Spectral Statistics and Luminosity Function of a Hard X-ray Complete Sample of Brightest AGNs
K.~\textsc{Shinozaki}$^1
$ Y.~\textsc{Ishisaki}$^1
$ Y.~\textsc{Ueda}$^3
$ Y.~\textsc{Ogasaka}$^4
$ K.~\textsc{Hayashida}$^5
$ H.~\textsc{Awaki}$^6$
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\title{Spectral Statistics and Luminosity Function of a Hard X-ray
Complete Sample of Brightest AGNs}

%\subtitle{Subtitle}    %use this when you want a subtitle

\author{K.~\textsc{Shinozaki}$^1,$\footnote{shino@phys.metro-u.ac.jp}
T.~\textsc{Miyaji}$^2,$
Y.~\textsc{Ishisaki}$^1,$
Y.~\textsc{Ueda}$^3,$
Y.~\textsc{Ogasaka}$^4,$
K.~\textsc{Hayashida}$^5,$
H.~\textsc{Awaki}$^6$
}

\inst{%         %Affiliation, neglected when [addenda] or [errata]
$^1$Experimental Astrophysics Group,
Department of Physics, Tokyo Metropolitan University
Tokyo, Japan\\
$^2$Department of Physics, Carnegie Mellon University\\
$^3$ISAS/JAXA\\
$^4$Department of Astrophysics, Nagoya University\\
$^5$Department of Astrophysics, Osaka University\\
$^6$Department of Physics, Ehime University\\

}


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%Prog.~Theor.~Phys.\ \textbf{XX} (19YY), page.}

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\abst{
Investigating the X-ray luminosity function of AGNs in different redshifts
is very important in understanding growth of super massive black holes in 
centers of galaxies over the cosmological time scale.
As a part of this, we are investigating the statistics of the X-ray spectral 
properties of a complete flux-limited sample of bright AGNs. The purpose
of this investigation is to provide the present-day constraint on the 
evolution of absorbed and unabsorbed AGNs, and to constrain the AGN 
population synthesis model of the total X-ray background.
}

\begin{document}

\maketitle

\begin{figure}[htb]
    \parbox{\halftext}{%   %\def\halftext{.471\textwidth}
      \centerline{\includegraphics[width=6.5cm]
        {plot-lb.eps}}
\caption{Spatial ditribution of AGNs in our two samples. 
Circles denote the Sample-1 (Piccinotti) and Squares denote
the Sample-2 (Grossan).
Dashed lines correspond to b=$\pm 20^{\circ}$, and Dotted region
represents the selected resion for the sample-2.}
    \label{fig:1}}
    \hfill
    \parbox{\halftext}{
      \centerline{\includegraphics[width=5.0cm]
        {piclma5_xlf.eps}}
      \caption{Hard X-ray luminosity function of all AGNs (Square), X-ray
unabsorbed AGNs (Circle), and absorbed AGNs (Triangle).}
    \label{fig:2}}
\end{figure}

We defined 28 AGNs in Picinotti et al. (1982)\cite{rf:1}, as a Sample-1,
selecting the R15 count rate $>$ 1.25 c s$^{-1}$
$\sim 3 \times 10^{-11}$ erg cm$^{-2}$ s$^{-1}$.
The Galactic latitude $\mid$b$\mid < 20^{\circ}$ 
and the LMC region were excluded.
Two sources which are also in Sample-2 were excluded.
This sample covers 65.5 \% of the sky.
We also defined Sample-2, which contains
20 sources from Grossan (1992)\cite{rf:2}.
This sample was selected from the MC-LASS catalog of HEAO-1 A1/A3
sources and with a flux-limit of  $\sim 1.7 \times 10^{-11}$
erg cm$^{-2}$ s$^{-1}$, inside the 55$^{\circ}$-radius from the NEP.
As a result, we selected 48 sources 
as a complete flux-limited sample with $z <$ 0.4 (Fig.~\ref{fig:1}).
Spectral studies have been made using ASCA (14 sources) or XMM-Newton
(22 sources) observations by ourselves, and other 12 sources were 
derived from literature\cite{rf:3}\tocite{rf:11}.
These two samples are also used to calculate a wide range HXLF in Ueda
et al. (2003)\cite{rf:13}.

