Morfologia e estereologia do peritônio de paca conservado em solução supersaturada de açúcar a 300% ou glicerina a 98% implantados na parede abdominal de ratos

Pós-graduação em Cirurgia Veterinária - FCAV

Carta geotécnica de suscetibilidade aos processos da dinâmica superficial do trecho KM 215 ao 249 da Rodovia Marechal Rondon - SP-300

Conselho Nacional de Desenvolvimento Científico e Tecnológico (CNPq)

Influência de ciclos térmicos na microestrutura e propriedades mecânicas da junta soldada do aço COS CIVIL 300

Coordenação de Aperfeiçoamento de Pessoal de Nível Superior (CAPES)

Caracterização microbiológica, molecular e contagem de células somáticas por citometria de fluxo (Somacount 300®) e por contagem microscopia (Prescott e Breed, 1910) do leite caprino mastítico

Pós-graduação em Medicina Veterinária - FMVZ

Caracterização mecânica e microestrutural do aço MARAGING 300, soldado a plasma e submetidas a reparos

Pós-graduação em Engenharia Mecânica - FEG

O uso do peritônio de paca conservado em solução supersaturada de açúcar a 300% ou glicerina a 98% implantados na parede abdominal de ratos

Fundação de Amparo à Pesquisa do Estado de São Paulo (FAPESP)

Caracterização de juntas soldadas em PAW e GTAW de chapas finas em aço maraging 300 submetidas a vários reparos

Pós-graduação em Engenharia Mecânica - FEG

Jornal da UNESP, 2014, ano XXVIII, n. 300

Jornal elaborado pela Assessoria de Comunicação e Imprensa da Reitoria da UNESP

Linkage & Selective Mapping and QTL Analysis in a Harosoy x Clark population of 300 RILs

Four of the 12 major Glycine max ancestors of all modern elite U.S.A. soybean cultivars were the grandparents of Harosoy and Clark, so a Harosoy x Clark population would include some of that genetic diversity. A mating of eight Harosoy and eight Clark plants generated eight F1 plants. The eight F1:2 families were advanced via a plant-to-row selfing method to produce 300 F6-derived RILs that were genotyped with 266 SSR, 481 SNP, and 4 classical markers. SNPs were genotyped with the Illumina 1536-SNP assay. Three linkage maps, SSR, SNP, and SSR-SNP, were constructed with a genotyping error of < 1 %. Each map was compared with the published soybean consensus map. The best subset of 94 RILs for a high-resolution framework (joint) map was selected based on the expected bin length statistic computed with MapPop. The QTLs of seven traits measured in a 2-year replicated performance trial of the 300 RILs were identified using composite interval mapping (CIM) and multiple-interval mapping (MIM). QTL x Year effects in multiple trait analysis were compared with results of multiple-interval mapping. QTL x QTL effects were identified in MIM.

NGC 2782: a merger remnant with young stars in its gaseous tidal tail

We have searched for young star-forming regions around the merger remnant NGC 2782. By using Galaxy Evolution Explorer far-ultraviolet and near-ultraviolet imaging and H i data we found seven ultraviolet sources, located at distances greater than 26 kpc from the centre of NGC 2782, and coinciding with its western H i tidal tail. These regions were resolved in several smaller systems when Gemini/Gemini multi-object spectrograph (GMOS) r-band images were used. We compared the observed colours to stellar population synthesis models and found that these objects have ages of similar to 1 to 11 Myr and masses ranging from 103.9 to 104.6 M circle dot. By using Gemini/GMOS spectroscopic data we confirm memberships and derive high metallicities for three of the young regions in the tail (12+log(O/H) = 8.74 +/- 0.20, 8.81 +/- 0.20 and 8.78 +/- 0.20). These metallicities are similar to the value presented by the nuclear region of NGC 2782 and also similar to the value presented for an object located close to the main body of NGC 2782. The high metallicities measured for the star-forming regions in the gaseous tidal tail of NGC 2782 could be explained if they were formed out of highly enriched gas which was once expelled from the centre of the merging galaxies when the system collided. An additional possibility is that the tail has been a nursery of a few generations of young stellar systems which ultimately polluted this medium with metals, further enriching the already pre-enriched gas ejected to the tail when the galaxies collided.

