Probing the 2D kinematic structure of early-type galaxies out to three effective radii

We detail an innovative new technique for measuring the two-dimensional (2D) velocity moments (rotation velocity, velocity dispersion and Gauss-Hermite coefficients h(3) and h(4)) of the stellar populations of galaxy haloes using spectra from Keck DEIMOS (Deep Imaging Multi-Object Spectrograph) multi-object spectroscopic observations. The data are used to reconstruct 2D rotation velocity maps. Here we present data for five nearby early-type galaxies to similar to three effective radii. We provide significant insights into the global kinematic structure of these galaxies, and challenge the accepted morphological classification in several cases. We show that between one and three effective radii the velocity dispersion declines very slowly, if at all, in all five galaxies. For the two galaxies with velocity dispersion profiles available from planetary nebulae data we find very good agreement with our stellar profiles. We find a variety of rotation profiles beyond one effective radius, i.e. rotation speed remaining constant, decreasing and increasing with radius. These results are of particular importance to studies which attempt to classify galaxies by their kinematic structure within one effective radius, such as the recent definition of fast- and slow-rotator classes by the Spectrographic Areal Unit for Research on Optical Nebulae project. Our data suggest that the rotator class may change when larger galactocentric radii are probed. This has important implications for dynamical modelling of early-type galaxies. The data from this study are available on-line.

Discovery of two distinct red clumps in NGC 419: a rare snapshot of a cluster at the onset of degeneracy

Colour-magnitude diagrams (CMDs) of the Small Magellanic Cloud (SMC) star cluster NGC 419, derived from Hubble Space Telescope (HST)/Advanced Camera for Surveys (ACS) data, reveal a well-delineated secondary clump located below the classical compact red clump typical of intermediate-age populations. We demonstrate that this feature belongs to the cluster itself, rather than to the underlying SMC field. Then, we use synthetic CMDs to show that it corresponds very well to the secondary clump predicted to appear as a result of He-ignition in stars just massive enough to avoid e(-)-degeneracy settling in their H-exhausted cores. The main red clump instead is made of the slightly less massive stars which passed through e(-) degeneracy and ignited He at the tip of the red giant branch. In other words, NGC 419 is the rare snapshot of a cluster while undergoing the fast transition from classical to degenerate H-exhausted cores. At this particular moment of a cluster`s life, the colour distance between the main-sequence turn-off and the red clump(s) depends sensitively on the amount of convective core overshooting, Lambda(c). By coupling measurements of this colour separation with fits to the red clump morphology, we are able to estimate simultaneously the cluster mean age (1.35(-0.04)(+0.11) Gyr) and overshooting efficiency (Lambda(c) = 0.47(-0.04)(+0.14)). Therefore, clusters like NGC 419 may constitute important marks in the age scale of intermediate-age populations. After eye inspection of other CMDs derived from HST/ACS data, we suggest that the same secondary clump may also be present in the Large Magellanic Cloud clusters NGC 1751, 1783, 1806, 1846, 1852 and 1917.

CDM accelerating cosmology as an alternative to Lambda CDM model

A new accelerating cosmology driven only by baryons plus cold dark matter (CDM) is proposed in the framework of general relativity. In this scenario the present accelerating stage of the Universe is powered by the negative pressure describing the gravitationally-induced particle production of cold dark matter particles. This kind of scenario has only one free parameter and the differential equation governing the evolution of the scale factor is exactly the same of the Lambda CDM model. For a spatially flat Universe, as predicted by inflation (Omega(dm) + Omega(baryon) = 1), it is found that the effectively observed matter density parameter is Omega(meff) = 1 - alpha, where alpha is the constant parameter specifying the CDM particle creation rate. The supernovae test based on the Union data (2008) requires alpha similar to 0.71 so that Omega(meff) similar to 0.29 as independently derived from weak gravitational lensing, the large scale structure and other complementary observations.

