Tuning the electronic hybridization in the heavy fermion cage compound YbFe2_{2}Zn20_{20} with Cd-doping

Tuning of the electronic properties of heavy fermion compounds by chemical substitutions provides excellent opportunities to further understand the physics of hybridized ions in crystal lattices. Here we present an investigation on the effects of Cd doping in flux-grown single crystals of the complex intermetallic cage compound YbFe$_{2}$Zn$_{20}$, that has been described as a heavy fermion with Sommerfeld coefficient of 535 mJ/mol.K$^{2}$. Substitution of Cd for Zn disturbs the system by expanding the unit cell and, in this case, the size of the Zn cages that surround Yb and Fe. With increasing amount of Cd, the hybridization between Yb $4f$ electrons and the conduction electrons is weakened, as evidenced by a decrease in the Sommerfeld coefficient, which should be accompanied by a valence shift of the Yb$^{3+}$ due to the negative chemical pressure effect. This scenario is also supported by the low temperature dc-magnetic susceptibility, that is gradually suppressed and evidences an increment of the Kondo temperature, based on a shift to higher temperatures of the characteristic broad susceptibility peak. Furthermore, the DC resistivity decreases with the isoelectronic Cd substitution for Zn, contrary to the expectation for an increasingly disordered system, and implying that the valence shift is not related to charge carrier doping. The combined results demonstrate excellent complementarity between positive physical pressure and negative chemical pressure, and point to a rich playground for exploring the physics and chemistry of strongly correlated electron systems in the general family of Zn$_{20}$ compounds, despite their structural complexity.Comment: J. Phys.: Cond. Mat. (accepted

The O’Neill Institute for National and Global Health Law: Discovering Innovative Solutions for the Most Pressing Health Problems Facing the Nation and the World

The connection between health and an individual’s ability to function in society, as well as the importance of health to a society’s economic, political, and social wellbeing necessitates finding innovative solutions to the world’s most pressing health problems. The O’Neill Institute for National and Global Health Law at Georgetown University seeks to demonstrate the role that academia can play in addressing complex national and global health problems in a comprehensive, evidence-based, intellectually-rigorous, and nonpartisan manner. The O’Neill Institute currently has three research programs: global health law, national health law, and the center for disease prevention and outcomes. Projects within these programs examine a broad range of health law and policy issues, such as global health governance, global tobacco control, health worker migration, emergency preparedness, national and Chinese health reform, HIV and AIDS issues, food safety, and personalized medicine. These projects merge the scholarly capacity within the institute with the resources of its partners, which include the World Health Organization, World Bank, the Bill & Melinda Gates Foundation, the U.S. Centers for Disease Control and Prevention, and the Campaign for Tobacco Free Kids. Additionally, the faculty and fellows of the O’Neill Institute regularly produce high-level scholarship and engage in teaching offering multi-disciplinary course offerings and innovative graduate degree programs. URL: http://www.law.georgetown.edu/oneillinstitute/documents/2010-03-09_oneill-solutions.pdf; http://mjlst.umn.edu/uploads/Pf/V1/PfV1QhiCT6lUOsv1AqDTCA/111_gostin.pdf

Stars and brown dwarfs in the sigma Orionis cluster. III. OSIRIS/GTC low-resolution spectroscopy of variable sources

Context. Although many studies have been performed so far, there are still dozens of low-mass stars and brown dwarfs in the young sigma Orionis open cluster without detailed spectroscopic characterisation. Aims. We look for unknown strong accretors and disc hosts that were undetected in previous surveys. Methods. We collected low-resolution spectroscopy (R ~ 700) of ten low-mass stars and brown dwarfs in sigma Orionis with OSIRIS at the Gran Telescopio Canarias under very poor weather conditions. These objects display variability in the optical, infrared, Halpha, and/or X-rays on time scales of hours to years. We complemented our spectra with optical and near-/mid-infrared photometry. Results. For seven targets, we detected lithium in absorption, identified Halpha, the calcium doublet, and forbidden lines in emission, and/or determined spectral types for the first time. We characterise in detail a faint, T Tauri-like brown dwarf with an 18 h-period variability in the optical and a large Halpha equivalent width of -125+/-15 AA, as well as two M1-type, X-ray-flaring, low-mass stars, one with a warm disc and forbidden emission lines, the other with a previously unknown cold disc with a large inner hole. Conclusions. New unrevealed strong accretors and disc hosts, even below the substellar limit, await discovery among the list of known sigma Orionis stars and brown dwarfs that are variable in the optical and have no detailed spectroscopic characterisation yet.Comment: A&A, in press (accepted for publication in section 14. Catalogs and data of Astronomy and Astrophysics

Dust loss from activated asteroid P/2015 X6

We present observations and dust tail models of activated asteroid P/2015 X6 from deep imaging data acquired at the 10.4m Gran Telescopio Canarias (GTC) from mid-December 2015 to late January 2016. The results of the modeling indicate that the asteroid has undergone a sustained dust loss over a two-month or longer period. The dust parameters, derived from multidimensional fits of the available images, are compatible with either ice sublimation or rotational instability processes. An impulsive event, as it could be associated to an impact with another body, is less likely. A power-law distribution of particles, with minimum and maximum radius of 1 $\mu$m and 1 cm, and power index of --3.3 is found to be consistent with the observations. Depending on the ejection velocity model adopted, the particle velocities are found in the 0.3 to 10 m s$^{-1}$ range. The activation time was between 18-26 days before discovery. The total ejected mass from that time to the most recent observation is in the range 5-9$\times$10$^6$ kg. No dust features giving indication of past activity earlier than the activation time have been observed.Comment: Accepted by ApJ, May 15th 201