dataesr/scientific-paragraphs-categorization huggingface dataset:
The benzene peaks remain at the same position up to 1 ML coverage and have an asymmetrical shape that is typical for diffraction patterns of two-dimensional poly-crystalline systems. 37, 38 The asymmetric shape of the diffraction peaks is caused by the random orientation of crystallographic domains, where the normal of the domain remains parallel to the surface normal. For a more detailed analysis of the sub-monolayer and monolayer structures we have simulated neutron diffraction patterns of a flat lying monolayer using the software package nxpattern, which allowed us to adjust a number of parameters manually. 39 The results of such a manual structural refinement are displayed in Fig. 3. The positions of the atoms in the deuterated benzene molecule were based on neutron diffraction data for deuterated benzene molecules.
Acknowledgments The  Agence Nationale de la Recherche  (Projet  ANR-11-INTB-1001 ) is acknowledged for its financial support. Part of the work presented in this review is a result of the cooperation within the European C-MAC and was possible thanks to the access to HPC resources of the  French institute IDRIS (Institut du Développement et des Ressources en Informatique Scientifique)  under allocation 99642 made by  GENCI  ( Grand Equipement National de Calcul Intensif ).
The exotic nucleus 8 He is investigated by means of the measurement of the angular distributions of the elastic channel and the 6 He and 4 He fragment yields produced in the collision with a 208 Pb target at two energies around the Coulomb barrier, 16 and 22 MeV. The experiment was performed at the GANIL-SPIRAL facility, with the aim of extracting information about the structure of 8 He and the relevant reaction mechanisms. In this contribution, details of the experimental setup and preliminary data on elastic cross sections are reported.
We present the discovery of a candidate multiply transiting system, the first one found in the CoRoT mission. Two transit-like features with periods of 5. 11 and 11. 76 d are detected in the CoRoT light curve around a main sequence K1V star of r = 15. 1. If the features are due to transiting planets around the same star, these would correspond to objects of 3. 7 ± 0. 4 and 5. 0 ± 0. 5 R ⊕ , respectively. Several radial velocities serve to provide an upper limit of 5. 7 M ⊕ for the 5. 11 d signal and to tentatively measure a mass of 28 +11 -11 M ⊕ for the object transiting with a 11. 76 d period. These measurements imply low density objects, with a significant gaseous envelope. The detailed analysis of the photometric and spectroscopic data serves to estimate the probability that the observations are caused by transiting Neptune-sized planets as much as over 26 times higher than a blend scenario involving only one transiting planet and as much as over 900 times higher than a scenario involving two blends and no planets.
CoRoT observations The target star CoRoT-24 was observed on the detector E1 of the CoRoT satellite during its second Long Run pointing at the direction opposite to the approximate galactic center ("anticenter" in the CoRoT jargon). The observations lasted from 16 Nov. 2008 until 8 March 2009, covering a total span of 111. 64 days. The target is faint, having a r mag of 15. 1 (see Table  3 ). A transit signal with a period of 11. 76 d was detected in the framework of the alarm mode  (Surace et al. 2008)  close to the end of the observations, and thus the last 10. 7 days of the run are sampled with a 32 s cadence, instead of the nominal 512 s of the rest of the observations. The EN2 data product 1 consists of 45 593 data points, out of which 28 672 are sampled with a 32 s cadence. The aperture used on-board is a monochromatic one, since the telemetry only allows for a recovery of chromatic information on a limited number of targets.
The orbital solution was calculated using the general nonlinear least squares fitting program GaussFit  (Jefferys et al. 1988 ). This resulted in K b = 0. 80 ± 3. 0 m s -1 and K c = 5. 2 ± 3. 2 m s -1. This suggests that any short-term variations in the RV measurements are dominated by CoRoT-24c. We then fitted the RV measurements using a variation of the floating offset fitting technique employed in detecting CoRoT-7b  (Hatzes et al. 2011). The RV data were divided into eleven subset data, four for Keck and seven for HARPS. The time span of each data subset ranged from two to seven days, with a median value of five days. On several nights there were three Keck RV measurements and for the fit we used the median value. An orbital fit was made keeping the period and phase fixed to transit values, but allowing the K-amplitude and zero-point offsets of the subset data to vary.
