Multiwavelength observations revealing the outbursts of the two soft X-ray transients XTE J1859+226 and XTE J1118+480
S.~Chaty
We report here on multiwavelength observations of the two new soft X-ray transients (SXTs) XTE J1859+226 and XTE J1118+480, which we observed with {HST}/{RXTE}/UKIRT. For XTE J1118+480 we also used {EUVE} since it is located at a very high galactic latitude and suffers from very low extinction. The two sources exhibited very different behaviour. XTE J1859+226 seems quite normal and therefore a good object for testing the accretion mechanisms in place during the outbursts, XTE J1118+480 is much more unusual because it exhibits i) a low X-ray to optical ratio and ii) a strong non-thermal contribution in the radio to optical domain, which is likely to be due to synchrotron emission. We concentrate here on the near-infrared (NIR) and optical observations of these two systems.
integral_sxt.tex
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%% Copyright 1999 Patrick W Daly
%% Max-Planck-Institut f\"ur Aeronomie
%% Max-Planck-Str. 2
%% D-37191 Katlenburg-Lindau
%% Germany
%% E-mail: daly@linmpi.mpg.de
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\title{Multiwavelength observations revealing 
the outbursts of the two soft X-ray transients
XTE J1859+226 and XTE J1118+480}
\author[1]{S.~Chaty}
\author[1]{C.A.~Haswell}
\author[2]{R.I.~Hynes}
\author[3]{C.R.~Shrader}
\author[4]{W.~Cui}
\author[5]{C.W.~Mauche}
\author[1]{A.J.~Norton}
\author[6]{\\ J.-E.~Solheim}
\author[6]{R.~\O stensen}
\author[7]{T.R.~Geballe}
\author[8]{Z.~Ioannou}
\author[9]{A.R.~King}
\affil[1]{Department of Physics and Astronomy, The Open University, 
Milton Keynes,
UK, s.chaty@open.ac.uk}
\affil[2]{Department of Physics and Astronomy, University of Southampton,
Southampton, UK}
\affil[3]{Laboratory for High-Energy Astrophysics, 
NASA Goddard Space Flight Center, Greenbelt, USA}
\affil[4]{Department of
Physics, Purdue University, West Lafayette, IN 47907, USA}
\affil[5]{Lawrence Livermore National Laboratory, L-43, 7000 East Avenue,
Livermore, CA 94550, USA}
\affil[6]{Astrophysics Group, Department of Physics,  
University of Troms\o, Troms\o, Norway}
\affil[7]{Gemini Observatory, 670 N. A'ohoku Place, Hilo, HI 96720, USA}
\affil[8]{Astrophysics Department, University of Texas, Austin,
TX 78718, USA}
\affil[9]{University of Leicester, University Road, Leicester, LE1 7RH, UK}

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\begin{document}

\keywords{stars: individual: XTE J1859+226, XTE J1118+480, X-rays: stars, infrared: stars}

\maketitle

\begin{abstract}

We report here on multiwavelength observations of the two new soft
X-ray transients (SXTs) XTE J1859+226 and XTE J1118+480, which we
observed with {\it HST}/{\it RXTE}/UKIRT.
For XTE J1118+480 we also used {\it EUVE} since it is located 
at a very high galactic latitude and suffers from very
low extinction. The two sources exhibited 
very different behaviour. 
XTE J1859+226 seems quite normal and therefore
a good object for testing the accretion mechanisms in place during
the outbursts, XTE J1118+480 is much more unusual 
because it exhibits i) a low X-ray to optical ratio and ii) 
a strong non-thermal contribution in the
radio to optical domain, which is likely to be due to synchrotron emission.
We concentrate here on the near-infrared (NIR) and optical observations
of these two systems.

\end{abstract}

\section{Introduction}

The SXTs, also called X-ray novae, 
are a class of low mass X-ray binaries (LMXBs), including
GRO J1655--40 and GRO J0422+32. In this class of sources,
more than 70\% are thought to contain Black Holes \citep{charles:1998}.
The compact object accretes
matter through an accretion disk 
from a low-mass star via Roche lobe overflow. The history
of these sources is characterized by long periods of quiescence, 
typically lasting decades, and punctuated by very dramatic 
outbursts, visible at every wavelength, although these
sources are usually discovered in X-rays or the optical, 
and often accompanied by radio activity. 
A prototypical outburst is characterized by 
X-ray emission dominated by thermal emission from the hot inner
accretion disk, and optical emission produced by reprocessing of X-rays.
Two such sources were discovered during the last year: XTE J1859+226
and XTE J1118+480.
Thanks to our override programs with {\it RXTE}/{\it HST}/UKIRT we could get 
early multiwavelength observations of these systems,
and follow the evolution of these systems from outburst
towards their quiescence, 
to get more information on the mechanisms underlying
 their outbursts.
We will describe in Section \ref{1859} the observations 
and results on XTE J1859+226 and in Section \ref{1118}
those on XTE J1118+480.

\section{XTE J1859+226} \label{1859}

The first source, XTE J1859+226, was discovered by ASM/{\it RXTE} on 1999
October 9 \citep{wood:1999}, 
at the galactic coordinates: ($l,b$) = ($54.05 \deg$, $+8.61 \deg$).
This source exhibited a fast rise ($\sim 5$ days) and 
exponential decay ($\sim 23$ days) typical of X-ray novae (see Fig. 1). 
The optical counterpart reached 15th magnitude at its maximum
\citep{garnavich:1999} exhibiting a period of 9.15 +/-
0.05 hr which could be the orbital period \citep{garnavich:2000}. 
\citet{sanchez-fernandez:2000} observed
the quiescent counterpart of the source at a magnitude of 23
and also confirmed this weak photometric modulation.
%with different claimed periods was
%reported, at 6.60, 6.734, 9.15 \& $14.79 \pm 0.05$ hr (\citet{uemura:1999}, 
%\citet{garnavich:2000}).
A strong radio counterpart was detected, but no jet feature
was observed \citep{pooley:1999}. 
The compact object could be a black hole, i) because of the hard
X-ray spectrum which showed a high-soft state in October 1999, described by
a temperature of T $\sim 0.9$ keV and a power-law of photon index 
$\alpha \sim 1.5$,
and ii) because of the presence of high-frequency QPOs ($\geq 100$ Hz),
as in GRS 1915+105, GRO J1655--40, and XTE J1550--564 \citep{Cui:2000}.
The column density was determined as 
$N_{H} \sim 3-8 \times 10^{21} \cmmoinsdeux$ (\citet{markwardt:1999b},
\citet{dalfiume:1999}).
We undertook a multi-epoch multiwavelength program
of observations with {\it HST}/{\it RXTE}/UKIRT
(see lightcurve in Fig. 1).
%\ref{1859_lc}.

	\subsection{Short timescale modulation}

To search for short timescale modulations, we observed
with the HiRAC camera on the Nordic Optical 
Telescope, used in a high speed photometric mode, during the first run of a
new camera operating system. This system allows a fast readout in a windowed
mode. The operating system was developed by R. \O stensen, and converts
existing CCD cameras which are equipped with the Copenhagen University
Observatory controllers into a fast photometer.
On Oct 17 we used an integration time of 5.3 s, readout time of 1.8 s and a
cycle time of 7.5 s, with the object and one reference star. The following
night we had a sample time of 30 s, and used 3 comparison stars.
We detected a faint modulation at 20--24 min (Fig. 2). 
%It is interesting to point out that the ratio between the claimed
%orbital period of $9.15$ hours and this faint modulation is close
%to the ratio predicted by \citet{king:1989} in the
%case of a quasi-periodic oscillation of the mass transfer rate
%below the inner Lagrange point.
This QPO may be the result of hydrodynamic oscillations at the $L_1$ point,
where a comparison with V404 Cyg predicts a value of $0.055 P_{orb}$
compared to the observed value of $0.042 P_{orb}$ \citep{king:1989}.
This modulation was also seen in several sets of data amounting to 
33 hr of optical data with different instruments/telescopes, 
in the NIR with UKIRT \citep{hynes:1999},
and much later in the outburst by \cite{charles:2000}.
No periodic modulation was seen in the NIR at shorter timescales.


