dataesr/scientific-paragraphs-categorization huggingface dataset:
For a given event, its GW p-value p GW is calculated by comparing the reconstructed ρ value to the background distribution of ρ in the same category as the event. Because the C1 and C2+C3 searches are statistically independent, we include a trial factor of 2 in our final significance. Overall, cWB identified 46 GW candidates during the T obs = 48. 6 days of coincident data from the LIGO Hanford and LIGO Livingston detectors, which is consistent with our background expectation. 23 of these candidates fell into the C1 category, while 23 were identified as C2+C3. To characterize the background distribution of the ranking statistic ρ for GW candidates, we carried out the same search over GW data after applying time shifts between the data from the two LIGO detectors, with time shifts much greater than travel time of GWs between the LIGO detectors (10 ms).
ANTARES The Antares neutrino telescope, located deep (2500 m) in the Mediterranean Sea, 40 km from Toulon, France, has been continuously operating since 2008. It is a 10 megaton-scale array of photosensors, detecting neutrinos with energies above O(100) GeV, with a duty cycle higher than 90%. The selection criteria for the Antares neutrino candidates were optimized based on the observed background rate and followed the same philosophy as the one used in the follow-up of GW170817  (Albert et al. 2017c ). The events were selected from the most recent offline-reconstructed dataset, that incorporated dedicated calibrations, in terms of positioning  (Adrián-Martínez et al. 2012) , timing  (Aguilar et al. 2011 ) and efficiency  (Aguilar et al. 2007). Only upgoing ν µ neutrino candidates, detected by their muon tracks, were considered in this analysis.
The Antares Collaboration acknowledge the financial support of the funding agencies:  Centre National de la Recherche Scientifique (CNRS) ,  Commissariat  à l'énergie atomique et aux énergies alternatives (CEA),  Commission Européenne (FEDER fund and Marie Curie Program) ,  Institut Universitaire de France (IUF) ,  IdEx program  and  UnivEarthS Labex program at Sorbonne Paris Cité  ( ANR-10-LABX-0023  and  ANR-11-IDEX-0005-02 ),  Labex OCEVU  ( ANR-11-LABX-0060 ) and the A* MIDEX  project ( ANR-11-IDEX-0001-02 ),  Région Île-de-France (DIM-ACAV) ,  Région Alsace  (contrat CPER),  Région Provence-Alpes-Côte d'Azur, Département du Var and Ville de La Seyne-sur-Mer, France ;  Bundesministerium für Bildung und Forschung (BMBF) ,  Germany ;  Istituto Nazionale di Fisica Nucleare (INFN), Italy ;  Nederlandse organisatie voor Wetenschappelijk Onderzoek (NWO) , the  Netherlands; Council of the President of the Russian Federation  for young scientists and leading scientific schools supporting grants,  Russia ;  National Authority for Scientific Research (ANCS) ,  Romania ;  Ministerio de Economía y Competitividad (MINECO) :  Plan Estatal de Investigación  (refs.
The present work reports on the charge and spin density modelling of YTiO 3 in its ferromagnetic state (T C = 27 K). Accurate polarized neutron diffraction and high-resolution X-ray diffraction (XRD) experiments were carried out on a single crystal at the ORPHE ´E reactor (LLB) and SPRING8 synchrotron source. The experimental data are modelled by the spin resolved pseudo-atomic multipolar model (Deutsch et al. , 2012). The refinement strategy is discussed and the result of this electron density modelling is compared with that from XRD measured at 100 K and with density functional theory calculations. The results show that the spin and charge densities around the Ti atom have lobes directed away from the O atoms, confirming the filling of the t 2g orbitals of the Ti atom. The d xy orbital is less populated than d xz and d yz , which is a sign of a partial lift of degeneracy of the t 2g orbitals.
, 2017). The present paper is devoted to the precise determination of the electronic state at low temperature which is absolutely necessary to understand the electronic properties of YTiO 3 as the Ti 3+ unpaired electron plays a crucial role in the control of its magnetic properties. The only attempt of charge density analysis on YTiO 3 has been made by Hester at 127 K  (Hester et al. , 1997)  using W K radiation ( = 0. 21069 A ˚) to reduce absorption and extinction effects. No multipolar analysis has been performed: only experimental deformation electron density maps revealed large charge depletions along the Ti-O bonds. In the present study, the electron density distributions of charge (r) and of spin s(r) have been determined using high-resolution XRD and PND data simultaneously. Combining these two techniques in the refinement of a unique model provides the spin resolved electron density using the spin-split extension of the Hansen-Coppens model  (Hansen & Coppens, 1978; Deutsch et al.
