\documentstyle[psfig,epsfig]{article} 

% ~/ss2/research/horace


\newcommand{\Ne}{$N_{\rm e}$}
\newcommand{\Te}{$T_{\rm e}$}

\newcommand{\cmt}{cm$^{-3}$}
\newcommand{\cm}{cm$^{-1}$}
\def\rsun{R$_\odot$}

\newcommand{\bi}{\begin{itemize}}
\newcommand{\ei}{\end{itemize}}


\begin{document}


I would like to aknwoledge the participation,
contribution/support  from:

\bi
\item
Gordon Bromage and  Hannah Leigh Worters, UCLAN, UK
\item
Carl Foley, Hilary McKay, Urmila Mitra Kraev, MSSL, UK
\item
Alan Whiting group (CTIO, Chile),
in particular Melissa Rice. 
\item
Carlos Alberto, Germano Quast 
and Ramiro Delareza (Brasil).
\item
The XMM/SOC at Villafranca, Madrid (Spain), 
for their professional support.
In particular, of  Nora Loiseau and
Pedro M. Rodriguez Pascual.
\item
Federico Gonzalez (CASLEO), Argentina
\item
Helen Mason, University of Cambridge UK
\ei



2RE J0241-53 (nicknamed Horace) is a binary of 
active X-ray emitting stars, classified as a member of an association 
of young Post-T-Tauri stars ($\sim$ 30 Myr) by Torres et al. (2000). 


Goal:

determine the
physical characteristics of the X-ray emission (during quiescent and flaring
state) of the visual binary 2RE J0241-53, and relate them to 
the properties of the stellar photospheres.

In particular in terms of chemical composition and
understand  the evolution from the T-Tauri phase.

It is likely that the X-ray emission from CTTS 
is due to  accretion (as proposed by 
Kastner et al. 2002 for TW Hya), while the 
PTTS have extended solar-like coronae.


{The target}

2RE J0241-53 (EUVE J0241-530) is  a bright XUV visual binary, discovered by 
the ROSAT (Pye et al., 1995) and EUVE  (Bowyer et al., 1996) all-sky
surveys (see also Jeffries et al. 1996).
Count rates in the 100~\AA\ bandpassess were comparable to those 
of the brightest flare stars.


Both stars have strong chromospheric emission
and have recurrent flares (Ball and Bromage 1995).


 dK7e and dM3e young and fast 
rotating  stars 

%, and studied in detail by Jeffries et al. (1996).

-Southern star is Li-rich.

Pushing to the limits

- OM fast mode windows

-angular spearation of 22''.

-multi-continent, multi-cultural experience



Ground-based spectroscopy 

\bi
\item
 SAAO 1.9m grating spectrograph with 1~\AA\ resolution and 
 $\simeq$90 s exposures.
\item
Wavelength range: 3700 - 4360~\AA\
\item
6 consecutive nights
\ei

%Total time coverage of 0241-53 on the night was 18:32 UT - 00:04 UT

%On XMM night:
%- Total no. of spectra
%        Northern star = 91
%        Southern star = 17

Ground-based photometry
\bi
\item
UBV aperture photometry with the SAAO 0.5-m telescope
\item 3 nights
\ei


{\bf On XMM night}


\bi
\item
CASLEO: cloudy

\item
SAAO 1.9m spectra  18:32 UT -- 00:04 UT

\item
CTIO low-resolution (17.2~\AA\ FWHM) 1.5m spectra 

\item
CTIO CCD B and U band  photometry with the 0.9m  
01:17  04:40 UT
%We started out in B but switched to U at 0224.

\item
SAAO U-band monitoring
% Northern star: 19:11 - 19:37 UT
%both stars 19:50 - 22:40 UT

\item
Brasil:  B-band monitoring
23:00 -- 00:30 UT 

\ei


\begin{figure}[!htbp]
\begin{center}
\centerline{\epsfig{figure=n5_lab.eps, width=10.0cm,angle=0}}
\centerline{\epsfig{figure=north_night7.ps,width=10.0cm,angle=0}}
\centerline{\epsfig{figure=southern_star_label.eps,width=10.0cm,angle=0}}
\caption{SAAO spectra of the northern star - 7th and 9th (XMM night)
 Feb 2004 and of the southern star - 7th Feb 2004.}
%variation in relative line strengths of the calcium and Balmer lines
\end{center}
\end{figure}

\begin{figure}[!htbp]
\begin{center}
\centerline{\epsfig{figure=southern_star_label.eps,width=10.0cm,angle=0}}
\centerline{\epsfig{figure=U-filter.ps,width=4.0cm,angle=0}
\epsfig{figure=om_filters.ps,width=4.0cm,angle=-90}
}
%\caption{SAAO spectra of the southern star - 7th Feb 2004.}
\end{center}
\end{figure}


\begin{figure}[!htbp]
\begin{center}
\centerline{\epsfig{figure=n5_lab.eps, width=10.0cm,angle=0}}
\centerline{\epsfig{figure=midut_191202.ps,width=11.0cm,angle=0}}
\centerline{\epsfig{figure=midut_191353.ps,width=11.0cm,angle=0}}
\caption{Bottom two plots: consecutive 90s exposures from XMM night (19:12,19:14 UT).
Notice the variation in the   Ca II (H and K) and H $\delta$.
%mid-exposure times of 19:12:02 UT and 19:13:53 UT
}
\end{center}
\end{figure}

%- Equivalent widths measured for H-delta and Ca II K for every northern
%star spectrum (using the splot routine in IRAF), the ratio of the two
%lines varying between ~0.14 and ~0.49.

