Discovery of a High-Energy Gamma-Ray-Emitting Persistent Microquasar

Microquasars are stellar x-ray binaries that behave as a scaled down version of extragalactic quasars. The star LS 5039 is a new microquasar system with apparent persistent ejection of relativistic plasma at a 3 kiloparsec distance from the sun. It may also be associated with a gamma-ray source discovered by the Energetic Gamma Ray Experiment Telescope (EGRET) on board the COMPTON-Gamma Ray Observatory satellite. Before the discovery of LS 5039, merely a handful of microquasars had been identified in the Galaxy, and none of them was detected in high-energy gamma-rays.

Studying the non-thermal lobes of IRAS 16547-4247 through a multi-wavelength approach

In recent years, massive protostars have turned out to be a possible population of high-energy emitters. Among the best candidates is IRAS 16547-4247, a protostar that presents a powerful outflow with clear signatures of interaction with its environment. This source has been revealed to be a potential high-energy source because it displays non-thermal radio emission of synchrotron origin, which is evidence of relativistic particles. To improve our understanding of IRAS 16547-4247 as a high-energy source, we analyzed XMM-Newton archival data and found that IRAS 16547-4247 is a hard X-ray source. We discuss these results in the context of a refined one-zone model and previous radio observations. From our study we find that it may be difficult to explain the X-ray emission as non-thermal radiation coming from the interaction region, but it might be produced by thermal Bremsstrahlung (plus photo-electric absorption) by a fast shock at the jet end. In the high-energy range, the source might be detectable by the present generation of Cherenkov telescopes, and may eventually be detected by Fermi in the GeV range.

Deep GMRT radio observations and a multi-wavelength study of the region around HESS J1858+020

Context. There are a number of very high energy sources in the Galaxy that remain unidentified. Multi-wavelength and variability studies, and catalogue searches, are powerful tools to identify the physical counterpart, given the uncertainty in the source location and extension. Aims. This work carries out a thorough multi-wavelength study of the unidentified, very high energy source HESS J1858+020 and its environs. Methods. We have performed Giant Metrewave Radio Telescope observations at 610 MHz and 1.4 GHz to obtain a deep, low-frequency radio image of the region surrounding HESS J1858+020. We analysed archival radio, infrared, and X-ray data as well. This observational information, combined with molecular data, catalogue sources, and a nearby Fermi gamma-ray detection of unidentified origin, are combined to explore possible counterparts to the very high energy source. Results. We provide with a deep radio image of a supernova remnant that might be related to the GeV and TeV emission in the region. We confirm the presence of an H ii region next to the supernova remnant and coincident with molecular emission. A potential region of star formation is also identified. We identify several radio and X-ray sources in the surroundings. Some of these sources are known planetary nebulae, whereas others may be non-thermal extended emitters and embedded young stellar objects. Three old, background Galactic pulsars also neighbour HESS J1858+020 along the line of sight. Conclusions. The region surrounding HESS J1858+020 is rich in molecular structures and non-thermal objects that may potentially be linked to this unidentified very high energy source. In particular, a supernova remnant interacting with nearby molecular clouds may be a good candidate, but a star forming region, or a non-thermal radio source of yet unclear nature, may also be behind the gamma-ray source. The neighbouring pulsars, despite being old and distant, cannot be discarded as candidates. Further observational studies are needed, however, to narrow the search for a counterpart to the HESS source.

CARCINOMA BRONQUÍOLO-ALVEOLAR: ASPECTOS NA TOMOGRAFIA COMPUTADORIZADA DE ALTA RESOLUÇÃO

O carcinoma bronquíolo-alveolar é um tipo de carcinoma broncogênico de crescimento insidioso, que surge nas paredes das vias aéreas distais e se dissemina utilizando o septo alveolar como um estroma, preservando a arquitetura pulmonar. Neste trabalho foram analisadas as tomografias computadorizadas de alta resolução de 17 pacientes com carcinoma bronquíolo-alveolar. Ao contrário do relatado na literatura, foram observados predomínio no sexo masculino (71%) e maior freqüência da associação das formas de consolidação e multinodular (53%) em relação à forma nodular solitária (12%), multinodular (12%) e de consolidação (23%). Os aspectos mais encontrados foram: áreas de consolidação (76%), broncograma aéreo (71%), áreas de baixa atenuação provavelmente devidas à presença de muco (60%), espessamento de septos interlobulares, opacidades em vidro fosco e nódulos confluentes (54% cada), e pavimentação em mosaico (36%). Os nódulos cavitados, a atelectasia, o sinal do halo e o aspecto de "árvore em brotamento" foram observados em apenas um caso cada.