Experimental The X-ray diffraction experiment was carried out using the SPring-8 synchrotron radiation source (beamline BL02B2) on a single crystal (0. 02 Â 0. 10 Â 0. 11 mm). A short wavelength of 0. 3506 A ˚was used to reduce absorption and extinction effects. The data were collected at 20 K, which is 7 K below the ferromagnetic phase transition temperature (T C = 27 K). The diffractometer is equipped with a cylindrical image plate which considerably enhances the signal-to-noise ratio. Data collection consisted of four scans at positions = 0, 15, 30 and 45 using a rotation angle of 11 (1 overlap between images) and 13 min exposure time. Due to overflow, 16 images were remeasured with 3 min exposure time. The indexing, intensity integration and the absorption correction were carried out using the in-house programme RAPID AUTO  (Rigaku, 2009).
A total of 100 406 reflections were collected, out of which, 96 986 reflections were averaged with SORTAV (Blessing, 1987) leading to 4584 unique reflections with an average redundancy of 21 and an internal agreement R int = 3. 66% up to sin max / = 1. 67 A ˚À1. The agreement factor R int increases smoothly with increasing resolution (Table  S1  of the supporting information) to reach about 8% in the last shell (1. 4-1. 67 A ˚À1 ), attesting to the very good quality of the data. Such high-quality ultra-high resolution data allows a thorough modelization of the atomic displacement parameters (ADPs). Polarized neutron diffraction measurements were carried out at the thermal polarized neutron lifting counter diffractometer 6 T2 (LLB-ORPHE ´E, Saclay) at low temperature (5 K) using a 5 T external magnetic field to fully magnetize the sample.
The statistical agreement factors for all 4584 data significantly dropped from R(F) = 2. 48%, R w = 2. 58% and GooF = 2. 83 for the harmonic model to R(F) = 1. 22%, R w = 1. 39% and GooF = 1. 53. Significant parameters (30/86 > 3) are summarized in Table  S2. Anharmonicity in YTiO 3 has not been described; it was not observed at 100 K for which the resolution was lower sin max / = 1. 28 A ˚À1  (Voufack, 2018)  nor at 127 K  (Hester et al. , 1997) , but was observed in other perovskites when the experiment temperature is close to the transition temperature such as in PbTiO 3  (Kiat et al. , 2000) , KNiF 3  (Ivanov et al. , 1999) , KMnF 3  (Ivanov et al. , 2004)  and CsPbCl 3  (Hutton & Nelmes, 1981). Anharmonicity in SrTiO 3 has been controversial for some time. Jauch used high-resolution -ray diffraction to show that a harmonic model was good enough to fit their data  (Jauch & Reehuis, 2005).
Methodology The experimental spin resolved electron density distribution was modelled using the program MOLLYNX  (Deutsch et al. , 2012) , a modified version of the Hansen-Coppens formalism  (Hansen & Coppens, 1978; Deutsch et al. , 2014)  where the pseudo-atomic spin resolved electron density is expanded on real spherical harmonic functions (y lmAE ) for magnetic atoms. In this formalism the charge density is expressed as: ðrÞ ¼ " ðrÞ þ # ðrÞ ¼ core ðrÞ þ "3 P " val ð " rÞ þ #3 P # val val ð # rÞ þ X ' " 0 3 R l ð " 0 rÞ X ' m ¼ 0 P " lmAE y lmAE r r þ X ' # 0 3 R l ð # 0 rÞ X ' m ¼ 0 P # lmAE y lmAE r r ; ð1Þ and the spin density is expresssed by: sðrÞ ¼ " ðrÞ À # ðrÞ ¼ "3 P " val ð " rÞ À #3 P # val val ð # rÞ þ X ' " 0 3 R l ð " 0 rÞ X ' m ¼ 0 P " lmAE y lmAE r r À X ' # 0 3 R l ð # 0 rÞ X ' m ¼ 0 P # lmAE y lmAE r r : ð2Þ core and val are core and valence contributions to the charge density, respectively; P val and P lmAE are valence and multipolar parameters for electrons, respectively, with spin up (") and spin down (#).