The spectral measurements enabled us to construct local HXLF for absorbed 
(${\rm Log}\,N_{\rm H}[{\rm cm^{-2}}]> 21.5$) and 
unabsorbed AGNs separately. We calculated each HXLF with the conventional
$\Sigma V_{\rm a}^{-1}$ method\cite{rf:12} (Fig.~\ref{fig:2}).
We found a high luminosity cut-off for the HXLF of the absorbed AGNs
compared with those of unabsorbed AGNs and all AGNs.
In the $L_{\rm x}-N_{\rm H}$ plot (Fig.~\ref{fig:3}), there are no AGNs
in the region where ${\rm Log}\,L_{\rm X} [\rm erg/s]> 44.5$ and 
${\rm Log}\,N_{\rm H}[\rm cm^{-2}]> 21.5$. We would have 9-10 AGNs
in this region if the shapes of the absorbed and unabsorbed AGN HXLF
were identical.
We found that the observed flux with ASCA or XMM-Newton was smaller
than that with HEAO-1 by a factor of 0.42 on average, which was expected
for re-observation of sources with a variability-amplitude of a factor 
$\sim$2.6 (Fig.~\ref{fig:4}).

\begin{figure}[htb]
    \parbox{\halftext}{%   %\def\halftext{.471\textwidth}
      \centerline{\includegraphics[width=5.0cm]
        {hxlf_shino5-3.eps}}
\caption{Relation between hard X-ray luminosity and intrinsic $N_{\rm H}$.}
    \label{fig:3}}
    \hfill
    \parbox{\halftext}{
      \centerline{\includegraphics[width=5.0cm]
        {hxlf_shino5-5.eps}}
      \caption{Comparison of observed flux between ASCA or XMM-Newton, and HEAO-1.}
    \label{fig:4}}
\end{figure}


%\section*{Acknowledgements}
%We would like to thank ...........


%\appendix
%\section{First Appendix} %Empty argument \section{} yields `Appendix'. 
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%\section{Second Appendix}


\begin{thebibliography}{99}
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%    \ANN  : Ann. of Phys.           \NPA, \NPB  : Nucl. Phys. [A,B]
%    \CMP  : Commun. Math. Phys.     \PLA, \PLB  : Phys. Lett. [A,B]
%    \IJMP : Int. J. Mod. Phys.      \PRA - \PRE : Phys. Rev. [A-E]     
%    \JHEP : J. High Energy Phys.    \PRL        : Phys. Rev. Lett.
%    \JMP  : J. Math. Phys.          \PRP        : Phys. Rep.
%    \JP   : J. of Phys.             \PTP        : Prog. Theor. Phys.     
%    \JPSJ : J. Phys. Soc. Jpn.      \PTPS       : Prog. Theor. Phys. Suppl.
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%  \JL{Nature,418,2002,123}   ==> Nature \textbf{418} (2002), 123
%  \andvol{B123,1995,1020}    ==> \textbf{B123} (1995), 1020
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\bibitem{rf:1}
Piccinotti, G., Mushotzky, R.F., Boldt, E.A., et al. \AJ{1982, 253, 485}
\bibitem{rf:2}
Grossan B.A. 1992, PhD Thesis,MIT
\bibitem{rf:3}
Reynolds, C.S. Royal Astronomical Society, Monthly Notices, 1997, 286, 513
\bibitem{rf:4}
Turner, T.J., George, I.M., Nandra, K., and Mushotzky, R.F. Astrophys. J. Supplement, 1997, 113, 23
\bibitem{rf:5}
Guainazzi, M. Astronomy and Astrophys, 2003, 401, 903
\bibitem{rf:6}
George, I.M., Turner, T.J., Netzer, H., et al. Astrophys. J. Supplement, 1998, 114, 73
\bibitem{rf:7}
Blustin, A.J., Branduardi-Raymont, G., Behar, E., et al. Astronomy and Astrophys, 2002, 392, 453
\bibitem{rf:8}
Gondoin, P., Orr, A., and Lumb, D. Astronomy and Astrophys, 2003, 398, 967
\bibitem{rf:9}
Gondoin, P., Orr, A., Lumb, D., and Siddiqui, H.
Astronomy and Astrophys, 2003, 397, 883
\bibitem{rf:10}
Malizia, A., Malaguti, G., Bassani, L., et al.
Astronomy and Astrophys, 2002, 394, 801
\bibitem{rf:11}
Turner, T.J., Netzer, H., and George, I.M. \AJ{1996, 463, 134}
%\bibitem{rf:12}
%Schmidt, M. and Green, R.F.\ \AJ{1983, 269, 352} 
\bibitem{rf:12}
Miyaji, T., Hasinger, G., and Schmidt, M.\ Astronomy and Astrophys 
2001, 369, 49a 
\bibitem{rf:13}
Ueda, Y., Akiyama, M., Ohta, K., and Miyaji, T.\ \AJ{2003, 598, 886}




