.3  -31 33 04  444   14.69  15430  87   
13 29 40.1  -28 15 57  444   15.03  10015 119   
13 29 45.1  -32 52 22  383   16.99  16678  54   
13 29 56.8  -29 14 31  444   16.11  14201 114   
13 30 01.3  -27 58 29  444   15.64  10237 114   
13 30 12.1  -29 30 06  444   16.41  14488  30   
13 30 12.7  -32 48 22  383   15.64  15666  78   
13 30 30.2  -34 37 16  383   15.23  21467  84   
13 30 40.8  -31 51 55  444   16.13  14470  75   
13 31 01.4  -32 37 18  383   16.26  15986  64   
13 31 09.6  -32 44 13  383   16.16   3468  95   
13 31 23.4  -33 53 52  383   16.18  22089  90   
13 31 51.4  -36 57 20  383   15.99  14996  97   
13 32 00.2  -36 18 35  383   15.61  20282  59   
13 32 05.4  -33 47 22  383   15.69   8770  66   
13 32 07.0  -33 19 03  383   15.36  13640  98   
13 32 15.2  -33 22 40  383   15.36  15243  81   
13 32 24.0  -33 14 19  383   15.25  13916  47   
13 32 27.2  -37 30 48  383   15.55  15295  29   
13 32 31.3  -33 09 42  383   15.19  14770  96   
13 32 34.3  -37 17 36  383   16.04  15687 101   
13 32 41.2  -35 09 15  383   15.90  15122  39   
13 32 48.8  -29 01 04  444   15.57   5526  93   
13 32 52.2  -34 43 06  383   16.00  36879  77   
13 32 55.1  -33 10 13  383   15.90  15698  50   
13 33 01.5  -33 06 01  383   15.44  14951  53   
13 33 05.7  -33 18 04  383   14.95  14838 115   
13 33 07.0  -34 26 59  383   15.91   7491  16   
13 33 07.0  -37 29 59  383   16.07  15164  67   
13 33 09.6  -31 36 12  444   15.33  14559 123   
13 33 12.6  -36 24 25  383   16.24  11095  87   
13 33 25.4  -33 56 57  383   15.11  22010 143   
13 33 25.8  -33 56 11  383   16.24  13810  67   
13 33 35.4  -31 28 25  444   15.84  15201  74   
13 33 44.9  -36 07 21  383   15.70  14951  63   
13 33 45.6  -35 24 20  383   16.26  15377 147   
13 33 53.5  -35 23 01  383   16.21  21640  89   
13 34 04.4  -35 19 44  383   16.16  12454  79   
13 34 05.6  -28 09 33  444   15.89   9187  74   
13 34 07.4  -31 29 21  444   15.46  14842  89   
13 34 11.6  -35 04 02  383   16.17  14917  69   
13 34 12.6  -32 58 38  383   15.96  15177  70   
13 34 13.7  -29 22 36  444   14.97  14008  96   
13 34 19.2  -35 17 27  383   15.79  14976  60   
13 34 22.7  -35 24 51  383   16.04   9416  65   
13 34 23.2  -31 44 07  444   15.70  16271  85   
13 34 33.1  -36 48 32  383   15.26   2398  17   
13 34 36.1  -35 20 50  383   16.28  14027  51   
13 34 41.1  -35 02 10  383   15.64   2367  21   
13 34 41.6  -33 31 12  383   15.87   3148  84   
13 34 45.7  -35 13 53  383   15.53  16579  20   
13 34 49.9  -34 14 44  383   15.60   3945  67   
13 34 54.7  -35 32 56  383   16.05  14931  83   
13 35 07.4  -36 38 22  383   15.99  15278  15   
13 35 09.0  -34 02 06  383   16.82   3878  52   
13 35 18.2  -37 17 39  383   15.39   9426  67   
13 35 18.4  -31 25 34  444   16.30  14845  86   
13 35 23.1  -34 09 39  383   15.43   7208  66   