Conclusions Low-temperature high-resolution X-ray diffraction has been carried out on YTiO 3 using the SPRING8 synchrotron radiation source. Despite the important absorption and extinction effects exhibited by the sample, a very accurate data set has been obtained. This has enabled realistic charge density modelling. At low temperature, Y and Ti atomic displacements are anharmonic. The joint refinement of X-ray and polarized neutron diffraction allowed a spin resolved experimental electron density determination. The obtained model shows that the titanium spin wavefunction can be approximated as a linear combination of d xz and d yz orbitals, which is in agreement with previous results  (Kibalin et al. , 2017). The integrated spin moments of different atomic basins seem to indicate that the magnetic pathway involves both O atoms, not just one of them  (Kibalin et al.
Error distributions of third-body parameters In this subsection we look at the distributions of 1σ errors for the parameters K and P, i. e. the third-body parameters which are interesting from an observational perspective. We report first the best and average error with which these parameters are recovered for detectable systems, i. e. for systems which already have relative errors on both K and P estimated to be below 30%. Again we focus on the optimistic, median, and pessimistic scenarios, as selected above. We only analyse data collected with a nominal four-year LISA mission. In the CBP optimistic (B1), median (C1), and pessimistic (A1) scenarios, we obtain an average relative error on K of the 14. 9%, 14. 9%, and 21. 0%, respectively. The best recovered K values are instead measured with relative errors of 0.
The LISA duty cycle and system identification Our study was based on the nominal LISA mission lifetime, i. e. four years of uninterrupted observations. However, during ∼ 30% of this time, LISA will not be acquiring scientific data because of expected maintenance operations (duty cycle). Nevertheless, even though the total effective observational period will be below four years, a periodic stop of scientific operation should not negatively impact the detection capability of LISA, at least for long-living GW sources if additional data analysis tools are employed  (Baghi et al. 2019). Our results should thus not be affected by the duty cycle of LISA, albeit we note that a future dedicated investigation is required to address this aspect fully. We expect DWDs to be very numerous in the Milky Way.
For example, high cadence (several observations per night) photometric surveys such as ZTF (Zwicky Transient Facility; Bellm 2014) can be used to search for variable sources with an orbital period provided by LISA. Surveys with longer cadence (one observation in a few days) such as PTF  (Palomar Transient Factory; Law et al. 2009)  or LSST, can also be used for finding DWD EM counterparts. However, in the latter case it will be important to account for the orbital period derivative (also provided by LISA if the system is chirping) caused by GW radiation; see example of retrieving J153932. 16+502738. 8 in PTF archival data in  Burdge et al. (2019). The work by  Korol et al. (2017)  in particular showed that at least 100 DWDs are expected to have GW counterparts. These predictions give us optimistic prospects for observing exoplanets and BDs around DWDs (but also other stellar compact object binaries), which would require monitoring DWDs for a few years.
Acknowledgements. We would like to thank  Pierre-Olivier Lagage ,  Vincent Van Eylen , and  Dimitri Veras , for useful discussions. C. D. acknowledges support from the  LabEx P2IO , the  French ANR  contract  05-BLAN-NT09-573739. V. K. and E. M. R. thank the  NWO WARP Program , grant  NWO 648. 003004APP-GW. V. K. acknowledges support from the  Netherlands Research Council NWO (Rubicon Science  grant  019. 183EN. 015 ). This work was supported by the  COST action   CA16104  " Gravitational waves, black holes and fundamental physics" (GWverse)  through a  Short Term Scientific Mission (STSM)  awarded to N. T. COST actions are supported by  COST (European Cooperation in Science and Technology). This work made use of the python package mw_plot (https://pypi. org/project/mw-plot/) and of the annotated image of the Milky Way by  NASA/JPL-Caltech/R.
The high-eccentricity, slow precession phase is supposedly the most dangerous one for the excitation of the cold population  (Batygin et al. 2011). Thus, if we will be able to obtain low-eccentricity particles during this phase it is likely that a cold population can be preserved throughout the whole evolution. We stress that selfgravity simulations are very slow and therefore it would not be possible to cover the whole time-range of Fig. 2. Thus, we need to select an interesting (and a priori the most defavorable) interval of time and restrict our numerical analysis on this interval. We adapted the integration package REBOUND  (Rein & Spiegel 2015)  to read the interpolated evolutions of the planets shown in Fig. 4  instead of solving for the planetary motion selfconsistently. The evolution of the particles is computed from the gravitational forces exerted by the planets from their interpolated positions.
ACKNOWLEDGMENTS R. R. S acknowledges support provided by grants # 2017/09919-8  and # 2015/15588-9 ,  São Paulo Research Foundation (FAPESP)  and the good hospitality received from  Observatoire de la Côte  d'Azur. R. R. S also thanks  Rafael Sfair  for turning possible our simulations on the cluster of computers that belongs to  São Paulo State University.
