dataesr/scientific-paragraphs-categorization huggingface dataset:
05. Before developing the multivariable prognostic models, we examined the log-linearity assumption for continuous characteristics using restricted cubic spline functions as well as the absence of collinearity between candidate predictors by calculating the variance inflation factors. To avoid case deletion in analyses due to missing data on baseline characteristics and outcomes, we imputed missing data by multiple imputations using a regression-switching approach (chained equations with m ϭ 10). The imputation procedure was performed under the missing at random assumption using all baseline characteristics and study outcomes with a predictive mean matching method for continuous variables and a multinomial or binary logistic regression model for categoric variables. Estimates obtained in the different imputed datasets were combined using the Rubin rules.
Predictors of 90-Day Favorable Outcome Center-adjusted analyses of predictors of favorable outcome are detailed in On-line Table  3. In backward stepwise multivariable regression analysis, age, admission NIHSS score, hypertension, time intervals between onset to imaging and imaging to groin puncture, prestroke mRSՆ1, general anesthesia, and non-M1 MCA occlusion were associated with a decrease in the favorable outcome rate, whereas intravenous thrombolysis was associated with an increase (Table  3 ). This prognosis model had good discrimination (median C-statistic, 0. 827; range, 0. 816 -0. 838 across imputed datasets).
Predictors of Successful and Complete Reperfusion Center-adjusted analyses of predictors of successful and excellent reperfusion outcome are detailed in On-line Tables  4  and 5. A higher ASPECTS (OR per 1-point increase, 1. 25; 95% CI, 1. 08 -1. 45) and no current smoking (OR, 0. 36; 95% CI, 0. 18 -0. 72) were independently associated with successful reperfusion in backward stepwise multivariate regression analysis (Table  3 ). This prognosis model had good discrimination (median C-statistic, 0. 681; range, 0. 672-0. 688 across imputed datasets). For excellent reperfusion, we identified 5 independent predictors: older age, previous antiplatelet medications, lower blood glucose, site of occlusion (with a greater rate of excellent reperfusion for MCA M1 and vertebrobasilar occlusions), and Sofia 6F catheters (Table  3 ).
Predictors of First-Pass Effect (mTICI 3 after 1 Pass) Center-adjusted analyses of predictors of FPE are detailed in Online Table  6. We identified 3 independent predictors: older age, site of occlusion (with a greater rate of excellent reperfusion after 1 pass for MCA M1 and verterbobasilar occlusions), and intravenous thrombolysis (Table  3 ). This prognosis model also showed good discrimination (median C-statistic, 0. 795; range, 0. 793-0. 795 across imputed datasets).
Participant selection The target population for hrHPV testing were women who were Romanian nationals, including women who self-identify as Romanian, Roma, Slovakian, Ukrainian, or Russians, and women from urban and rural remote areas (Figure  1 ). Women were contacted by their family doctors. To achieve high participation rate among ethnic minorities, information campaigns were conducted in rural and urban settlements with the aid of official staff members from the local mayor's offices. Roma from isolated communities were contacted by Roma community leaders specially trained in health promotion and in communication with the general Romanian health sector. Women agreeing to participate were questioned and examined by a single medical physician via face-to-face interview. From July 2015 to April 2017, data was collected on age, self-declared ethnicity, history of prior screening (yes or no), prior history of hysterectomy, and living area (urban [city] or rural).
Women who received a positive HPV test and abnormal cytology in this study are undergoing clinical follow-up for screening and/or colposcopy and biopsy. Precancer and cancer outcome data are being collected and will be assessed in future studies. Stratification by HPV and cervical cytology screening result are necessary to assess cervical cancer risk, and will be done to determine the optimal approach to define Romanian cervical cancer screening guidelines. The WHO recommends routine vaccination of girls 9-13 years old  [41]. In an ethnically diverse country like Romania, where large proportions of the population live in closed communities or areas with limited access to health services, an outreach delivery strategy may be appropriate to ensure equitable vaccination opportunities for all adolescent girls.
Acknowledgements This study was conducted as part of the  CEDICROM  project with the aim to conduct a hrHPV primary cervical screening in Romania, funded through the  European Economic Area (EEA)  grant under Project Contract number  10988/10. 12. 2014. We thank  Andreea Itu  and  Bianca Nicula  from the  Oncology Institute "Prof. Dr. Ion Chiricuta" of Cluj-Napoca ,  Romania  and  Allini Mafra  from the  Cancer Registry of Norway  for making this study possible.