13 35 39.1  -31 43 01  444   15.07  11794  98   
13 35 46.8  -35 34 14  383   16.28  15438  54   
13 35 49.8  -34 14 32  383   14.80   3372  77   
13 36 15.3  -36 53 45  383   15.48   3897  79   
13 36 29.0  -33 05 32  383   15.51  15688 105   
13 36 33.1  -34 04 28  383   15.81   3787  43   
13 36 34.6  -29 05 21  444   14.67   4516  89   
13 36 53.9  -36 34 15  383   14.91  17625  73   
13 36 57.8  -34 23 59  383   16.06   4133  76   
13 37 01.0  -28 32 01  444   16.41  15262  98   
13 37 02.9  -33 49 24  383   16.27  13931  87   
13 37 21.0  -34 53 25  383   15.00  29247 103   
13 37 34.3  -31 52 43  444   16.82  11598  98   
13 37 37.5  -34 31 57  383   15.73  22108  68   
13 37 41.6  -33 51 10  383   16.02  11289  85   
13 37 43.3  -35 29 44  383   15.93  15162  89   
13 37 47.7  -36 13 56  383   16.39  15316  57   
13 37 52.5  -35 38 27  383   15.47  15695  71   
13 38 08.1  -35 03 44  383   15.22  15162  92   
13 38 12.1  -31 57 02  444   15.90  14694 127   
13 38 14.2  -32 51 05  383   15.93  11489  23   
13 38 21.4  -35 57 42  383   16.39  11327  74   
13 38 45.4  -35 28 24  383   15.86  14685  37   
13 38 54.6  -36 26 51  383   16.22  13789  55   
13 38 57.5  -35 27 56  383   15.26  15803 139   
13 38 57.8  -35 37 29  383   16.46  15223  89   
13 38 58.9  -36 35 39  383   15.83  13755  74   
13 38 59.9  -32 36 04  444   16.18  16298  77   
13 39 01.2  -30 58 13  445   15.09   4107  95   
13 39 10.0  -31 00 36  445   15.46  22962 106   
13 39 10.3  -36 54 55  383   16.27  15741  44   
13 39 10.7  -34 02 35  383   16.73  21245  28   
13 39 26.0  -35 28 01  383   16.54  19147  68   
13 39 26.5  -36 20 36  383   15.81  36756 104   
13 39 31.1  -35 40 25  383   15.88  16009  51   
13 39 36.6  -34 01 06  383   16.32  15268  76   
13 39 36.9  -35 40 06  383   15.74  15791  78   
13 39 42.5  -35 48 51  383   15.54  15047  43   
13 39 43.6  -35 56 43  383   16.21  29346  77   
13 39 48.3  -33 39 19  383   15.80  15381  43   
13 39 48.4  -33 05 02  383   16.72  15345 135   
13 39 52.1  -32 05 42  445   15.77  11627  67   
13 39 58.8  -28 03 05  445   15.10  14314  70   
13 40 03.9  -33 04 04  383   16.15  11841  59   
13 40 06.5  -32 50 26  383   16.27   7254  14   
13 30 06.0  -34 21 10  383   15.00  21441  89   
13 40 16.8  -30 24 50  445   16.00  15199  76   
13 40 30.3  -33 59 18  383   16.14  14867  61   
13 40 33.7  -35 40 26  383   15.88  15641  57   
13 40 40.8  -30 26 59  445   15.83   4496 114   
13 40 41.7  -32 18 03  445   15.30  14394  59   
13 40 42.5  -30 17 49  445   15.94  11840  45   
13 40 43.9  -37 02 05  383   14.89  21697  77   
13 40 45.0  -31 47 24  445   16.14  11583  57   
13 40 52.5  -34 08 12  383   16.78  15579  30   
13 40 54.3  -33 40 33  383   15.82  15167  66   
13 40 54.9  -28 06 47  445   15.72  10964  61   
13 41 05.3  -34 22 22  383   16.66  15485  98   
