dataesr/scientific-paragraphs-categorization huggingface dataset:
Acknowledgements FA is supported by the  National Taiwan University (NTU)  under Project No. 103R4000  and by the  NTU Leung Center for Cosmology and Particle Astrophysics (LeCosPA)  under Project No. FI121. KK acknowledges support by the  Magnus Ehrnrooth Foundation. JV acknowledges support by the  Finnish Cultural Foundation. KK and JV work is supported in part by  Academy of Finland  grants  257989  and  295113. CJM is supported by an  FCT   Research Professorship , contract reference  IF/00064/2012 , funded by  FCT/MCTES  (Portugal) and  POPH/FSE (EC). Partial support by  ASI/INAF Agreement 2014-024-R. 1  for the  Planck LFI Activity of Phase E2. The calculations in this work were performed in CSC -the  IT Center for Science Ltd. (Finland) ,  IN2P3 Computer Center (France) ,  HPC -cluster facilities of  RWTH Aachen University (Germany) ,  INAF-IASF Bologna HPC cluster (Italy) , the  Cambridge COSMOS SMP system (UK) , part of the  STFC DiRAC HPC Facility  supported by  BIS NeI capital  grant  ST/J005673/1  and  STFC  grants  ST/H008586/1 ,  ST/K00333X/1.
One-parameter isocurvature extensions to the adiabatic ΛCDM model. Left: an "Axion" model (uncorrelated adiabatic and isocurvature modes, with n II = 1, cos ∆ = 0). Middle: "Curvaton I" (fully correlated adiabatic and isocurvature modes, with n II = n RR , cos ∆ = +1). Right: "Curvaton II", (fully anti-correlated adiabatic and isocurvature modes, with n II = n RR , cos ∆ = -1). The simulated Planck and LiteBIRD datasets contain only TT,TE,EE, but the simulated CORE-M5 is presented both with and without the lensing potential PP (but not with the BB nor delensing information). The real Planck data contain also a noisy B-mode at low-, consistent with zero. CORE-M5 has capability for an unprecedented constraining power in the curvaton models. RR σ(n RR ) 100β iso n RR σ(n RR ) 100β iso n RR σ(n RR ) n RR σ(n RR ) Planck TT,TE,EE+lowP LiteBIRD TT,TE,EE CORE-M5 TT,TE,EE,PP Ideal TT,TE,EE lmax=3000 Planck (sim.
The analysis of extended Fermi-LAT data sets has in the meantime provided increasing evidence for a substantial spectral break above a few GeV  (Sahakyan et al. 2013; Brown et al. 2017). This supports the conclusion that the TeV emission observed in 2004-2008 with H. E. S. S. belongs to a distinct, separate spectral component. In this paper, we present the results of long-term observations of the Cen A γ-ray core performed both with H. E. S. S. and with Fermi-LAT. These include new (more than 100 hr) VHE observations of the Cen A γ-ray core with H. E. S. S. (data set B) performed when the FGST was already in orbit. We report results of the spectral analysis of the complete H. E. S. S. data set (Sect. 2) with an exposure time that is twice that used in the previously published data set A, as well as an update (Sect.
H. E. S. S. observations and results Cen A is a weak VHE source with a measured integral flux above 250 GeV of about 0. 8% of the flux of the Crab Nebula. 2 The discovery of faint VHE γ-ray emission from Cen A motivated further observations with H. E. S. S. , which were performed in 2009-2010. In this section, we report the results of the Cen A observations with H. E. S. S. taken between 2004 and 2010. It includes a re-analysis of the H. E. S. S. data taken between 2004 and 2008 using refined methods. Using the combined H. E. S. S. data set (data sets A+B), we perform a detailed study of the VHE spectrum of Cen A.
The energy threshold increases with zenith angle. The observations of Cen A with H. E. S. S. reported in this paper were performed in wobble mode, that is with the target typically offset by about 0. 5 • or 0. 7 • from the pointing direction, allowing simultaneous background estimation in the same field of view  (Berge et al. 2007 ). The data were recorded in 28-minute exposures, called runs, which are chosen to minimise systematic changes in instrumental response. The observations of Cen A were carried out during the January-July visibility window. Data set A was taken between April 2004 and July 2008, and 111 hr of good-quality data (following a cut on the satisfactory hardware state of the cameras and good atmospheric conditions, as described in  Aharonian et al. 2006)  were recorded during 261 runs.
