A Cerenkov-ΔΕ-Cerenkov detector for high energy cosmic ray isotopes and an accelerator study of ^(40)Ar & ^(56)Fe fragmentation

This thesis has two major parts. The first part of the thesis will describe a high energy cosmic ray detector -- the High Energy Isotope Spectrometer Telescope (HEIST). HEIST is a large area (0.25 m²sr) balloon-borne isotope spectrometer designed to make high-resolution measurements of isotopes in the element range from neon to nickel (10 ≤ Z ≤ 28) at energies of about 2 GeV/nucleon. The instrument consists of a stack of 12 NaI(Tl) scintilla tors, two Cerenkov counters, and two plastic scintillators. Each of the 2-cm thick NaI disks is viewed by six 1.5-inch photomultipliers whose combined outputs measure the energy deposition in that layer. In addition, the six outputs from each disk are compared to determine the position at which incident nuclei traverse each layer to an accuracy of ~2 mm. The Cerenkov counters, which measure particle velocity, are each viewed by twelve 5-inch photomultipliers using light integration boxes.

HEIST-2 determines the mass of individual nuclei by measuring both the change in the Lorentz factor (Δγ) that results from traversing the NaI stack, and the energy loss (ΔΕ) in the stack. Since the total energy of an isotope is given by Ε = γM, the mass M can be determined by M = ΔΕ/Δγ. The instrument is designed to achieve a typical mass resolution of 0.2 amu.

The second part of this thesis presents an experimental measurement of the isotopic composition of the fragments from the breakup of high energy ⁴⁰Ar and ⁵⁶Fe nuclei. Cosmic ray composition studies rely heavily on semi-empirical estimates of the cross-sections for the nuclear fragmentation reactions which alter the composition during propagation through the interstellar medium. Experimentally measured yields of isotopes from the fragmentation of ⁴⁰Ar and ⁵⁶Fe are compared with calculated yields based on semi-empirical cross-section formulae. There are two sets of measurements. The first set of measurements, made at the Lawrence Berkeley Laboratory Bevalac using a beam of 287 MeV/nucleon ⁴⁰Ar incident on a CH₂ target, achieves excellent mass resolution (σ_m ≤ 0.2 amu) for isotopes of Mg through K using a Si(Li) detector telescope. The second set of measurements, also made at the Lawrence Berkeley Laboratory Bevalac, using a beam of 583 MeV/nucleon ⁵⁶FeFe incident on a CH₂ target, resolved Cr, Mn, and Fe fragments with a typical mass resolution of ~ 0.25 amu, through the use of the Heavy Isotope Spectrometer Telescope (HIST) which was later carried into space on ISEE-3 in 1978. The general agreement between calculation and experiment is good, but some significant differences are reported here.

A quantitative investigation of the solar modulation of cosmic-ray protons and helium nuclei

The differential energy spectra of cosmic-ray protons and He nuclei have been measured at energies up to 315 MeV/nucleon using balloon- and satellite-borne instruments. These spectra are presented for solar quiet times for the years 1966 through 1970. The data analysis is verified by extensive accelerator calibrations of the detector systems and by calculations and measurements of the production of secondary protons in the atmosphere.

The spectra of protons and He nuclei in this energy range are dominated by the solar modulation of the local interstellar spectra. The transport equation governing this process includes as parameters the solar-wind velocity, V, and a diffusion coefficient, K(r,R), which is assumed to be a scalar function of heliocentric radius, r, and magnetic rigidity, R. The interstellar spectra, j_D, enter as boundary conditions on the solutions to the transport equation. Solutions to the transport equation have been calculated for a broad range of assumed values for K(r,R) and j_D and have been compared with the measured spectra.

It is found that the solutions may be characterized in terms of a dimensionless parameter, ψ(r,R) = ^∞∫_r V dr'/(K(r',R). The amount of modulation is roughly proportional to ψ. At high energies or far from the Sun, where the modulation is weak, the solution is determined primarily by the value of ψ (and the interstellar spectrum) and is not sensitive to the radial dependence of the diffusion coefficient. At low energies and for small r, where the effects of adiabatic deceleration are found to be large, the spectra are largely determined by the radial dependence of the diffusion coefficient and are not very sensitive to the magnitude of ψ or to the interstellar spectra. This lack of sensitivity to j_D implies that the shape of the spectra at Earth cannot be used to determine the interstellar intensities at low energies.