13 41 16.2  -35 39 18  383   15.19  15068  85   
13 41 16.4  -30 51 03  445   16.94   4519  55   
13 41 32.8  -34 22 53  383   15.98  16973  66   
13 41 33.5  -33 56 22  383   15.75  15161  48   
13 41 34.8  -30 33 46  445   15.73  15595  73   
13 41 36.3  -31 52 47  445   15.55  11467  39   
13 41 42.0  -34 04 14  383   16.17  14610  47   
13 41 46.6  -35 52 42  383   15.38  11378  62   
13 41 49.4  -33 11 06  383   14.71  11945  65   
13 41 52.3  -32 34 39  445   15.44  12074  98   
13 41 53.0  -35 11 31  383   16.12  29928  49   
13 41 54.9  -32 26 36  445   16.19  11748  43   
13 42 19.0  -29 46 52  445   15.64  14476  65   
13 42 22.3  -37 11 27  383   15.33  11288  31   
13 42 29.1  -34 52 39  383   16.70   4454  51   
13 42 36.6  -34 52 40  383   16.17  26968  47   
13 42 39.4  -37 37 01  383   16.23  10122  76   
13 42 41.6  -27 58 34  445   16.13  13858  57   
13 42 44.6  -34 05 35  383   16.95   7543  13   
13 42 49.9  -36 10 21  383   15.94  21887 155   
13 42 50.7  -32 08 02  445   15.98  13325  54   
13 42 53.6  -31 07 17  445   15.94   4557  29   
13 42 55.7  -34 58 17  383   15.40  16170  50   
13 42 58.8  -31 53 10  445   14.74  11689  64   
13 42 59.3  -33 58 07  383   16.20  15096  30   
13 43 14.0  -28 28 17  445   16.08  10975  68   
13 43 21.6  -36 19 22  383   16.17  24883 122   
13 43 25.9  -33 14 48  383   15.96  12267  97   
13 43 29.8  -29 49 21  445   15.96  23270  72   
13 43 29.9  -37 38 48  383   15.82  11113  52   
13 43 33.9  -34 46 52  383   15.47  17030  72   
13 43 36.9  -36 25 03  383   15.07   4311  59   
13 43 39.2  -27 48 29  445   15.57  12231  58   
13 43 46.5  -35 04 30  383   15.29  14681  71   
13 43 49.0  -29 44 40  445   15.01   4123  68   
13 43 54.1  -29 50 02  445   16.10   4687  37   
13 43 54.3  -35 46 16  383   14.83  11637  28   
13 43 54.6  -36 11 42  383   16.42  11298 103   
13 44 08.7  -34 20 26  383   15.94  11202  76   
13 44 17.2  -34 06 31  383   15.88  11818  71   
13 44 17.6  -27 47 30  445   15.99  13811 110   
13 44 18.4  -36 37 45  383   16.21  11498  46   
13 44 39.6  -32 39 14  383   15.81  12438  76   
13 44 42.0  -34 00 51  383   15.21  15271  23   
13 44 43.7  -35 26 02  383   15.82  37694  72   
13 44 43.9  -30 03 28  445   16.40   4521  29   
13 44 45.3  -33 36 07  383   15.14  11063  31   
13 48 44.7  -30 10 59  445   15.62  11833  69   
13 44 49.3  -34 37 47  383   15.14  14660  48   
13 44 51.2  -32 03 59  445   15.91  11131  49   
13 44 54.0  -27 54 03  445   16.06  11011  49   
13 45 02.7  -32 53 27  383   16.08  12085  83   
13 45 02.9  -35 14 00  383   14.55  17045  66   
13 45 04.2  -31 38 06  445   15.67   4671  47   
13 45 05.7  -29 26 20  445   14.92  14738  56   
13 45 17.5  -32 38 48  383   16.08   9469  41   
13 45 25.7  -29 51 03  445   15.54  14846  74   
13 45 29.1  -36 46 59  383   16.23   7633  80   
