dataesr/scientific-paragraphs-categorization huggingface dataset:
Accounting for long-term variability As we will discuss in detail later, the Suzaku/HXD data show a higher hard X-ray flux level than Swift/BAT. Under the assumption that variability is dominated by the powerlaw, we introduced a further cross-normalization constant (CONST IPL ) in both models P and M to account for different intrinsic (i. e. IPL) source fluxes measured by Suzaku and Swift. In this scenario the absolute flux of the reflection and scattered components do not vary, with their normalizations being tied to the same value as the IPL between all instruments. The XIS regime, being reflection-dominated, is not greatly sensitive to changes in the IPL, though it is treated self-consistently throughout.
3) also has consequences for the lower energy range. It is important to remember that we have assumed the variability to be dominated by the IPL normalization alone, and that the absolute fluxes of the reflection and scattering components do not change because they ought to respond on long timespans. This means that any fit variables defined relative to the IPL (i. e. f SPL , R) also change depending upon the dataset considered. Table  1  states values relative to the long-term IPL flux probed by Swift/BAT. So when considering the values of these variables in the Suzaku data alone, these will effectively be lower by a factor of CONST IPL. Similarly, in Table  1 , we have distinguished between the absorption-corrected IPL luminosities L XIS (2-10) and L 2-10. L XIS (2-10) is the absorption-corrected 2-10 keV luminosity for the XIS consistent with the HXD flux level (the two instruments observed the source simultaneously on the same date).
On the other hand, L 2-10 is lower by a factor of CONST IPL , and may be considered the long-term average 2-10 keV IPL luminosity based upon the Suzaku/XIS and Swift/BAT datasets. These variables are collected and tabulated together with CONST IPL in Table  1. The inferred long-term absorption-corrected IPL luminosity for models P and M ranges over L 2-10 ∼(0. 7-1)×10 43 erg s -1. Mean X-ray bolometric corrections and Eddington fractions of the Swift/BAT AGN sample have been studied by  Vasudevan et al. (2010) , who showed that this sample has a comparatively low Eddington ratio distribution overall  (Vasudevan et al. 2010). For a typical bolometric correction (L Bol :L 2-10 )∼10-30, the mean L Bol of ESO 565-G019 lies within the range of ∼(0. 7-3)×10 44 erg s -1. If the accretion luminosity of the source is 10 % of the Eddington value on average, this would imply a supermassive black hole mass range of (0.
Hard X-ray spectrum and long-term variability Fitting over the full energy range available with Suzaku/XIS and Swift/BAT suggests that the IPL dominates above ∼100 keV in the BAT band, and E cutoff should lie beyond the BAT energy sensitivity range. The fitted Γ IPL values are consistent with the median of the distribution of hard X-ray photonindices for radio-quiet Seyferts  (Dadina 2008). N H (los) is found to be larger than N H (scatt) in model M, which may be a result of clumpiness in the absorber, as supported by a wide range of observational and theoretical work on AGN tori in general (e. g. Hoenig 2013 and references therein). But with the IPL dominating only in the two highest energy BAT bins, these data do not probe the underlying continuum in detail. This is an important limitation of reflectiondominated spectra, and leads to various degeneracies (e.
g. N H (los) being unconstrained at the high end; large uncertainties on CONST IPL ), and an even more reflection-dominated hard-band spectrum cannot be ruled out. The observed Suzaku/HXD flux (F 15-40 keV ≈1. 4×10 -11 erg s -1 cm -2 ) lies above that seen in Swift/BAT by a factor of ≈3-4 over the same energy range. Systematic uncertainties are important when accounting for the HXD/PIN background reproducibility. Typical earth-occultation data systematic errors are ∼3. 8% 19. Including an increased PIN background at this level reduces the HXD excess with respect to BAT to a factor ∼2. These differences cannot be caused by confusion and contamination of the HXD data, because the nearest neighbor in the BAT 70-month catalog is PKS 0921-213 at a distance of 2 •. 6, well outside the collimated ∼34 ′ -sized PIN fov.
