dataesr/scientific-paragraphs-categorization huggingface dataset:
Objects lacking a 2MASS counterpart were rejected. In rare cases, it may happen that more than one 2MASS source are found. Generally, there is one bright source and the others are much fainter. Then consideration of magnitudes allows to identify the true counterpart. However, when the choice is not obvious, the object was dropped. This first 2MASS cross-matching procedure leads to a list of 894 entries. Further cleaning is necessary for many reasons. Numerous objects are common to Drake's and Palaversa's catalogues, and there are 112 duplicates in our preliminary list. These duplicates are however interesting because they can inform about differences in amplitudes and periods provided by the two databases. There are also objects presented in the LINEAR or Catalina catalogues as being periodic variables, but a systematic examination of Catalina light curves shows them to be of poor quality, or almost constant, or not clearly periodic.
Radial velocities We first collected all Gaia radial velocities. We added those from the APOGEE  (Majewski et al. 2017)  and RAVE  (Steinmetz et al. 2006; Kordopatis et al. 2013 ) surveys, and a few from  Monaco et al. (2007). There is in most cases excellent agreement between them when two measurements are available, with differences of ≤ 2 km s -1. Our catalogue includes these velocities, their errors and references. Some additional velocities come from  Feast & Whitelock (2000) , and from  Smak & Preston (1965) , with errors ∼ 5 km s -1. Although less accurate, ∼ 12-15 km s -1 , a few velocities come from the LAMOST database  (Luo et al. 2016)  or the Sloan DR7 M dwarf catalogue  (West et al. 2011). Overall, of 429 stars on our catalogue, 90 have a radial velocity.
Acknowledgements. N. M. thanks our anonymous referee for remarks that greatly improved the mansucript. We also thank  Olivier Richard  for generous help,  Henri Reboul  and  Denis Puy  for encouragments, and the staff of LUPM for kind assistance. We appreciated remarks from  Patrick de Laverny  on a preliminary version of the manuscript. N. M. is grateful to the  Université de Montpellier  for support. This work makes use of the Catalina database ( California Institute of Technology, NASA ), the  Lincoln Near-Earth Asteroid Research LINEAR database  ( Massachusetts Institute of Technology Lincoln Laboratory ,  NASA  and  US Air Force) , the  Two Micron All Sky Survey (University of Massachusetts  and IPAC/ Caltech  funded by  NASA and NSF) , the European infrared photometry DENIS experiment.
This work was supported by the Agence Nationale de la Recherche (Grant No. ANR-13-BS10-0016, ANR-15-CE09-0017, ANR-11-LABX-0058 NIE, ANR-10-LABX-0026 CSC). MT acknowledges support by the Heisenberg Program (Grant No. TE 833/2-1) of the German Research Foundation. NL acknowledges support by the Spanish MINECO (Grant No. MAT2015-66888-C3-2-R).
The deformation and the curvature of the C-IPN are considerably large. This is challenging to measure distances with systems like laser. To measure the deformation and related forces of C-IPN with a large curvature, an image processing method is used and analyzes the lateral-view of the C-IPN recorded by the camera. Images are processed with a Sobel operator for edge detection. Since the lights, shadows, or any effects from the background influence the recorded image and cause imperfect detected edges, fragmented edge data are connected based on the algorithms of morphology. Applying the image processing procedure to the whole video, the shape of the C-IPN in each frame is obtained. Thus, the deformation of C-IPN cantilever can be tracked. The last tip displacement is used as the input of the mechanical model proposed in section III.
However, in the scope of this paper, we are mainly interested in results close to the tip of the actuator. This part is indeed in contact with the object. In a second experiment, the C-IPN actuator is in contact with a spring of a known stiffness k = 8. 0mN. mm -. The deformation of the spring is tracked with image processing, and the force that the polymer applies to it is measured. For this experiment, the length of the polymer is L = 10 mm. The input voltage is set to different values in the range of [0. 5 V , 3. 0 V ]. For each value, equation 8 is used to compute the force. The comparison between experimental data and the model is presented in figure  6. The maximum force generated with the polymer is around 2. 0 mN. 95% of this value is reached when the input voltage is set to 2. 5 V.