1. 2 and 2. 1. 3, respectively. The Image Pixel-wise fit for Atmospheric Cherenkov Telescope (ImPACT) analysis  (Parsons & Hinton 2014 ) was used to process the H. E. S. S. data. The gain of the ImPACT analysis in sensitivity is of more than a factor of 1. 5 over traditional image moments-fitting (Hillas-based) analyses, used by  Aharonian et al. (2009). The std ImPACT cut configuration, which requires a minimum of 60 photo-electrons per image, was used. The On-source counts were taken from the circular region around the Cen A radio core. The same On-region was selected for analyses of the data sets A and B, and for a combined analysis. The reflectedregion background method with multiple Off-source regions was used for spectral measurements. Given the angular resolution of H. E. S. S. , the giant outer lobes are expected to negligibly affect the VHE results.
Results for data set B The analysis of data set B yielded a γ-ray excess of 245 counts above the background (Table  1 ). This γ-ray excess corresponds to a firm detection with a statistical significance of 8. 8σ. Thus, the Cen A γ-ray core is clearly detected as a source of VHE emission in both of the H. E. S. S. data sets. The spectral analysis of the data taken in 2009-2010 yields a photon index of Γ = 2. 55 ± 0. 19 stat ± 0. 20 sys and a normalisation constant of N 0 = (1. 50 ± 0. 22 stat +0. 45 -0. 30sys ) × 10 -13 cm -2 s -1 TeV -1 at E 0 =1 TeV. To search for variability between the data sets A and B, one needs to compare the intrinsic spectral properties of the source in these two time intervals. A comparison of the spectral analyses of the H. E. S. S. data sets A and B shows that the values of the power-law photon indices are compatible with each other and with that previously reported.
1 , agree within error bars with those for the first and second data sets. The VHE spectrum of the Cen A core is compatible with a power-law function (χ 2 = 3. 9 with 6 DOF). If one takes the values of the spectral parameters from the LAT four-year Point Source Catalogue (3FGL)  (Acero et al. 2015)  obtained from the Fermi-LAT observations of Cen A between 100 MeV and 100 GeV assuming a single power-law spectrum, then one finds that N 0 = (0. 45 ± 0. 07) × 10 -13 ph cm -2 s -1 TeV -1 at 1 TeV and Γ = 2. 70 ± 0. 03. Therefore, the differential flux at 1 TeV derived from the H. E. S. S. observations in 2004-2010 is about 3. 5 times larger than that inferred from a power-law extrapolation of the 3FGL catalogue spectrum. This indicates that a deviation of the spectrum from a single power law ("hardening") should occur at GeV energies to match the TeV data (see Section 3).
We searched the combined data set for evidence of time variability at the position of the Cen A core. No significant variability was found on timescales of 28 minutes (individual runs), months, or years. The lack of apparent flux variability along with no change in spectral parameters between the two data sets justifies combining all available data when comparing the spectrum to that of Fermi-LAT. We note that given the low flux level of the Cen A γ-ray core, a flux increase by a factor of approximately ten would be needed to allow a significant detection of variability on timescales of 28 minutes (corresponding to a 5σ detection in individual runs).
2017). Finally, we tested for variability of the Cen A core both above and below the break energy (2. 8 GeV) by calculating light curves using a single power-law spectral model for each. Below the break, we divided the data into 64 45-day bins and calculated flux variability using the method described in  Nolan et al. (2012) Sect. 3. 6 , with systematic correction factor f = 0. 02. Keeping the power-law index fixed to 2. 70, we calculate 0. 09σ (χ 2 = 47. 3 with 63 DOF) significance for flux variability. Above the break, we divided the data into nine-month bins. Keeping the power-law index fixed to 2. 31, we do not see evidence for flux variability (1. 9σ, χ 2 = 16. 6 with 9 DOF). Moreover, the detection of VHE γ rays compatible with a power law up to ∼ 5 TeV raises the principal challenge of avoiding internal (i.
E. S. S. accumulated during the Fermi-LAT operation and provides a detailed characterisation of the complete VHE data set using advanced analysis methods. VHE γ-ray emission from the core of Cen A is detected at 12σ. No significant variability is apparent in the VHE data set. A spectral analysis of the complete data set yields a photon index of Γ = 2. 52 ± 0. 13 stat ± 0. 20 sys and a normalisation constant of N 0 = (1. 49±0. 16 stat +0. 45 -0. 30sys )×10 -13 cm -2 s -1 TeV -1 at E 0 =1 TeV. Spectral analyses of the H. E. S. S. data taken before and after the launch of the Fermi satellite give comparable results and validate the construction of a joined γ-ray spectrum based on Fermi-LAT and H. E. S. S. data. We also present an update of the Cen A core spectrum at GeV energies using eight years of Fermi-LAT Pass 8 data.
