dataesr/scientific-paragraphs-categorization huggingface dataset:
The changes observed in physics parameters are taken as systematic uncertainties. A systematic uncertainty is included which arises from the limited size of the simulated data sample used to determine ε Ω. The lower decay time acceptance is included in the PDF using the binned functions described in Sect. 6. A systematic uncertainty is determined by repeating the fits with the bin values varied randomly within their statistical precision. The standard deviation of the distribution of central values obtained for each fit parameter is then assigned as the systematic uncertainty. The slope of the acceptance correction at large lifetimes is β = (-8. 3±4. 0)×10 -  ps -1. This leads to a 4. 0×10 -3 ps -1 systematic uncertainty on Γ s. B 0 s → J/ψ K + K -signal events in data compared to simulated B 0 s → J/ψ φ signal events.
605 ± 0. 009 (stat) ± 0. 009 (syst) ps -1 , which, in the limit φ s = 0 and |λ| = 1, corresponds to Γ H. This result supersedes that reported in Ref. [46]. The uncertainty on the B 0 lifetime  [7]  used to calibrate the decay time acceptance is included in the statistical uncertainty. The remaining systematic uncertainty is evaluated by changing the background model and assigning half of the relative change between the fit results with and without the decay time acceptance correction included, leading to uncertainties of 0. 011 ps and 0. 021 ps, respectively. The total systematic uncertainty obtained by adding the two contributions in quadrature is 0. 024 ps. 12 Combined results for B 0 s → J/ψK + K -and B 0 s → J/ψπ + π -datasets This section presents the results from a simultaneous fit to both B 0 s → J/ψK + K -and B 0 s → J/ψπ + π -datasets.
Results of combined fit to the B 0 s → J/ψK + K -and B 0 s → J/ψπ + π -datasets. The first uncertainty is statistical and the second is systematic. Parameter Value Γ s [ ps -1 ] 0. 661 ± 0. 004 ± 0. 006 ∆Γ s [ ps -1 ] 0. 106 ± 0. 011 ± 0. 007 |A ⊥ | 2 0. 246 ± 0. 007 ± 0. 006 |A 0 | 2 0. 523 ± 0. 005 ± 0. 010 δ [rad] 3. 32 +0. 13 -0. 21 ± 0. 08 δ ⊥ [rad] 3. 04 ± 0. 20 ± 0. 08 φ s [rad] 0. 01 ± 0. 07 ± 0. 01 |λ| 0. 93 ± 0. 03 ± 0. 02.
Acknowledgements 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) ;  NSFC (China) ;  CNRS/IN2P3  and  Region Auvergne (France) ;  BMBF ,  DFG ,  HGF  and  MPG (Germany) ;  SFI (Ireland) ;  INFN (Italy) ;  FOM  and  NWO  (The Netherlands); SCSR (Poland);  ANCS/IFA (Romania) ;.
Fit description The yields of signal and background events in the data are determined in the mass range 5. 35-5. 85 GeV/c 2 using unbinned, extended maximum likelihood fits, for the Λ 0 b → Λµ + µ - and the Λ 0 b → J/ψ Λ modes. The likelihood function has the form L = e -(N S +N B +N P ) × N i=1 [N S P S (m i ) + N B P B (m i ) + N P P P (m i )] , (1) where N S , N B and N P are number of signal, combinatorial and peaking background events, respectively, and P j (m i ) are the corresponding probability density functions (PDFs). The mass of the Λ 0 b candidate, m i , is determined by a kinematic fit of the full decay chain in which the proton and pion are constrained such that the pπ -invariant mass corresponds to the Lbaryon mass  [29]. The signal shape, in both Λ 0 b → Λµ + µ -and Λ 0 b → J/ψ Λ modes, is described by the sum of two Gaussian functions that share a common mean but have independent widths.
Acknowledgements This Letter is dedicated to the memory of our friend and colleague  Javier Magnin. 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) ;  NSFC (China) ;  CNRS/IN2P3  and  Region Auvergne (France) ;  BMBF ,  DFG ,  HGF  and  MPG (Germany) ;  SFI (Ireland) ;  INFN (Italy) ;  FOM  and  NWO  (The Netherlands); SCSR (Poland);  ANCS/IFA (Romania) ;  MinES, Rosatom ,  RFBR  and  NRC "Kurchatov Institute" (Russia) ;  MinECo, XuntaGal and GENCAT (Spain) ;  SNSF  and  SER (Switzerland) ;  NAS Ukraine (Ukraine) ;  STFC  ( United Kingdom );  NSF (USA).
