dataesr/scientific-paragraphs-categorization huggingface dataset:
The Search Strategy Registries or databases reporting on AF management, identified from sources that included CINAHL, Medline, EMBASE, and the Cochrane Database of Systematic Reviews from 2000 to 2012, were selected for closer review, and publications from these registries were tracked. We identified 34 large international or national registries of AF patients, including 17 reporting on thromboprophylaxis and stroke prevention, 8 focused on antiarrhythmic drug (AAD) therapy and cardioversion, 7 studying AF ablation, and 2 detailing left atrial appendage closure (LAAC) registries.
The Adherence eValuation After Ischemic Stroke Longitudinal (AVAIL) registry, for example, expanded on the hospital-based Get with the Guidelines-Stroke quality improvement program and Carotid RX ACCULINK/RX ACCUNET Post-Approval Trial to Uncover Unanticipated or Rare Events (CAPTURE), a prototype registry from the Paul Coverdale National Acute Stroke Registry. 4, 5 ese evaluate whether patient management accords with practice guidelines and evidence-based research. The Nationwide Danish study,  11  Outcomes Registry for Better Informed Treatment of Atrial Fibrillation (ORBIT-AF)  12  and Prevention of thromboembolic events-European Registry in Atrial Fibrillation (PREFER-AF)  13  registries address this in European and U. S. patient cohorts. Data have been collected from each of these with the exception of CAPTURE, GARFIELD, and ORBIT-AF registries, which are ongoing.
42 Bleeding risks associated with OACs are a potential disadvantage of therapy, but data from registries help identify patients most likely to encounter bleeding complications. The concept of "net clinical benefit" aims to balance the risks of ischemic stroke and bleeding on OAC therapy  43  and was originally tested using U. S. registry data. This concept, used to compare NOACs and warfarin, have been facilitated by registry data. 11, 44 Banerjee et al. used "real-world" data on net clinical benefit of warfarin from the Danish National Patient Registry and modeled the expected net clinical benefit for NOACs (dabigatran, rivaroxaban, and apixaban) on the basis of recent clinical trial outcomes. 11 The findings indicated that when there is a high risk of both ischemic stroke and intracranial hemorrhage, all 3 of the new agents have a greater net clinical benefit, compared to warfarin (Figure).
Registry data from the National Cardiovascular Data Registry's Acute Coronary Treatment and Intervention Outcomes Network (ACTION) Registry-Get with the Guidelines program also suggest that the patients at highest risk of ischemic stroke are least likely to take OAC medication,  4  again highlighting the need for practice improvement and compliance to ensure the best outcomes among patients with AF. These data on utilization could be gleaned only from registries. Data from a number of registries providing information on the use of warfarin, NOACs, and aspirin are shown in Table  5. The PREFER-AF Registry found that OACs are now much more widely used than was reported in the German AFNET and the Euro Heart Survey registries on AF, and that NOACs are used by 6. 1% of patients with AF. 13  The increasing number of registries established in recent years to follow trends and outcomes linked to the NOACssuch as GARFIELD, GLORIA-AF, PREFER-AF, and Randomized Evaluation of Long-Term Anticoagulation Therapy (RE-LY)-will continue to highlight practice variations in diverse healthcare settings and patient populations.
For example, CARAF charted the use of antiarrhythmic and atrioventricular-nodal blocking drugs from 1991 to 2007 and showed a peak in AAD use in 1994 (42. 5%), followed by a gradual decline, whereas use of rate-controlling medications, particularly b-blockers, increased (52. 5% in 2007). 21 Data from a number of registries providing information on the use of rhythm-and rate-control treatments are shown in Table  5. The AFFECTS registry assessing patterns of care in the United States showed that most first-line therapies were aligned with the 2006 American College of Cardiology (ACC)/American Heart Association (AHA)/European Society of Cardiology guidelines. 18, 19 In AFFECTS, rhythm-control treatment was prescribed for 67% of patients with paroxysmal AF and 55% of patients with persistent AF and was more often the initial treatment strategy for older patients.
