First stars XII. Abundances in extremely metal-poor turnoff stars, and comparison with the giants

Context. The detailed chemical abundances of extremely metal-poor (EMP) stars are key guides to understanding the early chemical evolution of the Galaxy. Most existing data, however, treat giant stars that may have experienced internal mixing later. Aims. We aim to compare the results for giants with new, accurate abundances for all observable elements in 18 EMP turno. stars. Methods. VLT/UVES spectra at R similar to 45 000 and S/N similar to 130 per pixel (lambda lambda 330-1000 nm) are analysed with OSMARCS model atmospheres and the TURBOSPECTRUM code to derive abundances for C, Mg, Si, Ca, Sc, Ti, Cr, Mn, Co, Ni, Zn, Sr, and Ba. Results. For Ca, Ni, Sr, and Ba, we find excellent consistency with our earlier sample of EMP giants, at all metallicities. However, our abundances of C, Sc, Ti, Cr, Mn and Co are similar to 0.2 dex larger than in giants of similar metallicity. Mg and Si abundances are similar to 0.2 dex lower (the giant [Mg/Fe] values are slightly revised), while Zn is again similar to 0.4 dex higher than in giants of similar [Fe/H] (6 stars only). Conclusions. For C, the dwarf/giant discrepancy could possibly have an astrophysical cause, but for the other elements it must arise from shortcomings in the analysis. Approximate computations of granulation (3D) effects yield smaller corrections for giants than for dwarfs, but suggest that this is an unlikely explanation, except perhaps for C, Cr, and Mn. NLTE computations for Na and Al provide consistent abundances between dwarfs and giants, unlike the LTE results, and would be highly desirable for the other discrepant elements as well. Meanwhile, we recommend using the giant abundances as reference data for Galactic chemical evolution models.

DERIVING METALLICITIES FROM THE INTEGRATED SPECTRA OF EXTRAGALACTIC GLOBULAR CLUSTERS USING THE NEAR-INFRARED CALCIUM TRIPLET

The Ca II triplet (CaT) feature in the near-infrared has been employed as a metallicity indicator for individual stars as well as integrated light of Galactic globular clusters (GCs) and galaxies with varying degrees of success, and sometimes puzzling results. Using the DEIMOS multi-object spectrograph on Keck we obtain a sample of 144 integrated light spectra of GCs around the brightest group galaxy NGC 1407 to test whether the CaT index can be used as ametallicity indicator for extragalactic GCs. Different sets of single stellar population models make different predictions for the behavior of the CaT as a function of metallicity. In this work, the metallicities of the GCs around NGC 1407 are obtained from CaT index values using an empirical conversion. The measured CaT/metallicity distributions show unexpected features, the most remarkable being that the brightest red and blue GCs have similar CaT values despite their large difference in mean color. Suggested explanations for this behavior in the NGC 1407 GC system are (1) the CaT may be affected by a population of hot blue stars, (2) the CaT may saturate earlier than predicted by the models, and/or (3) color may not trace metallicity linearly. Until these possibilities are understood, the use of the CaT as a metallicity indicator for the integrated spectra of extragalactic GCs will remain problematic.

A comparison of dry and wet season aerosol number fluxes over the Amazon rain forest

Vertical number fluxes of aerosol particles and vertical fluxes of CO(2) were measured with the eddy covariance method at the top of a 53 m high tower in the Amazon rain forest as part of the LBA (The Large Scale Biosphere Atmosphere Experiment in Amazonia) experiment. The observed aerosol number fluxes included particles with sizes down to 10 nm in diameter. The measurements were carried out during the wet and dry season in 2008. In this study focus is on the dry season aerosol fluxes, with significant influence from biomass burning, and these are compared with aerosol fluxes measured during the wet season. Net particle deposition fluxes dominated in daytime in both seasons and the deposition flux was considerably larger in the dry season due to the much higher dry season particle concentration. The particle transfer velocity increased linearly with increasing friction velocity in both seasons. The difference in transfer velocity between the two seasons was small, indicating that the seasonal change in aerosol number size distribution is not enough for causing any significant change in deposition velocity. In general, particle transfer velocities in this study are low compared to studies over boreal forests. The reasons are probably the high percentage of accumulation mode particles and the low percentage of nucleation mode particles in the Amazon boundary layer, both in the dry and wet season, and low wind speeds in the tropics compared to the midlatitudes. In the dry season, nocturnal particle fluxes behaved very similar to the nocturnal CO(2) fluxes. Throughout the night, the measured particle flux at the top of the tower was close to zero, but early in the morning there was an upward particle flux peak that is not likely a result of entrainment or local pollution. It is possible that these morning upward particle fluxes are associated with emission of primary biogenic particles from the rain forest. Emitted particles may be stored within the canopy during stable conditions at nighttime, similarly to CO(2), and being released from the canopy when conditions become more turbulent in the morning.

