dataesr/scientific-paragraphs-categorization huggingface dataset:
The SEPIA-ACS1 TIMI 42 study recommended using intermediate doses of otamixaban in future studies as more appropriate: low doses were ineffective and high doses were shown to be dangerous. Treatment with otamixaban at doses of 0. 105 and 0. 140 mg/kg/h was associated with a 40% reduction in myocardial infarction, ischaemic events and all-cause death without a significant increase in bleeding rates compared to UFH plus eptifibatide (Table  5 )  (61). A phase III study (clinicaltrials. gov NCT01076764) has begun recruitment. Furthermore, the pharmacokinetic and pharmacodynamic profiles of otamixaban will be investigated in patients with mild, moderate or severe renal insufficiency (clinicaltrials. gov NCT01120314) and with mild or moderate hepatic insufficiency (clinicaltrials. gov NCT01126086).
5mg Warfarin (INR 2-3) Stroke or systemic 1. 27%/year vs Major bleeding 2. 13%/year vs 3. 09%/year randomized, double-blind years on average bid in selected embolism; death 1. 60%/year (p<0. 001) patients) from any cause (p<0. 001for non- inferiority, p=0. 01for superiority); 3. 52%/year vs 3. 94%/year (p=0. 047) Acetylsalicylic AVERROES / phase III, 5 599 / 1. 1 years 5mg bid (2. 5mg acide (81-324mg Stroke or systemic 1. 6%/year vs Major bleeding 1. 4%/year vs 1. 2%/year randomized, double-blind, on average bid in selected od) embolism 3. 7%/year (p=0. 57) superiority patients) (p<0. 001) Betrixaban EXPLORE-Xa / phase II, 508 / 3 months 40mg, 60mg or Open-label warfarin Underway Major and clinically Underway randomized, double-blind 80mg od (INR 2-3) relevant non-major bleeding events Edoxaban NCT00504556/ phase II, 1 146 / 3 30mg and 60mg Open-label warfarin Underway Major and clinically 10.
6%, 7. 8%, 3. 8%, 3. 0% randomized, double-blind months od, 30mg and (INR 2-3) relevant non-major for 60mg bid, 30mg bid, 60mg bid bleeding events 60mg od, 30mg od, respectively, vs 3. 2% ENGAGE-AF TIMI-48 / 20 500 / 24 30mg and 60mg Warfarin (INR 2-3) Stroke and systemic Underway Major bleeding Underway phase III, randomized, months od embolism double-blind, non-inferiority Darexaban NCT00448214 / phase II, 448 / 16 weeks 30mg, 60mg, Open-label warfarin Stroke and systemic No Major and clinically 2. 2%, 2. 2%, 3. 2% and (YM-150) randomized, double-blind 120mg and 240mg (INR 2-3) embolism thromboembolic relevant non-major 16. 7% for 30mg od, 60mg od strokes reported bleeding events od, 120mg od, 240mg od vs 2. 1% OPAL-2 / phase II, 1 280 / 16 6 doses Warfarin (INR 2-3) Stroke, systemic Not detailed Major and clinically Not detailed randomized, double-blind months embolism, all deaths relevant non-major bleeding events Abbreviations: bid, twice daily; INR, international normalized ratio; od, once daily.
4% respectively, vs 2. 8% TAK-442 NCT00677053 / 2 753 / 24 weeks 40, 80 and 160mg Placebo + Composite of Underway Major bleeding events Underway phase II, od, 10, 20, 40, 80 antiplatelet cardiovascular defined by the randomized, and 120mg bid + therapy mortality, non-fatal thrombolysis in MI scale double-blind antiplatelet therapy MI, non-fatal stroke or myocardial ischaemia requiring hospitalization Otamixaban SEPIA- 3 241 / 7-30 days 0. 08mg/kg bolus UFH + Composite of all- 7. 2%, 4. 6%, 3. 8%, 3. 6% et TIMI major or minor 1. 6%, 1. 6%, 3. 1%, 3. 4% (XRP0673) ACS1TIMI 42/ followed by eptifibatide cause death, MI, 4. 3% for 0. 035, 0. 070, bleeding not related to and 5. 4% for 0. 035, 0. 070, phase II, infusions of 0. 035, urgent 0. 105, 0. 140 and coronary-artery bypass 0. 105, 0. 140 and randomized, 0.
