dataesr/scientific-paragraphs-categorization huggingface dataset:
Sub-mm/mm ALMA Data The ALMA data used to resolve the dipper discs in our sample come from both our targeted ALMA programme as well as archival ALMA programmes, as described below. Data calibration and imaging are performed using CASA; the data were pipeline calibrated by NRAO staff and include standard flux, phase, bandpass, and gain calibrations. The ALMA Project IDs of the data used for each dipper are given in Table  1. Our targeted ALMA programme to resolve dipper discs (Project ID: 2016. 1. 00336. S; PI: Ansdell) was a highresolution Band 6 (λ ≈ 1. 3 mm) survey of nine dippers conducted in Cycle 4 using the C40-7 configuration (21-3638 m baselines). The continuum spectral windows were centred on  233. 29, 220. 40, and 217. 47  GHz with bandwidths of 2. 00, 2. 00, and 1. 88 GHz, respectively.
2 (∼25 au) and continuum rms values of 0. 15 mJy beam -1. We also use data from selected archival ALMA programmes when they offered higher spatial resolution. Thus the data for EPIC 203850058, 204638512, and 204514548 come from ALMA programmes 2012. 1. 00046. S, 2017. 1. 01180. S, and 2013. 1. 00498. S with PIs Phan-Bao, Loomis, and Perez, respectively. Finally, although we do not perform model fits to these data in this work, four dippers in our sample (EPIC 203843911 or DoAr 25, EPIC 203860592 or WSB 52, EPIC 204281213 or HD 143006, and EPIC 204514548 or HD 142666) have higher resolution (∼5 au) ALMA observations taken as part of the Disc Substructures at High Angular Resolution Project (DSHARP;  Andrews et al. 2018). In Section 3. 2, we discuss these DSHARP data within the context of this work.
Adaptive Optics Imaging All but two of the dippers in our sample (EPIC 204142243 and 205345560) have been inspected for close companions with high-contrast imaging (see Table  2  and Table C1 ). Ten of these were observed and/or analyzed as part of this work using adaptive optics (AO) imaging with the Near-infraRed imaging Camera (NIRC2) mounted on the 10-m Keck II telescope atop Maunakea. For the sources we observed with NIRC2, those with R < 13. 5 used natural guide star AO  (Wizinowich et al. 2000; van Dam et al. 2004 ), while the fainter sources used laser guide star AO  (Wizinowich et al. 2006; van Dam et al. 2006). Imaging was done with the narrow camera and several sources also used non-redundant aperture masking (NRM). For the NIRC2 data reduction, each frame is linearized and corrected for geometric distortion using the solution from  Yelda et al.
The latter method is more physically motivated, but can be limiting for moderate signal-to-noise and/or marginally resolved discs, which are common in large-scale ALMA disc surveys. However, the former method is not appropriate for discs with large inner cavities (there are a few of these "transition discs" in our sample; see Figure  1 ) and also does not provide posterior distributions that are useful for our analysis of the disc inclination distribution (see Section 4. 1). Thus we (re)derive the disc inclinations for our entire sample using the GALARIO computational library  (Tazzari et al. 2018 ) combined with the emcee package (Foreman-Mackey et al. 2013), which allows us to quickly fit 2D disc models to the ALMA visibilities by enabling the rapid exploration of parameter space. GALARIO is a Python library that uses GPUs, or alternatively multiple CPU cores, to speed up the computation of synthetic visibilities.
Because of its modular structure, we can use GALARIO for the likelihood computation in emcee, a Python implementation of MCMC Ensemble sampling for Bayesian parameter estimation. We use the GPU version of GALARIO, which is ∼150× faster than standard Python implementations that rely on scipy and numpy packages. Tazzari et al. (2018)  provides a detailed explanation of employing GALARIO to fit interferometric visibilities like those from ALMA and we follow their general implementation procedure. The fits typically use 120 walkers and 5000 steps for the MCMC; the mean accepted fraction of steps are all between 0. 2 and 0. 5, implying that the chains are converging. Most of the dippers in our sample are single stars whose discs lack resolved structure (e. g. , no gaps or rings), thus we most often fit the visibilities using a simple 2D Gaussian disc model with six free parameters: a flux normalization term, the full-width-half-max along the semi-major axis, the inclination (i d ) and position angle (P.