OBSERVATIONS, DATA REDUCTION AND DATA ANALYSIS NGC 1672 was observed as part of a large observing program with the MUSE spectrograph  (Bacon et al. 2010)  at the VLT (PHANGS 1  -MUSE survey; PI: Schinnerer). The inner spiral structure was mosaiced with eight pointings (Figure  1 ), each covering a 1 × 1 field of view with 0. 2 pixels and a typical spectral resolution of ∼2. 5 Å (FWHM) over the nominal wavelength range (4800-9300 Å). Each pointing was observed in four rotations, with two sky pointings, and a total on source integration time of 43 minutes. Typical seeing is 0. 8 (or 46 pc). Details on the data reduction and H II region catalog construction are contained in  Kreckel et al. (2019)  and briefly summarized here. Observations are reduced using pymusepipe, a pipeline built on esorex and the MUSE pipeline recipes  (Weilbacher et al.
The pyneb module version 1. 18 is adopted for extinction correc-tion and solving iteratively for electron temperature and density using multi-level atomic models  (Luridiana et al. 2012 ). The default atomic data are adopted. We assume an intrinsic Balmer decrement (Hα/Hβ) of 2. 85 and the CCM89 extinction curve  (Cardelli et al. 1989 , assume R V of 3. 1). The electron temperature derived from the [N II]λλ5755,6584 lines reflects the temperature of the low ionization zone of the nebula. In total, eighty H II regions with S/N of [N II]λ5755 greater than 3 are analyzed and presented below (out of 225 detections). A subset of 33 regions has S/N greater than 5.
INTRODUCTION The knowledge of the opacity and emissivity is very important when one deals with the radiative properties of ICF and astrophysical plasmas. The aim of this work is the calculation of the opacity and the comparison with experimental results. In a first calculation we compare the opacity of a pure silicon plasma to a recent experiment. In a second calculation, we study a mixture of carbon and silicon and investigate the role of the radiation field of the Hohhlram on the population kinetics. This means that processes like photoexcitation and photoionization are taken into account. We recently developed a Non Local Thermodynamic Equilibrium (NLTE) code which accounts for most collisional and radiative processes. The atomic database is obtained by the FAC code  [1]. It consists in a large set of level energies and spontaneous emission rates.
The cross-sections of the collisional and radiative processes are treated by modified semi-empirical formulas. For example, for the collisional excitation cross-section we started from the formula of Sampson and Zhang  [2, 3]. The Sampson and Zhang cross-section is multiplied by a function in order to retrieve accurate cross-sections given by the FAC code. The effect of the radiation field is modeled with a Planckian distribution, yielding rates whose effect on the population kinetics is investigated. Line broadening, line shift due to screening effects and Ionization Potential Depression (IPD) are also taken into account. In Sec. 2, we describe a collisional-radiative model. The NLTE code is used to calculate the opacity. The atomic database of carbon and silicon involving various ionic stages is provided by the FAC code.
In such a way, each configuration has its own set of wavefunctions. The latter are determined in a single-configuration approximation. One peculiarity of the code is that it does not rely on the "isolated atom" picture, but on a realistic atom-in-plasma modelling (equation of state). Relativistic effects are taken into account in the Pauli approximation. The DLA part of the spectrum is obtained using an adapted version of the RCG routine from Cowan's suite of atomic structure and spectra codes  [9]. The RCG source code was used for decades by spectroscopists, it has many available options and is well documented. The data required for the calculation of the detailed transition arrays (Slater, spin-orbit and dipolar integrals) are obtained from SCO, providing in this way a consistent description of the plasma screening effects on the wavefunctions.
CONCLUDING REMARKS We have calculated the opacity of a pure silicon plasma and compared our results to a recent experiment and to other calculations. We have also calculated the opacity of a mixture where the dopant is silicon. In the second study we have shown that the radiation field has a very small effect on the population kinetics. The calculations are performed by using a NLTE code developed at Laboratoire Aimé Cotton. The cross-sections of the various processes are fitted with empirical formula that involve new Gaunt factors. In a future work we will extend the atomic database of the dopant. To maintain the amount of calculation at a reasonable level, it would be necessary to treat statistically some intervals in the bb regions of the dopant.
