dataesr/scientific-paragraphs-categorization huggingface dataset:
Acknowledgments The authors would like to thank  Carlton Baugh ,  Carlos Frenk ,  Martin Haehnelt ,  Jonathan Davis ,  Erminia Calabrese ,  Joerg Jaeckel  and  Silvia Pascoli  for useful discussions,  Benjamin Audren  for his assistance with MONTE PYTHON, and the  Planck Editorial Board and Science Team  for their reading of this work. We acknowledge the use of the publicly available numerical codes CLASS and MONTE PYTHON, and the CMB data from the  WMAP, Planck , SPT and ACT experiments. RJW and CB are supported by the  STFC. This work was supported in part by the  National Science Foundation  under Grant No. PHYS-1066293 , and the hospitality of the  Aspen Center for Physics  and the  European Union   FP7 ITN INVISIBLES.
g. see  Ackermann et al. 2010a; Ando & Nagai 2012; Gao et al. 2012; Huang, Vertongen & Weniger 2012). The Virgo cluster is located about 16. 5 Mpc away and is the nearest large galaxy cluster. Due to Virgo's proximity, this cluster is an excellent target for γ -ray observations as it can spatially be resolved by Fermi-LAT at GeV energies. Recently, a signal consistent with that expected from DM annihilation from the Virgo cluster has been discussed by  Han et al. (2012a) , who have analysed the first 3 yr of data from Fermi-LAT. The reported signal is at a significant level of 4. 4σ for a model in which WIMPs, with mass M 28 GeV, annihilate via the b b channel. A large boost factor, ∼10 3 , is invoked by  Han et al. (2012a)  for the DM interpretation of the observational data. Phoenix simulations by  Gao et al.
O B S E RVAT I O N A N D DATA R E D U C T I O N Fermi was launched on 2008 June 11 into a nearly circular Earth orbit with an altitude of 565 km and inclination of 25. • 6, and an orbital period of 96 min. The principal instrument on Fermi is the LAT  (Atwood et al. 2009 ), a pair-production telescope with a large effective area (∼8000 cm 2 at 1 GeV) and field of view (2. 4 sr), sensitive to γ -rays between 20 MeV and >300 GeV. After the commissioning phase, the Fermi-LAT began routine science operations on 2008 August 4. The detector normally operates in sky-survey mode which provides a full-sky coverage every 3 h (i. e. two orbits). For the data analysis, we use the FERMI SCIENCE TOOLS v9r27p1 package 1  and P7V6 instrument response functions. We use accumulated events obtained from 2008 August 4 to 2012 June 12.
• 6) have been allowed to vary in their analysis. As shown in fig. 1  of  Han et al. (2012a) , the three point sources within the Virgo's virial radius are faint and, therefore, the residuals are dominated by the contribution from stronger γ -ray sources which are outside the virial radius. This is due to their spectral parameters not perfectly described by the values taken from the 2FGL catalogue, since the data from a longer Fermi-LAT observation are analysed. Since the values of the spectral parameters of the 16 strong point sources are derived from the likelihood analysis in our study, the calculated residual count maps (see Section 4) are more suitable for the morphological analysis. We will discuss the population of γ -ray point sources near the Virgo cluster which are not included in the 2FGL catalogue in Section 5, where the results of our likelihood analysis will be presented.
L I K E L I H O O D A NA LY S I S U S I N G 5 Y R O F DATA The result of the analysis presented above shows that the additional extended γ -ray source in the region of the ISM doughnut-shaped gas structure, that is located in the direction of the Virgo cluster, is statistically significant at 3. 4σ level. This emission can be attributed to DM annihilation in the halo of the Virgo cluster or to non-2FGL point sources near the Virgo cluster (see  Han et al. 2012b; Macías-Ramírez et al. 2012). It can also be caused by imperfections of the Galactic foreground model describing the ISM doughnut-shaped structure towards the Virgo cluster. To check these possibilities, we compared the two models M1 and M5 in Section 5. 2 and found that the additional extended γ -ray source is spatially inhomogeneous, under the assumption that the Galactic foreground model is perfectly modelled.
