dataesr/scientific-paragraphs-categorization huggingface dataset:
Conclusions We have shown that the lifetime of CDM must be above 160 Gyr (or 200 Gyr assuming that BICEP2 has detected gravitational waves), even for the most conservative case where CDM decays entirely into Dark Radiation. This is a model independent bound, since it relies only on the gravitational interactions of CDM and its decay product which can not be avoided in any particle physics model. If the decay product is allowed to have a mass, we would expect For the + {Γ dcdm , r, Ω k } model, comparison of the results for {ω dcdm+dr , Γ dcdm , r, Ω k } using the dataset set A (blue contours) and B (yellow/orange contours), for the 1d and 2d posterior distributions. The contours represent 68% and 95% confidence levels. this bound to worsen depending on the mass of the daughter particles. We will consider this scenario in a future publication.
Acknowledgements GM acknowledges support by the  Istituto Nazionale di Fisica Nucleare I. S. TASP  and by  MIUR ,  PRIN Fisica Teorica Astroparticellare. BA, JL  and TT received support from the  Swiss National Foundation. At LAPTh , this activity was developed coherently with the research axes supported by the  ANR Labex  grant ENIGMASS.
Scanning electron microscope images The OMLs were investigated using scanning electron microscopy (SEM, Hitachi S3400N or Zeiss Ultra60), optical microscopy (UMA600, Agilent), and a stylus profilometer (Dektak 3ST, Veeco) in order to determine the quality of the cavity surfaces and the perpendicularity and parallelism of the facets. The samples were coated by a 10 nm thick gold layer prior to SEM imaging, which was subsequently removed with potassium iodide. SEM images of OMLs of various shapes, including structures with rounded features, are presented in Fig. 2. They were analyzed using image analysis software (ImageJ, NIH) to obtain the widths, lengths, and heights of the OMLs. The SEM images demonstrate that cavities with high aspect ratios, very few defects, and almost arbitrary shapes can be obtained from laser dyedoped resins with both fabrication techniques.
The error bars correspond to the width of the peaks in the FTs of the lasing spectra. The optical length of the diamond orbit is indicated by the blue line, using a refractive index n g = 1. 51, determined by prism coupling and ellipsometry. The good agreement between the blue line and the data points confirms that the observed families of modes are related to the diamond orbit. Furthermore, Fig. 6(b)  shows the optical lengths obtained from the FTs of the lasing spectra for a series of cavities with varying height but identical side length a = 58 µm. This shows that the optical length is independent of the cavity height within the error margins. This is a clear indication that the underlying PO is two-dimensional, i. e. , it rests within the x-y-plane and has no reflections at the top and bottom facets.
Acknowledgments The work at the  Georgia Institute of Technology  was supported by the  U. S. Air Force Office of Scientific Research, BioPAINTS MURI Program  (Grant No. FA9550-09-0669 ). The authors thank  Dr. Canek Fuentes Hernandez  for assistance with refractive index measurements. The authors thank  Gilles Clavier ,  Rachel Méallet-Renault  and  Isabelle Leray  for fruitful discussions,  Maxime Boudreau  for ellipsometry measurements, and  Valentina Emiliani ,  Eirini Papagiakounou , and  Marc Guillon  for preliminary MPL experiments. S. B. gratefully acknowledges funding from the  PALM LABEX  and the  European Union Seventh Framework Programme  ( FP7/2007-2013 ) under Grant Agreement No. 246. 556. 10.
Finite Element Simulation Considering the problem, a 2-D axisymmetric FE model is built. For this study, the commercial FE code ABAQUS/Standard (version 6. 12-1) is used with implicit method. Considering a maximum indentation depth of 0. 5 µm, the dimension of the whole model was set to 50 µm×50 µm, which is assumed to be large enough to approximately represent a semi-infinite body. The whole model is considered as a representative volume element (RVE) loaded uniformly. Besides, considering the distributions of stress and strain fields in depth and in width due to the indentation test, the mesh in the zone beneath the indenter (5 µm×5 µm) was refined to guarantee the accuracy of the FE model. Moreover, simulations with different mesh size were performed to check the mesh sensitivity (results are not shown here).