A. d ) of the disc, and the offset in right ascension and declination of the source centre from the phase centre. For the two resolved binary discs in our sample (EPIC 203770559 and 203936815), we simultaneously fit two 2D Gaussians to the data. Four dippers  (EPIC 203950167, 204630363, 204638512, and 205238942 ) exhibit large inner cavities; for these, we use the aforementioned 2D Gaussian model, but with one more free parameter, an inner cutoff radius. EPIC 203843911 and EPIC 204281213 exhibit more complex features in the data that our simple models could not account for (i. e. , narrow gaps/rings and azimuthal asymmetries, respectively; see Figure  1 ). However, in both cases our inclinations agree well with those derived by  Huang et al. (2018)  from the extremely high resolution DSHARP observations of these objects.
For all sources in our sample with high-contrast imaging, detection limits as a function of separation from the primary, when available, are given in Table  C1. Moreover, we can use information from the Gaia Data Release 2 (DR2) as an independent check of binarity and also to assess the likeliness of any candidate companions being physically bound. The latter could be of interest when interpreting the dipper phenomenon and has implications as to whether the potential contaminants remain blended in the K2 light curves taken at different epochs. The imaged candidate companions to four of the dippers in our sample  (EPIC 203843911, 204211116, 204489514, 205238942)  are sufficiently separated and/or faint that they may be older background objects (e. g. , see discussion in  Barenfeld et al. 2019 ) and indeed we do not detect discs at the locations of their candidate companions in our ALMA data.
We build the ECDF by randomly sampling from the inclination posterior distributions inferred with GALARIO for each dipper, converting these to cos(i d ), then applying the ECDF package in the STATSMODEL Python module. We then repeat this 1000 times and take the mean and standard deviation as the final values and associated uncertainties of the ECDF. The result is shown in Figure  4  and compared to the isotropic case, constructed by randomly sampling from a uniform distribution between 0. 26 and 1. 0 for cos(i d ) (corresponding to 0 < i d < 75 • due to the observational bias discussed above) for each dipper in our sample (i. e. , the sample sizes are the same). The distributions clearly overlap, demonstrating that the dipper disc inclination distribution is consistent with isotropic. The average and standard deviation of the p-values of two-sided Kolmogorov-Smirnov tests, calculated for each of the 1000 draws and only considering cos(i d )> 0.
Dippers with Resolved Discs Disc inclinations in degrees: i d,lit are disc inclinations derived from ALMA data in the literature (references given in the Ref. i d,lit column); i d are the disc inclinations uniformly (re-)derived in this work using GALARIO to fit the ALMA datasets (Project IDs given in the ALMA ID column). The disc inclinations from C18 and C17 are calculated from the measured semi-major and semi-minor axes reported in those works, while those from H18 are their 2D Gaussian fits. c Position angle in degrees, measured positive East of North. We do not provide P. A. values for EPIC 203937317 or EPIC 204281213; the former was unconstrained by our fit due to its face-on geometry and the latter was unreliable due to the disc asymmetry. d EPIC 204281213 and 204514548 are listed under alternative K2 IDs ofEPIC 204281210 and 204514546, respectively, in.
ACKNOWLEDGEMENTS MA gratefully acknowledges the  NVIDIA Corporation  for donating the Quadro P6000 GPU used for this research. MA acknowledges support from  NSF  grant  AST-1518332  and  NASA  grants  NNX15AC89G  and  NNH18ZDA001N/EW. MA, GD, and IA acknowledge support from  NASA  grant  NNX15AD95G/NEXSS. MT is supported by the  UK Science and Technology research Council (STFC). JC acknowledges support from the  National Aeronautics and Space Administration  under grant No. 15XRP15 20140  issued through the  Exoplanets Research programme. GMK is supported by the  Royal Society as a Royal Society University Research Fellow. We thank  Scott Barenfeld  and  Lucas Cieza  for providing the calibrated ALMA visibilities of their disc survey programmes. Part of this research was carried out at the  Jet Propulsion Laboratory, Caltech , under a contract with  NASA.
Assumptions, corpus and methodology Our study is based on data provided by Linkfluence 3  , as part of an ANR project "Algopol: Algorithmic Policy" 4. Linkfluence has gathered around a hundred sites, taking into account citation links between these sites on one side and sites on the far right on another. This collection of sites is made on the basis of the principle of transitivity in sociology of social networks "the friends of my friends are my friends"  (HEIDER, 1946 , quoted by MERCKLÉ, 2004, p. 63-64). Linkfluence's study of the outgoing and incoming quotation links of the re-information sphere shows that the re-information sites are essentially pointing to themselves and to the political blogosphere of the far right. However, their relationship of affinity or "friendship" does not, in our opinion, constitute a reason for considering them a body of study.