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astro-ph0402363.extracted_bib
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%    \ANN  : Ann. of Phys.           \NPA, \NPB  : Nucl. Phys. [A,B]
%    \CMP  : Commun. Math. Phys.     \PLA, \PLB  : Phys. Lett. [A,B]
%    \IJMP : Int. J. Mod. Phys.      \PRA - \PRE : Phys. Rev. [A-E]     
%    \JHEP : J. High Energy Phys.    \PRL        : Phys. Rev. Lett.
%    \JMP  : J. Math. Phys.          \PRP        : Phys. Rep.
%    \JP   : J. of Phys.             \PTP        : Prog. Theor. Phys.     
%    \JPSJ : J. Phys. Soc. Jpn.      \PTPS       : Prog. Theor. Phys. Suppl.
% Usage:
%  \PRD{45,1990,345}          ==> Phys.~Rev.\ \textbf{D45} (1990), 345
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%  \andvol{B123,1995,1020}    ==> \textbf{B123} (1995), 1020
%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
  
\bibitem{rf:1}
Piccinotti, G., Mushotzky, R.F., Boldt, E.A., et al. \AJ{1982, 253, 485}
\bibitem{rf:2}
Grossan B.A. 1992, PhD Thesis,MIT
\bibitem{rf:3}
Reynolds, C.S. Royal Astronomical Society, Monthly Notices, 1997, 286, 513
\bibitem{rf:4}
Turner, T.J., George, I.M., Nandra, K., and Mushotzky, R.F. Astrophys. J. Supplement, 1997, 113, 23
\bibitem{rf:5}
Guainazzi, M. Astronomy and Astrophys, 2003, 401, 903
\bibitem{rf:6}
George, I.M., Turner, T.J., Netzer, H., et al. Astrophys. J. Supplement, 1998, 114, 73
\bibitem{rf:7}
Blustin, A.J., Branduardi-Raymont, G., Behar, E., et al. Astronomy and Astrophys, 2002, 392, 453
\bibitem{rf:8}
Gondoin, P., Orr, A., and Lumb, D. Astronomy and Astrophys, 2003, 398, 967
\bibitem{rf:9}
Gondoin, P., Orr, A., Lumb, D., and Siddiqui, H.
Astronomy and Astrophys, 2003, 397, 883
\bibitem{rf:10}
Malizia, A., Malaguti, G., Bassani, L., et al.
Astronomy and Astrophys, 2002, 394, 801
\bibitem{rf:11}
Turner, T.J., Netzer, H., and George, I.M. \AJ{1996, 463, 134}
%\bibitem{rf:12}
%Schmidt, M. and Green, R.F.\ \AJ{1983, 269, 352} 
\bibitem{rf:12}
Miyaji, T., Hasinger, G., and Schmidt, M.\ Astronomy and Astrophys 
2001, 369, 49a 
\bibitem{rf:13}
Ueda, Y., Akiyama, M., Ohta, K., and Miyaji, T.\ \AJ{2003, 598, 886}




\end{thebibliography}