Magnetic Fields in the Milky Way

This chapter presents a review of observational studies to determine the magnetic field in the Milky Way, both in the disk and in the halo, focused on recent developments and on magnetic fields in the diffuse interstellar medium. I discuss some terminology which is confusingly or inconsistently used and try to summarize current status of our knowledge on magnetic field configurations and strengths in the Milky Way. Although many open questions still exist, more and more conclusions can be drawn on the large-scale and small-scale components of the Galactic magnetic field. The chapter is concluded with a brief outlook to observational projects in the near future.Comment: 22 pages, 5 figures, to appear in "Magnetic Fields in Diffuse Media", eds. E.M. de Gouveia Dal Pino and A. Lazaria

Cassiopeia A, Cygnus A, Taurus A, and Virgo A at ultra-low radio frequencies

Context. The four persistent radio sources in the northern sky with the highest flux density at metre wavelengths are Cassiopeia A, Cygnus A, Taurus A, and Virgo A; collectively they are called the A-team. Their flux densities at ultra-low frequencies (< 100 MHz) can reach several thousands of janskys, and they often contaminate observations of the low-frequency sky by interfering with image processing. Furthermore, these sources are foreground objects for all-sky observations hampering the study of faint signals, such as the cosmological 21 cm line from the epoch of reionisation. Aims. We aim to produce robust models for the surface brightness emission as a function of frequency for the A-team sources at ultra-low frequencies. These models are needed for the calibration and imaging of wide-area surveys of the sky with low-frequency interferometers. This requires obtaining images at an angular resolution better than 15\u2033 with a high dynamic range and good image fidelity. Methods. We observed the A-team with the Low Frequency Array (LOFAR) at frequencies between 30 MHz and 77 MHz using the Low Band Antenna system. We reduced the datasets and obtained an image for each A-team source. Results. The paper presents the best models to date for the sources Cassiopeia A, Cygnus A, Taurus A, and Virgo A between 30 MHz and 77 MHz. We were able to obtain the aimed resolution and dynamic range in all cases. Owing to its compactness and complexity, observations with the long baselines of the International LOFAR Telescope will be required to improve the source model for Cygnus A further

Hepatitis C virus infection and mixed cryoglobulinemia: a striking association

The high frequency of liver involvement in cryoglobulinemia is well established. Although both etiology and pathogenesis have remained so far undefined, recent studies suggest an association of mixed cryoglobulinemia with hepatitis C virus infection. To explore this hypothesis further, we assessed the prevalence of hepatitis C virus antibodies and RNA in a large group of patients, including: (1) 35 patients with cryoglobulinemia without clinical evidence of liver involvement (group 1), (2) 15 patients with symptomatic cryoglobulinemia associated with chronic liver disease (group 2) and (3) 12 patients with asymptomatic cryoglobulinemia associated with chronic liver disease (group 3). Anti-hepatitis C virus antibodies were detected by a second-generation enzyme-linked immunosorbent assay and third-generation immunoblot (SIA Prototype RIBA), whereas the polymerase chain reaction was used for the detection of viral RNA. Anti-hepatitis C virus antibodies, as detected by enzyme-linked immunosorbent assay, were demonstrated in 21 (60%) patients from group 1, 11 (73.3%) from group 2 and 10 (83.3%) from group 3. The immunoblot identified as positive 3 further patients in group 1 (giving a prevalence of 68.6%) and all patients in groups 2 and 3. Hepatitis C virus RNA was demonstrated in cryoprecipitates from 21 of 24 immunoblot-positives and from 6 of 11 immunoblot-negatives, indicating an actual active viral replication in 77.1% of group 1. This was also found in 13 (86.7%) and 10 (83.3%) cryoprecipitates of groups 2 and 3, respectively. Type II cryoglobulinemia was the prevalent form in group 1 (88.6%) and group 2 (73.3%), whereas type III was found in group 3 (58.3%) and in 26.7% of group 2.(ABSTRACT TRUNCATED AT 250 WORDS

Axillary lymph node nanometastases are prognostic factors for disease-free survival and metastatic relapse in breast cancer patients

Purpose: Early breast cancer presents with a remarkable heterogeneity of outcomes. Undetected, microscopic lymph node tumor deposits may account for a significant fraction of this prognostic diversity. Thus, we systematically evaluated the presence of lymph node tumor cell deposits <= 0.2 mm in diameter [pN(o(i+)), nanometastases] and analyzed their prognostic effect. Experimental Design: Single-institution, consecutive patients with 8 years of median follow-up (n= 702) were studied. To maximize chances of detecting micrometastases and nanometastases, whole-axilla dissections were analyzed. pN(0) cases (n= 377) were systematically reevaluated by lymph node (n= 6676) step-sectioning and anticytokeratin immunohistochemical analysis. The risk of first adverse events and of distant relapse of bona fide pN(0) patients was compared with that of pN(0(i+)), pN(1mi), and pN(1) cases. Results: Minimal lymph node deposits were revealed in 13% of pN(0) patients. The hazard ratio for all adverse events of pN(o(i+)) versus pN(o(i-)) was 2.51 (P= 0.00019). Hazards of pN(1mi) and pN(o(i+)) cases were not significantly different. A multivariate Cox model showed a hazard ratio of 2.16 for grouped pN(o(i+))/pN(1mi) versus pN(o(i-)) (P= 0.0005). Crude cumulative incidence curves for metastatic relapse were also significantly different (Gray's test chi(2)= 5.54, P= 0.019). Conclusion: Nanometastases are a strong risk factor for disease-free survival and for metastatic relapse. These findings support the inclusion of procedures for nanometastasis detection in tumor-node-metastasis staging

Plasma Diagnostics of the Interstellar Medium with Radio Astronomy

Contains fulltext : 119335.pdf (preprint version ) (Open Access

LOFAR Bootes and 3C295 field sources

The Bootes and 3C 295 fields were simultaneously observed on 2012 April 12 as part of a multi-beam observation with the LOFAR LBA stations. The idea behind the multi-beam setup is that we use the 3C 295 observations as a calibrator field to transfer the gain amplitudes to the (target) Bootes field. The total integration time on both fields was 10.25 hr. Complete frequency coverage was obtained between 54 and 70 MHz for both fields, while non-contiguous frequency coverage was obtained between 30 and 54 MHz for the 3C 295 only. All four correlation products were recorded. By default, the frequency band was divided into sub-bands, each 195.3125 kHz wide. Each sub-band was further divided in 64 channels and the integration time was 1 s