	\subsection{Evolution of the Spectral Energy Distribution}

The early spectral energy distribution (SED)
observed by {\it HST} \& UKIRT (see Fig. 3) is well fitted
by a typical X-ray irradiated disk model ($T \propto R^{-3/7}$).
The model used was actually generated to fit the SED of GRO J0422+32
in outburst, which has an orbital period of 5.1 hr, and then
scaled to fit the new data with no other adjustment.
This suggests that XTE J1859+226 is also a relatively short 
period system (less than one day).
If the disk were heated by viscous processes instead of irradiation
we would expect intead to see $f_{\nu} \propto \nu^{1/3}$ 
(corresponding to $T\propto R^{-3/4}$).
Gratifyingly, this is seen in our last visit where the SED is
better fitted by a viscously heated accretion disk model 
with an edge temperature of $\sim 8000$ K,
suggesting evolution from an irradiation dominated to viscosity
dominated regime.

\section{XTE J1118+480} \label{1118}

The second source, XTE J1118+480, is a very unusual object, 
and therefore certainly very interesting.
Its galactic coordinates are ($l,b$) = ($157.62\deg$,$+62.32\deg$).
The X-ray object was discovered by {\it RXTE} on 2000 March 29 
\citep{remillard:2000} as a weak, slowly rising source, 
the post-analysis revealing
an outburst in January 2000, with a similar brightness (see Fig. 4).
The optical counterpart is a 13th magnitude star, coincident with a 18.8 mag
object in the DSS \citep{uemura:2000}.
Its optical spectrum was typical
of X-ray novae in outburst \citep{garcia:2000}.
This system was characterized by a very low X-ray to optical flux ratio
of 5 (see \citet{remillard:2000} \& \citet{uemura:2000}),
when the typical value is 500 (see e.g. \citet{tanaka:1996}).
A weak photometric modulation on 4.1 hr (0.17082 d) 
period was rapidly discovered \citep{cook:2000}, which was associated
with the orbital period, the shortest among the black hole
candidates. 
Flickering with an amplitude of $\sim 0.4$ mag,
and also a quasi-periodic oscillation (QPO) 
at 10 s, was observed in the optical, in the UV
\citep{haswell:2000c} and also in the X-rays, with an evolving frequency
\citep{wood:2000}.
A faint radio counterpart was detected at 6.2 mJy, but no jet feature
could be spatially resolved.
The large value of the mass function, f(M) = 5.9 +/- 0.4 solar masses,
suggests that the compact object is a black hole (\citet{wagner:2000} \&
\citet{mcclintock:2000a}).
%The compact object could be a black hole, i) because of the hard
%X-ray spectrum, and also ii) because of the absence of cut-off at high-energy
%\citep{mcclintock:2000}
%like in the spectra of neutron star systems \citep{barret:2000},
%and finally iii) because of the non-detection of high frequency variability 
%	($> 100$ Hz) which is thought to be the signature of neutron
%stars \citep{revnivtsev:2000}.

Its location at an unusually high galactic latitude ($b=+62 \deg$)
%close to the Lockman Hole 
at an estimated distance of $0.8 \kpc$
\citep{mcclintock:2000}
%$\geq 1.5 \kpc$ \citep{uemura:2000}
implied that there is a very low absorption along the line of sight
of the source, with a column density estimated to
$N_{H} \sim 0.75-1.3 \times 10^{20} \cmmoinsdeux$ (\citet{hynes:2000},
\citet{mcclintock:2000}).
Triggering our multi-epoch multiwavelength program
 with {\it HST}/{\it RXTE}/UKIRT and requesting Director's Discretionary
{\it EUVE} observations,
we got unprecedented broadband 
coverage (see lightcurve in Fig. \ref{1118_lc} \& SED in Fig. 6,
more details in \cite{hynes:2000}).
%\ref{1118_sed}). 
The SED suggests that the system was
exhibiting a low-state mini-outburst, with the inner radius
of the accretion disk at $\sim 2000 R_s$ ($R_s$: Schwarzschild
radius).
One of the most striking features 
was the strong non-thermal (likely synchrotron)
contribution
in the optical and NIR wavelengths.
Indeed, the SED shows a very flat spectrum from the NIR to the
UV ($\sim 1000  - 50\,000 \AA$),
suggesting that there is another source of NIR flux apart from thermal
disk emission, likely related to radio emission, and therefore
possibly synchrotron.


	\subsection{Non-thermal contribution}

The $\sim 10$ s QPO was also seen in the UV, implying a common
nature for this QPO from the optical to the X-rays.
We looked for a rapid periodicity in the NIR wavelengths,
and we therefore observed with the 
3.8-m U.K. Infrared Telescope and IRCAM3 instrument on 
June 24.23 UT when the source was at K = 11.512 +/-- 0.004 and 
on July 15.25 UT, when the source was at K = 11.948 +/-- 0.006.
The 0.02 mag/day mean decline between these two dates was 
therefore much stronger than from April to June
\citep{hynes:2000}, and
comparable to the 0.015 mag/day mean decline seen in the optical
(VSNET observations).
During both observations we took rapid photometric observations
for nearly 1 hour, with 2 s integration time on the source
and nearly 7 s sampling time. The source showed rapid fluctuations
through nearly 0.5 mag, with a 0.05 mag error bar for each individual
frame. A periodicity search analysis in both runs
did not show any secure quasi-periodic oscillation,
although there could be some modulations around 35 s.
Unfortunately our sampling time could not address the presence
or absence of the periodicity of 10 s seen in the optical and in
the X-rays.

However, we could detect flickering at NIR wavelengths, of bigger
amplitude ($\sim 0.8$ mag) than in the optical ($\sim 0.4$ mag).
This flickering in the K band is reported in Figure 5.
We also took a NIR K-band spectrum of this source using the
CGS 4 instrument and a $0.6 \asec$ slit
on June, 27.2 UT, which was featureless, also consistent with the fact
that the disk is not the only source of emission in this part of the spectrum.
These two facts suggest a strong non-thermal (likely synchrotron) emission in
the NIR wavelengths.
This is consistent with the flat slope of 
the SED, shown in Figure 6
%\ref{1118_sed}
from the radio to the IR, and will be developed in Chaty et al. (in prep.).

\subsection{The nature of the system}

In our {\it HST} UV spectra we observed a complete absence
of carbon and oxygen lines, suggesting that the material
accreted from the companion star has undergone significant
CNO-cycle processing resulting in C and O depletion \citep{haswell:2000b}.
Since a 4 hr binary would normally be thought to contain an M dwarf
companion, no CNO processing would be expected.
Therefore it is likely that the companion star is the core of
a larger star that has lost its envelope: a stripped giant.
To test this hypothesis and try to reveal the nature 
of the companion star of the system, we will need to observe this source
in quiescence with spectroscopic
observations, at both optical and NIR wavelengths.

\section{Conclusions}

XTE J1859+226 allows us to study the accretion mechanisms 
during the outburst and the changes in temperature distribution
due to irradiation.
XTE J1118+480 allowed us to get
broadband coverage from the radio to the X-rays, showing 
that it was exhibiting a very low-state mini-outburst,
with a strong non-thermal (likely synchrotron) contribution.


\section*{acknowledgements} 
S.C. is very grateful to the UKIRT staff for their availability and skills
to perform service observations for override programs,
and in particular to John Davies, Sandy Leggett and Andy Adamson.
We thank {\it HST/STScI} and {\it RXTE} staff for ongoing effort in these
multi-epoch campaigns, and {\it EUVE} staff for the DD observations.
S.C., C.A.H. R.I.H. and A.R.K. acknowledge
support from grant F/00-180/A from the Leverhulme Trust.

   \bibliographystyle{aa}
   \bibliography{science}
% The results are inserted directly here to simplify
% the demonstration.

