PHOTOIONIZATION MODELS FOR BALQSO PG 0946+301
Nahum Arav
This is a companion paper to the manuscript entitled: ``HST STIS Observations Of PG 0946+301: The Highest Quality UV Spectrum Of A BALQSO'' (Arav et al. 2001; accepted for publication in the ApJ). Here we present photoionization-modeling results for {all} the ionic column density constraints found in these data, most of which we were unable to include in the printed version of the paper.
nh_u_pl2.tex

 

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%




\begin{document}
%\vspace{-1in}

\title{PHOTOIONIZATION MODELS FOR BALQSO PG 0946+301}

%\author{Nahum Arav}

\author{
Nahum Arav\altaffilmark{1,2}, 
Kirk T. Korista\altaffilmark{3},
Martijn de~Kool\altaffilmark{4} 
%Fabrizio Nicastro\altaffilmark{5}
}


\altaffiltext{1}{Astronomy Department, UC Berkeley, Berkeley, 
CA 94720, I:arav@astron.Berkeley.EDU}
\altaffiltext{2}{Physics Department, University of California, Davis, CA 95616}
\altaffiltext{3}{Western Michigan Univ.,Dept. of Physics,1120 Everett Tower, 
Kalamazoo, MI  49008}
\altaffiltext{4}{Research School of Astronomy and Astrophysics, ANU ACT,
 Australia}
%\altaffiltext{5}{Smithsonian Astrophysical Observatory}


\begin{abstract}

This is a companion paper to the manuscript entitled: ``HST STIS
Observations Of PG 0946+301: The Highest Quality UV Spectrum Of A
BALQSO'' (Arav et al. 2001; accepted for publication in the ApJ). Here
we present photoionization-modeling results for {\it all} the ionic
column density constraints found in these data, most of which we
were unable to include in the printed version of the paper.


\end{abstract}

\section{DESCRIPTION}

In the following pages we present photoionization-modeling results
for {\it all} the ionic column densities constraints found in the
HST/STIS spectra of PG 0946+301.  We use the $\vy{N}{H}$/$U$ plane
presentation, applied to optically thin slabs, which is described in
\S~4 of the main paper.  Two incident spectra are used for the CLOUDY
models, the standard Mathews--Ferland  AGN spectrum and a modified
$\alpha$=--2 power-law spectrum which is more consistent with the
observed far UV spectral shape of the PG 0946+301 spectrum. Both
spectra are shown in figure \ref{mf_pl}.  Figures 2--4 show the
results for the modified $\alpha$=--2 power-law spectrum. In figure 2
we include only the hydrogen and helium results, for helium we have an
upper limit which therefore excludes the parameter area above the
curve.  Figure 3 shows results for the available ionic constraints from
8 ``metals.''  Each curve is labeled by its corresponding ion and the
number beneath the label is the $\log(N_{ion})$ constraint.  An *
following the $\log(N_{ion})$ denotes an upper limit (excluding the
parameter area above the curve), otherwise the constraint is a lower
limit (excluding the parameter area below the curve).  The small box
at the center of the plots identifies the area in parameter space
which is fully consistent with 21 ionic constraints, marginally
inconsistent with 3 and is strongly inconsistent with 2 (see \S~4 for
details).  Figure 4 is identical to figure 7 in the main paper.

Figures 5--8 are similar to figures 2--4, using the  
Mathews--Ferland  AGN spectrum. To ease the comparison between results from the 
two incident continua, we left the parameter space box at the same location
as for the power-law spectrum.



\clearpage




\begin{figure}
\centerline{\psfig{file=cloudy_m2_0946_n6_continuum.ps,height=21.0cm,width=21.0cm}}
\caption{Comparison between Mathews--Ferland and a modified $\alpha=-2$ power-law spectrum,
which is consistent with the observed far UV spectral-shape of the PG 0946+301 spectrum.
Ionization potentials for several important ions are marked by short vertical lines.}
\label{mf_pl}
\end{figure}

\begin{figure}
\centerline{\psfig{file=H_He.ps,height=20.0cm,width=20.0cm}}
\caption{The all-important hydrogen constraints and their origin for the 
modified $\alpha=-2$ power-law spectrum.  Also shown is
the \hei\ constraint.}
\label{pl_h}
\end{figure}