Stigmatic surface in the Vochysiaceae: reproductive and taxonomic implications

(Stigmatic surface, reproductive biology and taxonomy of the Vochysiaceae). The Vochysiaceae are Neotropical trees and shrubs, common in the savanna areas in Central Brazil (Cerrados). The family has been traditionally divided into two tribes: Erismeae, with three genera, and Vochysieae, with five genera. We investigated the stigmatic surface of six Vochysiaceae species, belonging to four genera of Vochysieae: Vochysia, Salvertia, Callisthene and Qualea. Flowers and buds at different developmental stages were collected. Morphological features were observed on fresh material and stigmatic receptivity was inferred based on esterasic activity. Pistils were fixed and embedded in paraplast and sectioned on a rotary microtome; the sections were stained before histological analysis. Stigmas of open flowers were also observed by scanning electron microscopy. Stigmas of all species were wet and showed esterasic activity at pre-anthesis and anthesis stages. Stigmatic surface was continuous with transmitting tissue of glandular nature. Vochysia and Salvertia stigmatic surfaces were formed by multicelular uniseriate hairs, and species of the remaining genera showed papillate surface. The exudate over mature stigmas in all species flowed without rupture of stigmatic Surface and pollen tubes grew down between hairs or papillae. Differences on the stigmatic surface agreed with a phylogenetic reconstruction that separated two clades and indicated that Vochysieae is not monophyletic. Stigmatic features could not be associated with pollination and breeding systems.

Stigma/style cell cycle inhibitor 1 (SCI1), a tissue-specific cell cycle regulator that controls upper pistil development

P>A cDNA encoding a small lysine-rich protein of unknown function was identified in a tobacco (Nicotiana tabacum) stigma/style suppression subtractive hybridization cDNA library. After its characterization, the corresponding gene was designated stigma/style cell cycle inhibitor 1 (SCI1). Fluorescence microscopy with an SCI1-GFP protein fusion demonstrated its nuclear localization, which was confined to the interchromatic region. Real-time RT-PCR and in situ hybridization experiments showed that SCI1 is stigma/style-specific and developmentally regulated. SCI1 RNAi knockdown and overexpression plants had stigmas/styles with remarkably enlarged and reduced areas, respectively, which was attributable to differences in cell numbers. These results indicate that SCI1 is a tissue-specific negative cell cycle regulator. The differences in cell division had an effect on the timing of the differentiation of the stigmatic papillar cells, suggesting that their differentiation is coupled to stigma cell divisions. This is consistent with a role for SCI1 in triggering differentiation through cell proliferation control. Our results revealed that SCI1 is a novel tissue-specific gene that controls cell proliferation/differentiation, probably as a component of a developmental signal transduction pathway.

TICK INNATE IMMUNITY

Ticks are blood feeding parasites transmitting a wide variety of pathogens to their vertebrate hosts. The vector competence of ticks is tightly linked with their immune system. Despite its importance, our knowledge of tick innate immunity is still inadequate and the limited number of sufficiently characterized immune molecules and cellular reactions are dispersed across numerous tick species. The phagocytosis of microbes by tick hemocytes seems to be coupled with a primitive complement-like system, which possibly involves self/nonself recognition by fibrinogen-related lectins and the action of thioester-containing proteins. Ticks do not seem to possess a pro-phenoloxidase system leading to melanization and also coagulation of tick hemolymph has not been experimentally proven. They are capable of defending themselves against microbial infection with a variety of antimicrobial peptides comprising lysozymes, defensins and molecules not found in other invertebrates. Virtually nothing is known about the signaling cascades involved in the regulation of tick antimicrobial immune responses. Midgut immunity is apparently the decisive factor of tick vector competence. The gut content is a hostile environment for ingested microbes, which is mainly due to the antimicrobial activity of hemoglobin fragments generated by the digestion of the host blood as well as other antimicrobial peptides. Reactive oxygen species possibly also play an important role in the tick-pathogen interaction. The recent release of the Ixodes scapularis genome and the feasibility of RNA interference in ticks promise imminent and substantial progress in tick innate immunity research.