71 this unselected cohort, treatment with flecainide, propafenone, sotalol, or amiodarone was not associated with increased risk of death, compared to treatment without AADs, even during the first 30 days when risk is usually highest. Registries assembled by regulatory agencies, such as the U. S. Food and Drug Administration (FDA) Mini-Sentinel program and the U. S. Department of Defense database, reported lower all-cause mortality with dronedarone than with other AADs. 72 Population-based administrative databases are able to provide information from a large general population of patients with AF, with longer follow-up than is possible in most RCTs. The FDA Mini-Sentinel program aims to detect and refine safety signals for marketed medical products and additionally identify algorithms used within administrative databases to detect and analyze health outcomes for patients with AF.
73  This registry suggests that a substantial proportion of the variation in AF prevalence across studies may be the result of the choice of different criteria for confirming AF. A systematic literature review was performed to characterize the validity of algorithms to identify patients with AF from electronic health data. 74 Use of nonrepresentative populations, a paucity of recent data, and a disproportionate focus on data from inpatients hindered conclusions about algorithm validity, and the researchers advised that additional research is needed in contemporary representative populations. Follow-up of patients in registries can track AF recurrence, although inferences require confirmatory evidence from clinical trials. In the MADRE registry, dronedarone was administered for rhythm control in a small cohort of patients followed for 300 days.
Unlike RCTs, which include highly selected patients that limit generalizability, registries are population based and therefore subject to bias. Registries lack controls from which to draw comparative assessments. Furthermore, data are lacking for some regions, and the majority have focused on Europe and the United States, although studies such as RECORD-AF Asia Pacific seek to address this. It has been also suggested, by the 2014 AHA/ACC/Heart Rhythm Society guidelines for management of patients with AF, that comparisons between registries from different sociocultural backgrounds may be obscured by the difficulty to quantify and report individualized antithrombotic therapy based on a shared physician-patient decision. 84 An important factor to consider when studying registry data is whether the registry is sponsored through industry, given that this may introduce the possibility of bias into the outcomes.
Some challenges face those attempting to initiate registries, such as specifying the purpose of the registry early on, how the data will be used, who will analyze it, who will have access to it, and, most important, who will fund it. 36, 85 This information can, for example, determine whether patients in the registry are similar to those enrolled in RCTs, generate hypotheses for future clinical trials, and determine the effectiveness of therapy in subpopulations. Obtaining sufficient funding for a registry is also a critical challenge. Previous registries have been either voluntary or linked to reimbursement. 36 Determining the best funding mechanism for a registry early on is one of the most critical first steps to the success of such a registry. Investment in a national registry certainly requires substantial resources.
Conclusions As highlighted in this review, registries extend knowledge of the natural history, risk factors, treatment practices, and longterm outcomes and risks of management strategies within a truly representative population of AF patients managed in clinical practice. Together with patient database evaluations, these resources can greatly improve understanding of the needs and gaps in care for diverse patient subgroups. Though a comprehensive review of administrative databases was not within the scope of this review, increasingly relevant literature derived from mining of patient data can inform the management of patients with AF in an array of care settings. Registry data are the means by which to determine whether patients are managed in line with evidence-based guidelines-but they offer more than just a reflection of whether everyday practice adheres to accepted norms or ideals.
, 2008). Recall that a spatial correlation of speckle is a feature typical for SAR images  (Solbo&Eltoft, 2008 , Lukin et al. , 2008; Lukin et al. , 2009; Ponomarenko et al. , 2011)  which is not often taken into account in SAR image simulations. Thus, we come to a necessity to perform intensive testing of BENC methods without having a set of standard test images. Our idea then is to create a set of test SAR images with a priori known characteristics of the speckle similar to those ones observed in practice. In this sense, TerraSAR-X images can be a good choice (in Section 2, we explain this in detail). Note that quite many of them are now available in the convenient form and their amount is rapidly growing (see http://www. infoterra. de/free-sample-data). Then, it becomes possible to test BENCs for simulated data (Section 3) and to predict what could happen in practice.