Tunnelling dI/dV spectra were recorded with Tip A still in a tunnelling contact junction mode on the Pb(111) surface. As presented in Fig. 2b , indeed a µ  change by +/-30 mV shifts the dI/dV spectra accordingly with no deformation. The Tip A to Tip B apex distance can be as large as 6 mm on our instrument with no voltage drop along the superconducting Pb(111) surface while scanning Tip A with an immobile Tip B. Such dI/dV recording certifies that the virtual ground on the Tip B STM electronics is working perfectly through the input transistors differential pair of its I-V convertor. For the data set selectively presented Fig. 3ii  to Fig. 3iv  and with both junction bias set up at 30 mV, a pair of set point currents (  ,   ) corresponds here to a relative     +  resistance ratio of respectively 0.
SELECTION CRITERIA AND THE INTEGRATED PROPERTIES OF SELECTED GALAXIES Our galaxies were selected from the SDSS Data Release 14 (DR14)  (Abolfathi et al. 2018). We adopted the following selection criteria for each galaxy: 1) it has a very high O 32 > 20, which is an indication of either a density-bounded H ii region or a high ionization parameter. 2) it has a compact structure in the SDSS image in order to observe the total flux of the galaxy with the small 2. 5 arcsec COS aperture. 3) it is isolated from other sources to avoid contamination in the HST/COS spectra. 4) it is sufficiently bright in the UV range (GALEX NUV magnitude brighter than 22 mag) to be acquired with COS. In total, we selected the 8 brightest galaxies satisfying the above conditions. The SDSS spectra of the selected galaxies reveal considerably lower oxygen abundances, in the range 12 + log(O/H) = 7.
HST/COS OBSERVATIONS AND DATA REDUCTION HST/COS spectroscopy of the eight galaxies was obtained in program GO 15136 (PI: Y. I. Izotov) during the period January 2018 -February 2019. The observational details are presented in Table  4. The galaxies were acquired by COS near ultraviolet (NUV) imaging. Since our targets are compact but faint, as based on shallow GALEX imaging, a considerable fraction of one orbit was spent per object for deep NUV imaging and reliable acquisition. The NUV-brightest region of each target was centered in the 2. 5 arcsec diameter spectroscopic aperture (Fig. 4 ). We note that acquisition observations failed for J1242+4851. We do not know the reason for that. The acquisition image has a flag raised in the header: EXPFLAG='INVALID CHECK IMAGE'. Possibly, something went wrong during one of the two acquisition exposures.
ACKNOWLEDGEMENTS We thank the anonymous referee for valuable comments. These results are based on observations made with the  NASA/ESA Hubble Space Telescope , obtained from the data archive at the  Space Telescope Science Institute. STScI is operated by the  Association of Universities for Research in Astronomy, Inc. under  NASA  contract  NAS 5-26555. Support for this work was provided by  NASA  through grant number  HST-GO-15136. 002 -Afrom the  Space Telescope Science Institute , which is operated by  AURA, Inc. , under  NASA  contract  NAS 5-26555. Y. I. I. and N. G. G. acknowledge support from the  National Academy of Sciences of Ukraine  (Project No. 0116U003191 ) and by its  Program of Fundamental Research of the Department of Physics and Astronomy  (Project No. 0117U000240 ) of the  National Academy of Sciences of Ukraine.
G. W. has been supported by the  Deutsches Zentrum für Luft-und Raumfahrt (DLR)  through grant number  50OR1720. I. O. acknowledges grants  GACR 14-20666P  and  17-06217Y  of the  Czech National Foundation. Funding for the  Sloan Digital Sky Survey IV  has been provided by the  Alfred P. Sloan Foundation , the  U. S. Department of Energy Office of Science , and the Participating Institutions. SDSS-IV acknowledges support and resources from the  Center for High-Performance Computing at the University of Utah. The SDSS web site is www. sdss. org. SDSS-IV is managed by the  Astrophysical Research Consortium  for the Participating Institutions of the SDSS Collaboration. GALEX is a NASA mission managed by the  Jet Propulsion Laboratory. This publication makes use of data products from the  Wide-field Infrared Survey Explorer , which is a joint project of the  University of California, Los Angeles , and the  Jet Propulsion Laboratory/California Institute of Technology , funded by the  National Aeronautics and Space AdministrationGALEX  is a NASA mission managed by the  Jet Propulsion Laboratory.