Fractions containing protein after elution with 300 mM imidazole were concentrated and further purified by SEC using a Superdex 75 Hiload 16 60 column in 15 mM HEPES, pH 7. 4 and 150 mM NaCl and concentrated to 10 mg/mL. Isothermal titration calorimetry. Isothermal titration calorimetry (ITC) was performed using a MicroCal Auto ITC200 (Malvern Instruments Ltd). A 10 µM solution of LRP6 P3E3P4E4 in DPBS was placed into the 200 μL sample cell at 25 °C. Titration was performed with 2 µL injections (first injection 0. 5 µL) of VHHs in DPBS at a concentration of 100 µM every 120 s (26 injections total). Data were fitted using the MicroCal PEAQ-ITC Analysis Software (Malvern Instruments Ltd) according to standard procedures. Fitted data yielded the stoichiometry (n), the dissociation constant (kD), enthalpy (H) and entropy (S).
Each ligand test was performed in triplicate and values for n, kD, H and S represent mean ± s. d. of three independent experiments. QCM data collection and analysis. Quartz crystal microbalance (QCM) technology was used to analyze the affinities of the VHHs towards LRP6. The experiments were performed using an Attana A200 C-Fast system (Attana AB). LRP6 P3E3P4E4 was immobilized on a low-non-specific binding chip (LNB) via amine coupling according to the manufacturer's protocol. Two sensor chips were docked in the instrument and the temperature was set to 22 °C. HBS-T was passed over the surfaces at a flow rate of 100 µL/min until the baseline was stabilized (frequency change ≤ 0. 2 Hz over 600 s). After reduction of the flow rate to 10 µL/ min, a freshly prepared activation solution (0. 2 M 1-ethyl-3-(3-dimethylaminopropyl)-carbodiimide, 0.
After each cycle the surface was regenerated with an 84 s pulse of 10 mM glycine, pH 3. 5. All VHHs were injected in duplicate in two independent experiments. Data were collected using Attester software (Attana AB) and analyzed with Evaluation software (Attana AB) and Clamp XP (University of Utah). The signal obtained from the reference surface was subtracted from the sensograms obtained for the LRP6 P3E3P4E4immobilized surface. To calculate the kinetic parameters (k a and k d ) and affinity constant (K D ), the experimental data were fitted using a homogeneous ligand model (1:1 fitting model). Crystallization of LRP6-VHH complexes. Purified LRP6 P3E3P4E4 was mixed with purified L-P2-B10 (C-terminal His 6 -tag) or VHH L-P2-D07 (C-terminal V5-FLAG 3 -His 6 -tag), respectively in a 1:1. 05 receptor:VHH ratio and incubated for 2-4 h at 4 °C.
X-ray crystallography data collection and complex refinement. LRP6 P3E3P4E4 -L-P2-B10 crystals were collected by helical collection and diffracted to 2. 6 Å resolution at beamline ID 23-2 at European Synchrotron Radiation facility (ESRF Grenoble, France). X-ray diffraction data for complex LRP6 P3E3P4E4 -L-P2-D07 was collected at beamline ID29 at ESRF and diffracted to 2. 9 Å resolution, see Table  1. X-ray diffraction data for both complexes were integrated with DIALS  69  and scaled using Aimless 70 in the CCP4 suite  71. Data processing statistics are shown in Table  1. Phasing of both datasets was performed by molecular replacement using program PHASER  72  , by previously solved structures of LRP6 (PDB ID: 4A0P  41  ) and VHH framework without CDRs (PDB ID: 4KRN  73  ) as search models.
Acknowledgements We thank members of the laboratory of M. M. M. for experimental support, helpful discussions and suggestions. We thank the  European Synchrotron Radiation Facility (ESRF)  for the provision of synchrotron radiation facilities; and beamline scientists of the  ESRF  for assistance. We thank  U-protein Express  for the provision of protein expression facilities. We thank  Guangyun Yu  and  Ronald Pieters  ( Utrecht University, Department of Pharmaceutical sciences -Molecular Pharmacy, The Netherlands ), for providing access to the MicroCal Auto ITC200. This work is part of the  Oncode Institute , which is partly financed by the  Dutch Cancer Society. This work was supported by  European Research Council   Starting Grant   242958 , the  Netherlands Organization for Scientific Research NWO   VICI Grant   91815604 ,  ECHO Grant 711.
