\documentclass[pdf,azure1,colorBG]{prosper}
% dvips -Ppdf -G0 talk1.dvi -o talk1.ps

% ps2pdf -dPDFsettings=/prepress talk1.ps talk1.pdf 

%\documentclass[ps,azure1,colorBG]{prosper}
% dvips -Ppdf -G0 talk1.dvi -o talkps.ps

%\documentclass[pdf,slideColor,contemporain,colorBG]{prosper}

%\documentclass[pdf,slideColor, gdz1]{prosper}

%\documentclass[pdf,slideColor,azure,colorBG]{prosper}

%\documentclass[ps,slideColor,darkblue,colorBG]{prosper}

% ~/ss2/research/horace


\usepackage{amsmath, epsfig, amsfonts, amsbsy, pstricks, pst-node, pst-text, pst-3d}


\newcommand{\items}[1]{\begin{itemize} \item #1 \end{itemize}}
\newcommand{\itemss}[2]{\begin{itemize} \item #1 \item #2 \end{itemize}}
\newcommand{\itemsss}[3]{\begin{itemize} \item #1 \item #2 \item #3 
\end{itemize}}
\newcommand{\itemssss}[4]{\begin{itemize} \item #1 \item #2 \item #3 \item #4
\end{itemize}}

%\newcommand{\slidetextsize}{\footnotesize}
%\newcommand{\captionstyle}[1]{\scriptsize \textbf{#1}}


\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}}

\title{X-ray emission from PTT stars}
%\subtitle{

\author{Giulio Del Zanna}

\institution{Department of Applied Mathematics and Theoretical Physics \\
 University of Cambridge}

%\includegraphics[scale=0.58]{UniversityLogo.eps}}

\slideCaption{COSPAR 2004:  X-ray emission from PTT stars}

\Logo(8.3,7.78){\includegraphics[scale=0.4]{UniversityLogo.eps}}

\DefaultTransition{Replace}

%Box dissolve replace wipe 

%\FontTitle{Large}{}

\begin{document}
\maketitle

%\FontText{ \white\usefont{T1}{phv}{m}{n}\fontsize{14.4pt}{14pt}\selectfont}

%\footnotesize

\begin{slide}{Summary}
\bi
\item
Coordinated XMM-Newton and ground-based spectroscopic
+ photometric observations  of two Post T Tauri stars.
\item
The observations were done in February 
$\to $ results are only preliminary !
\ei

\end{slide}

%---------------------------------------------------------------------- SLIDE -

\begin{slide}{Acknowledgements}

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

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

\item
PPARC
\ei

\end{slide}

%------------------------------------------------------------------------------

%---------------------------------------------------------------------- SLIDE -
\overlays{7}{%
\begin{slide}{Goals}

\begin{itemstep}
\item
Determine the
{\red physical characteristics of the X-ray emission}
 (during quiescent and flaring state) of PTT stars to help 
understand  the evolution from the T-Tauri phase;

\item
 relate them to 
the properties of the stellar {\red photospheres};

\item
in particular in terms of {\red chemical composition}
(study the FIP/anti-FIP effect).

\item
It is possible that the X-ray emission from CTTS 
is due to  accretion (as proposed by 
Kastner et al. 2002 for TW Hya)

\item the 
PTTS have strong X-ray emission, and
could have extended solar-like coronae.

\item
This is perhaps the first XMM observation.
 Only one other PTTS (PZ Tel, Argiroffi et al. 2004).

\item
{\blue Multiwavelength {\Large multiwavelength} {\Huge multiwavelength}
}
\end{itemstep}
\end{slide}
}
%------------------------------------------------------------------------------

%---------------------------------------------------------------------- SLIDE -
\overlays{5}{%
\begin{slide}{The target}

\begin{itemstep}
\item
2RE J0241-53 (EUVE J0241-530 but we nicknamed Horace) is a binary of 
active X-ray emitting stars in the southern sky 
(Horologium), discovered by 
the ROSAT  and EUVE all-sky
surveys (see also Jeffries et al. 1996).

\item
 classified as a member of an association 
of young PTT stars ($\sim$ 30 Myr) by the 
brasilians (Torres et al. 2000). 

\item
Count rates in the 100~\AA\ bandpassess were comparable to those 
of the brightest flare stars.

\item
Both stars have strong chromospheric emission
and have recurrent flares (Ball and Bromage 1995).
$\to$ kill two birds with a stone... and double 
the chances of observing {\Huge big} flares.

\item
 dK7e and dM3e  fast 
rotating  stars ($v$ sin $i$=12, 70 km/s).
Southern star is Li-rich.