Values of ψ determined from electron data were used to calculate the spectra of protons and He nuclei near Earth. Interstellar spectra of the form j_D α (W - 0.25m)^-2.65 for both protons and He nuclei were found to yield the best fits to the measured spectra for these values of ψ, where W is the total energy and m is the rest energy. A simple model for the diffusion coefficient was used in which the radial and rigidity dependence are separable and K is independent of radius inside a modulation region which has a boundary at a distance D. Good agreement was found between the measured and calculated spectra for the years 1965 through 1968, using typical boundary distances of 2.7 and 6.1 A.U. The proton spectra observed in 1969 and 1970 were flatter than in previous years. This flattening could be explained in part by an increase in D, but also seemed to require that a noticeable fraction of the observed protons at energies as high at 50 to 100 MeV be attributed to quiet-time solar emission. The turnup in the spectra at low energies observed in all years was also attributed to solar emission. The diffusion coefficient used to fit the 1965 spectra is in reasonable agreement with that determined from the power spectra of the interplanetary magnetic field (Jokipii and Coleman, 1968). We find a factor of roughly 3 increase in ψ from 1965 to 1970, corresponding to the roughly order of magnitude decrease in the proton intensity at 250 MeV. The change in ψ might be attributed to a decrease in the diffusion coefficient, or, if the diffusion coefficient is essentially unchanged over that period (Mathews et al., 1971), might be attributed to an increase in the boundary distance, D.

Volatiles in Protoplanetary Disks

Planets are assembled from the gas, dust, and ice in the accretion disks that encircle young stars. Ices of chemical compounds with low condensation temperatures (<200 K), the so-called volatiles, dominate the solid mass reservoir from which planetesimals are formed and are thus available to build the protoplanetary cores of gas/ice giant planets. It has long been thought that the regions near the condensation fronts of volatiles are preferential birth sites of planets. Moreover, the main volatiles in disks are also the main C-and O-containing species in (exo)planetary atmospheres. Understanding the distribution of volatiles in disks and their role in planet-formation processes is therefore of great interest.

This thesis addresses two fundamental questions concerning the nature of volatiles in planet-forming disks: (1) how are volatiles distributed throughout a disk, and (2) how can we use volatiles to probe planet-forming processes in disks? We tackle the first question in two complementary ways. We have developed a novel super-resolution method to constrain the radial distribution of volatiles throughout a disk by combining multi-wavelength spectra. Thanks to the ordered velocity and temperature profiles in disks, we find that detailed constraints can be derived even with spatially and spectrally unresolved data -- provided a wide range of energy levels are sampled. We also employ high-spatial resolution interferometric images at (sub)mm frequencies using the Atacama Large Millimeter Array (ALMA) to directly measure the radial distribution of volatiles.

For the second question, we combine volatile gas emission measurements with those of the dust continuum emission or extinction to understand dust growth mechanisms in disks and disk instabilities at planet-forming distances from the central star. Our observations and models support the idea that the water vapor can be concentrated in regions near its condensation front at certain evolutionary stages in the lifetime of protoplanetary disks, and that fast pebble growth is likely to occur near the condensation fronts of various volatile species.

Measurement of the Polarization of the Cosmic Microwave Background with the BICEP2 and Keck Array Telescopes

Precision polarimetry of the cosmic microwave background (CMB) has become a mainstay of observational cosmology. The ΛCDM model predicts a polarization of the CMB at the level of a few μK, with a characteristic E-mode pattern. On small angular scales, a B-mode pattern arises from the gravitational lensing of E-mode power by the large scale structure of the universe. Inflationary gravitational waves (IGW) may be a source of B-mode power on large angular scales, and their relative contribution to primordial fluctuations is parameterized by a tensor-to-scalar ratio r. BICEP2 and Keck Array are a pair of CMB polarimeters at the South Pole designed and built for optimal sensitivity to the primordial B-mode peak around multipole l ~ 100. The BICEP2/Keck Array program intends to achieve a sensitivity to r ≥ 0.02. Auxiliary science goals include the study of gravitational lensing of E-mode into B-mode signal at medium angular scales and a high precision survey of Galactic polarization. These goals require low noise and tight control of systematics. We describe the design and calibration of the instrument. We also describe the analysis of the first three years of science data. BICEP2 observes a significant B-mode signal at 150 GHz in excess of the level predicted by the lensed-ΛCDM model, and Keck Array confirms the excess signal at > 5σ. We combine the maps from the two experiments to produce 150 GHz Q and U maps which have a depth of 57 nK deg (3.4 μK arcmin) over an effective area of 400 deg² for an equivalent survey weight of 248000 μK². We also show preliminary Keck Array 95 GHz maps. A joint analysis with the Planck collaboration reveals that much of BICEP2/Keck Array's observed 150 GHz signal at low l is more likely a Galactic dust foreground than a measurement of r. Marginalizing over dust and r, lensing B-modes are detected at 7.0σ significance.