%- Ratio of H-delta:Ca II H lines often seen to vary within 2 minutes
%(e.g. midut_191202.ps cf midut_191353.ps), perhaps due to the changing
%ratio of calcium and Balmer lines in the decay of a small flare.


\begin{figure}[!htbp]
\begin{center}
\centerline{\epsfig{figure=ew_n_9feb.ps,width=11.0cm,angle=90}}
%\caption{Equivalent widths for the Northern star}
\end{center}
\end{figure}


\begin{figure}[!htbp]
\centerline{\epsfig{file=OM_UVW1.ps, width=12.0cm,angle=-90 }}
\centerline{
\epsfig{file=fast_source1.ps, width=6.0cm,angle=0 }
\epsfig{file=fast_source2.ps, width=6.0cm,angle=0 }
}
\caption{One XMM/OM optical image (full FOV, UVW1 filter) of the target.
%The two stars are in the centre of the FOV.
Below are two sample images from the fast-mode extraction
windows. }
\end{figure}

\begin{figure}[!htbp]
\centerline{\epsfig{file=om_lc_n_all.ps, width=9.0cm,angle=90 }}
\centerline{\epsfig{file=om_lc_s_all.ps, width=9.0cm,angle=90 }}
\caption{XMM OM photometry}
\end{figure}

- two ground station handovers, one
on 10-02-2004 at 04:14, and 05:37 UT. 
During handovers, that have
a margin of about 1800 sec., the OM has to remain closed, which
creates gaps in the OM data. 
The handovers do not affect the other instruments.


\begin{figure}[!htbp]
\centerline{\epsfig{file=EPIC.ps, width=12.0cm,angle=-90 }}
\caption{One EPIC MOS 1 image}
\end{figure}

\begin{figure}[!htbp]
\centerline{\epsfig{file=epic_lc_n.ps, width=12.0cm,angle=90 }}
\centerline{\epsfig{file=epic_lc_s.ps, width=12.0cm,angle=90 }}
\caption{One EPIC PN light curves }
\end{figure}

\begin{figure}[!htbp]
\centerline{\epsfig{file=flare1_n_comp.ps, width=12.0cm,angle=90 }}
\centerline{\epsfig{file=flare2_n_comp.ps, width=12.0cm,angle=90 }}
\caption{Flares on Northern star. }
\end{figure}

\begin{figure}[!htbp]
\centerline{\epsfig{file=flare_s_comp.ps, width=12.0cm,angle=90 }}
\centerline{\epsfig{file=flat_top.ps, width=12.0cm,angle=90 }}
\caption{Flares on the Southern star.}
\end{figure}

\begin{figure}[!htbp]
\centerline{\epsfig{file=spectrum_mos1_s_grp.ps, width=12.0cm,angle=-90 }}
\caption{EPIC MOS 1 spectrum of the Southern star.}
\end{figure}

\begin{figure}[!htbp]
\centerline{\psfig{figure=fig1.ps,width=10.0cm,angle=90}}
\centerline{\psfig{figure=rgs1_1st.ps,width=10.0cm,angle=90}}
\caption{Top: the RGS 1 first order predicted spectrum.
 Bottom: the observed one. {\bf Where is all the Iron gone ?}}
\label{fig1}
\end{figure}
%-----------------------------Figure End----------------------------------

\begin{figure}[!htbp]
\centerline{\epsfig{file=rgs2_all.ps, width=12.0cm,angle=90 }}
\centerline{\epsfig{file=pz_tel_meg1_all.ps, width=12.0cm,angle=90 }}
\caption{Horace vs. PZ Tel }
\end{figure}


\begin{figure}[!htbp]
\centerline{\epsfig{file=ne_9_comp.ps, width=12.0cm,angle=0 }}
\caption{Ne IX spectral region. }
\end{figure}

\begin{figure}[!htbp]
\centerline{\epsfig{file=rgs1_o_7.ps, width=12.0cm,angle=90 }}
\caption{O VII spectral region. }
\end{figure}

\section{Summary of preliminary results}

\bi
\item
This is one of the few (two ?) X-ray 
observations of PTT stars.

\item
The XMM/OM fast-mode windows worked very well 
but data are missing.

\item
Both stars confirmed to be active, with flares.

\item
Ground-based  SAAO and CTIO observations are nicely
complementary.

\item
We confirm Linsky's law (the most interesting events 
occurr at the end of the observation).

\ei



\end{document}
