dataesr/scientific-paragraphs-categorization huggingface dataset:
These effects lead to a broadening of the photon transverse momentum distribution in this approach  [28]. The scale uncertainties on these predictions vary from about 31% at 30 < p γ T < 40 GeV to about 50% in the highest p γ T bin. Table I also contains predictions from the pythia  [19]  MC event generator with the cteq6. 1L PDF set. It includes only 2 → 2 matrix elements (ME) with gb → γb and q q → γg scatterings (defined at LO) and with g → b b splitting in the parton shower (PS). We also provide predictions of the sherpa MC event generator  [18]  with the cteq6. 6M PDF set  [27]. For γ + b production, sherpa includes all the MEs with one photon and up to three T. The uncertainties on the data points include statistical and systematic contributions added in quadrature. The measurements are compared to the NLO QCD calculations  [4]  using the cteq6.
Absolute deflection measurement. To determine the absolute position of the antiproton fringe pattern (parameter a in Fig. 2b ), we conduct a comparison with the measurement with light. The results are represented in Fig. where the detected intensity is indicated by the red shading. The alignment is achieved by overlaying the contact patterns as depicted on the right of Fig. 3b. The moirepattern can now be directly compared with the Talbot-Lau pattern (left of Fig. 3b ) to extract a possible deflection. For the quantitative analysis, we extract the orientation of the antimatter (Rayleigh test) and light patterns (Fourier transformation as the data is discrete in space). We find that the relative angle of the two antiproton patterns, which are 15 mm apart, deviates from the angle measured between the two corresponding light patterns by Dy ¼ 0.
Acknowledgements This work was supported by:  DFG  research grant,  excellence initiative of Heidelberg University, ERC  under the European Union's  Seventh Framework Program  ( FP7/2007-2013)/ERC Grant  agreement no. (291242),  Austrian Ministry for Science, Research and Economy, Research Council of Norway, Bergen Research Foundation ,  Istituto Nazionale di Fisica Nucleare (INFN-Italy ). J. S. wishes to acknowledge the  Swiss National Science Foundation. Technical support by the  Cockcroft Institute ,  U. K. is gratefully acknowledged. We are grateful to the  CERN AD team  for providing the antiproton beam.
We present the first Public Data Release (PDR-1) of the VIMOS Public Extragalactic Survey (VIPERS). It comprises 57 204 spectroscopic measurements together with all additional information necessary for optimal scientific exploitation of the data, in particular the associated photometric measurements and quantification of the photometric and survey completeness. VIPERS is an ESO Large Programme designed to build a spectroscopic sample of 100 000 galaxies with i AB < 22. 5 and 0. 5 < z < 1. 2 with high sampling rate ( 45%). The survey spectroscopic targets are selected from the CFHTLS-Wide five-band catalogues in the W1 and W4 fields. The final survey will cover a total area of nearly 24 deg 2 , for a total comoving volume between z = 0. 5 and 1. 2 of 4 × 10 7 h -3 Mpc 3 and a median galaxy redshift of z 0.
8. The release presented in this paper includes data from virtually the entire W4 field and nearly half of the W1 area, thus representing 64% of the final dataset. We provide a detailed description of sample selection, observations and data reduction procedures; we summarise the global properties of the spectroscopic catalogue and explain the associated data products and their use, and provide all the details for accessing the data through the survey database (http://vipers. inaf. it) where all information can be queried interactively.
A-0886 and partly 070. A-9007. Also based on observations obtained with MegaPrime/MegaCam, a joint project of CFHT and CEA/DAPNIA, at the Canada-France-Hawaii Telescope (CFHT), which is operated by the National Research Council (NRC) of Canada, the Institut National des Sciences de l'Univers of the Centre National de la Recherche Scientifique (CNRS) of France, and the University of Hawaii. This work is based in part on data products produced at TER-APIX and the Canadian Astronomy Data Centre as part of the Canada-France-Hawaii Telescope Legacy Survey, a collaborative project of NRC and CNRS. The VIPERS web site is http://vipers. inaf. it/. excellent statistics, large-scale structure studies have been extended well into the linear regime (r 10 h -1 Mpc) while at the same time having a detailed characterization of small-scale clustering and its dependence on galaxy properties like luminosity, colour and morphology (e.