ACKNOWLEDGMENTS We are grateful to three anonymous reviewers for their detailed and constructive comments on the manuscript, and to  Don Porcelli  for his editorial handling. F. M. acknowledges funding from the  European Research Council [ERC Starting  grant agreement 637503-Pristine] to as well as the financial support of the  UnivEarthS Labex program at Sorbonne Paris Cité  [ ANR-10-LABX-0023  and  ANR-11-IDEX-0005-02 ] and a chaire d'excellence  ANR-Idex Sorbonne Paris Cité. We are grateful to three anonymous reviewers for constructive comments on an earlier version of this manuscript. Parts of this work were supported by  IPGP  multidisciplinary program PARI, and by  Region île-de-France SESAME  Grant no. 12015908.
We show that modified GW propagation is a completely generic phenomenon in modified gravity. We then use a simple parametrization of the effect in terms of two parameters (Ξ 0 , n), that is shown to fit well the results from a large class of models, to study the prospects of observing modified GW propagation using supermassive black hole binaries as standard sirens with LISA. We construct mock source catalogs and perform detailed Markov Chain Monte Carlo studies of the likelihood obtained from LISA standard sirens alone, as well as by combining them with CMB, BAO and SNe data to reduce the degeneracies between cosmological parameters. We find that the combination of LISA with the other cosmological datasets allows one to measure the parameter Ξ 0 that characterizes modified GW propagation to the percent level accuracy, sufficient to test several modified gravity theories.
Our best fits are obtained through a nonlinear fit of the theoretical points with the parametrization curve(s) with the least squares method. Although differences in parametrizations are not especially relevant for LISA standard sirens at high redshifts (e. g. , MBH mergers) due to the large error bars, the issue of model reconstruction and the use of Information Criteria may be useful when considering low-z standard sirens (for instance, stellar-mass black holes), or if one uses parametrizations with a different number of free parameters. Ξ(z) = e -(1-Ξ 0 )[1-(1+z) n ] (1+z) 2n Ξ 0 + (1 -Ξ 0 )(1 + z) -n , (3. 23) Ξ(z) = Ξ 0 + (1 -Ξ 0 ) e -z n , (3. 24) δ(z) = n(1 -Ξ 0 )(1 + z) z n-1 1 + Ξ 0 (e z n -1). ( 3 The parametrization with smaller BIC or AIC is to be preferred. In the present case, the difference ∆ := |(IC model 1) -(IC model 2)| is the same for the BIC and the AIC, since the number of data points and the number of free parameters are exactly the same for all parametrizations.
They will also provide useful data to test modified theories of gravity through a modified cosmological propagation of GWs. In this section we outline our strategy to build simulated catalogs of LISA MBHBs with EM counterparts, while in section 5 we will use these catalogs to constrain modified gravity theories. To produce catalogs of MBHB standard sirens with EM counterpart, we employ a similar approach to the one adopted in  [35]. In what follows, we summarize the procedure to construct such catalogs, highlighting the differences with respect to the analysis of  [35]. d d gw L (z) d em L (z) 1 + (Ξ 0 -1)z n , ( 3 To describe the cosmological evolution of massive black holes, and specifically MBHBs, we use the semi-analytic galaxy formation model of  [170]  (with later incremental improvements described in  [171, 172] ).
The semi-analytical simulations of MBHB catalogs described above contain all the necessary data (mass in stars, nuclear gas, etc. ) needed to compute the magnitude of the EM emission of each MBHB merger in both the optical and radio bands. Following  [35]  we can thus determine the number of counterparts detected by future EM facilities, specifically  LSST [199] , SKA  [200]  and ELT  [201]. Note however that over the sky location region of the source there might appear several EM transients that could likely be identified with the EM counterpart of the MBHB merger. As in  [35]  we will however assume that the true EM counterpart can be efficiently identified (e. g. through timing, EM spectrum characterization and evolution, or information on the host galaxy), and leave a more thorough investigation of this issue to future analyses.
For each catalog we then perform a quick Fisher matrix cosmological analysis assuming ΛCDM. We ranked the 22 catalogs of each MBHB astrophysical model according to the area of the 1σ contour ellipses in the (Ω m , H 0 ) parameter space of ΛCDM. This quantity provides us with a rough measure of the cosmological constraining power of each catalog. Finally we select the median catalog among all ranked 22 catalogs as the representative catalog for each MBHB astrophysical model, similarly to the recipe employed in  [205]. We perform this procedure for Scenario 1 and then use the same selected catalogs for Scenario 2, but using different assumptions for the redshift errors as explained above. This allows us to directly compare results between the two different scenarios. The final product are thus six catalogs (corresponding to the three different MBHB astrophysical models, each one combined with the two scenarios for the redshift measurement accuracy) to use as mock data for the MCMC analysis presented in the following section.