Sacode a poeira e dá a volta por cima: resiliência em mulheres que vivenciaram violência sexual

O objeto deste estudo foi o processo de construção da resiliência em mulheres que vivenciaram violência sexual. A violência sexual contra a mulher é um problema antigo no mundo, onde o Brasil dispõe de elevadas estatísticas. As justificativas para a violência contra a mulher constroem-se sob normas e preceitos sociais de gênero, os quais definem as diferenças nos papéis e responsabilidades dos homens e das mulheres na sociedade e na família. As consequências físicas e psicológicas para a mulher em situação de violência sexual são alarmantes, podendo ocasionar traumas por longo prazo ou até mesmo para a vida inteira, impedindo-a de retomar seus direitos humanos e de se reinserirem em suas famílias e na sociedade. Entretanto, após a vivência de uma violência algumas mulheres têm seus comportamentos transformados a fim de retomarem o curso de suas vidas. Tais comportamentos dizem respeito à postura resiliente diante à violência sexual vivida e à sua superação. Reconhecendo este comportamento como uma nova possibilidade de promoção da saúde dessas mulheres, traçou-se como objetivo geral do estudo compreender o processo de construção da resiliência em mulheres que vivenciaram violência sexual. Desenvolveu-se uma pesquisa exploratória com abordagem qualitativa, realizada através da coleta da história de vida com seis mulheres que vivenciaram violência sexual atendidas em um hospital municipal do Rio de Janeiro (Brasil), referência no atendimento dessas mulheres. Os dados produzidos foram interpretados à luz da modalidade temática da análise de conteúdo de Bardin. Deste processo emergiram duas categorias: A violência sexual vivida expressa nas atitudes do cotidiano: sentimentos e emoções e A resiliência de mulheres em situação de violência sexual. Na primeira categoria identificaram-se as atitudes, sentimentos e emoções decorrentes da adversidade. Destacaram-se os sentimentos de medo, tristeza, culpa e perda como sendo as principais mudanças ocorridas com a violência. Na segunda categoria emergiram elementos existentes na vida das mulheres que vivenciaram violência sexual e que favoreceram no processo de construção da resiliência, sendo os aspectos individuais, familiares e sociais. A pesquisa considerou que a resiliência é elemento fundamental na promoção da saúde das mulheres que vivenciaram violência sexual assim como uma oportunidade de melhoria de sua qualidade de vida, uma vez que reduz os agravos decorrentes dessa violência e incorpora sentido de vida, serenidade, autoconfiança, autossuficiência e perseverança na vida da mulher. Contudo, a resiliência para ser desenvolvida precisa além dos aspectos individuais da mulher, uma rede de apoio familiar e social significativa e eficaz. A consulta de Enfermagem estabelecida nos princípios da humanização, integralidade e dialogicidade entre profissional e a mulher, seja nas Estratégias de Saúde da Família ou nos ambientes ambulatoriais e hospitalares, caracteriza-se como campo fértil na promoção e apoio a essa rede familiar e social. A enfermeira torna-se facilitadora na construção da resiliência em mulheres em situação de violência sexual, onde é preciso oferecer escuta sensível e sem preconceitos, incentivar a construção de sentido de vida, a recuperação da autoestima e autoconfiança e de sua reinserção social.

Toward Understanding Astrophysical Phenomena

Fast radio bursts (FRBs), a novel type of radio pulse, whose physics is not yet understood at all. Only a handful of FRBs had been detected when we started this project. Taking account of the scant observations, we put physical constraints on FRBs. We excluded proposals of a galactic origin for their extraordinarily high dispersion measures (DM), in particular stellar coronas and HII regions. Therefore our work supports an extragalactic origin for FRBs. We show that the resolved scattering tail of FRB 110220 is unlikely to be due to propagation through the intergalactic plasma. Instead the scattering is probably caused by the interstellar medium in the FRB's host galaxy, and indicates that this burst sits in the central region of that galaxy. Pulse durations of order $\ms$ constrain source sizes of FRBs implying enormous brightness temperatures and thus coherent emission. Electric fields near FRBs at cosmological distances would be so strong that they could accelerate free electrons from rest to relativistic energies in a single wave period. When we worked on FRBs, it was unclear whether they were genuine astronomical signals as distinct from `perytons', clearly terrestrial radio bursts, sharing some common properties with FRBs. Recently, in April 2015, astronomers discovered that perytons were emitted by microwave ovens. Radio chirps similar to FRBs were emitted when their doors opened while they were still heating. Evidence for the astronomical nature of FRBs has strengthened since our paper was published. Some bursts have been found to show linear and circular polarizations and Faraday rotation of the linear polarization has also been detected. I hope to resume working on FRBs in the near future. But after we completed our FRB paper, I decided to pause this project because of the lack of observational constraints.

