dataesr/scientific-paragraphs-categorization huggingface dataset:
Acknowledgments The authors acknowledge the NASA, the CNES, their partner agencies and Institutions (UKSA, SSO, DLR, JPL, IPGP-CNRS, ETHZ, IC, and MPS-MPG) and the flight operations team at JPL, SISMOC, MSDS, IRIS-DMC, and PDS for providing the SEED SEIS data. Z. X. thanks Mark Wieczorek for fruitful discussion. The authors thank Caroline Beghein for providing their surfacewave group-velocity measurements. The authors also thank Yann Capdeville for sharing the homogenization package. The authors thank editor Andrew Dombard and one anonymous reviewer for their constructive feedback that helped improve this manuscript. This research is supported by CNES, ANR MAGIS (ANR-19-CE31-0008-08), and the Initiative d'Excellence (IdEx) Université Paris Cité (ANR-18-IDEX-0001). This study is InSight contribution number 276.
Search for doubly charged Higgs boson production in multi-lepton final states using 139 fb -1 of proton-proton collisions at √ 𝒔 = 13 TeV with the ATLAS detector The ATLAS Collaboration A search for pair production of doubly charged Higgs bosons ( ±± ), each decaying into a pair of prompt, isolated, and highly energetic leptons with the same electric charge, is presented. The search uses a proton-proton collision data sample at a centre-of-mass energy of 13 TeV corresponding to an integrated luminosity of 139 fb -1 recorded by the ATLAS detector during Run 2 of the Large Hadron Collider (LHC). This analysis focuses on same-charge leptonic decays,  ±± → ℓ ± ℓ ± where ℓ, ℓ = , , , in two-, three-, and four-lepton channels, but only considers final states which include electrons or muons. No evidence of a signal is observed.
The CMS Collaboration performed a similar search using √  = 7 TeV   collisions collected during Run 1  [22] , establishing lower bounds on the  ±± mass between 204 GeV and 459 GeV in the 100% branching fraction scenarios, depending on the flavour content of the two-lepton final states. A complementary analysis from the ATLAS Collaboration searched for doubly charged Higgs bosons in the  ±± →  ±  ± decay channel using the whole 139 fb -1 dataset from Run 2 of the LHC and excluded  ±± masses up to 350 GeV  [23]. The doubly charged Higgs boson can decay to  or ℓℓ (ℓ, ℓ = , , ), depending on the vacuum expectation value of the Δ  Higgs triplet,  Δ  [5]. In this paper, it is assumed that  Δ is smaller than 10 -8 GeV. Therefore, only leptonic decays of doubly charged Higgs bosons,  ±± → ℓ ± ℓ ± , are relevant.
It is worth stressing that lepton-flavour-violating decays such as  ±± →  ±  ± ,  ±± →  ±  ± or  ±± →  ±  ± are also allowed by the model. This fact connects high-energy searches at LHC with low-energy neutrinoless double beta decay searches  [26]. The analysis presented in this paper searches for leptonic decays  ±± → ℓ ± ℓ ± of doubly charged Higgs boson pairs, resulting in same-charge lepton pairs in final states with two, three or four leptons. Since these events are produced very rarely in proton-proton ( ) collisions by SM processes, same-charge lepton pairs represent a striking signature for BSM physics. The analysis only considers light leptons ( and ) in the two-, three-and four-lepton final states, thereby including leptonic  decays, using the whole 139 fb -1 dataset from Run 2 of the LHC.
Dataset and simulated event samples This analysis uses data from   collisions occurring every 25 ns at √  = 13 TeV, collected during Run 2 of the LHC from 2015 to 2018. Events selected for analysis are required to pass standard data-quality requirements  [32]  and they amount to a total integrated luminosity of 139 fb -1. The uncertainty in the combined 2015-2018 integrated luminosity is 1. 7%  [33] , obtained using the LUCID-2 detector  [34]  for the primary luminosity measurements. Events were collected using two-lepton triggers that select pairs of electrons  [35]  or muons  [36]  or electron-muon combinations  [35]. The transverse momentum ( T ) thresholds of the unprescaled two-lepton triggers were raised during Run 2 because of the increasing luminosity of the colliding beams but were never higher than 24 GeV (24 GeV) for the (sub-)leading electron or 22 GeV (14 GeV) for the (sub-)leading muon.