13 45 33.3  -35 16 10  383   16.06  17237  50   
13 45 35.5  -31 53 36  445   15.90  23564  46   
13 45 37.0  -30 47 12  445   16.90  22436  72   
13 45 40.6  -30 51 08  445   15.01  40196  74   
13 45 40.9  -29 53 38  445   16.17   4351  64   
13 45 41.5  -35 21 35  383   15.67  17363  38   
13 45 49.6  -34 01 54  383   15.81  15058  33   
13 45 56.0  -32 13 44  445   16.15  15174  74   
13 45 57.2  -33 16 32  383   14.74  11407  65   
13 46 01.4  -33 44 39  383   16.14  24838  61   
13 46 02.8  -30 10 06  445   16.14   4542  80   
13 46 11.5  -34 29 50  383   15.12  24806  35   
13 46 19.0  -31 45 44  445   15.86  12502  54   
13 46 22.2  -33 10 22  383   15.72  11760  52   
13 46 25.0  -29 53 18  445   16.05  11359  64   
13 46 25.0  -31 09 02  445   15.62   4121  44   
13 46 25.6  -32 39 58  383   16.74  12884  52   
13 46 28.3  -28 00 59  445   15.35  24039 109   
13 46 30.8  -32 28 45  445   15.98  10352  52   
13 46 33.1  -30 33 00  445   15.95  14399  69   
13 46 34.0  -35 12 01  383   15.34  11423  15   
13 46 35.4  -28 20 09  445   15.91   2612  94   
13 46 37.0  -32 23 11  445   15.58  15259  55   
13 46 39.6  -30 47 30  445   15.65  14781  71   
13 46 40.9  -31 34 53  445   16.01  11035  64   
13 46 42.9  -30 51 59  445   15.54   5092  78   
13 46 47.7  -28 38 59  445   14.82  11091  39   
13 46 48.9  -29 45 21  445   15.54  14350  48   
13 46 52.5  -30 48 40  445   16.47  11758 105   
13 46 55.2  -33 19 03  383   15.58  11113 157   
13 47 01.4  -35 18 51  383   16.53  11453  47   
13 47 02.7  -32 29 15  445   16.14  10681  66   
13 47 02.9  -37 27 31  383   15.99  11357  50   
13 47 08.5  -32 54 27  383   16.04  12304 159   
13 47 09.4  -33 23 36  383   14.94  11518  77   
13 47 10.5  -32 30 56  445   16.37  11840  52   
13 47 13.1  -33 38 41  383   15.68  13010  70   
13 47 18.4  -36 22 28  383   15.83  10963  66   
13 47 19.1  -29 05 55  445   15.50  11548  32   
13 47 22.6  -33 05 47  383   14.58  11694  49   
13 47 22.7  -30 37 22  445   15.88   4127  80   
13 47 22.8  -33 36 11  383   14.85  16117  48   
13 47 29.8  -32 08 29  445   15.53  12689  54   
13 47 34.2  -30 40 03  445   15.51  11952  52   
13 47 40.2  -28 18 16  445   16.07  11107 155   
13 47 46.3  -30 21 58  445   15.47   3827  88   
13 47 47.4  -32 19 45  445   15.44  11678  60   
13 47 50.0  -33 11 01  383   16.12  10328  29   
13 47 53.8  -29 06 26  445   15.85  14756  46   
13 47 58.5  -32 52 08  383   15.74  11789  80   
13 48 01.6  -31 48 50  445   15.33  12277 115   
13 48 02.9  -31 27 47  445   15.16   4862  33   
13 48 03.6  -32 37 46  445   15.07  10447  60   
13 48 04.4  -33 21 03  383   14.71  11901  34   
13 48 06.1  -32 30 34  445   16.36  11666  55   
13 48 09.1  -27 42 57  445   16.05  11348  62   
13 48 11.8  -32 47 20  383   16.17  12585 138   
13 48 14.3  -30 44 17  445   15.88  14738  79   