Substructure and Dynamics of the Fornax Cluster

We present the first dynamical analysis of a galaxy cluster to include a large fraction of dwarf galaxies. Our sample of 108 Fornax Cluster members measured with the UK Schmidt Telescope FLAIR-II spectrograph contains 55 dwarf galaxies (15.5 > b(j) > 18.0 or -16 > M-B > -13.5). H alpha emission shows that of the dwarfs are star forming, twice the fraction implied by morphological classifications. The total sample has a mean velocity of 1493 +/- 36 kms s(-1) and a velocity dispersion of 374 +/- 26 km s(-1). The dwarf galaxies form a distinct population: their velocity dispersion (429 +/- 41 km s(-1)) is larger than that of the giants () at the 98% confidence level. This suggests that the dwarf population is dominated by infalling objects whereas the giants are virialized. The Fornax system has two components, the main Fornax Cluster centered on NGC 1399 with cz = 1478 km s(-1) and sigma (cz) = 370 km s(-1) and a subcluster centered 3 degrees to the southwest including NGC 1316 with cz = 1583 km s(-1) and sigma (cz) = 377 km s(-1). This partition is preferred over a single cluster at the 99% confidence level. The subcluster, a site of intense star formation, is bound to Fornax and probably infalling toward the cluster core for the first time. We discuss the implications of this substructure for distance estimates of the Fornax Cluster. We determine the cluster mass profile using the method of Diaferio, which does not assume a virialized sample. The mass within a projected radius of 1.4 Mpc is (7 +/- 2) x 10(13) M-., and the mass-to-light ratio is 300 +/- 100 M-./L-.. The mass is consistent with values derived from the projected mass virial estimator and X-ray measurements at smaller radii.

Compact stellar systems in the Fornax Cluster: Super-massive star clusters or extremely compact dwarf galaxies?

We describe a population of compact objects in the centre of the Fornax Cluster which were discovered as part of our 2dF Fornax Spectroscopic Survey. These objects have spectra typical of old stellar systems, but are unresolved on photographic sky survey plates. They have absolute magnitudes - 13 < M-B

Galaxy threshing and the formation of ultracompact dwarf galaxies

Recent spectroscopic and morphological observational studies of galaxies around NGC 1399 in the Fornax Cluster have discovered several ultracompact dwarf galaxies with intrinsic sizes of similar to 100 pc and absolute B-band magnitudes ranging from -13 to -11 mag. In order to elucidate the origin of these enigmatic objects, we perform numerical simulations on the dynamical evolution of nucleated dwarf galaxies orbiting NGC 1399 and suffering from its strong tidal gravitational field. Adopting a plausible scaling relation for dwarf galaxies, we find that the outer stellar components of a nucleated dwarf are totally removed. This is due to them being tidally stripped over the course of several passages past the central region of NGC 1399. The nucleus, however, manages to survive. We also find that the size and luminosity of the remnant are similar to those observed for ultracompact dwarf galaxies, if the simulated precursor nucleated dwarf has a mass of similar to 10(8) M.. These results suggest that ultracompact dwarf galaxies could have previously been more luminous dwarf spheroidal or elliptical galaxies with rather compact nuclei.

The large-scale distribution of neutral hydrogen in the Fornax region

Using data from the H I Parkes All Sky Survey (HIPASS), we have searched for neutral hydrogen in galaxies in a region similar to25x25 deg(2) centred on NGC 1399, the nominal centre of the Fornax cluster. Within a velocity search range of 300-3700 km s(-1) and to a 3sigma lower flux limit of similar to40 mJy, 110 galaxies with H I emission were detected, one of which is previously uncatalogued. None of the detections has early-type morphology. Previously unknown velocities for 14 galaxies have been determined, with a further four velocity measurements being significantly dissimilar to published values. Identification of an optical counterpart is relatively unambiguous for more than similar to90 per cent of our H I galaxies. The galaxies appear to be embedded in a sheet at the cluster velocity which extends for more than 30degrees across the search area. At the nominal cluster distance of similar to20 Mpc, this corresponds to an elongated structure more than 10 Mpc in extent. A velocity gradient across the structure is detected, with radial velocities increasing by similar to500 km s(-1) from south-east to north-west. The clustering of galaxies evident in optical surveys is only weakly suggested in the spatial distribution of our H I detections. Of 62 H I detections within a 10degrees projected radius of the cluster centre, only two are within the core region (projected radius