SOAR Narrow-band optical imaging was performed with the 4. 1 m Southern Astrophysical Research (SOAR) telescope on July 8, 2008 (UT) using the SOAR Optical Imager (SOI). The night was photometric with a seeing of around 1. 0. The CTIO 6693/76 narrow-band filter was used for the Hα+[N II] lines, and the CTIO 6520/76 filter for the continuum. Three 600 sec exposures were taken with the 6693/76 filter and three 360 sec exposures with the 6520/76 filter. Each image was reduced using the standard procedures in the IRAF MSCRED package and the spectroscopic standard EG 274. The pixels were binned 2×2, for a scale of 0. 154 arcsec per pixel. More details on the SOI data reduction and the continuum subtraction can be found in  Sun et al. (2007). The net (continuum subtracted) Hα image has been published in Sun (2012).
HST Observations were made using the Wide Field Camera 3 (WFC3) UVIS channel on the Hubble Space Telescope (HST) on 2011 February 2 in the F300X, F555W and F814W filters. The total exposure times in each filter were 5427, 1335 and 1044 s respectively. Throughput of the F555W filter at the redshifted wavelengths of the strong emission lines, Hα+[N II] ∼6700 Å, is only of order a few percent. Standard procedures were used to bias-subtract and flat-field the data frames and to drizzle the science frames together, these procedures use the software DrizzlePac and are described in the HST WFC3 data handbook. The optical images are shown in Figs. 2, 3 and 4. No corrections for reddening have been made to the images, although a relative intrinsic E(B -V ) image of the galaxy is shown in the right-hand panel of Fig.
To convert the map to E(B -V ) units requires the assumption of an attenuation curve. We assume the  Cardelli et al. (1989)  extinction law and calculate A λ /AV from the HST filters. We use the pivot wavelengths of the F555W and F814W filters given in the HST WFC3 data handbook as the effective wavelength of the filters. Due to the broad nature of the filters and the low redshift of our object, no K-correction is made.
The result is that the eastern side of our field-of-view has additional coverage of the redshifted spectral line of [O III]λ5007. The total exposure time of these observations was 4500 seconds. The data were reduced by the VIPGI 1  pipeline (see  Scodeggio et al. 2005  for a description of VIPGI). The data cubes were combined, transmission corrected, sky absorption and emission corrected and corrected for Galactic extinction (E(B -V ) = 0. 060 ± 0. 001) using a set of IDL routines. The O2 telluric absorption feature at ∼ 6800 -6900 Å falls over the [S II] doublet and as such warranted special attention. We use observations of two standard stars taken just before and after the science observations to correct for this feature. Due to the nature of the filamentary system we choose to bin the data based on the surface brightness of [N II]λ6583 emission, the strongest line observed, using the contour binning technique of  Sanders (2006)  and binning to a signal-to-noise of 10.
X-RAY DATA Chandra X-ray data of Abell 3581, with an exposure time of 85 ks, were taken on 2011 January 3rd (ObsID 12884). The observations were conducted with the Advanced CCD Imaging Spectrometer (ACIS). The data was reprocessed using the CIAO  (Fruscione et al. 2006 ) ACIS PROCESS EVENTS tool, applying the VFAINT processing to lower the non X-ray background. To look for contaminating flares, we examined the lightcurve of ACIS CCD 5 between 2. 5 and 7 keV in 200s bins. A sigma clipping algorithm was used to search for flared periods, of which there were none. Standard blank-sky background datasets were used, re-projected to match the observation and with the exposure time adjusted to match the background-dominated 9 to 12 keV observational count rate. To make the spectral maps, we used the Contour Binning algorithm  (Sanders 2006 ) to create regions with a signal to noise ratio of 20 (around 400 counts).
The image is in the energy range 0. 5-7 keV. Despite the asymmetry of the cluster, the model fits the data reasonably well. However, deviations from the fit are seen at ∼50 arcsec, ∼80 arcsec, and in the central 20 arcsec. These deviations correspond to surface brightness edges which will be examined further in Section 5. 2. Double-β fits to individual sectors and empirical azimuthally averaged profiles are also fit and removed from the surface brightness images to highlight substructure. For the temperature and density profiles across the 'bubble' and 'cold front' (see Section 5. 2) we extracted spectra from the regions of interest, and fitted the spectrum within Xspec (version 12. 8. 0a 2 ) with an absorbed MEKAL model. The regions for the spectral analysis were chosen such that there were at least 3000 counts in each bin.