070, 0. 105, revascularisation or 0. 175mg/kg/h, respectively, grafting up to 7 days 0. 175mg/kg/h, respectively, double-blind 0. 140 or bailout glycoprotein vs 6. 2% vs 2. 7% 0. 175mg/kg/h IIb/IIIa inhibitor use up to 7 days NCT01076764 / 30-180 days UFH + Composite of all- Underway TIMI major and minor phase III, eptifibatide cause death and MI bleeding randomized, double-blind, superiority UnderwayAbbreviations: bid, twice daily; MI, myocardial infarction; od, once daily; TIMI, thrombolysis in myocardial infarction; UFH, unfractionated heparin.
Andrews, Scotland; -FTS: the 2-m Faulkes Telescope South located at Siding Spring Observatory in New South Wales, Australia; -EulerCam: the new camera at the 1. 2-m Euler-Swiss telescope at La Silla, Chile; -BUSCA: at the Calar Alto Observatory 2. 2-m telescope, Spain; -OverSky: the 0. 36-m telescope at the OverSky Observatory, La Palma, Spain; -NITES: a 0. 4-m telescope at La Palma, Spain. The dates of the transit observations made with these facilities as well as the filters used are reported in Table  2. Standard aperture photometry was carried out on all these datasets, using comparison stars available in the different fields for relative photometry. The extra light curves of WASP-52, 59, and 60 are plotted in the upper panels of Figs. 1, 3, and 4, respectively.
The surface gravity log g * was determined from the Ca i lines at 6162 Å and 6439 Å  (Bruntt et al. 2010a ), along with the Na i D and Mg i b lines. The spectral types were established from T eff using the table in  Gray (2008). The elemental abundances were determined from equivalent width measurements of several clean and unblended lines. The microturbulence ξ t was evaluated from Fe i using the method of  Magain (1984). The quoted error estimates include that given by the uncertainties in T eff , log g * and ξ t , as well as the scatter due to measurement and atomic data uncertainties. The projected stellar rotation velocities v sin i * were determined by fitting the profiles of several unblended Fe i lines. They agree with the measurements secured from the crosscorrelation function following  Boisse et al.
EulerCam data also show irregularities. We have analyzed the SuperWASP light curve to determine whether they are periodic, and possibly due to the combination of magnetic activity and the rotation of the star. The value of v sin i * derived above together with the estimated stellar radius implies a rotation period of 5 -15 days, assuming that the rotation axis of the star is approximately aligned with the orbital axis of the planet. We show below in Sect. 3. 3 that this is not exactly the case, but the misalignment remains low. We used the sinewave fitting method described in  Maxted et al. (2011)  to calculate the periodograms shown in Fig. 6. These are calculated over 4096 uniformly spaced frequencies from 0 to 2. 5 cycles/day. The false-alarm probability levels shown in these figures are calculated using a boot-strap Monte Carlo method also described in  Maxted et al.
(2011). Variability due to star spots is not expected to be coherent on long timescales as a consequence of the finite lifetime of star-spots and differential rotation in the photosphere, and so we analyzed the two seasons of data for WASP-52 separately. The second season of data shows a highly significant periodic modulation with a period of 16. 4 ± 0. 04 days and an amplitude of 9. 6 milli-magnitudes. We used a boot-strap Monte Carlo method to estimate the error on this period. We also calculated periodograms of three stars with similar magnitudes and colors to WASP-52 observed simultaneously with the same WASP camera. None of these stars showed significant periodic modulation in the same frequency interval. The strongest peak in the first season of data is marginally significant and is consistent with the 1-day alias of the period detected in the second season of data.