The BAT data represent a long-term average of the source flux between Dec 2004 and Sep 2010. Suzaku observations were carried out 20 months later, so hard X-ray variability may explain the difference. Reflection and scattering are generally thought to occur on ∼pc-scale toroidal clouds. Rapid variations are naturally associated with the IPL (as we have modeled). The lower limit of the IPL variation in this scenario is at least a factor of ∼2. It should be noted that we cannot completely rule out strong variations of the hard band Compton hump originating in an inner disc reflection component (e. g. due to light-bending). This possibility can be tested in follow-up X-ray monitoring to search for rapid changes in the reflection continuum and Fe line.
(2012, their Fig. 5 ), but not significantly different from the overall distribution of Seyfert colors. This relatively-high 90:9 µm flux ratio suggests the presence of large quantities of cool dust which is well-known for NGC 6240 and NGC 5728 (e. g. Rieke et al. 1985; Schommer et al. 1988) , but atypical for an early-type galaxy like ESO 565-G019 (this is discussed further in section 5. 6). The observed (absorbed) 2-10 keV X-ray luminosity in the Suzaku data is L 2-10 ∼4×10 41 erg s -1 , and the modeled absorption-corrected power is 1-2 orders of magnitude higher depending upon which dataset is considered. X-ray modeling of CT-AGN can be highly sensitive to the geometry of the absorber and reflector when the underlying continuum cannot be probed clearly (e. g. Yaqoob 2012). It is thus useful to compare against other diagnostics of the intrinsic power, as an independent check of the appropriateness of the X-ray modeling.
Few emission line spectroscopic measurements of the source have been published. Considering photometric data, it has been shown that there is a close correlation between the monochromatic 12µm continuum torus luminosity and intrinsic 2-10 keV power for local Seyferts (e. g. Horst et al. 2008; Asmus et al. 2011). The best constraints come from isolating the torus spatially in high angular resolution imaging, but such data are not available for ESO 565-G019. The source is detected in the WISE all-sky survey 20  (Wright et al. 2010). Its W3 band (12 µm) flux is F (W3)=96±11 mJy, or λL λ (W3)=1. 6×10 43 erg s -1. Using Eq. 2 from  Gandhi et al. (2009)  then implies L predicted 2-10 =1. 1(±0. 2)×10 43 erg s -1. This is smaller than the instantaneous IPL power L XIS (2-10) measured in the XIS, but closely matches the inferred long-term intrinsic power estimates L 2-10 (Table  1 ).
CONCLUSIONS We have presented the first X-ray spectrum of ESO 565-G019 below 10 keV, as well as broadband X-ray spectral modeling. A reflection-dominated nuclear continuum and prodigious Fe fluorescence emission have been revealed with Suzaku. The line-of-sight obscuring column density is greater than 1. 6×10 24 cm -2 (90% confidence) and the Fe Kα equivalent width with respect to the observed continuum is close to 1 keV. There is evidence of hard X-ray variability when comparing our Suzaku data with the long-term Swift/BAT average spectrum. This object is one of the few bona fide reflectiondominated AGN known to be hosted in an early-type galaxy. Mid-and far-infrared detections point to the likely presence of massive quantities of large-scale dust and on-going starformation in the host. The most likely scenario for triggering nuclear activity is a minor merger, though there may also be an ongoing interaction with its neighbor ESO 565-G018.
PG acknowledges support from  JAXA  and  STFC. The authors would like to express their thanks to Suzaku team members. Swift/BAT transient monitor data are used herein. This research has made use of the NASA/IPAC Extragalactic Database (NED) which is operated by the  Jet Propulsion Laboratory, California Institute of Technology , under contract with the  National Aeronautics and Space Administration. WISE is a project of  Univ. California, Los Angeles , and  Jet Propulsion Laboratory (JPL)/California Institute of Technology (Caltech) , funded by the  NASA. 2MASS  is a project of the  Univ. Massachusetts and the  Infrared Processing and Analysis Center/Caltech , funded by  NASA  and the  National Science Foundation. Akari is a project of the  Japan Aerospace Exploration Agency  with the participation of the  European Space Agency.
The  NASA/IPAC Infrared Science Archive (IRSA)  operated by  JPL  under contract with  NASA , was used for querying the infrared databases. The Hyper-LEDA database was also useful in this work. The reviewer provided constructive criticisms which improved the paper. PG thanks  S. F. Hönig  for comments. KV would like to thank  Y. Wadadekar  and  S. Barway  for enlightening discussions.