\begin{figure}
\centerline{\psfig{file=Carbon.ps,height=10.0cm,width=10cm} 
\psfig{file=Nitrogen.ps,height=10.0cm,width=10cm}}
%\caption{}
%\label{}
\centerline{\psfig{file=Oxygen.ps,height=10.0cm,width=10cm}
\psfig{file=Neon.ps,height=10.0cm,width=10cm}}
\caption{Metal-ion constraints for the 
modified $\alpha=-2$ power-law spectrum, an~*
following the $\log(N_{ion})$ value denotes an upper limit (excluding the
parameter area above the curve), otherwise the constraint is a lower
limit (excluding the parameter area below the curve).  }
\label{pl_metals}
\end{figure}
%\clearpage

\begin{figure}
\centerline{\psfig{file=Silicon.ps,height=10.0cm,width=10cm}
\psfig{file=Phosphorus.ps,height=10.0cm,width=10cm}}
%\caption{}
%\label{}
\centerline{\psfig{file=Sulfur.ps,height=10.0cm,width=10cm}
\psfig{file=Argon.ps,height=10.0cm,width=10cm}}
Fig. 3 continued 
%\caption{Fig. 3 continued }
\label{}
\end{figure}

%\begin{figure}
%\centerline{\psfig{file=Iron.ps,height=12.0cm,width=12.0cm}}
%\caption{.}
%\label{al2}
%\end{figure}

\begin{figure}
\centerline{\psfig{file= most_important_constraints.ps,height=20.0cm,width=20.0cm}}
\caption{Some of the more important ionization constraints from several elements
(identical to Fig.~7 in the main paper).}
\label{pl_fig7}
\end{figure}


%%%%%%%%%%%%%%%%%%%%%%% MF results %%%%%%%%%%%%%%%%%%%%%%%%%


\begin{figure}
\centerline{\psfig{file=mf_H_He.ps,height=20.0cm,width=20.0cm}}
\caption{The all-important hydrogen constraints and their origin for
the Mathews--Ferland spectrum.  Also shown is the \hei\ constraint.}
\label{mf_h}
\end{figure}


\begin{figure}
\centerline{\psfig{file=mf_Carbon.ps,height=10.0cm,width=10cm} 
\psfig{file=mf_Nitrogen.ps,height=10.0cm,width=10cm}}
%\caption{}
%\label{}
\centerline{\psfig{file=mf_Oxygen.ps,height=10.0cm,width=10cm}
\psfig{file=mf_Neon.ps,height=10.0cm,width=10cm}}
\caption{Metal-ion constraints for the Mathews--Ferland spectrum, an~*
following the $\log(N_{ion})$ value denotes an upper limit (excluding the
parameter area above the curve), otherwise the constraint is a lower
limit (excluding the parameter area below the curve).  }
\label{mf_metals}
%\caption{ }
%\label{}
\end{figure}

\begin{figure}
\centerline{\psfig{file=mf_Silicon.ps,height=10.0cm,width=10cm}
\psfig{file=mf_Phosphorus.ps,height=10.0cm,width=10cm}}
%\caption{}
%\label{}
\centerline{\psfig{file=mf_Sulfur.ps,height=10.0cm,width=10cm}
\psfig{file=mf_Argon.ps,height=10.0cm,width=10cm}}
Fig. 6 continued 
%\caption{ }
%\label{}
\end{figure}

%\begin{figure}
%\centerline{\psfig{file=mf_Iron.ps,height=12.0cm,width=12.0cm}}
%\caption{.}
%\label{al2}
%\end{figure}

\begin{figure}
\centerline{\psfig{file=mf_most_important_constraints.ps,height=20.0cm,width=20.0cm}}
\caption{Some of the more important ionization constraints from several elements
for the Mathews--Ferland spectrum. } 
\label{mf_fig7}
\end{figure}