Conclusion and Future Work This paper presents our current research towards a multi-UAV and human interaction driving system that would exploit human's mental state estimation. The main idea is to integrate the latest advances of physiological computing into a high-level mission coordinator. State-of-the-art approaches were presented as well as promising physiological markers. A mission scenario was also proposed, in which a human pilot should coordinate his actions along with UAVs' requests (MUM-T). In this scenario, four conditions would be evaluated in order to study the variations of engagement of human pilot. In particular, such conditions would constitute labels to the collected data therefore allowing the design of the subsequent smart estimation system. The next step of this work is to define the experimental protocol of the proposed mission scenario in details, to implement a rigorous experimental setup, hence ensuring the validity of the expected results.
Source regions of X-type NEAs For our study we extract asteroid information from the Minor Planet Physical Properties Catalogue (mp3c. oca. eu), developed and hosted at Observatoire de la Côte d'Azur. This database contains orbits and physical properties of both MBAs and NEAs. Especially, for NEAs it also includes albedo and spectral classes obtained from the Data Base of Physical and Dynamical Properties of Near Earth Asteroid of the E. A. R. N. (European Asteroid Research Node) hosted by the DLR Berlin (http://earn. dlr. de). We select NEAs of the X, Xk, Xc, Xe, E, M, P-types according to Tholen  (Tholen & Barucci 1989) , Bus  (Bus & Binzel 2002)  and  Bus-DeMeo (DeMeo et al. 2009)  taxonomies. As a second filter we require their geometric visible albedo (p V ) to be in the range 0. 1 < p V < 0.
Selection of asteroids We restrict our search for the intermediate albedo component of the X-complex (see Fig. 1 ) and thus we select all asteroids of the inner Main Belt (with 2. 1 < a < 2. 5 au) with 0. 1 ≤ p V ≤ 0. 3 belonging to the X-complex, having spectral taxonomic classes of X, Xc, Xe, Xk, Xt, M, E, as described in section 2. We also check for  Tholen & Barucci (1989)  P-types in the IMB, which could have a revised p V > 0. 1, finding no such cases. This selection resulted in a pool of 386 asteroids. We use the database of  Delbo et al. (2017) , which can now be accessed from the mp3. oca. eu (see section 3) to perform these extractions. The database is used to extract proper orbital elements and diameter values for the selected asteroids on which we apply the family searching technique.
In this database, all known asteroids as of 2016 November 4 from the Minor Planet Center (https://www. minorplanetcenter. net, downloaded Nov 2016) are crossmatched with (i) the synthetic and analytic (for those asteroids without synthetic) proper elements  Milani et al. (2014)  of the AstDys-2 database (http: //hamilton. dm. unipi. it/astdys/); (ii) radiometric diameters and albedos taken from  Nugent et al. (2016 Nugent et al. ( , 2015)) ;  Masiero et al. (2012a) ;  Tedesco et al. (2002) ;  Ryan & Woodward (2010) ;  Usui et al. (2011) ;  Masiero et al. (2011 Masiero et al. ( , 2014) )  combined in reverse order of preference (i. e. results from a following-cited reference overwrite those of a preceding-cited one, in order to have a unique diameter and albedo value for each asteroid); (iii) spectral classification from several sources Neese (2010);  Carvano et al.
As discussed in section 6, we define as planetesimals those asteroids that cannot be included into V-shapes. Gaia Data Release 3 in 2021, will contain asteroid spectra and should help to further constrain family membership. Fourteen core members of the Athor family -asteroids numbered  2419, 11977, 12425, 17710, 21612, 30141, 30814, 33514, 34545, 42432, 43739, 54169, 68996 , 80599 -and seven members of the halo of Athor family -1697 2346 3865 8069 29750 42016 79780 -were also linked by  Nesvorný et al. (2015)  to the family of the asteroid (4) Vesta. None of these asteroids is classified as V-type, which would be expected given the composition of (4) Vesta and its family. The geometric visible albedo distribution of these asteroids has a mean value of 0. 18 and standard deviation of 0. 04, while that of the Vesta family has a mean value of 0.
