Treatment and control: a qualitative study of older mentally ill offenders' perceptions on their detention and care trajectory

The life of older mentally ill offenders (OMIOs) is often characterized by successive periods of detention in correctional facilities, admissions to psychiatric services, and unsuccessful attempts to live independently. Through in-depth interviews, eight personal stories from OMIOs under supervision of the commission of social defence in Ghent (Belgium) were analyzed in the phenomenological research tradition. The results of the study reveal that OMIOs had more positive and less negative experiences in prison settings when compared with other institutional care settings. Independent living, unsurprisingly, is favored the most. This may be due to the fact that the latter option fosters personal competence, feelings of being useful, personal choices, and contact with the outside world. Even in later lifetime, a combined approach of risk assessment with improvement of well-being remains valuable to stimulate offender rehabilitation. Therefore, more research into concepts that could be used to support OMIOs needs further consideration

Dense multipath component polarization and wall attenuation at 1.35 GHz in an office environment

This paper presents an analysis of dense multipath components in office meeting rooms. Radio channel sounding measurements at 1.35 GHz were performed with transmitter and receiver in the same room (intra-room) and in adjacent rooms (inter-room). Specular and dense multipath components were estimated with the RiMAX maximum-likelihood algorithm. The dense multipath reverberation characteristics were found to be not significantly different between polarization subchannels for both the intra-room and the inter-room channels, supporting the validity of a scalar dense multipath model. The specular and dense multipath wall attenuation losses were found to be 12.0 and 5.4 dB, respectively

Géochimie des muscovites comme indicateur du fractionnement des pegmatites de la région de Kabarore-Mparamirundi (nord-ouest du Burundi, Afrique centrale)

The Kabarore-Mparamirundi area hosts numerous pegmatites spatiotemporally related to lcucogranites dated at 986 +/- 10 Ma in Karagwe-Ankole belt. The deposits arc intensively exploited for columbitc-tantalite and cassiterite. Alkali metals in muscovite (Rb 370-7590 ppm, Cs 8-1470 ppm) are modeled by Rayleigh fractional crystallization from a parental leucogranitic composition (K 4.1 wt%, Rb 321 ppm and Cs 9 ppm). The power law declining behavior of the ratio K/Rb versus Cs indicates the Rayleigh fractional crystallization as the main process of differentiation of the various pegmatite facies. Moreover, the continuous trend from granite to the most evolved, exploited pegmatites demonstrates a co-genetic link among them. The fractionation model shows that umnined and abandoned pegmatites are less fractionated (less than 94% of fractionation) while mined pegmatites are highly fractionated and constitute fractionated products of more than 94% of the initial leucogranite composition. The Rb, Cs, Ta, Sn and Li elements in muscovite can be used as a valuable tool in the exploration of fertile and sterile pegmatites in this area.La région de Kabarore-Mparamirundi renferme de nombreuses pegmatites liées aux leucogranites de 986 ± 10 Ma investigués dans la chaîne Karagwe-Ankole. Elles sont intensément exploitées pour la columbite-tantalite et la cassitérite. Les éléments alcalins présents dans la muscovite (370 à 7590 ppm de Rb, 8 à 1470 ppm de Cs) sont modélisés par la cristallisation fractionnée de Rayleigh à partir d'une composition leucogranitique parentale (4,1 % de K, 321 ppm de Rb et 9 ppm de Cs). Le comportement décroissant du rapport K/Rb en fonction de Cs indique que la cristallisation fractionnée de Rayleigh est le principal processus de différenciation des divers faciès de pegmatites. De plus, la trajectoire continue depuis le granite parental jusqu’aux pegmatites exploitées démontre un lien co-génétique entre eux. Les pegmatites non exploitées et celles des exploitations abandonnées correspondent à des pegmatites qui sont les moins fractionnées selon le modèle (avec moins de 94 % de fractionnement) tandis que les pegmatites exploitées sont les plus fractionnées et constituent des produits de fractionnement de plus de 94 % de la composition initiale du leucogranite. Les éléments Rb, Cs, Ta, Sn et Li contenus dans les muscovites peuvent servir d’outil précieux dans l’exploration des pegmatites

Measurement of the cosmic ray spectrum above 4×10184{\times}10^{18} eV using inclined events detected with the Pierre Auger Observatory

