dataesr/scientific-paragraphs-categorization huggingface dataset:
e. , with the pedestal width. Crystal occupancy (the LAC rate) is reported continuously by Data Quality Monitoring ( § 2. 4) as are the pedestal widths. LAT event reconstruction  (Atwood et al. 2013; Bruel et al. 2018 ) is robust against a modest number of CAL noise hits, so there is no immediate need to respond to noisy channels when they occur. Over the first ten years in orbit, the typical pedestal width has remained constant, although several channels show increased noise, detailed in § 4. 3. To accommodate the increased noise in those few cases, we have raised the LAC threshold to its maximum possible value on 3 channels, effectively disabling them. Because a given crystal is qualified for inclusion in the CAL data stream by the LAC discriminator on either endface, and because the energy deposited in the crystal is calculated from the geometric mean of the energy calculated at each end-face, the modest number of noisy channels has no effect on the science performance of the CAL.
Should one of these cataclysms yield near-simultaneous GW and GRB arrivals at Earth, confidence in Fermi 's clocks could become an important element in how an observed lag is interpreted. § 9 of  Abdo et al. (2009)  describes pre-launch measurements of the accuracy of the timestamps assigned to LAT events. Atmospheric muons traversing both the LAT and a standalone muon detector allowed us to compare times recorded using a standalone GPS receiver with those recorded by the LAT. The timestamps were shown to be accurate to ∼ 300 ns, root-mean-square (rms). The least significant digit of timestamp data in the data files used for astronomical analyses is 1 µs, contributing an rms of 300 ns to the pulsar results described below. To compare an arrival time at the satellite with an event time at a different observatory, Fermi 's position must also be known accurately.
Acknowledgements: The  Fermi LAT Collaboration  acknowledges generous ongoing support from a number of agencies and institutes that have supported both the development and the operation of the LAT as well as scientific data analysis. These include the  National Aeronautics and Space Administration  and the  Department of Energy in the United States , the  Commissariat à l'Energie Atomique  and the  Centre National de la Recherche Scientifique / Institut National de Physique Nucléaire et de Physique des Particules in France , the  Agenzia Spaziale Italiana  and the  Istituto Nazionale di Fisica Nucleare in Italy , the  Ministry of Education, Culture, Sports, Science and Technology (MEXT) ,  High Energy Accelerator Research Organization (KEK)  and  Japan Aerospace Exploration Agency (JAXA) in Japan , and the  K.
The Solar magnetograms To verify that the wind model produces reasonable results, we compare our modelling results to Solar cases corresponding to Solar minimum and Solar maximum. We chose the GONG magnetograms from Solar cycle 24 (2008 December-2019 December) that exhibited the highest and lowest average surface magnetic field strength: these were the magnetograms from Carrington Rotation 2157 (Solar maximum, 2014 November) and 2211 (Solar minimum, 2018 December). Unlike the ZDI magnetograms which are reconstructed from spectropolarimetric data as the star rotates, the Solar magnetograms are reconstructed from observations of the extended Solar disc. The GONG Solar magnetograms have degree max = 60, i. e. the smallest length scale is 3 • ; in comparison to the ZDI magnetograms they are highly detailed.
C O N C L U S I O N S We have started out with a desire to study the space weather of the Sun at 0. 6 Gyr using magnetogram data from the Hyades cluster. This is close to the age when life first arose on the Earth  (Mojzsis et al. 1996). We have seen that even though the Solar system would have been a different, more active place when the Sun's age was 0. 6 Gyr as the Hyades stars are today, the steady state wind pressure would not significantly hinder a young Earth from holding on to its atmosphere and shielding it from the Solar wind. As the Solar-type stars in the Hyades cluster are of similar age and provenance, we have been able to directly study the effect of magnetic field strength and complexity on key parameters such as mass-loss, angular momentum loss and wind pressure over a range of magnetic field strength values.
This work has made use of the Vienna Atomic Line Database (VALD), operated at  Uppsala University , the  Institute of Astronomy RAS in Moscow , and the  University of Vienna. We acknowledge the use of the SIMBAD data base. This research has made use of the VizieR catalogue access tool, CDS, Strasbourg, France (DOI: 10. 26093/cds/vizier). The original description of the VizieR service was published in A&AS 143, 23h. This research has made use of  NASA 's Astrophysics Data System. We acknowledge use of  NASA/GSFC's Space Physics Data Facility 's OMNIWeb service, and OMNI data. This work was carried out using the SWMF tools developed at The  University of Michigan Center for Space Environment Modelling (CSEM)  and made available through the  NASA Community Coordinated Modelling Center (CCMC).