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%---------------------------------------------------------------------------
\begin{figure}
\centerline{\psfig{file=multilc_colour.ps,angle=0.,width=7.cm}}
%\vspace*{-3.cm}
{\bf Figure 1 -- The Outburst History:}
{\small \it Respectively from top to bottom are shown: {\it RXTE}/ASM 2-12 keV counts, {\it HST}/STIS 
1450 Angstr\"oms, Keele V, and UKIRT K bands.
%and radio flux densities (mJy).
%The radio comes from Hjellming, 1999, private communication.
} \label{1859_lc}
\end{figure}
%---------------------------------------------------------------------------

%\vspace*{-1.cm}

%---------------------------------------------------------------------------
\begin{figure}
\centerline{\psfig{file=NOTperiod.ps,angle=-90.,width=7.cm}}
%%\vspace*{-1.2cm}
{\bf Figure 2 -- Periodicities:}
{\small \it A $\sim 23$ min periodicity (frequency $\sim 62$ per day)
was seen in the Nordic Optical Telescope
data acquired on 1999 October 17--18th, perhaps 
related to a Lagrange point oscillation.} \label{1859_not}
\end{figure}
%---------------------------------------------------------------------------

%\vspace*{-1.cm}

%---------------------------------------------------------------------------
\begin{figure}
\centerline{\psfig{file=allsed.ps,angle=+90.,width=7.cm}}
%%\vspace*{-1.cm}
{\bf Figure 3 -- The irradiation view:}
{\small \it Note the change from an irradiated spectrum during the outburst
(top curves) to a viscously heated disk after the outburst
(bottom curve).} \label{1859_ir}
\end{figure}
%---------------------------------------------------------------------------

%\vspace*{-1.cm}

%---------------------------------------------------------------------------
\begin{figure}
\centerline{\psfig{file=tout.ps,angle=90.,width=8.cm}}
%%\vspace*{-1.cm}
{\bf Figure 4 -- The Outburst History:}
{\small \it {\it RXTE}/ASM 2-12 keV counts (top) \& UKIRT K bands (bottom).
%, optical VSNET magnitudes and radio flux densities (mJy).
%The radio comes from Hjellming, 2000, private communication.
} \label{1118_lc}
\end{figure}
%---------------------------------------------------------------------------

%---------------------------------------------------------------------------
%\begin{figure}
%\centerline{\psfig{file=/usr/home/schaty/Sources/Xtej1118/uvpds.ps,angle=90.,width=8.cm}}
%%\vspace*{-1.cm}
%{\bf QPO:}
%{\tiny \it $\sim 10s$ QPO in the UV as seen by {\it HST}/STIS.}
%\end{figure}
%---------------------------------------------------------------------------

%\vspace*{-1.cm}

%---------------------------------------------------------------------------
\begin{figure}
\centerline{\psfig{file=xte1118_color.ps,angle=90.,width=8.cm}}
%%\vspace*{-1.cm}
{\bf Figure 5 -- IR Flickering:}
{\small \it Significant Flickering as seen in K band with UKIRT, on a 0.8 mag amplitude
with error bars of only 0.1 mag.} \label{1118_flick}
\end{figure}
%---------------------------------------------------------------------------

%\vspace*{-1.cm}

%---------------------------------------------------------------------------
\begin{figure}
\centerline{\psfig{file=fig3.ps,angle=90.,width=8.cm}}
%%\vspace*{-1.5cm}
{\bf Figure 6 -- \small Spectral Energy Distribution:}
{\small \it The {\it EUVE} fluxes are corrected with $N_H = 0.35, 0.75, \& 1.15 \times
10^{20} \cmmoinsdeux$. Dashed lines: two steady-state
disk models with an outer disk layer  at 8000K and internal disk
layer at 2000 Rs (model A) and 3 Rs (model B).
Dotted lines: different power laws, with spectral indices of 0.5,
0.0 and -0.8 \citep{hynes:2000}.} \label{1118_sed}
\end{figure}
%---------------------------------------------------------------------------

%---------------------------------------------------------------------------
%\begin{figure}
%\centerline{\psfig{file=/usr/home/schaty/Sources/Xtej1118/multi_uv_spec.ps,angle=90.,width=8.cm}}
%%\vspace*{-1.8cm}
%{\bf CNO Process:}
%{\tiny \it Note the absence of C IV emission in the case of XTE J1118+480 in
%comparison with the more normal SXT XTE J1859+226. The CNO seems
%therefore processed in XTE J1118+480, which suggests that 
%this source is a more evolved system than the usual SXT.}
%\end{figure}
%---------------------------------------------------------------------------

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%
\def\ps@dir{/}
\def\ExistsFile#1#2{%
   \openin1=\ps@predir#1\ps@dir#2
   \ifeof1
       \closein1
       %\ps@typeout{...not: \ps@predir#1\ps@dir#2}
   \else
       \closein1
       %\ps@typeout{...in:  \ps@predir#1\ps@dir#2}
        \ifx\ps@founddir\leer
          %\ps@typeout{set founddir #1}
           \edef\ps@founddir{#1}
        \fi
   \fi}
%------------------------------------------------------
%
% Get dir in path or error
%
\def\get@dir#1{%
  \def\ps@founddir{}
  \def\SearchedFile{#1}
  \DoPaths\figurepath
%  \fi
}
%------------------------------------------------------
%%% END of Searching Unixpaths