To get an imagination on fully developed speckle PDF, consider real-life data produced by TerraSAR-X imager. Its attractive feature is that data (images) are freely available at the aforementioned site. These data have full description of parameters of the imaging system operation mode used for obtaining each presented image. Large size images (thousands to thousands pixels) for many different areas of the Earth are offered. Furthermore, a brief description of a territory, observed effects and cover types is given. This allows selecting and processing data with different numbers of looks, properties of a sensed terrain, a desired polarization, etc. Fragments of certain size as 512x512 pixels can be easily cut from large size data arrays and studied more thoroughly. Another positive feature is that single-look images are presented in the complex valued form.
This allows obtaining single-look images in aforementioned forms (representations). It also makes possible to analyze distributions of real and imaginary part values for image fragments, etc. While considering single-look SAR images in this paper, we use amplitude images since it is the most common form and it provides convenient representation for visual analysis. One more advantage is that TerraSAR-X is a high quality system designed by specialists from German Aerospace Agency DLR who have large experience in creation and management of spaceborne SAR systems  (Herrmann et al. , 2005). The TerraSAR-X imager provides a stability of noise characteristics and practical absence of an additive noise in formed images. Later, it will be explained why this is so important for further analysis. To partly corroborate conformity of theory and practice for single-look SAR images, we have manually cropped several sub-arrays of complex valued data that correspond to homogeneous terrain regions.
For all considered real-life SAR images, the value of r was larger than 1. 05  (Lukin et al. , 2011b)  for single-look SAR images and considerably larger for multi-look ones. This additionally gives an evidence in favor of the hypothesis that speckle is spatially correlated. Thus, we can state that speckle is spatially correlated in the considered TerraSAR-X images, both singleand multi-look ones. Then, this effect should be taken into account in simulations. To simulate single-and multi-look SAR images, we have used four aerial optical images as I tr (all test images are of size 512x512pixels). These four images are presented in Fig. 3. Positive features of these images allowing to use them in simulation of SAR data are the following. First, these images have practically no self-noise that could later influence blind estimation of speckle statistics.
Thus, we can state that speckle is spatially correlated in the considered TerraSAR-X images, both single-and multi-look ones. Then, this effect should be taken into account in simulations. To simulate single-and multi-look SAR images, we have used four aerial optical images as tr I (all test images are of size 512x512pixels). These four images are presented in Fig. 3. Positive features of these images allowing to use them in simulation of SAR data are the following. First, these images have practically no self-noise that could later influence blind estimation of speckle statistics. Second, these are the images of natural scenes and, thus, they contain large quasi-homogeneous regions, edges with different contrasts, various textures and small-sized targets. Note that we have simulated speckle with the same statistics for all pixels ignoring the fact that for small-sized targets it might differ from speckle in homogeneous image regions.
7. The obtained array C is transformed to 2D array RES of size K=I Im × J Im in the way inverse to it has been done in step 2. The source code in Matlab that realizes the described algorithm is presented below: I ij n , i = 1,. I Im , j = 1,. , J Im. The image presented in Fig. 4 (b) has been obtained in the way described above. Moreover, this allows getting multi-look images if several realizations of the speckle with desired spectrum are generated and then averaged.
Then one has σ ̑loc = F I ¯loc where F is the fitted straight line parameter that serves as the estimate σ ̑μ. This kind of a scatter-plot is shown in Fig. 8(c ) for the same singlelook SAR image. Visual analysis of the scatter-plots in Figs. 8(b ) and 8(c) shows that for them there are also some clusters of normal local estimates whereas abnormal estimates are present as well. An advantage of the latter two approaches is that it is, in general, simpler to fit a straight line than a higher order polynomial. In particular, there are standard means for this purpose as, e. g. , the Matlab version of robustfit method (DuMouchel&O'Brien, 1989). For methods analyzed below, we have used the approach based on (6). Finally, there are also methods that exploit scatter-plot data to find cluster centers and curve (line) fitting using these scatter-plot centers  (Zabrodina et al.
