dataesr/scientific-paragraphs-categorization huggingface dataset:
Acknowledgements. INERIS is funded by the  French Ministry of Ecology, Sustainable Development and Energy. The EBAS database has largely been funded by the  CLRTAP-EMEP programme, AMAP  and  NILU  internal resources. Specific developments have been possible due to projects like EUSAAR (EBAS web interface),  EBAS-Online  (upgrading of database platform) and HTAP (import and export routines to build a secondary repository in support of www. htap. org. A large number of specific projects have supported development of data and metadata reporting schemes in dialog with data providers (CREATE, ACTRIS and others). Edited by: J. -L. Attie Reviewed by: two anonymous referees.
The sphericity was checked by the Mauchley test, and when it was not met, the significance of F-ratios was adjusted according to the Greenhouse-Geisser procedure or the Huyn-Feldt procedure. When significant differences were obtained, a Bonferroni post hoc test was conducted. To compare the G NMES and G UEPE PRs, the data after the intervention period were expressed in percentage of baseline values, and then analyzed from the general linear model with a two-way design (groups and severity). Significant differences were identified from the Bonferroni post hoc test. Statistical significance was set at P,0. 05 and all analyses were performed with the Statistical Package for the Social Sciences (release 18. 0; SPSS Inc. , Chicago, IL, USA).
Acknowledgments The authors would like to thank the rehabilitation team who managed the patients:  G Tywoniuk ,  S Duriez ,  F Urbain ,  V Wauquier , and  M Lambinet. The authors would also like to thank  Adair, France Oxygène, Homeperf, LVL Medical, Orkyn, Santélys, SOS Oxygène, Sysmed, VitalAire, and ARS Nord-Pas-de-Calais  for their support of the home-based  PR program.
Background: Significant advances in extracorporeal technology have led to the more widespread use of veno-arterial extracorporeal membrane oxygenation (VA ECMO) for cardiac failure. However, procedures for weaning from VA ECMO are not standardized. High death rate after successful weaning shows that many questions remain unresolved in this field. Objectives: In this review, we discuss data from the literature and propose a strategy to optimize the weaning process. Data synthesis and conclusions: It is especially important that the VA ECMO is not removed while the patient is still recovering from the condition that necessitated the use of VA ECMO implantation. Damaged organs need to recover before attempting weaning and the patient should be considered hemodynamically stable. The etiology of cardio-circulatory dysfunction must be compatible with myocardial recovery.
Luyt et al. examined whether biomarkers could predict cardiac recovery in patients receiving VA ECMO  [16]. They studied 41 consecutive patients with potentially reversible cardiogenic shock, and examined circulating concentrations of the N-terminal fragment of the B-type natriuretic peptide, troponin Ic, the midregional fragment of the proatrial natriuretic peptide, proadrenomedullin, and copeptin on days 1, 3, and 7 post-ECMO. There was no difference in the absolute values of these biomarkers or in their kinetics during the first week between patients who were weaned from ECMO and those who were not. Thus, the current data suggest that echocardiography is an important tool to determine both the recovery of LV function and the readiness of patients for weaning from ECMO support, whereas early measurements of cardiac biomarkers are not useful for identifying those who will recover  [17, 18].
DR1  in the GSA Data Repository 1  ). The orientation of the strain gauge bridge was chosen so that the bridge would record the net differential stress s 1 -s 3. The sample was then placed in a nitrile jacket equipped with 14 piezoelectric transducers. The geometry of the sensor array is shown in Fig-  ure DR1. The samples were placed into a triaxial deforma tion apparatus (e. g. ,  Brantut et al. , 2011). Stick-slip events were produced by imposing a constant shortening rate on the sample, equivalent to a net slip rate of 8 mm/s across the saw cut. The signals from the piezoelectric transducers were recorded, unamplified, with a 10 MHz digital oscilloscope. The signal from the strain gauge was amplified and recorded using two dedicated oscilloscope channels. The voltage measured from the amplified strain gauge was calibrated and converted into differential stress by matching the measured axial load during the elastic loading stage at the beginning of each experiment (prior to the onset of frictional sliding).
04 mm 2 /s) is the thermal diffusivity of antigorite  (Rempel and Weaver, 2008). The strength t c was estimated from the product of the friction coefficient and the constant normal stress given as a function of the Moh hardness H as 0. 123 × H 2. 3 GPa  (Beeler et al. , 2008). The friction coefficient involved in the computation of t c is a local one at the asperity contact; following  Bowden and Tabor (1964) , this local friction coefficient is considered equal to the macroscopic measured friction. Here, we used the average of the friction coefficients measured immediately prior to stick-slip events in all our experiments, which is 0. 86. Based on an average hardness H = 3. 75 for antigorite (cf. http://www. mindat. org database), the computed asperity shear stress is thus t c = 2. 2 GPa.
