dataesr/scientific-paragraphs-categorization huggingface dataset:
Survey data consists of the complete SPC dataset, along with a subsampling of the full resolution SPAN data and a series of moment calculations on the SPAN data. All full resolution SPAN data are archived onto flash memory within the SWEM. Following an encounter, all of the SPC data, and the SPAN survey data will be telemetered down to the ground and the science team will examine it for periods of interests based on scientific goals for the orbit. The SWEM will then be commanded to transfer the full-resolution SPAN data from those periods of interest to the SPP solid-state recorder. The full resolution data will then be telemetered during a downlink period later in the non-encounter phase of the orbit. A baseline science observing plan is developed for each encounter for the SWEAP suite with inputs and in coordination with the SPP orbit planning.
Acknowledgements We acknowledge support from  NASA  under contract  NNN06AA01C (Task NNN10AA08T ). We are grateful for the creativity and dedication of the many people at SWEAP institutions who make this investigation possible. We also acknowledge early support for technology development by the  Smithsonian Institution ,  NASA Marshall Space Flight Center  and the  CNRS PROMES research group in Odeillo-Font Romeu, France. We thank  Jean-Yves Prado  and  CNES  for providing financial support for our activities in France. We also thank  NASA  and the rest of the SPP team for their support on this project. J. C. Kasper  personally thanks  John Alexander Simpson  and  Alan Jay Lazarus  for their contributions to Solar Probe and for exposing a student to this exciting mission of discovery.
5-7. 7 mag, far from the limit of the naked human eye. The specific advantage of CARMENES is the wide wavelength coverage and high spectral resolution in both visible and near-infrared channels. Simultaneous observation from 0. 5 to 1. 7 µm is a powerful tool for distinguishing between genuine planet detections and false positives caused by stellar activity, which have plagued planet searches employing spectrographs with a smaller wavelength coverage, especially in the M-type spectral domain  (Reiners et al. 2010; Barnes et al. 2011). A substantial amount of guaranteed time for the completion of the key project is also an asset. A precise knowledge of the targets is critical to ensure that most of the CARMENES guaranteed time is spent on the most promising targets. This selection involves not only a comprehensive data compilation from the literature, but also summarises our observational effort to achieve new low-and high-resolution optical spectroscopy and high-resolution imaging.
The present publication on low-resolution spectroscopy is the first paper of a series aimed at describing the selection and characterisation of the CARMENES sample. We have shown some preliminary results at conferences before that described the input catalogue description and selection  (Caballero et al. 2013; Morales et al. 2013) , low-resolution spectroscopy  (Klutsch et al. 2012; Alonso-Floriano et al. 2013a) , high-resolution spectroscopy  (Alonso-Floriano et al. 2013b; Passegger et al. 2014) , resolved multiplicity  (Béjar et al. 2012; Cortés-Contreras et al. 2013 ), X-rays  (Lalitha et al. 2012) , exploitation of public databases  (Montes et al. 2015) , or synergies with Kepler K2  (Rodríguez-López et al. 2014). This first item of the CARMENES science-preparation series details the low-resolution optical spectroscopy of M dwarfs with the CAFOS spectrograph at the Zeiss 2.
CARMENES sample To prepare the CARMENES input catalogue with the best targets, we systematically collected all published M dwarfs in the literature that fulfilled two simple criteria: -They had to be observable from Calar Alto with target declinations δ > -23 deg (i. e. , zenith distances < 60 deg, air masses at culmination < 2. 0). -They were selected according to late spectral type and brightness. We only catalogued confirmed dwarf stars with an accurate spectral type determination from spectroscopic data (i. e. , not from photometry) between M0. 0 V and M9. 5 V. Additionally, we only compiled the brightest stars of each spectral type. Our database contains virtually all known M dwarfs that are brighter than the completeness magnitudes shown in Table  1 , and most of them brighter than the limiting magnitudes.