IceCube and ANTARES are neutrino detectors sensitive to energies from 20 GeV up to PeV. Both detectors have been completed and take data. Several years of data have been already analysed including periods with the partly assembled detectors. The primary goal of these two neutrino telescopes is the observation of astrophysical sources of neutrinos. Results from searches for such neutrinos with different strategies will be presented as well as measurements of atmospheric neutrinos which are an irreducible background for such searches, but they are an interesting study object by themselves.
A possible solution, suggested over 20 years ago, is the use of water or ice as a Cherenkov target-detector. The prove of this concept has been performed in lake Baikal with the unambiguous detection of atmospheric neutrinos in the NT-96 detector  [1]. Today two large detectors, ANTARES in the Mediterranean Sea and IceCube at the South pole take data and produce physics results. These two projects will be presented in the following.
In particular 40 K, abundant in salty sea water, is absent in ice. Further, no light-producing biological activity occurs. Therefore, the observed optical background rate at the single photon level is only 500 Hz per PMT in IceCube. Beginning with the installation of the first string in 2005, IceCube has been operated in approximately yearlong data taking seasons. During the antarctic summer seasons in December and January new strings had been deployed at a pace of about 20 strings per year. IceCube construction was finished in December 2010. From May 2008 to April 2009 IceCube operated with 40 installed strings, the so-called IC40 configuration. From May 2009 to April 2010 59 strings had been active (IC59). The results which will be presented in the following have been obtained from analysing these two data-taking periods.
Energy [GeV] The energy range of the limit lines in Figure  1  indicates the central range in which 90% of the signal events are expected. For the muon channel, the lowest testable energies are at the level, where the contribution from atmospheric neutrinos becomes stronger. As this contribution is significantly lower in the cascade channel (not shown in the figure), the limits derived in this channel extend subsequently to lower energies. The most recent result has been obtained by analysing 21943 events from 348 days of data taking with the IC59 setup in IceCube  [27]. It is interesting to note, that the resulting limit is slightly worse than the limit which had been previously obtained with the smaller IC40 setup  [11]. This is due to fluctuations in the high energy tail of the IC59 data set.
CONCLUSION In this paper, we have derived general equation to calculate the n-order response of the energy of a system with respect to a geometric perturbation, calculated within SCC-DFTB approach. The implementation of these equations in the deMonNano code makes use of automatic differentiation which enable the calculation of derivatives up to any order provided the fact that memory and computational time is available. Due to storage limitation, only derivatives up to fourth-order have been calculated in this work. The implementation has been benchmarked by comparing the results with derivatives computed by the finite differences method. The analytical calculation is much faster than the latter approach. Such derivatives can be used to obtain an approximated PES of he system through a Taylor expansion up to a given order.
Vertical profiles A stratospheric balloon carrying the two STAC instruments was launched by the French space agency CNES on 12 March 2011, from Kiruna, northern Sweden (67 • 53 ′ N, 21 • 04 ′ E). The balloon flight lasted from 20:00 to 22:05 UTC. Measurements with the STAC instruments were conducted during the ascent in the 480-28 hPa altitude range and during the slow descent in the 28-130 hPa altitude range with the vertical speed in the range of 2-5 m s -1. STAC sampled the aerosol data once per second. Measurements were integrated over 75 s, which provides a good compromise between removing local fluctuations whilst permitting detection of vertical structures. This timescale corresponds to ∼ 300 m vertically, depending on the balloon ascent or descent rate. Figure  1  shows the measurement of uncharged aerosol concentrations during the measurement process as described above.
Acknowledgements. The  AEROWAVE  project is funded by  CNES  and  CNRS/INSU. This work is supported by the  Labex Voltaire  ( ANR-10-LABX-100-01 ) from  University of Orleans. The work at the  University of Bath  is supported by the  Natural Environment Research Council (NERC)  under grant  NE/H024921/1. The modelling work at  IIT, Kanpur , is supported by  Ministry of Earth Sciences, India. We thank the  CNES balloon launching team  for the STAC flight and  J. -P. Lebreton  ( LPC2E-CNRS ) for helpful comments. Stratospheric aerosol data and other balloon measurements on stratospheric species are available on the ETHER website: http://ether. ipsl. jussieu. fr/Edited by: M. Schulz The publication of this article is financed by  CNRS-INSU.
