Aligning the CMS muon chambers with the muon alignment system during an extended cosmic ray run

The alignment system for the muon spectrometer of the CMS detector comprises three independent subsystems of optical and analog position sensors. It aligns muon chambers with respect to each other and to the central silicon tracker. System commissioning at full magnetic field began in 2008 during an extended cosmic ray run. The system succeeded in tracking muon detector movements of up to 18 mm and rotations of several milliradians under magnetic forces. Depending on coordinate and subsystem, the system achieved chamber alignment precisions of 140-350 μm and 30-200 μrad, close to the precision requirements of the experiment. Systematic errors on absolute positions are estimated to be 340-590 μm based on comparisons with independent photogrammetry measurements. © 2010 IOP Publishing Ltd and SISSA.

Precise mapping of the magnetic field in the CMS barrel yoke using cosmic rays

The CMS detector is designed around a large 4 T superconducting solenoid, enclosed in a 12 000-tonne steel return yoke. A detailed map of the magnetic field is required for the accurate simulation and reconstruction of physics events in the CMS detector, not only in the inner tracking region inside the solenoid but also in the large and complex structure of the steel yoke, which is instrumented with muon chambers. Using a large sample of cosmic muon events collected by CMS in 2008, the field in the steel of the barrel yoke has been determined with a precision of 3 to 8% depending on the location. © 2010 IOP Publishing Ltd and SISSA.

Performance of CMS muon reconstruction in cosmic-ray events

The performance of muon reconstruction in CMS is evaluated using a large data sample of cosmic-ray muons recorded in 2008. Efficiencies of various high-level trigger, identification, and reconstruction algorithms have been measured for a broad range of muon momenta, and were found to be in good agreement with expectations from Monte Carlo simulation. The relative momentum resolution for muons crossing the barrel part of the detector is better than 1% at 10 GeV/c and is about 8% at 500 GeV/c, the latter being only a factor of two worse than expected with ideal alignment conditions. Muon charge misassignment ranges from less than 0.01% at 10GeV/c to about 1% at 500 GeV/c. © 2010 IOP Publishing Ltd and SISSA.

Efeito do FGF10 na maturação oocitária e produção de embriões bovinos in vitro

Coordenação de Aperfeiçoamento de Pessoal de Nível Superior (CAPES)

Estudo das talassemias do tipo alfa em dois estados das regiões nordeste e sudeste do Brasil

Pós-graduação em Genética - IBILCE

Identificação de espermatozóides portadores do cromossomo X em búfalos (Bubalus bubalis)

Pós-graduação em Medicina Veterinária - FMVZ

Agonista versus antagonista do GnRH em ciclos de reprodução assistida: morfologia oocitária

Coordenação de Aperfeiçoamento de Pessoal de Nível Superior (CAPES)

Ativação partenogenética de oócitos maturados in vitro de Cebus apella

O objetivo deste trabalho foi avaliar a maturação oocitária in vitro (MIV) na espécie C. apella, relacionando com a expansão das células do cumulus e promovendo a produção in vitro de embriões (PIVE), por meio da ativação partenogenética e fecundação in vitro (FIV). Os oócitos puncionados dos folículos antrais medindo 2-9 mm de diâmetro foram classificados em desnudos (OD), com poucas células do cumulus (PCC) e complexo cumulus-oophorus intacto (CCO intacto). A expansão das células do cumulus foi analisada nos tempos de 0, 36 e 40 h de MIV e classificada em cinco categorias de expansão. A competência meiótica nos oócitos foi verificada pela extrusão do 1º corpúsculo polar (CP) após 40 h de MIV. Os oócitos foram divididos em 3 grupos para PIVE: grupo controle (FIV), ativação partenogenética utilizando 5 μM de ionomicina em associação com 2 mM de 6-DMAP ou em associação com 50 μM de roscovitina. Para a FIV, os espermatozóides obtidos do coágulo seminal, foram diluídos em água de coco em pó (ACP-118®) e submetidos ao resfriamento para serem levados posteriormente ao cultivo in vitro com os oócitos. O aumento no tempo da MIV e a presença de várias células do cumulus associadas aos oócitos proporcionaram maior expansão das células do cumulus, pois somente os CCO intactos alcançaram a expansão total em 40 h de MIV (p < 0,005). A presença das células do cumulus nos oócitos (PCC e CCO intactos) maturados in vitro por 40 h promoveu a competência meiótica (metáfase II) significamente mais elevada que os OD (p < 0,005). Após 6 h de resfriamento em ACP-118® e separação pelo método do swin-up, os espermatozóides utilizados na FIV possuíam 80% de motilidade e vigor 4. O tratamento com ionomicina/roscovitina promoveu a extrusão do 2º CP e formação pronuclear e com ionomicina/6-DMAP formou pronúcleos, sem extrusão do 2º CP. O protocolo utilizando a ionomicina/6-DMAP e da FIV originou as primeiras divisões embrionárias, observada pela taxa de clivagem. Os resultados encontrados sugerem que em C. apella a presença e a expansão total das células do cumulus estão relacionadas com a competência oocitária. A utilização dos oócitos maturados in vitro e dos espermatozóides diluídos e resfriados em ACP-118® promoveu a PIVE por diferentes métodos nesta espécie.

