Explore the vast range of titles available.

We present the study of a wreck, in a foreshore area, in the North of Brittany, France, using two different digitization methods, photogrammetry and laser scanning. The digitization process had to deal with the tide constraints. The 3D data produced using these technologies has been deployed in a large immersive infrastructure dedicated to virtual reality research, in order to propose new practises for archaeologists. The overall purpose of our research project is to define an innovative and efficient methodology for the study and preservation of cultural heritage in an inter-tidal context. In the inter-tidal context, heritage is really fragile and the risk of destruction is real (storms, erosion, coastal development...). The traditional methods are no longer efficient. This paper describes preliminary results, through the joint work of a research institute specialized in underwater archaeology, a research laboratory of archaeology and archaeosciences, and a research laboratory in computer science.

Accurate knowledge of the morphology of halos and its evolution are key constraints on the galaxy formation model as well as a determinant parameter of the strong-lensing phenomenon. Using the cosmological hydrodynamic simulation, the Evolution and Assembly of GaLaxies and their Environments (EAGLE), we aim to provide a comprehensive analysis of the evolution of the morphology of galaxy halos and of their mass distributions with a focus on the snapshot at redshift \\(z=0.5\\). We developed an iterative strategy involving a principal component analysis (PCA) to investigate the properties of the EAGLE halos and the differences in alignment between the various components. The mass distributions of the dark-matter (DM), gas, and star halos are characterised by a half-mass radius, a concentration parameter and (projected) axis ratios. We present statistics of the shape parameters of 336\\,540 halos from the EAGLE RefL0025N0376 simulation and describe their evolution from redshift \\(z=15\\) to \\(z=0\\). We measured the three-dimensional and two-dimensional projected shape parameters for the DM, the gas, and the star components as well as for all particles. At \\(z=0.5\\), the minor axis of gas aligns with the minor axis of DM for massive halos (\\(M>10^12\\) M\\(_\\)), but this alignment is poorer for less massive halos. The DM halos axis ratios \\(b/a\\) and \\(c/a\\) have median values of \\(0.82 0.11\\) and \\(0.64 0.12\\), respectively. The sphericity of gas in halos w/ and w/o stars appears to be negatively correlated to the total mass, while the sphericity of DM is insensitive to it. The measured projected axis ratios, \\(b_p/a_p\\), of star halos at \\(z=0.5\\) have a median value of \\(0.80 0.07\\), which is in good agreement with ground-based and space-based measurements within 1 \\(\\). For DM halos, we measure a value of \\(0.85 0.06\\).

Determining the Hubble constant tension requires alternative strategies, and multiply imaged quasars, with their intermediate redshifts, can potentially be used in this regard. We provide a currently complete catalogue of spectroscopically confirmed lensed quasars with ESA/ıt Gaia astrometry and photometry, as well as redshifts and time delays when available. In addition to the improved astrometry, the catalogue increases the number of lensed quasars by a factor of 1.5 (now 364, of which 277 are doubles and 87 are quads or triples) and significantly increases the number of lensing galaxies detected (now 218), which represents a major step forward. Redshifts are provided for 347 quasars and 188 deflectors. A completely new table of time delays, required for estimates of \\(H_0\\), is presented, with 195 time delays from 73 systems. ıt Gaia absolute astrometry is sub-milliarcsecond and covers the entire sky. Future ıt Gaia data releases will provide long-term photometry, which should provide many more time delays. The catalogues as presented here enable machine-learning techniques to be trained and tested and subsequently applied to the ıt Gaia data releases. Finally, we derive simple but homogeneous models of the 18 quadruply imaged quasars for which images of all four components are presented in ıt Gaia DR3.

This paper presents an application of photogrammetry on ceramic fragments from two excavation sites located north-west of France. The restitution by photogrammetry of these different fragments allowed reconstructions of the potteries in their original state or at least to get to as close as possible. We used the 3D reconstructions to compute some metrics and to generate a presentation support by using a 3D printer. This work is based on affordable tools and illustrates how 3D technologies can be quite easily integrated in archaeology process with limited financial resources. 1. INTRODUCTION Today, photogrammetry and 3D modelling are an integral part of the methods used in archeology and heritage management. They provide answers to scientific needs in the fields of conservation, preservation, restoration and mediation of architectural, archaeological and cultural heritage [2] [6] [7] [9]. Photogrammetry on ceramic fragments was one of the first applications contemporary of the development of this technique applied in the archaeological community [3]. More recently and due to its democratization, it was applied more generally to artifacts [5]. Finally joined today by the rise of 3D printing [8] [10], it can restore fragmented artifacts [1] [12]. These examples target one or several particular objects and use different types of equipment that can be expensive. These aspects can put off uninitiated archaeologists. So it would be appropriate to see if these techniques could be generalized to a whole class of geometrically simple and common artifacts, such as ceramics. From these observations, associated to ceramics specialists with fragments of broken ceramics, we aimed at arranging different tools and methods, including photogrammetry, to explore opportunities for a cheap and attainable reconstruction methodology and its possible applications. Our first objective was to establish a protocol for scanning fragments with photogrammetry, and for reconstruction of original ceramics. We used the digital reconstitutions of the ceramics we got following our process to calculate some metrics and to design and 3D print a display for the remaining fragments of one pottery.