35 and standard deviation of 0. 11. The albedo values and spectra or spectrophotometric data of these asteroids are thus incompatible with those of the Vesta family, making them very likely interlopers that are linked to (4) Vesta by the HCM because of their orbital element proximity. While the V-shape family identification is quite robust against including interlopers, in particular because we apply it on compositionally similar asteroids, the presence of interlopers are still possible. In our case, interlopers are mostly the results of uncertainties in the albedo and spectral identification. We estimated the effect of albedo uncertainty on the selection of asteroids following the Monte Carlo method described in section 4. 2. We find the number of asteroids selected by the criterion 0. 1 ≤ p V ≤ 0.
Fig. 6. Cumulative size distribution of planetesimals. This is the cumulative size distribution of those asteroids that are outside V-shapes and thus probably do not belong to a family. Additionally, in this dataset, are included the parent bodies of families, as originally they belonged to the planetesimal population. The distribution is then corrected for the maximum number of objects that were lost, due to the collisional and dynamical evolution, in order to obtain an upper limit for the distribution of the planetesimals (open squares). Functions of the form ) N(> D) = N 0 D β , Proper semimajor axis (au) X-types (0. 1 < p V < 0. 3) Athor family V-shape Baptistina family V-shape Zita family V-shape   , 757, 1697, 1998, 2194 3007, 3665, 3704 3865, 4353, 4548, 4889, and 4845. The average reflectance spectra of the Xe, Xc, Xk, and C of the DeMeo et al.
Acknowledgements. The work of C. A. was supported by the  French National Research Agency  under the project " Investissements d'Avenir" UCA JEDI  with the reference number  ANR-15-IDEX-01. M. D. acknowledges support from the  French National Program of Planetology (PNP). This work was also partially supported by the  ANR   ORIGINS  ( ANR-18-CE31-0014 ). Here we made use of asteroid physical properties data from https://mp3c. oca. eu/, Observatoire de la Côte d'Azur , which database is also mirrored at https://www. cosmos. esa. int/web/astphys. We thank  Bojan Novakovic  for his thorough review.
1. INTRODUCTION AU Mic is a nearby  (9. 8 pc; Gaia Collaboration et al. 2018) , M1Ve star that is a member of the 23±3 Myr old β Pic moving group  (Mamajek & Bell 2014). Since the discovery and early observations of the spatially resolved, edgeon debris disk associated with the system  (Kalas et al. 2004; Liu 2004 ) that is gas poor  (Roberge et al. 2005) , subsequent high contrast imaging has probed the structure of disk in scattered light from projected stellocentric radii of 10 au  (Wang et al. 2015)  to 210 au  (Schneider et al. 2014) , as well as distances in between  (Metchev et al. 2005; Krist et al. 2005; Graham et al. 2007; Fitzgerald et al. 2007; Boccaletti et al. 2015 Boccaletti et al. , 2018)). Along with longer wavelength mm observations, these data suggest the general architecture of AU Mic's debris system might be similar to the asteroid belt and Kuiper Belt in our own Solar System.
g. Wood et al. 2005). Sezestre et al. (2017)  note that these dramatically different mass-loss rates have profound impacts on the grain blowout sizes that would be in operation. In this paper, we present new white-light optical coronagraphic imagery of the inner region of AU Mic's disk obtained with the Hubble Space Telescope Imaging Spectrograph (HST/STIS) in 2018 using the BAR5 occulter. We describe the acquisition and reduction of these data in Section 2. We highlight the new morphologies of AU Mic's disk revealed by these data, including dramatic apparent loop-like structures seen in projection, in Section 3. We explore some of the potential mechanisms that could create these morphological features in the context of preliminary analysis of new constraints on the star's activity as enabled by NASA/TESS data in Section 4.
Within each orbit, 20-21 images of 16. 6 second duration were obtained at each of three cross-BAR5 dither positions offset by (-1/4, 0, +1/4) pixels orthogonally with respect to the midline of the occulter. HD 191849 was observed immediately thereafter using two sequential orbits, using the same cross-BAR5 dither technique, as a PSF reference. 22-26 images per dither location were obtained using 11. 5 second per image integrations. We also obtained a single-orbit observation of AU Mic on 22 Sept 2018 with the disk aligned along the long axis of the BAR5 occulter, using the same dither and integration scheme described above. These disk-obscured images provide perfect color-matching to explore alternate methods to achieve better PSF subtraction. These data were reduced and calibrated using the same procedures and techniques as outlined in  Schneider et al.