√ L and theoretical errors halved. These estimates are displayed in Fig. 12  and compared to a fit of the TLEP projectionsextracted with the same assumptions about the theoretical uncertainties in Higgs boson decays. Within the mildly model-dependent assumptions used in the fit -no exotic decays, and correlated up-type-quark couplings -the projections for HL-LHC in Scenario 2 are truly impressive, and will further improve by including the other detector (ATLAS projections are available in Ref. [48] ) and additional dedicated analyses in the combination. In this challenging context, TLEP data collected at 250 and 350 GeV would enable very significant improvements on these coupling measurements well beyond the HL-LHC projected precision, and with an accuracy adequate to become sensitive to multi-TeV new physics.
Sensitivity to new physics and theory uncertainties As examples of new physics models that would be probed with precision Higgs measurements at TLEP, supersymmetric models that are compatible with current measurements, including the non-observation The red and blue bars correspond to the combination of the data at 240-250 GeV and 350 GeV, while the green bars hold for the sole period of TLEP at 240 GeV. The dashed lines show the ±1% band, relevant for sensitivity to multi-TeV new physics. Also indicated are the expected uncertainties on the total decay width and on the invisible decay width. The Hµµ and Hγγ coupling uncertainties, which do not fit in the ±6% scale of the figure for ILC, can be read off Table  8. of supersymmetric particles at the LHC, are considered. These models are simplified, in that they assume universal supersymmetry-breaking masses for squarks and sleptons, and for gauginos, at a high scale.
In the case of the CMSSM, this assumption is extended to include the supersymmetric Higgs bosons, but this assumption is relaxed in the NUHM1 model  [49]. A global frequentist analysis of the present data found two CMSSM fits that yield very similar values of the global χ 2 function, with lower and higher sparticle masses respectively, whilst the best NUHM1 fit is qualitatively similar to the low-mass CMSSM fit. These fits have not been excluded by the 2012 LHC run at 8 TeV, but lie within the potential reach of the forthcoming LHC 13/14 TeV run. On the other hand, the high-mass CMSSM point is likely to lie beyond the reach of the LHC. Thus, these models represent different potential challenges for the TLEP precision physics programme: verify predictions of new physics models at the quantum level, or find indirect evidence for new physics beyond the reach of the LHC.
The next LHC run at 13-14 TeV, to start in 2015, will bring clarity in this respect. Discovery of a new particle lighter than 1. 5 TeV in the 13-14 TeV LHC data would rejuvenate the proposal of CLIC at √ s = 3 TeV. A 100 TeV proton-proton collider,in the context of the FCC project, would instead be able to produce new coloured particles up to several tens of TeV, thus opening a unique window at high energy. A detailed study of the VHE-LHC physics case has started in this context, in order to have relevant answers ready for the next European Strategy update, to take place around 2018.
Acknowledgements We are indebted to  Andreas Hoecker  for his help with the GFitter fitting program (http://cern. ch/gfitter),and for his patient explanations of the underlying physics. We would like to acknowledge the contributions of all participants in the design study and in the first five TLEP workshops. Writing this article was greatly eased by the use of the online collaborative editor, Authorea (https://www. authorea. com/),ceaselessly improved by the founders,  Nathan Jenkins  and  Alberto Pepe. The support of the CERN Director for Accelerators and Technology and of the PH department, of the  European Commission  under the  FP7 Research Infrastructures project EuCARD , grant agreement no. 227579  ( http://cern. ch/eucard)and under the  FP7 Capacities project EuCARD-2 , grant agreement no.
LBA Observations and Data Reduction Very Long Baseline Interferometer (VLBI) observations of PSR B1259-63 were conducted with the Australian Long Baseline Array (LBA) at 2. 3 GHz (13 cm) on 2011 January 13 (MJD 55574), from 12:00 to 23:55 UTC. The orbital phase of the binary system during the observation was 0. 243, computed using the ephemerides in Wang,  Johnston & Manchester (2004) , and corresponds to 29. 3 days after the periastron passage. Six antennas participated in the observations: ATCA (as a phased array), Ceduna, Hobart, Mopra, Parkes, and Tidbinbilla (we note that the data from Tidbinbilla could not be properly calibrated and were not included in the final data reduction). The data were obtained with dual circular polarization. ATCA, Mopra, and Parkes recorded eight 16 MHz subbands (four for each right-and left-handed polarization) for a total data bit-rate of 512 Mbps per station, and the rest of the antennas recorded four 16 MHz subbands, for a total bit-rate of 256 Mbps.
