Search

We employ third family Yukawa unification, predicted by simple supersymmetric SO(10) models, to estimate the lightest MSSM Higgs boson mass. For μ > 0 (or μ < 0) and mt = 173.1GeV, the Higgs mass is estimated to lie close to 123-124 GeV. The theoretical uncertainty in this estimate is ±3 GeV. We highlight some LHC testable benchmark points which also display the presence of neutralino-stau coannihilation channel. [ABSTRACT FROM AUTHOR]

This paper presents an overview of the instrumentation and experiments developed for the beamlines at Synchrotron SOLEIL in France. Currently fourteen beamlines are opened to users out of the twenty six scheduled. About half of the beamlines cover the soft x-rays region using spectroscopy and imagery techniques. The second half covers the hard x-rays field studying diffraction of matter. Some sample environments carried out for beamlines, for biology, chemistry and surface sciences are described. For the soft x-rays beamlines, carbon contamination of optics is a crucial issue. Different experiments are currently under study in order to reduce or even avoid this effect. Other studies relate to the improvement of metrological methods for beamline optics, to the reduction of vibrational effects for the microbeams and development of computer control for diffractometers. The various types of instruments and experiments will be presented both with an overview of the status of the beamlines in operation and under construction. [ABSTRACT FROM AUTHOR]

In the framework of ground-based science campaign dedicated to the encounter with Rosetta spacecraft, the mineralogies of the asteroids (21) Lutetia and (2867) Steins were investigated. Near-infrared (NIR) spectra of the asteroid in the 0.8–2.5 μm spectral range have been obtained with SpeX/IRTF in remote-observing mode from Meudon, France, and Cambridge, MA, in March, April and December 2006 and in January and March 2007. A χ2 test using meteorite spectra from the RELAB database was performed in order to find the best fit of complete visible+infrared (VNIR) spectra of Lutetia. To constrain the possible composition of Steins’ surface, we constructed a simple mixing model using a linear (areal) mix of three components obtained from the RELAB database. A space-weathering model was applied to the aubrite ALH-78113 spectrum. In the case of (21) Lutetia we find a clear spectral variation (slope), and a good correspondence between spectral variations and rotational phase. The surface mixing model places Steins in a subdivision of the E-type class with objects like Angelina, Eger, and Nereus, a group not sampled by the current collection of aubrite meteorites. [ABSTRACT FROM AUTHOR]