Números curiosos: o azarento 13 (parte II)

Na sua obra "Unpopular Essays", de 1950, o conhecido matemático e filósofo Bertrand Russel refere que o ser humano é um animal crédulo que precisa acreditar em algo e que, na ausência de uma boa crença, ele fica satisfeito com a má. Na cultura ocidental, o 13 é um dos números com mais impacto no universo das superstições e das crenças populares. Há mesmo quem leve muito a sério a suposta influência negativa deste número e que, por isso mesmo, o evite a todo o custo. (...) Algumas companhias aéreas, como a Air France e a Lufthansa, ainda omitem a fila 13 nos seus aviões. Em algumas partes do mundo, é raro conseguir encontrar um Hotel que não tenha renumerado o seu décimo terceiro andar (substituindo o 13 pelo 14 ou por 12A). É o caso, por exemplo, de Nova Iorque. O curioso é que ainda antes dos prédios terem 13 andares, já se saltava do 12 para o 14 na numeração dos quartos. Mas há quem vá mais longe, recusando-se a pernoitar, por exemplo, num quarto 454, por entender que esse número está a camuflar o 13 (note-se que 4+5+4=13). Stephen King, conhecido autor de contos de horror fantástico e de ficção, revelou que, quando está a ler um livro, nunca pára nas páginas 94, 193, 283 e em todas as outras em que a soma dos algarismos seja 13. Os jogadores de críquete da Austrália costumam chamar ao 87 "o número do diabo", já que 87=100-13. Há também quem evite morar numa casa com o número 13 ou que não queira dar um nome ao seu filho com exatamente 13 letras. Outro aspeto referido com frequência tem a ver com o facto do décimo terceiro Arcano Maior do Tarot ser a carta da morte (...) Alguns acontecimentos históricos ajudaram a alimentar a fobia ao 13. Lançada no dia 11 de abril de 1970, às 13h13, a Apollo 13 consistiu na terceira missão tripulada do Projeto Apollo com destino à Lua (note-se que, se adicionarmos os algarismos de 11/04/70, obtém-se 13). Devido a um acidente causado por uma explosão num dos módulos, não foi possível concluir a missão. Mesmo assim, os tripulantes conseguiram regressar com a nave à Terra, após seis dias no espaço. (...)

Relatório de estágio em gabinete de engenharia na componente de climatização

Trabalho Final de Mestrado para obtenção do grau de Mestre em Engenharia Mecânica com especialização em Energia, Climatização e Refrigeração

Análise do recurso a novas tecnologias no ensino de autistas

A massificação das tecnologias, abrangendo cada vez mais instituições e população em geral, originou uma aproximação da informação e do conhecimento às pessoas, permitindo um novo olhar para esta área, para as novas tecnologias e para o seu uso. Tendo como ponto de partida, a sociedade de informação e o recurso às tecnologias, recursos esses tão patentes actualmente, é possível pensar em criar as condições necessárias para que seja viável evoluir sempre mais, através da imaginação e de ideias criativas. Com base na aproximação das tecnologias que são cada vez mais acessíveis, o presente estudo pretende avaliar se as novas tecnologias, nas suas mais variadas formas, podem ser uma mais valia no ensino de autistas. O autismo começa a ser encarado como um campo a desenvolver estudos e a explorar os conceitos tecnológicos. O estudo aqui apresentado, não pretende ser apenas mais um, mas antes mostrar o trabalho efectuado até à data e o que pode ser realizado, expondo propostas. No sentido de conhecer um pouco melhor os conceitos relacionados com a área do autismo, foi necessário recorrer a pesquisas na Internet, à leitura de livros e a reuniões com pessoas ligadas a essa área, tornando possível uma aquisição de saberes e uma nova visão sobre a temática. Explorados os conceitos iniciais do autismo tornou-se imprescindível a procura dos recursos educativos utilizados nesta área, não só recursos empregados no método tradicional de ensino, como também, os modelos que procuram usar as novas tecnologias. A análise dos recursos existentes permitiu conhecer o panorama actual dos métodos e modelos em uso que conjugado com o levantamento de necessidades efectuado no decorrer deste trabalho, contribuíram para compreender as carências existentes e assim com base nesse conhecimento adquirido efectuar uma proposta de modelo educativo baseado em tecnologias para apoio educativo de autistas.