The correlation of the data was conducted at the correlator in the International Centre for Radio Astronomy Research (ICRAR), which produced the final visibilities with an integration time of 2 seconds. Two passes of the correlator were conducted: one with all the data and for all sources, and a second one correlated only during the on-pulse of PSR B1259-63 using pulsar binning. The pulsar ephemerides were obtained from long-term timing observations conducted with Parkes. The observations were performed using phase referencing on the calibrator J1256-6449, located at 1. 2 • from PSR B1259-63. J1256-6449 was correlated at α J2000. 0 = 12 h 56 m 03. s 4032 and δ J2000. 0 = -64 • 49 ′ 14. ′′ 814, which has an absolute uncertainty in the ICRF (International Celestial Reference Frame) of 2. 8 mas in right ascension and in declination.
The cycle time was 6 minutes, spending half of the time on the phase calibrator and the target source alternatively. The sources J1332-6646 and J1352-4412 were observed as fringe finders. The data reduction was performed using the NRAO Astronomical Image Processing System (AIPS) 1. We applied a priori flagging on telescope off-source times because of antenna slewing, and ionospheric corrections obtained from total electron content (TEC) models based on GPS data obtained from the Crustal Dynamics Data Information System (CDDIS) data archive 2. The amplitude calibration was performed using the system temperatures measured at each station, although no antenna gain curves were available. The amplitude calibration was fixed by scaling the individual antenna gains by a factor obtained from the phase calibrator and fringe-finder models.
X-RAY OBSERVATIONS AND RESULTS We conducted an X-ray monitoring campaign on PSR B1259-63 with XMM-Newton Swift and Suzaku telescopes, covering the period between t p -131 days and t p + 79 days. These observations are summarized in Tables 3, 4 and 5. Each of these tables lists an identifier for the data set, UT date, MJD, time relative to periastron passage, true anomaly of the orbit, and exposure time for each observation.
XMM-Newton observations The log of the XMM-Newton data analyzed in this paper is presented in Table  3. In all XMM-Newton observations, the source   (Strüder et al. 2001)  detectors in the small window mode with a medium filter. The XMM-Newton Observation Data Files (ODFs) were obtained from the online Science Archive 5 and analyzed with the Science Analysis Software (sas) v11. 0. 0. During the data cleaning, all events that have energies above 10 keV and a count rate higher than 0. 5 cts s -1 for the PN or 0. 35 cts s -1 for the MOS detectors were removed. The event lists for spectral analysis were extracted from a 22. 5 ′′ radius circle for the MOS1 and MOS2 observations and from a 45 ′ ′ radius circle for the PN observations. For the spectral analysis, we made a simultaneous fit to the MOS1, MOS2 and PN data without imposing constraints on the intercalibration factors.
Swift observations Swift has closely monitored the PSR B1259-63 2010 periastron passage, and the data log is shown in Table  4. The Swift/X-ray Telescope (XRT)  (Gehrels et al. 2004 ) data were taken in photon 5 http://xmm. vilspa. esa. es/external/xmm data acc/xsa/index. shtml mode with 500 × 500 window size. We processed all the data with standard procedures using the FTOOLS 6  task xrtpipeline (version 0. 12. 6 under the HEAsoft package 6. 12). We extracted source events from a circular region with a radius of 1 ′ , and to account for the background we extracted events from a nearby circle of the same radius. Due to the low countrate (less than 0. 4 cts s -1 ), no pile up correction was necessary. After spectral extraction, the data were rebinned with a minimum of 25 counts per energy bin to allow χ 2 fitting.
Suzaku observations There were three Suzaku observations taken shortly after the 2010 periastron passage of PSR B1259-63 (see Table  5 ). The Suzaku observations were performed with three X-ray CCDs (the X-ray Imaging Spectrometers or XISs;  Koyama et al. 2007 ) in the range 0. 3-12 keV and the Hard X-ray Detector (HXD; Takahashi et al. 2007) in the range 13-600 keV. The XISs consists of one backilluminated CCD camera (XIS-1) and two front-illuminated CCDs (XIS-0 and XIS-3). In this paper we discuss only the results of the XIS observations, while the HXD data will be discussed in a separate paper. Our analysis was performed using the HEAsoft software package (version 6. 12). We analyzed the XIS data using pipeline processing version 2. 5. 16. 29. We made use of cleaned event files of the XIS observations, with standard event screening applied.