The pulsar triple system, J0733+1715, has its orbital parameters fitted to high accuracy owing to the precise timing of the central $\ms$ pulsar. The two orbits are highly hierarchical, namely $P_{\mathrm{orb,1}}\ll P_{\mathrm{orb,2}}$, where 1 and 2 label the inner and outer white dwarf (WD) companions respectively. Moreover, their orbital planes almost coincide, providing a unique opportunity to study secular interaction associated purely with eccentricity beyond the solar system. Secular interaction only involves effect averaged over many orbits. Thus each companion can be represented by an elliptical wire with its mass distributed inversely proportional to its local orbital speed. Generally there exists a mutual torque, which vanishes only when their apsidal lines are parallel or anti-parallel. To maintain either mode, the eccentricity ratio, $e_1/e_2$, must be of the proper value, so that both apsidal lines precess together. For J0733+1715, $e_1\ll e_2$ for the parallel mode, while $e_1\gg e_2$ for the anti-parallel one. We show that the former precesses $\sim 10$ times slower than the latter. Currently the system is dominated by the parallel mode. Although only a little anti-parallel mode survives, both eccentricities especially $e_1$ oscillate on $\sim 10^3\yr$ timescale. Detectable changes would occur within $\sim 1\yr$. We demonstrate that the anti-parallel mode gets damped $\sim 10^4$ times faster than its parallel brother by any dissipative process diminishing $e_1$. If it is the tidal damping in the inner WD, we proceed to estimate its tidal quantity parameter ($Q$) to be $\sim 10^6$, which was poorly constrained by observations. However, tidal damping may also happen during the preceding low-mass X-ray binary (LMXB) phase or hydrogen thermal nuclear flashes. But, in both cases, the inner companion fills its Roche lobe and probably suffers mass/angular momentum loss, which might cause $e_1$ to grow rather than decay.

Several pairs of solar system satellites occupy mean motion resonances (MMRs). We divide these into two groups according to their proximity to exact resonance. Proximity is measured by the existence of a separatrix in phase space. MMRs between Io-Europa, Europa-Ganymede and Enceladus-Dione are too distant from exact resonance for a separatrix to appear. A separatrix is present only in the phase spaces of the Mimas-Tethys and Titan-Hyperion MMRs and their resonant arguments are the only ones to exhibit substantial librations. When a separatrix is present, tidal damping of eccentricity or inclination excites overstable librations that can lead to passage through resonance on the damping timescale. However, after investigation, we conclude that the librations in the Mimas-Tethys and Titan-Hyperion MMRs are fossils and do not result from overstability.

Rubble piles are common in the solar system. Monolithic elements touch their neighbors in small localized areas. Voids occupy a significant fraction of the volume. In a fluid-free environment, heat cannot conduct through voids; only radiation can transfer energy across them. We model the effective thermal conductivity of a rubble pile and show that it is proportional the square root of the pressure, $P$, for $P\leq \epsy^3\mu$ where $\epsy$ is the material's yield strain and $\mu$ its shear modulus. Our model provides an excellent fit to the depth dependence of the thermal conductivity in the top $140\,\mathrm{cm}$ of the lunar regolith. It also offers an explanation for the low thermal inertias of rocky asteroids and icy satellites. Lastly, we discuss how rubble piles slow down the cooling of small bodies such as asteroids.

Electromagnetic (EM) follow-up observations of gravitational wave (GW) events will help shed light on the nature of the sources, and more can be learned if the EM follow-ups can start as soon as the GW event becomes observable. In this paper, we propose a computationally efficient time-domain algorithm capable of detecting gravitational waves (GWs) from coalescing binaries of compact objects with nearly zero time delay. In case when the signal is strong enough, our algorithm also has the flexibility to trigger EM observation {\it before} the merger. The key to the efficiency of our algorithm arises from the use of chains of so-called Infinite Impulse Response (IIR) filters, which filter time-series data recursively. Computational cost is further reduced by a template interpolation technique that requires filtering to be done only for a much coarser template bank than otherwise required to sufficiently recover optimal signal-to-noise ratio. Towards future detectors with sensitivity extending to lower frequencies, our algorithm's computational cost is shown to increase rather insignificantly compared to the conventional time-domain correlation method. Moreover, at latencies of less than hundreds to thousands of seconds, this method is expected to be computationally more efficient than the straightforward frequency-domain method.

Modelagem e otimização de misturas ternárias de polipropileno (PP), borracha de etileno-propileno-dieno (EPDM) e pó de pneu (SRT).

O aumento nos rejeitos industriais e a contínua produção de resíduos causam muitas preocupações no âmbito ambiental. Neste contexto, o descarte de pneus usados tem se tornado um grande problema por conta da pequena atenção que se dá à sua destinação final. Assim sendo, essa pesquisa propõe a produção de uma mistura polimérica com polipropileno (PP), a borracha de etileno-propileno-dieno (EPDM) e o pó de pneu (SRT). A Metodologia de Superfície de Resposta (MSR), coleção de técnicas estatísticas e matemáticas úteis para desenvolver, melhorar e optimizar processos, foi aplicada à investigação das misturas ternárias. Após o processamento adequado em extrusora de dupla rosca e a moldagem por injeção, as propriedades mecânicas de resistência à tração e resistência ao impacto foram determinadas e utilizadas como variáveis resposta. Ao mesmo tempo, a microscopia eletrônica de varredura (MEV) foi usada para a investigação da morfologia das diferentes misturas e melhor interpretação dos resultados. Com as ferramentas estatísticas específicas e um número mínimo de experimentos foi possível o desenvolvimento de modelos de superfícies de resposta e a otimização das concentrações dos diferentes componentes da mistura em função do desempenho mecânico e além disso com a modificação da granulometria conseguimos um aumento ainda mais significativo deste desempenho mecânico.