The histopathology of cutaneous leishmaniasis due to Leishmania (Leishmania) mexicana in the Yucatan peninsula, Mexico

Localized Cutaneous Leishmaniasis (LCL) known as "chiclero's ulcer" in southeast Mexico, was described by SEIDELIN in 1912. Since then the sylvatic region of the Yucatan peninsula has been documented as an endemic focus of LCL. This study of 73 biopsies from parasitological confirmed lesions of LCL cases of Leishmania (Leishmania) mexicana infection was undertaken: 1) to examine host response at tissue level; and 2) to relate manifestations of this response to some characteristics of clinical presentation. Based on Magalhães' classification we found that the most common pattern in our LCL cases caused by L. (L.) mexicana was predominantly characterized by the presence of unorganized granuloma without necrosis, (43.8%). Another important finding to be highlighted is the fact that in 50/73 (68.5%) parasite identification was positive. There was direct relation between the size of the lesion and time of evolution (r s = 0.3079, p = 0.03), and inverse correlation between size of the lesion and abundance of amastigotes (r s = -0.2467, p = 0.03). In view of the complexity of clinical and histopathological findings, cell-mediated immune response of the disease related to clinical and histopathological features, as so genetic background should be studied.

Dieta, tecnología y cronología en la arqueología del Valle de Ambato, Catamarca

El Valle Ambato fue el escenario donde surgió una nueva modalidad de organización socioeconómica e ideológica que se conoce como Cultura Aguada, resultando de la conjunción de una serie de elementos que ya existían y otros aparecen por primera vez. Esta dinámica es la reunión de profundas transformaciones en distintas esferas de la vida social, que desembocará en una nueva organización de la misma: los vínculos de las personas rebasarán los tradicionales del parentesco inmediato, a la vez que se institucionalizarán relaciones basadas en la división social del trabajo y en el acceso desigual a la riqueza y el poder. El elemento aglutinante de la integración es un sólido núcleo ideológico. El indicador más impactante es la presencia de unidades arquitectónicas monumentales, tales como el adobes pintes, sitio que nos ocupa en este proyecto. En la temporada de trabajo de 1996 excavamos el mencionado sitio y es necesario continuar con dicha excavación. El plan de trabajo se organiza en función de la etapa post-excavación, es decir básicamente consistirá en trabajar los materiales exhumados en la temporada anterior, reformular las preguntas iniciales, profundizar determinados aspectos y volver a excavar. Los aspectos a tratar en este momento son: 1) estudios de dieta en base a los restos de subsistencia, a análisis de carbono 13 y observación de los restos bioantropológicos; 2) análisis tecnológico de herramientas de reducción y obtención de recursos, fundamentalmente instrumental lítico, metalurgia, pigmentos, materiales de construcción, canteras y alfarería; 3) resolución de la ocupación del sitio Piedras Blancas, por medio de microestratigrafía y cronología absoluta (carbono 14); 4) excavación de determinados sectores de las Piedras Blancas: basurero, patio central y/o montículo.

Search for very high energy Gamma radiation from the Starburst Galaxy IC 342

This thesis describes a search for very high energy (VHE) gamma-ray emission from the starburst galaxy IC 342. The analysis was based on data from the 2003 — 2004 observing season recorded using the Whipple 10-metre imaging atmospheric Cherenkov telescope located on Mount Hopkins in southern Arizona. IC 342 may be classed as a non-blazar type galaxy and to date only a few such galaxies (M 87, Cen A, M 82 and NGC 253) have been detected as VHE gamma-ray sources. Analysis of approximately 24 hours of good quality IC 342 data, consisting entirely of ON/OFF observations, was carried out using a number of methods (standard Supercuts, optimised Supercuts, scaled optimised Supercuts and the multivariate kernel analysis technique). No evidence for TeV gamma-ray emission from IC 342 was found. The significance was 0.6 a with a nominal rate of 0.04 ± 0.06 gamma rays per minute. The flux upper limit above 600 GeV (at 99.9 % confidence) was determined to be 5.5 x 10-8 m-2 s-1, corresponding to 8 % of the Crab Nebula flux in the same energy range.