The imprint of the interaction between dark sectors in galaxy clusters

Based on perturbation theory, we study the dynamics of how dark matter and dark energy in the collapsing system approach dynamical equilibrium when they are in interaction. We find that the interaction between dark sectors cannot ensure the dark energy to fully cluster along with dark matter. When dark energy does not trace dark matter, we present a new treatment on studying the structure formation in the spherical collapsing system. Furthermore we examine the cluster number counts dependence on the interaction between dark sectors and analyze how dark energy inhomogeneities affect cluster abundances. It is shown that cluster number counts can provide specific signature of dark sectors interaction and dark energy inhomogeneities.

The signature of dark energy perturbations in galaxy cluster surveys

Models of dynamical dark energy unavoidably possess fluctuations in the energy density and pressure of that new component. In this paper we estimate the impact of dark energy fluctuations on the number of galaxy clusters in the Universe using a generalization of the spherical collapse model and the Press-Schechter formalism. The observations we consider are several hypothetical Sunyaev-Zel`dovich and weak lensing (shear maps) cluster surveys, with limiting masses similar to ongoing (SPT, DES) as well as future (LSST, Euclid) surveys. Our statistical analysis is performed in a 7-dimensional cosmological parameter space using the Fisher matrix method. We find that, in some scenarios, the impact of these fluctuations is large enough that their effect could already be detected by existing instruments such as the South Pole Telescope, when priors from other standard cosmological probes are included. We also show how dark energy fluctuations can be a nuisance for constraining cosmological parameters with cluster counts, and point to a degeneracy between the parameter that describes dark energy pressure on small scales (the effective sound speed) and the parameters describing its equation of state.

Signature of the interaction between dark energy and dark matter in galaxy clusters

We investigate the influence of ail interaction between dark energy and dark matter upon the dynamics of galaxy clusters. We obtain file general Layser-Irvine equation in the presence of interactions, and find how, in that case. the virial theorem stands corrected. Using optical, X-ray and weak lensing data from 33 relaxed galaxy clusters, we put constraints on the strength of the coupling between the dark sectors. Available data Suggests that this coupling is small but positive, indicating that dark energy might be decaying into dark matter. Systematic effects between the several mass estimates, however, should be better known, before definitive conclusions oil the magnitude and significance of this coupling could be established. (C) 2009 Published by Elsevier B.V.

Update on the correlation of the highest energy cosmic rays with nearby extragalactic matter

Data collected by the Pierre Auger Observatory through 31 August 2007 showed evidence for anisotropy in the arrival directions of cosmic rays above the Greisen-Zatsepin-Kuz`min energy threshold, 6 x 10(19) eV. The anisotropy was measured by the fraction of arrival directions that are less than 3.1 degrees from the position of an active galactic nucleus within 75 Mpc (using the Veron-Cetty and Veron 12th catalog). An updated measurement of this fraction is reported here using the arrival directions of cosmic rays recorded above the same energy threshold through 31 December 2009. The number of arrival directions has increased from 27 to 69, allowing a more precise measurement. The correlating fraction is (38(-6)(+7))%, compared with 21% expected for isotropic cosmic rays. This is down from the early estimate of (69-(+11)(13))%. The enlarged set of arrival directions is examined also in relation to other populations of nearby extragalactic objects: galaxies in the 2 Microns All Sky Survey and active galactic nuclei detected in hard X-rays by the Swift Burst Alert Telescope. A celestial region around the position of the radiogalaxy Cen A has the largest excess of arrival directions relative to isotropic expectations. The 2-point autocorrelation function is shown for the enlarged set of arrival directions and compared to the isotropic expectation. (C) 2010 Elsevier B.V. All rights reserved.