ACKNOWLEDGMENTS This work was supported by the  Natural Environment Research Council  (grant  NE/K009656/1  to Brantut) and the  Agence Nationale pour la Recherche  (project " DELF "  ANR-12-JS06-0003  to Schubnel). We thank  Takehiro Hirose ,  Hiroki Sone ,  Brooks Proctor , and  Greg Hirth  for their constructive review comments.
, 2012). The genotyping was performed at the Gentyane platform (INRA). Only the microsatellite markers and individuals with <50% missing data were used for the rest of the analyses. The data set was then composed of the genotypes for 30 microsatellite markers from 186 adult samples from Dourdan, 12 samples from the AFAF, 13 samples from commercial seeds, 442 from the Dourdan forest and orchard, and 167 seeds (including 99 seeds from the orchard and 68 nongerminated seeds) retrieved after the second experiment described above. We used the software Cervus  (Marshall, Slate, Kruuk, & Pemberton, 1998)  to check for identical genotypes in the adult tree data set.
We then regressed germination timing, growth rate and rate of increase in leaf number against the P dom of the seedlings. A mixed-model multiple linear regression analysis, with the mother tree's identity as a random blocking factor, was run to investigate effects of tree density and P dom of the parent trees on pollination distances. All of the statistical analyses were performed using the software JMP v7 (SAS Institute), using arcsine-transformed values for P dom and rates to improve normality. To check for a correlation between geographic distances between trees and similarity in their introgression levels, we calculated the difference in P dom for each pair of trees. We then used a Mantel test to compare the introgression difference matrix with that of the pairwise geographic distance using the R-package ncf  (Bjornstad, 2013).
ACKNOWLEDGEMENTS We declare no conflict of interest. We thank the  Région Ile de France (PICRI  and  DIM R2DS ),  IDEEV ,  and laboratoire d'Excellence BASC  for funding, and the  Plateforme de Génotypage GENTYANE INRA   UMR 1095 ,  Douae BenHDech  and  William Fontanaud , for assistance with genotyping and fitness measures. We thank those who helped with sampling, in particular  Didier Desseaux  (ONF). We also thank  Maud Tenaillon ,  Pierre Gladieux ,  Eric Collin ,  Stéphanie Le Prieur ,  Séverin Lavoyer  and  Charly Chauveau  for help during the project.
Observations and data reduction We observed HD 144432 on 2009 Apr 18 and 2010 Apr 18 with the VLTI/AMBER instrument (see Table  1 ). The AMBER instrument is a near-infrared beam combiner that records threebeam interferograms  (Petrov et al. 2007 ). The instrument was operated in the low spectral resolution mode (R=35) and recorded fringes in the H and K bands simultaneously. The fringe tracker FINITO was not used. The observations of HD 144432 were conducted using the linear baseline configuration E0-G0-H0 1 and the triangle configuration D0-H0-G1 of the 1. 8 m auxiliary telescopes (ATs). For data processing, we used the AMBER data reduction package amdlib 3. 0 2. We selected 30% of the target and calibrator frames with the highest fringe signal-to-noise-ratio (SNR) to improve the visibility SNR  (Tatulli et al.
b: χ 2 1,red maps of Model run A. For each subset of parameters, the χ 2 1,red shown is the lowest value for all combinations with other parameters. For example, for each pair of (R in , R out ) values, the χ 2 1,red values for all possible (h in , p h ) combinations within the described ranges were compared and the minimum value found is plotted into the map at left panel. c: The dust density distribution of the model, in units of g cm -3. d: K-(left) and N-band (right) model images A1, in units of erg cm -2 s -1 Hz -1. e: NIR and MIR visibilities, and closure phases CP (red dots: observations; black lines: model). The VLTI data are our own data. The data sets  2004 IOTA, 2003 KI, 2007 KI, and 2003 MIDI mentioned  in the panels are taken from  Monnier et al. (2006) ,  Monnier et al. (2005) ,  Eisner et al.
