Astronomy & Astrophysics

All Figures

$\begin{figure} {\includegraphics[width=8cm]{2234fig0.ps} } \end{figure}$ Figure 1: The m_B - m_V vs. m_V - m_I colours for the galaxies in our field. Cluster members are selected to lie inside the polygon. BCG colours are given as a triangle. In addition we plot as crosses all the galaxies which have a photometric redshift estimate $0.4<z_{\rm phot}<0.5$ .
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In the text

$\begin{figure} \par\includegraphics[width=7.2cm,clip]{2234fig1.ps}\end{figure}$ Figure 2: The photometric redshift distributions of the cluster members selected as described in Sect. 2.1.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm]{2234fig2.ps}\end{figure}$ Figure 3: The upper panels show the spatial variation of the PSF anisotropy in I (34 stars) and R (32 stars). The length of the sticks give the amplitude of the stellar ellipticities (the length corresponding to $\left\vert \epsilon \right\vert = 0.01$ is given at the top-left). The maximum ellipticity is around 2%. The lower panels show the ellipticity distribution after correction with a second-order polynomial. The formal residuals are about 0.005 in each component. Because of the small field of view and the small number of stars, the true errors are probably higher but difficult to estimate.
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In the text

$\begin{figure} \par\mbox{\includegraphics[width = 6.3cm]{2234fig3.ps}\hspace*{4m... ...{2234fig4.ps} } \par {\hspace*{3.3cm}{(a)}\hspace*{6.5cm}{(b)}} \par\end{figure}$ Figure 4: The redshift distributions of background sources used for weak lensing analysis (only sources with $z_{\rm phot}>0.55$ were considered) for I-band a) and R-band catalogue b). The mean photometric redshift of the samples is $\left\langle z_{I} \right\rangle = 1.18$ and $\left\langle z_{R} \right\rangle = 1.14$ .
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In the text

$\begin{figure} \par\mbox{\includegraphics[width = 6.3cm]{2234fig5.ps}\hspace*{4m... ...ps} } {\hspace*{3.5cm}{(a)}\hspace*{6.5cm}{(b)}\hspace*{3.5cm}} \par\end{figure}$ Figure 5: Average tangential ellipticity $\left\langle \epsilon_{\rm t} \right\rangle$ vs. projected radius $\left\langle \theta \right\rangle$ in radial bins centred on the brightest cluster member containing 50 galaxies per bin for the I-band data a) and 35 galaxies for the R-band data b). The errors are obtained by randomising the phases of the measured ellipticities, while preserving their absolute values. 100 randomisations were performed. The dashed line shows the best-fit SIS profile to the unbinned data, for the I-band we obtain $\sigma_{I, \rm SIS} = 950 \pm 60 ~\mbox{ km~s}^{-1}$ and for the R-band $\sigma_{R, \rm SIS} = 960 \pm 70 ~\mbox{ km~s}^{-1}$ (both $1\sigma$ error bars). It is plotted here for the average source redshifts of $\left\langle z_{I} \right\rangle = 1.18$ and $\left\langle z_{R} \right\rangle = 1.14$ . In the interval $0^{\prime} < \left\langle \theta \right\rangle \lesssim 0\hbox{$.\mkern-4mu^\prime$ }25$ the expectation value of the observed ellipticity (for these models) is given by $1/g(\theta ,z)^{*}$ and the tangential ellipticity profile has a steep gradient at $\left\langle \theta \right\rangle \simeq 0\hbox{$.\mkern-4mu^\prime$ }1$ (for both bands) where $Z(\left\langle z_{R, I} \right\rangle) \kappa = 1$ [since $g=Z\gamma / \left ( 1 - Z\kappa \right )$ ]. At $\left\langle \theta \right\rangle\gtrsim 0\hbox{$.\mkern-4mu^\prime$ }25$ the expectation value of the observed ellipticity is given by $g(\theta ,z)$ .
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In the text