Spectral Analysis The X-ray spectral analyses were done with NASA/GSFC XSPEC v12. 7. 1 software package. A simple power law with a photoelectric absorption describes the data well, with no evidence for any line features. In Table  6  we present the results of the three parameter fits to the XMM-Newton, Swift and Suzaku data in the 0. 5-10 keV energy range. The uncertainties are given at the 1σ statistical level and do not include systematic uncertainties. The quality of the Swift data does not allow us to look for both spectral slope and absorption column density, so we decided to fix the latter to the value N H = 5 × 10 21 cm -2 consistent with the value found in the XMM-Newton and Suzaku observations. Similar to the observations of previous periastron passages, we found that several months before the periastron the spectral index was quite soft, Γ ∼ 1.
The analysis of the Fermi-Ł data in this paper is similar to the method used in  Abdo et al. (2011b). We used the P7SOURCE data set and the associated P7SOURCE V6 instrument response functions. The analysis was performed using the Fermi Science Tools 09-27-01 package 7. A zenith angle cut of < 100 • was applied to the data to reject atmospheric γ-rays from the Earth's limb. The standard binned maximum likelihood analysis was performed on events extracted from a 20 • × 20 • region around the location of PSR B1259-63 in the energy range 0. 1-300 GeV. The source model used in the maximum likelihood analysis included 2 years (2FGL) Fermi catalog  (Nolan et al. 2012 ) γ-ray sources within the analysed region, PSR B1259-63 and the diffuse Galactic and extragalactic components. Galactic diffuse emission was modelled using the gal 2yearp7v6 v0.
fits model, and the isotropic diffuse component was modelled using the iso p7v6source. txt model. The Ł data analysed in this paper covers the 4. 5 years period between 2008 August 4 and 2013 February 19. This covers the time period over which the pulsar was near apastron until well after the passage of the pulsar through the dense equatorial disk of the Be star. First we analysed the whole 4. 5 years of available data, modelling the spectrum of each point source with a catalog model. The normalizations and indexes of catalog point sources as well as the normalization of the extragalactic diffuse background were then fixed to their best-fit values in order to build the PSR B1259-63 lightcurve around the periastron. The power law index of PSR B1259-63 was fixed to the best-fit value (2. 86) obtained for the time period around the periastron passage.
H. E. S. S. OBSERVATIONS AND RESULTS The High Energy Stereoscopic System (H. E. S. S. ) is an array of imaging atmospheric Cherenkov telescopes located in the Khomas Highland of Namibia at an altitude of 1800 m above sea level. H. E. S. S. phase I (consisting of four 13 m diameter telescopes) is optimized for the detection of very high energy γ-rays in the range of 100 GeV to 20 TeV. The total field of view is 5 • and the angular resolution of the system is 0. 1 •. The average energy resolution is about 15%. The H. E. S. S. I array is capable of detecting point sources with a flux of 1% of the Crab nebula flux at a significance level of 5σ in 25 hours when observing at low zenith angles  (Aharonian et al. 2006). Observations of PSR B1259-63 around its 2010 periastron passage resulted in a rather small dataset compared to observations around the 2004  (Aharonian et al.
Possible connection of the Be star disk perturbation and the GeV Flare. In this paper we discuss the possibility that the detected GeV flare could be related to the reduction in the size/mass of the equatorial disk of the massive Be star in the system. Unfortunately, a gap in the Hα data does not allow us to make a firm identification of the start of the GeV flare with the start of the decrease of the equivalent width of the Hα line. The possibility of triggering the flare by the disk disruption event has to be verified with the future observations with denser coverage of the Hα measurements around the onset of the flare. The decrease of W Hα and the enhanced blue wing of the He I λ6678 line indicate the presence of strong perturbations in the interacting pulsar wind -stellar wind system. In the absence of perturbation of the Be star disk, the relativistic particles can escape from the system along a bow-shaped contact surface of the pulsar and stellar winds and in a direction opposite to the contact surface apex.
CONCLUSIONS In this paper, we have reported the results of multi-wavelength observations of PSR B1259-63 during its 2010 periastron passage. This was the first periastron for which complete monitoring in the high-energy gamma-ray band was available. These data have revealed a puzzling GeV flare occurring ≃ 30 days after the periastron  (Abdo et al. 2011b). Our multi-wavelength data show that the source behavior in the radio and X-ray band is qualitatively similar to the previous periastron passages and that there are no obvious counterparts of the GeV flare in other wavebands, from radio to TeV γ-rays. However, both in the X-rays and radio data from previous periastron passages there might be small irregularities in the behaviour of the lightcurves at the moment of the onset of the GeV flare.