Paracoccidioidomicose pulmonar: aspectos na tomografia computadorizada de alta resolução

O comprometimento pulmonar na paracoccidioidomicose é muito freqüente, podendo até ser a única manifestação da doença. Neste trabalho são analisados os aspectos encontrados nas tomografias computadorizadas de alta resolução do tórax de 30 pacientes com paracoccidioidomicose confirmada. Por meio desta análise foram determinados os achados mais comuns e suas formas de apresentação e distribuição nos pulmões. Os aspectos mais freqüentemente observados foram: espessamento esparso de septos interlobulares (96,7%), opacidades em vidro fosco (66,7%), nódulos (60%), aumento irregular do espaço aéreo (enfisema paracicatricial) (56,7%), espessamento de paredes brônquicas (46,7%), espessamento pleural (36,7%), cavidades (36,7%), dilatação da traquéia (33,3%), distorção arquitetural (30%), consolidação do espaço aéreo (30%), bandas parenquimatosas (23,3%), reticulado intralobular (13,3%) e espessamento irregular do interstício axial peri-hilar (10%). A radiografia do tórax apresenta limitada capacidade de avaliar doenças pulmonares difusas, tornando a tomografia computadorizada de alta resolução do tórax essencial para avaliação dos pacientes com paracoccidioidomicose pulmonar.

Carcinoma do esôfago com invasão do canal medular: relato de caso e revisão da literatura

Os autores apresentam o caso de paciente do sexo masculino, 62 anos de idade, com emagrecimento há quatro meses e diminuição da força muscular associada a parestesias em membros inferiores há dois dias. Foi submetido a mielotomografia, que demonstrou massa no mediastino posterior com destruição dos corpos vertebrais e invasão do canal medular, além de espessamento irregular das paredes do esôfago. Na evolução, foi submetido a estudo contrastado do esôfago, que demonstrou falha de enchimento irregular. A biópsia confirmou a presença de carcinoma de células escamosas. Este é o primeiro relato na literatura latino-americana (Lilacs) de carcinoma de esôfago com invasão de canal medular e manifestação inicial de síndrome de compressão medular.

Gamma-ray emission from massive young stellar objects

Context.Massive stars form in dense and massive molecular cores. The exact formation mechanism is unclear, but it is possible that some massive stars are formed by processes similar to those that produce the low-mass stars, with accretion/ejection phenomena occurring at some point of the evolution of the protostar. This picture seems to be supported by the detection of a collimated stellar wind emanating from the massive protostar IRAS 16547-4247. A triple radio source is associated with the protostar: a compact core and two radio lobes. The emission of the southern lobe is clearly non-thermal. Such emission is interpreted as synchrotron radiation produced by relativistic electrons locally accelerated at the termination point of a thermal jet. Since the ambient medium is determined by the properties of the molecular cloud in which the whole system is embedded, we can expect high densities of particles and infrared photons. Because of the confirmed presence of relativistic electrons, inverse Compton and relativistic Bremsstrahlung interactions are unavoidable. Aims.We aim to make quantitative predictions of the spectral energy distribution of the non-thermal spots generated by massive young stellar objects, with emphasis on the particular case of IRAS 16547-4247. Methods.We study the high-energy emission generated by the relativistic electrons which produce the non-thermal radio source in IRAS 16547-4247. We also study the result of proton acceleration at the terminal shock of the thermal jet and make estimates of the secondary gamma rays and electron-positron pairs produced by pion decay. Results.We present spectral energy distributions for the southern lobe of IRAS 16547-4247, for a variety of conditions. We show that high-energy emission might be detectable from this object in the gamma-ray domain. The source may also be detectable in X-rays through long exposures with current X-ray instruments. Conclusions.Gamma-ray telescopes such as GLAST, and even ground-based Cherenkov arrays of new generation can be used to study non-thermal processes occurring during the formation of massive stars.