13 48 18.0  -32 09 11  445   15.78  29272  73   
13 48 21.4  -29 59 23  445   15.66   5117  82   
13 48 24.4  -34 41 06  383   16.10  13896  88   
13 48 25.1  -27 34 10  445   14.90  11118 102   
13 48 27.3  -35 53 45  383   14.93   7538  52   
13 48 29.7  -29 31 55  445   16.66   4235 160   
13 48 33.0  -35 41 09  383   16.17  30107  78   
13 48 37.5  -29 02 26  445   16.09  14697  42   
13 48 42.8  -34 39 25  383   15.95  27740  73   
13 48 42.8  -28 33 52  445   16.00  28728  72   
13 48 45.9  -37 29 47  383   16.14  11128  83   
13 48 48.9  -32 06 52  445   15.79  12523  55   
13 48 55.3  -30 24 24  445   14.78   4681  52   
13 48 58.0  -32 51 26  383   14.82  11396  42   
13 48 58.4  -30 57 47  445   15.36   4597  66   
13 48 59.0  -33 24 38  383   15.89  10868  31   
13 49 00.3  -33 58 12  383   16.07  11327  35   
13 49 03.7  -28 04 44  445   15.59   4883  76   
13 49 05.9  -30 28 47  445   14.97   4157  29   
13 49 14.1  -30 20 13  445   16.10   3800  71   
13 49 23.6  -28 55 08  445   16.17  14997  70   
13 49 25.3  -32 09 21  445   15.70  11477  65   
13 49 27.1  -30 03 03  445   16.10  11869  91   
13 49 29.0  -31 25 42  445   15.75  14777  93   
13 49 35.8  -30 09 23  445   15.56   4719  61   
13 49 39.7  -29 20 55  445   15.44  15212  55   
13 49 44.5  -30 08 20  445   14.96  22419  58   
13 49 48.8  -29 36 41  445   14.69   4280  63   
13 49 51.3  -27 30 49  445   14.98  11670  50   
13 49 51.4  -35 28 59  383   16.24  28576 122   
13 49 53.6  -33 17 23  383   16.42  16129  67   
13 49 54.3  -28 08 57  445   15.78  14513  63   
13 49 55.9  -30 40 52  445   16.02  12335 136   
13 50 00.1  -36 45 49  383   16.10  30091  89   
13 50 07.2  -31 15 07  445   14.43  14416  62   
13 50 09.6  -30 45 23  445   15.48  14731  87   
13 50 12.7  -31 16 50  445   15.14   4649  93   
13 50 15.4  -30 20 09  445   15.99  22737 103   
13 50 16.1  -33 04 29  383   14.86  10522  50   
13 50 22.7  -32 08 23  445   15.86  12267  49   
13 50 31.4  -32 40 45  383   15.83  11098  51   
13 50 33.4  -31 09 05  445   14.68  11648  65   
13 50 35.7  -32 13 34  445   16.08   4673  31   
13 50 38.8  -30 51 04  445   15.00   4294  42   
13 50 42.4  -32 53 42  383   15.74  11270  37   
13 50 51.0  -31 51 41  445   15.80  11575  64   
13 50 52.5  -36 48 19  384   16.13   4137  16   
13 50 59.1  -27 53 13  445   16.37  15688  30   
13 51 02.6  -30 56 59  445   15.31  14853  71   
13 51 04.5  -36 05 01  383   16.24  22610  95   
13 51 05.6  -31 03 08  445   15.07  14602  59   
13 51 07.7  -31 25 42  445   15.26  14720  46   
13 51 10.5  -33 44 53  383   16.58  12172  71   
13 51 14.5  -31 45 55  445   15.77  15593  69   
13 51 20.5  -31 50 14  445   15.24  15438  66   
13 51 25.3  -28 16 23  445   14.49   4706  56   
13 51 27.4  -29 15 21  445   16.35  11834  84   