%
% @psdo control structure -- similar to Latex @for.
% I redefined these with different names so that psfig can
% be used with TeX as well as LaTeX, and so that it will not 
% be vunerable to future changes in LaTeX's internal
% control structure,
%
\def\@nnil{\@nil}
\def\@empty{}
\def\@psdonoop#1\@@#2#3{}
\def\@psdo#1:=#2\do#3{\edef\@psdotmp{#2}\ifx\@psdotmp\@empty \else
    \expandafter\@psdoloop#2,\@nil,\@nil\@@#1{#3}\fi}
\def\@psdoloop#1,#2,#3\@@#4#5{\def#4{#1}\ifx #4\@nnil \else
       #5\def#4{#2}\ifx #4\@nnil \else#5\@ipsdoloop #3\@@#4{#5}\fi\fi}
\def\@ipsdoloop#1,#2\@@#3#4{\def#3{#1}\ifx #3\@nnil 
       \let\@nextwhile=\@psdonoop \else
      #4\relax\let\@nextwhile=\@ipsdoloop\fi\@nextwhile#2\@@#3{#4}}
\def\@tpsdo#1:=#2\do#3{\xdef\@psdotmp{#2}\ifx\@psdotmp\@empty \else
    \@tpsdoloop#2\@nil\@nil\@@#1{#3}\fi}
\def\@tpsdoloop#1#2\@@#3#4{\def#3{#1}\ifx #3\@nnil 
       \let\@nextwhile=\@psdonoop \else
      #4\relax\let\@nextwhile=\@tpsdoloop\fi\@nextwhile#2\@@#3{#4}}
% 
% \fbox is defined in latex.tex; so if \fbox is undefined, assume that
% we are not in LaTeX.
% Perhaps this could be done better???
\ifx\undefined\fbox
% \fbox code from modified slightly from LaTeX
\newdimen\fboxrule
\newdimen\fboxsep
\newdimen\ps@tempdima
\newbox\ps@tempboxa
\fboxsep = 3pt
\fboxrule = .4pt
\long\def\fbox#1{\leavevmode\setbox\ps@tempboxa\hbox{#1}\ps@tempdima\fboxrule
    \advance\ps@tempdima \fboxsep \advance\ps@tempdima \dp\ps@tempboxa
   \hbox{\lower \ps@tempdima\hbox
  {\vbox{\hrule height \fboxrule
          \hbox{\vrule width \fboxrule \hskip\fboxsep
          \vbox{\vskip\fboxsep \box\ps@tempboxa\vskip\fboxsep}\hskip 
                 \fboxsep\vrule width \fboxrule}
                 \hrule height \fboxrule}}}}
\fi
%
%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
% file reading stuff from epsf.tex
%   EPSF.TEX macro file:
%   Written by Tomas Rokicki of Radical Eye Software, 29 Mar 1989.
%   Revised by Don Knuth, 3 Jan 1990.
%   Revised by Tomas Rokicki to accept bounding boxes with no
%      space after the colon, 18 Jul 1990.
%   Portions modified/removed for use in PSFIG package by
%      J. Daniel Smith, 9 October 1990.
%
\newread\ps@stream
\newif\ifnot@eof       % continue looking for the bounding box?
\newif\if@noisy        % report what you're making?
\newif\if@atend        % %%BoundingBox: has (at end) specification
\newif\if@psfile       % does this look like a PostScript file?
%
% PostScript files should start with `%!'
%
{\catcode`\%=12\global\gdef\epsf@start{%!}}
\def\epsf@PS{PS}
%
\def\epsf@getbb#1{%
%
%   The first thing we need to do is to open the
%   PostScript file, if possible.
%
\openin\ps@stream=\ps@predir#1
\ifeof\ps@stream\ps@typeout{Error, File #1 not found}\else
%
%   Okay, we got it. Now we'll scan lines until we find one that doesn't
%   start with %. We're looking for the bounding box comment.
%
   {\not@eoftrue \chardef\other=12
    \def\do##1{\catcode`##1=\other}\dospecials \catcode`\ =10
    \loop
       \if@psfile
	  \read\ps@stream to \epsf@fileline
       \else{
	  \obeyspaces
          \read\ps@stream to \epsf@tmp\global\let\epsf@fileline\epsf@tmp}
       \fi
       \ifeof\ps@stream\not@eoffalse\else
%
%   Check the first line for `%!'.  Issue a warning message if its not
%   there, since the file might not be a PostScript file.
%
       \if@psfile\else
       \expandafter\epsf@test\epsf@fileline:. \\%
       \fi
%
%   We check to see if the first character is a % sign;
%   if so, we look further and stop only if the line begins with
%   `%%BoundingBox:' and the `(atend)' specification was not found.
%   That is, the only way to stop is when the end of file is reached,
%   or a `%%BoundingBox: llx lly urx ury' line is found.
%
          \expandafter\epsf@aux\epsf@fileline:. \\%
       \fi
   \ifnot@eof\repeat
   }\closein\ps@stream\fi}%
%
% This tests if the file we are reading looks like a PostScript file.
%
\long\def\epsf@test#1#2#3:#4\\{\def\epsf@testit{#1#2}
			\ifx\epsf@testit\epsf@start\else
\ps@typeout{Warning! File does not start with `\epsf@start'.  It may not be a PostScript file.}
			\fi
			\@psfiletrue} % don't test after 1st line
%
%   We still need to define the tricky \epsf@aux macro. This requires
%   a couple of magic constants for comparison purposes.
%
{\catcode`\%=12\global\let\epsf@percent=%\global\def\epsf@bblit{%BoundingBox}}
%
%
%   So we're ready to check for `%BoundingBox:' and to grab the
%   values if they are found.  We continue searching if `(at end)'
%   was found after the `%BoundingBox:'.
%
\long\def\epsf@aux#1#2:#3\\{\ifx#1\epsf@percent
   \def\epsf@testit{#2}\ifx\epsf@testit\epsf@bblit
	\@atendfalse
        \epsf@atend #3 . \\%
	\if@atend	
	   \if@verbose{
		\ps@typeout{psfig: found `(atend)'; continuing search}
	   }\fi
        \else
        \epsf@grab #3 . . . \\%
        \not@eoffalse
        \global\no@bbfalse
        \fi
   \fi\fi}%
%
%   Here we grab the values and stuff them in the appropriate definitions.
%
\def\epsf@grab #1 #2 #3 #4 #5\\{%
   \global\def\epsf@llx{#1}\ifx\epsf@llx\empty
      \epsf@grab #2 #3 #4 #5 .\\\else
   \global\def\epsf@lly{#2}%
   \global\def\epsf@urx{#3}\global\def\epsf@ury{#4}\fi}%
%
% Determine if the stuff following the %%BoundingBox is `(atend)'
% J. Daniel Smith.  Copied from \epsf@grab above.
%
\def\epsf@atendlit{(atend)} 
\def\epsf@atend #1 #2 #3\\{%
   \def\epsf@tmp{#1}\ifx\epsf@tmp\empty
      \epsf@atend #2 #3 .\\\else
   \ifx\epsf@tmp\epsf@atendlit\@atendtrue\fi\fi}


% End of file reading stuff from epsf.tex
%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%

%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
% trigonometry stuff from "trig.tex"
\chardef\psletter = 11 % won't conflict with \begin{letter} now...
\chardef\other = 12

\newif \ifdebug %%% turn me on to see TeX hard at work ...
\newif\ifc@mpute %%% don't need to compute some values
\c@mputetrue % but assume that we do

\let\then = \relax
\def\r@dian{pt }
\let\r@dians = \r@dian
\let\dimensionless@nit = \r@dian
\let\dimensionless@nits = \dimensionless@nit
\def\internal@nit{sp }
\let\internal@nits = \internal@nit
\newif\ifstillc@nverging
\def \Mess@ge #1{\ifdebug \then \message {#1} \fi}

{ %%% Things that need abnormal catcodes %%%
	\catcode `\@ = \psletter
	\gdef \nodimen {\expandafter \n@dimen \the \dimen}
	\gdef \term #1 #2 #3%
	       {\edef \t@ {\the #1}%%% freeze parameter 1 (count, by value)
		\edef \t@@ {\expandafter \n@dimen \the #2\r@dian}%
				   %%% freeze parameter 2 (dimen, by value)
		\t@rm {\t@} {\t@@} {#3}%
	       }
	\gdef \t@rm #1 #2 #3%
	       {{%
		\count 0 = 0
		\dimen 0 = 1 \dimensionless@nit
		\dimen 2 = #2\relax
		\Mess@ge {Calculating term #1 of \nodimen 2}%
		\loop
		\ifnum	\count 0 < #1
		\then	\advance \count 0 by 1
			\Mess@ge {Iteration \the \count 0 \space}%
			\Multiply \dimen 0 by {\dimen 2}%
			\Mess@ge {After multiplication, term = \nodimen 0}%
			\Divide \dimen 0 by {\count 0}%
			\Mess@ge {After division, term = \nodimen 0}%
		\repeat
		\Mess@ge {Final value for term #1 of 
				\nodimen 2 \space is \nodimen 0}%
		\xdef \Term {#3 = \nodimen 0 \r@dians}%
		\aftergroup \Term
	       }}
	\catcode `\p = \other
	\catcode `\t = \other
	\gdef \n@dimen #1pt{#1} %%% throw away the ``pt''
}

\def \Divide #1by #2{\divide #1 by #2} %%% just a synonym

\def \Multiply #1by #2%%% allows division of a dimen by a dimen
       {{%%% should really freeze parameter 2 (dimen, passed by value)
	\count 0 = #1\relax
	\count 2 = #2\relax
	\count 4 = 65536
	\Mess@ge {Before scaling, count 0 = \the \count 0 \space and
			count 2 = \the \count 2}%
	\ifnum	\count 0 > 32767 %%% do our best to avoid overflow
	\then	\divide \count 0 by 4
		\divide \count 4 by 4
	\else	\ifnum	\count 0 < -32767
		\then	\divide \count 0 by 4
			\divide \count 4 by 4
		\else
		\fi
	\fi
	\ifnum	\count 2 > 32767 %%% while retaining reasonable accuracy
	\then	\divide \count 2 by 4
		\divide \count 4 by 4
	\else	\ifnum	\count 2 < -32767
		\then	\divide \count 2 by 4
			\divide \count 4 by 4
		\else
		\fi
	\fi
	\multiply \count 0 by \count 2
	\divide \count 0 by \count 4
	\xdef \product {#1 = \the \count 0 \internal@nits}%
	\aftergroup \product
       }}

