Astronomy & Astrophysics

All Figures

$\begin{figure} \par\includegraphics[width=7.1cm,clip]{3419f1.eps} \end{figure}$ Figure 1: X-ray intensity of IGR J00291+5934 throughout the 2004 outburst. The open triangle indicates the discovery with INTEGRAL . The 2.5-25 keV PCA flux evolution is shown (open squares). The time of our Chandra observation is indicated by the arrow on the right. After MJD 53 355 the source flux is strongly influenced by residual flux and variability of (at least) the nearby V709 Cas.
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In the text

$\begin{figure} \par\includegraphics[width=8.6cm,clip]{3419f2.eps} \end{figure}$ Figure 2: Chandra HEG (order ${m}=\pm$ 1 combined, black) and MEG (order ${m}=\pm$ 1 combined, blue) spectra of IGR J00291+5934. The model shown is an absorbed power-law.
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In the text

$\begin{figure} \par\includegraphics[width=8.6cm,clip]{3419f3.eps} \end{figure}$ Figure 3: HEG data uniformly rebinned by a factor of 7, where we fitted this region with a power law plus broad line plus absorption feature. The latter is the most significant feature in our HEG spectra (approximately 99.3% significant) and is also present in the zeroth-order spectrum.
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In the text

$\begin{figure} \par\includegraphics[width=8.6cm,clip]{3419f4.eps} \end{figure}$ Figure 4: HEG (black), MEG (blue), and PCA (red) spectra of IGR J00291+5934. The fit shown is a composition of an absorbed power-law and disc blackbody.
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In the text

$\begin{figure} \par\includegraphics[width=8.6cm,clip]{3419f5.eps} \end{figure}$ Figure 5: HEG (black), MEG (blue), PCA (red), and HETGS zeroth-order (green) count spectra of IGR J00291+5934. Note the emission/absorption line features already discussed (Fig. 3) in both the zeroth-order and HEG spectra. The break in the HEG spectrum (data points between 1-1.3 keV) is due to the fact that in this range we have used HEG m=+1 alone and not the averaged $m=\pm 1$ orders, due to the contamination by V709 Cas in the HEG m=-1 order.
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In the text

$\begin{figure} \par\includegraphics[width=7.1cm,clip]{3419f1.eps} \end{figure}$	Figure 1: X-ray intensity of IGR J00291+5934 throughout the 2004 outburst. The open triangle indicates the discovery with INTEGRAL . The 2.5-25 keV PCA flux evolution is shown (open squares). The time of our Chandra observation is indicated by the arrow on the right. After MJD 53 355 the source flux is strongly influenced by residual flux and variability of (at least) the nearby V709 Cas.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.6cm,clip]{3419f2.eps} \end{figure}$	Figure 2: Chandra HEG (order ${m}=\pm$ 1 combined, black) and MEG (order ${m}=\pm$ 1 combined, blue) spectra of IGR J00291+5934. The model shown is an absorbed power-law.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.6cm,clip]{3419f3.eps} \end{figure}$	Figure 3: HEG data uniformly rebinned by a factor of 7, where we fitted this region with a power law plus broad line plus absorption feature. The latter is the most significant feature in our HEG spectra (approximately 99.3% significant) and is also present in the zeroth-order spectrum.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.6cm,clip]{3419f4.eps} \end{figure}$	Figure 4: HEG (black), MEG (blue), and PCA (red) spectra of IGR J00291+5934. The fit shown is a composition of an absorbed power-law and disc blackbody.
Open with DEXTER