Methods A modified Delphi procedure was used to develop consensus statements, if possible based on evidence, otherwise on experts' opinions, experience and intuitive judgement, as the Delphi method acknowledges the importance of this relatively subjective data in the absence of hard scientific data  [20]. The steering committee (NO, SJ, FAW and GK) was formed by the principal researcher (FAW) and the process was supervised by a clinical epidemiologist (JvL). Ten spinal orthopedic surgeons (SB, MC, RC, DE, CG, VK, MK, WM, NO, and KW), 6 pediatricians (NG, PvH, SJ, PO, RP, FW) and 3 physiotherapists (PH, ESH and AR), all experienced in the treatment and follow-up of patients with MPS I, were invited to participate in this modified Delphi procedure. To initiate the procedure a literature review was conducted by one of the researchers (GK) to evaluate the current evidence for the benefit of kyphosis surgery in MPS I (all phenotypes).
The CPP1 crystals loaded with DOX were tested for monitoring the cumulative drug release over a period of 48 h by UV-VIS spectrometer (Perkin Elmer, LAMBDA 950) measurement of the incubation solution (as per the loading measurements for the chloramphenicol. The assynthesized and drug loaded materials used in the present work are summarised in Table  1. The crystal structure and purity of the synthesized mineral phases were analysed by X-Ray powder diffraction using a Philips X'Pert MPD, with monochromatic Cu Kα radiation (0. 1541 nm). For the X-Ray measurements, the step size was 0. 065°and the 2θ scanning range was from 10°to 65°. The data were collected over a period of approximately 25 min with a scan speed of 0. 014°s -1. Scanning electron microscopy (SEM, a Hitachi SU8230 1-30 kV cold field emission gun) was used to investigate the size and shape of the powder crystals and to verify pore formation.
Acknowledgments The authors acknowledge the sponsors of this work, i) the  EU-Marie-Curie-IF PRe-FActo  ( 660147-Recipient A. D. Anastasiou) and ii) Medical Technologies Innovation and Knowledge Centre  (phase 2 -Regenerative Devices), funded by the  EPSRC  under grant number  EP/N00941X/1. Also authors would like to acknowledge  Dr. K. Triantafillidis  for his kind contribution to the gas adsorption porosimetry experiments. Finally authors would like to acknowledge  Mr. John Harrington  and  Mr. Stuart Micklethwaite  for SEM support. The authors declare that they have no conflict of interest.
Contact Angle Measurements For the static contact angle measurements, 3 μL of distilled water (ρ = 18. 2 MΩ•cm) was dropped on the air side surface of the PTFE membrane at room temperature, and the contact angle was measured after 10 sec. The given values correspond the average ± one standard deviation over n = 3 measurements. A OneAttension goniometer fitted with the OneAttension 3. 1 software and image acquisition software was used for those measurements (Biolin Scientific).
Electron Microscopy Sample processing e-PTFE samples after cell culture were fixed in 4% glutaraldehyde and 1% paraformaldehyde buffered in sodium cacodylate 0. 1 M at pH = 7. 4. After 3 washes of 10 min in the same buffer, the samples were post-fixed with 1% osmic acid in a 0. 1 M sodium cacodylate solution for 45 min. These chemicals were purchased from Euromedex (Souffelweyersheim, France). Then, the samples were dehydrated in graded series of ethanol for 10 min each. In order to increase resin im- were carried out at constant approach and withdrawal velocities. To characterize the micro-scale stiffness of the samples, the recorded force curves were processed using the commercial NanoScope Analysis software (Bruker Corporation, Santa Barbara, CA USA), which offers a full suite of force curve analysis tools.
In this paper, we complement this study by targeting a dust-lane ETG in the Fornax Cluster: FCC 167 (NGC 1380). It is one of the few dust-lane ETGs with MUSE data available, and contains only a circumnuclear ISM, making it more comparable to the majority of the gas-rich ETG population  (Young et al. 2011; Davis et al. 2013). The dust in FCC 167 could therefore be quite different from the large-scale dust lane observed in NGC 5626. The additional advantage of IFU observations is that the morphology and kinematics of the ionised gas can be studied simultaneously. The total flux of the ionised gas highlights its projected morphology, while the kinematic moment maps reveal its dynamics. This offers an insight in the 3D distribution of the ISM. The ionised gas may be diffuse or located in photodissociation regions (PDRs) around new stars.
