Fingerprints of the Hierarchical Building up of the Structure on the Mass-Metallicity Relation

We study the mass-metallicity relation of galactic systems with stellar masses larger than 10^9 Mo in Lambda-CDM scenarios by using chemical hydrodynamical simulations. We find that this relation arises naturally as a consequence of the formation of the structure in a hierarchical scenario. The hierarchical building up of the structure determines a characteristic stellar mass at M_c ~10^10.2 Moh^-1 which exhibits approximately solar metallicities from z ~ 3 to z=0. This characteristic mass separates galactic systems in two groups with massive ones forming most of their stars and metals at high redshift. We find evolution in the zero point and slope of the mass-metallicity relation driven mainly by the low mass systems which exhibit the larger variations in the chemical properties. Although stellar mass and circular velocity are directly related, the correlation between circular velocity and metallicity shows a larger evolution with redshift making this relation more appropriate to confront models and observations. The dispersion found in both relations is a function of the stellar mass and reflects the different dynamical history of evolution of the systems.Comment: 4 pages, 4 figures. Accepted MNRAS Letter

Clues for the origin of the fundamental metallicity relations. I: The hierarchical building up of the structure

We analyse the evolutionary history of galaxies formed in a hierarchical scenario consistent with the concordance $\Lambda$-CDM model focusing on the study of the relation between their chemical and dynamical properties. Our simulations consistently describe the formation of the structure and its chemical enrichment within a cosmological context. Our results indicate that the luminosity-metallicity (LZR) and the stellar mass-metallicity (MZR) relations are naturally generated in a hierarchical scenario. Both relations are found to evolve with redshift. In the case of the MZR, the estimated evolution is weaker than that deduced from observational works by approximately 0.10 dex. We also determine a characteristic stellar mass, $M_c \approx 3 \times 10^{10} M_{\odot}$, which segregates the simulated galaxy population into two distinctive groups and which remains unchanged since $z\sim 3$, with a very weak evolution of its metallicity content. The value and role played by $M_c$ is consistent with the characteristic mass estimated from the SDSS galaxy survey by Kauffmann et al. (2004). Our findings suggest that systems with stellar masses smaller than $M_c$ are responsible for the evolution of this relation at least from $z\approx 3$. Larger systems are stellar dominated and have formed more than 50 per cent of their stars at $z \ge 2$, showing very weak evolution since this epoch. We also found bimodal metallicity and age distributions from $z\sim3$, which reflects the existence of two different galaxy populations. Although SN feedback may affect the properties of galaxies and help to shape the MZR, it is unlikely that it will significantly modify $M_c$ since, from $z=3$ this stellar mass is found in systems with circular velocities larger than 100 \kms.Comment: 17 pages, 13 figures. Minor changes to match accepted version. Accepted October 3 MNRA

Milky Way type galaxies in a LCDM cosmology

We analyse a sample of 52,000 Milky Way (MW) type galaxies drawn from the publicly available galaxy catalogue of the Millennium Simulation with the aim of studying statistically the differences and similarities of their properties in comparison to our Galaxy. Model galaxies are chosen to lie in haloes with maximum circular velocities in the range 200-250 km/seg and to have bulge-to-disk ratios similar to that of the Milky Way. We find that model MW galaxies formed quietly through the accretion of cold gas and small satellite systems. Only 12 per cent of our model galaxies experienced a major merger during their lifetime. Most of the stars formed in situ, with only about 15 per cent of the final mass gathered through accretion. Supernovae and AGN feedback play an important role in the evolution of these systems. At high redshifts, when the potential wells of the MW progenitors are shallower, winds driven by supernovae explosions blow out a large fraction of the gas and metals. As the systems grow in mass, SN feedback effects decrease and AGN feedback takes over, playing a more important role in the regulation of the star formation activity at lower redshifts. Although model Milky Way galaxies have been selected to lie in a narrow range of maximum circular velocities, they nevertheless exhibit a significant dispersion in the final stellar masses and metallicities. Our analysis suggests that this dispersion results from the different accretion histories of the parent dark matter haloes. Statically, we also find evidences to support the Milky Way as a typical Sb/Sc galaxy in the same mass range, providing a suitable benchmark to constrain numerical models of galaxy formationComment: 10 pages, 7 figures, mne2.cls, MNRAS, replaced with accepted versio

Vibrations of free and embedded anisotropic elastic spheres: Application to low-frequency Raman scattering of silicon nanoparticles in silica

Vibrational mode frequencies and damping are calculated for an elastic sphere embedded in an infinite, homogeneous, isotropic elastic medium. Anisotropic elasticity of the sphere significantly shifts the frequencies in comparison to simplified calculations that assume isotropy. New low frequency Raman light scattering data are presented for silicon spheres grown in a SiO2 glass matrix. Principal features of the Raman spectrum are not correctly described by a simple model of the nanoparticle as a free, isotropic sphere, but require both matrix effects and the anisotropy of the silicon to be taken into account. Libration, not vibration, is the dominant mechanism

An Imperative for Change: Bridging Special and Language Learning Education to Ensure a Free and Appropriate Education in the Least Restrictive Environment for ELLs with Disabilities in Massachusetts

English Language Learners (ELLs) are the fastest-growing group of school-age students in public schools across the nation, and in Massachusetts. In this state, even as the total student enrollment declines slightly, the number of ELLs grows steeply. They number 68,820 in the 2010-2011 school year, an increase of 9,662 from the year before. The number of ELLs identified as also having a disability doubled in Massachusetts (a striking increase of 115.4%) from 2001-2002 to 2010-2011. The proportion of ELLs placed in Special Education has increased by 5 percentage points, from 9.8% to 14.8%. This time period coincides almost exactly with the implementation of Question 2 (a public referendum approved by voters in 2002), which changed the state’s primary Language Learning Education policy from Transitional Bilingual Education to Sheltered English immersion, a language-restrictive policy similar to those in California and Arizona. Misrepresentation of language minorities in Special Education has been a major problem in education for many years in the United States, including Massachusetts

Superscaling in electron- and neutrino-nucleus scattering

The superscaling properties of electron scattering data are used to extract model-independent predictions for neutrino-nucleus cross sections.Comment: Contibution to NuInt05, 4th international workshop on neutrino-nucleus interaction in the few GeV region, Sept. 26 - 29 2005, Okayama, Japa

Calculation of Field Quality in Fast-Ramping Superconducting Magnets

Fast-ramping superconducting (SC) accelerator magnets are the subject of R&D efforts at various laboratories. The simulation of field quality in fast-ramping magnets requires modifications of magnet design tools such as the CERN field computation program ROXIE. In this paper we present the efforts towards dynamic 2-D simulations of fast-ramping SC magnets. Models for persistent currents, inter-strand coupling currents, inter-filament coupling currents, and for eddy-currents in conducting coil-wedges are described and validated