\def\r@duce{\ifdim\dimen0 > 90\r@dian \then   % sin(x+90) = sin(180-x)
		\multiply\dimen0 by -1
		\advance\dimen0 by 180\r@dian
		\r@duce
	    \else \ifdim\dimen0 < -90\r@dian \then  % sin(-x) = sin(360+x)
		\advance\dimen0 by 360\r@dian
		\r@duce
		\fi
	    \fi}

\def\Sine#1%
       {{%
	\dimen 0 = #1 \r@dian
	\r@duce
	\ifdim\dimen0 = -90\r@dian \then
	   \dimen4 = -1\r@dian
	   \c@mputefalse
	\fi
	\ifdim\dimen0 = 90\r@dian \then
	   \dimen4 = 1\r@dian
	   \c@mputefalse
	\fi
	\ifdim\dimen0 = 0\r@dian \then
	   \dimen4 = 0\r@dian
	   \c@mputefalse
	\fi
%
	\ifc@mpute \then
        	% convert degrees to radians
		\divide\dimen0 by 180
		\dimen0=3.141592654\dimen0
%
		\dimen 2 = 3.1415926535897963\r@dian %%% a well-known constant
		\divide\dimen 2 by 2 %%% we only deal with -pi/2 : pi/2
		\Mess@ge {Sin: calculating Sin of \nodimen 0}%
		\count 0 = 1 %%% see power-series expansion for sine
		\dimen 2 = 1 \r@dian %%% ditto
		\dimen 4 = 0 \r@dian %%% ditto
		\loop
			\ifnum	\dimen 2 = 0 %%% then we've done
			\then	\stillc@nvergingfalse 
			\else	\stillc@nvergingtrue
			\fi
			\ifstillc@nverging %%% then calculate next term
			\then	\term {\count 0} {\dimen 0} {\dimen 2}%
				\advance \count 0 by 2
				\count 2 = \count 0
				\divide \count 2 by 2
				\ifodd	\count 2 %%% signs alternate
				\then	\advance \dimen 4 by \dimen 2
				\else	\advance \dimen 4 by -\dimen 2
				\fi
		\repeat
	\fi		
			\xdef \sine {\nodimen 4}%
       }}

% Now the Cosine can be calculated easily by calling \Sine
\def\Cosine#1{\ifx\sine\UnDefined\edef\Savesine{\relax}\else
		             \edef\Savesine{\sine}\fi
	{\dimen0=#1\r@dian\advance\dimen0 by 90\r@dian
	 \Sine{\nodimen 0}
	 \xdef\cosine{\sine}
	 \xdef\sine{\Savesine}}}	      
% end of trig stuff
%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%

\def\psdraft{
	\def\@psdraft{0}
	%\ps@typeout{draft level now is \@psdraft \space . }
}
\def\psfull{
	\def\@psdraft{100}
	%\ps@typeout{draft level now is \@psdraft \space . }
}

\psfull

\newif\if@scalefirst
\def\psscalefirst{\@scalefirsttrue}
\def\psrotatefirst{\@scalefirstfalse}
\psrotatefirst

\newif\if@draftbox
\def\psnodraftbox{
	\@draftboxfalse
}
\def\psdraftbox{
	\@draftboxtrue
}
\@draftboxtrue