Monte Carlo (MC) methods were used to model signal and background events. The G 4 toolkit  [37]  was used to simulate the response of the ATLAS detector  [38]. Simulated events were reconstructed with the same algorithms as those applied to data  [31]  and were corrected with calibration factors to better match the performance measured in data. The various tools and set-ups used to simulate the different processes are summarised in Table  1. To minimise the impact of the theoretical uncertainties on the final result, the normalisation of the MC samples that model the dominant backgrounds is considered a free parameter in the final likelihood fit, described in Section 7. Signal events were generated at leading order (LO) with the LRSM package in P 8. 212  [39] , which implements the  ±± scenario described in Ref.
Conclusion The ATLAS detector at the Large Hadron Collider was used to search for doubly charged Higgs bosons in the same-charge two-lepton invariant mass spectrum, using  ±  ± ,  ±  ± and  ±  ± final states as well as final states with three or four leptons (electrons and/or muons). The search was performed with 139 fb -1 of data from proton-proton collisions at √  = 13 TeV, recorded during the Run 2 data-taking period lasting from 2015 to 2018. No significant excess above the Standard Model prediction was found. Lower limits are set on the mass of doubly charged Higgs bosons in the context of the left-right symmetric type-II seesaw and Zee-Babu models. These vary between 520 GeV and 1050 GeV for LRSMs and between 410 GeV and 880 GeV for the Zee-Babu model, depending on the lepton multiplicity channel, assuming that ℓℓ B ( ±± → ℓ ± ℓ ± ) = 100% and that decays to each of the , , , , ,  final states are equally probable.
Conclusion Following their derivation done decades ago, we have extended the modelling of the atomic exchange effect from  Pyper and Harston (1988) , originally established only for the allowed transitions, to the forbidden unique decays. Assuming the same hypotheses, their formulation can be deduced from our modelling, which is fully consistent with the formalism of beta decays from  Behrens and Bühring (1982). Demonstration has been done that the allowed exchange correction applied to the Fermi function is a good approximation for the forbidden unique transitions. With a willing of dissemination, we have included these results in the BetaShape code thanks to an extensive tabulation of the correction factors. In order to ensure accurate predictions at very low energy, we also revised the screening effect in the BetaShape modelling, tabulating the correction factors on the Fermi function and the λ k parameters.
Barker (1979)  explored a magnetic model for the peculiar V/R-active episode in the 1970s. However, while about 15±3% of all non-Be and nonsupergiant B stars have large-scale magnetic fields  (Wade et al. 2021) , that fraction is zero among classical Be stars  (Wade et al. 2016). For γ Cas,  Baldwin (1940)  considered a rotational-pulsational model (see also  McLaughlin 1961) , which is now an obsolete predecessor of the m = 1 density-wave model discussed below (Sect. 3. 2). From the published rich optical observational database, there are no indications of major differences between the central stars of γ Cas and 59 Cyg and those of other early-type Be systems. That is, the apparent peculiarities of γ Cas and 59 Cyg most probably lie in the disk dynamics and associated geometry. Similar to many other Be stars, γ Cas and 59 Cyg are binaries with a low-mass companion that may have a significant impact on the disk.
(2001)  appears consistent with near-critical rotation but cannot be reconciled with a disk inclination angle of 43±3 • (see next paragraph) unless disk and stellar equator are strongly misaligned. This conflict nearly vanishes if the v sin i of Chauville  et al. (2001, 432±11 km s -1 ) is combined with v crit = 577 km s -1 from  Frémat et al. (2005) , who corrected the observations for gravity darkening but also derived an inclination angle of 76. 4 •. Analyzing near-infrared long-baseline interferometry data, Paper II determined the disk inclination angle at times with little or no V/R activity to be 43±3 •. The time baseline of broad-band polarimetry is even longer, and, from the combination of the two datasets, Paper II concludes that the orientation in space of the disk of γ Cas was invariant for decades.
(Persistent shell stars may temporarily lose their narrow shell absorptions, but, then, the emission lines disappear as well. ) The Gaia DR2 parallax of 59 Cyg, namely 2. 51 ± 0. 32 mas (Gaia Collaboration 2018), is well consistent with the HIPPARCOS measurement of 2. 30 ± 0. 42 mas (van Leeuwen 2007). However, the Gaia EDR3 value of 1. 47 ± 0. 37 mas (Gaia Collaboration 2020) differs quite strongly from both. Over the past decades, Hα profiles in the BeSS database 1  (Neiner et al. 2011)  have not exceeded a peak-to-continuum (E/C) ratio of ∼2. 2, in agreement with the long-term record traced by  Harmanec et al. (2002). The much lower emission level than in γ Cas may be due to the large difference in separation of the component stars, which in 59 Cyg is 73. 3 R ⊙  (Peters et al. 2013)  but in γ Cas amounts to about 350 R ⊙ (Sect.