Ausencia, prohibición y carencia : Estudio de los personajes y el deseo frustrado en tres obras de García Lorca

In this thesis, the main male characters in three of the plays written by Federico García Lorca are analysed with the aim of seeingthe role they play in the frustration of desire. After two chapters dedicated to a review of published critical studies on Lorca and tocertain theoretical considerations, Chapter Three examines desire drawing on Ubersfeld's actancial model and observes that thesemale characters can be divided into two groups: those who are desired and those who are undesired.In Chapter Four this classification is linked to an analysis of absence, prohibition and lack. Absence is here defined not asrelated to their non-appearance on stage but rather to their non-presence in the lives of the desiring female protagonists. It isobserved that a number of male characters are absent in the plays mainly due to death or a journey. As far as prohibition isconcerned, in two of the works, there is a moral code associated with concepts such as "honour" and "decency", which blocks thefemale characters' access to the males they desire. Chapter Four also shows how several characters can be considered as lacking inthe sense that they do not possess the ideal male qualities contained in the plays. This chapter reaches the conclusion that desiredmale characters are either absent or forbidden in the world of the desiring female, whereas undesired male characters are lacking inthe sense that they fail to live up to the ideal highlighted in the plays.Chapter Five analyses the female characters' perception of the male figures, making use of René Girard's notion of"transfiguration", which alludes to a process of idealisation of the object of desire. Our analysis reveals a connection betweendesire, denied access to the object of desire and transfiguration in the main subjects of desire. The phenomenon of "transfiguration"has several functions in the play: firstly, the creation of hyperbolical male characters; secondly, that of transmitting the intensity ofthe desire experienced and, finally, the highlighting of the lack of certain qualities in several male characters.We thus observe that, in these three plays written by García Lorca, Girard's pessimistic view of desire is confirmed, since desireneeds a series of obstacles, such as absence or prohibition, to survive. However, this is not the only explanation for the frustrationof desire: other factors, like the actions of certain male characters or destiny, also play a decisive role.

Análise de campos profundos da LMC imageados com o HST

Apresentamos fotometria profunda (V ~ 25,5) nas bandas V e I obtidas com a Wide Field and Planetary Camera 2 a bordo do telesc opio espacial Hubble para 7 campos distantes ~5º do centro da Grande Nuvem de Magalhães. Ajustamos isócronas aos diagramas cor-magnitude a fim de identficar diferentes populaões estelares nestes campos. Uma população velha (τ > 10¹º anos) foi encontrada em todos os campos. Alguns eventos de elevada formação estelar, com idades entre 2 x 109 e 4 x 109 anos, foram também encontrados em alguns campos localizados na região N/NO. Funções de luminosidade de estrelas de baixa massa (m ≤ 1; 1msol) foram obtidas para todos os campos. Aparentemente não há diferenças na mistura de populações entre os campos como sugerido através do teste Kolmogorov-Smirnov aplicados as funções de luminosidade. Finalmente, derivamos perfis de densidade para estrelas velhas e de idade intermediária. O primeiro apresenta uma inclinação levemente maior quando comparado com o último.