Method For a given system, all the available data were fitted simultaneously: the radial velocities with a Keplerian orbit, and the transit light curves with the  Mandel & Agol (2002)  algorithm using four non-linear limb-darkening coefficients from the tabulations of  Claret (2004). The global fit was done with the latest version of the Markov-chain Monte-Carlo (MCMC) procedure presented in detail by Collier  Cameron et al. (2007b)  and  Pollacco et al. (2008). The free parameters in the fits are the transit epoch T 0 , the orbital period P, the depth of the transit or the planet/star area ratio (R p /R * ) 2 , the total transit duration t T , the impact parameter b, the eccentricity e of the orbit, the argument of periastron ω, the semi-amplitude K 1 of the radial velocity variations, the n systemic radial velocities γ n (one for each of the n radial velocity datasets).
WASP-52 There is a good agreement between the stellar mass obtained from the MCMC and that estimated from mass tracks in evolution diagrams for WASP-52. The red noise levels in the light curves are negligible; averaging the photometric data in 6-to 10-minute bins made no appreciable difference to the error bars on the derived parameters. The radial velocity fit provide sys-temic radial velocities of -0. 8953 ± 0. 0075, -1. 0415 ± 0. 0033, -0. 9265 ± 0. 0062, and -0. 8877 ± 0. 0040 km s -1 for SOPHIE HE1, HE2, HR, and CORALIE, respectively, with a dispersion of the residuals of the order of 13 m s -1. We fit the data using only parts of the radial velocity datasets, which provide similar results. This suggests that the systematic shift of 146 ± 8 m s -1 between the two SOPHIE HE datasets (see Sect.
2. 2) has no significant impact on the derived parameters of the system. There is a hint of a drift of ∼ +40 m s -1 over the 15-month time span of our observations. It could be due to an extra component in the system, but the unknown systematic shifts between datasets do not allow any firm conclusion to be drawn on the source of the drift. No significant eccentricity is detected. The orbital period is 1. 75 day. The one-day alias of that signal is 2. 33 days; it should be considered as the photometric and radial velocity observations were made with a typical 1day frequency. The periodograms show signal at both frequen-Fig. 7. HR diagrams for WASP-52, 58, 59, and 60 (Yonsei-Yale stellar models). Each host star is denoted by a blue cross as a function of the stellar density and the effective temperature.
WASP-60 The systemic radial velocities of WASP-60 are -26. 4967 ± 0. 0103 km s -1 and -26. 6288 ± 0. 0054 km s -1 for the two HE datasets. The systematic shift between them (132 ± 12 m s -1 ) agrees with that found above for WASP-52 (146 ± 8 m s -1 ); this reinforces our conclusion that this shift has an instrumental origin (see Sect. 2. 2). The radial velocity residuals show a 20-m s -1 dispersion, in agreement with the expected error bars on their measurements. There is a hint of a drift of ∼ +70 m s -1 over the 16-month time span of our observations. Again, this may suggest the presence of an additional body in the system, but the unknown systematic shift between the two datasets prevents any firm conclusion from being drawn. The stellar mass obtained from the MCMC analysis agrees with that estimated from evolutionary tracks in the densitytemperature plane diagrams for WASP-60.
Their uncertainties are negligible here for the fit of the Rossiter-McLaughlin anomaly. We checked that varying them in their 1-σ intervals has no impact on the quality of the fit nor on the derived λ value. The main parameters that play a role in this fit are the systemic velocity of that particular dataset, λ, and v sin i *. As these parameters could be correlated in the Rossiter-McLaughlin fit, we computed the χ 2 of the fit on a three-dimensional grid scanning all their possible values. The systemic velocity was determined with a ±5-m s -1 accuracy. It is constrained thanks to the observations secured immediately before and after the transit. The confidence interval contours estimated from χ 2 variations for the λ and v sin i * show no correlation between these two parameters, as expected for systems with impact parameter b significantly different from zero.