\end{document}
%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%

\begin{table}[htb]
\begin{center}
\begin{tabular}{llll}
\multicolumn{4}{c}{\sc Priority list Summary} 
\\[0.02cm]
\hline
\hline
\multicolumn{1}{c}{Object}
&\multicolumn{1}{c}{Priority}
&\multicolumn{1}{c}{rec exp}
&\multicolumn{1}{c}{motivation}\\
% \\[0.05cm]
\hline
0014-0107  & medium  &  1 hr   &  \aliii\ \civ\ \siiv.,  $C(V)$ and $\tau(V)$   \\
0046+0104  & high    &  1 hr   &  \civ, \siiv, \nv, \Ly   very bright object  \\
0135-0213  &  medium &   1 hr  &  \civ, \siiv     \\
0221-0122  & high    &  1 hr   &  Deep narrow \mgii\ suggestive of good \feii\ and \aliii \\ 
0729+2524  & high    &   1 hr  & \nv\ may give full $C(V)$ and $\tau(V)$      \\ 
0910+2612  & HIGHEST &  4 hrs  &  many excellent lines,  possible line locking    \\ 
0957+2356  & medium  &   1 hr  &  similar to 1603     \\ 
1044+3656  & medium  &   1 hr  &  new lines: \caii, \hei, better S/N for \feii\ lines     \\ 
1150+2819  & high    & 1 hr    &  \civ, \nv, \Ly, \ovi\ + interesting interv metal system  \\ 
\\[0.01cm]
\hline
\hline
\end{tabular}
\end{center}
\end{table} 

\vspace{-.3in}



\begin{figure}
\centerline{\psfig{file=0910_vel_si4_c2_al3_line_lock.ps,height=14.0cm,angle=-90,width=22.0cm}}
\caption{Outflow in velocity presentation, troughs associated with
\cii\ and \aliii\ clearly coincide with the high velocity component of
\siiv\ (both doublet components of \aliii\ are detected).  All the
major \siiv\ troughs are separated by the doublet separation (to
within the accuracy of the observations), which suggest a case of line
locking. }\label{mg2_mg1.ps}
\end{figure}

\begin{figure}
\centerline{\psfig{file=0910_vel_c4_n5_si4.ps,height=14.0cm,angle=-90,width=22.0cm}}
\caption{Comparison in velocity space between the toughs associated with \civ,
\siiv\ and \nv. }\label{mg2_mg1.ps}
\end{figure}


\begin{figure}
\centerline{\psfig{file=0910_vel_c4_o6_h1.ps,height=14.0cm,angle=-90,width=22.0cm}}
\caption{Same as the previous figure  \civ\ \ovi\ and \Ly.} 
\label{mg2_mg1_a.ps}
\end{figure}

%%%%%%%%%%%%%%%%%%%%%%%%%% 1150

%\section{FIRST 1150+2819}

\begin{figure}
\centerline{\psfig{file=1150_spec.ps,height=14.0cm,angle=-90,width=22.0cm}}
\caption{spectrum of FIRST 1150+2819,  main absorption features are marked.
Several strong absorption troughs are associated with the metal line system
at z=1.62 (notably five \feii\ transitions). The marked \civ intervening is not part of the same system.} 
\label{mg2_mg1_a.ps}
\end{figure}




\begin{figure}
\centerline{\psfig{file=1150_vel_c4_o6.ps,height=14.0cm,angle=-90,width=22.0cm}}
\caption{Outflow in velocity presentation,  \civ\ and \ovi\ 
troughs.  The \ovi\ doublet is largely unblended which will greatly assist in a detailed analysis. The \Lyb\ trough is seen at -3500 \kms in this presentation and comparison between it and the \Lya\ trough (see next figure) will determine the real column
density of of \hi} 
\label{mg2_mg1_a.ps}
\end{figure}


\begin{figure}
\centerline{\psfig{file=1150_vel_c4_nv_h1.ps,height=14.0cm,angle=-90,width=22.0cm}}
\caption{Same as the previous figure for  \civ\ \nv\ and \Ly.} 
\label{mg2_mg1_a.ps}
\end{figure}

\begin{figure}
\centerline{\psfig{file=1150_vel_c4_si4.ps,height=14.0cm,angle=-90,width=22.0cm}}
\caption{Marginal evidence for the existence of \siiv.  If it is there
we have an excellent opportunity to get accurate column density for
it.}
\label{mg2_mg1_a.ps}
\end{figure}

\end{document}