JVLA High frequency radio observations of Abell 3581 were obtained with the NRAO 3  JVLA  (Perley et al. 2011 ) at L band (1-2 GHz). Due to the low declination of the target, the observations were undertaken in the hybrid BnA configuration on 2012 Sept. 08 (project ID: SB0410). The extended north arm of the hybrid configuration allows for a more circular beam for the target. The observations were a total of 4 hours and were taken with two 512 MHz wide basebands centered at 1314 and 1686 MHz. We configurated the WIDAR correlator so that each baseband had 8 subbands with 64 channels per subband for a frequency resolution of 1 MHz. We used   3C286 as our absolute flux and bandpass calibrator and J1351-1449 as our phase calibrator. The data were flagged and calibrated using NRAO's Common Astronomy Software Applications (CASA 4  ) data reductions package.
GMRT Abell 3581 was observed with the GMRT at 235 MHz and 610 MHz (project 18-009) in May 2010, for approximately 3 hours, including calibration overheads. The observations were made using the dual-frequency mode. The 610 MHz data were collected using the upper and lower side bands (USB and LSB) with an observing bandwidth of 16 MHz each. Only the USB was used at 235 MHz, with a bandwidth of 8 MHz. We chose the default spectral-line observing mode, with 128 channels for each band at 610 MHz (64 channels at 240 MHz) and a spectral resolution of 125 kHz/channel. The datasets were calibrated and reduced using the NRAO Astronomical Image Processing System package (AIPS) as described in  Giacintucci et al. (2011). Self-calibration was applied to the data to reduce residual phase variations and improve the quality of the final images.
Morphology The BGG in Abell 3581 has a smooth, relaxed appearance in broad band optical images. However, the narrow band Hα+[N II] image shows striking filaments of ionised gas. These filaments connect to the nucleus in the easterly and westerly directions, parallel to the current radio axis, then curve sharply towards the north and south respectively (see Fig. 2 ). In the easterly direction the filaments arc round and apparently encase one of the previously detected X-ray bubbles. The filament system is complex, formed of at least a few strands in each direction and is not one continuous structure. Filaments of this nature have now been observed in many massive galaxies dominating the centres of X-ray bright cool core groups and clusters. Our VLT VIMOS IFS data show the emission lines of Hα, [N II], [S II] and [O I] in the inner filament all share the same morphology.
The 'weather' is perhaps still generated by bulk sloshing motions but the cooler gas is now dredged up from the nucleus rather than cooling from the core. NGC 4636 differs in that its spiral arms are hotter, not colder than the surrounding medium suggesting these are the result of shocks driven into the ICM due to the inflation of the bubbles. In Abell 3581 the X-ray data appears to favour a single spiral structure. The slow rotation in the radio emission and the directional change along the filaments indicates the rise direction differences are not due to jet precession and that some other process changed the bubbles direction after it had left the nucleus. This is unlikely to be simply the path of least pressure as there is a rotational symmetry to the directional change in the filaments.
ACKNOWLEDGMENTS Support for this work was provided by  NASA  through award number  1428053  issued by  JPL/Caltech. REAC acknowledges a scholarship from the  Cambridge Philosophical Society  and a  Royal Astronomical Society  grant. MS is supported by the  NASA  grants  GO1-12103A ,  NNH12CG03C  and  HST-GO-12373. TEC was supported in part for this work by the  National Aeronautics and Space Administration , through  Chandra Award Number   GO1-12159Z. Basic research in radio astronomy at the  Naval Research Laboratory  is supported by 6. 1 Base funding. SG acknowledges the support of  NASA  through  Einstein Postdoctoral Fellowship   PF0-110071  awarded by the  Chandra X-ray Center (CXC) , which is operated by  SAO. SWA acknowledges support from the  U. S. Department of Energy  under contract number  DE-AC02-76SF00515.
PEJN was supported by  NASA  contract  NAS8-03060. CLS was supported in part by  NASA   Chandra Grant   G01-12169X. We thank the reviewer of this article,  Dr G. Tremblay , for his constructive comments and suggestions. REAC would also like to thank  Anja von der Linden  and  Adam Mantz  for interesting and enlightening discussions. 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.