II. LIGO INTERFEROMETERS AND S6 SCIENCE RUN The LIGO gravitational wave network consists of two observatories, one in Hanford, Washington and the other in Livingston, Louisiana, separated by a 3000-km baseline. During the S6 run each site housed one suspended interferometer with 4-km long arms. Although the sixth science run spanned more than one year period of data acquisition, the analysis in this paper used data only from GPS 951534120 (2010 Mar 02 03:01:45 UTC) through GPS 971619922 (2010 Oct 20 14:25:07 UTC), selected for good strain sensitivity and noise stationarity. Since interferometers sporadically fall out of operation ("lose lock") due to environmental or instrumental disturbances or for scheduled maintenance periods, the data set is not contiguous. For the time span used in the search the Hanford interferometer H1 had a duty factor of 53%, while the Livingston interferometer L1 had a duty factor of 51%.
Only pulsars with galactic latitude less than 0. 06 rad are shown in the figure. We observe loose association with galactic arms, which is skewed by observational bias. In particular, the area searched by Parkes survey marked as a blue sector contains many more pulsars than elsewhere on the map. The expected reach of the all-sky search in S6 data, assuming a neutron star ellipticity of 10 -6 , is illustrated by the pink circle. A computationally feasible spotlight search can reach twice as far, but the globular clusters and galactic center remain out of its reach in the S6 data set. A closer alternative is to look in the local neighbourhood of the Sun along the Orion spur -a grouping of stars that connects the Perseus and Sagittarius arms of our galaxy. For this search we have chosen two regions (Table  I ), exploring two nearly opposite directions along the Orion spur.
IV. SEARCH ALGORITHM The results presented in this paper were obtained with the loosely coherent search, implemented as part of the PowerFlux program. We have used the follow-up procedure developed for the all-sky S6 search, but where the first loosely coherent stage is applied directly to the entire A and B regions. A detailed description of the loosely coherent code can be found in  [5, 16]. Mathematically, we transform the input data to the Solar System barycentric reference frame, correct for putative signal evolution given by frequency, spindown and polarization parameters, and then apply a low-pass filter which bandwidth determines the coherence length of the search. The total power in the computed time series is then compared to power obtained for nearby frequency bins in a 0. 25 Hz interval.
A signal-to-noise ratio and an upper limit are derived for each frequency bin using a universal statistic method  [25]  that establishes 95% CL upper limit for an arbitrary underlying noise distribution. If the noise is Gaussian distributed the upper limits are close to optimal values that would be produced with assumption of Gaussianity. The arc shown for the PARKES survey  [1]  shows search area, not the range. The green stars show locations of pulsars from the ATNF database (retrieved on January 29, 2015,  [22] ) with galactic latitude Gb below 0. 06 radians. The background image is due to R. Hurt  [24]  (color online) For non-Gaussian noise the upper limits are conservatively correct. Maxima of the SNR and upper limits over marginalized search parameters are presented in the plots 2, 3 and 4.
After transfer to nitrocellulose, membrane was blocking with 1% BSA, samples were probed with primary antibody followed by a horseradish peroxidase couple secondary antibody. Primary antibodies against LC3 was from Medical & Biological Laboratories (Nagoya, Japan) and antibody against VMP1 was homemade. 11 Polyclonal antibody against β-Tubulin was used as a loading control was from Sigma-Aldrich (St. Louis, MO). Image acquisition was made in Fusion FX image acquisition system (Vilber Lourmat) and bands were quantified ImageJ software (NIH). RT-qPCR. One μg RNA from pancreas was reversed transcribed using the Go Script reagent (Promega) according to manufacturer's instructions. Real-time quantitative PCR for VMP1 was performed in a Stratagene cycler using Takara reagents with the following primers sequences 5′-CTGGCAGTTCAAAAACTAGTAC-3′ and 5′-CCGGGG ACAGCACCAATGAAAG-3′ which recognize both human and mouse transcripts.
Acknowledgements. This work was supported by  La Ligue Contre le Cancer ,  INCa ,  Canceropole PACA ,  DGOS (labellisation SIRIC ) and INSERM to JLI,  National Institutes of Health  grants  DK52913  (RU), CA178627 (GL), the  Mayo Clinic Center for Cell Signaling in Gastroenterology  ( P30DK084567 ), and the  Mayo Foundation (RU).
Measurement of microwave emission from the solution Broadband radiothermometer (microwave analyzer) RTM-01 RES, operating in the 3. 4-4. 2 GHz range, was used as a microwave emission detector. For the measurements, flagpole antenna of microwave analyzer was fully immersed into the sample solution in the measuring cell. The antenna was not removed from the cell throughout the experiment. The addition of solutions into the cuvette and stirring were carried out using automatic pipette. The data on microwave emission measurements are presented using the brightness temperature (T SHF ) units, in which the radiothermometer is calibrated. The measurement accuracy was 70. 1 °С. The measurement data are presented as the T SHF vs time (T SHF (t)) dependence.