Alternatively, these companions could be detected spectroscopically. Despite being challenging for ground-based observations, the progress in the recent years have shown that it might be possible to detect the transits of CoRoT-24c (and probably also CoRoT-24b) and thus refine the ephemeris. A more intense radial velocity campaign devoted to CoRoT-24 might result in a more precise measurement of the masses of the planets, and thus their densities. These data could serve to better model the long period signal seen in the radial velocities, and to evaluate the effects of additional planetary companions in the system not considered in this work. Since the star shows photometric activity at the 2% level and a period of around 29 days, the observing strategy should be designed in order to minimize or to understand better the effect of the activity on the measured masses.
Acknowledgements. We wish to thank the  ESO  staff for their support and for their contribution to the success of the  HARPS  project and operation at  ESO La Silla Observatory. Some of the data presented are from observations made with the IAC80 operated at  Teide Observatory  on the island of Tenerife by the  Instituto de Astrofísica de Canarias. The team at the IAC acknowledges support by grants  ESP2007-65480-C02-02  and  AYA2010-20982-C02-02  of the  Spanish Ministry of Science and Innovation (MICINN). The CoRoT/Exoplanet catalogue (Exodat) was made possible by observations collected for years at the  Isaac Newton Telescope (INT) , operated on the island of  La Palma  by the  Isaac Newton group in the Spanish Observatorio del Roque de Los Muchachos  of the  Instituto de Astrofísica de Canarias.
The  German CoRoT team (TLS and University of Cologne ) acknowledges  DLR  grants  50OW0204 ,  50OW0603 , and  50QM1004. The French team wishes to thank the  CNES  and the  French National Research Agency  ( ANR-08-JCJC-0102-01 ) for their continuous support to our planet search program. The Swiss team acknowledges the  ESA PRODEX program  and the  Swiss National Science Foundation  for their continuous support on CoRoT ground follow-up. R. Alonso acknowledges support from  Spanish Ministry  through its  Ramón y Cajal program   RYC-2010-06519. A. S. Bonomo acknowledges a  CNES grant. S. Aigrain  acknowledges  STFC  grant  ST/G002266. M. Gillon  acknowledges support from the  Belgian Science Policy Office  in the form of a Return Grant. M. Endl,  W. D. Cochran  and  P. J. MacQueen  were supported by  NASA Origins of Solar Systems  grant  NNX09AB30G.
T. Mazeh  acknowledges support from the  Israeli Science Foundation  (grant No. 655/07 ). A. Santerne acknowledges support from the  European Research Council/European Community  under the  FP7 through Starting Grant  agreement number  239953. This research has made use of the SIMBAD database, operated at the  CDS, Strasbourg, France , and of  NASA 's Astrophysics Data System. Part of the data presented herein were obtained at the  W. M. Keck Observatory  from telescope time allocated to the  National Aeronautics and Space Administration  through the agency's scientific partnership with the  California Institute of Technology  and the  University of California. The Observatory was made possible by the generous financial support of the  W. M. Keck Foundation.
Acknowledgments We would like to thank  Benjamin Basso ,  Pedro Vieira  and  Evgeny Sobko  for discussions. J. P. and V. G. wish to thank  CERN  for the great hospitality during our visit in the spring of 2013 when this work was initiated. M. S. C and V. G also thank IPMU at  Tokyo University  for the great hospitality during the progress of this work. J. P. is grateful to  Perimeter Institute  for the hospitality in July of 2013. The research leading to these results has received funding from the  [European Union ]  Seventh Framework Programme  [ FP7-People-2010-IRSES ] under grant agreements No  269217 ,  317089. This work was partially funded by the grant  CERN/FP/123599/2011  and by the  Matsumae International Foundation in Japan. Centro de Fisica do Porto  is partially funded by the  Foundation for Science and Technology of Portugal (FCT).
al (DSSV)  [9, 10] , resulting in an integral ∆G [0. 05,0. 2] dssv08 = 0. 005 +0. 129  -0. 164 in the Bjorken-x range [0. 05, 0. 2]. As detailed in  [20] , the full x range probed by the PHENIX A π 0 LL measurements is [0. 02, 0. 3]. The A η LL has also been measured  [17] , but it has not yet been used in global fits. One reason for this is that existing e + + e -data does not constrain η fragmentation functions as well as those for the pions  [24, 25]. However, PHENIX has released results for the η/π 0 cross section ratio in p+p collisions  [17, 26]  with systematic uncertainties much smaller than on either cross section measurement alone. Future inclusion of this ratio in global fits could be used to circumvent this issue with the fragmentation functions. In this paper, we present measurements of A LL in π 0and η-meson production in longitudinally polarized p+p collisions at √ s = 200 GeV, based on data collected in 2009, which approximately doubles the statistics in the √ s = 200 GeV PHENIX neutral meson A LL dataset  [17, 20]  and extends the measured p T range.