8 in terms of the distributions of fundamental properties such as luminosity, colours and stellar mass, tracing their evolution with cosmic time  (Davidzon et al. 2013; Fritz et al. 2013). 4. To reconstruct the density field at z 0. 8 in order to: (a) determine the bias parameter and its evolution b(z)  (Branchini et al. , in preparation) ; (b) quantify at these redshifts the relationship between galaxy properties and local environment, elucidating the role of mass and environment in the evolution of galaxies. 5. To provide the community with an unprecedented spectroscopic database at 0. 5 < z < 1. 2, including extensive information on galaxy physical properties. The latter is made possible by combining the spectral information with the CFHTLS five-band magnitudes on which the survey is based 1 (Goranova  et al.
2009), plus additional ancillary data in the UV and infrared bands (GALEX, UKIDSS, VISTA, SWIRE, VLA, XMM-LSS), enabling to derive Spectral Energy Distribution information  (Marchetti et al. 2013 , Davidzon et al. 2013 ) and automatic galaxy/AGN/stellar classification  (Małek et al. 2013). Although carried out within the standard (proprietary) scheme of the ESO Large Programmes, VIPERS was conceived from its start as a public survey, with the clear idea that the range of science that will be performed by the community should greatly exceed the core analyses described above. The set of data that is described in this paper and made public with the VIPERS Public Data Release 1 (PDR-1), is the same used for all papers of the first VIPERS science release of March 2013. Several aspects of the survey construction and the data are also discussed in  Guzzo et al.
Star-galaxy separation and target definition VIPERS was conceived in 2007, focusing on the study of clustering and redshift-space distortions at z 0. 5 -1. 2, but with a desire to enable broader goals involving large-scale structure and galaxy evolution. The survey design was also strongly driven by the specific features of the VIMOS spectrograph, which has a relatively small field of view compared to fibre-fed instruments ( 18 × 16 arcmin 2  ), but a larger yield in terms of redshifts per unit area (up to 1000 spectra per exposure: Le  Fèvre et al. 2003). The VIPERS overall sky coverage and field layout is shown in Figure  1 ; the solid red line delimits the planned area, while the black dots show the spectroscopically observed objects. Table  1  shows the area planned in each of the two survey fields as well as the area already spectroscopically covered, which is the subject of the current data release.
6 ≤ (u -g) < 1. 2 ∧(g -r) > 0. 5(u -g) + 0. 036 (g -r) < 1 ∧ 0. 6 ≤ (u -g) < 2. 6 ∧(gr) < 0. 5(ug) + 0. 214 (gr) < 1 ∧ (ug) > 2. 6. (2) These criteria were calibrated on the VVDS point-like objects brighter than i AB = 21, and we expected a sample with a completeness of 87. 5% and with a stellar contamination of 36%. These percentages were not confirmed by the actual data at the end of the first observing season, indicating a significantly higher than expected contamination from stars. While investigating the origin of this discrepancy, we decided to revise criteria towards a more restrictive definition, following which an AGN candidate must satisfy CC1 (equation 2) and : CC2 :          (u -g) < 0. 6 ∧ -0. 2 < (g -i) < 1 0. 6 ≤ (u -g) < 1 ∧ -0. 2 < (g -i) < 0. 2 (u -g) ≥ 1 ∧ (g -i) < 0.
VLT-VIMOS Observations The VIPERS survey is being performed in the framework of the ESO Large programmes and is carried out using VIMOS on 'Melipal', the Very Large Telescope (VLT) Unit 3  (Le Fèvre et al. 2003). VIMOS (Visible Imager Multi Object Spectrograph) makes use of slits cut out from masks. Its field of view of 18 × 16 arcmin 2 is divided into four quadrants, each having an area of 7 × 8. 1 arcmin 2. Each quadrant corresponds to an independent spectrograph and the four spectrographs observe in the same configuration for the same exposure time. The standard VIMOS observing procedure requires the acquisition of a direct image, which is used for mask preparation with the vmmps software  (Bottini et al. 2005)  distributed by ESO: vmmps assigns the slit length taking into account object dimensions and sky subtraction regions as specified by the user.