13 51 30.7  -29 51 10  445   15.38  14709  96   
13 51 31.7  -32 01 09  445   15.92  29299 114   
13 51 41.7  -30 16 17  445   16.03  22321  60   
13 51 44.1  -28 14 53  445   15.04   5064 112   
13 51 46.0  -29 19 09  445   15.86  14146  38   
13 51 46.6  -28 54 34  445   16.09  13756 137   
13 51 49.1  -30 18 36  445   16.42   7036  48   
13 51 52.1  -28 27 34  445   15.39  11130 107   
13 51 54.8  -34 04 36  384   15.71  11064  38   
13 51 55.7  -30 03 32  445   15.11  22269  76   
13 52 07.2  -31 49 52  445   16.89   4409  24   
13 52 07.9  -30 27 06  445   15.80   4671  81   
13 52 09.1  -31 04 34  445   14.98  14569  83   
13 52 15.3  -29 00 14  445   16.31  13807  81   
13 52 25.8  -35 49 34  384   15.28  21934  66   
13 52 30.6  -27 56 23  445   15.63  14854  54   
13 52 37.4  -28 02 08  445   15.44  15393  85   
13 52 51.7  -28 48 12  445   15.37   5321  68   
13 52 54.1  -30 51 18  445   14.83   6910  58   
13 52 55.5  -28 34 00  445   16.23  14658  73   
13 52 56.7  -27 54 35  445   14.48  14988  94   
13 53 05.8  -28 47 58  445   15.89   5344  79   
13 53 12.8  -30 25 31  445   15.43  21992 124   
13 53 16.5  -28 59 59  445   15.98   4621  84   
13 53 21.9  -29 23 34  445   15.89  14887  50   
13 53 27.9  -27 58 28  445   15.53  15835  93   
13 53 28.9  -27 52 43  445   16.50  13576  96   
13 53 30.2  -35 37 48  384   15.41  11175  70   
13 53 32.2  -34 07 09  384   16.64  11028  28   
13 53 40.6  -33 56 57  384   15.54  11107  56   
13 53 44.6  -30 31 41  445   16.05   7056  25   
13 53 49.9  -27 51 24  445   16.61  14152 114   
13 53 55.7  -29 26 06  445   15.71   4358  68   
13 53 59.1  -27 57 08  445   15.49  13819  80   
13 54 00.2  -31 04 59  445   16.30  15011  56   
13 54 03.9  -27 51 41  445   15.65  15408 117   
13 54 07.6  -32 54 04  384   15.21   4397  37   
13 54 17.6  -30 18 08  445   15.91  21993  68   
13 54 18.1  -36 55 25  384   15.29  15204  83   
13 54 18.7  -30 29 54  445   16.55  12620  55   
13 54 18.7  -34 44 43  384   16.14  14923  24   
13 54 20.5  -32 12 25  445   15.25  12016  56   
13 54 26.2  -27 52 22  445   16.07  15931  76   
13 54 34.8  -31 28 12  445   16.22   5685  39   
13 54 42.0  -32 31 29  445   16.12  23230 126   
13 54 47.8  -29 54 34  445   15.95  21816  63   
13 54 56.1  -31 49 33  445   15.48  14936  58   
13 54 57.0  -32 17 25  445   16.69  11385  99   
13 55 07.9  -29 05 45  445   16.19  13782  60   
13 55 14.0  -29 20 38  445   16.19  12880  83   
13 55 18.1  -32 12 41  445   16.23  21456  53   
13 55 24.4  -31 18 21  445   16.01  22978  71   
13 55 49.1  -27 41 18  445   15.44  11902  39   
13 55 57.1  -29 08 02  445   15.56  11387  32   
13 56 04.6  -29 19 00  445   16.13   4623  61   
13 56 07.3  -28 19 37  445   15.67  30343 118   
13 56 15.2  -27 35 54  445   16.94  11914  36   
13 56 21.3  -35 10 48  384   16.11  18901  93   