The pulsar first induces growth of the disk in mass and size. The disk growth stops after the periastron passage and further interaction of the pulsar / pulsar wind with the disk leads to a perturbation of the disk structure, which possibly triggers the GeV band flare. This perturbation manifests itself in the reduction of the equivalent widths of the Hα and He I λ6678 lines. On the other hand, the disk disruption that we observe may be a normal occurrence in binary Be systems due to gravitational interactions near the close passage. Unfortunately, the optical spectroscopy data have a gap at the moment of the onset of the GeV flare, so we are not able to make an unambiguous link between the flare onset and changes in the Be star disk state. This possible link should be verified with a denser optical spectroscopy coverage of the periastron passage in 2014.
ACKNOWLEDGEMENTS The  Fermi LAT Collaboration  acknowledges support from a number of agencies and institutes for both development and the operation of the LAT as well as scientific data analysis. These include  NASA  and  DOE  in the United States,  CEA/Irfu  and  IN2P3/CNRS in France ,  ASI  and  INFN in Italy, MEXT ,  KEK , and JAXA in Japan, and the  K. A. Wallenberg Foundation , the  Swedish Research Council  and the  National Space Board in Sweden. Additional support from  INAF in Italy and CNES in France  for science analysis during the operations phase is also gratefully acknowledged. The Parkes radio telescope and the  Australian Long Baseline Array are part of the Australia Telescope  which is funded by the  Commonwealth Government  for operation as a National Facility managed by  CSIRO.
We thank our colleagues for their assistance with the radio timing observations. This work made use of the  Swinburne University of Technology  software correlator, developed as part of the  Australian Major National Research Facilities Programme  and operated under licence. A. N. is grateful to the  Swiss National Science Foundation  for the support under grant  PP00P2 123426/1. M. V. M. is grateful for support from the  National Science Foundation  under grant  AST-1109247  and from  NASA  under DPR number  NNX11AO41G. J. M. , M. R. and J. M. P. acknowledge support by the  Spanish Ministerio de Economía y Competitividad (MINECO)  under grants  AYA2010-21782-C03-01  and  FPA2010-22056-C06-02. J. M. acknowledges support by  MINECO  under grant  BES-2008-004564. M. R. acknowledges financial support from  MINECO  and  European Social Funds  through a  Ramón y Cajal fellowship.
J. M. P. acknowledges financial support from  ICREA Academia. Based on observations made with  ESO Telescopes at the La Silla Paranal Observatory  under programme  ID 086. D-0511. This work was supported by the  Centre National d'Etudes Spatiales (CNES) , based on observations obtained with MINE -the  Multiwavelength INTEGRAL NEtwork. The authors thank the  International Space Science Institute  ( ISSI, Bern ) for support within the  ISSI team  " Study of Gammaray Loud Binary Systems " and  SFI/HEA Irish Centre for High-End Computing (ICHEC)  for the provision of computational facilities and support.
Context. Debris discs are thought to be formed through the collisional grinding of planetesimals, and then can be considered as the outcome of planet formation. Understanding the properties of gas and dust in debris discs can help us comprehend the architecture of extrasolar planetary systems. Herschel Space Observatory far-infrared (IR) photometry and spectroscopy have provided a valuable dataset for the study of debris discs gas and dust composition. This paper is part of a series of papers devoted to the study of Herschel-PACS observations of young stellar associations. Aims. This work aims at studying the properties of discs in the Beta Pictoris Moving Group (BPMG) through far-IR PACS observations of dust and gas. Methods. We obtained Herschel-PACS far-IR photometric observations at 70, 100, and 160 µm of 19 BPMG members, together with spectroscopic observations for four of them.
2005). Only the β Pic debris disc appears to have a full inventory of gaseous species, both atomic and molecular (see e. g. Lagrange et al. 1998; Thi et al. 2001; Roberge et al. 2006). The Herschel Space Observatory  (Pilbratt et al. 2010 ) has produced a valuable dataset for the study of circumstellar environments, allowing both the dust in the continuum and gas emission in the far-IR to be observed. The Photodetector Array Camera & Spectrometer-PACS  (Poglitsch et al. 2010)  can study debris discs with high sensitivity in the wavelength range  (55-220 µm)  where cold dust emission peaks. PACS spectroscopy allows for detecting a few bright emission lines for molecular species such as CO, H 2 O, and OH and the strong cooling lines of  [OI]  and  [CII]  at 63 and 158 µm, respectively. Some Herschel key time programmes, such as DUNES  (Eiroa et al.