Spectroscopic observations and data reduction 4. 1. Quality of VIMOS raw data VIPERS observations started in September 2008 and have proceeded at a steady rate since then. The median airmass of PDR-1 data is 1. 14, and remains below 1. 3 in 90% of the exposures. To match the slit width and minimize slit losses, the requested maximum seeing was 1 arcsec. Figure  3  shows the seeing distribution as measured from the scientific exposures. The median seeing is 0. 8 arcsec and 90% of exposures have a seeing below 1. 05 arcsec. 85% of observations have been carried out in dark time, while the remaining fraction either had a moon illumination below 20%, or a moon distance above 70 deg. In spring/summer 2010, VIMOS was upgraded with new red-sensitive CCDs in each of the 4 channels  (Hammersley et al.
We then run EZ  (Garilli et al. 2010 ) on all 1D extracted spectra for a first automatic redshift measurement. All data reduction has been centralised in our data reduction and management centre at INAF -IASF Milano. When ready, the fully reduced data are made available to the team within a dedicated database. The full management of these operations within the EasyLife environment is described in  Garilli et al. (2012).
Statistical confidence levels corresponding to redshift flags A first estimate of the actual, statistical confidence level of the redshift flags associated to our redshift measurements has been presented in  Guzzo et al. (2013)  using the available duplicated observations mentioned above. These results are reported in the top part of Table  2. Here we extend and complement this analysis, making use of external measurements. The confidence level of a given Flag class (e. g. Flag 3+4) from VIPERS, which we call survey X for simplicity, can be estimated from the fraction of measurements in agreement among those galaxies observed independently by another survey, Y, with comparable or better reliability. We note that while this latter aspect is easy to evaluate when comparing VIPERS to a survey like VVDS, which was observed with a very similar setup, evaluating the intrinsic redshift reliability of a very different data set, for which additionally we may only have literature information, is less straightforward.
Colour Sampling Rate The Colour Sampling Rate (CSR) defines the completeness of galaxies detected in spectroscopy with respect to a purely i < 22. 5 magnitude-limited sample. It accounts for the missed galaxies at the boundaries of the colour-based redshift selection criterion. Such incompleteness affects only galaxies with redshift close to the nominal lower limit of z 0. 5. The adopted colour criteria were in fact calibrated using the purely flux limited data of the VVDS survey  (Guzzo et al. 2013 ). These calibration tests show that in the (ri) vs (ug) plane, the distance of a galaxy from the adopted threshold is a monotonic function of redshift. As such, the CSR is expected to be close to a step function changing from 0 to 1 around the nominal redshift threshold of z = 0. 5. To compute the CSR, we have used the VVDS Deep and Wide datasets, which not only are purely flux limited surveys but also share the same CFHTLS photometry of VIPERS.
Public Data Release and Database Access The data of the first VIPERS Public Data Release (PDR-1) are available at http://vipers. inaf. it. The release comprises: -Spectroscopic catalogue, described in Table  8. -Parent photometric catalogue, described in Table  9. It contains all sources in the CFHTLS catalogue falling within the surveyed area and having i AB < 24. 0. -Photometric masks, as described in  Guzzo et al. (2013). The photometric mask marks regions of the VIPERS survey in which the target selection may be affected by poor photometric quality in the parent CFHTLS catalogue. These regions should be excluded from scientific analyses. The fraction of the area lost is 2. 4% for the W1 field and 3. 0% for the W4 field. The photometric mask is provided separately for the two VIPERS fields W1 and W4.
1). have changed due to a deeper look into the more problematic spectra. As a consequence, for this release we have re-computed also the TSR, SSR and CSR. However we underline that these differences are too small to affect the scientific results contained in previous papers. A full release of the one dimensional fully calibrated spectra, together with the spectroscopic features measurements, is foreseen in 2014. Catalogues are distributed in three different forms: -A single tar file containing the full release -A web interface connected to the VIPERS (see next section) database (free registration required), which allows to perform SQL selections through an ergonomic, easy to use interface -At a later stage, data will also be queryable via the Virtual Observatory.
VIPERS database web interface The WEB interface to the VIPERS data base allows one to perform queries using a confortable User Interface. Once logged in, the user is presented with the list of tables to be queried. Queries can be applied to a single table, or to a combination of tables: if more than one table is selected, the query can be conducted either in parallel and independently on each of the tables, or joining all tables, using the object ID as joining field. Extensive information on the content of each table can be accessed by clicking on the table name, while generic help on the usage of the interface is available clicking on the HELP button on the left. Queries can be of type Simple or Advanced. The Simple query allows one to select all objects within a sky region (query by Position) or to retrieve objects within a user specified list (query By Input List), or to select objects satisfying simple selection conditions (query By Parameters).