Acknowledgements We thank  Diamond Light Source  for the use of the I19 beamline under proposal MT8521. We acknowledge the  Synchrotron Light Source ANKA  for provision of instruments on the PDIFF beamline. We thank  Ms Alexandra Siakouli-Galanopoulou  and  Aleka Manousaki  for expert technical assistance with the SEM and FESEM operation and  Michael Su  ¨pfle for FT-IR measurements. Financial support in Heraklion from the  European Commission  ( FP7-REGPOT-2008-1 , Project  BIOSOLENUTI No. 229927 ) and Special Research Account from  University of Crete  is gratefully acknowledged. A. M. and E. G. acknowledge funding from the grant number  3941  ' PHOTOPEPMAT', ARISTEIA II Action , which is part of the action 'Education and  Lifelong Learning ' and is co-financed by the  European Union  (the  European Social Fund ) and national funds.
A. M. acknowledges support from ' AngioMatTrain', Marie Curie Industry Initial Training Network (ITN ), call  FP7-PEOPLE 2012-ITN , grant agreement number  317304. M. L. thanks  SERC (Swedish e-Science Research Center)  for funding and  SNIC  for providing computer resources. D. B. is a FNRS Research Director. H. K. and J. C. acknowledge support by the  DFG-Center for Functional Nanostructures (CFN). A. K. P. thanks the  Helmholtz STN  programme for funding. The work in Marseille was partially funded by the  FP7 Future and Emerging Technologies for Energy Efficiency project  ' PEPDIODE ', grant number  256672 , the  CNRS , the  Aix-Marseille University  through the A* MIDEX  project ' EtNA ' and the  Region Provence-Alpes Cote d'Azur through projects 'NanoMosaı ¨que' and 'CaliGraph'.
Data availability. Crystallographic data (excluding structure factors) for the structure in this paper have been deposited with the Cambridge Crystallographic Data Centre (CCDC), under deposition number CCDC 1415777. These data can be obtained free of charge from The Cambridge Crystallographic Data Centre via www. ccdc. cam. ac. uk/data_request/cif. All remaining data that support the findings of this study are available from the corresponding authors upon request.
OBSERVATIONS The observational data on which the present catalogue is based consists of a set of images of the L1495 cloud in the Taurus star-forming region, made as part of the HGBS 1  (André et al. 2010). The data were taken using PACS  (Poglitsch et al. 2010 ) at 70 µm and 160 µm and SPIRE  (Griffin et al. 2010 ) at 250 µm, 350 µm, and 500 µm in fast-scanning (60 ′′ s -1 ) parallel mode. The North-South scan direction for L1495 was split into two observations taken on 12 February 2010 and 7 August 2010, while the East-West cross-scan direction was observed in a single run on 8 August 2010. The corresponding Herschel Observation IDs are 1342202254, 1342190616, and 1342202090. An additional PACS observation (Observation ID 1342242047) was taken on 20 March 2012 in the orthogonal scan direction to fill a gap found in the previous PACS data.
Calibrated scan-map images at the PACS wavelengths 1 http://gouldbelt-herschel. cea. fr were produced in the HIPE Version 10 pipeline  (Ott 2010)  using Scanamorphos Version 20  (Roussel 2013). The SPIRE images were produced in the same pipeline using the "naive" map-making procedure and the destriper module. The arbitrary sky offset values were corrected by comparison with Planck and IRAS data using a procedure similar to that employed by  Bernard et al. (2010). The estimated offset values 2 for SPIRE correspond well to the ones determined from the zero-point correction task in HIPE. The spatial resolution values (FWHM beamsizes) of these maps are approximately 8. 5 ′′ , 13. 5 ′′ , 18. 2 ′′ , 24. 9 ′′ , and 36. 3 ′′ in the 70 µm, 160 µm, 250 µm, 350 µm, and 500 µm wavelength bands, respectively.