13 56 32.6  -32 29 20  445   16.29   4512  32   
13 56 45.6  -31 35 08  445   16.26  24209  93   
13 56 49.5  -35 33 58  384   15.52  26685 100   
13 56 52.3  -30 53 46  445   15.62  12514  58   
13 57 05.6  -36 05 46  384   15.18  10888  62   
13 57 14.4  -31 36 01  445   16.70  11137  54   
13 57 17.3  -33 23 47  384   16.27  27528  40   
13 57 23.0  -31 14 33  445   16.95  22480  84   
13 57 27.6  -33 04 42  384   16.40  27843  59   
13 58 05.3  -33 30 58  384   15.45   4333  15   
13 58 06.7  -32 36 53  445   15.30   4205  85   
13 58 18.5  -30 28 01  445   15.42  11424  55   
13 58 31.6  -28 42 43  445   15.77   4975  30   
13 58 36.6  -30 51 09  445   16.97   4395  22   
13 58 57.2  -34 24 29  384   15.23  53089  75   
13 59 07.8  -28 47 08  445   15.08  11266  59   
13 59 16.3  -28 31 20  445   16.18   6786  28   
13 59 18.3  -30 48 36  445   15.86  11270  52   
13 59 34.0  -32 04 06  445   14.88  15231  33   
13 59 36.7  -30 55 04  445   15.48  15574  51   
13 59 37.0  -31 01 51  445   16.29  22042  58   
13 59 41.3  -29 17 14  445   15.71  15129  92   
13 59 42.9  -28 41 32  445   16.41  13669  66   
13 59 53.9  -31 08 55  445   16.07  27343  56   
13 59 57.0  -28 06 50  445   15.42  34600 124   
13 59 58.4  -28 23 43  445   16.28  14855  99   
14 00 00.5  -29 05 26  445   16.82  16506  29   
14 00 19.9  -35 46 57  384   16.02  23394  80   
14 00 20.7  -36 01 50  384   16.56  18696  77   
14 00 31.9  -32 36 04  445   15.95  18065  73   
14 00 47.6  -31 31 34  445   16.71  24726  64   
14 00 48.5  -30 30 11  445   16.07  20626  94   
14 00 53.1  -36 29 23  384   16.07   4117  34   
14 00 55.3  -28 23 05  445   16.70  15124  78   
14 01 07.0  -36 00 19  384   15.81  16903 145   
14 01 12.3  -31 27 36  445   15.62  24495  76   
14 01 36.9  -29 39 05  445   15.98  28459  89   
14 01 39.8  -29 56 50  445   16.91  21966  48   
14 01 43.9  -36 17 09  384   15.87  15400  73   
14 01 50.3  -29 41 50  445   16.02  28139 153   
14 01 53.6  -30 20 19  445   16.07  15854  67   
14 01 56.3  -30 08 02  445   16.79  20020  78   
14 02 01.1  -34 10 13  384   16.10   3605  78   
14 02 02.9  -29 42 49  445   15.49  29164 126   
14 02 05.4  -34 27 24  384   15.89  19629  61   
14 02 09.3  -32 28 08  445   16.08  20993 118   
14 02 11.3  -28 53 33  445   15.83   5761  61   
14 02 18.1  -28 29 20  445   15.62  16976 113   
14 02 22.9  -29 03 00  445   16.28  22158  90   
14 02 34.5  -33 50 49  384   16.70   3839  58   
14 02 35.6  -28 44 55  445   16.81  21358  79   
14 02 35.8  -31 14 59  446   15.80  19205  98   
14 02 43.1  -32 34 19  445   15.45   6991 111   
14 02 44.7  -34 57 45  384   16.40   4125  73   
14 02 46.4  -33 07 26  384   15.72  11273  57   
14 02 50.6  -37 02 24  384   16.54  19169  66   
14 03 04.7  -30 37 57  445   15.75  11684 112   
14 03 14.8  -32 10 59  446   16.11  16985  41   