This in turn is informed by an accurate and spatially resolved measurement for the attenuation curve and by the ionised-gas kinematics. While answering this question, we also hope to better understand the origin of the ISM within FCC 167. The observations and data analysed here are discussed in Sect. 2. In Sect. 3 we outline our measurements of the attenuation in the dust lane and we discuss other ISM tracers in 4. Radiative transfer modeling of the central regions of FCC 167 is presented in Sect. 5 before a more general discussion in Sect. 6. Finally, we formulate our conclusions in Sect. 7.
Observations and Data FCC 167 (α J2000 = 03 h 36 m 27. 55 s , δ J2000 = -34 For more information on the observing strategy and data reduction process, we refer to the F3D survey paper  (Sarzi et al. 2018). We measure a full width half maximum (FWHM) of 4 MUSE pixels or 0. 8 arcsec for the instrument point spread function (PSF), corresponding to a physical resolution of 70 pc. During this investigation, we also made use of several ancillary observations of FCC 167 (see Sect. 4 and 5). To estimate the structure and content of molecular gas we rely on ALMA observations from the ALMA Fornax Cluster Survey (PI: T. Davis). They map the CO(1-0) transition in the galaxy. For details of the survey including moment maps we refer to  Zabel et al. (2018). To constrain the dust heating by hot gas electrons and the associated dust survival timescale we investigate archival X-ray data from the Chandra X-ray Observatory.
Finally, our panchromatic radiative transfer models predict the emission in the FIR and submm wavelength regime. To estimate the energy balance in the galaxy and the dust heating mechanisms, we compare the model SED to fluxes from the Herschel space telescope  (Pilbratt et al. 2010 ). These fluxes were measured from the PACS  (Poglitsch et al. 2010)  and SPIRE  (Griffin et al. 2010 ) images provided by the DustPedia  (Davies et al. 2017)  database. We performed our own aperture photometry using the Python photutils package  (Bradley et al. 2018)  to match the MUSE field-of-view and adequately compare the model and observed fluxes.
5  (middle and right panels). The molecular gas exhibits regular rotation, with line-ofsight rotational velocities up to 250 km s -1. Typical line widths are between 40-160 km s -1 with the highest values in the center due to beam smearing. We constructed a dynamical model for the molecular gas again using KinMS  (Davis et al. 2013). The output of KinMS is a three-dimensional RA-Dec-velocity data cube, that can be compared directly with the ALMA data cube. We use Markov chain Monte Carlo (MCMC) methods, in particular the adamet Python package of  Cappellari et al. (2013) , which implements the Adaptive Metropolis algorithm of  Haario et al. (2001) , to constrain the morphology of the molecular gas in the centre of the galaxy. Both exponential disks and ring morphologies were fitted to the data, only a ring-shaped model results in a good fit.
Acknowledgements. S. V. is supported by the  UGent-BOF  fund and the UHerts visitor fund. E. M. C. and L. M. acknowledge financial support from  Padua University  through grants  DOR1699945/16 ,  DOR1715817/17 ,  DOR1885254/18 , and  BIRD164402/16. GvdV acknowledges funding from the  European Research Council (ERC)  under the European Union's  Horizon 2020 research and innovation programme  under grant agreement No  724857  ( Consolidator Grant ArcheoDyn ). We thank  Anthony Jones  for several stimulating discussions. Based on observations collected at the  European Organisation for Astronomical Research in the Southern Hemisphere  under  ESO  programme  296. B-5054 (A). This research has made use of data obtained from the  Chandra Data Archive. This paper makes use of the following ALMA data: ADS/JAO.
Statistical analysis For part A to D, the insect count (i. e. , presence or absence) in each area have been modelled using a logistic regression under a quasi-binomial distribution assumption. Binary choices between areas for one replicate have been analyzed using z-tests. For part E, a dendrogram based on a hierarchical clustering approach was created to qualify the differences between replications (experiments with a ratio of 20/40). Finally, Mann-Whitney test has been used to compare mean temperature selection to the one reported in Aubernon et al. ,  [20]. Logistic regression and hierarchical clustering have been performed using R software v. 3. 3. 2 (R development Core Team). Z and Mann-Whitney tests were performed using XLStat (XLStat, Addinsoft, Paris, France, 2016).