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

\end{itemstep}
\end{slide}
}
%------------------------------------------------------------------------------

%---------------------------------------------------------------------- SLIDE -
\begin{slide}{Pushing to the limits}

\begin{itemstep}
\item
Problems in coordinating multi-wavelength observations
\item
XMM OM fast mode windows
\item
angular separation of 22'' --  roll angle
\item
multi-continent, multi-cultural experience
\item
we need an observatory on Easter Island!
\end{itemstep}

\begin{figure}[!htbp]
\begin{center}
\centerline{\epsfig{figure=w3.ps,width=4.0cm,angle=0}}
\end{center}
\end{figure}

\end{slide}


%---------------------------------------------------------------------- SLIDE -
\begin{slide}{Ground-based } 

Two-weeks observing in South Africa.

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

Photometry
\bi
\item
UBV aperture photometry with the SAAO 0.5-m telescope
\item 3 nights
\ei
\end{slide}


%---------------------------------------------------------------------- SLIDE -
\begin{slide}{On the XMM night (19-20 Feb 2004)}


\bi
\item
Argentina -- CASLEO: cloudy !

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

\item
Chile: 
\bi
\item
CTIO low-resolution (17.2~\AA\ FWHM)  spectra at the 1.5m
\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.
\ei

\item
South Africa:
\bi
\item
SAAO 1.9m spectra  18:32 UT -- 00:04 UT
\item
SAAO U-band monitoring
% Northern star: 19:11 - 19:37 UT
%both stars 19:50 - 22:40 UT
\ei
\ei

{\red $\to$ ground-based only covered part of the XMM observation}

\end{slide}

%---------------------------------------------------------------------- SLIDE -
\begin{slide}{SAAO spectra -  northern star}

Two spectra on the  7th and 9th Feb 2004:

\begin{figure}[!htbp]
\begin{center}
\centerline{\epsfig{figure=n5_lab.eps, width=6.0cm,angle=0}
\epsfig{figure=north_night7.ps,width=7.0cm,angle=0}}
%\centerline{\epsfig{figure=southern_star_label.eps,width=5.0cm,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}

\end{slide}

%---------------------------------------------------------------------- SLIDE -
\begin{slide}{Filters - CTIO}

\begin{figure}[!htbp]
\begin{center}
\centerline{\epsfig{figure=U-filter.ps,width=5.0cm,angle=0}
\epsfig{figure=southern_star_label.eps,width=8.0cm,angle=0}}
%\caption{SAAO spectra of the southern star - 7th Feb 2004.}
\end{center}
\end{figure}



\end{slide}

%------------------------------------------------------------------------------
\begin{slide}{Filters - OM}
\begin{figure}[!htbp]
{\epsfig{figure=om_filters.ps,width=4.0cm,angle=-90}}
\end{figure}

\end{slide}


%---------------------------------------------------------------------- SLIDE -
\begin{slide}{Chromospheric variability}

Consecutive 90s exposures from XMM night (19:12,19:14 UT).
Notice the variation in the   Ca II (H and K) and H $\delta$.

\begin{figure}[!htbp]
\begin{center}
%\centerline{\epsfig{figure=n5_lab.eps, width=10.0cm,angle=0}}
\centerline{\epsfig{figure=midut_191202.ps,width=6.5cm,angle=0}
\epsfig{figure=midut_191353.ps,width=6.5cm,angle=0}}
%\caption{
%mid-exposure times of 19:12:02 UT and 19:13:53 UT
%}
\end{center}
\end{figure}

\end{slide}
%------------------------------------------------------------------------------

%- 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.

%---------------------------------------------------------------------- SLIDE -
\begin{slide}{EW for the Northern star}

\begin{figure}[!htbp]
\begin{center}
\centerline{\epsfig{figure=ew_n_9feb.ps,width=7.0cm,angle=90}}
%\caption{Equivalent widths for the Northern star}
\end{center}
\end{figure}

\end{slide}
%---------------------------------------------------------------------- SLIDE -
\begin{slide}{XMM OM }

\begin{figure}[!htbp]
\begin{center}
\epsfig{file=OM_UVW1.ps, width=5.0cm,angle=-90}
\begin{center}
\epsfig{file=fast_source2.ps, width=3.0cm,angle=0 }
\epsfig{file=fast_source1.ps, width=3.0cm,angle=0 }
\end{center}
\end{center}
%\begin{center}
%\end{center}
%\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}

\end{slide}
%---------------------------------------------------------------------- SLIDE -
\begin{slide}{OM light curves}

\begin{figure}[!htbp]
\centerline{\epsfig{file=om_lc_n_all.ps, width=4.5cm,angle=90 }
\epsfig{file=om_lc_s_all.ps, width=4.5cm,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.

