Evaluation of ribavirin efficacy and tolerance in subjects with chronic hepatitis C virus infection

Stanimirovic, Violeta; Nikolić, Dejan; B, Stanimirović; Nikolić, Aleksandra; Cucak, Spomenka

doi:10.2298/vsp0205479s

Cited by 12 publications

(12 citation statements)

References 7 publications

(6 reference statements)

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“…Here we combine two single-dish datasets: one with much better resolution (Herschel) than the other (Planck). Therefore, we can make a loose analogy to previous interferometric techniques (e.g., Thompson et al 1986;Stanimirovic 2002) aimed at combining data sets that are observed at significantly different angular resolutions. Here Herschel would represent the interferometer data while Planck would represent the lower resolution single-dish data.…”

Section: Methods and Implementationmentioning

confidence: 99%

Fourier-space combination ofPlanckandHerschelimages

Abreu-Vicente

Stutz

Henning

et al. 2017

A&A

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Context. Herschel has revolutionized our ability to measure column densities (N H ) and temperatures (T ) of molecular clouds thanks to its far infrared multiwavelength coverage. However, the lack of a well defined background intensity level in the Herschel data limits the accuracy of the N H and T maps. Aims. We aim to provide a method that corrects the missing Herschel background intensity levels using the Planck model for foreground Galactic thermal dust emission. For the Herschel/PACS data, both the constant-offset as well as the spatial dependence of the missing background must be addressed. For the Herschel/SPIRE data, the constant-offset correction has already been applied to the archival data so we are primarily concerned with the spatial dependence, which is most important at 250 µm. Methods. We present a Fourier method that combines the publicly available Planck model on large angular scales with the Herschel images on smaller angular scales. Results. We have applied our method to two regions spanning a range of Galactic environments: Perseus and the Galactic plane region around l = 11 deg (HiGal-11). We post-processed the combined dust continuum emission images to generate column density and temperature maps. We compared these to previously adopted constant-offset corrections. We find significant differences ( 20%) over significant (∼15%) areas of the maps, at low column densities (N H 10 22 cm −2 ) and relatively high temperatures (T 20 K). We have also applied our method to synthetic observations of a simulated molecular cloud to validate our method. Conclusions. Our method successfully corrects the Herschel images, including both the constant-offset intensity level and the scaledependent background variations measured by Planck. Our method improves the previous constant-offset corrections, which did not account for variations in the background emission levels.

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Section: Methods and Implementationmentioning

confidence: 99%

Fourier-space combination ofPlanckandHerschelimages

Abreu-Vicente

Stutz

Henning

et al. 2017

A&A

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“…The total interferometric flux of SMM1 at 1.3 mm is only 6.3% of the flux estimated from single-dish obervations whereas the interferometric flux for SMM2 is 12.5% expected from a single-dish measurement. This is probably due to the fact that structures larger than ≈1/4 of the primary beam size are filtered out by the interferometer (Stanimirovic 2002). With the larger 3 mm beam about 40 to 60% of the expected fluxes are recovered.…”

Section: High-resolution Mappingmentioning

confidence: 99%

A massive protostellar core with an infalling envelope

Birkmann

Krause

Hennemann

et al. 2007

A&A

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Context. Due to the short timescales involved and observational difficulties, our knowledge of the earliest phases of massive star formation remains incomplete. Aims. We aim to explore the physical conditions during the initial phases of high-mass star formation and to detect a genuine massive (mass M > 8 M ) protostar at an early evolutionary stage. Methods. We have launched a multi-wavelength study of young and massive star-forming regions that were identified by the ISOPHOT Serendipity Survey (ISOSS) performed with the ISO space telescope. The follow-up observations include ground-based near-infrared imaging and (sub)mm continuum and molecular line measurements (both single-dish and interferometric), as well as mid-to far-infrared measurements with the Spitzer Space Telescope. The combined spectrophotometric data are used to determine source temperatures T and masses M. Results. ISOSS J23053+5953 is a massive (M ∼ 900 M , luminosity L ∼ 2100 L ) and cold (T ∼ 17 K) star-forming region with two protostellar/protocluster candidates (T < ∼ 20 K and T ∼ 17.5 K, M ∼ 200 M each). The low temperatures are strongly confined by the spectrophotometric Spitzer data in the FIR. Interferometric observations reveal that the colder core (SMM2) has a mass of M = 26 M within a region of 8700 × 5600 AU and drives an outflow. It also shows signs of infall in both single-dish and interferometric measurements, and its luminosity can be explained by accretion. We also detect a large-scale jet that is traced by H 2 emission. Conclusions. The cold mm-core ISOSS J23053+5953 SMM2 is a promising candidate for a high-mass protostar in an early evolutionary stage and one of the few objects showing both infall signatures and jets as a sign of accretion.

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“…Then, these large-scale data can be added to the interferometer data (Uyaniker et al 1998;Stanimirovic 2002). However, for the WSRT 350 MHz observations this is not possible.…”

Section: Wsrt Observations From 312-381 Mhzmentioning

confidence: 99%

Linear polarization structures in LOFAR observations of the interstellar medium in the 3C 196 field

Jelić

Bruyn

Pandey

et al. 2015

A&A

157

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Aims. This study aims to characterize linear polarization structures in LOFAR observations of the interstellar medium (ISM) in the 3C 196 field, one of the primary fields of the LOFAR-Epoch of Reionization key science project. Methods. We have used the high band antennas (HBA) of LOFAR to image this region and rotation measure (RM) synthesis to unravel the distribution of polarized structures in Faraday depth. Results. The brightness temperature of the detected Galactic emission is 5−15 K in polarized intensity and covers the range from -3 to +8 rad m −2 in Faraday depth. The most interesting morphological feature is a strikingly straight filament at a Faraday depth of +0.5 rad m −2 running from north to south, right through the centre of the field and parallel to the Galactic plane. There is also an interesting system of linear depolarization canals conspicuous in an image showing the peaks of Faraday spectra. We used the Westerbork Synthesis Radio Telescope (WSRT) at 350 MHz to image the same region. For the first time, we see some common morphology in the RM cubes made at 150 and 350 MHz. There is no indication of diffuse emission in total intensity in the interferometric data, in line with results at higher frequencies and previous LOFAR observations. Based on our results, we determined physical parameters of the ISM and proposed a simple model that may explain the observed distribution of the intervening magneto-ionic medium. Conclusions. The mean line-of-sight magnetic field component, B , is determined to be 0.3 ± 0.1 µG and its spatial variation across the 3C 196 field is 0.1 µG. The filamentary structure is probably an ionized filament in the ISM, located somewhere within the Local Bubble. This filamentary structure shows an excess in thermal electron density (n e B > 6.2 cm −3 µG) compared to its surroundings.

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Evaluation of ribavirin efficacy and tolerance in subjects with chronic hepatitis C virus infection

Abstract: In this study ribavirin was more effective than placebo in reducing ALT levels during the treatment period of the applied therapy in patients with chronic active hepatitis C.

Cited by 12 publications

References 7 publications

Fourier-space combination ofPlanckandHerschelimages

Fourier-space combination ofPlanckandHerschelimages

A massive protostellar core with an infalling envelope

Linear polarization structures in LOFAR observations of the interstellar medium in the 3C 196 field

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