O gás ionizado em galáxias ativas

Foram analisados espectros óticos de fenda longa de 29 galáxias que hospedam núcleos ativos (AGNs), sendo 6 galáxias Seyfert 1, 18 galáxias Seyfert 2, 4 Rádio-galáxias de linhas estreitas (NLRG) e 1 Rádio-galáxia de linhas largas (BLRG). Estas galáxias apresentam emissão por gás de alta excitação que se estende em alguns casos a 10 kpc do núcleo. O objetivo do presente trabalho consiste em estudar e caracterizar as propriedades físicas da região estendida de linhas estreitas (ENLR) destes objetos bem como propriedades da fonte central. A distribuição radial de parâmetros que caracterizam o gás emissor em cada galáxia, tais como brilho superficial das linhas de emissão, densidade do gás, massa, extinção e excitação são obtidos. Estes valores característicos são comparados entre as diferentes classes de atividade nuclear presentes em nossa amostra, bem como às propriedades de galáxias normais com o mesmo tipo de Hubble quando possível. Nós encontramos que a massa de gás ionizado é consistente com a hipótese de que o gás é “originado” na fotoionização pela fonte central das nuvens de HI préexistentes na galáxia hospedeira. Os valores observados das razões entre as linhas estreitas de emissão são comparados com os obtidos através de modelos de fotoionização gerados com o código MAPPINGS Ic, obtendo os parâmetros do modelo – densidade, índice espectral da distribuição de energia e da metalicidade do gás – que melhor reproduzem as observações. Observamos que a variação da abundância química do gás é necessária para explicar o espalhamento nos valores observados. Adicionalmente, comparamos os valores observados com os obtidos com modelos de choques gerados por Dopita & Sutherland. Investigamos também a influência da emissão proveniente de regiões HII ao espectro observado – a qual concluímos ser importante particularmente nas regiões emissoras mais distantes do que 2 kpc do núcleo. Nós determinamos a luminosidade ionizante da fonte central nos AGNs usando a aproximação de que as nuvens de gás são limitadas por radiação, e obtivemos os correspondentes valores para o fator de cobertura do gás. Esta luminosidade ionizante foi então comparada com a luminosidade observada em raios-X na banda 2 –10 keV, através de aproximações para a distribuição espectral de energia (SED). Para 9 galáxias Seyfert 2 a luminosidade observada está disponível, e verificamos que nosso método recupera a luminosidade do AGN em raios-X – assim como obtida dos dados do satélite ASCA – bem como identifica os 3 casos Compton espessos. Por fim, investigamos a natureza do contínuo infravermelho (IR) médio e distante – comparandose a luminosidade observada no IR, calculada a partir dos fluxos IRAS, com a luminosidade predita para um toro que envolve a fonte central absorvendo a radiação incidente e re-emitindo esta no infravermelho. Encontramos que a luminosidade observada no IR é consistente com a luminosidade predita para o torus.

Vínculos ao histórico de formação estelar da LMC

Apresentamos a fotometria de 6 campos estelares profundos distribuídos na Grande Nuvem de Magalhães obtidos com a Wide Field and Planetary Camera 2/Hubble Space Telescope em duas bandas fotométricas: F814W (~I) e F555W (~V). Foram selecionadas ao todo 15997 estrelas pela nossa amostra, que somadas às estrelas da amostra de Castro et aI. 2001 [9] contabilizaram 22239 estrelas, dentro de limites de magnitude típicos que estão no intervalo 18.5<-V <-26. Investigamos o comportamento do erro fotométrico através da tarefa PHOT/IRAF, bem como via medidas independentes de magnitude de um mesmo objeto obtidas com diferentes exposições. Implementamos um método de correção para a completeza fotométrica como função da posição no diagrama cor-magnitude, isto é, com função tanto da magnitude como da cor e analisamos a sensibilidade das funções de luminosidade obtidas para diferentes métodos de correção. Foram obtidos os diagramas cor-magnitude, com os quais ajustamos isócronas de Pádova com idades T ;S 16 Gano e metalicidades 0.001 < Z < 0.004 ou -1.3 < [Fe/H] < -0.7. A população mais velha (r~12 Gano) pode ser encontrada através do ponto de turn-off em V~22. Estrelas de idade intermediária (r~1 - 8 Gano) podem ser localizadas pela presença de um clump. Os campos próximos aos aglomerados jovens NGC1805 e NGC1818 são os campos mais populosos, apresentando estrelas com r~1 Gano. Construímos funções de luminosidade para 18.5<-V <-25, utilizando os dados das duas amostras; não foram encontradas diferenças significativas entre os campos Desenvolvemos um método para geração de diagramas cor-magnitude (CMDs) artificiais a partir de um modelo de histórico de formação estelar. Este método incorpora os efeitos de erros fotométricos, binarismo não resolvido, avermelhamento e permite o uso de formas variadas de função de massa inicial e do próprio histórico. Implementamos o Método dos Modelos Parciais para modelamento de CMDs, incluindo experimentos controlados para a comprovação da validade deste método na busca de vínculos ao histórico de formação estelar da Grande Nuvem de Magalhães em dife!entes regiões. Recuperamos SFHs confiáveis para cada um dos 6 campos da LMC. Observamos variações na formação estelar de um campo para outro. Em todos os campos encontramos uma lacuna na formação estelar com 7 rv 700 Mano. Os dois campos próximos à barra (NGC1805 e NGC1818) apresentam alguns pequenos surtos, tendo formado em sua maioria, estrelas velhas ou relativamente jovens. Já os campos próximos a NGC1831 e NGC1868 apresentam formação estelar que se aproxima de um histórico de formação estelar uniforme, com alguns pequenos surtos. Os campos NGC2209 e Hodge 11 apresentam três períodos de formação estelar muitos semelhantes.