Broad end-to-end overviews of this stage in the history of γ Cas were given by  Baldwin (1939b) ,  Edwards (1956), and Pottasch (1959). To complement these mostly chronological, loglike accounts, the following subsubsections describe the episode by observables. In addition to these reviews, there are several dozen original observational publications for almost all of which the SAO/NASA Astrophysics Data System (ADS 4  ) hardly lists a handful of citations. Regrettably, not even scans are available for the publications in Russian. Scans of some other papers are lacking the last page(s). The SIMBAD bibliography  (Wenger et al. 2000)  is extremely incomplete for the time interval in question because SIMBAD's focus is on publications that appeared after the foundation of the Centre de données astronomiques de Strasbourg in 1972.
g. , in Underhill et al. 1982). In γ Cas, there would have been two such cycles in the observational database. The first one started before the discovery of emission lines in 1866 and ended in the 1940s when the second one started, which is still on-going. The dynamic and structural relevance of these six differences for the disk between 1932 and 1942 can only be deduced from the series of spectra which appear to trace two main activity cycles. However, on the one hand, it seems hardly possible to extract a comprehensive and comprehensible picture from verbal descriptions of the complex variability of the various spectroscopic parameters. On the other hand, the temporal sampling of some parameters is too low for a meaningful X/Y-diagram-like representation. Therefore, Table  1  and Fig. 1  attempt a hybrid, semi-graphical approach with a bin size of 2 months.
85 mag to 1. 65 mag. Later,  Cherrington (1937)  mentioned prediscovery plates from 20 June 1936 in which Nassau measured magnitudes of 1. 24 and 1. 35 mag, respectively. Visual light curves (covering different time intervals) are available from  Cherrington (1938) ,  Huffer (1939, photoelectric measurements) ,  Ashbrook (1940) ,  Baldwin & Torp-Smith (1941) , the AAVSO database 9  , and the compilations by  Pottasch (1959) ,  Howarth (1979), and Harmanec (2002). After a steep drop between 1937 May and December by more than 0. 5 mag, photoelectric photometry found a very broad, much shallower maximum around ∼1. 6 mag in 1938 August  (Huffer 1939). Thereafter, the decline continued at a roughly constant lower rate, and in 1940 attained a minimum brightness of ≳2. 8 mag about which value it kept hovering through the late 1940s (with a shallow maximum in 1941/1942).
02 nm) from the beginning of the first shell event (1972 October) and the late stage of the second one (1975 November), respectively. It should be noted that these data are of much higher technical quality than the groundbased photographic spectra. The flux level of the first Copernicus observation was lower everywhere, by more than 10% in some regions. Since from 1972 June to 1973 June (when the shell was discovered in an optical spectrum) there had been a drop by more than a magnitude in UV flux  (Beeckmans 1976 ), the variability seems to be part of the shell event. In agreement with this, Hubert-Delplace & Hubert (1981) cite a private communication from Gilra that in 1974 December (during the second shell phase) the UV flux measured with the Astronomical Netherlands Satellite was about 1 mag lower than in 1975 November and December (when there was no shell).
Interferometry  (Quirrenbach et al. 1997 ) has proven this (quasi)spherical notion wrong. But there is concern that this fierce controversy has prevented the proper exploitation of the substantial archive of observations with IUE of Be stars at large. Nevertheless, this database established that, on average, winds from Be stars are stronger than from main-sequence non-Be stars, and the UV observations of 59 Cyg constitute one of the strongest empirical arguments in support of radiative ablation of the disk as a contributor to winds from Be stars (see Sect. 7. 1). The results of coordinated monitoring of UV wind lines and the Hα emission in 59 Cyg some years after the shell phase  (Doazan et al. 1980 (Doazan et al. , 1985 (Doazan et al. , 1989 ) are an important pillar on which this conclusion is based (see Sects.
