Astronomy & Astrophysics

All Figures

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{1426fig1.ps} \end{figure}$ Figure 1: Distribution of velocities for the 20 galaxies showing a low velocity tail at $\Delta _v\sim -6000$ km s^-1. The curve shows a Gaussian distribution centered at $\langle v\rangle=244~736$ km s^-1 with width given by the derived $\sigma _{\rm V}=1407$ km s^-1 (not corrected to the first order for cosmological redshift) and normalized for the 18 galaxies considered as cluster members.
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In the text

$\begin{figure} \par\includegraphics[width=11.5cm,clip]{1426fig2.ps} \end{figure}$ Figure 2: 1800 s I-band image of RX J1821.6+6827 taken at the UH 2.2 m telescope. The combined MOS1 and MOS2 image was smoothed with a Gaussian to have 16 pixels per cell (corresponding to 8 $^{\prime \prime }$ ). The energy range is 0.3-8 keV band. Units for the smoothed overlayed X-ray contours are (6.5, 7.8, 9.1, 13, 18.2, 24.7, 32. $5)\times 10^{-3}$ counts s^-1 arcmin^-2 over the background which correspond to (2.5, 3, 3.5, 5, 7, 9.5, 12.5) $\sigma$ over the background. The circles indicate 14 out of 20 cluster members. The cD galaxy is marked as galaxy # 7. The other 6 galaxies at the redshift of the cluster fall outside the field of view (see Table 1). The image measures $1092 \times 1092$ pixels covering a field of $4'\times 4'$ ( $1.98~h_{50}^{-1}\times1.98~h_{50}^{-1}$ Mpc at z = 0.8163).
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.8cm,clip]{1426fig3.ps} \end{figure}$ Figure 3: Binned X-ray spectrum and residuals for RX J1821.6+6827. The spectrum was binned in such a way that each resulting energy channel has a signal-to-noise ratio of at least 4. The solid line represents the best fit MEKAL model. The top grey spectrum is the pn spectrum, while the lower and darker spectra are the MOS1 and MOS2 spectra.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{1426fig4.ps} \end{figure}$ Figure 4: Long-slit spectrum taken at the UH 2.2 m of the QSO at z=1.692 associated to RX J1821.9+6818. The total integration time was of 2400 s. The dashed lines indicate the positions of the CIV, CIII], Mg emission lines at the QSO redshift. Wavelengths of atmospheric absorption bands are also indicated.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.8cm,clip]{1426fig5.ps} \end{figure}$ Figure 5: Binned X-ray spectrum and residuals for RX J1821.9+6818, the QSO in the XMM- Newton field. The spectrum was binned in such a way that each resulting energy channel has a signal-to-noise ratio of at least 5. The solid line represents the best fit power law model. The top grey spectrum is the pn spectrum, the MOS1 and MOS2 spectra are the two lower and darker spectra.
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{1426fig1.ps} \end{figure}$	Figure 1: Distribution of velocities for the 20 galaxies showing a low velocity tail at $\Delta _v\sim -6000$ km s^-1. The curve shows a Gaussian distribution centered at $\langle v\rangle=244~736$ km s^-1 with width given by the derived $\sigma _{\rm V}=1407$ km s^-1 (not corrected to the first order for cosmological redshift) and normalized for the 18 galaxies considered as cluster members.
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$\begin{figure} \par\includegraphics[angle=-90,width=8.8cm,clip]{1426fig3.ps} \end{figure}$	Figure 3: Binned X-ray spectrum and residuals for RX J1821.6+6827. The spectrum was binned in such a way that each resulting energy channel has a signal-to-noise ratio of at least 4. The solid line represents the best fit MEKAL model. The top grey spectrum is the pn spectrum, while the lower and darker spectra are the MOS1 and MOS2 spectra.
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$\begin{figure} \par\includegraphics[width=8.5cm,clip]{1426fig4.ps} \end{figure}$	Figure 4: Long-slit spectrum taken at the UH 2.2 m of the QSO at z=1.692 associated to RX J1821.9+6818. The total integration time was of 2400 s. The dashed lines indicate the positions of the CIV, CIII], Mg emission lines at the QSO redshift. Wavelengths of atmospheric absorption bands are also indicated.
Open with DEXTER

$\begin{figure} \par\includegraphics[angle=-90,width=8.8cm,clip]{1426fig5.ps} \end{figure}$	Figure 5: Binned X-ray spectrum and residuals for RX J1821.9+6818, the QSO in the XMM- Newton field. The spectrum was binned in such a way that each resulting energy channel has a signal-to-noise ratio of at least 5. The solid line represents the best fit power law model. The top grey spectrum is the pn spectrum, the MOS1 and MOS2 spectra are the two lower and darker spectra.
Open with DEXTER