Two Heavy Neutral Leptons We close this section by discussing the possibility of having more than one HNL in our region of interest. In general, the 3+1 model already captures most of the collider implications of the existence of a HNL. Nevertheless, in seesaw-like models at least two heavy neutrinos are needed in order to accommodate neutrino oscillation data and, consequently, some remarks should be made in this latter case with two HNL, which we effectively describe by a 3+2 model. Under the lack of a positive experimental signal, one might consider the possibility of reinterpreting the bounds on the 3+1 model in terms of the 3+2 parameters. The production cross section in the 3+2 would be the sum 4  of the 2 HNL contributions and, if they do not have a large separation in mass, one can set bounds on the sum |V N 1 | 2 + |V N 2 | 2.
Acknowledgments The authors would like to thank  Nishita Desai ,  Claudia García-García ,  Deywis Moreno ,  Richard Ruiz  and  Jakub Scholtz  for fruitful discussions. We acknowledge partial support from the  European Union   Horizon 2020 research and innovation programme  under the  Marie Sk lodowska-Curie :  RISE InvisiblesPlus  (grant agreement No  690575 ) and the  ITN Elusives  (grant agreement No  674896 ). NB and ML are also supported by the  Universidad Antonio Nariño  grants  2017239  and  2018204. NB was also partially supported by the  Spanish MINECO  under Grant  FPA2017-84543-P. ML thanks  LPT-Orsay  and  CEA-Saclay  for hospitality during the completion of this work. In addition to the software packages cited above, this research made use of IPython [80], Matplotlib [81], SciPy [82] and python-ternary [83].
Conversely in Scandinavian countries as well as in the UK the management of sarcoma patients must be carried out in dedicated reference centers  [9, 22]. It is also recommended that patients with a suspected diagnosis of sarcoma should be referred at a sarcoma center before any treatment in international Clinical Practice Guidelines  [5] [6] [7] [8]. The French National Cancer Institute (INCa) funded a clinical network for sarcoma (called NETSARC) in 2009, to improve the management and outcome of sarcoma patients. Twenty-six reference centers throughout the nation were identified. A Network for expert pathology diagnosis in sarcoma (RRePS) gathering 23 reference centers for pathology in charge of the second histological review for each suspected case was also created. A common database (netsarc.
org) gathering all cases of sarcoma presented to MDTB was created and implemented, collected data on the diagnostic, therapeutic management, and the clinical outcome in terms of relapse and survival. From 1 January 2010 to 1 May 2018, this database prospectively included a 47 023 patient population with 35 784 patients with sarcoma or tumor of intermediate malignancy. 11 239 (24%) patients in the database discussed in a NETSARC MDTB had a diagnosis which was not that of a sarcoma (benign tumor, e. g. lipoma, carcinoma, lymphoma, etc. ). The aim of the present study was to evaluate (i) the impact of predisposing conditions and patient history and (ii) the impact of surgery carried out in a NETSARC reference center on relapse and survival in the population of patients included in the NETSARC database.
The network Each NETSARC center organizes an MDTB gathering sarcoma specialized pathologist(s), radiologist(s), surgeon(s), radiation oncologist(s), medical oncologist(s), and often molecular biologist(s), orthopedist(s), and pediatrician(s). All sarcoma or suspected sarcoma patient cases presented to the MDTB of all 26 centers were recorded in the database, by a dedicated team of Clinical research assistant, supervised by three coordinating centers (Centre Leon Berard, Gustave Roussy, Institut Bergonie). Patient files may be presented before any diagnostic procedure, before initial biopsy, before primary surgery, after primary surgery, at relapse, and/or in case of a possible inclusion in a clinical trial. Patients and treatment data were prospectively included and regularly updated by the dedicated study coordinators.
The NETSARC database The NETSARC database allows (i) to exhaustively describe the incident and prevalent population of sarcoma patients in France, by cross comparison of the pathological review database (rreps. org) and of the clinical database (netsarc. org), (ii) to monitor the diagnostic and initial treatment procedures, and (iii) to monitor patient outcome in particular survival and relapse. The database includes a limited set of data, on purpose, describing patients and tumor characteristics, surgery, relapse, and survival  [12]. The center which carried out the first resection is documented, as well as potential secondary surgery, and the final quality of resection after all surgical procedures. The surgical resection system (R) from the Union Internationale contre le Cancer was chosen to define the quality of surgery, including the margins of resection.