5 times the 70 µm beam size; (vii) source not spatially coincident with a known galaxy, based on comparison with the NASA Extragalactic Database (NED) or with a known young stellar object (YSO) based on the published list of Widefield Infrared Survey Explorer (WISE) detections  (Rebull et al. 2011) ; (viii) source appears real based on visual examination of the SPIRE images and column density maps. Imposition of the last criterion is facilitated by examination of the "summary card" for each source, included as one of the on-line catalogue products 4. It includes a cutout column density image of the source, upon which is superposed the elliptical 50% contour as estimated by getsources. To provide some additional confidence in the reality of the extracted source, the subimage is also superposed with a source ellipse estimated by an entirely different source extraction technique, namely the Cardiff Source-finding AlgoRithm (CSAR) discussed in Appendix B of  Kirk et al.
1) are more easily detectable than their prestellar counterparts due to their systematically higher temperatures. The simulated completeness for prestellar cores may be compared with the expected behaviour based on the model described by  Könyves et al. (2015) , indicated by the black dashed curve. present within its 50% column density contour. Their derived properties are more uncertain and their masses may be underestimated by a factor of ∼ 2. We detect 11 such objects in L1495. They are not considered further in the present work, but will be discussed in a forthcoming paper. The rightmost column of Table  B1  indicates matches with objects listed in the SIMBAD database and includes several previous surveys of dense cores. In most cases, those surveys were made at lower resolution and typically have blended the core either with neighbouring cores or with associated background filamentary structure.
ACKNOWLEDGMENTS We thank the referee for helpful comments. SPIRE has been developed by a consortium of institutes led by  Cardiff Univ. (UK)  and including:  Univ. Lethbridge (Canada) ;  NAOC (China) ;  CEA ,  LAM (France) ;  IFSI ,  Univ. Padua (Italy) ;  IAC (Spain) ;  Stockholm Observatory (Sweden) ;  Imperial College London ,  RAL ,  UCL-MSSL ,  UKATC ,  Univ. Sussex (UK) ; and  Caltech ,  JPL ,  NHSC ,  Univ. Colorado (USA). This development has been supported by national funding agencies:  CSA (Canada) ;  NAOC (China) ;  CEA ,  CNES ,  CNRS (France) ;  ASI (Italy) ; MCINN (Spain) ;  SNSB (Sweden) ;  STFC ,  UKSA (UK) ; and  NASA (USA). PACS has been developed by a consortium of institutes led by  MPE (Germany)  and including  UVIE (Austria) ;  KU Leuven, CSL, IMEC (Belgium) ;  CEA ,  LAM (France) ;  MPIA (Germany) ;  INAFIFSI/ OAA/OAP/OAT, LENS, SISSA (Italy) ;  IAC (Spain).
This development has been supported by the funding agencies  BMVIT (Austria) ,  ESA-PRODEX (Belgium) ,  CEA/CNES (France) ,  DLR (Germany) ,  ASI/INAF (Italy) , and  CICYT/MCYT (Spain). This work has received support from the  European Research Council  under the European Union's  Seventh Framework Programme  ( ERC Advanced Grant  Agreement no. 291294 , ' ORISTARS ') and from the  French National Research Agency  (Grant no. ANR-11-BS56-0010 -' STARFICH '). This research has made use of the SIMBAD database, operated at  CDS, Strasbourg, France. It has also made use of the NASA/IPAC Extragalactic Database (NED) which is operated by the  Jet Propulsion Laboratory, California Institute of Technology , under contract with the  National Aeronautics and Space Administration.
(2009)  using a 2-year data set. Although important conclusions and perspectives for the capability of IASI to sound HNO 3 were drawn from this study, the FORLI algorithm at that time only allowed for total column retrievals, and it was not possible to do a rigorous validation study due to the absence of archived data from ground-based FTIR measurements. Moreover, the total column retrieval combined with its maximum sensitivity in the stratosphere was shown to largely mask the potential of IASI to sound HNO 3 in lower layers. After this study, the Fast Optimal Retrieval on Layers for IASI (FORLI) software was adapted to allow retrieval of HNO 3 vertical profiles from IASI  (Hurtmans et al. , 2012). A full 8-year data set of global profiles is now available  (2008) (2009) (2010) (2011) (2012) (2013) (2014) (2015)  but has not yet been used for extensive analysis (a subset was used in  Cooper et al.
, 2014  to constrain lightning NO x emissions in models). The product characterization and validation are also still lacking. This paper uses a full year (2011) of HNO 3 profiles retrieved from IASI on Metop-A to do the following: fully characterize the HNO 3 retrieved concentrations in terms of vertical sensitivity and errors (Sect. 3) on the profiles and partial columns, validate the profiles and columns using correlative data from the NDACC FTIR network, which are also detailed here (Sects. 4 and 5), provide an overview of how the product can be used to analyse spatial and temporal variability (Sect. 6).