Primary cosmic-ray positrons and negatrons in 1968 at energies between 11 and 204 MeV

The cosmic-ray positron and negatron spectra between 11 and 204 MeV have been measured in a series of 3 high-altitude balloon flights launched from Fort Churchill, Manitoba, on July 16, July 21, and July 29, 1968. The detector system consisted of a magnetic spectrometer utilizing a 1000-gauss permanent magnet, scintillation counters, and a lucite Čerenkov counter.

Launches were timed so that the ascent through the 100 g/cm² level of residual atmosphere occurred after the evening geomagnetic cutoff transition. Data gathered during ascent are used to correct for the contribution of atmospheric secondary electrons to the flux measured at float altitude. All flights floated near 2.4 g/cm².

A pronounced morning intensity increase was observed in each flight. We present daytime positron and negatron data which support the interpretation of the diurnal flux variation as a change in the local geomagnetic cutoff. A large diurnal variation was observed in the count rate of positrons and negatrons with magnetic rigidities less than 11 MV and is evidence that the nighttime cutoff was well below this value.

Using nighttime data we derive extraterrestrial positron and negatron spectra. The positron-to-total-electron ratio which we measure indicates that the interstellar secondary, or collision, source contributes ≾50 percent of the electron flux within this energy interval. By comparing our measured positron spectrum with the positron spectrum calculated for the collision source we derive the absolute solar modulation for positrons in 1968. Assuming negligible energy loss during modulation, we derive the total interstellar electron spectrum as well as the spectrum of directly accelerated, or primary, electrons. We examine the effect of adiabatic deceleration and find that many of the conclusions regarding the interstellar electron spectrum are not significantly altered for an assumed energy loss of up to 50 percent of the original energy.

A theory of strong and weak scintillations with applications to astrophysics

The propagation of waves in an extended, irregular medium is studied under the "quasi-optics" and the "Markov random process" approximations. Under these assumptions, a Fokker-Planck equation satisfied by the characteristic functional of the random wave field is derived. A complete set of the moment equations with different transverse coordinates and different wavenumbers is then obtained from the characteristic functional. The derivation does not require Gaussian statistics of the random medium and the result can be applied to the time-dependent problem. We then solve the moment equations for the phase correlation function, angular broadening, temporal pulse smearing, intensity correlation function, and the probability distribution of the random waves. The necessary and sufficient conditions for strong scintillation are also given.

We also consider the problem of diffraction of waves by a random, phase-changing screen. The intensity correlation function is solved in the whole Fresnel diffraction region and the temporal pulse broadening function is derived rigorously from the wave equation.

The method of smooth perturbations is applied to interplanetary scintillations. We formulate and calculate the effects of the solar-wind velocity fluctuations on the observed intensity power spectrum and on the ratio of the observed "pattern" velocity and the true velocity of the solar wind in the three-dimensional spherical model. The r.m.s. solar-wind velocity fluctuations are found to be ~200 km/sec in the region about 20 solar radii from the Sun.

We then interpret the observed interstellar scintillation data using the theories derived under the Markov approximation, which are also valid for the strong scintillation. We find that the Kolmogorov power-law spectrum with an outer scale of 10 to 100 pc fits the scintillation data and that the ambient averaged electron density in the interstellar medium is about 0.025 cm^-3. It is also found that there exists a region of strong electron density fluctuation with thickness ~10 pc and mean electron density ~7 cm^-3 between the PSR 0833-45 pulsar and the earth.

Deep near-infrared spectroscopy of high-redshift galaxies: the physical growth of passive systems

The assembly history of massive galaxies is one of the most important aspects of galaxy formation and evolution. Although we have a broad idea of what physical processes govern the early phases of galaxy evolution, there are still many open questions. In this thesis I demonstrate the crucial role that spectroscopy can play in a physical understanding of galaxy evolution. I present deep near-infrared spectroscopy for a sample of high-redshift galaxies, from which I derive important physical properties and their evolution with cosmic time. I take advantage of the recent arrival of efficient near-infrared detectors to target the rest-frame optical spectra of z > 1 galaxies, from which many physical quantities can be derived. After illustrating the applications of near-infrared deep spectroscopy with a study of star-forming galaxies, I focus on the evolution of massive quiescent systems.