Acknowledgements. The support of the  Namibian authorities and of the University of Namibia  in facilitating the construction and operation of H. E. S. S. is gratefully acknowledged, as is the support by the  German Ministry for Education and Research (BMBF) , the  Max Planck Society , the  German Research Foundation (DFG) , the  Helmholtz Association , the  Alexander von Humboldt Foundation , the  French Ministry of Higher Education, Research and Innovation ,  the Centre National de la Recherche Scientifique  ( CNRS/IN2P3  and  CNRS/INSU) , the Commissariat à l'énergie atomique et aux énergies alternatives (CEA), the  U. K. Science and Technology Facilities Council (STFC) , the  Knut and Alice Wallenberg Foundation , the  National Science Centre, Poland  grant no. 2016/22/M/ST9/00382 , the  South African Department of Science and Technology and National Research Foundation , the  University of Namibia , the  National Commission on Research, Science & Technology of Namibia (NCRST) , the  Austrian Federal Ministry of Education, Science and Research and the Austrian Science Fund (FWF) , the  Australian Research Council (ARC) , the  Japan Society for the Promotion of Science , and by the  University of Amsterdam.
The red (resp. black) line shows the theoretical prediction obtained using (resp ignoring) the EWT with the Soukhovitski ĩ optical model potential  [26]. The blue line shows the predictions obtained ignoring width fluctuation corrections. Experimental data are taken from the EXFOR database  [29]. where E g is the energy of the emitted gamma of type X (X = E or M for electric or magnetic transitions) and multipolarity ℓ, and where f Xℓ (E g ) is the energy dependent gamma-ray strength function whose analytical expression follows a Lorentzian shape. For thermal neutrons, the compound nucleus excitation energy corresponds to the neutron separation energy S n and the average radiative with G g is entirely due to s-wave neutrons, so that the gamma-ray strength function satisfies the following equation 2pG g D 0 ¼ G norm X JP X Xℓ X I 0 Jþℓ I 0 JÀℓ X P 0 ∫ S n 0 T Xℓ E g rS n ÀE g I 0 p 0 dXℓP 0 dE g : ð3Þ In this equation, the J, P sum runs over the compound nucleus states with spin J and parity P that can be formed with s-wave incident neutrons and I   3 ) is verified.
This procedure is illustrated in Figure  9  for the 177 Lu E1 and M1 strengths. 5 Fe cross-section as function of the neutron incident energy. The black squares correspond to EXFOR data  [29] , the full black line is the prediction obtained using the default level density model implemented in the TALYS code  [1, 30] , the red dotted line using the combinatorial level density model of reference  [31]  and the green dashed line the combinatorial level density model of reference  [32]. Bottom panel : ratio between the strength functions obtained after the normalization deduced from equation (  3 ) is applied and the strength function corresponding to the default level density option. Fig. 9. E1 and M1 strength function of 177 Lu. The full black line shows the so-called Kopecky and Uhl  [33]  model implemented in TALYS for the E1 strength.
To date, no direct measurements of p production in pHe collisions have been made, and no data are available at a nucleon-nucleon center-of-mass (c. m. ) energy of √ s NN ∼ 100 GeV, relevant for the production of cosmic antiprotons above 10 GeV  [12]. This Letter reports the first measurement of prompt p production in pHe collisions carried out with the LHCb experiment at CERN using a proton beam with an energy of 6. 5 TeV impinging on a helium gas target. The forward geometry and particle identification (PID) capabilities of the LHCb detector are exploited to reconstruct antiprotons with momentum, p, ranging from 12 to 110 GeV/c and transverse momentum, p T , between 0. 4 and 4. 0 GeV/c. The integrated luminosity is determined from the yield of elastically scattered atomic electrons. The LHCb detector is a single-arm forward spectrometer covering the pseudorapidity range 2 < η < 5, described in detail in Refs.
The scintillating-pad (SPD) detector and the electromagnetic calorimeter (ECAL) included in the calorimeter system are also used in this study. The SMOG (System for Measuring Overlap with Gas) device  [16, 17]  enables the injection of noble gases with pressure of O(10 -7 ) mbar in the beam pipe section crossing the VELO, allowing LHCb to operate as a fixed-target experiment. This analysis is performed on data specifically acquired for this measurement in May 2016. Helium gas was injected when the two beams circulating in the LHC accelerator  [18]  consisted of a small number, between 52 and 56, of proton bunches. The proton-beam energy of 6. 5 TeV corresponds to √ s NN = 110. 5 GeV. In the proton-nucleon c. m. frame, the LHCb acceptance corresponds to central and backward rapidities -2. 8 < y * < 0.
