Le contrat en travail social : fondements éthiques et opérationnalité

Alors que la pratique d'un contrat exigé par les dispositifs d'action sociale tend à se développer (aides au logement, jeunes majeurs, hébergement...), il n'est pas inutile de nous interroger sur les fondements du contrat en travail social et de nous rappeler les principes éthiques et l'intérêt opérationnel de cet outil. C'est le but de cet article qui se propose de définir ce qu'est le contrat, son intérêt et sa place dans la méthodologie professionnelle des travailleurs sociaux. Comme il s'agit d'une technique dont l'utilisation se révèle parfois peu aisée, nous traiterons des difficultés les plus courantes. Enfin, nous aborderons les fondements étiques du contrat en travail social et plus particulièrement les notions d'autonomie et d'acceptation du client, de confiance et d'engagement réciproques.While the practice of a contract as required by the mechanisms of social action tends to develop (housing support, help to young adults, sheltering…), it is worth asking ourselves about the foundation of the contract in social work and to recall the ethical principles as well as the operational interest of this tool. The purpose of the present article is to explain what a contract is, and what its interest and its place are within the social workers' professional methodology. Since the use of this technique is sometimes uneasy, we will concentrate on the more usual difficulties. Finally, we will tackle the ethical basis of a contract in social work, and more specifically the notions of autonomy and acceptance of a client, of mutual trust and involvement

The Role of Mergers in Early-type Galaxy Evolution and Black Hole Growth

Models of galaxy formation invoke the major merger of gas-rich progenitor galaxies as the trigger for significant phases of black hole growth and the associated feedback that suppresses star formation to create red spheroidal remnants. However, the observational evidence for the connection between mergers and active galactic nucleus (AGN) phases is not clear. We analyze a sample of low-mass early-type galaxies known to be in the process of migrating from the blue cloud to the red sequence via an AGN phase in the green valley. Using deeper imaging from SDSS Stripe 82, we show that the fraction of objects with major morphological disturbances is high during the early starburst phase, but declines rapidly to the background level seen in quiescent early-type galaxies by the time of substantial AGN radiation several hundred Myr after the starburst. This observation empirically links the AGN activity in low-redshift early-type galaxies to a significant merger event in the recent past. The large time delay between the merger-driven starburst and the peak of AGN activity allows for the merger features to decay to the background and hence may explain the weak link between merger features and AGN activity in the literature.Comment: 5 pages, 3 figures. ApJ Letters, in press

Estimating oil concentration and flow rate with calibrated vessel-mounted acoustic echo sounders

As part of a larger program aimed at evaluating acoustic techniques for mapping the distribution of subsurface oil and gas associated with the Deepwater Horizon-Macondo oil spill, observations were made on June 24 and 25, 2010 using vessel-mounted calibrated single-beam echo sounders on the National Oceanic and Atmospheric Administration ship Thomas Jefferson. Coincident with visual observations of oil at the sea surface, the 200-kHz echo sounder showed anomalously high-volume scattering strength in the upper 200 m on the western side of the wellhead, more than 100 times higher than the surrounding waters at 1,800-m distance from the wellhead, and weakening with increasing distance out to 5,000 m. Similar high-volume scattering anomalies were not observed at 12 or 38 kHz, although observations of anomalously low-volume scattering strength were made in the deep scattering layer at these frequencies at approximately the same locations. Together with observations of ocean currents, the acoustic observations are consistent with a rising plume of small (\u3c 1-mm radius) oil droplets. Using simplistic but reasonable assumptions about the properties of the oil droplets, an estimate of the flow rate was made that is remarkably consistent with those made at the wellhead by other means. The uncertainty in this acoustically derived estimate is high due to lack of knowledge of the size distribution and rise speed of the oil droplets. If properly constrained, these types of acoustic measurements can be used to rapidly estimate the flow rate of oil reaching the surface over large temporal and spatial scales

Signals and Power Distribution in the CMS Inner Tracker

\begin{abstract} This Note describes how the interconnection between the 3540 modules of the CMS Inner Tracker has been approached, focusing on the signal, high voltage and low voltage line distribution. The construction and tests of roughly a thousand interconnects called ``Mother Cables" is described. \end{abstract

HR Del remnant anatomy using 2-D spectral data and 3-D photoionization shell models

The HR Del nova remnant was observed with the IFU-GMOS at Gemini North. The spatially resolved spectral data cube was used in the kinematic, morphological and abundance analysis of the ejecta. The line maps show a very clumpy shell with two main symmetric structures. The first one is the outer part of the shell seen in H-alpha, that forms two rings projected in the sky plane. These ring structures correspond to a closed hourglass shape, first proposed by Harman and O'Brien (2003). The equatorial emission enhancement is caused by the superimposed hourglass structures in the line of sight. The second structure seen only in the [OIII] and [NII] maps is located along the polar directions inside the hourglass structure. Abundances gradients between the polar caps and equatorial region were not found. However, the outer part of the shell seems to be less abundant in Oxygen and Nitrogen than the inner regions. Detailed 2.5D photoionization modeling of the 3D shell was performed using the mass distribution inferred from the observations and the presence of mass clumps. The resulting model grids are used to constrain the physical properties of the shell as well as the central ionizing source. A sequence of 3D clumpy models including a disk shaped ionization source is able to reproduce the ionization gradients between polar and equatorial regions of the shell. Differences between shell axial ratios in different lines can also be explained by aspherical illumination. A total shell mass of 9 x 10-4 Msun is derived from these models. We estimate that 50% to 70% of the shell mass is contained in neutral clumps with density contrast up to a factor of 30.Comment: 31 pages 12 figures 4 tables title correcte