$\begin{figure} \par\includegraphics[width=12cm,clip]{figure6.eps}\par\end{figure}$ Figure 6: The BRK colour composite of the $\sim$ $3 \times 3.2 \mbox{ amin}^2$ field of RX J1347.5-1145. Overlaid is in white contours the combined weak and strong lensing mass reconstruction from Fig. 9a1. The contour levels are the same (the field here is smaller), we smooth them here using a Gaussian kernel characterised by $\sigma =5^{\prime \prime }$ for clarity of the plot. Yellow circles show the multiple image system we use. North is up and East is left.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm]{2234fig10.eps}\end{figure}$ Figure 7: The $2.7 \times 2.4 \mbox{ arcmin}^2$ combined UBVRIKs image of the RX J1347.5-1145 showing previously known (system A and C) and newly discovered (systems B, D, and E) arc candidates (see Table 2). All are marked with a label and an arrow, further arc candidates are marked with an arrow only. The image was scaled non-linearly and the scaling varies across the field (in order to enhance the details of the image).
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In the text

$\begin{figure} \par\includegraphics[width=8cm]{2234fig11.eps}\end{figure}$ Figure 8: A $\sim$ $1\hbox {$.\mkern -4mu^\prime $ }0 \times 0\hbox {$.\mkern -4mu^\prime $ }6$ cutout of the Ks-band image of RX J1347.5-1145 showing one of the arcs used for strong lensing, the newly discovered very red arc system B1-B2 (two images almost merging, cf. Fig. 6) and the long thin arc C.
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In the text

$\begin{figure} \par\includegraphics[width=12cm]{2234f9.eps}\par\end{figure}$ Figure 9: $\kappa$ -maps obtained from combined strong and weak lensing reconstruction of the cluster RX J1347.5-1145. Left panels show the reconstructions using I-band data and for the ones on the right we use the R-band data. For the I-band data we have $N_{\rm g} = 210$ background source galaxies, and for the R-band $N_{\rm g} = 148$ , all with known photometric redshifts. In a1) and a2) we use the best fit model from the strong lensing analysis of the cluster IM as initial condition, in b1) and b2) we use the IS model (SIS model fitted to tangential ellipticities, centred on the brightest cluster member) - for both IM and IS see Sect. 4.2. In c1 and c2) we use I0, i.e. $\kappa ^{(0)}=0$ on all grid points. The positions of the 10 brightest cluster members are plotted as white circles.
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In the text

$\begin{figure} \par\mbox{\includegraphics[width = 5.6cm]{2234fig18.ps}\hspace*{6... ...width = 5.6cm]{2234fig19.ps} } {\hspace*{2.8cm}(a)\hspace*{6cm}(b)} \end{figure}$ Figure 10: The I-band a) and R-band b) brightness distribution of the RX J1347.5-1145 in $10^{12}~L_{\odot} / \mbox{ arcmin}^2$ . The cluster members are selected using the colour cuts described in the text, the ten brightest ones (in I) are plotted as white circles. Their luminosities of the cluster members have been smoothed using a Gaussian kernel characterised by $\sigma =9^{\prime \prime }$ .
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In the text

$\begin{figure} {\includegraphics[width=8cm]{2234fig0.ps} } \end{figure}$	Figure 1: The m_B - m_V vs. m_V - m_I colours for the galaxies in our field. Cluster members are selected to lie inside the polygon. BCG colours are given as a triangle. In addition we plot as crosses all the galaxies which have a photometric redshift estimate $0.4<z_{\rm phot}<0.5$ .
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$\begin{figure} \par\includegraphics[width=7.2cm,clip]{2234fig1.ps}\end{figure}$	Figure 2: The photometric redshift distributions of the cluster members selected as described in Sect. 2.1.
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$\begin{figure} \par\mbox{\includegraphics[width = 6.3cm]{2234fig3.ps}\hspace{4m... ...{2234fig4.ps} } \par {\hspace{3.3cm}{(a)}\hspace*{6.5cm}{(b)}} \par\end{figure}$	Figure 4: The redshift distributions of background sources used for weak lensing analysis (only sources with $z_{\rm phot}>0.55$ were considered) for I-band a) and R-band catalogue b). The mean photometric redshift of the samples is $\left\langle z_{I} \right\rangle = 1.18$ and $\left\langle z_{R} \right\rangle = 1.14$ .
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$\begin{figure} \par\includegraphics[width=8cm]{2234fig11.eps}\end{figure}$	Figure 8: A $\sim$ $1\hbox {$.\mkern -4mu^\prime $ }0 \times 0\hbox {$.\mkern -4mu^\prime $ }6$ cutout of the Ks-band image of RX J1347.5-1145 showing one of the arcs used for strong lensing, the newly discovered very red arc system B1-B2 (two images almost merging, cf. Fig. 6) and the long thin arc C.
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