We estimate the energy resolution for this dataset based on interpolating the values given for photon energies of 0. 5 and 10 TeV  [2]. 2. Forecast Analysis: A detailed forecast of H. E. S. S. sensitivity, based on Monte Carlo simulations of the expected background, the instrument response functions, and the analysis pipeline  [44]. We perform a likelihood analysis that incorporates both spatial and spectral information, for both signal and background. In this section we show results (reproduced from  [44] ) assuming an Einasto profile for the DM density, although this method is generalizable to alternate DM density profiles. We compute the sensitivity to a pure line and compare that to the prediction of our NLL spectrum. This forecast includes cuts on the data that allow an effective energy resolution of 10% independent of energy.
mass. Another aspect of Fig. 12a  and Fig. 12b  that deserves comment is the fact that the mock limit and the forecast limit performances are similar for the important mass range near M χ ∼ 3 TeV, even though the forecast limit assumes a larger data set. This behavior occurs for two reasons. First, the forecast limit utilizes a more sophisticated background determination method, with less flexibility to incorrectly absorb a signal into the background model, and less sensitivity to fluctuations in the background determination. Consequently, estimating the relative strength of the expected limits in the two analyses is non-trivial. Additionally, the mock analysis is based on observed data, not expected data, and the 2013 dataset from which the mock limit was derived placed a stronger-than-expected upper limit on the flux near 3 TeV  [3] , likely due to a downward fluctuation in the background.
Another way of testing the fixed-bin approach is to explore the extent to which the H. E. S. S. endpoint analysis can be reproduced by using a single endpoint bin with an effective size, and compare that size with the H. E. S. S. resolution. To this end, we provide results computed by rescaling the limit on (or sensitivity estimate for) the line cross section, proportionally to the number of photons in the endpoint bin, and then determine what bin size is needed to reproduce the constraint (or sensitivity estimate) obtained by the endpoint analysis involving the full spectrum. In Fig. 12c , we plot the effective bin size required to reproduce the constraint obtained by the endpoint analysis in the first calculation above, compared with the true H. E. S. S. resolution for the 2013 dataset. We see that the effective bin size varies non-trivially as a function of the DM mass, which could not be predicted without a full calculation of the shape of the distribution.
For example, we found that the non-electroweak-gauge-singlet nature of the incoming and outgoing states led to a non-trivial remaining Glauber phase in the final cross section. We think this would be interesting to explore further in a more general context than that considered here. The H. E. S. S. telescope has collected a large dataset of photons from the Galactic Center region, with an energy resolution of ∼ 10%, permitting sensitive searches for spectral features. Using both a mock H. E. S. S. analysis and a detailed forecasting framework, we studied the importance of using the full photon spectrum computed in this paper as compared with a single endpoint bin approximation when computing experimental limits. We find that the mapping to an effective bin width is a highly non-trivial function of the DM mass.
Acknowledgments We are grateful to  Mikhail Solon  for his collaboration on the leading log result. We thank  Torsten Bringmann ,  Camilo Garcia-Cely , and  Graham Kribs  for useful discussions. Several Feynman diagrams were drawn using [96]. MB is supported by the  U. S. Department of Energy , under grant number  DE-SC-0000232627. TC is supported by the  U. S. Department of Energy , under grant number  DE-SC0018191  and  DE-SC0011640. IM is supported by the  U. S. Department of Energy , under grant number  DE-AC02-05CH11231. NLR and TRS are supported by the  U. S. Department of Energy , under grant numbers  DE-SC00012567  and  DE-SC0013999. NLR is further supported by the  Miller Institute for Basic Research in Science  at the  University of California, Berkeley. IWS is supported by the  Office of Nuclear Physics of the U.
ACKNOWLEDGEMENTS The authors wish to thank  M. Wouters  for crucial discussions in the early stage of this project. P. S, J. B. , A. A. G, and M. R. acknowledge funding from the french  ANR  contract " QFL " ( ANR-16-CE30-0021 ). I. C. J. B. A. L. A. A. acknowledge funding from the  H2020-FETFLAG-2018-2020  project " PhoQuS", (nb 820392 ). A. M. acknowledges funding from the french  ANR  contract " SuperRing " ( ANR-15-CE30-0012 ). J. G. R. acknowledges the  "ETIUDA" program  from the polish NCN.
Acknowledgements. We are indebted to the anonymous referee for the insightful comments that increased the quality of the paper. This work was supported by  ANR   CRADDLE  ( ANR-15-CE31-0004 ) and by  IDEX Sorbonne Paris Cité. We acknowledge the financial support from the  UnivEarthS Labex program of Sorbonne Paris Cité  ( ANR-10-LABX-0023  and  ANR-11-IDEX-0005-02 ). R. H. acknowledges the financial support of  JSPS   Grants-in-Aid  ( JP17J01269 ,  18K13600 ). We thank  J. Dr ążkowska ,  Y. Alibert ,  A. Morbidelli , and  S. Okuzumi  for very constructive comments.