A microquasar model applied to unidentified gamma-ray sources

Among unidentified gamma-ray sources in the galactic plane, there are some that present significant variability and have been proposed to be high-mass microquasars. To deepen the study of the possible association between variable low galactic latitude gamma-ray sources and microquasars, we have applied a leptonic jet model based on the microquasar scenario that reproduces the gamma-ray spectrum of three unidentified gamma-ray sources, 3EG J1735-1500, 3EG J1828+0142 and GRO J1411-64, and is consistent with the observational constraints at lower energies. We conclude that if these sources were generated by microquasars, the particle acceleration processes could not be as efficient as in other objects of this type that present harder gamma-ray spectra. Moreover, the dominant mechanism of high-energy emission should be synchrotron self-Compton (SSC) scattering, and the radio jets may only be observed at low frequencies. For each particular case, further predictions of jet physical conditions and variability generation mechanisms have been made in the context of the model. Although there might be other candidates able to explain the emission coming from these sources, microquasars cannot be excluded as counterparts. Observations performed by the next generation of gamma-ray instruments, like GLAST, are required to test the proposed model.

Optical spectroscopy of microquasar candidates at low Galactic latitudes

We report optical spectroscopic observations of a sample of 6 low-galactic latitude microquasar candidates selected by cross-identification of X-ray and radio point source catalogs for |b|<5 degrees. Two objects resulted to be of clear extragalactic origin, as an obvious cosmologic redshift has been measured from their emission lines. For the rest, none exhibits a clear stellar-like spectrum as would be expected for genuine Galactic microquasars. Their featureless spectra are consistent with being extragalactic in origin although two of them could be also highly reddened stars. The apparent non-confirmation of our candidates suggests that the population of persistent microquasar systems in the Galaxy is more rare than previously believed. If none of them is galactic, the upper limit to the space density of new Cygnus X-3-like microquasars within 15 kpc would be 1.1\times10^{-12} per cubic pc. A similar upper limit for new LS 5039-like systems within 4 kpc is estimated to be 5.6\times10^{-11} per cubic pc.

LS 5039: A runaway microquasar ejected from the galactic plane

We have compiled optical and radio astrometric data of the microquasar LS 5039 and derived its proper motion. This, together with the distance and radial velocity of the system, allows us to state that this source is escaping from its own regional standard of rest, with a total systemic velocity of about 150 km/s and a component perpendicular to the galactic plane larger than 100 km/s. This is probably the result of an acceleration obtained during the supernova event that created the compact object in this binary system. We have computed the trajectory of LS 5039 in the past, and searched for OB associations and supernova remnants in its path. In particular, we have studied the possible association between LS 5039 and the supernova remnant G016.8-01.1, which, despite our efforts, remains dubious. We have also discovered and studied an HI cavity in the ISM, which could have been created by the stellar wind of LS 5039 or by the progenitor of the compact object in the system. Finally, in the symmetric supernova explosion scenario, we estimate that at least 17 solar masses were lost in order to produce the high eccentricity observed. Such a mass loss could also explain the observed runaway velocity of the microquasar.

O uso da ultra-sonografia no diagnóstico e evolução da apendicite aguda

OBJETIVO: Aproximadamente 35% das apendicites agudas têm diagnóstico clínico pré-operatório duvidoso ou incorreto, particularmente grávidas e crianças. A ultra-sonografia, em virtude do seu baixo custo e facilidade de acesso, tem-se mostrado um método diagnóstico importante. Este estudo propôs-se a demonstrar os principais achados de imagem das diversas fases da apendicite, com o objetivo de auxiliar o ultra-sonografista no diagnóstico precoce desta afecção. MATERIAIS E MÉTODOS: São relatados 14 casos de ultra-sonografias abdominais realizadas no período de janeiro a julho de 2001, em pacientes que se apresentavam com quadro de abdome agudo. O exame foi realizado com transdutores de 3,5 MHz e 7,5 MHz. RESULTADOS: O estudo ultra-sonográfico antes da perfuração demonstra apêndice não compressível, com espessamento e perda focal da definição das paredes. Após a perfuração, o apêndice pode não ser visualizado ao exame de ultra-sonografia, sendo evidenciadas alterações secundárias como efeito de massa, formação de plastrão, liquefação e formação de abscesso, além de ar dentro da coleção. CONCLUSÃO: O diagnóstico precoce da apendicite é essencial para minimizar a morbidade, que se mantém elevada se ocorrer perfuração. Apresentações atípicas resultam em confusão diagnóstica e retarde no tratamento. As principais dificuldades e erros são apendicite retrocecal, apendicite focal ou perfurada.