No target fainter than J = 11. 5 mag is in our catalogue. We started to fill the CARMENES database with the M dwarfs from the Research Consortium on Nearby Stars at http://www. recons. org, which catalogues all known stars with measured astrometric parallaxes that place them within 10 pc (e. g. ,  Henry et al. 1994; Kirkpatrick et al. 1995; Riedel et al. 2014; Winters et al. 2015). The RECONS stellar compilation was next completed with the Palomar/Michigan State University survey catalogue of nearby stars  (PMSU -Reid et al. 1995 , 2002; Hawley et al. 1996; Gizis et al. 2002). Afterwards, we gave special attention to the comprehensive proper-motion catalogues of  Lépine et al. (2003 Lépine et al. ( , 2009 Lépine et al. ( , 2013) )  and  Lépine & Gaidos (2011) , and the "Meeting the Cool Neighbors" series of papers  (Cruz & Reid 2002; Cruz et al.
2003 Cruz et al. , 2007;; Reid et al. 2003 Reid et al. , 2004 Reid et al. , 2008)). Table  2  provides the sources of our information on M dwarfs. Until we start our survey at the end of 2015, we will still include some new, particularly bright, late, single, M dwarfs 2. As of February 2015, our input catalogue, dubbed CARMENCITA (CARMENES Cool dwarf Information and daTa Archive), contains approximately 2200 M dwarfs. For each target star, we tabulate a number of parameters compiled from the literature or measured by us with new data: accurate astrometry and distance, spectral type, photometry in 20 bands from the ultraviolet to the mid-infrared, rotational, radial, and Galactocentric velocities, Hα emission, X-ray count rates and a Some other publications and meta-archives that we have searched for potential CARMENES targets are  Kirkpatrick et al.
Low-resolution spectroscopic data Observations were secured with the Calar Alto Focal reductor and Spectrograph (CAFOS) mounted on the Ritchey-Chrétien focus of the Zeiss 2. 2 m Calar Alto telescope  (Meisenheimer 1994). We obtained more than 900 spectra of 745 targets during 38 nights over four semesters from 2011 November to 2013 April. All observations were carried out in service mode with the G-100 grism, which resulted in a useful wavelength coverage of 4200-8300 Å at a resolution R ∼ 1500. Exposure times ranged from shorter than 1 s to 1 h. The longest exposures were split into up to four sub-exposures. On some occasions, another star fell in the slit aperture (usually the primary of a close multiple system containing our M-dwarf candidate main target). We also added the 13 red dwarfs and giants observed in 2011 March by  Jiménez-Esteban et al.
Additionally, there are wavelength intervals of fluxes in the numerator that are either redder and bluer than the one in the denominator, which translates into different slopes in the index-spectral type relations. Of the 31 tabulated indices, nine are related to TiO features, seven to VO, six to CaH, three to the "pseudo-continuum" (i. e. , relative absence of features), and the rest to H and neutral metallic lines (Ti, Na). For every star observed with CAFOS, we computed the stellar numerator and denominator fluxes using an automatic trapezoidal integration procedure. When all indices were available, we plotted all spectral index vs. spectral type diagrams for the standard stars listed in Table  3  and fitted low-order polynomials to the data points. Although some spectral indices allowed linear (e.
2). However, over 93 % of the compared stars have disagreements lower than or equal to 2 subtypes. We emphasize that our CARMENCITA data base is very homogeneous because more than 95 % of the spectral type determinations come from either PMSU,  Lépine et al. (2013) , or our CAFOS data, which are consistent with each other, as shown above. Of the 683 CAFOS M-type dwarfs (and subdwarfs), 414 and 106 M dwarfs satisfy our criteria in Table  1  of restrictive J-band spectral type limiting and completeness, respectively. In total, 261 dwarfs have spectral type M4. 0 V or later. The brightest, latest of them are being followed-up with high-resolution spectrographs and imagers and with data from the bibliography to identify the most suitable targets for CARMENES (no physical or visual companions at less than 5 arcsec, low v sin i; see forthcoming papers of this series).
Financial support was also provided by the Universidad Complutense de Madrid, the Comunidad Autónoma de Madrid, the Spanish Ministerios de Ciencia e Innovación and of Economía y Competitividad, and the Fondo Europeo de Desarrollo Regional (FEDER/ERF) under grants AP2009-0187, SP2009/ESP-1496, AYA2011-30147-C03-01, -02, and -03, AYA2012-39612-C03-01, and ESP2013-48391-C4-1-R. Based on observations collected at the Centro Astronómico Hispano Alemán (CAHA) at Calar Alto, operated jointly by the Max-Planck Institut für Astronomie and the Instituto de Astrofísica de Andalucía. This research made use of the SIMBAD, operated at Centre de Données astronomiques de Strasbourg, France, the NASA's Astrophysics Data System, the RECONS project database (http://www. recons. org), the M, L, T, and Y dwarf compendium housed at http://dwarfarchives.