This polarimeter can determine both the relative magnitude of the polarization and any variation across the width of the beam  [28]. This measurement was normalized by comparing its average over the entire dataset to the average of an absolute polarization measurement from the second polarimeter, which is based on scattering of the beam with a continuously-running polarized hydrogen gas-jet target  [29]. For 2009 √ s = 200 GeV running, the average beam polarizations were P B = 0. 56 for the blue beam and P Y = 0. 55 for the yellow beam, for a product P B P Y = 0. 31. The overall relative scale uncertainty on the product P B P Y was 6. 5%, with 4. 8% of that considered correlated with the polarization uncertainties from RHIC runs in 2005 and 2006  [30].
Luminosity Monitors PHENIX has two luminosity monitors with which to normalize the luminosity variations between same and opposite helicity bunch crossings. The main luminosity monitor is the beam-beam counter (BBC)  [31] , which comprises two arms located |z| = 144 cm from the interaction-point (IP) along the beam axis, covering a pseudorapidity range of 3. 1 < |η| < 3. 9. Each arm has 64 quartz crystal Čerenkov radiators attached to photomultiplier tubes. The BBC also functions as the minimumbias (MB) collision trigger for this dataset, with a requirement that at least one photomultiplier tube fire in each arm and that the timing of the hits reconstructs to a collision with a z-vertex within 30 cm of the nominal IP. The yield of MB triggers in crossings where the data acquisition system was ready to take data was used to determine the luminosity.
III. DATA ANALYSIS A. Event and Photon Selection Events used in this analysis require a MB trigger in coincidence with a high energy trigger in the EMCal. An offline vertex cut is applied, which requires that the vertex reconstructed using the BBC be within |z| = 30 cm of the nominal IP. On the order of two billion events passing this offline cut were analyzed. Photon candidates are selected from all energy deposit clusters in the EMCal. A minimum energy of 100 MeV in PbSc and 200 MeV in PbGl is required to reduce the impact of noise in the detector. Clusters centered on towers that are markedly noisy or dead, or centered on towers neighboring a markedly noisy or dead tower, are discarded. Clusters centered within two towers of the edge of each EMCal sector's acceptance are also excluded. A major source of background in the photon candidate sample are charged hadrons, which are removed by three cuts based on shower shape, time of flight (ToF) and association with hits in the PC3.
Polarization Direction Another hardware based uncertainty that has been present in all longitudinal RHIC runs is that of the remaining transverse polarization component after the beams have passed through the Spin Rotator magnets, discussed in detail in Section II A. The total resultant scaling uncertainty in the longitudinal component of P B P Y , which applies globally to the 2009 dataset, is ( +0. 026 -0. 042 ). This can be added in quadrature to the polarization scale uncertainty listed in Section II A, and the results of that combination are given in Figures  10  and 11  as well as Tables IV and V.
Since the background fraction w BG is small at high p T , this effect is negligible in the final result. The overestimation of uncertainties at low p T is due to conservative calculation of uncertainties in the cases where triggers were scaled to match the data acquisition bandwidth. For the π 0 , the largest overestimation was about 6% of the statistical uncertainty, for the signal region in the lowest p T bin. Measurements of single-spin asymmetries, in which the polarization of one beam is summed over, were also performed. Such asymmetries, if physical, would be parity violating. As expected for a parity-conserving QCD process, they were found to be consistent with zero. Comparisons were also made between the two different electromagnetic calorimeter technologies. In these comparisons, both double and single-spin asymmetries were measured separately in the PbSc and PbGl, and no inconsistency between the two detectors was found.
The results of that analysis, which yields a much more accurate determination of ∆g(x), are compared with A π 0 LL in Fig. 12 (a). We also ran an updated version of the dssv08 analysis to include final versions of the RHIC data through 2006  [18, 20, 22]  along with the final A π 0 LL results presented here. We obtained ∆G Systematic uncertainties for the RHIC dataset were not included in the dssv08 analysis. However, the PHENIX relative-luminosity systematic uncertainty now exceeds the statistical uncertainty on A π 0 LL in the lowest p T bins. To understand the impact of this on the fit result, we shifted the PHENIX √ s = 200 GeV data up and down by the systematic uncertainties given in the final column of Table VI, while ignoring the systematic uncertainties of all other data sets. As demonstrated in Fig.
