Radiative Electroweak Symmetry Breaking in a Little Higgs Model

We present a new Little Higgs model, motivated by the deconstruction of a five-dimensional gauge-Higgs model. The approximate global symmetry is $SO(5)_0\times SO(5)_1$, breaking to $SO(5)$, with a gauged subgroup of $[SU(2)_{0L}\times U(1)_{0R}]\times O(4)_1$, breaking to $SU(2)_L \times U(1)_Y$. Radiative corrections produce an additional small vacuum misalignment, breaking the electroweak symmetry down to $U(1)_{EM}$. Novel features of this model are: the only un-eaten pseudo-Goldstone boson in the effective theory is the Higgs boson; the model contains a custodial symmetry, which ensures that $\hat{T}=0$ at tree-level; and the potential for the Higgs boson is generated entirely through one-loop radiative corrections. A small negative mass-squared in the Higgs potential is obtained by a cancellation between the contribution of two heavy partners of the top quark, which is readily achieved over much of the parameter space. We can then obtain both a vacuum expectation value of $v=246$ GeV and a light Higgs boson mass, which is strongly correlated with the masses of the two heavy top quark partners. For a scale of the global symmetry breaking of $f=1$ TeV and using a single cutoff for the fermion loops, the Higgs boson mass satisfies 120 GeV $\lesssim M_H\lesssim150$ GeV over much of the range of parameter space. For $f$ raised to 10 TeV, these values increase by about 40 GeV. Effects at the ultraviolet cutoff scale may also raise the predicted values of the Higgs boson mass, but the model still favors $M_H\lesssim 200$ GeV.Comment: 32 pages, 10 figures, JHEP style. Version accepted for publication in JHEP. Includes additional discussion of sensitivity to UV effects and fine-tuning, revised Fig. 9, added appendix and additional references

Turbulence and galactic structure

Interstellar turbulence is driven over a wide range of scales by processes including spiral arm instabilities and supernovae, and it affects the rate and morphology of star formation, energy dissipation, and angular momentum transfer in galaxy disks. Star formation is initiated on large scales by gravitational instabilities which control the overall rate through the long dynamical time corresponding to the average ISM density. Stars form at much higher densities than average, however, and at much faster rates locally, so the slow average rate arises because the fraction of the gas mass that forms stars at any one time is low, ~10^{-4}. This low fraction is determined by turbulence compression, and is apparently independent of specific cloud formation processes which all operate at lower densities. Turbulence compression also accounts for the formation of most stars in clusters, along with the cluster mass spectrum, and it gives a hierarchical distribution to the positions of these clusters and to star-forming regions in general. Turbulent motions appear to be very fast in irregular galaxies at high redshift, possibly having speeds equal to several tenths of the rotation speed in view of the morphology of chain galaxies and their face-on counterparts. The origin of this turbulence is not evident, but some of it could come from accretion onto the disk. Such high turbulence could help drive an early epoch of gas inflow through viscous torques in galaxies where spiral arms and bars are weak. Such evolution may lead to bulge or bar formation, or to bar re-formation if a previous bar dissolved. We show evidence that the bar fraction is about constant with redshift out to z~1, and model the formation and destruction rates of bars required to achieve this constancy.Comment: in: Penetrating Bars through Masks of Cosmic Dust: The Hubble Tuning Fork strikes a New Note, Eds., K. Freeman, D. Block, I. Puerari, R. Groess, Dordrecht: Kluwer, in press (presented at a conference in South Africa, June 7-12, 2004). 19 pgs, 5 figure