A first search for such events has been undertaken in the literature and databases  (Baade et al. , in prep. ). The cases found are not statistically representative but suggest that major disk tilting events (i) are rare, (ii) are not generally linked to V/R activity, (iii) can have accelerations that are as fast and timescales that are as short as those observed in γ Cas and 59 Cyg, and (iv) can lead to both shell and single-line stages in one and the same star. Warping disks have also been identified. As have been cases, in which 3D effects of one-armed disk oscillations probably dominate. The results may provide a first glimpse of whether tilting Be disks are merely interesting or convey information about physical processes that are worth learning more about. Hardly any of the early ideas to elucidate the nature of the extreme variations of γ Cas and 59 Cyg have survived.
Acknowledgements. We warmly thank  Professor Douglas Gies , whose referee report enabled us to clarify and correct various aspects of the paper. We especially acknowledge the motivation he provided for the discussion in Sect. 7. 4. D. B. sincerely thanks  Mrs. Sarah Burbidge  for providing him with a copy of her mother's PhD thesis; we appreciate her generous permission to reproduce Appendix A from that thesis. D. B. is grateful to  Prof. Ian Howarth  for having established the contact with  Mrs. Burbidge. We acknowledge with gratitude the permission by the editors of the Journal of the  Royal Astronomical of Canada  to reproduce the figure in Heard (1938) as our Fig. 4. This work A47, page 26 of 29 Baade, D. , et al. : A&A, 678, A47 (2023) has made use of  NASA 's Astrophysics Data System (ADS) bibliographic services, the SIMBAD database, operated at  CDS, Strasbourg, France , and the Be Star  Spectra (BeSS)  database, operated at  LESIA ,  Observatoire de Meudon, France  (http://basebe.
obspm. fr). The authors warmly thank the BeSS observers, most notably  Eric Bruyssinck ,  Christian Buil ,  Bertrand de Batz ,  Joan Guarra Fló ,  Keith Graham ,  Benjamin Mauclaire ,  Coralie Neiner , and  Carl Sawicki , for obtaining and publicly sharing their spectra, and they acknowledge with thanks the variable star observations from the AAVSO International Database contributed by observers worldwide and used in this research. This work makes use of observations from the  Las Cumbres Observatory global  telescope network with the  NRES  instruments at the  Cerro Tololo Interamerican Observatory, McDonald Observatory , and  Wise Observatory. This paper includes data collected by the TESS mission, which are publicly available from the  Mikulski Archive for Space Telescopes (MAST). Funding for the TESS mission is provided by  NASA's Science Mission directorate.
Acknowledgments We thank  Sudarshan Ananth ,  Glenn Barnich  and  Marc Geiller  for many fruitful discussions. We thank  François Delduc  for useful comments on the manuscript. The author is grateful to the  LABEX Lyon Institute of Origins  ( ANR-10-LABX-0066 ) Lyon for its financial support within the  Plan France 2030  of the French government operated by the  National Research Agency (ANR).
This approach is complementary to the study of the correlation between the CIB and the lensing convergence of the CMB (Planck Collaboration XVIII 2014b ;  Maniyar et al. 2018 ; Cao et al. 2020 ; Darwish et al. 2021b ; McCarthy & Madhavacheril 2021 )  with two advantages. Firstly, cosmic shear data provide a handle on the redshift dependence of the signal via tomography. Secondly , while the CIB is a known contaminant for CMB lensing reconstruction, no such contamination exists for cosmic shear. This paper is structured as follows. Section 2 presents the theoretical background and the methods used in the analysis. The data sets used are described in Section 3. The measured cross-correlations are presented and analysed in Section 4 , where we also present the associate constraints on star formation models.
Likelihood We will make use of a Gaussian likelihood, -2 log p( d | ) = ( d -m ( )) T C -1 d ( d -m ( )) + K, ( 27 ) to constrain the free parameters of the star-formation model. In this expression d is the data vector, containing all cross-correlations between tomographic cosmic shear bins and CIB maps, C d is the covariance of d , m is the theoretical model for d , and denotes the free parameters of the model. The posterior distribution is then given by the product of this likelihood and the parameter priors. Our fiducial model contains 4 parameters describing the halo model for the star formation history, described in Section 2. 1. 3 : { m 0 , m z , η 0 , η z }. We also marginalize o v er two intrinsic alignment parameters A DES / KiDS 0 , describing the amplitude of IAs in the DES and KiDS samples.