\newif\if@prologfile
\newif\if@postlogfile
\def\pssilent{
	\@noisyfalse
}
\def\psnoisy{
	\@noisytrue
}
\psnoisy
%%% These are for the option list.
%%% A specification of the form a = b maps to calling \@p@@sa{b}
\newif\if@bbllx
\newif\if@bblly
\newif\if@bburx
\newif\if@bbury
\newif\if@height
\newif\if@width
\newif\if@rheight
\newif\if@rwidth
\newif\if@angle
\newif\if@clip
\newif\if@verbose
\def\@p@@sclip#1{\@cliptrue}
%
%
\newif\if@decmpr
%
\def\@p@@sfigure#1{\def\@p@sfile{null}\def\@p@sbbfile{null}\@decmprfalse
   % look directly for file (e.g. absolute path)
   \openin1=\ps@predir#1
   \ifeof1
	\closein1
	% failed, search directories for file
	\get@dir{#1}
	\ifx\ps@founddir\leer
		% failed, search directly for file.bb
		\openin1=\ps@predir#1.bb
		\ifeof1
			\closein1
			% failed, search directories for file.bb
			\get@dir{#1.bb}
			\ifx\ps@founddir\leer
				% failed, lose.
				\ps@typeout{Can't find #1 in \figurepath}
			\else
				% found file.bb in search dir
				\@decmprtrue
				\def\@p@sfile{\ps@founddir\ps@dir#1}
				\def\@p@sbbfile{\ps@founddir\ps@dir#1.bb}
			\fi
		\else
			\closein1
			%found file.bb directly
			\@decmprtrue
			\def\@p@sfile{#1}
			\def\@p@sbbfile{#1.bb}
		\fi
	\else
		% found file in search dir
		\def\@p@sfile{\ps@founddir\ps@dir#1}
		\def\@p@sbbfile{\ps@founddir\ps@dir#1}
	\fi
   \else
	% found file directly
	\closein1
	\def\@p@sfile{#1}
	\def\@p@sbbfile{#1}
   \fi
}
%
%
%
\def\@p@@sfile#1{\@p@@sfigure{#1}}
%
\def\@p@@sbbllx#1{
		%\ps@typeout{bbllx is #1}
		\@bbllxtrue
		\dimen100=#1
		\edef\@p@sbbllx{\number\dimen100}
}
\def\@p@@sbblly#1{
		%\ps@typeout{bblly is #1}
		\@bbllytrue
		\dimen100=#1
		\edef\@p@sbblly{\number\dimen100}
}
\def\@p@@sbburx#1{
		%\ps@typeout{bburx is #1}
		\@bburxtrue
		\dimen100=#1
		\edef\@p@sbburx{\number\dimen100}
}
\def\@p@@sbbury#1{
		%\ps@typeout{bbury is #1}
		\@bburytrue
		\dimen100=#1
		\edef\@p@sbbury{\number\dimen100}
}
\def\@p@@sheight#1{
		\@heighttrue
		\dimen100=#1
   		\edef\@p@sheight{\number\dimen100}
		%\ps@typeout{Height is \@p@sheight}
}
\def\@p@@swidth#1{
		%\ps@typeout{Width is #1}
		\@widthtrue
		\dimen100=#1
		\edef\@p@swidth{\number\dimen100}
}
\def\@p@@srheight#1{
		%\ps@typeout{Reserved height is #1}
		\@rheighttrue
		\dimen100=#1
		\edef\@p@srheight{\number\dimen100}
}
\def\@p@@srwidth#1{
		%\ps@typeout{Reserved width is #1}
		\@rwidthtrue
		\dimen100=#1
		\edef\@p@srwidth{\number\dimen100}
}
\def\@p@@sangle#1{
		%\ps@typeout{Rotation is #1}
		\@angletrue
%		\dimen100=#1
		\edef\@p@sangle{#1} %\number\dimen100}
}
\def\@p@@ssilent#1{ 
		\@verbosefalse
}
\def\@p@@sprolog#1{\@prologfiletrue\def\@prologfileval{#1}}
\def\@p@@spostlog#1{\@postlogfiletrue\def\@postlogfileval{#1}}
\def\@cs@name#1{\csname #1\endcsname}
\def\@setparms#1=#2,{\@cs@name{@p@@s#1}{#2}}
%
% initialize the defaults (size the size of the figure)
%
\def\ps@init@parms{
		\@bbllxfalse \@bbllyfalse
		\@bburxfalse \@bburyfalse
		\@heightfalse \@widthfalse
		\@rheightfalse \@rwidthfalse
		\def\@p@sbbllx{}\def\@p@sbblly{}
		\def\@p@sbburx{}\def\@p@sbbury{}
		\def\@p@sheight{}\def\@p@swidth{}
		\def\@p@srheight{}\def\@p@srwidth{}
		\def\@p@sangle{0}
		\def\@p@sfile{} \def\@p@sbbfile{}
		\def\@p@scost{10}
		\def\@sc{}
		\@prologfilefalse
		\@postlogfilefalse
		\@clipfalse
		\if@noisy
			\@verbosetrue
		\else
			\@verbosefalse
		\fi
}
%
% Go through the options setting things up.
%
\def\parse@ps@parms#1{
	 	\@psdo\@psfiga:=#1\do
		   {\expandafter\@setparms\@psfiga,}}
%
% Compute bb height and width
%
\newif\ifno@bb
\def\bb@missing{
	\if@verbose{
		\ps@typeout{psfig: searching \@p@sbbfile \space  for bounding box}
	}\fi
	\no@bbtrue
	\epsf@getbb{\@p@sbbfile}
        \ifno@bb \else \bb@cull\epsf@llx\epsf@lly\epsf@urx\epsf@ury\fi
}	
\def\bb@cull#1#2#3#4{
	\dimen100=#1 bp\edef\@p@sbbllx{\number\dimen100}
	\dimen100=#2 bp\edef\@p@sbblly{\number\dimen100}
	\dimen100=#3 bp\edef\@p@sbburx{\number\dimen100}
	\dimen100=#4 bp\edef\@p@sbbury{\number\dimen100}
	\no@bbfalse
}
% rotate point (#1,#2) about (0,0).
% The sine and cosine of the angle are already stored in \sine and
% \cosine.  The result is placed in (\p@intvaluex, \p@intvaluey).
\newdimen\p@intvaluex
\newdimen\p@intvaluey
\def\rotate@#1#2{{\dimen0=#1 sp\dimen1=#2 sp
%            	calculate x' = x \cos\theta - y \sin\theta
		  \global\p@intvaluex=\cosine\dimen0
		  \dimen3=\sine\dimen1
		  \global\advance\p@intvaluex by -\dimen3
% 		calculate y' = x \sin\theta + y \cos\theta
		  \global\p@intvaluey=\sine\dimen0
		  \dimen3=\cosine\dimen1
		  \global\advance\p@intvaluey by \dimen3
		  }}
\def\compute@bb{
		\no@bbfalse
		\if@bbllx \else \no@bbtrue \fi
		\if@bblly \else \no@bbtrue \fi
		\if@bburx \else \no@bbtrue \fi
		\if@bbury \else \no@bbtrue \fi
		\ifno@bb \bb@missing \fi
		\ifno@bb \ps@typeout{FATAL ERROR: no bb supplied or found}
			\no-bb-error
		\fi
		%
%\ps@typeout{BB: \@p@sbbllx, \@p@sbblly, \@p@sbburx, \@p@sbbury} 
%
% store height/width of original (unrotated) bounding box
		\count203=\@p@sbburx
		\count204=\@p@sbbury
		\advance\count203 by -\@p@sbbllx
		\advance\count204 by -\@p@sbblly
		\edef\ps@bbw{\number\count203}
		\edef\ps@bbh{\number\count204}
		%\ps@typeout{ psbbh = \ps@bbh, psbbw = \ps@bbw }
		\if@angle 
			\Sine{\@p@sangle}\Cosine{\@p@sangle}
	        	{\dimen100=\maxdimen\xdef\r@p@sbbllx{\number\dimen100}
					    \xdef\r@p@sbblly{\number\dimen100}
			                    \xdef\r@p@sbburx{-\number\dimen100}
					    \xdef\r@p@sbbury{-\number\dimen100}}
%
% Need to rotate all four points and take the X-Y extremes of the new
% points as the new bounding box.
                        \def\minmaxtest{
			   \ifnum\number\p@intvaluex<\r@p@sbbllx
			      \xdef\r@p@sbbllx{\number\p@intvaluex}\fi
			   \ifnum\number\p@intvaluex>\r@p@sbburx
			      \xdef\r@p@sbburx{\number\p@intvaluex}\fi
			   \ifnum\number\p@intvaluey<\r@p@sbblly
			      \xdef\r@p@sbblly{\number\p@intvaluey}\fi
			   \ifnum\number\p@intvaluey>\r@p@sbbury
			      \xdef\r@p@sbbury{\number\p@intvaluey}\fi
			   }
%			lower left
			\rotate@{\@p@sbbllx}{\@p@sbblly}
			\minmaxtest
%			upper left
			\rotate@{\@p@sbbllx}{\@p@sbbury}
			\minmaxtest
%			lower right
			\rotate@{\@p@sbburx}{\@p@sbblly}
			\minmaxtest
%			upper right
			\rotate@{\@p@sbburx}{\@p@sbbury}
			\minmaxtest
			\edef\@p@sbbllx{\r@p@sbbllx}\edef\@p@sbblly{\r@p@sbblly}
			\edef\@p@sbburx{\r@p@sbburx}\edef\@p@sbbury{\r@p@sbbury}
%\ps@typeout{rotated BB: \r@p@sbbllx, \r@p@sbblly, \r@p@sbburx, \r@p@sbbury}
		\fi
		\count203=\@p@sbburx
		\count204=\@p@sbbury
		\advance\count203 by -\@p@sbbllx
		\advance\count204 by -\@p@sbblly
		\edef\@bbw{\number\count203}
		\edef\@bbh{\number\count204}
		%\ps@typeout{ bbh = \@bbh, bbw = \@bbw }
}
%
% \in@hundreds performs #1 * (#2 / #3) correct to the hundreds,
%	then leaves the result in @result
%
\def\in@hundreds#1#2#3{\count240=#2 \count241=#3
		     \count100=\count240	% 100 is first digit #2/#3
		     \divide\count100 by \count241
		     \count101=\count100
		     \multiply\count101 by \count241
		     \advance\count240 by -\count101
		     \multiply\count240 by 10
		     \count101=\count240	%101 is second digit of #2/#3
		     \divide\count101 by \count241
		     \count102=\count101
		     \multiply\count102 by \count241
		     \advance\count240 by -\count102
		     \multiply\count240 by 10
		     \count102=\count240	% 102 is the third digit
		     \divide\count102 by \count241
		     \count200=#1\count205=0
		     \count201=\count200
			\multiply\count201 by \count100
		 	\advance\count205 by \count201
		     \count201=\count200
			\divide\count201 by 10
			\multiply\count201 by \count101
			\advance\count205 by \count201
			%
		     \count201=\count200
			\divide\count201 by 100
			\multiply\count201 by \count102
			\advance\count205 by \count201
			%
		     \edef\@result{\number\count205}
}
\def\compute@wfromh{
		% computing : width = height * (bbw / bbh)
		\in@hundreds{\@p@sheight}{\@bbw}{\@bbh}
		%\ps@typeout{ \@p@sheight * \@bbw / \@bbh, = \@result }
		\edef\@p@swidth{\@result}
		%\ps@typeout{w from h: width is \@p@swidth}
}
\def\compute@hfromw{
		% computing : height = width * (bbh / bbw)
	        \in@hundreds{\@p@swidth}{\@bbh}{\@bbw}
		%\ps@typeout{ \@p@swidth * \@bbh / \@bbw = \@result }
		\edef\@p@sheight{\@result}
		%\ps@typeout{h from w : height is \@p@sheight}
}
\def\compute@handw{
		\if@height 
			\if@width
			\else
				\compute@wfromh
			\fi
		\else 
			\if@width
				\compute@hfromw
			\else
				\edef\@p@sheight{\@bbh}
				\edef\@p@swidth{\@bbw}
			\fi
		\fi
}
\def\compute@resv{
		\if@rheight \else \edef\@p@srheight{\@p@sheight} \fi
		\if@rwidth \else \edef\@p@srwidth{\@p@swidth} \fi
		%\ps@typeout{rheight = \@p@srheight, rwidth = \@p@srwidth}
}
%		
% Compute any missing values
\def\compute@sizes{
	\compute@bb
	\if@scalefirst\if@angle
% at this point the bounding box has been adjsuted correctly for
% rotation.  PSFIG does all of its scaling using \@bbh and \@bbw.  If
% a width= or height= was specified along with \psscalefirst, then the
% width=/height= value needs to be adjusted to match the new (rotated)
% bounding box size (specifed in \@bbw and \@bbh).
%    \ps@bbw       width=
%    -------  =  ---------- 
%    \@bbw       new width=
% so `new width=' = (width= * \@bbw) / \ps@bbw; where \ps@bbw is the
% width of the original (unrotated) bounding box.
	\if@width
	   \in@hundreds{\@p@swidth}{\@bbw}{\ps@bbw}
	   \edef\@p@swidth{\@result}
	\fi
	\if@height
	   \in@hundreds{\@p@sheight}{\@bbh}{\ps@bbh}
	   \edef\@p@sheight{\@result}
	\fi
	\fi\fi
	\compute@handw
	\compute@resv}
%
%
%
\def\OzTeXSpecials{
	\special{empty.ps /@isp {true} def}
	\special{empty.ps \@p@swidth \space \@p@sheight \space
			\@p@sbbllx \space \@p@sbblly \space
			\@p@sbburx \space \@p@sbbury \space
			startTexFig \space }
	\if@clip{
		\if@verbose{
			\ps@typeout{(clip)}
		}\fi
		\special{empty.ps doclip \space }
	}\fi
	\if@angle{
		\if@verbose{
			\ps@typeout{(rotate)}
		}\fi
		\special {empty.ps \@p@sangle \space rotate \space} 
	}\fi
	\if@prologfile
	    \special{\@prologfileval \space } \fi
	\if@decmpr{
		\if@verbose{
			\ps@typeout{psfig: Compression not available
			in OzTeX version \space }
		}\fi
	}\else{
		\if@verbose{
			\ps@typeout{psfig: including \@p@sfile \space }
		}\fi
		\special{epsf=\ps@predir\@p@sfile \space }
	}\fi
	\if@postlogfile
	    \special{\@postlogfileval \space } \fi
	\special{empty.ps /@isp {false} def}
}
\def\DvipsSpecials{
	%
	\special{ps::[begin] 	\@p@swidth \space \@p@sheight \space
			\@p@sbbllx \space \@p@sbblly \space
			\@p@sbburx \space \@p@sbbury \space
			startTexFig \space }
	\if@clip{
		\if@verbose{
			\ps@typeout{(clip)}
		}\fi
		\special{ps:: doclip \space }
	}\fi
	\if@angle
		\if@verbose{
			\ps@typeout{(clip)}
		}\fi
		\special {ps:: \@p@sangle \space rotate \space} 
	\fi
	\if@prologfile
	    \special{ps: plotfile \@prologfileval \space } \fi
	\if@decmpr{
		\openin1=\ps@predir\@p@sfile.gz
		\ifeof1
		        \closein1
		        % failed, supposed to be a *.Z file
			\if@verbose{
				\ps@typeout{psfig: including \@p@sfile.Z \space }
			}\fi
			\special{ps: plotfile "`zcat \@p@sfile.Z" \space }
		\else
                        \closein1
			% found .gz file
			\if@verbose{
				\ps@typeout{psfig: including \@p@sfile.gz \space }
			}\fi
			\special{ps: plotfile "`gunzip -c \@p@sfile.gz" \space }
		\fi
	}\else{
		\if@verbose{
			\ps@typeout{psfig: including \@p@sfile \space }
		}\fi
		\special{ps: plotfile \@p@sfile \space }
	}\fi
	\if@postlogfile
	    \special{ps: plotfile \@postlogfileval \space } \fi
	\special{ps::[end] endTexFig \space }
}
%
% \psfig
% usage : \psfig{file=, height=, width=, bbllx=, bblly=, bburx=, bbury=,
%			rheight=, rwidth=, clip=}
%
% "clip=" is a switch and takes no value, but the `=' must be present.
\def\psfig#1{\vbox {
	% do a zero width hard space so that a single
	% \psfig in a centering enviornment will behave nicely
	%{\setbox0=\hbox{\ }\ \hskip-\wd0}
	%
	\ps@init@parms
	\parse@ps@parms{#1}
	\compute@sizes
	%
	\ifnum\@p@scost<\@psdraft{
		\PsfigSpecials 
		% Create the vbox to reserve the space for the figure.
		\vbox to \@p@srheight sp{
		% 1/92 TJD Changed from "true sp" to "sp" for magnification.
			\hbox to \@p@srwidth sp{
				\hss
			}
		\vss
		}
	}\else{
		% draft figure, just reserve the space and print the
		% path name.
		\if@draftbox{		
			% Verbose draft: print file name in box
			% 10/93 TJD changed to fbox from frame
			\hbox{\fbox{\vbox to \@p@srheight sp{
			\vss
			\hbox to \@p@srwidth sp{ \hss 
			        % 10/93 TJD deleted to avoid ``_'' problems
				% \@p@sfile
			 \hss }
			\vss
			}}}
		}\else{
			% Non-verbose draft
			\vbox to \@p@srheight sp{
			\vss
			\hbox to \@p@srwidth sp{\hss}
			\vss
			}
		}\fi	