Precise measurements of the neutron lifetime are important for elementary particle physics, astrophysics and cosmology  [1, 2]. In accordance to Particle Data Group (PDG)  [3] , the neutron mean lifetime world value is estimated using works  [4] [5] [6] [7] [8] [9] [10] [11] ; it is equal to 880. 3 ± 1. 1 s. The main contribution to the mean world value comes from work  [6] , which uses the method of storage of ultracold neutrons (UCNs); its result is τ β = 878. 5 ± 0. 7 st ± 0. 3 meth s. Other results using this method  [4, 5, 7, 8]  are significantly less precise; uncertainties in these experiments are 2-3 s. Main limitations of the UCN storage method are related to systematic corrections. The probability of UCN loss from a trap λ = λ l + λ β , where λ l = pμ is the probability of UCN loss in the trap walls, λ β = 1/τ β is the probability of neutron decay, p is the frequency of UCN collisions with the trap walls, and μ is the probability of UCN absorption and inelastic scattering per bounce.
Then, λ β was evaluated by linearly extrapolating the experimental data λ(λ l ) to the zero probability λ l = 0. Systematic corrections inherent for this approach are related to the differences in the efficiency of detection of UCNs and thermal neutrons originating from UCNs up-scattered on trap walls. Recently, results of many UCN storage experiments were largely shifted or selected a posteriori due to additional analysis or new data. Moreover, results of measurements using the method of UCN storage  [4] [5] [6] [7] [8]  and those using the method of in-flight decay of cold neutrons  [9] [10] [11]  differ by many seconds. Thus, the most precise in-flight experiment  [11]  provides the value of neutron lifetime τ β = 887. 7 ± 1. 2 st ± 1. 9 meth s that differs from the result  [6]  by 9. 2 s, by far larger then the estimated uncertainties of these experiments.
Acknowledgments C. Wang 's work is supported by  China Scholarship Council. F. Grillot's work is supported by the the  European Office of Aerospace Research and Development (EOARD)  under Grant  FA9550-15-1-0104  and  Partenariat Hubert Curien  under Grant  30794RC  ( Campus France/ DAAD ). The authors would like to thank  Professor Marek Osiński  from the  University of New Mexico, USA  for helpful discussions.
Acknowledgments We thank  Olivier Herscovici  and  Claudio Castellani  for discussions and insights. We thank CalMiP for access to its supercomputers and the  University Paul Sabatier  ( OMASYC  project). This work was supported by  Programme Investissements d'Avenir  under the program  ANR-11-IDEX-0002-02 , reference  ANR-10-LABX-0037-NEXT , and by the  ANR  grant  K-BEC  No  ANR-13-BS04-0001-01. JM is grateful to the  University of Liège  for the use of the NIC4 supercomputer (SEGI facility), and for funding (project  C-13/86 ). I. G. M. received support from  ANCyPT  grant  PICT 2010-1556  and from  CONICET  grant  PIP 114-20110100048. I. G. M. and J. M. received support from  CONICET-FNRS  binational project, and B. G. and I. G. M. from the  CONICET-CNRS  bilateral project  PICS06303.
[10]. The analysis is performed with a data sample corresponding to an integrated luminosity of 3. 0 fb -1 of proton-proton (pp) collisions, recorded by the LHCb experiment at centre-of-mass energies of 7 TeV and 8 TeV in 2011 and 2012, respectively. The analysis proceeds in two steps. The first step, described in detail in Sec. 3, consists of a multivariate selection of B → J/ψ K 0 S candidates. In the second step a maximum likelihood fit is performed to the selected data. The fit model includes a prominent B 0 → J/ψ K 0 S component, which is used to improve the modelling of the B 0 s → J/ψ K 0 S signal. In addition, the measurement of CP asymmetries associated with B 0 → J/ψ K 0 S decays offers a validation of the likelihood method's implementation. However, the stringent event selection necessary to isolate the B 0 s → J/ψ K 0 S candidates limits the precision on these two CP observables.