Efeito da dapsona na geração de estresse oxidativo em pacientes com hanseníase em uso de poliquimioterapia

O processo inflamatório decorrente da infecção por Mycobacterium leprae e a administração de fármacos com propriedades oxidativas, como a dapsona, são fatores de riscos ao estresse oxidativo ocasionado em pacientes com hanseníase. Este trabalho visa determinar as concentrações plasmáticas de dapsona em pacientes com hanseníase em uso de poliquimioterapia (PQT), correlacionando ao desenvolvimento do estresse oxidativo. Para o estudo, foram selecionados indivíduos saudáveis e pacientes com hanseníase, acompanhados antes (D0) e após a terceira dose supervisionada de PQT (D3). As concentrações plasmáticas de dapsona dos pacientes sob tratamento foram mesuradas por cromatografia liquida de alta eficiência. A avaliação do estresse oxidativo foi realizada através da determinação de metemoglobina (MetHb) e das concentrações de glutationa reduzida (GSH), óxido nítrico (NO), malondialdeído (MDA), capacidade antioxidante total (TEAC) e avaliação das atividades das enzimas catalase (CAT), superóxido dismutase (SOD) e da presença de corpúsculo de Heinz em esfregaços sanguíneos. No período de estudo foram obtidas 23 amostras de pacientes com hanseníase D0, 13 pacientes em D3 e 20 de indivíduos saudáveis e sem a doença. As alterações no pacientes antes do tratamento estavam associadas ao aumento de NO (D0=18.91± 2.39; controle= 6.86±1.79mM) e a redução significativa na enzima SOD (D0=69.88±12.26;controle= 138.42±14.99nmol/mL). Com relação aos pacientes sob tratamento, a concentração de dapsona no plasma foi 0.552± 0.037 μg/mL e as principais alterações observadas foram o aumento significativo no percentual de MetHb (D3= 3.29±0.74;controle=0.66±0.051%) e presença de corpúsculo de Heinz. Nos pacientes em tratamento também se observou aumento nos níveis de GSH (7.01±1.09μg/mL) quando comparados ao controle (3.33±1.09g/mL) e diminuição da atividade de CAT (D3= 10.29± 2.02; controle= 19.52±2.48 U/g de proteínas). Os níveis de MDA antes e durante o PQT não mostraram alteração, enquanto os níveis de TEAC aumentaram significativamente neste pacientes (D0=2.90 ± 0.42; D3=3.04±0.52; controle= 1.42±0.18μmol/mL). Estes dados sugerem que a PQT é a principal responsável pelo desenvolvimento de estresse oxidativo, através da geração de danos oxidativos identificados pela presença de corpúsculo de Heinz e aumento no percentual de MetHb.

Expressão de fatores relacionados à morte celular programada em embriões bovinos infectados com BHV-5

Pós-graduação em Microbiologia - IBILCE

Aspectos reprodutivos, morfologia dos gametas e desenvolvimento embrionário de Astyanax altiparanae Garutti & Britski (Teleostei, Characidae)

Pós-graduação em Aquicultura - FCAV

Search for gravitational wave ringdowns from perturbed intermediate mass black holes in LIGO-Virgo data from 2005-2010

We report results from a search for gravitational waves produced by perturbed intermediate mass black holes ( IMBH) in data collected by LIGO and Virgo between 2005 and 2010. The search was sensitive to astrophysical sources that produced damped sinusoid gravitational wave signals, also known as ringdowns, with frequency 50 <= f(0)/Hz <= 2000 and decay timescale 0.0001 less than or similar to tau/s less than or similar to 0.1 characteristic of those produced in mergers of IMBH pairs. No significant gravitational wave candidate was detected. We report upper limits on the astrophysical coalescence rates of IMBHs with total binary mass 50 <= M/ M circle dot <= 450 and component mass ratios of either 1: 1 or 4: 1. For systems with total mass 100 <= M/M circle dot <= 150, we report a 90% confidence upper limit on the rate of binary IMBH mergers with nonspinning and equal mass components of 6.9 x 10(-8) Mpc(-3) yr(-1). We also report a rate upper limit for ringdown waveforms from perturbed IMBHs, radiating 1% of their mass as gravitational waves in the fundamental, l = m = 2, oscillation mode, that is nearly three orders of magnitude more stringent than previous results.