ACKNOWLEDGMENTS We thank the staff of the  Collider-Accelerator and Physics Departments at Brookhaven National Laboratory  and the staff of the other PHENIX participating institutions for their vital contributions. We acknowledge support from the  Office of Nuclear Physics in the Office of Science of the Department of Energy , the  National Science Foundation ,  Abilene Christian University Research Council, Research Foundation of SUNY, and Dean of the College of Arts and Sciences, Vanderbilt University (U. S. A) ,  Ministry of Education, Culture, Sports, Science, and Technology  and the  Japan Society for the Promotion of Science (Japan) ,  Conselho Nacional de Desenvolvimento Científico e Tecnológico and Fundação de Amparo à Pesquisa do Estado de São Paulo (Brazil) ,  Natural Science Foundation of China (P.
Acknowledgements We acknowledge financial support from the  National Basic Research Program of China  (Grants No. 2012CB927401 ,  2011CB921902 ,  2013CB921902  and  2011CB922200 ),  NSFC  (Grants No. 11374206 ,  91021002 ,  11274228 ,  10904090 ,  11174199  and  11134008 ), GLL acknowledges support by the  2D - NANOLATTICES  project of the  Future and Emerging Technologies (FET) program  within the  7th Framework Program for Research  of the  European Commission , under  FET  Grant No. 270749. DQ acknowledges support from the  Top-notch Young Talents Program. CLG acknowledges support from  Shu Guang  project supported by the  Shanghai Municipal Education Commission. PV acknowledges support by the  Deutsche Forschungsgemeinschaft (DFG)  under Grant No. VO1261/3-1.
Acknowledgments DO acknowledges financial support by the  European Research Council  starting investigator grant  SINSLIM 258221 , by the  I-CORE Program of the Planning and Budgeting Committee  and the  Israel Science Foundation  and from the  Laboratoire Européen Associé NaBi  between the CNRS and the  Weizmann Institute. VE  acknowledges financial support by the  Human Frontier Science Program  ( RGP0013/2010 ), the  'Fondation pour la Recherche Mèdicale' (FRM Èquipe)  and the  'Agence Nationale de la Recherche ' (grants  ANR-12-BSV5-0011-01 ,  Neurholog ) and by the  France-BioImaging  infrastructure supported by the  French National Research Agency  ( ANR-10-INSB-04 , Investments for the future). OH acknowledges the program  Nanotechnologies France-Israël  for financial support.
A search is presented for dark matter pair production in association with a W or Z boson in pp collisions representing 20. 3 fb -1 of integrated luminosity at √ s = 8 TeV using data recorded with the ATLAS detector at the Large Hadron Collider. Events with a hadronic jet with the jet mass consistent with a W or Z boson, and with large missing transverse momentum are analyzed. The data are consistent with the standard model expectations. Limits are set on the mass scale in effective field theories that describe the interaction of dark matter and standard model particles, and on the cross section of Higgs production and decay to invisible particles. In addition, cross section limits on the anomalous production of W or Z bosons with large missing transverse momentum are set in two fiducial regions.
1. The Tevatron and LHC collaborations have reported limits on the cross section of pp → χ χ + X where X is a hadronic jet  [2] [3] [4]  or a photon  [5, 6]. Other LHC data have been reinterpreted to constrain models where X is a leptonically decaying W  [7]  or Z boson  [8, 9]. In each case, limits are reported in terms of the mass scale M * of the unknown interaction expressed in an effective field theory as a four-point contact interaction  [10] [11] [12] [13] [14] [15] [16] [17] [18]. In the models considered until now, the strongest limits come from monojet analyses, due to the large rate of gluon or quark initial-state radiation relative to photon, W or Z boson radiation. The operators studied in these monojet and monophoton searches assume equal couplings of the dark matter particles to up-type and down-type quarks [C(u) = C(d)].
The ATLAS detector  [19]  at the LHC covers the pseudorapidity [20] range |η| < 4. 9 and the full azimuthal angle φ. It consists of an inner tracking detector surrounded by a thin superconducting solenoid, electromagnetic and hadronic calorimeters, and an external muon spectrometer incorporating large superconducting toroidal magnets. A three-level trigger system is used to select interesting events for recording and subsequent offline analysis. Only data for which beams were stable and all subsystems described above were operational are used. Applying these requirements to pp collision data, taken at a center-of-mass energy of √ s = 8 TeV during the 2012 LHC run, results in a data sample with a time-integrated luminosity of 20. 3 fb -1. The systematic uncertainty on the luminosity is derived, following the same methodology as that detailed in Ref.