Amiloidose pulmonar: aspectos na tomografia computadorizada

Neste trabalho foram estudados os aspectos tomográficos observados em cinco pacientes com diagnóstico de amiloidose pulmonar confirmado histopatologicamente. Dois deles apresentaram a forma traqueobrônquica da doença e mostraram nodulações e formação de placas nas paredes traqueais, com calcificações. Dois tinham a forma parenquimatosa difusa, um deles com opacidades reticulares e nodulares subpleurais, e o outro com espessamento nodular de septos interlobulares e consolidações parenquimatosas. Ambos apresentavam calcificações de permeio às lesões. O último paciente tinha a forma nodular da doença, com nódulos de contornos regulares em ambos os pulmões, com calcificações. Os aspectos tomográficos observados, embora não patognomônicos, são muito sugestivos do diagnóstico de amiloidose.

Linfangioliomiomatose pulmonar: aspectos na tomografia computadorizada de alta resolução

Neste trabalho foram estudados, retrospectivamente, 17 pacientes com linfangioliomiomatose pulmonar diagnosticada por biópsia pulmonar a céu aberto. Todos os pacientes eram do sexo feminino, com idade média de 39,6 anos. Duas pacientes tiveram também o diagnóstico de esclerose tuberosa. As pacientes foram submetidas a tomografia computadorizada de alta resolução, cujos achados revelaram cistos com conteúdo gasoso, de formas variadas e com diferentes tamanhos, não ultrapassando 60 mm de diâmetro. A grande maioria tinha as paredes finas. Todos os cistos apresentaram distribuição difusa pelo parênquima pulmonar. Somente duas pacientes apresentaram pneumotórax associado. Nódulos parenquimatosos e espessamento de septos interlobulares não foram observados. Dessa forma, as características tomográficas utilizadas para o diagnóstico foram a ausência de nódulos e a presença de cistos de tamanhos variados, em geral menores que 20 mm, arredondados e distribuídos difusamente pelo parênquima pulmonar.

Bupivacaine 0.5 % versus articaine 4 % for the removal of lower third molars. A crossover randomized controlled trial

Objective: To compare the anesthetic action of 0.5% bupivacaine in relation to 4% articaine, both with 1:200,000 epinephrine, in the surgical removal of lower third molars. As a secondary objective hemodynamic changes using both anesthetics were analyzed. Study Design: Triple-blind crossover randomized clinical trial. Eighteen patients underwent bilateral removal of impacted lower third molars using 0.5% bupivacaine or 4% articaine in two different appointments. Preoperative, intraoperative and postoperative variables were recorded. Differences were assessed with McNemar tests and repeated measures ANOVA tests. Results: Both solutions exhibited similar latency times and intraoperative efficacy. Statistical significant lower pain levels were observed with bupivacaine between the fifth (p=0.011) and the ninth (p=0.007) postoperative hours. Bupivacaine provided significantly longer lasting soft tissue anesthesia (p<0.05). Systolic blood pressure and heart rate values were significantly higher with articaine. Conclusions: Bupivacaine could be a valid alternative to articaine especially due to its early postoperative pain prevention ability.

EVN+MERLIN observations of microquasar candidates at low galactic latitudes

In an attempt to increase the number of known microquasars, Paredes et al. (2002) have presented a long-term project focused on the search for new objects of this type. They performed a cross-identification between X-ray and radio catalogs under very restrictive selection criteria for sources with |b|<5 degrees, and obtained a sample of 13 radio-emitting X-ray sources. Follow-up observations of 6 of these sources with the VLA provided accurate coordinates, which were used to discover optical counterparts for all of them. We have observed these six sources with the EVN and MERLIN at 5 GHz. Five of the six objects have been detected and imaged, presenting different morphologies: one source has a two-sided jet, three sources have one-sided jets, and one source is compact. With all the presently available information, we conclude that two of the sources are promising microquasar candidates in our Galaxy.