Volatile distribution in VLS pyroxenes SIMS analyses were performed in 31 VLS cpx and 31 VLS opx (including 28 samples with both opx and cpx data), resulting in a total of 235 analyses after filtering for data quality (see the Supplementary Materials for details). Average H 2 O and fluorine contents in opx vary from 81 to 362 g g -1 and 0. 15 to 21 g g -1 , respectively, while average H 2 O and fluorine contents in cpx vary from 189 to 724 g g -1 and 0. 25 to 51 g g -1 , respectively (table  S1 ). No systematic hydrogen loss or gain from cores to rims is observed as a function of crustal ages, but cpx H 2 O abundances are slightly more scattered from the 1:1 line compared to the opx (Fig. 1 ). Fluorine core-to-rim concentrations show tight correlations in both opx and cpx, with limited deviation from the 1:1 line.
of 10 H 2 O and other incompatible elements are not expected during serpentinization. In addition, no large core to rim variations are observed, inconsistent with transient serpentinization. Last, hydrogen diffusivities at serpentinization temperatures may be too low to affect primary H 2 O abundances in pyroxenes, although this is still debated  (37). Previous studies have reviewed the effects of depth and pressure on H partition coefficients between olivine and opx for peridotites equilibrated in the spinel and garnet stability field. Natural pyroxenes and bulk peridotites from global datasets display order of magnitude variations in H 2 O contents at similar pressures of equilibration in the spinel stability field  (7) , casting doubt that pressure is the main controller of hydrogen distribution in the oceanic lithospheric mantle.
The glass calibration slope was used to reduce data for C, P, S, and Cl. Analytical uncertainties over five counting cycles were combined with calibration slope uncertainties to yield typical total uncertainty (2 SE, 95% confidence intervals) of <12, <12, <8, and <9% for C, P, S, and Cl, respectively. For reference, total uncertainties for OH and F in glass reference materials are <4 and <3%, respectively. Because volatile measurements on the SIMS are often affected by matrix effects, we also measured the same volatile elements on opx-cpx reference materials requested from the Department of Minerals Sciences, Smithsonian Museum (USA) and calibrated using mount NMNH 118331. Opx reference materials that were used for the calibration curve included NMNH 116610-29, 117322-245, 116610-5, and 109426-1.
Cpx reference materials that were used for the calibration curve included NMNH 117213-5, 11610-18, 116610-15, 118317-1 (KH03-27), and 118318 (SC-J1). These reference materials have been calibrated for SIMS in a previous study using reference materials from Carnegie Institution  (68). The reference materials from Carnegie Institution had been cross-calibrated by multiple independent absolute techniques such as FTIR, elastic recoil detection analysis, and vacuum manometry; see complete list of references in  (68). Representative calibration curves are presented in fig. S5  and were used to calculate the water and fluorine contents of pyroxenes. Measurements where the internal precision of 16 O 1 H/ 30 Si and/or 19 F/ 30 Si was greater than 10% were excluded from the dataset. The vast majority of internal 2 SE are much lower than 10%, with an average of 0.
Acknowledgments: We thank an anonymous reviewer,  L. Doucet ,  C. Langmuir , and  P. Tollan  for thoughtful reviews that improved this manuscript. We thank  B. Schoene  for editorial handling of the manuscript. Funding: Funding for this study was supported by  NSF   EAR-P&G 1524311  and  1839128  to V. L. R. and the  Andrew W. Mellon Foundation Award for Innovative.
Acknowledgements This research was supported by the  Ministerio de Educación y Ciencia/Ciencia e Innovación of Spain  (projects  CGL2017-85038-P ,  CGL2013-47521-P ,  CGL2010-18851/ BTE ,  CGL2007-64061/BTE ,  CGL2004-02338/BTE ); the  European Region Development Fund, European Union ;  Gobierno Vasco/EJ  (research groups  IT1418-19 ,  IT1044-16 ,  IT834-13 ,  GIC07/14-361 ); and  Universidad del País Vasco/ EHU  ( PPG17/05, 9/UPV 00121. 310-15303/2003 ). The second author (A. B. ) acknowledges financial assistance from the  UPV/EHU  (predoctoral grant). This paper was written as part of a research collaboration program between the  Centre National de la Recherche Scientifique (CNRS, France) , the  Muséum national d'Histoire naturelle (MNHN, Paris)  and the  Universidad del País Vasco/Euskal Herriko Unibertsitatea  ( UPV/EHU, Bilbao ), with the  Arabako Natur Zientzien Museoa/Museo de Ciencias Naturales de Álava  as a partner in this work.