Most of this thesis is based on two samples collected at the W. M. Keck Observatory that represent a significant step forward in the spectroscopic study of z > 1 quiescent galaxies. All previous spectroscopic samples at this redshift were either limited to a few objects, or much shallower in terms of depth. Our first sample is composed of 56 quiescent galaxies at 1 < z < 1.6 collected using the upgraded red arm of the Low Resolution Imaging Spectrometer (LRIS). The second consists of 24 deep spectra of 1.5 < z < 2.5 quiescent objects observed with the Multi-Object Spectrometer For Infra-Red Exploration (MOSFIRE). Together, these spectra span the critical epoch 1 < z < 2.5, where most of the red sequence is formed, and where the sizes of quiescent systems are observed to increase significantly.

We measure stellar velocity dispersions and dynamical masses for the largest number of z > 1 quiescent galaxies to date. By assuming that the velocity dispersion of a massive galaxy does not change throughout its lifetime, as suggested by theoretical studies, we match galaxies in the local universe with their high-redshift progenitors. This allows us to derive the physical growth in mass and size experienced by individual systems, which represents a substantial advance over photometric inferences based on the overall galaxy population. We find a significant physical growth among quiescent galaxies over 0 < z < 2.5 and, by comparing the slope of growth in the mass-size plane dlogR_e/dlogM_∗ with the results of numerical simulations, we can constrain the physical process responsible for the evolution. Our results show that the slope of growth becomes steeper at higher redshifts, yet is broadly consistent with minor mergers being the main process by which individual objects evolve in mass and size.

By fitting stellar population models to the observed spectroscopy and photometry we derive reliable ages and other stellar population properties. We show that the addition of the spectroscopic data helps break the degeneracy between age and dust extinction, and yields significantly more robust results compared to fitting models to the photometry alone. We detect a clear relation between size and age, where larger galaxies are younger. Therefore, over time the average size of the quiescent population will increase because of the contribution of large galaxies recently arrived to the red sequence. This effect, called progenitor bias, is different from the physical size growth discussed above, but represents another contribution to the observed difference between the typical sizes of low- and high-redshift quiescent galaxies. By reconstructing the evolution of the red sequence starting at z ∼ 1.25 and using our stellar population histories to infer the past behavior to z ∼ 2, we demonstrate that progenitor bias accounts for only half of the observed growth of the population. The remaining size evolution must be due to physical growth of individual systems, in agreement with our dynamical study.

Finally, we use the stellar population properties to explore the earliest periods which led to the formation of massive quiescent galaxies. We find tentative evidence for two channels of star formation quenching, which suggests the existence of two independent physical mechanisms. We also detect a mass downsizing, where more massive galaxies form at higher redshift, and then evolve passively. By analyzing in depth the star formation history of the brightest object at z > 2 in our sample, we are able to put constraints on the quenching timescale and on the properties of its progenitor.

A consistent picture emerges from our analyses: massive galaxies form at very early epochs, are quenched on short timescales, and then evolve passively. The evolution is passive in the sense that no new stars are formed, but significant mass and size growth is achieved by accreting smaller, gas-poor systems. At the same time the population of quiescent galaxies grows in number due to the quenching of larger star-forming galaxies. This picture is in agreement with other observational studies, such as measurements of the merger rate and analyses of galaxy evolution at fixed number density.

Avaliação da influência do material de confecção das matrizes no teste de conversão monomérica por espectrometria no infravermelho de um compósito