Data available and uncertainties on stellar properties The CoRoT photometric time series used in this work were obtained in the so-called exofield during the first long CoRoT runs in the direction of the Galactic centre (LRc01) and in the opposite direction (LRa01). These long runs lasted approximately 140 days, providing us with a frequency resolution of about 0. 08 µHz. A first analysis of these data was made by  [9] ,  [10]  and  [11]. Solar-like oscillations were detected in 435 and 1626 giants belonging to LRa01 and LRc01, respectively. To derive M,R, and distance we use the values (and uncertainties) of ν max and ∆ν as determined by  [12]. The typical uncertainty on ν max and ∆ν for the 150-d long CoRoT observations is of the order of 2. 4 % and 0. 6 %, respectively. The uncertainties on the stellar properties are estimated using Monte Carlo simulations adopting the following constraints: -Apparent magnitudes: uncertainties on J and K s are taken from the 2MASS photometry available in the EXODAT  [13]  catalogue (the median uncertainty is 0.
CoRoT target selection We retrieved from EXODAT  [13]  photometric information on all the stars in the field, as well as the targets observed. As shown in Fig. 3 , targets within each field of view were selected largely on the basis of colour-magnitude criteria. Within the observed targets, solar-like oscillations were searched for in stars belonging to a limited colour-magnitude domain: 0. 6 < J -K s < 1 and K s < 12 [see 12]. Restricting to this domain, we find no significant difference in the target selection bias applied to LRc01 compared to LRa01. Fig. 2. Upper panel: Ratio ∆ν/∆ν to (ρ/ρ ) 1/2 as a function of T eff for models computed using the ATON code  [34] , with initial heavy-elements mass fraction Z = 0. 02, initial helium mass fraction Y = 0. 278, and mass between 0. 7 M and 3.
Evidence for the role of the current density profile is suggested by changes in sawtooth behavior. LHCD plasmas that had sawtooth oscillations showed countercurrent velocity increments, whereas in the cocurrent rotation increment discharges, the sawteeth were suppressed due to a significant change in the q profile. Table  I  summarizes the sawtooth behavior for a database of 243 low density target C-Mod plasmas with LHCD. No coincrement discharges exhibited sawtooth oscillations whereas all sawtoothing discharges underwent countercurrent rotation changes. Only a few counterincrement plasmas were without sawteeth. LHCD discharges without sawteeth also experienced cocurrent rotation increments in JT-60U  [4] , EAST  [8] , JET  [10] , and Tore Supra. A summary of the LHCD rotation parameters from various tokamaks is shown in Table  II.
Studies of the spin and parity quantum numbers of the Higgs boson are presented, based on proton-proton collision data collected by the ATLAS experiment at the LHC. The Standard Model spin-parity J P = 0 + hypothesis is compared with alternative hypotheses using the Higgs boson decays H→ γγ, H → ZZ * → 4 and H→ WW * → ν ν, as well as the combination of these channels. The analysed dataset corresponds to an integrated luminosity of 20. 7 fb -1 collected at a centre-of-mass energy of √ s = 8 TeV. For the H → ZZ * → 4 decay mode the dataset corresponding to an integrated luminosity of 4. 6 fb -1 collected at √ s = 7 TeV is added. The data are compatible with the Standard Model J P = 0 + quantum numbers for the Higgs boson, whereas all alternative hypotheses studied in this letter, namely some specific J P = 0 -, 1 + , 1 -, 2 + models, are excluded at confidence levels above 97.
The measurements are based on the kinematic properties of the three final states H→ γγ, H → ZZ * → 4 and H→ WW * → ν ν, where denotes an electron or a muon. To improve the sensitivity to different spin-parity hypotheses, several final states are combined. To test the 0 -spin-parity hypothesis, only the H → ZZ * decay mode is used, while for the 1 + and 1 -hypotheses the H → ZZ * and H → WW * channels are combined. For the 2 + study, all three decay modes are combined. The full dataset collected at √ s = 8 TeV, corresponding to an integrated luminosity of 20. 7 fb -1 , is analysed for all three channels. For the H → ZZ * decay mode, a dataset corresponding to an integrated luminosity of 4. 6 fb -1 collected at √ s = 7 TeV is also included. While for the SM Higgs boson the Lagrangian structure and its couplings are fully determined, the alternative hypotheses can be described by a wide variety of models, characterised by different structures and effective couplings.