These ages are obtained in two laboratories using the same protocol and samples (see supplementary Fig. 5  and Supplementary Data 1 for spectra, isochrons, and full data). Average ages for belizite and Pantasma glass are 792. 1 ± 9. 2 ka (2σ; n = 4; Mean Squares Weighted Deviation (MSWD) = 0. 05; Probability (P) = 0. 98) and 809. 1 ± 6. 4 ka (n = 4; MSWD = 1. 2; P = 0. 30). We also tested if these age distributions could result from a single impact event by using a χ 2 test on the entire dataset. Using the present eight  40  Ar/  39  Ar plateau ages returns a P-value of 0. 081 which is concordant, yielding a weighted mean age of 803. 7 ± 8. 5 ka (n = 8; MSWD = 1. 8). The available  40  Ar/  39  Ar data are thus fully compatible with belizites and Pantasma impact glasses being both produced from the same impact event.
4  Cr isotopic data. ε 54 Cr data obtained on a belizite sample, the Pantasma breccia bulk (after  19  ) and magnetic extract, compared to carbonaceous and ordinary chondrites  28  , as well as terrestrial rocks  29. 2σ error bars shown. presence of Fe-Ti oxide inclusions similar to those observed in Pantasma impact glasses (supplementary Fig. 6 ). This also supports a common origin, as well as the ordinary chondrite signature found in both Pantasma impact breccia PB5 and belizites (ref. 19 and Fig. 3 ). In fact, the magnetic extract from P5B breccia, with ε 54 Cr = -0. 44 ± 0. 22, appears more contaminated by extraterrestrial matter compared to the bulk P5B (ref. 19 and Fig. 4 ), thus reinforcing the evidence for extraterrestrial contamination in Pantasma breccia. The numerous evidence for cogenesis between belizites and Pantasma impactites listed above thus supports the interpretation of coeval  40  Ar/ 39 Ar age determinations.
Discussion The proposed belizites-Pantasma crater couple is the fourth known tektite-crater couple, and presently the youngest. The suggested synchronism of this event with the australasites  18  is not supported by our composite age for belizite-Pantasma, at 803. 7 ± 8. 5 ka, compared to the most recent high-precision age for australasite, at 788. 1 ± 2. 5 ka  38  ; both ages were obtained in the same laboratories and are reported with 2σ error bars. Besides the observed common features among the four tektite-crater couples, plus the australasite strewn-field, the Central American couple displays a number of peculiarities. It is the only strewn-field to show a mantle signature due to its derivation from volcanic arc Fig. 6  Normalized average composition of belizites. Average composition of belizites (see Supplementary Data 2) normalized to the average of the Pantasma volcanic rocks or impact glass  19.
Acknowledgements This work was supported by A*midex fundation from  Aix-Marseille Université   CIVA  project and  Agence Nationale de la Recherche   ANR-15-CE31-0011-01   SVPintMex  project. Three reviewers are thanked for their improvement of the initial manuscript. For their help with the fieldwork, we are deeply indebted to the  Centre d'Etudes Mexicaines et Centro-Americaines (CEMCA)  and its director S. Hardy. P. R. thanks  INSU  for funding his sabbatical leave during writing the paper, and  C. Andrieu  for discussion on Mayan archeology. The ASTER AMS national facility (CEREGE, Aix-en-Provence) is supported by the  INSU/CNRS , the  ANR  through the  "Projets thématiques d'excellence"program for the "Equipements d'excellence" ASTER-CEREGE action  and  IRD. V. D. thanks the  FRS-FNRS  and  ERC StG  "ISoSyC"  FP7/336718  for support and  S.
Cauchies  for technical support. Parts of this work were supported by  IPGP  multidisciplinary program PARI, by  Region Île-de-France Sesame  Grants no. 12015908  and  EX047016  and the  IdEx Université de Paris  grant,  ANR-18-IDEX-0001. B. R. acknowledges support from  INSU  through the national Raman facility in Lyon, and from the  LABEX Lyon Institute of Origins  ( ANR-10-LABX-0066 ), within the program " Investissements d'Avenir"  ( ANR-11-IDEX-0007 ) at  Université de Lyon. P. B. acknowledges funding from the  Centre National d'Etude Spatiale. Studied samples collected by J. C. in Belize and P. R. in Nicaragua did not request sampling permits.