Acknowledgements. We thank the 2010 cohort of the AS4025 Observational Astrophysics class at the  University of St Andrews  for their help in analyzing and eliminating astrophysical false positives in the JGT data, and for recognising WASP-52 as a good potential planet candidate. The research leading to these results has received funding from the  European Communitys Seventh Framework Programme  ( FP7/2007-2013)  under grant agreement num-ber RG226604 (OPTICON), as well as the  Programme National de Planétologie (PNP)  of  CNRS/INSU (France). RFD is supported by  CNES.
Detector and data samples The LHCb detector  [16]  is a single-arm forward spectrometer covering the pseudorapidity range 2 < η < 5 (forward region), designed for the study of particles containing b or c quarks. The detector includes a high precision tracking system consisting of a silicon-strip vertex detector (VELO) surrounding the proton-proton interaction region, a large-area silicon-strip detector located upstream of a dipole magnet with a bending power of about 4 Tm, and three stations of silicon-strip detectors and straw drift-tubes placed downstream. The combined tracking system has a momentum resolution p/p that varies from 0. 4% at 5 GeV/c to 0. 6% at 100 GeV/c, and an impact parameter resolution of 20 μm for tracks with high transverse momentum. Charged hadrons are identified using two ring-imaging Cherenkov detectors.
The protons are only marginally deflected and remain undetected inside the beam pipe. Therefore the signature for exclusive vector meson production is an event containing two muons and no other activity. The analysis is performed using 36 pb -1 of proton-proton collision data collected at LHCb in 2010. In this data taking period, the average number of interactions per bunch crossing varied up to a maximum of about 2. 5, with most luminosity accumulated at larger values. In order to identify exclusive candidates, the analysis is restricted to events with a single interaction. Dedicated Monte Carlo generators have been used to produce signal and background events which are passed through a GEANT4  [17]  based detector simulation, the trigger emulation and the event reconstruction chain of the LHCb experiment.
Inelastic background determination The requirement of two tracks and no other visible activity enriches the sample in exclusive events. However, this does not guarantee that there is no other activity in the regions outside the LHCb acceptance. The contributions from two non-exclusive processes have been considered: inclusive prompt charmonium produced through colour strings, which leads to large numbers of additional particles; and inelastic J/ψ photoproduction (as shown in figure  3 ), where gluon radiation or proton dissociation lead to a small number of additional particles. The former has been evaluated using simulated samples of prompt charmonium, generated using PYTHIA  [20]  and normalized using a data sample where the zero backward tracks requirement has been removed; it is found to be negligible.
Evaluation of the photon-proton cross-section The differential cross-sections for the process pp → pJ/ψ p given in table 4 are transformed into cross-sections for the process γ p → J/ψ p using a re-arrangement of equation (  3 )  The photoproduction cross-sections at W + and W -are determined independently using equation  (6)  and substituting into the right-hand side the expected cross-section for the alternative W solution from the power law determined above. σ γ p→V p (W ± ) = 1/r(y) dσ dy pp→pV p -k ∓ dn dk ∓ σ γ p→V p (W ∓ ) k ± dn dk ±. ( 6 The LHCb data are plotted together with the H1 and ZEUS data in figure  6. The power law dependences determined from LHCb data and from HERA data are also indicated. The uncertainty on the LHCb power law determination is shown by the shaded band. Only experimental uncertainties are shown on the LHCb data, which have significant bin-to-bin correlations due to the purity determination.
