All Figures

Figure 1: Colour image of Abell 1703 from F850W, F625W and F475W observations (Stott 2007). North is up, east is left. Size of the field of view is equal to , corresponding to 326 kpc  454 kpc. Multiply imaged systems used in the analysis are shown, and colour images are given in Appendix. The central ring formed by four bright images is found close to the cD galaxy. The giant arc (systems 10-11) falls south-east, at distance of 35 . System 2 is a straight arc located south of the cD and composed of two merging images. System 15 and 16 follow each other, forming a kind of Einstein cross configuration. In the north, we find a set of tangential systems (4-5-6-7-8-9). Then, two bright merging images form system 3, located close to galaxy 852 which present a blue nearby lensing feature. The filamentary structure can be appreciated on this image. See also the Subaru H band image in Appendix which is more extended.

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In the text

	Figure 2: Spectroscopic observation of image 1.1. Left: position of the slit. Right: 1D spectrum. The doublet is easily identified.
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In the text

	Figure 3: Integrated luminosity profile of the cD galaxy, in the B band rest frame, for the fit with reddening (solid) and without reddening (dashed), The corresponding mass profile used in the strong lensing analysis is shown as dot-dashed line. Both profiles have the same behaviour for .
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In the text

	Figure 4: Results of the SED fitting procedure. Luminosities are computed in an aperture of 7 . The red solid line corresponds to the fit with reddening, and the blue dotted-dashed line corresponds to the fit without reddening. In each case, the fit is good ( ) and leads to the same estimation of the stellar mass.
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In the text

Figure 5: Mass differences between model (0) and model (1) (solid), model (2) (dashed) and model (3) (dotted). The dot-dashed line correspond to the accuracy on the mass measurement, expressed as a percentage. If mass differences are below the accuracy up to 125 kpc, we see that for R>150 kpc, mass differences between model (0) and models (1) and (2) are above the accuracy on the mass measurement, which means that we are able to discriminate between these different mass models.

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In the text

	Figure 6: Mass contours overlaid on the ACS F850W frame. Also shown is the light distribution from the cD galaxy (dashed white contours), which is found to be consistent in orientation with the one of the mass distribution within a few degrees. Note how the light and the massfollow the filamentary structure. Size of panel is .
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In the text

Figure 7: Degeneracy plots between and (from left to right): cD stellar mass, c200 and . corresponds to the logarithmic slope of the underlying dark matter mass distribution parametrized by a generalized NFW profile. c200 and correspond to the concentration parameter and the scale radius respectively for this mass distribution. Note that the scale radius is found larger than the range within which we have observational constraints.

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In the text

Figure A.1: System 1, the central ring composed by 4 bright images. For its counter image, see Fig. A.8 below. Top panel: colour image from F850W, F625W and F465W observations. Size of panel is . Bottom panel: F775W image where the light from the cD galaxy has been subtracted. We plot the tangential and radial critical lines at z=0.88 (redshift of system 1). We also report a radial feature that is coming out from the cD galaxy (see Fig. 1), that is not used in the analysis since we have not been able to detect the counter images. Size of panel is .

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In the text

	Figure A.2: System 2, constituted by two magnified merging images. Two counter images are predicted to be more than two magnitudes fainter, we have not been able to detect any. Size of panel is .
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In the text

	Figure A.3: System 3, constituted by two magnified merging images and a demagnified one a bit further west. Size of panel is .
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In the text

	Figure A.4: System 4-5. These two systems are assumed to belong to the same background source galaxy. System 4 is systematically brighter than system 5. From top to bottom: images 4.1 and 5.1; 4.2 and 5.2; 4.3 and 5.3. Size of each panel is .
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In the text

	Figure A.5: System 6. From top to bottom: image 6.1, 6.2 and 6.3. Size of each panel is .
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In the text

	Figure A.6: Systems 7, 8 and 9. Size of each panel is .
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In the text

	Figure A.7: Systems 10 and 11 corresponds to two substructures identified on the giant arc. Note than more can be defined along this giant arc. Top panel: images 10.1, 11.1, 11.2 and 10.2. Size of panel is . Bottom panel: counter image of both systems, also presentingsubstructures. Size of panel is .
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In the text

	Figure A.8: Systems 15 and 16. Images belonging to system 15 are systematically brighter than images belonging to system 16. First panel, north to south: image 1.5, counter image of the central ring (Fig. A.1); image 15.1 and image 16.1. Second panel: images 15.2 and 16.2. Third panel: images 15.3 and 16.3. Last panel: images 15.4 and 16.4. Size of each panel is .
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In the text

	Figure A.9: Galaxy 852, located in the northern part of the ACS field, at . Size of panel is . The blue lensed feature is easily detected on this picture.
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In the text

	Figure A.10: Subaru image of Abell 1703 (H band). Size of panel is . The filamentary structure identified in Fig. 1 can be appreciated further on this image. The frame corresponds to the size of Fig. 1.
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In the text