Herschel and Spitzer HLS0918 was discovered as an unusually bright '500 µm peaker' source towards the edge of Herschel/SPIRE  (Pilbratt et al. 2010; Griffin et al. 2010 ) maps (250, 350 and 500 µm) of Abell 773, observed as part of the "Herschel Lensing Survey"  (Egami et al. 2010). The SPIRE observations use large map mode, with a coverage of ∼17 ′ × 17 ′. The images were produced via the standard reduction pipeline in HIPE v9. 0, the SPIRE Photometer Interactive Analysis (SPIA) package v1. 7, and v8. 1 calibration product. Note that this is a significant re-reduction since C12, including an improved treatment of the baseline removal (also known as 'de-striping'). The SPIRE images are confusion limited  (3 σ = 17, 19, 20 mJy; Nguyen et al. 2010)  with beam sizes of 18, 25, 36 ′′ (250, 350, 500 µm respectively).
Calibration of the uv visibilities was performed using the Interactive Data Language (IDL) MIR package. The blazar 3C84 was used as the primary bandpass calibrator and Titan was used for absolute flux calibration. The nearby quasars 0927+390 (F 880µm = 0. 5 Jy, 6 degrees from target) and 0920+446 (F 880µm = 2. 2 Jy, 15 degrees from target) were used for phase and amplitude gain calibration, respectively. The Multichannel Image Reconstruction, Image Analysis, and Display (MIRIAD) software package  (Sault et al. 1995)  was used to invert the uv visibilities and deconvolve the dirty map. Natural weighting was chosen to obtain maximum sensitivity and resulted in an elliptical Gaussian beam with a full-width half-maximum (FWHM) of 1. 33 ′′ × 1. 10 ′′ and position angle of 94 degrees east of north.
For reference, the morphology of the continuum map is replicated in the other panels as white contours. dow. The bright (S 18. 5GHz ≈ 0. 8 Jy) calibration source, J0937+5008, was observed every few minutes to determine accurate complex gain solutions and bandpass corrections. 3C 286 was observed to set the absolute flux scale, and the pointing accuracy was checked locally every hour. The data were reduced and imaged using aips following the recipes described by  Ivison et al. (2011) , though with a number of significant changes: data were loaded using bdf2aips, avoiding any compression, and fring was used to optimize the delays, in software, based on 1 min of data for 3C 286. The basebands were knitted together using the noifs task, yielding a uv dataset with 1024 × 2-MHz channels centered near the expected frequency of the CO line.
Lensing model Derivation of the absolute luminosity, along with other source-plane characteristics such as the true morphology, requires a well-constrained model of the magnification and distortion due to lensing. For HLS0918, the lens model has to combine the effect of both Abell 773 (z = 0. 22) and the foreground galaxy at z = 0. 63. The large distance from the centre of A773 (5. 6 ′ ) means that the cluster lens effect is secondary (∼ 10% contribution). The best possible lens model is derived using LensTool  (Jullo et al. 2007 ), via constraints obtained from both the SMA data described in this paper, and additional observations from the Plateau de Bure Interferometer (PdBI), to be presented in  Boone et al. (in prep. ). Comprehensive, quantitative details of the observed constraints and parameters for the lens model, including an in-depth analysis of differential lensing enabled by the higher spatial resolution PdBI imaging, will be given in Boone et al.
High-z sources often exhibit ratios an order of magnitude or more larger than local star-forming galaxies of similar FIR luminosity (e. g. Stacey et al. 2010; Swinbank et al. 2012) , which is usually attributed to large, extended [CII] reservoirs. Figure  6  displays this ratio as a function of FIR luminosity, correcting for the effect of magnifica-   2010 ) and  Valtchanov et al. (2011). Low redshift star-forming galaxies based on ISO data from  Malhotra et al. (2001)  and Herschel/PACS data from  Sargsyan et al. (2012)  shown as crosses and open squares respectively. For the local data, we calculate the median (dotted line) and scatter (1 σ = grey shaded area). HLS0918 is located in the same region as the other high luminosity, high redshift sources, which exhibit L [CII] approximately an order of magnitude larger than local galaxies with similar FIR luminosity.