Another debate has concerned the use of PEEP and the recruitability of the lungs of these patients. Recommendations have varied between high PEEP (initially) and low PEEP-inspiratory oxygen fraction (F IO 2 ) tables. As for classical ARDS, however, an individual titration seems desirable since various degrees of lung recruitability have been described both in classical ARDS and in CARDS  [16, 17]. One ongoing trial is testing an individualised approach compared to the use of PEEP-F IO 2 tables (NCT03963622). Other aspects discussed have concerned the monitoring of the dead space or one of its surrogates (e. g. the ventilatory ratio), elevation of which could raise the suspicion of micro or macrovascular thrombi; but the evidence there is very weak and cannot replace other markers. The need to monitor and control the respiratory drive under assisted ventilation after the initial phase has also been emphasised, to potentially avoid mechanisms of self-inflicted lung injury  [18].
This reconstruction, BedMachineV3, provides substantial improvements in estimates of bedrock geometry beneath glaciers and within their fjords, revealing connections between subglacial valleys and submarine troughs and the presence or absence of ridges in the glacial fjords. In addition, CTD data collected in the fjords diagnose the presence (or absence) of subsurface Atlantic Water (AW) in deep (or shallow) fjords and on the continental shelf  (18). Here, we combine these extensive new observations with ocean modeling to assess the extent to which ocean warming has induced ice front retreat at 226 marineterminating glaciers that controlled 96% of ice discharge from the Greenland Ice Sheet between 1992 and 2017. S C I E N C E A D V A N C E S | R E S E A R C H A R T I C L E 2 of 10.
Glacier retreat and ocean TF Between 1992 and 2017, Greenland's marine-terminating glaciers lost 3536 Gt (gigaton = 10 12 kg) of mass and 2452 km 2 of grounded ice (Table  1 ). The largest retreats occurred in northwest (NW) (28%), north (N) (22%), northeast (NE) (15%), and southeast (SE) (14%) (table  S1 ). To compare grounded ice retreat with oceanic TF, we reconstruct ocean temperature using two ocean state estimates from the Estimating the Circulation and Climate of the Ocean (ECCO) consortium combined with the CTD data (see Materials and Methods). TF is calculated as the depth-integrated difference between the in situ ocean temperature and the salinity-and pressuredependent freezing point of seawater from the lower 60% of the water column. We identify three periods based on the temporal trends in TF: (i) a stable TF period in 1992-1997, (ii) a warming period of rapid change in 1998-2007 averaging 0.
Ice front retreat Ice front retreat is manually digitized from level 1 Landsat 5, 7, and 8 products from 1985 to 2018. The resolution of Landsat data is 30 m S C I E N C E A D V A N C E S | R E S E A R C H A R T I C L E 8 of 10 for Landsat 5  (1985) (1986) (1987) (1988) (1989) (1990) (1991) (1992) (1993) (1994) (1995) (1996) (1997) (1998) (1999)  and 15 m for  Landsat 7 and 8 (1999 Landsat 7 and 8 ( -2013 Landsat 7 and 8 ( and 2013 Landsat 7 and 8 ( -2018, respectively), respectively). Ice front positions digitized as part of this project were supplemented with those publicly available from  (6, 7, 34). We formulate an areal record of ice front retreat by calculating the total change in area between successive fronts and within the fjord boundaries. We calculate a linear record of ice front retreat by dividing the areal record by the mean width of the glacier front in between two epochs.
The fact that they seem not to-and that any discrepancy between them is uncorrelated with galaxy environment-has yielded the constraint f R0 < ∼ 10 -7  [164, 165]. Notice that astrophysical constraints yield tighter bounds on f (R) models than solar system tests. Variable stars are also useful for more general tests of gravity. [166]  showed that the consistency between the mass estimates of Cepheids from stellar structure vs astroseismology allows a constraint to be placed on the effective gravitational constant within the stars. Using just 6 Cepheids in the Large Magellanic Cloud afforded a 5% constraint on G N , and application of this method to larger datasets spanning multiple galaxies will allow a test of the environment-dependence of G N predicted by screening. Screening may also provide a novel local resolution of the Hubble tension  [165, 167, 168].
21 and p 2 = 1. 503 log 10 |f R (z)-1| 1+z + 21. 64. This works well for f R0 ∈ 10 -6. 5 , 10 -4 and z ∈ [0, 1]. To test this effect, cluster strong lensing may be compared to X-ray masses or the velocity dispersions of the cluster galaxies  [188, 228] , and stacked weak lensing can be compared to Sunyaev-Zel'dovich masses or infall motions at the cluster outskirts  [229]. Dynamical masses can also be estimated from X-ray data of cluster temperature and pressure profiles. The combination of weak lensing measurements with measurements of the X-ray brightness, temperature and Sunyaev-Zel'dovich signal from the Coma cluster  [230]  (or from multiple clusters' weak lensing and X-ray signals  [231] ) implies f R0 < ∼ 6 × 10 -5 , and this test has also been applied to galileons  [232]. The modification to clusters' dynamical masses under a fifth force can be probed without requiring lensing data by assuming that the gas fractions of clusters are constant in order to estimate the true total mass.