The By Parameter form allows one to set many selection conditions as ranges, equality or likeness, for example extragalactic objects (zspec>0) with a secure redshift flag (zflg between 2 and 10) observed in epoch 2. Conditions can be imposed on any column of the selected tables and all the conditions are joined together with an AND syntax. The Advanced query panel page has been thought to provide a more flexible tool for expert users. It allows to insert formulas in the selection statement, to define the selection condition in a customizable complex way, to sort the output using a specified data column order and it also allows one to limit the result output. The query output page allows one to directly inspect the query results, to make simple simple plots for quick statistical inspection of the results and to save results into ASCII files, VOTables or FITS binary tables.
Summary We have presented here the first first Public Data Release (PDR-1) of the VIPERS survey, which includes 57 204 spectroscopic measurements of galaxies, AGN and stars. Complementing the general description given in  Guzzo et al. (2013) , we have discussed the details of the target selection, observations, data reduction and redshift measurements, providing all relevant information for a proper use of the data. This includes the photometric and angular selection functions, as well as the weighting schemes to be adopted to correct for the survey incompleteness. Both internal tests and comparison with external redshifts indicate a high reliability of the bulk of the VIPERS redshift data: redshifts classified as Flags 3 and 4 (33 102 objects) in our internal grading system show a confidence level of 99% in their value, while that of the combined Flags 2 and 9 (49 087 objects) is > 90%.
Using more than 1500 objects with repeated observations, we have estimated a redshift rms error of 0. 00047(1 + z) and shown that this value does not vary significantly along the different Flag classes considered as reliable (i. e. 2, 3, 4 and 9). The overall stellar contamination of the galaxy target sample is found to be smaller than 3%, confirming the goodness of our original star-galaxy separation. To provide hints on the global spectroscopic quality of the VIPERS data, we have presented first measurements of some basic spectral features, as the Balmer break index and the strength of the [OII] λ3727 line. We have also included first comparisons of these spectroscopic markers of mean stellar age and star formation rate to galaxy classification schemes used in other VIPERS papers. This clearly shows the huge potential of this data set for statistical studies of the galaxy population at an average redshift z ∼ 0.
Acknowledgements. We acknowledge the crucial contribution of the  ESO  staff in the management of service observations. In particular, we are deeply grateful to  M. Hilker  for his constant help and support of this programme. We thanks an anonymous referee for the useful comments and suggestions. Italian participation in VIPERS has been funded by  INAF  through  PRIN 2008  and 2010 programmes. LG and BRG acknowledge support of the  European Research Council  through the  Darklight ERC Advanced Research Grant  (#  291521 ). OLF and LAMT acknowledge support of the  European Research Council  through the  EARLY ERC Advanced Research Grant  (#  268107 ). Polish participants have been supported by the  Polish National Science Centre  (grants N  N203 51 29 38  and  2012/07/B/ST9/04425 ), the  Polish-Swiss Astro  Project (co-financed by a grant from  Switzerland , through the  Swiss Contribution  to the enlarged European Union), the  European Associated Laboratory Astrophysics Poland-France HECOLS  and a  Japan Society for the Promotion of Science (JSPS)   Postdoctoral Fellowship for Foreign Researchers  ( P11802 ).
GDL acknowledges financial support from the  European Research Council  under the European Community's  Seventh Framework Programme  ( FP7/2007-2013) / ERC  grant agreement n. 202781. WJP and RT acknowledge financial support from the  European Research Council  under the European Community's  Seventh Framework Programme  ( FP7/2007-2013) / ERC  grant agreement n. 202686. WJP is also grateful for support from the  UK Science and Technology Facilities Council  through the grant  ST/I001204/1. EB, FM and LM acknowledge the support from grants  ASI-INAF I/023/12/0  and PRIN MIUR 2010-2011. YM acknowledges support from  CNRS/INSU (Institut National des Sciences de l'Univers)  and the  Programme National Galaxies et Cosmologie (PNCG). CM is grateful for support from specific project funding of the  Institut Universitaire de France  and the  LABEX OCEVU.