The paucity of lower redshift galaxies with either 12 CO(1-0) observations, or such large SFR surface densities, means that a direct comparison is difficult: are these bright examples offset due to an intrinsic difference in the mode of star formation, or is this a selection effect whereby we are only probing the upper edge of the population? We can examine the resolved KS relation for HLS0918. Although we can separate the individual components, we do not know the spatial extent of each clump and cannot directly determine the surface densities. Instead, we grid the spatial data to calculate the mean surface densities for different regions of HLS0918 (in the image plane). We adopt the 12 CO(1-0) map pixel size (0. 3×0. 3 ′′ ) as the most convenient binning regime. The continuum map is smoothed to the 12 CO(1-0) beam and re-binned, to give SFR surface density in bins exactly matched to the gas surface densities.
7 merger BR1202-0725, which has a quasar host galaxy as a close companion, where two recent analyses of the ALMA [CII] data differ significantly in their conclusions concerning the existence of an outflow (e. g. Wagg et al. 2012; Carniani et al. 2013). In HLS0918, the derived conditions are not so extreme as to rule out VB simply being a third galaxy rather than an outflow. Before either scenario can be adopted, further observations are required, such as maps of e. g. OH + , CH + , H 2 O +. Such species are excellent tracers of molecular outflows, and have been reported for several local ULIRGs, e. g. Arp220,  (Rangwala et al. 2011) and Mrk231 (van der Werf et al. 2010).
2 shows the power of gravitational lensing in revealing star formation and galaxy evolution in the early Universe. This paper also offers a preview of the type of analysis that will become possible for a large number of high-redshift galaxies once ALMA progresses to full science operations. TDR is supported by a European Space Agency (ESA) Research Fellowship at the European Space Astronomy Centre (ESAC), in Madrid, Spain. IRS acknowledges support from STFC, a Leverhulme Fellowship, the ERC Advanced Investigator programme DUSTYGAL 321334 and a Royal Society/Wolfson Merit Award. The authors acknowledge fruitful discussions within the international team lead by D. Schaerer on "Exploiting the Multi-Wavelength Lensing Survey" at ISSI (International Space Science Institute) in Bern 2010-2013. Submillimeter Array is a joint project between the Smithsonian Astrophysical Observatory and the Academia Sinica Institute of Astronomy and Astrophysics and is funded by the Smithsonian Institution and the Academia Sinica.
This work also includes observations carried out with the Karl G. Jansky Very Large Array (VLA): The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. Additionally, based on observations carried out with the IRAM Plateau de Bure Interferometer and the IRAM 30m Telescope. IRAM is supported by INSU/CNRS (France), MPG (Germany) and IGN (Spain). This work follows on from observations made with the Herschel Space Observatory, a European Space Agency Cornerstone Mission with significant participation by NASA. Support for this work was provided by NASA through an award issued by JPL/Caltech. We would also like to thank the HSC and NHSC consortia for support with data reduction.
No asymmetries due to the CME are expected in the left and right hemispheres separated by the plane normal to the reaction plane. In this paper, a new correlation technique is introduced that may be sensitive to the charge separation that was previously investigated in STAR. Consistency is found between the previously published data  [14, 15]  and the results from the present analysis when using the same charge correlator observable (see Appendix A). In this paper, a new approach is used to explore the charge asymmetries on an event-by-event basis, which extends the previous STAR measurements. The results obtained from d+Au and Au+Au collisions at √ s NN = 200 GeV at RHIC measured by the STAR experiment are reported  [17]. This paper is organized as follows. The analysis method is described in Sec.
9 million d+Au events (Run III) were used in this analysis. The Run VII data used for comparison and for the ZDC first harmonic event plane study consists of 70 million minimum-bias Au+Au events. The Au+Au collision centrality is defined according to the measured charged particle multiplicity in the main Time Projection Chamber (TPC) within the pseudorapidity range |η| < 0. 5  [21]. Results will be presented as a function of centrality in terms of the number of participant nucleons, N part , which was obtained from a Monte Carlo Glauber calculation  [22]. The corresponding impact parameters and the uncorrected and corrected charged hadron multiplicities can be found in Ref. [22]. The main detector used for this analysis was the Time Projection Chamber (TPC)  [23, 24]. The TPC is surrounded by a solenoidal magnet providing a uniform magnetic field of 0.