9 ), the models were still a very good fit to CMB temperature, lensing and Baryon Acoustic Oscillation (BAO) data, using Planck-2013 temperature and lensing  [251]  and WMAP-9 polarization  [252]  data. For BAO they used 6dF, SDSS DR7 and BOSS DR9 data (  [253] [254] [255] ). In the absence of massive neutrinos (model dubbed Galileon in Fig. 9 ), however, ΛCDM was favoured by data. Nevertheless, they showed that the νGalileon model shows a negative ISW effect that is hard to reconcile with current observations. More recently, a paper by  [256]  performed a detailed study of self-accelerating Galileon models using CMB data from Planck-15 in temperature and polarization and CMB lensing  [257]. They also included BAO data, H 0 data and ISW data. As in the older analysis, they showed that the cubic Galileon predicts a negative ISW effect and therefore it is in a 7.
utdallas. edu/mishak/isitgr/ 19 https://github. com/sfu-cosmo/MGCAMB 20 http://miguelzuma. github. io/hi class public/ 21 http://eftcamb. org to be treated perturbatively, in order to make accurate predictions. This involves using either Eulerian or Lagrangian perturbation theory  [292, 293]  and furthermore using resummation techniques to capture accurately the large scale contributions  [294, 295]. For smaller scales, formalisms such as the effective field theory of large scale structures are needed in order to take into account the UV divergences of the perturbative models  [296]. For the models we are interested in here, there has been some recent work by  [236, 297] , some new work on GridSPT by  [298]  and some more foundational work by  [299, 300]. To obtain meaningful constraints with weak lensing, the power spectrum needs to be calculated at even higher kvalues, for up to k ≈ 10Mpc -1 , which is only possible using N-body simulations, which capture the full evolution of the nonlinear gravitational dynamics.
Constraints on f (R) models From the CMB, constraints have been placed by the Planck collaboration on the f (R) model in terms of the Compton wavelength parameter, which is defined as B ≡ f RR f R R H H , (183) and its value today B 0 is related to the fundamental parameter f R,0. Indeed we have the relation B = Ω m 1 + ω H 2 m 2 f R (184) where ω is the equation of state of the Universe and m f R is the mass of the scalaron  (166). Notice that the denominator 1 + ω is very small and therefore B is less suppressed than the ratio H 2 /m 2 f R In the analysis of  [315]  the datasets used were Planck TT+lowP+BAO+SNIa + local H0 measurements (these last three observations are usually abbreviated as BSH), while CMB lensing was used to remove the degeneracy between B 0 and the optical depth τ. At the 95% confidence level, they found B 0 < 0.
285 at the 99% C. L. In a more recent analysis by  [261] , the authors used the combined data of the Planck CMB temperature, polarization, and lensing reconstruction, the Pantheon supernova distances, BOSS measurements of BAO, along with the joint 3 × 2pt dataset of cosmic shear, galaxy-galaxy lensing, and galaxy clustering from KiDS and 2dFLenS. They took into account perturbation theory and N-body calculations from COLA and RAMSES to compute the theoretical predictions for the power spectrum. They constrain the JBD coupling constant to be ω BD > 1540 at the 95% C. L. and the effective gravitational constant, G eff /G = 0. 997 ± 0. 029. They also found that the uncertainty in the gravitational theory alleviates the tension between KiDS, 2dFLenS and Planck to below 1σ and the tension  [332]  in the Hubble constant between Planck and the local measurements to 3σ.
Furthermore, they relate the evolution of α M to a linear (p=1) and exponential (p > 1, varying free) parametrization  [315]. Using the Planck TT+TE+EE+BSH data set combination (BSH standing again for BAO, SN and local Hubble constraints) they find α today M < 0. 043 (95% confidence level) for the linear case and α today M < 0. 062 and p = 0. 92 0. 53 0. 24 (95% confidence level) for the exponential case. ΛCDM is recovered for p = 1 and α today M = 0, therefore placing relatively strong limits on possible deviations of Einstein's GR. As we discussed above, the gravitational wave event GW170817 constrained the Horndeski theory to be effectively composed only of Brans-Dicke models and cubic Galileons, and the latter are effectively ruled out by ISW observations. This limits then the interest on an overall analysis of Horndeski models in general.