Power spectra, validation, and goodness of fit The data vector that will form the basis of our fiducial analysis is the set of nine cross-correlations between the coadded CIB map described in Section 3. 2. 2 and the cosmic shear E -mode in the four DES and five KiDS tomographic redshift bins. These measurements and their statistical uncertainties are shown in Fig. 4. We obtain clear detections of the cross-correlation especially at the higher redshifts, where the amplitude of both the cosmic shear and CIB signals grows. As a first model-independent estimate of the total signal-to-noise ratio ( S / N ) of this cross-correlation, we find S/N = χ 2 0 -N d = 20. 3 , ( 33 ) where χ 2 0 is the χ 2 statistic for a null hypothesis (i. e. χ 2 0 ≡ d T C -1 d d in the notation of Section 2. 3 ), and N d = 180 is the size of the data vector.
6  , with qualitati vely equi v alent results found for KiDS. As before, the solid orange lines show the best-fit model found using all the crosscorrelations with the coadded CIB map, and the dotted blue line shows the best-fits using only cross-correlations with DES. In turn, the red dashed lines show the best-fit prediction using only the crosscorrelations with one of the three frequency maps. The fiducial bestfit model is largely consistent with the predictions from the 545 and 857 GHz channels. It, ho we ver, consistently under-predicts the 353 GHz power spectra in both DES and KiDS. A similar trend, where the amplitude of the CIB signal is somewhat consistently higher in the 353 GHz channel was also found in cross-correlation with galaxies by J22. This could be due to both systematics in the data (e.
g. contamination from CIB or other extragalactic foregrounds), or a mis-modeling of the CIB spectrum in this channel. Nevertheless, as we will see in Section 4. 3 , the 353 GHz data lead to constraints on the model parameters that are largely compatible with those of the other two frequencies, and with our fiducial constraints. Thus, and since the coadded CIB map is dominated by the 857 and 545 GHz channels, MNRAS 520, 583-598 (2023) Figure  4. panels: cross-power spectra between the coadded CIB map and the four DES tomographic samples. Bottom panels: as abo v e for the five KiDS tomographic bins. The orange solid lines show the best-fit model found by fitting all power spectra simultaneously, while blue dotted lines show the best-fit model for each surv e y (DES or KiDS) independently. We find consistent results between both surv e ys.
we have kept the 353 GHz data in our fiducial analysis. Furthermore, we find that the best-fit model from the coadded CIB map is a good fit to the full multifrequency data vector, with a χ 2 = 547. 6 for 536 degrees of freedom ( p = 0. 35). Calculating the significance of the detection for the multifrequency data, as described above in the case of the coadded power spectra, yields S/N = √ 951. 3 -547. 6 = 20. 1. ( 35 ) This is in striking agreement with the detection significance using only the coadded CIB map, which demonstrates that virtually no information is lost by coadding the thee CIB maps, due to the tight correlation between them. This has the advantage of simplifying the analysis significantly, since each likelihood e v aluation is three times faster and, more importantly, we are not sensitive to the impact on the final parameter constraints of a potential mis-modelling of the cross-frequenc y co variance matrix.
Constraints on star formation models Combining the nine cross-power spectra with the coadded CIB map, we are able to place constraints on the four free parameters of the halo-based SFR model of Section 2. 1. 3 , { m 0 , m z , η 0 , η z }. The resulting 1 and 2-σ contours are shown in red in the left panel of Fig. 7. The data are able to constrain both the current value of the peak mass, m 0 , as well as its evolution with redshift m z. In turn, the two parameters describing the redshift evolution of the peak efficiency η * , { η 0 , η z } , are significantly degenerate and, whereas we are able to constrain η 0 , η z is completely unconstrained. In particular the data are most sensitive to a linear combination of both parameters that is approximately equal to the value of η * ( z) at the peak of the lensing kernel z = 0.
Furthermore, the uncertainties in the power spectra measured here receive a significant contribution from shape noise in the KiDS sample, which is uncorrelated with the DELS data. Thus, the actual correlation between the b ρ SFR measurements and the cross-correlation data used here is minimal. We estimate that the correlation between the CIB-shear power spectra used here, and the DELS ×CIB cross-correlations used in Jego et al. (  2022 ) is below 10 per cent for all scales used here. We therefore neglect this correlation in our analysis. The grey contours in the left panel of Fig. 7  show the constraints on the SFR parameters obtained solely from the b ρ SFR measurements (which coincide with the results published by J22). The blue contours, in turn, show the constraints obtained from the combination of the shear-CIB C s and the b ρ SFR measurements.