Astronomy & Astrophysics

All Tables

Table 1: Properties of the data used in this work. The $5\sigma$ limiting magnitudes were determined with SExtractor using an aperture of $2^{\prime \prime }$ .
Table 2: The properties of the arcs A1-A5 and the candidate counter-image AC used in the strong lensing analysis of the cluster. We also present additional arc candidates (systems B, C, D, and E) - see also Fig. 7. The properties of systems A, and C are measured from the I-band, while B is measured from the Ks-band image, and D and E are measured from the combined UBVRIKs image. The positions and position angles are given with respect to the brightest cluster member; the position angle of $90^{\circ }$ means that the arc is tangentially aligned with the BCG. All are measured with SExtractor. Because of the proximity of B1 and B2 to a cluster member we can not measure their ellipticities accurately.
Table 3: The photometric properties of the arcs A1, A2, A4, A5, and the candidate counter image AC. Given are three colours ( m_B -m_I, m_V -m_I, and m_R -m_I) in magnitudes (measured from the isophotal magnitudes), VRI peak surface brightnesses S_V,R,I (in magnitudes), and photometric redshifts. For A1-A5 we determine them using 6 bands, for AC Ks is not available. If objects belong to the same source the colours and surface brightnesses need to be conserved.
Table 4: Reconstructed mass of RX J1347.5-1145 within a cylinder of $360~ {h^{-1}}\mbox{ kpc}$ radius around the BCG from I-band (left) and R-band (right) weak lensing data and one candidate 3-image system. Three different $\kappa ^{(0)}$ models have been used. We use the best fit model from the multiple image system IM, IS is the best fit SIS model from the process of parametrised fitting of weak lensing data and I0 has $\kappa ^{(0)}=0$ on all grid points (see Sect. 4.2). In brackets we give for comparison the velocity dispersion of an SIS having the same enclosed mass within $360~ {h^{-1}}\mbox{ kpc}$ .