STACKING MEASUREMENTS We base our study on the Herschel /SPIRE imaging of the COSMOS field obtained within the framework of the Her-MES key program  (Oliver et al. 2012). Most of the objects from our UV-selected samples are not detected individually in these images, so we rely on a stacking analysis. We use the same methods as those presented in  Heinis et al. (2013)  to measure flux densities using stacking 2. We recall here only the main characteristics of the methods. We perform stacking using the IAS library  (Bavouzet 2008; Béthermin et al. 2010)   3. We use mean stacking, without cleaning images from detected sources. We showed in  Heinis et al. (2013)  that using our method or median stacking with cleaning images from detected sources, yields similar results. We correct the stacking measurements for stacking bias, using extensive simulations of the detection process of the sources.
CONCLUSIONS We studied the FIR properties of large samples of UVselected galaxies at 1. 5 < z < 4, by combining the COS-MOS multiwavelength dataset with the HerMES/Herschel SPIRE imaging. We measured by stacking the average IR luminosity as a function of UV luminosity, stellar mass, and both. Our results can be summarised as follows: (i) At z ∼ 1. 5, there is a good correlation between LIR and LFUV(8 × 10 9 < LFUV/L⊙ < 5 × 10 10 ), while at z ∼ 3 and z ∼ 4, LIR and LFUV are not well correlated. (ii) Consequently, the ratio LIR /LFUV at z ∼ 3, 4 is decreasing with LFUV. (iii) The average dust attenuation (as traced by the LIR /LFUV ratio) is well correlated with stellar mass at 1. 5 < z < 4, and does not show significant evolution in this redshift range, in the range of masses we explore. (iv) We investigated the joint dependence of dust attenuation with stellar mass and LFUV.
ACKNOWLEDGMENTS We thank the referee for useful comments and suggestions. S. H. and V. B. acknowledge support from the  Centre National d'Etudes Spatiales. We thank the  COSMOS team  for sharing data essential to this study. SPIRE has been developed by a consortium of institutes led by  Cardiff Univ. (UK)  and including:  Univ. Lethbridge (Canada) ;  NAOC (China) ;  CEA ,  LAM (France) ;  IFSI ,  Univ. Padua (Italy) ;  IAC (Spain) ;  Stockholm Observatory (Sweden) ;  Imperial College London ,  RAL ,  UCL-MSSL ,  UKATC ,  Univ. Sussex (UK) ; and  Caltech ,  JPL ,  NHSC ,  Univ. Colorado (USA). This development has been supported by national funding agencies:  CSA (Canada) ;  NAOC (China) ;  CEA ,  CNES ,  CNRS (France) ;  ASI (Italy) ;  MCINN (Spain) ;  SNSB (Sweden) ;  STFC ,  UKSA (UK) ; and  NASA (USA).
I. INTRODUCTION Extensions to the Standard Model (SM), such as quark/lepton compositeness and large extra dimensions, predict modifications to the SM dilepton invariant mass spectra. This paper presents a comparison of the number of expected and observed events at high mass in the dielectron and dimuon datasets collected by the ATLAS detector  [1]  in 2011. These events resulted from protonproton collisions produced at √ s = 7 TeV by the LHC  [2]. The data are interpreted in the context of contact interactions (CI) and virtual graviton exchange in the Arkani-Hamed-Dimopoulos-Dvali (ADD) model  [3]. In the SM, quarks and leptons are fundamental particles. However, if they are composite particles, with at least one common constituent, the interactions of these constituents would manifest themselves through an effective four-fermion contact interaction at energies well below the compositeness scale.
IV. EVENT SELECTION AND COMPARISON BETWEEN EXPECTED AND OBSERVED YIELDS This analysis follows the same event selection as the search for new heavy resonances  [59]  in the dielectron channel but uses a somewhat tighter selection in the dimuon channel. The data sample was collected during LHC operation in 2011 and corresponds to a total integrated luminosity of 4. 9 and 5. 0 fb -1 in the e + e -and µ + µ -final states, respectively. The events recorded by the ATLAS detector were selected by requiring that they pass specific triggers. The trigger for the dielectron dataset required the presence of two electromagnetic clusters consistent with originating from electrons with transverse momentum p T above 20 GeV, whereas events in the muon dataset were required to pass at least one of two single-muon triggers with p T thresholds of 22 GeV and 40 GeV.