Multilayer optimization in radio resource allocation for the packet transmission in wireless networks

In the last decade mobile wireless communications have witnessed an explosive growth in the user’s penetration rate and their widespread deployment around the globe. It is expected that this tendency will continue to increase with the convergence of fixed Internet wired networks with mobile ones and with the evolution to the full IP architecture paradigm. Therefore mobile wireless communications will be of paramount importance on the development of the information society of the near future. In particular a research topic of particular relevance in telecommunications nowadays is related to the design and implementation of mobile communication systems of 4th generation. 4G networks will be characterized by the support of multiple radio access technologies in a core network fully compliant with the Internet Protocol (all IP paradigm). Such networks will sustain the stringent quality of service (QoS) requirements and the expected high data rates from the type of multimedia applications to be available in the near future. The approach followed in the design and implementation of the mobile wireless networks of current generation (2G and 3G) has been the stratification of the architecture into a communication protocol model composed by a set of layers, in which each one encompasses some set of functionalities. In such protocol layered model, communications is only allowed between adjacent layers and through specific interface service points. This modular concept eases the implementation of new functionalities as the behaviour of each layer in the protocol stack is not affected by the others. However, the fact that lower layers in the protocol stack model do not utilize information available from upper layers, and vice versa, downgrades the performance achieved. This is particularly relevant if multiple antenna systems, in a MIMO (Multiple Input Multiple Output) configuration, are implemented. MIMO schemes introduce another degree of freedom for radio resource allocation: the space domain. Contrary to the time and frequency domains, radio resources mapped into the spatial domain cannot be assumed as completely orthogonal, due to the amount of interference resulting from users transmitting in the same frequency sub-channel and/or time slots but in different spatial beams. Therefore, the availability of information regarding the state of radio resources, from lower to upper layers, is of fundamental importance in the prosecution of the levels of QoS expected from those multimedia applications. In order to match applications requirements and the constraints of the mobile radio channel, in the last few years researches have proposed a new paradigm for the layered architecture for communications: the cross-layer design framework. In a general way, the cross-layer design paradigm refers to a protocol design in which the dependence between protocol layers is actively exploited, by breaking out the stringent rules which restrict the communication only between adjacent layers in the original reference model, and allowing direct interaction among different layers of the stack. An efficient management of the set of available radio resources demand for the implementation of efficient and low complexity packet schedulers which prioritize user’s transmissions according to inputs provided from lower as well as upper layers in the protocol stack, fully compliant with the cross-layer design paradigm. Specifically, efficiently designed packet schedulers for 4G networks should result in the maximization of the capacity available, through the consideration of the limitations imposed by the mobile radio channel and comply with the set of QoS requirements from the application layer. IEEE 802.16e standard, also named as Mobile WiMAX, seems to comply with the specifications of 4G mobile networks. The scalable architecture, low cost implementation and high data throughput, enable efficient data multiplexing and low data latency, which are attributes essential to enable broadband data services. Also, the connection oriented approach of Its medium access layer is fully compliant with the quality of service demands from such applications. Therefore, Mobile WiMAX seems to be a promising 4G mobile wireless networks candidate. In this thesis it is proposed the investigation, design and implementation of packet scheduling algorithms for the efficient management of the set of available radio resources, in time, frequency and spatial domains of the Mobile WiMAX networks. The proposed algorithms combine input metrics from physical layer and QoS requirements from upper layers, according to the crosslayer design paradigm. Proposed schedulers are evaluated by means of system level simulations, conducted in a system level simulation platform implementing the physical and medium access control layers of the IEEE802.16e standard.