Spectral analysis In order to investigate the electronic resonance effect in multiplex TSFG spectra, we have analyzed obtained data in the following procedure. First, we obtained TSFG spectra of the sample at bulk a/bulk b interface (I a/b ). For the determination of the signal at the interface, the intensity of TSFG signal was plotted along the axial direction as shown in Fig. 4(b). The peak position should correspond to the center position of the interface. In order to take account of the aberration originated from the tight-focusing condition, the multiplex TSFG spectrum was averaged over the interface within ± 2 μm. The averaged spectrum is denoted as the multiplex TSFG spectrum at bulk a/bulk b interface, I a/b. Second, the TSFG spectrum at the upper glass/solution interface was used as the sample spectrum, and was divided with that at the glass/air interface as a reference spectrum in order to obtain intensity-corrected spectra.
Acknowledgments This work is supported by  JSPS-MESR-MAEE bilateral joint research project (SAKURA program ) and The  NOVARTIS Foundation (Japan) for the Promotion of Science. The authors thank the  LEUKOS company  for technical support with the dual-output supercontinuum light source. The authors gratefully acknowledge  J. Ukon ,  UKON CRAFT SCIENCE, Ltd. for assisting with a fruitful collaboration between Japanese and  French labs.
Acknowledgements We thank  Massimo Passera ,  Andrea Wulzer ,  Anatoly Dymarsky  and  Roberto Contino  for valuable discussions. B. B thanks  Slava Rychkov ,  Andi Weiler ,  Alfredo Urbano ,  Filippo Sala  and  Borut Bajc  for useful discussions, and  Flip Tanedo  for reading the manuscript. B. B. would like to express special thanks to the  Mainz Institute for Theoretical Physics (MITP)  for its hospitality and support. R. T. thanks  Adam Falkowski  for valuable comments and  Christoffer Petersson  and  Andrea Thamm  for fruitful conversations. B. B. is supported in part by the  MIUR-FIRB  grant  RBFR12H1MW , and by the  Agence Nationale de la Recherche  under contract  ANR 2010 BLANC 0413 01. The work of R. T. was supported by the  ERC  Advanced Grant no. 267985 DaMeSyFla and by the  Research Executive Agency (REA)  of the  European Union  under the Grant Agreement number PITN-GA-2010-264564 LHCPhenoNet.
6 ± 0. 8) × 10 -6  [20]. Direct CP violation, defined as A CP ≡ (BF b -BF b )/(BF b + BF b ), where b (b) denotes a B (B) parent, is expected to be suppressed well below the 1% level in both exclusive and inclusive b → sℓ + ℓ -transitions  [25] [26] [27] [28] ; however, in beyond-SM models with four quark generations, significant enhancements are possible, particularly in the high-q 2 region  [10, 11]. The BABAR  [29]  and Belle  [30]  Collaborations have previously published B → X s ℓ + ℓ -BFs based on a sum over exclusive final states using only ∼ 25% of each experiment's final dataset. More recently, both collaborations (along with LHCb and CDF) have published BFs, and time-integrated rate and angular asymmetries, for the exclusive decays B → K ( * ) ℓ + ℓ -  [31] [32] [33] [34] [35] [36] [37].