Este estudo teve por objetivo avaliar, in vitro, a influência do material de confecção das matrizes, traçando um perfil da conversão monomérica de um compósito micro-híbrido, além de avaliar qual dos materiais testados mais se assemelha a uma matriz de dentina. A avaliação foi feita através da análise do grau de conversão (GC). Foram confeccionadas 3 matrizes bipartidas, sendo estas de teflon negro, tefon branco e aço inoxidável, ambas com 10mm de diâmetro e 2 mm de profundidade. Para o grupo controle foi utilizado um incisivo central bovino, o qual teve sua face vestibular aplainada em uma lixadeira sob refrigeração constante, com o auxílio de uma lixa de carbeto de silício, número 800. Após, este dente foi preparado com uma broca diamantada número 2294 (KG Sorensen) em alta rotação, própria para a preparação de cavidades padronizadas para ensaios de laboratório, apresentando um limitador de penetração. Em seguida, com um motor de baixa rotação foi realizado o acabamento das paredes, obtendo-se uma cavidade de 2,0 mm de profundidade por 9,0 mm de diâmetro. Pela palatina desse dente, com uma broca carbide cilíndrica de numeração 2056 (KG Sorensen), fez-se uma penetração até se obter uma parede de dentina extremamente fina, porém sem que esta fosse rompida. Assim, com uma agulha, fez-se uma pequena perfuração no centro dessa dentina para que este instrumental servisse como um pino para remoção do corpo de prova de dentro da matriz de dente. Os corpos de prova (CP) foram obtidos a partir da inserção do compósito no interior da perfuração das matrizes em um único incremento e cobertos na superfície externa com uma matriz de poliéster mais uma lamínula de vidro. Os CP foram fotopolimerizados por 40 s pela fonte de luz halógena Optilux 501 (Demetron), com 500 mW/cm. Imediatamente após a polimerização, os corpos de prova eram submetidos no topo e na base para a análise de espectrometria no infravermelho para a determinação da profundidade de polimerização, pela técnica do filme vazado para o compósito não polimerizado e pela técnica da pastilha de brometo de potássio (KBr) para o compósito polimerizado. Foram confeccionados 5 CP de cada grupo. Em cada grupo, o compósito da base e do topo das amostras foi moído até se obter de 1,5 a 2,0 mg de pó e misturado com 70 mg de KBr, para obtenção da pastilha de KBr. Foi feita a análise de espectrofotometria no infravermelho por Transformada de Fourier (FTIR). As absorções selecionadas para o cálculo foram 1610 cm-1 e 1637 cm-1, os picos dos espectros das ligações dos carbonos aromáticos e alifáticos, respectivamente. Os dados obtidos foram tratados estatisticamente. Os grupos Gr1B, Gr2B, Gr3B e Gr4B representam, respectivamente, as bases dos CP confeccionados pelas matrizes de DB, TN, TB e AI. Já os Gr1T, Gr2T, Gr3T e Gr4T representam os topos. Médias (%) e DP: Gr1T (46,461,99), Gr2T (39,864,51), Gr3T (44,053,44) e Gr4T (38,045,08). Gr1B (40,441,49), Gr2B (36,153,81), Gr3B (40,093,18) e Gr4B (35,593,35). Em posse dos resultados, pôde-se concluir que os grupos do teflon negro, teflon branco e aço inoxidável não apresentaram diferenças entre o grau de conversão do topo e da base, enquanto que o grupo da dentina apresentou maior conversão do topo. Comparando as matrizes entre elas, pôde-se perceber que no topo, o GC do dente bovino é maior que o GC do aço inoxidável e do que o de teflon negro, o GC do teflon branco é maior que o GC do aço inoxidável e do que o de teflon negro. Já o topo dos grupos de dente bovino e teflon banco foram semelhantes. Nas bases dos CPs, não houve diferença significativa entre os grupos testados. De acordo com os resultados obtidos no experimento, pôde-se concluir que nos grupos do teflon negro, teflon branco e aço inoxidável não houve diferença entre 0 e 2 mm, ou seja, topo e base, o que mostra que o material de confecção da matriz não influênciou o grau de conversão do compósito. Já para o grupo da matriz de dentina, o topo apresentou valor de conversão monomérica maior, mostrando que, neste caso, o material da matriz interferiu no grau de conversão. Pode-se perceber também que existe uma tendência da matriz de teflon branco se assemelhar mais a matriz de dentina, pois foi o único grupo que apresentou semelhança nos valores de conversão monomérica no topo das amostras. Porém analisando a base das amostras, percebe-se que todos os grupos se comportaram de forma semelhante, obtendo valores do grau de conversão sem diferença significante.

O uso da Técnica de Oscilações Forçadas na análise da mecânica ventilatória de indivíduos portadores de silicose classificados em diferentes graus de obstrução

O termo silicose refere-se ao processo de fibrose pulmonar causado pela inalação de poeira contendo sílica. É uma doença ocupacional, incurável, que se inicia nas vias aéreas distais e pode progredir independente do término da exposição. Os testes de função pulmonar, apesar de não serem utilizados como ferramenta diagnóstica para silicose, são amplamente empregados para acompanhar longitudinalmente esses indivíduos. Estudos recentes sugerem que a Técnicas de Oscilações Forçadas (FOT) pode ser aplicada para detecção de alterações pulmonares precoces em indivíduos com silicose. Contudo, existem poucos estudos descrevendo as alterações de mecância respiratória associada com a silicose através da FOT. Neste contexto, os objetivos deste estudo são: (1) analisar as alterações de mecânica respiratória de indivíduos portadores de silicose com diferentes graus de obstrução e (2) avaliar a capacidade da FOT em detectar alterações na função pulmonar decorrentes da silicose. Trata-se de um estudo transversal controlado com avaliação de casos prevalentes, tendo como unidade de avaliação o indivíduo. Os exames realizados incluíram medidas de espirometria e FOT. Foi selecionado um total de 67 indivíduos, 46 portadores de silicose e 21 sadios, caracterizando o grupo controle. Os indivíduos com diagnóstico de silicose foram divididos em três grupos classificados de acordo com o nível de obstrução sugerido pela espirometria. Essa classificação resultou em três categorias: Indivíduos normais ao exame espirométrico (NE), n= 12; com distúrbio ventilatório obstrutivo leve (DVOL), n=22; com distúrbio ventilatório obstrutivo moderado ou acentuado (DVOMA), n= 12. Todos os indivíduos realizaram exames da FOT para análise das propriedades resistivas e reativas do sistema respiratório. Posteriormente aos exames da FOT os indivíduos foram submetidos à espirometria. Considerando os grupos divididos a partir da espirometria, os parâmetros resistivos e reativos e a impedância do sistema respiratório em 4Hz (Z4Hz) se modificaram significativamente com a progressão da distúrbio obstrutivo. Na análise do poder diagnóstico da FOT os parâmetros R0, Rm, Rsr4 e |Z4Hz| mostraram-se precisos para identificar as modificações de mecânica respiratória em pacientes com silicose apresentando distúrbio ventilatório obstrutivo leve. Para distúrbio ventilatório obstrutivo moderado e acentuado todos os parâmetros analisados apresentaram habilidade para identificar essas alterações. Na análise entre o grupo controle e normal ao exame, nenhum parâmetro da FOT apresentou valor de acurácia adequado para uso clínico. Esses resultados são coerentes com as alterações fisiopatológicas relacionadas à silicose, confirmando o potencial da FOT na avaliação das modificações de mecânica respiratória em doentes com silicose.