Acknowledgments: I would like to thank the organizers,  Guiseppe Dito  and  Hermano Velten , for the invitation to the " Estate Quantistica " conference held in Scalea (Italy) in June 2018. It is a pleasure to thank  Vincent Vennin  for a long-term collaboration on the issues discussed in this paper and a careful reading of the manuscript. I also would like to thank  Amaury Micheli  for helpful comments. This contribution is dedicated to  Julio Fabris ,  Richard Kerner  and  Winfried Zimdahl  on the occasion of their birthday. I am especially indebted to  Richard Kerner  and  Julio Fabris  for everything I have learned from them.
SuperIso Relic is a public computing program for the calculation of flavour observables and relic density in supersymmetry (MSSM and NMSSM). We present new extensions of the code dedicated to the calculation of dark matter direct and indirect detection constraints from the latest experimental results. Contrary to most of the existing programs, this new version allows the user to consider straightforwardly the uncertainties related to nuclear form factors, dark matter density and velocity, as well as cosmic-ray propagation through the galactic medium. The user thus finds a direct way to calculate "conservative" , "standard" or "stringent" constraints according to the chosen set of uncertainties. Some examplified results showing the impact of such uncertainties are also presented.
Introduction SuperIso Relic v4 1   [1]  is a mixed C / Fortran public program for the calculation of flavour and dark matter observables in the MSSM and NMSSM. It is an extension of the program SuperIso  [2]  devoted to the calculation of flavour observables that also includes the calculation of dark matter (DM) relic density in standard and modified cosmological scenarios  [3]. Numerous new features were implemented since the previous release, including the possibility of multiprocessor calculation of the relic density, and new cosmological models whose impact on the relic density were studied in detail in  [4]. In the following, we present the new extensions for the calculation of direct and indirect detection observables of neutralino (χ) dark matter in the (N)MSSM. The new features include the constraints from recent direct detection experiments (XENON1T  [5] , PICO60  [6] , PANDAX-2  [7] ), Fermi-LAT dwarf spheroidal galaxy constraints  [8]  and limits from AMS-02 antiproton data  [9].
ACKNOWLEDGMENTS The experiments were carried out at the "CANAM" infrastructure, as well as at the infrastructure of "Experimental nuclear reactors  LVR-15  and  LR-0 " in Řež, both supported by the  Ministry of Education, Youth and Sports  under the Projects No. LM2015056  and No. LM2015074 , respectively. The experiment was also supported by the  Grant Agency of the Czech Republic  under the Project No. P108-12G-108. We are grateful to the  PSI  crew  A. Hagel ,  D. Viol ,  R. Erne ,  K. Geissmann ,  O. Morath ,  F. Heinrich , and  B. Blau  for the 7 Be collection at the SINQ cooling system. This research was partially funded by the  European Atomic Energy Community (Euratom) Seventh Framework  Programme No. FP7/2007-2011 under Project  CHANDA  (Grant No. 605203 ). We acknowledge the support provided by the  Federal Ministry of Education and Research (BMBF)  through Grant No.
A computer-controlled data-acquisition and analysis system, using LabVIEW  allows to control the magnet array temperature, the input data of frequency, the duration and number of the series of opening and closing of the shutter. A Matlab  program allows filtering, smoothing, average and analysis of the output signals then the calculation of the characteristic parameters of the system and of the laser power. This new LPM benefits from three main improvements in order to reduce the uncertainties and increase the sensitivity: -a box with glass windows to protect it against movements of air. -rubber absorbers against vibrations. This implies to implement a method to check that the LPM is perfectly horizontal. -a one-dimensional PSD Sitek 1L10 (2 mm × 10 mm) with an amplifier SEEPOS to measure accurately the position of the laser spot that falls upon its active area.
A diaphragm beam shutter with controller is fixed in the front of the laser head and allows to generate a power step. The alignment must be optimized to allow that more than 99 % of the gaussian beam power passes through the two diaphragms. For this end, the alignment is adjusted to reach a maximum value detected by a commercial powermeter placed at the output of the second diaphragm. The coefficient r of the broadband dielectric mirror receiving the laser beam under test is determined from the reflectance versus wavelength data provided by the manufacturer. The mirror is chosen to have a reflectance larger than 0. 99 at the wavelength considered. Of course, the coefficient r should be measured by the calibration service of the LCM LNE-Cnam to ensure a real traceability. The length lm of about 25 mm between the centre of the laser spot on the mirror and the rotation centre of the levitated system is quite complicated to measure.