2, and p production can be studied for values of x-Feynman, the ratio of the p longitudinal momentum to its maximal value, comprised between -0. 24 and 0. To avoid background from pp collisions, the events used for this measurement were recorded when a bunch in the beam pointing toward LHCb crosses the nominal interaction region without a corresponding colliding bunch in the other beam. The online event selection consists of a hardware stage, which requires activity in the SPD detector, and a software stage requiring at least one reconstructed track in the VELO. An unbiased control sample of randomly selected events is acquired independently of this online selection. Simulated data samples are generated for pHe collisions with EPOS-LHC  [19] , and for pe -normalization events with ESEPP  [20].
Three sets of templates for each particle species are determined from simulation, from pHe data, and from pp data collected in 2016. The pHe calibration samples consist of selected K 0 S → π + π -decays for pions, Λ → pπ -(Λ → pπ + ) for (anti)protons and φ → K + K - for kaons. Calibration samples in pp data also include D * ± → ( ) D 0 (K ∓ π ± )π ± decays. Simulation is used for the template of fake tracks. Two methods are used to determine the p fraction in each kinematic bin: a twodimensional binned extended-maximum-likelihood fit, illustrated in Fig. 1 , and a cutand-count method  [24] , which uses exclusive high-purity samples selected with tight requirements for each particle species. The probability P ij that a candidate of species i is classified as species j is obtained from the templates.
These are due to hyperon decays, in 90% of cases, or secondary interactions. This fraction is corrected by a factor 1. 5 ± 0. 3, to account for differences between simulation and data as determined in the region of the χ 2 IP distribution dominated by hyperon decays. The resulting correction to the p yield averages to -2. 4%. Collisions on the residual gas in the LHC beam vacuum, with a pressure of O(10 -9 ) mbar and unknown composition, can contribute to the p yield. Residual-gas analysis, performed in the absence of beam, indicates that the contamination is O(1)% and is dominated by hydrogen. To evaluate this background source, including a possible beam-induced component, a control sample of beam-gas collisions was acquired before injection of the helium gas. Data collected with and without helium gas have the same vacuum pumping configuration and thus identical residual gas composition and pressure.
The yield of selected events in data without helium gas, scaled according to the corresponding number of protons on target, is subtracted from the result leading to an average correction of (-0. 6 ± 0. 1)%, where the uncertainty accounts for the background variation over time. The average PV track multiplicity is found to be smaller in collisions without injected gas, confirming that the residual gas is dominated by hydrogen. Since the injected gas pressure is not precisely known, the integrated luminosity of the data sample is determined from the yield of electrons from elastic scattering of the proton beam. Scattered electrons are simulated in the polar angle range 3 < θ < 27 mrad,   /c ). The (DLL pK , DLL pπ ) distribution, shown in the top plot, is fitted to determine the relative contribution of π -, K -and p particles, using simulation to determine the template distributions and the fraction of fake tracks (which are barely visible).
Loose requirements are placed on the response of the BDT discriminants, with a combined efficiency of 96% for simulated pe -events. The overlap of a pe -event with another beam-gas interaction causes an additional inefficiency, measured to be (9. 4 ± 0. 7)% in the unbiased control sample. A possible charge asymmetry of the background, estimated from the EPOS simulation, leads to a systematic uncertainty of 1. 9%. As is done for the p candidates, the unbiased control events are used to measure the online selection efficiency, (98. 3 ± 0. 3)%, and the data without helium gas are used to determine the contribution from scattering on residual gas, (1. 0 ± 0. 3)%. The momentum distributions of the selected candidates are shown in Fig. 2 , where a good agreement with the simulated pe -signal is observed after background subtraction.
The net effect of migration between kinematic bins due to resolution effects is found to be negligible. A major difference between the fixed-target configuration and the standard pp-collision data taking in LHCb is the extension of the luminous region. As a consequence, the result is checked to be independent of z PV within the quoted uncertainty in all kinematic bins. Furthermore, the results do not show any significant dependence on the time of data taking. The p production cross-section is determined in each kinematic bin from a sample of 33. 7 million reconstructed pHe collisions, yielding 1. 5 million antiprotons as determined from the PID analysis. In Fig. 3 , the results, integrated in different kinematic regions, are compared with the prediction of several models: EPOS-LHC  [19] , the pre-LHC EPOS version 1.