The BDT is trained on simulated signal events after full reconstruction and event selection. Dedicated discriminants are defined for the separation between the Standard Model J P = 0 + hypothesis and each of the considered alternative models, J P = 0 -, 1 + , 1 -, 2 +. In the case of the spin-2 hypothesis, the studies are performed as a function of the q q production fraction, f q q. The response of the BDT classifiers is evaluated separately for each pair of signal hypotheses, including the expected backgrounds from other SM processes. In addition, to improve the overall sensitivity, the BDT re- Figure  4 : Distributions of the BDT output for data (points with error bars) and expectations based on MC simulation (histograms). The distribution of each discriminant is shown for a pair of spin and parity hypotheses for the signal: J P = 0 + (solid line) and J P = 0 -(dashed line) in (a), J P = 0 + (solid line) and J P = 1 + (dashed line) in (b).
Acknowledgements We thank  CERN  for the very successful operation of the LHC, as well as the support staff from our institutions without whom ATLAS could not be operated efficiently. We 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 , Poland; GRICES and FCT, Portugal; MERYS (MECTS), Romania; MES of Russia and ROSATOM, Russian Federation; JINR; MSTD, Serbia; MSSR, Slovakia; ARRS and MIZ Š, Slovenia; DST/NRF, South Africa; MICINN, 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 ;  DOE  and  NSF ,  United States of America.
We present our new measurement of the cross-section for charm dimuon production in neutrino-iron interactions based upon the full statistics collected by the NO-MAD experiment. After background subtraction we observe 15,344 charm dimuon events, providing the largest sample currently available. The analysis exploits the large inclusive charged current sample -about 9 × 10 6 events after all analysis cuts -and the high resolution NOMAD detector to constrain the total systematic uncertainty on the ratio of charm dimuon to inclusive Charged Current (CC) crosssections to ∼ 2%. We also perform a fit to the NOMAD data to extract the charm production parameters and the strange quark sea content of the nucleon within the NLO QCD approximation. We obtain a value of m c (m c ) = 1. 159 ± 0. 075 GeV/c 2 for the running mass of the charm quark in the MS scheme and a strange quark sea suppression factor of κ s = 0.
The knowledge of the strange quark sea content of the nucleon and of charm production is also the dominant contribution to the systematic uncertainties in the electroweak measurements from (anti)neutrino DIS interactions  [1]. Traditionally, charm dimuon production in (anti)neutrino interactions has always been measured in massive calorimeters, mainly composed of passive heavy materials (iron, marble, lead etc. ) in order to obtain a sizeable number of events  [2, 3, 4, 5, 6, 7, 8]. This detection technique, while relatively simple and efficient, is ultimately limited by the coarse resolution of the detectors and by the resulting systematic uncertainties. ν µ µ - W + N s/d c W + ν µ µ + X s/d The high resolution NOMAD data allow a new level of precision in the measurement of charm dimuon production in neutrino interactions.
Trigger and Calibration The main trigger selection used for the analysis of FCAL data requires an energy deposition in the FCAL of at least 3. 15 m. i. p. -m. i. p. is the signal of a minimum ionizing particle crossing one FCAL stack -and no signal in the V 8 veto scintillator plane: V8 × F CAL -(FCAL trigger). This trigger vetoes through-going muons and has a live time of 90 ± 3%. A second independent trigger selection with lower threshold is used to measure the FCAL trigger efficiency from data (FCAL ′ trigger). For this trigger an energy deposition of at least 1. 2 m. i. p. in the FCAL is requested, in addition to the coincidence with a signal from the scintillator plane in the TRD region: V8 × T 1 × T 2 × F CAL ′. The live time is 90 ± 3%. We measure the efficiency of the FCAL trigger directly from data in the following way: ǫ F CAL = N DAT A F CAL&F CAL ′ N DAT A F CAL ′ (6) We determine the FCAL trigger efficiency separately for each of the 4 stacks and each of the 4 years of data taking, for a total of 16 configurations.