acknowledge the support of ANPCyT, Argentina; YerPhI, Armenia; ARC, Australia; BMWF and FWF, Austria; ANAS, Azerbaijan; SSTC, Belarus; CNPq and FAPESP, Brazil; NSERC, NRC, and CFI, Canada; CERN; CONICYT, Chile; CAS, MOST, and NSFC, China; COLCIENCIAS, Colombia; MSMT CR, MPO CR, and VSC CR, Czech Republic; DNRF, DNSRC, and Lundbeck Foundation, Denmark; EPLANET, ERC, and NSRF, European Union; IN2P3-CNRS, CEA-DSM/IRFU, France; GNSF, Georgia; BMBF, DFG, HGF, MPG, and AvH Foundation, Germany; GSRT and NSRF, Greece; ISF, MINERVA, GIF, DIP, and Benoziyo Center, Israel; INFN, Italy; MEXT and JSPS, Japan; CNRST, Morocco; FOM and NWO, Netherlands; BRF and RCN, Norway; MNiSW and NCN, Poland; GRICES and FCT, Portugal; MNE/IFA, Romania; MES of Russia and ROSATOM, Russian Federation; JINR; MSTD, Serbia; MSSR, Slovakia; ARRS and MIZ Š, Slovenia; DST/NRF, South Africa; MINECO, Spain; SRC and Wallenberg Foundation, Sweden; SER, SNSF, and Cantons of Bern and Geneva, Switzerland; NSC, Taiwan; TAEK, Turkey; STFC, the Royal Society, and Leverhulme Trust, United Kingdom; U.
Acknowledgment. We would like to thank  J. Ablinger ,  S. Alekhin ,  S Moch  and  C. Schneider  for discussions. This work has been supported in part by  DFG   Sonderforschungsbereich Transregio 9, Computergestützte Theoretische Teilchenphysik , by the  EU Networks LHCPHENOnet   PITN-GA-2010-264564  and  HIGGSTOOLS PITN-GA-2012-316704 , and by  FP7 ERC Starting  Grant  257638 PAGAP.
In this paper, we explore the impact of Dark Matter-photon interactions on the CMB angular power spectrum. Using the one-year data release of the Planck satellite, we derive an upper bound on the Dark Matter-photon elastic scattering cross section of σ DM-γ ≤ 8×10 -31 (m DM /GeV) cm 2 (68% CL) if the cross section is constant and a present-day value of σ DM-γ ≤ 6 × 10 -40 (m DM /GeV) cm 2 (68% CL) if it scales as the temperature squared. For such a limiting cross section, both the B-modes and the T T angular power spectrum are suppressed with respect to ΛCDM predictions for 500 and 3000 respectively, indicating that forthcoming data from CMB polarisation experiments and Planck could help to constrain and characterise the physics of the dark sector. This essentially initiates a new type of dark matter search that is independent of whether dark matter is annihilating, decaying or asymmetric.
IV. CONCLUSION We have studied the effects of introducing an interaction between DM and photons on the evolution of primordial matter fluctuations and in particular, the CMB temperature and polarisation power spectra. By comparing the T T and EE components in the presence of a DM-γ coupling with the one-year data release from Planck, we have set a stringent constraint on the elastic scattering cross section of σ DM-γ ≤ 8 × 10 -31 (m DM /GeV) cm 2 (68% CL), assuming it is constant at late times. This bound is an order of magnitude stronger than the previous work of Ref. [33] , where a limit was placed by comparing the temperature anisotropy spectrum with ΛCDM predictions (before any experimental results were published). For a heavy DM particle (∼ TeV), the maximal cross section is too large to exclude the possibility that DM has significant interactions with photons, while for light DM particles (∼ MeV), the cross section is of the order typically expected for weak interactions.
If instead, the cross section is proportional to the temperature squared, we obtain a significantly tighter present-day bound of σ DM-γ ≤ 6 × 10 -40 (m DM /GeV) cm 2 (68% CL), giving a weaker constraint in the past. We note that an even stronger result could be achieved using forthcoming data on the B-modes and measurements of the T T spectrum at very high , provided an excellent knowledge of the foregrounds. We expect these limits to be weaker than those from the matter power spectrum, when combined with data from large-scale structure surveys and Lyman-α constraints (at present, a limit can only be set by analogy with collisionless WDM). However, CMB constraints will be important to compare to since they do not depend on the non-linear evolution of the matter fluctuations. Importantly, we have shown that one can effectively use cosmological data to restrict the allowed region of parameter space for DM interactions, independently of any theoretical prejudice.