The uncertainty in the extrapolation to the inclusive rate is characterized through variations that attempt to quantify our lack of knowledge of the true dilepton mass-squared distribution and hadronization of the X s system beyond the specific final states and m Xs range that we observe. We average the most recent B → K ( * ) ℓ + ℓ -BFs  [57] , excluding BABAR results, and use the latest BABAR result  [58]  for the ratio of chargedto-neutral Υ (4S) → bb decays, Γ(B + B -)/Γ(B 0 B 0 ) = 1. 006 ± 0. 036 ± 0. 031. Each of these terms is varied by its one-standard-deviation uncertainty. We examine an alternate m Xs transition point of 1. 0 GeV/c 2 between the B → K ( * ) ℓ + ℓ -and B → X s ℓ + ℓ -models. To account for hadronization uncertainties in m Xs > 1. 1 GeV/c 2 events, we generate 20 simulated datasets with varied JETSET tunings, two different values for the B-meson Fermi motion, and two different b-quark mass values.
We search for CP violation in each q 2 bin by dividing our dataset into four disjoint samples according to lepton identity (e + e -or µ + µ -) and the B or B flavor as determined by the kaon and pion charges of the X s system. Modes with X s = K 0 S , K 0 S π 0 or K 0 S π + π -are not used; and, because we perform no model-dependent extrapolation of signal rates, we measure A CP only for the particular combination of final states used here. We simultaneously fit all four datasets, sharing a single value of A CP as a free parameter, using the BFs fit model described above. Our A CP results are shown in Table  I ; a plot of the results as a function of q 2 is included as part of our supplemental EPAPS material  [56]. We analyze the vetoed J/ψ dataset, where CP violation is ex-pected to be trivially small  [69, 70] , with the same fitting methodology used for the signal q 2 bins; we find A ccs CP = 0.
Introduction This Supplemental Material includes: • Figure  2 , plotting the A CP results as a function of q 2 ; • Figure  3 , plotting the differential branching fraction as a function of m Xs ; • Table  II , giving in each individual q 2 and m Xs bin the fitted raw number of signal events N sig , as well as the fitted number of random combinatorial BB background events N BB present in the signal enhanced region with m ES > 5. 27 GeV/c 2 ; • Tables III-VIII, detailing individual contributions to the "additive" and "multiplicative" branching fraction systematics (as defined in the article main text), and the model-dependent extrapolation systematics; and • Figures 4-23, which show the projections of our branching fraction fits onto their respective datasets. ACP results. Results for ACP as a function of q 2.
The data used in this analysis are from pp collisions recorded by the LHCb experiment, corresponding to an integrated luminosity of 1. 0 fb -1 at a center-of-mass energy of 7 TeV and 2. 0 fb -1 at 8 TeV. The LHCb detector  [23]  is a single-arm forward spectrometer covering the pseudorapidity range 2 < η < 5, designed for the study of particles containing b or c quarks. The detector includes a high-precision tracking system consisting of a silicon-strip vertex detector surrounding the pp interaction region, a large-area silicon-strip detector located upstream of a dipole magnet with a bending power of about 4 Tm, and three stations of silicon-strip detectors and straw drift tubes placed downstream  [24]. The combined tracking system provides a momentum measurement with relative uncertainty varying from 0.
For the signal yields, the systematic uncertainty is obtained by varying the invariant mass fit functions of the two modes. The effect of geometrical acceptance is evaluated by comparing the efficiencies obtained from samples simulated with different data taking conditions. The systematic uncertainty due to the trigger requirement is studied by comparing the trigger efficiency in data and simulated samples, using a large J/ψ sample  [7, 43]. The impact of the uncertainty of the B + c lifetime is evaluated from the variation of the relative efficiency when the B + c lifetime is changed by one standard deviation of the LHCb measurement  [12]. The systematic uncertainty associated with the reconstruction efficiency of the two additional hadron tracks, p and p, in the B + c → J/ψ ppπ + mode compared to the B + c → J/ψ π + mode, is also studied.
