Astronomy & Astrophysics

$\begin{figure} \par\includegraphics[height=8.2cm,width=18cm,clip]{xrayoptimg.ps} \end{figure}$ Figure 1: Left panel: merged EPIC pn+MOS1+MOS2 image of the L1551 region. Right panel: the same region (to scale) in the red Palomar plates (from the Digital Sky Survey). The bright nebulosity near the center of the optical image is the outflow from the IRS5 embedded protostar.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[angle=270,width=8cm,clip]{src22_HD285845_lc.... ...ace*{8mm} \includegraphics[angle=270,width=8cm,clip]{hd282tvxpec.ps}\end{figure}$ Figure 2: Top: X-ray light curve of HD 285845 during the XMM-Newton and Chandra observations. Bottom: XMM-Newton and Chandra X-ray spectra of HD 285845. The fits to the spectra with absorbed 2-temperature plasma models with varying metal abundances are also shown.
Open with DEXTER

In the text

$\begin{figure} \par\leavevmode \mbox{ \epsfig{file=src2_MHO5_lc.ps, height=8.0c... ...angle=270, bbllx=99, bblly=43, bburx=554, bbury=700, clip=} } \par\end{figure}$ Figure 3: EPIC-pn light curves and spectra for the pre-main sequence stars detected in the XMM-Newton observations of the star-forming complex L1551. Best fit 2-T spectra are also plotted with the spectra. From top to bottom: [BHS98] MHO 5, V826 Tau, V827 Tau.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[angle=270,width=5.8cm,clip]{src18_XZTau_seg1... ...} \includegraphics[angle=270,width=5.8cm,clip]{src18_XZTau_seg3.ps} \end{figure}$ Figure 5: The spectra of XZ Tau during three different intervals of the XMM-Newton observation. From left to right: the spectrum from the first 20 ks, the spectrum from the subsequent 20 ks and the spectrum from the last 14 ks. The fits to the spectra with an absorbed 2-T model are also shown.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[height=8.2cm,width=18cm,clip]{xrayoptimg.ps} \end{figure}$	Figure 1: Left panel: merged EPIC pn+MOS1+MOS2 image of the L1551 region. Right panel: the same region (to scale) in the red Palomar plates (from the Digital Sky Survey). The bright nebulosity near the center of the optical image is the outflow from the IRS5 embedded protostar.
Open with DEXTER

$\begin{figure} \par\includegraphics[angle=270,width=8cm,clip]{src22_HD285845_lc.... ...ace*{8mm} \includegraphics[angle=270,width=8cm,clip]{hd282tvxpec.ps}\end{figure}$	Figure 2: Top: X-ray light curve of HD 285845 during the XMM-Newton and Chandra observations. Bottom: XMM-Newton and Chandra X-ray spectra of HD 285845. The fits to the spectra with absorbed 2-temperature plasma models with varying metal abundances are also shown.
Open with DEXTER

$\begin{figure} \par\leavevmode \mbox{ \epsfig{file=src2_MHO5_lc.ps, height=8.0c... ...angle=270, bbllx=99, bblly=43, bburx=554, bbury=700, clip=} } \par\end{figure}$	Figure 3: EPIC-pn light curves and spectra for the pre-main sequence stars detected in the XMM-Newton observations of the star-forming complex L1551. Best fit 2-T spectra are also plotted with the spectra. From top to bottom: [BHS98] MHO 5, V826 Tau, V827 Tau.
Open with DEXTER

$\begin{figure}\par\leavevmode \mbox{\epsfig{file=src7_V1075_lc.ps, height=8.0cm... ...angle=270, bbllx=99, bblly=43, bburx=554, bbury=700, clip=} } \par \end{figure}$	Figure 3: continued. From top to bottom: V1075 Tau, V710 Tau, XZ Tau.
Open with DEXTER

$\begin{figure} \par\includegraphics[angle=270,width=8.2cm,clip]{src7_V1075_seg1.... ...m} \includegraphics[angle=270,width=8.2cm,clip]{src7_V1075_seg2.ps} \end{figure}$	Figure 4: Left: the spectrum of V1075 Tau from the first 30 ks of observation; right: the spectrum from the last 24 ks. The fits to the spectra with an absorbed 2-T model are also shown.
Open with DEXTER

$\begin{figure} \par\includegraphics[angle=270,width=5.8cm,clip]{src18_XZTau_seg1... ...} \includegraphics[angle=270,width=5.8cm,clip]{src18_XZTau_seg3.ps} \end{figure}$	Figure 5: The spectra of XZ Tau during three different intervals of the XMM-Newton observation. From left to right: the spectrum from the first 20 ks, the spectrum from the subsequent 20 ks and the spectrum from the last 14 ks. The fits to the spectra with an absorbed 2-T model are also shown.
Open with DEXTER

$\begin{figure}\par\leavevmode \mbox{\epsfig{file=xztaulc2ks.ps, height=8.0cm, a... ... angle=270, bbllx=99, bblly=43, bburx=554, bbury=700, clip=} } \par\end{figure}$	Figure 6: Chandra ACIS light curves and spectra (together with best-fitting 2-T spectra) of (from top to bottom): XZ Tau, HL Tau.
Open with DEXTER