The globular cluster kinematics and galaxy dark matter content of NGC 3923

This paper presents further results from our spectroscopic study of the globular cluster (GC) system of the group elliptical NGC 3923. From observations made with the GMOS instrument on the Gemini South Telescope, an additional 50 GC and ultra-compact dwarf (UCD) candidates have been spectroscopically confirmed as members of the NGC 3923 system. When the recessional velocities of these GCs are combined with the 29 GC velocities reported previously, a total sample of 79 GC/UCD velocities is produced. This sample extends to over 6 arcmin (>6 R-e similar to 30 kpc) from the centre of NGC 3923 and is used to study the dynamics of the GC system and the dark matter content of NGC 3923. It is found that the GC system of NGC 3923 displays no appreciable rotation, and that the projected velocity dispersion is constant with radius within the uncertainties. The velocity dispersion profiles of the integrated light and GC system of NGC 3923 are indistinguishable over the region in which they overlap. We find some evidence that the diffuse light and GCs of NGC 3923 have radially biased orbits within similar to 130 arcsec. The application of axisymmetric orbit-based models to the GC and integrated light velocity dispersion profiles demonstrates that a significant increase in the mass-to-light ratio (from M/L-V = 8 to 26) at large galactocentric radii is required to explain this observation. We therefore confirm the presence of a dark matter halo in NGC 3923. We find that dark matter comprises 17.5(-4.5)(+7.3) per cent of the mass within 1 R-e, 41.2(-10.6)(+18.2) per cent within 2 R-e and 75.6(-16.8)(+15.4) per cent within the radius of our last kinematic tracer at 6.9 R-e. The total dynamical mass within this radius is found to be 1.5(-0.25)(+0.4) x 10(12) M-circle dot. In common with other studies of large ellipticals, we find that our derived dynamical mass profile is consistently higher than that derived by X-ray observations, by a factor of around 2.

CNO and F abundances in the globular cluster M22 (NGC 6656)

Context. Recent studies have confirmed the long standing suspicion that M 22 shares a metallicity spread and complex chemical enrichment history similar to that observed in omega Cen. M 22 is among the most massive Galactic globular clusters and its color-magnitude diagram and chemical abundances reveal the existence of sub-populations. Aims. To further constrain the chemical diversity of M 22, necessary to interpret its nucleosynthetic history, we seek to measure relative abundance ratios of key elements (carbon, nitrogen, oxygen, and fluorine) best studied, or only available, using high-resolution spectra at infrared wavelengths. Methods. High-resolution (R = 50 000) and high S/N infrared spectra were acquired of nine red giant stars with Phoenix at the Gemini-South telescope. Chemical abundances were calculated through a standard 1D local thermodynamic equilibrium analysis using Kurucz model atmospheres. Results. We derive [Fe/H] = -1.87 to -1.44, confirming at infrared wavelengths that M 22 does present a [Fe/H] spread. We also find large C and N abundance spreads, which confirm previous results in the literature but based on a smaller sample. Our results show a spread in A(C+N+O) of similar to 0.7 dex. Similar to mono-metallic globular clusters, M 22 presents a strong [Na/Fe]-[O/Fe] anticorrelation as derived from Na and CO lines in the K band. For the first time we recover F abundances in M 22 and find that it exhibits a 0.6 dex variation. We find tentative evidence for a flatter A(F)-A(O) relation compared to higher metallicity globular clusters. Conclusions. Our study confirms and expands upon the chemical diversity seen in this complex stellar system. All elements studied to date show large abundance spreads which require contributions from both massive and low mass stars.

Sviluppo di un sistema tomografico con tubo a raggi x da 300 kv: progettazione e test preliminari.

In questo elaborato sono descritti la progettazione e lo sviluppo di un sistema tomografico con sorgente di raggi X da 300 kV per analisi nel campo dei Beni Culturali; in particolare sono stati effettuati test preliminari sia per verificare le prestazioni del tubo a raggi X e dello schermo scintillatore sia per avere indicazioni utili alla progettazione (e conseguente costruzione) del box di rivelazione. Il collaudo della sorgente di raggi X è stato eseguito con lo studio dell'andamento della dose integrale e/o del rateo di dose in funzione della tensione, della corrente e del tempo d'irraggiamento. La caratterizzazione dello schermo scintillatore di CsI(Tl) è basata sul confronto delle sue caratteristiche con uno schermo analogo di spessore differente nelle stesse condizioni sperimentali, attraverso lo studio dei parametri standard dei dispositivi per imaging, quali la curva di risposta, il rapporto segnale-rumore e la risoluzione spaziale. Inoltre, come ulteriore test, lo schermo scintillatore è stato utilizzato per l’indagine tomografica di alcuni pani di terra contenenti olle di epoca villanoviana. Per la progettazione del box rivelatore sono state invece svolte misure di tipo ottico. I vari test svolti in laboratorio hanno dato risultati positivi e hanno dimostrato la validità dei componenti scelti per il nuovo sistema tomografico, il cui assemblaggio verrà completato a breve, essendo stata ultimata proprio in queste settimane la costruzione del box di rivelazione.