Comparative approaches to genome evolution in Blastocystis and Entamoeba

Parasitism has arisen independently in numerous lineages of eukaryotes. Investigating the origins of parasitism is a core question in evolutionary biology and allows identification of parasite-specific factors that aid in diagnosis and treatment. Comparative genomic studies have often been applied within clades of parasites, which allows their ancestral state to be imagined, but cannot elucidate the processes that surrounded the emergence of parasitism. This question must be approached by comparison with a free-living out-group, to reconstruct the ancestral non-parasitic state. In this thesis, I examine free-living relatives of two intestinal protists of global importance, Blastocystis sp. and Entamoeba histolytica, to explore their evolution. A draft genome sequence for Proteromonas lacertae, the non-pathogenic sister-taxon of Blastocystis, is presented along with a transcriptome for Cafeteria roenbergensis, a free-living out-group to the Blastocystis-Proteromonas clade. Together with the published Blastocystis sp. genome sequences, the P. lacertae genome and the C. roenbergensis transcriptome were used in a comparative genomic analysis. This revealed that the Blastocystis genomes are genuinely small, compared to other Stramenopiles and that this reduction is genome-wide as well as with respect to specific cellular apparatus, such as the flagellum and other motility-associated genes, which have been totally lost from the ancestor of Blastocystis. Rather than observe the same loss of function from metabolic capability, this reduction was associated with loss of gene complexity and is indicative of genomic streamlining. This is coupled with gene family expansion of Ig-like domain-containing proteins, potentially bestowing adhesive qualities to the cell surface. A transcriptome for Mastigamoeba sp., a free-living out-group to the Entamoeba genus, is also presented. The Mastigamoeba sp. transcriptome was used in a comparative analysis of the E. histolytica genome. This analysis revealed large-scale expansion of Ras-family proteins in the ancestor of Entamoeba, which may be linked to motility and phagocytosis required for pathogenesis. Analysis of cathepsins revealed processes of genomic reduction and expansion occurring within the same gene family indicating genomic streamlining and subsequent specialisation in the parasite. I have shown how we might revisit crucial questions in evolutionary biology using the latest genome sequencing technology. By generating new genomic resources for free-living protists, this thesis exposes the mechanism by which two common intestinal parasites of humans and animals evolved. It makes substantial contribution to our understanding of the origins of parasite genomes, and of microbial biodiversity, while revealing numerous parasite-specific features that will sustain future research

An introduction to Graph Data Management

A graph database is a database where the data structures for the schema and/or instances are modeled as a (labeled)(directed) graph or generalizations of it, and where querying is expressed by graph-oriented operations and type constructors. In this article we present the basic notions of graph databases, give an historical overview of its main development, and study the main current systems that implement them

Higgs boson production in photon-photon collision at ILC: a comparative study in different little Higgs models

We study the process \gamma\gamma->h->bb_bar at ILC as a probe of different little Higgs models, including the simplest little Higgs model (SLH), the littlest Higgs model (LH), and two types of littlest Higgs models with T-parity (LHT-I, LHT-II). Compared with the Standard Model (SM) prediction, the production rate is found to be sizably altered in these little Higgs models and, more interestingly, different models give different predictions. We find that the production rate can be possibly enhanced only in the LHT-II for some part of the parameter space, while in all other cases the rate is suppressed. The suppression can be 10% in the LH and as much as 60% in both the SLH and the LHT-I/LHT-II. The severe suppression in the SLH happens for a large \tan\beta and a small m_h, in which the new decay mode h->\eta\eta (\eta is a light pseudo-scalar) is dominant; while for the LHT-I/LHT-II the large suppression occurs when f and m_h are both small so that the new decay mode h->A_H A_H is dominant. Therefore, the precision measurement of such a production process at the ILC will allow for a test of these models and even distinguish between different scenarios.Comment: Version in JHEP (h-g-g & h-gamma-gamma expressions added

Implications of a High-Mass Diphoton Resonance for Heavy Quark Searches

Heavy vector-like quarks coupled to a scalar $S$ will induce a coupling of this scalar to gluons and possibly (if electrically charged) photons. The decay of the heavy quark into $Sq$, with $q$ being a Standard Model quark, provides, if kinematically allowed, new channels for heavy quark searches. Inspired by naturalness considerations, we consider the case of a vector-like partner of the top quark. For illustration, we show that a singlet partner can be searched for at the 13$\,$TeV LHC through its decay into a scalar resonance in the $2\gamma+\ell + X$ final states, especially if the diphoton branching ratio of the scalar $S$ is further enhanced by the contribution of non coloured particles. We then show that conventional heavy quark searches are also sensitive to this new decay mode, when $S$ decays hadronically, by slightly tightening the current selection cuts. Finally, we comment about the possibility of disentangling, by scrutinising appropriate kinematic distributions, heavy quark decays to $St$ from other standard decay modes.Comment: 8 pages, 3 figures and 1 table; v3: typos fixed. Matches published versio

The stellar and sub-stellar IMF of simple and composite populations

The current knowledge on the stellar IMF is documented. It appears to become top-heavy when the star-formation rate density surpasses about 0.1Msun/(yr pc^3) on a pc scale and it may become increasingly bottom-heavy with increasing metallicity and in increasingly massive early-type galaxies. It declines quite steeply below about 0.07Msun with brown dwarfs (BDs) and very low mass stars having their own IMF. The most massive star of mass mmax formed in an embedded cluster with stellar mass Mecl correlates strongly with Mecl being a result of gravitation-driven but resource-limited growth and fragmentation induced starvation. There is no convincing evidence whatsoever that massive stars do form in isolation. Various methods of discretising a stellar population are introduced: optimal sampling leads to a mass distribution that perfectly represents the exact form of the desired IMF and the mmax-to-Mecl relation, while random sampling results in statistical variations of the shape of the IMF. The observed mmax-to-Mecl correlation and the small spread of IMF power-law indices together suggest that optimally sampling the IMF may be the more realistic description of star formation than random sampling from a universal IMF with a constant upper mass limit. Composite populations on galaxy scales, which are formed from many pc scale star formation events, need to be described by the integrated galactic IMF. This IGIMF varies systematically from top-light to top-heavy in dependence of galaxy type and star formation rate, with dramatic implications for theories of galaxy formation and evolution.Comment: 167 pages, 37 figures, 3 tables, published in Stellar Systems and Galactic Structure, Vol.5, Springer. This revised version is consistent with the published version and includes additional references and minor additions to the text as well as a recomputed Table 1. ISBN 978-90-481-8817-