The multijet and W +jets backgrounds are not negligible in the dielectron channel. They are estimated primarily from the data using several methods  [59]. The first method determines the multijet background from the data and relies on the MC simulation for the W +jets contribution. The background is measured with a template built by reversing one of the electron identification criteria and normalized to data in the range 70 < m ee < 200 GeV. Another independent method that is sensitive to both multijet and W +jets backgrounds uses jet-enriched data samples either from jet triggers or from the same trigger used to select the events in this analysis. The method relies on jet misidentification rates, defined as the number of jets that pass the full electron selection divided by the number that pass a loose electron selection obtained by reversing one of the identification criteria.
IX. CONCLUSIONS A search for contact interactions and large extra dimensions has been performed in dielectron and dimuon events produced in LHC proton-proton collisions at √ s = 7 TeV. The data sample corresponds to an integrated luminosity of 4. 9 (5. 0) fb -1 of pp collisions in the dielectron (dimuon) channel recorded with the ATLAS detector. No significant deviation from the Standard Model is observed in the dilepton mass distributions. Using a Bayesian approach with a prior flat in 1/Λ 2 , as was done in most previous searches at hadron colliders, the following 95% C. L. limits are set on the energy scale of contact interactions: Λ -> 12. 1 TeV (Λ + > 9. 5 TeV) in the di-TABLE VIII. Observed 95% C. L. lower limits on MS (in units of TeV), including systematic uncertainties, for ADD signal in the GRW, Hewett and HLZ formalisms with K factors of 1.
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 and  ERC ,  European Union ;  IN2P3-CNRS ,  CEA-DSM/IRFU , France; GNSF, Georgia; BMBF,  DFG ,  HGF ,  MPG  and  AvH Foundation , Germany; GSRT, 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,.
The longest buckle-free fiber sections had lengths between 150 mm and 200 mm. A visual inspection of the samples indicated good optical quality without obvious defects. The absorption coefficient was measured at 633 nm (HeNe laser) for 18 samples from three different growth runs with a length from 2. 1 cm to 16. 5 cm. The beam waist was kept smaller than the sample diameter in order to avoid influences from the outer surface. Taking into account the losses at the end faces due to Fresnel reflection the resulting absorption coefficients were in the range of <0. 005 cm -1 to 0. 045 cm -1 with the majority of samples near 0. 01 cm -1. The absorption was essentially independent of the sample thickness. For comparison, recently reported data for conventionally grown bulk material were in the range of 0.
Therefore, line-driven winds are not expected to be relevant unless shielding from the X-ray irradiation is taking place in some UV-emitting part of the disc  (Proga & Kallman 2002, hereafter PK02). In contrast, the same X-rays that prevent UV line opacity can heat low density gas to a temperature ∼ 10 7 K and potentially drive thermal winds. Assuming the accretion disc is concave and exposed to X-rays from the central source, its upper layers are expected to puff up and expand into an atmosphere, corona or wind (Jimenez-Garate et al. 2002). The upper boundary of the atmosphere is the Compton temperature corona, which is less dense and hotter than the underlying atmosphere. The evaporated photoionised plasma will remain bound to the disc as an atmosphere/corona or be emitted as a thermal wind, depending on whether the thermal velocity exceeds the local escape velocity  (Begelman et al.
88 × 10 -2 T -1/2 IC8 L Edd (see their eq. 4. 4), where L Edd is the Eddington luminosity and T IC8 is the Compton temperature in units of 10 8 K. Therefore, for T IC ∼ 1. 3 × 10 7 K the wind could be gravitationally inhibited for luminosities below 0. 16 L Edd (see their Fig. 17 ). Consequently, for NS systems, at a disc radius of ∼2. 6 × 10 10 cm an isothermal wind will develop for luminosities above ∼ 3×10 37 erg s -1 , while such a wind could be inhibited by gravity at lower luminosities. For larger radii, a steadily heated free wind could develop already at luminosities below ∼ 3×10 37 erg s -1. Interestingly, PK02 found that when they included the radiation force, although the line force is dynamically unable to drive a wind, the radiation force due to electrons can be important for very luminous systems: it lowers the effective gravity and subsequently the escape velocity and allows a hot robust disc wind to be already produced at ∼ 0.