Acknowledgments We thank  Lucian Harland-Lang ,  Valery Khoze ,  James Stirling  and  Graeme Watt  for many helpful discussions. We express our gratitude to our colleagues in the CERN accelerator departments for the excellent performance of the LHC. We thank the technical and administrative staff at the LHCb institutes. We acknowledge support from  CERN  and from the national agencies:  CAPES ,  CNPq ,  FAPERJ  and  FINEP (Brazil) ;  NSFC (China) ;  CNRS/IN2P3  and  Region Auvergne (France) ;  BMBF ,  DFG ,  HGF  and  MPG (Germany) ;  SFI (Ireland) ;  INFN (Italy) ;  FOM  and  NWO  (The Netherlands); SCSR (Poland);  ANCS/IFA (Romania) ;  MinES, Rosatom ,  RFBR  and  NRC 'Kurchatov Institute' (Russia) ;  MinECo, XuntaGal and GENCAT (Spain) ;  SNSF  and  SER (Switzerland) ;  NAS Ukraine (Ukraine) ;  STFC  ( United Kingdom );  NSF (USA).
We also acknowledge the support received from the  ERC  under  FP7. The Tier1 computing centres are supported by  IN2P3 (France) ,  KIT  and  BMBF (Germany) ,  INFN (Italy) ,  NWO  and SURF (The Netherlands),  PIC (Spain) ,  GridPP  ( United Kingdom ). We are thankful for the computing resources put at our disposal by  Yandex LLC (Russia) , as well as to the communities behind the multiple open source software packages that we depend on.
Acknowledgments We would like to thank  Diego Marqués ,  Ruben Minasian ,  Eran Palti  and  Daniel Waldram  for useful discussions. This work was supported in part by the  ANR  grant  08-JCJC-0001-0  and the  ERC   Starting Grants 259133 -ObservableString and 240210 -String-QCD-BH.
Site description, climate and data This study was performed in the high Arctic surroundings of the research facilities in Ny-A ˚lesund, Svalbard (78855?N, 11858?E), where the average (1961Á1990) annual temperature is Á6. 391. 4 8C with February the coldest month (Á14. 693. 4 8C) and July the warmest (4. 990. 8 8C)  (Førland et al. , 1997). The average annual precipitation in the Svalbard archipelago ranges from 190 to 525 mm. Ny-A ˚lesund has an annual precipitation of 385 mm and shows greatest precipitation in AugustÁOctober and March, while MayÁJune receives the least  (Førland et al. , 1997). All snow measurements in this study were conducted on the glacier, Austre Brøggerbreen, a few kilometres outside the research village (Fig. 1 ). Atmospheric concentrations of HNO 3 and p-NO 3 were measured by Norwegian Institute for Air Research 1 (NILU)  (Aas et al.
Measurements 2. 3. 1. Snow Tray. Dry deposition of dissolved nitrate onto the snow surface was measured during the field campaign on the middle part of Austre Brøggerbreen (Fig. 1 ) where pre-cleaned PE-plastic trays (5 )25 )30 cm) were used to evaluate nitrate concentration changes in the snow over time  (Cadle et al. , 1985; Johansson and Granat, 1986; Cadle, 1991; Cress et al. , 1995). The plastic trays were filled with surface snow, weighed and then either collected immediately (zero samples) or inserted to the snow pack (exposed samples) with their exposed snow surface levelled with the surrounding snow. Attention was paid to extract snow for zero and exposed samples from adjacent locations across a homogenous surface snow using a clean 1 Data available at: ebas. nilu. no 2 Data available at: www.
64990. 012 mg m (2 (Fig. 8c  and Table  2 ). The corresponding estimates for the spring field campaign period were (0. 01190. 002 and (0. 06990. 001 mg m (2 for F pÀNO 3 (DMPS) and F pÀNO 3 (LND), respectively (Table  2 ). Due to the occasional distinctly smaller wind velocities measured at the upper levels of the CCT, indicating a very shallow boundary layer, and also the occasional absence of atmospheric concentration estimates, the loss of modelled hourly data was up to 63% for the F HNO 3 method during the winter season. For F pÀNO 3 , 66 and 63% of the hourly data were missing (DMPS and LND, respectively) due to the same reason. Since daily averages have been used for the calculations the lack of hourly data was smoothed out, resulting in 22% of HNO 3 data and 25 or 22% paucity of p-NO 3 data (DMPS and LND, respectively) missing in the final winter season sum up.