\end{slide}
%---------------------------------------------------------------------- SLIDE -
\begin{slide}{EPIC MOS 1 image}

\begin{figure}[!htbp]
\centerline{\epsfig{file=EPIC.ps, width=8.0cm,angle=-90 }}
%\caption{One EPIC MOS 1 image}
\end{figure}

\end{slide}
%---------------------------------------------------------------------- SLIDE -
\begin{slide}{EPIC PN light curves}

\begin{figure}[!htbp]
\centerline{\epsfig{file=epic_lc_n.ps, width=7.0cm,angle=90 }}
%\epsfig{file=epic_lc_s.ps, width=7.0cm,angle=90 }}
%\caption{EPIC PN light curves }
\end{figure}

\end{slide}

%---------------------------------------------------------------------- SLIDE -
\begin{slide}{EPIC PN light curves}
\begin{figure}[!htbp]
\centerline{\epsfig{file=epic_lc_s.ps, width=7.0cm,angle=90 }}
%\caption{EPIC PN light curves }
\end{figure}

\end{slide}


%---------------------------------------------------------------------- SLIDE -
\begin{slide}{Flares  on Northern star }

\begin{figure}[!htbp]
\centerline{\epsfig{file=flare1_n_comp.ps, width=7.0cm,angle=90 }}
%\centerline{\epsfig{file=flare2_n_comp.ps, width=12.0cm,angle=90 }}
%\caption{Flares on Northern star. }
\end{figure}

\end{slide}
%---------------------------------------------------------------------- SLIDE -

\begin{slide}{Flares  on Northern star }

\begin{figure}[!htbp]
\centerline{\epsfig{file=flare2_n_comp.ps, width=7.0cm,angle=90 }}
%\caption{Flares on Northern star. }
\end{figure}

\end{slide}

%---------------------------------------------------------------------- SLIDE -

\begin{slide}{Flares  on the Southern star.}

\begin{figure}[!htbp]
\centerline{\epsfig{file=flare_s_comp.ps, width=7.0cm,angle=90 }}
%\centerline{\epsfig{file=flat_top.ps, width=12.0cm,angle=90 }}
%\caption{Flares on the Southern star.}
\end{figure}

\end{slide}
%---------------------------------------------------------------------- SLIDE -

\begin{slide}{Flares  on the Southern star.}

\begin{figure}[!htbp]
\centerline{\epsfig{file=flat_top.ps, width=7.0cm,angle=90 }}
%\caption{Flares on the Southern star.}
\end{figure}

\end{slide}


%---------------------------------------------------------------------- SLIDE -
\begin{slide}{EPIC MOS 1 spectrum of the Southern star}

\begin{figure}[!htbp]
\centerline{\epsfig{file=spectrum_mos1_s_grp.ps, width=7.0cm,angle=-90 }}
%\caption{EPIC MOS 1 spectrum of the Southern star.}
\end{figure}
\end{slide}

%---------------------------------------------------------------------- SLIDE -
\begin{slide}{RGS - here is why we need \\
spectroscopy }

{\red \Large Where is all the Iron gone ?}

\begin{figure}[!htbp]
\centerline{\epsfig{figure=fig1.ps,width=5.0cm,angle=90}
\epsfig{figure=rgs1_1st.ps,width=5.0cm,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----------------------------------
\end{slide}

%---------------------------------------------------------------------- SLIDE -
\begin{slide}{Gallery - (from Huenemoerder, 2002)}

\begin{figure}[!htbp]
\centerline{\epsfig{figure=gallery.ps,width=8.0cm,angle=90}}
\end{figure}

\end{slide}

%---------------------------------------------------------------------- SLIDE -
\begin{slide}{Horace vs. PZ Tel }

\begin{figure}[!htbp]
\centerline{\epsfig{file=rgs2_all.ps, width=4.8cm,angle=90 }
\epsfig{file=pz_tel_meg1_all.ps, width=4.8cm,angle=90 }}
%\caption{Horace vs. PZ Tel }
\end{figure}

\end{slide}

%---------------------------------------------------------------------- SLIDE -
\begin{slide}{Densities - Ne IX}

\begin{figure}[!htbp]
\flushleft{\epsfig{file=ne_9_comp.ps, width=6.0cm,angle=0 }}
%\caption{Ne IX spectral region. }
\end{figure}

\end{slide}

%---------------------------------------------------------------------- SLIDE -
\begin{slide}{Densities - O VII}

\begin{figure}[!htbp]
\centerline{\epsfig{file=rgs1_o_7.ps, width=6.0cm,angle=90 }}
%\caption{O VII spectral region. }
\end{figure}

\end{slide}

%---------------------------------------------------------------------- SLIDE -
\overlays{8}{%
\begin{slide}{Summary }

\begin{itemstep}
\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 variability and flares.

\item
The coronae are mostly abundant in Ne,O.

\item
Compared to other young stars and PZ Tel, 
these stars have no `hot' emission (more like CTTS).
We need more observations.

\item
They were in a remarkably quiescent state 
(stellar cycles?).

\item
Ground-based  SAAO and CTIO observations are nicely
complementary but missed all the action !

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

\end{itemstep}


\end{slide}
}
%---------------------------------------------------------------------- SLIDE -


\end{document}