(2018). Following bias, dark, and flat field correction using the temporally nearest calibration data, we located the position of the occulted star in each image using the "X marks the spot" diffraction spike fitting method of  Schneider et al. (2014). Within each orbit, all images observed with the same dither position were then median combined and cleaned of cosmic-rays. Image co-registration, and later PSF subtractions, were done with sinc-apodized bi-cubic sub-pixel interpolation using the IDL-based, IDP3 software  (Stobie & Ferro 2006). The relative brightness and (x,y) position of the PSF star HD 191849 were treated, and iteratively adjusted, as free parameters to minimize the variance in difference image pixels not dominated by disk flux. We found that while chromatic residuals were fully mitigated with our disk-obscurred BAR5 observation of AU Mic on 22 Sept 2018, using this orbit as a PSF template led to substantial PSF subtraction residuals caused by differential wavefront errors induced by the non-contemporaneous (e.
e. ∼1. 2 resolution elements yr -1 ; Grady 2019, submitted), annual observations are commensurate with resolvable motions of this sub-structure. HST GO-15907 is pursuing these observations and could enable discrimination of the potential role of projection. Moreover, a larger portion of the disk will be read-out in these planned observations, allowing us to determine whether other known moving features in the disk exhibit loop-like morphologies similar to that found for feature A. To further explore new information encoded within these high-resolution BAR5 imagery, we applied a high-pass filter to these data (panel d, Figure  1 ). We fit two 1-dimensional Guassians to the loop-like structure to quantify its size and projected location. These fits reveal the loop-like structure has a projected width of 1.
Full 20,000 step MCMC explorations were independently run for each inclination, and the best (lowest χ 2 ) solution from the converged portion of the chains was considered. This grid found the rotation axis is weakly constrained from the starspot data alone, with the best model of i = 75 • being only slightly preferred (∆χ 2 ∼ 1) over the edge-on solution. The STSP models more strongly rule out highly inclined scenarios of 45 • and 30 •. Thus, since we know the system inclination is likely edge-on from our spatially re- solved imagery, the STSP results support the suggestion that the effective B field of AU Mic is mis-alignment with its rotational axis. Further quantifying the detailed topology of AU Mic's B field via Zeeman-Doppler Imaging is strongly encouraged. The resultant best fit synthetic spot modeling light curve is shown in Figure  4  (red), along with the underlying TESS data (blue).
Alternate Forms of Mis-alignment and Potential Ramifications Our spot modeling (Section 3. 3) and the associated interpretation of these results (Section 4. 2) utilized previous research and observational properties of the system that indicated co-alignment of AU Mic's stellar and disk rotational axes. We remark that if we relax this co-alignment prior, the observed phase-dependence of AU Mic's spot coverage (two spot complexes visible for ∼60% and ∼40% of the rotational period respectively) would demand mis-alignment between the edge-on disk and the stellar rotational axis. In such a scenario, our available data would not place constraints on the relative orientation of the B field. However, this misalignment would expose the disk to seeing different amounts of the equatorial versus more polar wind with each rotation of the star.
Using Edge-on Disks to Break Starspot Modeling Degeneracies The advent of high precision, high cadence, long duration photometric datasets from space-based missions like Kepler and TESS provide a unique opportunity to identify and characterize stellar activity arising from spot modulation across a large sample of low mass stars. We remark that our work with AU Mic reveals another unique way to break the degeneracy between stellar inclination and spot latitudes. Much like the special case of transiting planetary systems, whereby the presence of a transit allows one to deduce the stellar inclina-tion angle with high precision  (Morris et al. 2017) , the subset of circumstellar disk systems that offer detailed inclination angle information (e. g. as measured from spatially resolved imaging for both edge-on, face-on, and intermediate inclination systems, or as inferred from photometric behavior like so-called "dipper" systems, which could suggest a likely near edge-on inclination  (Cody et al.
In addition, changes in sequence length (leading to an expansion of the sequence space) provide new spaces (called by the author ''blank tape'') in which environmental information and increase of complexity associated with the ongoing evolution can be recorded  (Adami et al. 2000 ). Thus, by continuously feeding databases with novel sequences, the topographical map extends, allowing the exploration of still unsuspected fitness landscapes. With all these considerations, the size (dimension) of the protein universe (i. e. the total number of possible protein sequences) can be viewed as infinite  (Adami et al. 2000). Actually, with an average protein length between 283 for Archaea and 438 for Eukaryotes  (Lukasz and Kozlowski 2017) , the number of different protein sequences can be estimated between 20 283 and 20 438 (i.