Acknowledgements As a part of the international project 'Sources, sinks and impacts of atmospheric nitrogen deposition in the Arctic' (NSINK), this project received financial support from an EU Marie Curie Initial Stage Training Network Award NSINK (FP7 215503) and fieldwork were supported by an Arctic Field Grant, Svalbard Science Forum. NILU's atmospheric monitoring program at the Zeppelin Station is financed by the Norwegian Climate and Pollution Agency and ITM's research at the same station is supported by the Swedish Environmental Protection Agency. This is also a contribution to 'Crysophere-Atmosphere interaction in a changing Arctic climate (CRAICC)' a Top-Level Research Initiative (TRI). Logistic support was provided by the Norwegian Polar Institute staff at the Sverdrup Station, Ny-A ˚lesund, while A.
Inlet lines ran from the measurement level (5 m agl) to an air-conditioned house. This site represents large land use changes and associated regional biomass burning as characteristic of Amazonia in contact with human interferences. At the PVH site, the dry season is from June to December, and the wet season from January to May. Adding to the ground based in situ measurements, remote sense data from the NASA/AERONET sunphotometers network and from the MODIS satellite sensor were also analysed. Reported AOD observations from AERONET are level 2. 0, and data were taken from two sites in southern Amazonia (same region as the PVH site): Abracos Hill (10S; 62W) and Ji-Parana-SE (10S; 61W), and from two sites in central Amazonia (same forest reservation as the TT34 site): Balbina (1S; 59W), and Manaus-EMBRAPA (2S; 59W).
Dry Season Wet Season for truncation errors. 68 Aerosol particle absorption was measured using MAAP absorption photometers (MultiAngle Absorption Photometry -Thermo Inc. , Model 5012). 69 The MAAP reports equivalent black carbon (BC e ) concentrations at 637 nm, which were converted to absorption coefficients assuming a mass absorption coefficient of 6. 6 m 2 g À1. A 5% correction was applied to the data to account for an adjustment of wavelength. Pressure and temperature measured inside the nephelometer were used for adjusting scattering and absorption coefficients to 1013 mbar and 0 C. 44  No trends in aerosol mass concentrations can be observed in the preserved central Amazonia. The concentrations of equivalent black carbon at the TT34 site have a pronounced seasonal behaviour (Fig. 4 ), with increased concentrations from August to December due to long-range transport of biomass burning aerosol.
Aerosol mass spectrometry measurements in Amazonia Aerosol mass spectrometry (AMS) is a valuable tool to measure aerosol composition in real time. ACSMs were recently deployed at the sites in Porto Velho (PVH) and central Amazonia (TT34), with the intention that they begin a multiyear record of data. At the PVH site, the system collected data from 6 to 30 September 2012 during the SAMBBA (South American Biomass Burning Analysis) campaign. This period comprised the transition between the end of the dry season, hereaer named intense biomass burning (BB) period, and the beginning of the wet season for that year (moderate BB period). Based on meteorological data, aerosol composition and optical properties, the date of 25 September was chosen to divide the measurements into distinct periods. An important parameter retrieved using the AMS/ACSM system is the fraction f 60 of the organic signal at m/z 60.
There is an excellent agreement between the AERONET and MODIS datasets, in spite of the different methods used in each AOD retrieval. A strong seasonal variation is evident at both regions. In the preserved central Amazonia, AOD reached up to 1. 0 in the dry season, whereas in the impacted southern Amazonia it reached very high values up to 5. 0 at 500 nm. These long-term time series plots give an overview of the variable aerosol loading in Amazonia, both from wet to dry seasons and also the large annual variability due to climatic conditions. It is possible to observe that aer the deforestation started to get reduced (see Fig. 1 ) AOD at the PVH site was reduced, but at the strong drought of 2010, smoke has increase signicantly compared to 2008 and 2009. Overall, the seasonal variability of the aerosol optical properties indicates that in the dry season biomass burning particle emissions overwhelm biogenic emissions, signicantly changing the physical properties of the natural aerosol population.