Acknowledgements We acknowledge useful discussions with  Daniel Butter ,  Franz Ciceri ,  Gianluca Inverso ,  Ralf Köhl ,  Hermann Nicolai ,  Jakob Palmkvist ,  Henning Samtleben  and  Peter West. We thank the  Mitchell foundation  for support during the Brinsop Court meeting 2018. AK acknowledges support from the  Simons Center for Geometry and Physics ,  Stony Brook , and from  École Polytechnique , Paris, where part of this work was carried out. GB and ES thank the  Albert Einstein Institute, Potsdam , for hospitality during the final stages of this work. The work of GB and AK was partially supported by  PHC PROCOPE , projet No  37667ZL  and  DAAD PPP  grant  57316852  (XSUGRA). The work of GB was partially supported by the  ANR  grant  Black-dS-String  ( ANR-16-CE31-0004 ). The work of ES is supported in part by the  NSF  grants  PHY-1521099  and  PHY-1803875.
We ran AIMDEF trajectories with a modified version of the Vienna atomistic simulation package (VASP)  [33, 34, 45, 46] , with either only the electron temperature included and the surface kept fixed, or with both temperatures T el and T ph included and (most) Cu atoms being allowed to move also. Further details are described in Appendix J. Already with single AIMDEF trajectories basic features of the hot-electron (and hot-phonon) driven vibrational dynamics FIG. 6. Probability distribution functions P(X, Y ) at different times, averaged over 20 000 trajectories, for the MDEF-GLO model and a fluence of F = 170 J/m 2. The contours enclose regions with probabilities to find CO with 25% probability (1st Q), 50% probability (2nd Q), and 75% probability (3rd Q). emerge. In Fig. 8 (a) we show how, for the T el -only case, in response to the elevated electronic temperature, the CO molecule acquires kinetic energy (upper panel) and starts to move.
The same, nonlinear two-temperature model with the 170 J/m 2 laser pulse as before [cf. Fig. 2(b) ] was adopted. All calculations were done with a modified version of the Vienna atomistic simulation package (VASP)  [33, 45, 46]. In a first set of calculations (with one example shown in the main text), only the electron temperature was included and the surface atoms were kept fixed. In a second set of calculations (with one example shown in the main text also), both temperatures T el and T ph were included and, besides the CO molecule, also the uppermost four Cu layers were allowed to move. In the T el + T ph calculations, C and O only feel T el , while T ph acts on the upper three Cu layers (the lowest two Cu layers were fixed, and the remaining third-lowest layer was allowed to move, but not exposed to temperature).
ACKNOWLEDGMENTS We thank  T. Klamroth  ( Potsdam ) for fruitful discussions and for his floating FFT transform code. Valuable discussions with  Jörg Meyer (Leiden ) and  Reinhard Maurer  (Warwick) on electronic friction are also acknowledged. This work was supported by the  Deutsche Forschungsgemeinschaft (DFG) , through project  Sa 547/8-3. J. I. J. and M. A. acknowledge the  Spanish Ministerio de Economía y Competitividad  [Grant No. FIS2016-76471-P (AEI/FEDER , UE)] and  Gobierno Vasco-UPV/EHU  project  IT1246-19. I. L. was supported by the  European Union  through the  European Regional Development Fund-the Competitiveness and Cohesion Operational Programme  ( KK. 01. 1. 1. 06 ).
tional waves and high-energy neutrinos from astrophysical transients with minimal assumptions using data from Advanced LIGO from its first observing run O1, and data from the Antares and IceCube neutrino observatories from the same time period. We focused on candidate events whose astrophysical origin could not be determined from a single messenger. We found no significant coincident candidate, which we used to constrain the rate density of astrophysical sources dependent on their gravitational wave and neutrino emission processes.
2011; Adrián-Martínez et al. 2013a; Aartsen et al. 2014a ). In addition, searches have been carried out for the neutrino counterparts of binary black hole mergers detected during Advanced LIGO's first  (Adrián-Martínez et al. 2016a; Albert et al. 2017a; Gando et al. 2016; Aab et al. 2016; Abe et al. 2016; Agostini et al. 2017)  and second observing runs  (Albert et al. 2017b; Agostini et al. 2017) , and BNS merger GW170817/GRB 170817A  (Albert et al. 2017c; Abe et al. 2018). In this paper we present a multi-messenger search for common transient sources of GWs and high-energy neutrinos using GW data from Advanced LIGO's first observing run (O1) and neutrino data from both Antares and IceCube. The paper is organized as follows. In Section 2, we describe the GW and neutrino observatories, and the data used in this analysis.