Methods and results of a search for gravitational waves associated with gamma-ray bursts using the GEO 600, LIGO, and Virgo detectors

In this paper we report on a search for short-duration gravitational wave bursts in the frequency range 64 Hz-1792 Hz associated with gamma-ray bursts (GRBs), using data from GEO 600 and one of the LIGO or Virgo detectors. We introduce the method of a linear search grid to analyze GRB events with large sky localization uncertainties, for example the localizations provided by the Fermi Gamma-ray Burst Monitor (GBM). Coherent searches for gravitational waves (GWs) can be computationally intensive when the GRB sky position is not well localized, due to the corrections required for the difference in arrival time between detectors. Using a linear search grid we are able to reduce the computational cost of the analysis by a factor of O(10) for GBM events. Furthermore, we demonstrate that our analysis pipeline can improve upon the sky localization of GRBs detected by the GBM, if a high-frequency GW signal is observed in coincidence. We use the method of the linear grid in a search for GWs associated with 129 GRBs observed satellite-based gamma-ray experiments between 2006 and 2011. The GRBs in our sample had not been previously analyzed for GW counterparts. A fraction of our GRB events are analyzed using data from GEO 600 while the detector was using squeezed-light states to improve its sensitivity; this is the first search for GWs using data from a squeezed-light interferometric observatory. We find no evidence for GW signals, either with any individual GRB in this sample or with the population as a whole. For each GRB we place lower bounds on the distance to the progenitor, under an assumption of a fixed GW emission energy of 10(-2)M circle dot c(2), with a median exclusion distance of 0.8 Mpc for emission at 500 Hz and 0.3 Mpc at 1 kHz. The reduced computational cost associated with a linear search grid will enable rapid searches for GWs associated with Fermi GBM events once the advanced LIGO and Virgo detectors begin operation.

Search for Gravitational Waves Associated with gamma-ray Bursts Detected by the Interplanetary Network

We present the results of a search for gravitational waves associated with 223 gamma-ray bursts (GRBs) detected by the InterPlanetary Network (IPN) in 2005-2010 during LIGO's fifth and sixth science runs and Virgo's first, second, and third science runs. The IPN satellites provide accurate times of the bursts and sky localizations that vary significantly from degree scale to hundreds of square degrees. We search for both a well-modeled binary coalescence signal, the favored progenitor model for short GRBs, and for generic, unmodeled gravitational wave bursts. Both searches use the event time and sky localization to improve the gravitational wave search sensitivity as compared to corresponding all-time, all-sky searches. We find no evidence of a gravitational wave signal associated with any of the IPN GRBs in the sample, nor do we find evidence for a population of weak gravitational wave signals associated with the GRBs. For all IPN-detected GRBs, for which a sufficient duration of quality gravitational wave data are available, we place lower bounds on the distance to the source in accordance with an optimistic assumption of gravitational wave emission energy of 10(-2)M(circle dot)c(2) at 150 Hz, and find a median of 13 Mpc. For the 27 short-hard GRBs we place 90% confidence exclusion distances to two source models: a binary neutron star coalescence, with a median distance of 12 Mpc, or the coalescence of a neutron star and black hole, with a median distance of 22 Mpc. Finally, we combine this search with previously published results to provide a population statement for GRB searches in first-generation LIGO and Virgo gravitational wave detectors and a resulting examination of prospects for the advanced gravitational wave detectors.

The NINJA-2 project: detecting and characterizing gravitational waveforms modelled using numerical binary black hole simulations

The Numerical INJection Analysis (NINJA) project is a collaborative effort between members of the numerical relativity and gravitational-wave (GW) astrophysics communities. The purpose of NINJA is to study the ability to detect GWs emitted from merging binary black holes (BBH) and recover their parameters with next-generation GW observatories. We report here on the results of the second NINJA project, NINJA-2, which employs 60 complete BBH hybrid waveforms consisting of a numerical portion modelling the late inspiral, merger, and ringdown stitched to a post-Newtonian portion modelling the early inspiral. In a 'blind injection challenge' similar to that conducted in recent Laser Interferometer Gravitational Wave Observatory (LIGO) and Virgo science runs, we added seven hybrid waveforms to two months of data recoloured to predictions of Advanced LIGO (aLIGO) and Advanced Virgo (AdV) sensitivity curves during their first observing runs. The resulting data was analysed by GW detection algorithms and 6 of the waveforms were recovered with false alarm rates smaller than 1 in a thousand years. Parameter-estimation algorithms were run on each of these waveforms to explore the ability to constrain the masses, component angular momenta and sky position of these waveforms. We find that the strong degeneracy between the mass ratio and the BHs' angular momenta will make it difficult to precisely estimate these parameters with aLIGO and AdV. We also perform a large-scale Monte Carlo study to assess the ability to recover each of the 60 hybrid waveforms with early aLIGO and AdV sensitivity curves. Our results predict that early aLIGO and AdV will have a volume-weighted average sensitive distance of 300 Mpc (1 Gpc) for 10M circle dot + 10M circle dot (50M circle dot + 50M circle dot) BBH coalescences. We demonstrate that neglecting the component angular momenta in the waveform models used in matched-filtering will result in a reduction in sensitivity for systems with large component angular momenta. This reduction is estimated to be up to similar to 15% for 50M circle dot + 50M circle dot BBH coalescences with almost maximal angular momenta aligned with the orbit when using early aLIGO and AdV sensitivity curves.