The efficiency calculated using the observed distribution in data relative to the efficiency determined using the simulated decay model is 0. 949 ± 0. 067, where the uncertainty is statistical. Since the value is consistent with unity within the uncertainty, no correction to the efficiency is made and a systematic uncertainty of 6. 7% is assigned. The total systematic uncertainty associated with the relative branching fraction measurement is 8. 9%. As a result the ratio of branching fractions is measured to be B(B + c → J/ψ ppπ + ) B(B + c → J/ψ π + ) = 0. 143 + 0. 039 -0. 034 (stat) ± 0. 013 (syst), which is consistent with the expectation from the spectator decay model assuming factorization  [45] , B(B + c →J/ψ ppπ + ) B(B + c →J/ψ π + ) ∼ B(B 0 →D * -ppπ + ) B(B 0 →D *π + ) = 0. 17 ± 0.
02. The branching fractions for B 0 → D * -ppπ + and B 0 → D * -π + decays are taken from Ref. [28]. In conclusion, the decay B + c → J/ψ ppπ + is observed with a significance of 7. 3 standard deviations, using a data sample corresponding to an integrated luminosity of 3. 0 fb -1 collected by the LHCb experiment. Thi is the first observation of a baryonic decay of the B + c meson. The branching fraction of this decay relative to that of the B + c → J/ψ π + decay is measured. The mass of the B + c meson is measured to be 6274. 0 ± 1. 8 (stat) ± 0. 4 (syst) MeV/c 2. In combination with previous results by LHCb  [7, 11] , the B + c mass is determined to be 6274. 7 ± 0. 9 (stat) ± 0. 8 (syst) MeV/c 2. [9] LHCb collaboration, R.
The rich X-ray phenomenology has not yet been fully exploited, leaving a number of open questions. Here we report the results of deep joint XMM-Newton and Chandra observations aimed at searching for pulsations and performing a phaseresolved spectral analysis of the radio-quiet Fermi-LAT pulsar J1813-1246 (hereafter, J1813) in the soft X-ray band (0. 3-10 keV). Our X-ray observations also enable us to study the possible extended emission from its pulsar wind nebula (PWN). J1813 was discovered within a few months of the launch of Fermi, in a blind pulsation search of LAT data  (Abdo et al. 2009a ). It is one of the brightest γ-ray pulsars, making it into the Fermi-LAT Bright Source List as 0FGL J1813. 5-1248 (Abdo et al. 2009b ). Its period P ∼ 48. 1 ms and period derivative Ṗ ∼ 1. 76 × 10 -14 s s -1 point to a spin-down energy loss rate Ė ∼ 6.
Observations and data reduction Our deep XMM-Newton observation of J1813 was performed on 2013 March 10 and lasted 108. 9 ks. The PN camera  (Struder et al. 2001 ) of the EPIC instrument was operating in Small Window mode, with a time resolution of 5. 6 ms over a 4' × 4' Field Of View (FOV), while the Metal Oxide Semi-conductor (MOS) detectors  (Turner et al. 2001)  were set in Full Frame mode  (2. 6  s time resolution on a 15' radius FOV). The thin optical filter was used for the PN and the medium filter for the MOS cameras. We used the XMM-Newton Science Analysis Software (SAS) v13. 0. We performed a standard analysis of high particle background  (following De Luca et al. 2005). We crosschecked the results with the SAS tool bkgoptrate (also used for the 3XMM source catalog 2 ). This tool searches for the point at which the maximum signal-to-noise (S/N) ratio is achieved for the given background time series after the bins above a threshold are excluded.
Both analyses revealed no significant contamination from flares. We selected 0-4 pattern events for PN and 0-12 for the MOS detectors in the 0. 3-10 keV energy range, following  Marelli et al. (2013). Then, we excluded the 0. 3-0. 4 keV energy range for the PN owing to the presence of bright columns. Due to the high degree of absorption in our source, the number of expected counts in the 0. 3-0. 4 keV energy range is negligible (10 -12 counts s -1 for the best fit spectrum, obtained using the WebPimms HEASARC tool). For each spectrum we generated ad hoc response matrices and effective area files using the SAS tools rmfgen and arfgen. To fully characterize both the pulsar and its putative nebula, we also obtained a Chandra/ACIS-S  (Garmire et al. 2003)  exposure of the field. The observation was performed on 2013 July 22 and lasted 50.