A more detailed description of the beamline is given in ref. 48. The obtained scattering images were processed, converted into diagrams of scattered intensities versus scattering vector q where q is defined in terms of the scattering angle 2y and the wavelength l X of the radiation, thus q = 4p/l X sin y, and employing an algorithm of the computer program FIT2D. 49 he materials were heated at a heating rate of 10 K min À1 in order to be consistent with the DSC measurements.
Neutron scattering Neutron scattering measurements are carried out at the time focusing time-of-flight spectrometer IN6 at the Institut Laue Langevin in Grenoble, France. 50 The instrument was used with an incident wavelength of l n = 5. 12 Å resulting in a resolution of 100 meV (full width at half maximum). The raw data were corrected following the usual procedure using the program INX 51 for background and absorption. Different detectors have been interpolated to obtain constant q values. The maximal accessible elastic scattering vector in this configuration is q = 2. 05 Å À1. The VDOS is measured at 80 K. This makes sure that the inelastic scattering due to the vibrations is not overlaid by quasielastic scattering caused by molecular motions. The resolution of the instrument was obtained by measuring the sample under investigation at 2 K where all molecular motion and vibrations are frozen.
Acknowledgements  D. Neubert  and  S. Rolf  are thanked for experimental help. The financial support from the  German Science foundation  ( DFG SCHO 470/21-1  and  HU 850/3-1 ) is gratefully acknowledged. The  Institut Laue-Langevin  and the  Helmholtz Centre Berlin for Materials and Energy  are thanked for enabling the neutron and X-ray scattering experiments.
The structure of deuterated benzene films adsorbed on the graphite (0001) basal plane: what happens below and above the monolayer coverage? Emanuel Bahn,* ab Holly Hedgeland, c Andrew P. Jardine, b Paul F. Henry, d Thomas C. Hansen a and Peter Fouquet* a An exact description of the interactions in aromatic carbon systems is a key condition for the design of carbon based nanomaterials. In this paper we investigate the binding and adsorbate structure of the simplest prototype system in this class -the single aromatic ring molecule benzene on graphite. We have collected neutron diffraction data of the ordered phase of deuterated benzene, C 6 D 6 , adsorbed on the graphite (0001) basal plane surface. We examined relative coverages from 0. 15 up to 1. 3 monolayers (ML) in a temperature range of 80 to 250 K.
Deuterium has to be used instead of hydrogen, as hydrogen scatters predominantly incoherently and, hence, contributes very little to the diffraction peaks. The measurements cover for the first time relative surface coverages between 0. 15 and 1. 3 monolayers (ML) in a coherent experiment. This represents a full overview of the structure from isolated molecules to the beginning of multi-layer formation. Our data indicate the formation of nano-clusters with a bulkcrystalline order at coverages of more than 1 ML. The structure was measured from low temperature across the melting transition up to 250 K. This paper is organised as follows: after this general introduction, describe the sample preparation procedure and the instrument parameters used for the measurements. In the subsequent section, we present the experimental results and the analysis.
Diffraction measurements Neutron diffraction measurements were carried out using the high intensity powder diffractometer D20 at Institut Laue-Langevin (ILL), Grenoble, France, using a wavelength of l = 2. 4 Å. 33  Data were taken in a range of momentum transfers Q = | - k f À - k i | = [0. 2 to 5. 1] Å À1 , where k i and k f are the neutron wavevectors before and after scattering from the sample, respectively. The resolution in this set-up for a 2 cm diameter sample is about DQ/Q = 0. 03. 33 Measurements were performed at relative surface coverages of 0. 15 ML, 0. 5 ML, 0. 8 ML, and 1. 3 ML, respectively, and at temperatures in the range [80 to 250] K. The temperature was controlled using a standard liquid helium cryostat ('orange' cryostat,  34  ). Additional diffraction measurements of the clean graphite sample were performed at all temperatures.
Neutron spin echo measurements Supplemental neutron spin echo (NSE) measurements were performed on the NSE spectrometer IN11 at ILL using the high signal set-up IN11C, which uses a 30 degree detector bank. 35 ere, we used a wavelength of l = 5. 5 Å for the maximum signal. The spectra were normalized using a standard procedure: all data were divided by a spectrum that was obtained in situ at the cryostat base temperature of 1. 5 K, where the system can safely be assumed to be static in the dynamic window of the.