14 03 24.8  -32 58 16  384   15.49  11610  57   
14 03 28.8  -29 05 20  446   15.65  11260  71   
14 03 40.5  -34 10 58  384   16.45   4474  47   
14 04 02.3  -35 43 25  384   15.08  10420  51   
14 04 16.7  -33 36 48  384   16.58  11458  43   
14 04 29.1  -28 03 08  446   16.28   6948  55   
14 04 32.6  -34 18 17  384   15.80  15930 106   
14 05 09.9  -35 58 51  384   15.62  19012  65   
14 05 31.5  -32 56 05  384   16.36  11762  42   
14 06 25.2  -34 17 14  384   15.60   4840  69   
14 06 43.0  -32 00 57  446   15.81  17046  91   
14 07 02.7  -33 54 07  384   16.73   4125  55   
14 07 24.0  -32 18 35  446   16.12  22511  69   
14 07 34.8  -37 21 42  384   16.32  10654  44   
14 07 40.4  -31 43 37  446   15.64  17605  72   
14 07 50.6  -34 51 27  384   15.96  10296  79   
14 07 56.8  -30 05 56  446   16.02   9050  62   
14 07 59.8  -37 16 45  384   16.28  11456  99   
14 08 37.1  -34 12 15  384   16.96  10219  54   
14 08 56.0  -36 19 57  384   16.28  11100  53   
14 09 03.1  -34 18 58  384   15.72  11337  26   
14 09 16.2  -31 12 13  446   16.47   4172  13   
14 09 53.6  -35 23 28  384   16.10  11369  62   
14 10 06.5  -34 00 39  384   16.37  30000  68   
14 10 08.8  -31 24 31  446   16.12  25700  87   
14 10 11.5  -36 11 29  384   16.27  13154  39   
14 10 18.4  -33 16 13  384   15.47  16151  88   
14 10 48.2  -33 44 47  384   15.00  30212 112   
14 10 48.7  -36 44 11  384   16.24  18759  97   
14 11 01.9  -34 20 08  384   16.90  22947 100   
14 11 17.7  -34 03 21  384   16.77  11146  22   
14 11 26.7  -32 06 05  446   16.34  18513  80   
14 11 34.2  -33 09 19  384   15.65  16048  48   
14 12 32.6  -33 04 23  384   16.44  15729  31   
14 12 38.9  -35 25 50  384   16.28  11579  73   
14 12 53.9  -32 53 03  384   16.91  15003  85   
14 13 00.4  -34 42 49  384   16.76  37950  60   
14 13 00.9  -34 39 09  384   15.87  11196  52   
14 13 10.2  -32 04 38  446   15.90   4334  62   
14 13 14.6  -34 05 58  384   16.53  11410  55   
14 13 23.3  -34 30 47  384   16.75  11199  54   
14 13 31.2  -36 37 43  384   16.21  30392  60   
14 14 05.5  -32 10 06  446   16.48  27822  85   
14 15 11.2  -33 36 45  384   16.30  11427  98   
14 15 48.7  -32 29 44  446   16.44   3823   9   
14 15 55.6  -28 33 45  446   16.75  16898  67   
14 16 38.6  -31 00 09  446   16.29  28461  70   
14 17 51.5  -32 39 53  446   16.79  31473 131   
14 18 06.4  -31 37 21  446   17.14  45265  58   
14 18 35.4  -31 41 01  446   17.01  15894  66   
14 19 13.8  -31 01 52  446   17.16  20616  91   
14 21 15.9  -30 46 14  446   17.35  31472  61   
14 21 20.1  -31 43 40  446   17.07  38635  83   
14 21 34.9  -30 53 51  446   17.01  31718  80   
14 22 16.8  -32 16 54  446   17.07  11846  65   
14 23 47.6  -28 44 19  446   17.02  10749  33   
14 24 07.2  -30 06 03  446   17.05   8879  67   
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