4 ks. The telemetry mode was set to Very Faint, recommended in order to reduce background in extended sources. We used the Chandra Interactive Analysis of Observation (CIAO) software v4. 5. We also re-analyzed a public 25. 7ks Suzaku  (Mitsuda et al. 2007 ) observation performed on 2010 March 22. The HEAsoft package (v6. 15) was used to analyze Suzaku data, following the standard recommendations 3.
γ-ray analysis The Fermi-LAT dataset we used to extend the γ-ray ephemeris of J1813 spans five years, from 2008 August 4 to 2013 August 4. P7REP Source class events were selected with reconstructed energies from 0. 1 to 100 GeV and with arrival directions within 20 • of the source position. We excluded γ-rays collected when the LAT was not in nominal science operations mode, when the spacecraft rocking angle exceeded 52 • , or when the Sun was within 5 • of the pulsar position. Moreover, to reduce contamination by residual γ rays from the bright limb of the Earth, we excluded photons with measured zenith angles > 100 •. We performed a binned maximum likelihood analysis, following  Abdo et al. (2013). We used the Fermi Science tools v09r32p04, Instrument Response Functions P7REP SOURCE V15, the Galactic and isotropic models obtained by the LAT collaboration from the analysis of four years of data 4.
Following the prescriptions of  Abdo et al. (2013) , we obtained an acceptable fit (χ 2 red =1. 78, 40dof, null hypothesis probability, nhp=0. 002) using two gaussians to describe the first peak and one for the second. 6 o perform a >0. 1 GeV γ-ray phase-resolved spectral analysis on the 5-year dataset, we rebinned the light curve into 25 bins. For each phase bin, we re-ran the binned likelihood spectral analysis to search for variations in the spectral parameters as a function of the pulsar phase. We used the same region of the phase-averaged analysis but we fixed spectral parameters of all the other sources at the best fitted ones. We left free to vary all the spectral parameters of J1813, as well as the Galactic and isotropic spectral parameters. Anyway, we note that by freezing the Galactic and isotropic spectral parameters we obtain consistent results.
X-ray observations and analysis Figure  3  shows the 0. 3-10 keV XMM-Newton FOV. Source detection using maximum likelihood fitting was done simultaneously on each of the EPIC-PN, MOS1, and MOS2 with the SAS tool edetect chain. We also performed a source detection on the Chandra dataset by using the CIAO tool wavdetect. The best X-ray position of the pulsar is 18 h 13 m 23 s. 77, -12 • 45 59. 9 (0. 015 +0. 6 90% statistical plus systematic errors). We analyzed the pulsar radial brightness profiles in XMM-Newton and Chandra datasets and compared them with the theoretical PSFs. The PSF of the EPIC-PN camera onboard XMM-Newton is best described by an off-axis, energy-dependent King function  (Read 2004 ). The full width half maximum of the PSF for an on-axis source at 1. 5 keV is typically less than 12.
X-ray Timing Analysis To search for X-ray pulsations from J1813, we used the SAS tool barycen to barycenter the PN events using the precise Chandra pulsar position. In order to improve the sensitivity to pulsations, we decided to apply a photon weighting technique similar to the one used for Fermi-LAT, assigning to each photon a probability of coming from the pulsar, in order to help with background rejection and improve the sensitivity to pulsations. Kerr (2011)  notes that this technique is applicable to any photon-counting instrument in which sources are not perfectly separated from their background, e. g. , searches for X-ray pulsation in observations of a pulsar. While in the X-ray domain the positional errors are much smaller than in the γ-ray band, the problem of superposition of sources is more critical.