	}\fi
}}
\psfigRestoreAt
\setDriver
\let\@=\LaTeXAtSign




symbols.tex
% USEFUL SYMBOLS

\def\ie{\mbox{\'{\i}}}

% NOMS DE SOURCES

\def\unedzs{1 \mbox{E } 1207.4-5209}
\def\annihilateur{1 \mbox{E } 1740.7-2942}
\def\unedhqu{1 \mbox{E } 1841-045}
\def\azsv{\mbox{A}0620-00}
\def\cicam{\mbox{CI Cam}}
\def\cirxu{\mbox{Circinus X-1}}
\def\cygxu{\mbox{Cygnus X-1}}
\def\cygxt{\mbox{Cygnus X-3}}
\def\grb{\mbox{GRB} 990712}
\def\gro{\mbox{GRO J} 1655-40}
\def\grs{\mbox{GRS } 1915+105}
\def\grsdstq{\mbox{GRS } 1734-292}
\def\grsdstn{\mbox{GRS } 1739-278}
\def\grsdsch{\mbox{GRS } 1758-258}
\def\gx{\mbox{GX } 339-4}
\def\gxtcq{\mbox{GX } 354-0}
\def\irasnord{\mbox{IRAS } 19124+1106}
\def\irassud{\mbox{IRAS } 19132+1035}
\def\ksdsvq{\mbox{KS } 1724-356}
\def\ksdstu{\mbox{KS } 1731-260}
\def\lmcxu{\mbox{LMC } X-1}
\def\lmcxt{\mbox{LMC } X-3}
\def\novmus{\mbox{Nova Muscae 1991}}
\def\novoph{\mbox{Nova Ophiuchi 1993}}
\def\qu{\mbox{4U } 1630-47}
\def\saxjdsqs{\mbox{SAX J1747.0-2853}}
\def\saxjdhzh{\mbox{SAX J1808.4-3658}}
\def\saxjdhdn{\mbox{SAX J1819.3-2525}}
\def\scoxu{\mbox{Sco X-1}}
\def\seyfert{\mbox{Seyfert}}
\def\sgrzcvc{\mbox{SGR } 0525-66}
\def\sgrsvs{\mbox{SGR } 1627-41}
\def\sgr{\mbox{SGR } 1806-20}
\def\sgrdnc{\mbox{SGR } 1900+14}
\def\slx{\mbox{SLX } 1735-269}
\def\smcxu{\mbox{SMC X-1}}
\def\snr{\mbox{SNR G } 45.7-0.4}
\def\ss{\mbox{SS } 433}
\def\terzanu{\mbox{Terzan\,\,}1}
\def\terzanun{\mbox{Terzan\,\,}1}
\def\vqcqc{\mbox{V} 404 \mbox{Cyg}}
\def\wc{\mbox{W } 50}
\def\xtejzqvu{\mbox{XTE J} 0421+560}
\def\xtejodh{\mbox{XTE J} 1118+480}
\def\xtejqcq{\mbox{XTE J} 1550-564}
\def\xtejdsqh{\mbox{XTE J}1748-288}
\def\xtejdscc{\mbox{XTE J} 1755-324}
\def\xtejdhcn{\mbox{XTE J} 1859+226}