A measurement of the cosmic-ray spectrum for energies exceeding $4{\times}10^{18}$ eV is presented, which is based on the analysis of showers with zenith angles greater than $60^{\circ}$ detected with the Pierre Auger Observatory between 1 January 2004 and 31 December 2013. The measured spectrum confirms a flux suppression at the highest energies. Above $5.3{\times}10^{18}$ eV, the "ankle", the flux can be described by a power law $E^{-\gamma}$ with index $\gamma=2.70 \pm 0.02 \,\text{(stat)} \pm 0.1\,\text{(sys)}$ followed by a smooth suppression region. For the energy ($E_\text{s}$) at which the spectral flux has fallen to one-half of its extrapolated value in the absence of suppression, we find $E_\text{s}=(5.12\pm0.25\,\text{(stat)}^{+1.0}_{-1.2}\,\text{(sys)}){\times}10^{19}$ eV.Comment: Replaced with published version. Added journal reference and DO

Energy Estimation of Cosmic Rays with the Engineering Radio Array of the Pierre Auger Observatory

The Auger Engineering Radio Array (AERA) is part of the Pierre Auger Observatory and is used to detect the radio emission of cosmic-ray air showers. These observations are compared to the data of the surface detector stations of the Observatory, which provide well-calibrated information on the cosmic-ray energies and arrival directions. The response of the radio stations in the 30 to 80 MHz regime has been thoroughly calibrated to enable the reconstruction of the incoming electric field. For the latter, the energy deposit per area is determined from the radio pulses at each observer position and is interpolated using a two-dimensional function that takes into account signal asymmetries due to interference between the geomagnetic and charge-excess emission components. The spatial integral over the signal distribution gives a direct measurement of the energy transferred from the primary cosmic ray into radio emission in the AERA frequency range. We measure 15.8 MeV of radiation energy for a 1 EeV air shower arriving perpendicularly to the geomagnetic field. This radiation energy -- corrected for geometrical effects -- is used as a cosmic-ray energy estimator. Performing an absolute energy calibration against the surface-detector information, we observe that this radio-energy estimator scales quadratically with the cosmic-ray energy as expected for coherent emission. We find an energy resolution of the radio reconstruction of 22% for the data set and 17% for a high-quality subset containing only events with at least five radio stations with signal.Comment: Replaced with published version. Added journal reference and DO

Measurement of the Radiation Energy in the Radio Signal of Extensive Air Showers as a Universal Estimator of Cosmic-Ray Energy

We measure the energy emitted by extensive air showers in the form of radio emission in the frequency range from 30 to 80 MHz. Exploiting the accurate energy scale of the Pierre Auger Observatory, we obtain a radiation energy of 15.8 \pm 0.7 (stat) \pm 6.7 (sys) MeV for cosmic rays with an energy of 1 EeV arriving perpendicularly to a geomagnetic field of 0.24 G, scaling quadratically with the cosmic-ray energy. A comparison with predictions from state-of-the-art first-principle calculations shows agreement with our measurement. The radiation energy provides direct access to the calorimetric energy in the electromagnetic cascade of extensive air showers. Comparison with our result thus allows the direct calibration of any cosmic-ray radio detector against the well-established energy scale of the Pierre Auger Observatory.Comment: Replaced with published version. Added journal reference and DOI. Supplemental material in the ancillary file

JWST CEERS probes the role of stellar mass and morphology in obscuring galaxies

A population of massive galaxies invisible or very faint in deep optical/near-infrared surveys, but brighter at longer wavelengths has been uncovered in the past years. However, the nature of these optically dark/faint galaxies (OFGs, among other nomenclatures) is highly uncertain. In this work, we investigate the drivers of dust attenuation in the JWST era. Particularly, we study the role of stellar mass, size, and orientation in obscuring star-forming galaxies (SFGs) at $3 < z < 7.5$, focusing on understanding why galaxies like OFGs are so faint at optical/near-infrared wavelengths. We find that stellar mass is the primary proxy of dust attenuation among those studied. Effective radius and axis ratio do not show a clear link with dust attenuation, with the effect of orientation close to random. However, there is a subset of highly dust attenuated ($A_V > 1$, typically) SFGs, of which OFGs are a specific case. For this subset, we find that the key distinctive feature is their compact size (for massive systems with $\log (M_{*}/M_{\odot}) > 10$), exhibiting 30% smaller effective radius than the average SFGs at the same stellar mass and redshift. On the contrary, they do not exhibit a preference for low axis ratios (i.e., edge-on disks). The results in this work show stellar mass as a primary proxy of dust attenuation and compact stellar light profiles behind thick dust columns obscuring typical massive SFGs.Comment: Submitted to A&A. 13 pages, 9 figure