Acknowledgements We are grateful to our colleagues from the cosmic ray community,  O. Adriani ,  F. Donato ,  L. Bonechi  and  A. Tricomi , for suggesting this measurement, to  T. Pierog  and  S. Ostapchenko  for their advice on the theoretical models for antiproton production, and to  B. Ward  and  A. V. Gramolin  for their advice on the model and uncertainty for pe -scattering. We express our gratitude to our colleagues in the CERN accelerator departments for the excellent performance of the LHC. We thank the technical and administrative staff at the LHCb institutes. We acknowledge support from  CERN  and from the national agencies:  CAPES ,  CNPq ,  FAPERJ  and  FINEP (Brazil) ;  MOST  and  NSFC (China) ;  CNRS/IN2P3  (France);  BMBF ,  DFG  and  MPG (Germany) ;  INFN (Italy) ;  NWO (Netherlands) ;  MNiSW  and  NCN (Poland) ;  MEN/IFA (Romania) ;  MSHE (Russia) ;  MinECo (Spain) ;  SNSF  and  SER (Switzerland) ;  NASU (Ukraine) ;  STFC  ( United Kingdom );  NSF (USA).
Coupling with microfluidics and automation Microfluidics channels for experiments with vesicle, polyelectrolyte and cell experiments were straight channels of dimensions 50 μm x 100 μm x 4 mm. The devices were fabricated using standard soft lithography procedures  [8]. A positive mold was created by photolithography with SU-8 2050 negative resins (Microchem, Newton, MA, USA) on a silicon wafer (Siltronix, Archamps, France). A replica was made with polydimethylsiloxane, PDMS (Sylgard 184 Silicone Elastomer Kit, Dow Corning, Midland, USA). Ports to plug inlet and outlet tubings were punched with a gauge needle in the PDMS replica. The devices were finalized by sealing the PDMS piece on a wet-surf via O 2 -plasma activation (Harrick plasma, Ithaca, NY, USA) of both surfaces. The layer by layer polyelectrolyte deposition process was automatized with a Labview code piloting sequential injections of polyelectrolyte and rinsing solutions with 4 syringe pumps (RAZEL R100-E, St Albans, VT, USA), and a 6 way valves (nonapeak, Scivex, Oak Harbour, WA, USA).
Acknowledgments This work was supported by the  Nanolane company (Le Mans), Solvay company (Bordeaux), Alveole company (Paris), C-Nano PACA Network, Labex INFORM network, Centuri network ,  ANR   Recrute grant , the  European Union 's  Horizon 2020 research and innovation program  under the  Marie Skłodowska-Curie  grant agreement  No713750. It has also been carried out with the financial support of the  Regional Council of Provence-Alpes-Cote d'Azur  and of the A � MIDEX (n˚ANR- 11-IDEX-0001-02 ), funded by the  Investissements d' Avenir  project funded by the  French Government , managed by the  French National Research Agency (ANR). We acknowledge  Vincent Studer  for fruitful advices on LIMAP printing protocols as well as the  PLANETE CT PACA cleanroom facility  for electron lithography processes.
This work was supported by the  Nanolane company (Le Mans), Solvay company (Bordeaux), Alveole company (Paris), C-Nano PACA Network, Labex INFORM network, Centuri network ,  ANR   Recrute grant , the  European Union 's  Horizon 2020 research and innovation program  under the  Marie Skłodowska-Curie  grant agreement  No713750. It has also been carried out with the financial support of the  Regional Council of Provence-Alpes-Cote d'Azur  and of the A � MIDEX (n˚ANR- 11-IDEX-0001-02 ), funded by the  Investissements d' Avenir  project funded by the  French Government , managed by the  French National Research Agency (ANR). The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. MM was employed by  Nanolane. Nanolane  provided support in the form of salaries for author MM, but did not have any additional role in the study design, data collection and analysis, decision to publish, or preparation of the manuscript.
Energy calibration and stability With the setup for Ir L 3 -edge RIXS, we checked the reliability on the energy scale of the RIXS spectrometer by measuring the well known dispersion of longitudinal acoustic phonons in diamond along the (H, 0, 0) direction. This is shown in Fig. 6  (open blue circles) to overlap with literature data (red line)  (Warren et al. , 1967). Finally, we also tested the stability of the energy scale in the long term; the inset of Fig. 6  shows the change in the phonon energy at (3, 0, 0) momentum transfer over several hours. A small drift is observed, which can be.