% UNITES

\def\angstrom{\mbox{ \scriptsize{A} \vspace*{1.cm}\hspace{-2.9mm}}^{\circ}}
\def\arcsecdeux{\mbox{ arc.s}^{2}}
\def\cmmoinsdeux{\mbox{ cm}^{-2}}
\def\cmmoinstrois{\mbox{ cm}^{-3}}
\def\cm{\mbox{ cm}}
\def\metre{\mbox{ m}}
\def\kg{\mbox{ kg}}
\def\micrometre{\mbox{ } \mu \mbox{m}}
\def\microns{\mbox{ } \mu \mbox{m}}
\def\hz{\mbox{ Hz}}
\def\msmoinsun{\mbox{ m.s}^{-1}}
\def\msmoinsdeux{\mbox{ m.s}^{-2}}
\def\kms{\mbox{ km\,s}^{-1}}
\def\pc{\mbox{ pc}}
\def\kpc{\mbox{ kpc}}
\def\Mpc{\mbox{ Mpc}}
\def\kmh{\mbox{ km\,h}^{-1}}
\def\Kkms{\mbox{ K\,km\,s}^{-1}}
\def\Msol{\mbox{ }M_{\odot}}
\def\Lsol{\mbox{ }L_{\odot}}
\def\mag{\mbox{ magnitude}}
\def\mags{\mbox{ magnitudes}}
\def\mJy{\mbox{ mJy}}
\def\Jy{\mbox{ Jy}}
\def\mT{\mbox{ mT}}
\def\rad{\mbox{ rad}}
\def\G{\mbox{ G}}
\def\J{\mbox{ J}}
\def\K{\mbox{ K}}
\def\sparan{\mbox{ s an}^{-1}}
\def\paran{\mbox{ an}^{-1}}
\def\jours{\mbox{ jours}}
\def\JparK{\mbox{ J K}^{-1}}
\def\NAmoinsdeux{\mbox{ N A}^{-2}}
\def\WattCmMoinsDeuxMuMoinsUn{\mbox{ W cm}^{-2}\mu \mbox{m}^{-1}}
\def\Wattmetremoinsdeux{\mbox{ W m}^{-2}}
\def\WparHz{\mbox{ W Hz}^{-1}}
\def\erg{\mbox{ erg}}
\def\ergpars{\mbox{ erg\,s}^{-1}}
\def\ergs{\mbox{ erg\,s}^{-1}}
\def\ergcms{\mbox{ erg s}^{-1} \mbox{cm}^{-2}}
\def\ergcmsarcmin{\mbox{ erg cm}^{-2} \mbox{s}^{-1} \mbox{arcmin}^{-2}}
\def\ergcmsang{\mbox{ erg cm}^{-2} \mbox{s}^{-1} \mbox{A \hspace{-6mm}}^{\circ}}
\def\arcminmoinsdeux{\mbox{arcmin}^{-2}}
\def\keV{\mbox{ keV}}
\def\W{\mbox{ W}}
\def\countss{\mbox{ counts s}^{-1}}
\def\coupss{\mbox{ coups s}^{-1}}
\def\cmmoinstrois{\mbox{ cm}^{-3}}
\def\masparan{\times 10^{-3 \, \prime \prime} \mbox{ an}^{-1}}
\def\mJyparbeam{\mbox{ mJy\,beam}^{-1}}
\def\janskyparbeam{\mbox{ Jansky\,faisceau}^{-1}}
\def\gcmcube{\mbox{ g cm}^{-3}}

% ANGLES

\def\deg{^{\circ}}
\def\degp{{\rlap.}^{\circ}}
\def\amin{^\prime}
\def\aminp{{\rlap.}^{\prime}}
\def\asec{^{\prime \prime}}
\def\asecp{{\rlap.}^{\prime \prime}}

\def\heu{^{h}}
\def\heup{{\rlap.}^{h}}
\def\hmin{^{m}}
\def\hminp{{\rlap.}^{m}}
\def\hsec{^{s}}
\def\hsecp{{\rlap.}^{s}}

% MOLECULES ET TRANSITIONS

\def\douzecoabb{^{12} \mbox{CO}}
\def\treizecoabb{^{13} \mbox{CO}}
\def\hcoabb{\mbox{H}^{13}\mbox{CO}^{+}}
\def\siodeuxabb{\mbox{SiO}_{2-1}}
\def\siotroisabb{\mbox{SiO}_{3-2}}
\def\siocinqabb{\mbox{SiO}_{5-4}}
\def\csabb{\mbox{CS}}

\def\douzecounzero{^{12} \mbox{CO } (\mbox{J} = 1 - 0)}
\def\douzecodeuxun{^{12} \mbox{CO } (\mbox{J} = 2 - 1)}
\def\treizecodeuxun{^{13} \mbox{CO } (\mbox{J} = 2 - 1)}
\def\treizecounzero{^{13} \mbox{CO } (\mbox{J} = 1 - 0)}
\def\hcoplus{\mbox{H}^{13}\mbox{CO}^{+ }(\mbox{J} = 1 - 0)}
\def\siodeuxun{\mbox{SiO } (\mbox{J} = 2 - 1, v = 0)}
\def\siotroisdeux{\mbox{SiO } (\mbox{J} = 3 - 2, v = 0)}
\def\siocinqquatre{\mbox{SiO } (\mbox{J} = 5 - 4, v = 0)}
\def\csdeuxun{\mbox{CS } (\mbox{J} = 2 - 1)}
\def\hdeux{\mbox{H}_{2}}

\def\Ta{\mbox{T}_{A}^{*}}

% ABBREVATIONS

\def\Av{A_{\rm v}}
\def\plusoumoins{\, \pm \,}
\def\pom{\, \pm \,}
\def\cad{\mbox{c'est-\`a-dire}}
\def\taf{\mbox{tout � fait}}
\def\foot{\footnotemark\footnotetext}
\def\hdeuxromain{\mbox{H\,{\sc ii}}}
\def\nh{N \mbox{(H)}}
\def\rg{r_{\scriptsize g}}
\def\ltsima{\; \buildrel < \over \sim \;}
\def\simlt{\lower.5ex\hbox{\ltsima}}            % < over MMM
\def\gtsima{\; \buildrel > \over \sim \;}
\def\simgt{\lower.5ex\hbox{\gtsima}}            % > over MMM

% NOMS

\def\M{\mbox{Mirabel}}
\def\R{\mbox{Rodr\'{\i}guez}}

integral_sxt.bbl
\begin{thebibliography}{24}
\expandafter\ifx\csname natexlab\endcsname\relax\def\natexlab#1{#1}\fi
\expandafter\ifx\csname url\endcsname\relax
  \def\url#1{{\tt #1}}\fi
\expandafter\ifx\csname urlprefix\endcsname\relax\def\urlprefix{URL }\fi

\bibitem[{{Charles}(1998)}]{charles:1998}
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\bibitem[{{Cook} et~al.(2000){Cook}, {Patterson}, {Buczynski}, \&
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\bibitem[{{Cui} et~al.(2000){Cui}, {Shrader}, {Haswell}, \& {Hynes}}]{Cui:2000}
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\bibitem[{{Garnavich} et~al.(1999){Garnavich}, {Stanek}, \&
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\bibitem[{{Haswell} et~al.(2000{\natexlab{a}}){Haswell}, {Hynes}, {King}
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  7294, 2+

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\bibitem[{{King}(1989)}]{king:1989}
{King} A.R., 1989, {Mon. Not. R. astr. Soc.}, 241, 365

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  2+

\bibitem[{{McClintock} et~al.(2000{\natexlab{a}}){McClintock}, {Garcia},
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\end{thebibliography}