Características biogeoquímicas da interação atmosfera criosfera na Antártica ocidental

O manto polar antártico retêm informação paleoclimatologica por entres suas camadas de neve e gelo. O gelo antártico tem revelado a base de dados paleoclimática de maior resolução para os últimos 800 mil anos. Os padrões de transporte atmosférico refletem a composição e a fonte do particulado encontrado na neve e no gelo do continente Antártico. Estando relacionado a processos climáticos, as características desse transporte alteram em quantidade e qualidade as espécies químicas que se depositam sobre o manto de gelo. Dessa forma, o estudo dos depósitos de particulado ao longo das camadas de neve/gelo na Antártica pode sugerir mudanças nos padrões de transporte atmosférico. Atualmente a comunidade científica discute as diferenças de padrões climáticos entre o leste e o oeste antártico. Enquanto de forma geral observa-se instabilidade no setor oeste, o clima da antártica oriental demonstra relativa estabilidade climática. Neste estudo, analisamos dois testemunhos de gelo recente de duas regiões com características climáticas diferentes do continente Antártico. No Platô Detroit situado na Península Antártica (6410′S/0600′O), analisamos a variabilidade de Black Carbon (BC) ao longo de 20 metros de neve. O BC encontrado na Península Antártica apresentou baixas concentrações comparáveis as encontradas no gelo do Artico período pré-industrial. Nossos resultados sugerem que sua variabiliade corresponde à sazonalidade dos períodos de queimada nos continentes do Hemisfério Sul. No interior do continente Antártico, analisamos o particulado em geral por um processo de microanálise ao longo de um testemunho de 40 metros extraído em Mont Johns (79o55′S/09423′O). Encontramos uma tendência negativa na deposição de poeira mineral (AlSi) entre 1967 e 2007. Nossos resultados sugerem que esta tendência seja resultado de um crescente isolamento atmosférico da região central do continente antártico pelo aumento da intensidade dos ventos ao redor da Antártica. Este aumento na intensidade dos ventos reflete por sua vez o resfriamento da alta atmosfera no centro antártico causado pela depleção da camada de ozônio na região. Adicionalmente, amostras de diferentes microambientes de Patriot Hills (8018′S/08121′O) foram coletadas de maneira asséptica para análise microbiológica. As amostras foram cultivadas em meio R2 e paralelamente o DNA total extraído foi sequenciado pela técnica de pirosequenciamento. Os resultados preliminares desta analise mostram grande riqueza de espécies dos mais variados grupos. Os resultados deste trabalho caracterizam três diferentes parâmetros relacionados a deposição atmosférica em duas áreas pouco exploradas e de grande interesse científico do continente antártico.

基于光散射的粉尘浓度测量的研究

文章介绍了一种智能激光粉尘测试系统的软硬件结构设计，详细给出了系统光学传感器的原理结构及使用方法，传感器非线性信号处理以及系统的数字滤波方案。最后系统测量了苏州大学物理实验中心外距地面约2米的空气中的粉尘相对质量浓度，连续测量36天，并与国家环保总局苏州地区每天预报的空气污染指数转换后的可吸入颗粒物（PMIO）浓度值相比较，得出对应关系，运用MATLAB拟和直线对系统进行标定。

光学薄膜中界面层和表面吸附层对相位延迟的影响

多层介质反射镜在非正入射的时候，两个不同的偏振态之间会产生不同的相移．根据空气与膜层、膜层之间的实际情况，建立了界面层和表面吸附层模型，并运用它分析相位延迟产生误差的原因．通过优化设计，入射角为54°，在1285～1345nm之间p，s波获得了270±1°的相移，同时也使反射率在99．5％以上．用离子束溅射技术制备相位延迟膜，用分光光度计测试了光谱特性和用椭偏仪测试了相位特性，在相应波段获得了262．4±1．8°的相移，同时也使反射率在99．6％以上．误差的主要来源是离子源工作特性会产生不均匀的过渡层和最