This opens a window for the time to digital converter (model CTNM4, Institut de Physique Nucléaire, Orsay, France) to accept the four signals from the delay line detector  [19]  and the ion signal from the TOF spectrometer. All of the events are stored and are sorted later by the software to extract all of the information either in single hit or in coincidence. In a typical TOF spectrum the various natural isotopes of Xe can be easily separated by the apparatus (see the inset of figure  1  for an example of the TOF spectrum). By selecting a range of arrival times and thus masses of the ions we can select only the electrons formed in coincidence with ions of that mass and therefore a velocity mapped photoelectron image for each isotope can be built up. These images were then inverted using the pBasex software  [20]  in order to extract the parameters describing the electron angular distributions resulting from ionization of the = I 0( Xe) 132,134,136 ), = I.
Acknowledgments We thank the general technical SOLEIL staff for smoothly running the facility, and for the allocated beamtime under project  20100271. The experimental research reported here has received funding from the  European Community 's  Seventh Framework Programme  ( FP7/2007-2013 ) under Grant Agreement No. 226716. EVG, ANG acknowledge support by the  Russian Foundation for Basic Research (RFBR)  under grant  12-02-01123  and hospitality at the  European XFEL (Hamburg, Germany ), where a part of this work was done. EVG gratefully acknowledges financial support by the  Dynasty Foundation  via the  Support Program for Young Scientists. MM acknowledges support by the  Deutsche Forschungsgemeinschaft (DFG)  under grant no. SFB 925/A1.
Numerical simulation A numerical simulation has been performed to model the evolution of the spatio-temporal density around an obstacle for high velocity inflow. Our main interest has been to correlate the increase of density directly in the rear front of the shockwave with the increase of velocity. The numerical simulation has been performed using the free software Tycho-cfd (Tyrolean Computational Hydrodynamics), which is a multidimensional compressible hydrodynamic code fully parallelized. The system simulated is a bidimensional channel with a circular obstacle. The coordinates are cartesian and the size of the domain is 2x4 m height and width. The ablation during the arrival on the atmosphere is not taken into account. We assume that our body is perfectly circular and has gained during its entry in the atmosphere a temperature of 2000°K.
Acknowledgements We are greatly indebted to  Marc Sibeaud  and  Alain Cayrol  ( CEA Gramat ) at the Direction of Military Applications,  CEA Gramat Center (France)  for offering access to the Persephone Light gas gun experiments. We thank  Magali Michel ,  Michaël Vaillant  and  Brigitte Deniaux  for their assistance in the field survey of the 2011 August 3 rd debris fall. Guispert Guirardo  and  Mercè Moncusi  at the  SRiCT-Tarragona  university are acknowledged for their technical assistance. We thank  Sylvie Bonnamy  and  Fabienne Warmont  at the  CRMD-Orleans university  for the TEM analyis and  Dimitri Gorand  at the  C2M-Perpignan university  for the SEM analysis. We thank  Wolfgang Kapferer  for the implementation of the tycho cfd-software.
Magnetically-induced forces on the inertial masses on-board LISA Pathfinder are expected to be one of the dominant contributions to the mission noise budget, accounting for up to 40%. The origin of this disturbance is the coupling of the residual magnetization and susceptibility of the test masses with the environmental magnetic field. In order to fully understand this important part of the noise model, a set of coils and magnetometers are integrated as a part of the diagnostics subsystem. During operations a sequence of magnetic excitations will be applied to precisely determine the coupling of the magnetic environment to the test mass displacement using the on-board magnetometers. Since no direct measurement of the magnetic field in the test mass position will be available, an extrapolation of the magnetic measurements to the test mass position will be carried out as a part of the data analysis activities.
Conclusions Magnetically induced forces on the LISA Pathfinder test masses will be an important contribution to the final mission noise budget. Understanding the magnetic environment on board and characterising the magnetic properties of the test mass is crucial for the mission. During the 4th operational exercise, the experiments to induce a magnetic signal and thereby measure the magnetic moment and susceptibility of the test masses were simulated and the data analysis pipeline successfully tested, providing a successful characterisation. The interpolation of the magnetic field from the magnetometers to the test mass position is a difficult task given the distribution of magnetic sources in the satellite surrounding the test masses. We have reported a first characterisation of the impact of individual magnetically active components to the total measured magnetic field.