The stellar halo of the Galaxy

Stellar halos may hold some of the best preserved fossils of the formation history of galaxies. They are a natural product of the merging processes that probably take place during the assembly of a galaxy, and hence may well be the most ubiquitous component of galaxies, independently of their Hubble type. This review focuses on our current understanding of the spatial structure, the kinematics and chemistry of halo stars in the Milky Way. In recent years, we have experienced a change in paradigm thanks to the discovery of large amounts of substructure, especially in the outer halo. I discuss the implications of the currently available observational constraints and fold them into several possible formation scenarios. Unraveling the formation of the Galactic halo will be possible in the near future through a combination of large wide field photometric and spectroscopic surveys, and especially in the era of Gaia.Comment: 46 pages, 16 figures. References updated and some minor changes. Full-resolution version available at http://www.astro.rug.nl/~ahelmi/stellar-halo-review.pd

Adiponectin SNP45TG is associated with gestational diabetes mellitus

INTRODUCTION: Diabetes and pregnancy can be associated in two ways: pregnancy that occurs in women who are already diabetic (diabetes of pre-gestational origin); and diabetes that occur in women who are already pregnant [gestational diabetes mellitus (GDM) (O'sullivan 1961)]. Patients with previous GDM history have higher risk of developing diabetes outside of pregnancy. Accumulating literature had suggested that adiponectin plays a role in the pathophysiology of this metabolic syndrome, and several of the common single nucleotide polymorphisms (SNP) in adiponectin gene have been identified in type 2 diabetes. Thus, one of the commonly found SNP was studied to determine its association with GDM. OBJECTIVE: To identify the association of SNP45TG with GDM. METHODS: This is a cross-sectional study involving pregnant mothers of <18 gestational weeks, who were recruited from three local antenatal clinics in Selangor, Malaysia. Their genomic DNA was extracted from EDTA treated whole blood using commercialized kit. Adiponectin gene was amplified through conventional PCR and SNP was detected using restriction enzyme SmaI. Plasma adiponectin level, fructosamine level and HbA(1c) percentage were also examined. RESULTS: Among the 79 antenatal patients recruited, 53 patients were normal and 26 were diagnosed with GDM. Among the 53 normal patients, 18 carry TG/GG genotype. Meanwhile, among the 26 patients that were diagnosed with GDM 15 carry TG/GG genotype. Significant association was found between SNP45TG with GDM ( χ(2) = 4.038; P < 0.05). In addition, normal patients with TT genotype have significantly higher plasma adiponectin level compared to other groups. CONCLUSION: We concluded that SNP45TG in adiponectin gene is associated with the occurrence of GDM

Interpreting a 750 GeV diphoton resonance

We discuss the implications of the significant excesses in the diphoton final state observed by the LHC experiments ATLAS and CMS around a diphoton invariant mass of 750 GeV. The interpretation of the excess as a spin-zero s-channel resonance implies model-independent lower bounds on both its branching ratio and its coupling to photons, which stringently constrain dynamical models. We consider both the case where the excess is described by a narrow and a broad resonance. We also obtain model-independent constraints on the allowed couplings and branching fractions to final states other than diphotons, by including the interplay with 8 TeV searches. These results can guide attempts to construct viable dynamical models of the resonance. Turning to specific models, our findings suggest that the anomaly cannot be accounted for by the presence of only an additional singlet or doublet spin-zero field and the Standard Model degrees of freedom; this includes all two-Higgs-doublet models. Likewise, heavy scalars in the MSSM cannot explain the excess if stability of the electroweak vacuum is required, at least in a leading-order analysis. If we assume that the resonance is broad we find that it is challenging to find a weakly coupled explanation. However, we provide an existence proof in the form of a model with vectorlike quarks with large electric charge that is perturbative up to the 100 TeV scale. For the narrow-resonance case a similar model can be perturbative up to high scales also with smaller charges. We also find that, in their simplest form, dilaton models cannot explain the size of the excess. Some implications for flavor physics are briefly discussed