Indeed, the wide range of spectral shapes for different source classes in X-rays and the complexity of the background of X-ray telescopes (for XMM-Newton see e. g. Kunz&Snowden 2008) make such techniques as important as in the γray domain. To this end, we developed and used a Python tool to assign to each photon weights quantifying the probability that such an event comes from each of the sources within the region of interest. The tool requires: -the position, (best fitted) spectral model, flux and fitted PSF of each source; -the (best fitted) spectral model and flux of the background. The tool produces columns of weights that are added to the events file, replicating the Fermi tool gtsrcprob. Tests conducted on a sample of pulsars (e. g. the magnificent seven pulsars and Geminga,  Treves et al.
Such best fit H-values have been obtained by using not-randomized XMM-Newton events. In the Small Window mode of the EPIC-PN camera, arriving photons are read only during a cycle of 3. 9809 ms (=integration time), then the charges are transferred (transfer time=0. 068 ms) and read (readout time=1. 521 ms). The real arrival time of each photon is then stored as a multiple of the frame time (=integra-tion+transfer+readout time) of ∼5. 7 ms  (Kuster 1999). For standard analysis, a tool included in the SAS epproc usually randomizes the arrival time of each event within the 5. 7 ms windows. Here, we chose not to randomize the arrival times in order to achieve a better timing resolution for our fast rotating pulsar. The un-randomized event file basically consists of sets of photons with the same arrival times, at the middle of each 5.
7 ms window. By using this type of events, we avoid the error from the randomization process on the entire 5. 7 ms window (while the integration time is only 4 ms). For comparison, a randomized, unweighted test on J1813 with the best energy and spatial cuts gives an H-value of 8735. The resulting X-ray light curve shows two very sharp peaks, about 8 ms wide, with an off-pulse component detected with a 17σ significance. Here, we define as off-pulse the sum of phase bins for which the count rate can be fitted by a constant. All the bins that deviate more than 3σ from the fitted value are considered on-pulse. In such a way, we obtain two off-pulse intervals, between 0. 15-0. 4 and 0. 65-0. 9 in phase. The pulse profile is expected to be heavily affected by the PN camera frame time binning. Thus we developed a Python script to simulate the deformation of simple input light curves due to such PN (Small Window mode) readout cycles.
The hard X-ray band and Spectral Energy Distribution Searching at the position of J1813 in the hard X-ray band (∼100 keV), we found a hint of a detection with INTEGRAL IBIS/ISGRI  (Lebrun et al. 2003). We used the automated HEAVENS online tool 8 to create a counts map, sensitivity map and light curve of the source with all the public INTEGRAL observations. The possible steady source has a count rate of 0. 12±0. 02 counts s -1 in the 30-520 keV energy band, that corresponds to a flux of ∼ 5. 3 × 10 -11 erg cm -2 s -1. Although the significance of the detection is > 6σ, such a source comes from an automated script instead of from a dedicated analysis. We therefore conservatively decided to treat it as an upper limit. In order to find the spectral energy distribution (SED) points in the X-ray band we regrouped the XMM-Newton and Chandra spectra.
We plotted the X-ray unfolded spectrum with XSPEC by using the best fitted spectral model reported in Section 4. 1. To find the SED points in the γ-ray band, we divided our dataset in logarithmically uniform energy bins. Then, for each bin we re-ran the binned analysis reported in Section 3. We derived the 1σ confidence N -dimensional ellipsoids (where N is the number of free parameters in the models) from the covariance matrices obtained as an output of XSPEC and gtlike for the X-ray and γ-ray band, respectively. Then, we simulated 10 4 spectra for each band with parameters following the contours and reported these in Figure  8  (butterfly plot). The meaning of the butterfly can be understood as follows: any absorbed power-law model (for X-rays) or power-law with exponential cutoff (for γ-rays) that is drawn on the plot which is not fully contained in the envelope is outside the 1σ confidence region for such models, and hence is excluded by the data at the 1σ confidence level.