This argument obviously holds only in the kinematical regions where the influence of the isovector component is significant. We have previously tested our model on the MiniBooNE data for the differential cross sections  [3, 17] , independently for neutrinos  [8]  and antineutrinos  [13]. The good fit of the data provided by our model did not contradict our statement on the respective roles of np-nh. However in these works, the test was performed separately for the neutrinos and the antineutrinos and we did not specifically address the detailed comparison between the two. As this comparison is essential for the CP violation detection we want to investigate in the present work this question in more details. For Cherenkov detectors, such as the MiniBooNE or the Super-Kamiokande ones, are we able to describe quantitatively the difference between neutrinos and antineutrinos nuclear interactions? The wealth of experimental data which has accumulated in the last years by the MiniBooNE experiment allows an experimental test for this comparison and we will explore the message which can be drawn from these data.
5 1 1. 5 2 E ν (GeV) -0. 5 0 0. 5 1 1. 5 Normalized Fluxes Φ(E ν ) (GeV -1 ) MiniBooNE Φ ν µ MiniBooNE Φ ν µ Φ + Φ - FIG. 1:  (color online) Normalized MiniBooNE ν µ and νµ fluxes derived from Refs. [3]  and  [17]  respectively. Their half sum (Φ + ) and half difference (Φ -) are also shown. while for the difference dif the sign plus is changed to a minus one. Notice from Eq. (  1 ) that the difference, dif , contains only one term, the axial vector interference one. It is this quantity which governs the difference in cross sections of ν and ν but it is not accessible directly from neutrino data since only derivatives with respect to the emitted lepton energy are measurable. We also introduce S and D, the corresponding flux integrated quantities, which are instead experimentally accessible in the MiniBooNE data, S(cos θ, E µ ) = d 2 σ ν d cos θdE µ + d 2 σ ν d cos θdE µ (4) D(cos θ, E µ ) = d 2 σ ν d cos θdE µ - d 2 σ ν d cos θdE µ (5) in which quantities such as d 2 σν d cos θdEµ have been defined previously in Eq.
It will be the object of a future investigation. Notice that the present study is done for the muonic neutrinos of the MiniBooNE experiment, for which data are available while CP violating experiments through the asymmetry of the oscillations rates of muonic neutrinos and antineutrinos into electron ones involve the detection of electrons or positrons produced in a detector by the charged current interactions of these electron neutrinos. We have already addressed the question of electron neutrino cross sections, versus the muon neutrino ones  [21]. The effect of the small change in kinematics due to the smaller electron mass will not affect the present conclusions: the electron neutrino nuclear interactions produce by themselves an important ν e νe asymmetry. The present study indicates that the multinucleon role is essential in this problem and to what precision this asymmetry can be mastered.
These combinations remain rather pure with respect to the axial vector interference term which is either dominant (difference) or nearly absent (sum). This allows more specific tests of our theoretical model on the axial vector interference term, important for the CP violation data. Our model gives a good fit for the MiniBooNE data for the sum and the difference of the cross sections reproducing well the data in the full range of muon energy and emission angle. The introduction of the multinucleon component is necessary for a good fit, an important test for its presence in the axial vector interference term. The success of our description indicates that we can reach a good understanding of the nuclear effects in neutrino interactions, also for what concerns the comparison between neutrinos and antineutrinos cross sections.
We have concentrated in this work on the interactions of muonic neutrinos where a complete set of data is available. Our predictions can easily be extended to electron neutrinos, relevant for CP violation data. The nuclear cross section difference for neutrinos and antineutrinos stands as a potential obstacle in the interpretation of experiments aimed at the measurement of the CP violation angle, δ. The present analysis, performed on the MiniBooNE data, shows the importance, for Cherenkov detectors, of the inclusion of the multinucleon contribution to the quasielastic-like cross section for mastering this difference.
Disformally coupled, light scalar fields arise in many of the theories of dark energy and modified gravity that attempt to explain the accelerated expansion of the universe. They have proved difficult to constrain with precision tests of gravity because they do not give rise to fifth forces around static non-relativistic sources. However, because the scalar field couples derivatively to standard model matter, measurements at high energy particle colliders offer an effective way to constrain and potentially detect a disformally coupled scalar field. Here we derive new constraints on the strength of the disformal coupling from LHC run 1 data and provide a forecast for the improvement of these constraints from run 2. We additionally comment on the running of disformal and standard model couplings in this scenario under the renormalisation group flow.