dataesr/scientific-paragraphs-categorization huggingface dataset:
2MASS We cross-correlate DR14Q with the All-Sky Data Release Point Source catalog  (Skrutskie et al. 2006 ) using a matching radius of 2. We report the Vega-based magnitudes in the J, H and Kbands and their error together with the signal-to-noise ratio of the detections. We also provide the value of the 2MASS flag rd_flg  [1] , which defines the peculiar values of the magnitude and its error for each band 3. There are 16 427 matches in the catalog. This number is quite small compared with the number of DR14Q quasars because the sensitivity of 2MASS is much less than that of SDSS. Applying the same method as described in Section 7. 1, we estimate that 0. 8% of the matches are false positives.
XMM-Newton DR14Q was cross-correlated with the seventh data release of the Third XMM-Newton Serendipitous Source Catalog  (Rosen et al. 2016)  7 (3XMM-DR7) using a standard 5. 0 matching radius. For each of the 14 736 DR14Q quasars with XMM-Newton counterparts, we report the soft (0. 2-2 keV), hard (4. 5-12 keV) and total (0. 2-12 keV) fluxes, and associated errors, that were computed as the weighted average of all the detections in the three XMM-Newton cameras (MOS1, MOS2, PN). Corresponding observed X-ray luminosities are computed in each band and are not absorption corrected. All fluxes and errors are expressed in erg cm -2 s -1 and luminosities are computed using the redshift value Z from the present catalog.
2017). 4. The 64-bit integer that uniquely describes the objects that are listed in the SDSS (photometric and spectroscopic) catalogs (THING_ID). 5-7. Information about the spectroscopic observation (Spectroscopic plate number, Modified Julian Date, and spectroscopic fiber number) used to determine the characteristics of the spectrum. These three numbers are unique for each spectrum, and can be used to retrieve the digital spectra from the public SDSS database. When an object has been observed more than once, we selected the best quality spectrum as defined by the SDSS pipeline (   (Oke & Gunn 1983 ) and errors (not corrected for Galactic extinction) in the five SDSS filters. These magnitudes are Asinh magnitudes as defined in  Lupton et al. (1999). 43. The absolute magnitude in the i band at z = 2 calculated using a power-law (frequency) continuum index of -0.
Conclusion We have presented the quasar catalog of the SDSS-IV/eBOSS survey corresponding to Data Release 14 of SDSS and resulting from the first two years of SDSS-IV observations. The catalog, DR14Q, contains 526 356 quasars, 144 046 of which are Isabelle  Pâris et al. :  The Sloan Digital Sky Survey Quasar Catalog: Fourteenth Data Release new discoveries. We provide robust identification from the application of an automated procedure and partial visual inspection of about 10% of the sample (likely ill-identified targets by the automated procedure). Refined redshift measurements based on the result of a principal component analysis of the spectra are also given. The present catalog contains about 80% more quasars at z < 2 than our previous release  (Pâris et al. 2017). As part of DR14Q, we also provide a catalog of 21 877 BAL quasars and their properties.
Acknowledgements. IP acknowledges the support of the  OCEVU Labex  ( ANR-11-LABX-0060 ) and the A* MIDEX  project ( ANR-11-IDEX-0001-02 ) funded by the " Investissements d'Avenir" French government program  managed by the  ANR. The French Participation Group to SDSS-IV was supported by the  Agence Nationale de la Recherche  under contracts  ANR-16-CE31-0021. AW acknowledges support from a  Leverhulme Trust Early Career Fellowship. ADM and BWL acknowledge support from  National Science Foundation  grants  1515404  and  1616168. IP thanks warmly the Great and Extremely COol team, especially  Samuel Boissier ,  Jean-Claude Bouret ,  Sylvain de la Torre ,  Audrey Delsanti ,  Olivier Groussin ,  Olivier Perfect Ilbert ,  Éric Jullo ,  Vincent Le Brun , and  Sébastien Vives , for encouraging creativity and for dealing with its unexpected consequences.
A special attention should be particularly paid to low-bandgap materials (Ge and most of III-V materials), envisaged as channel replacement for MOSFETs and steep switching tunnel FETs for low voltage application  [2] , due to their low ionization energy susceptible to amplify charge generation from sea-level neutron radiation. Following a methodology previously developed for the study of neutron-silicon interactions  [3] , the present work precisely examines nuclear events resulting from the interaction of atmospheric neutrons at the terrestrial level with a target layer composed of Si, Ge, SiC, C (diamond), GaAs, and GaN materials and representative of the whole sensitive volume of a typical integrated circuit. To perform this task, we constructed using the Geant4 toolkit  [4, 5]  a specific source of atmospheric neutrons and compiled large databases of neutron-semiconductor interaction events corresponding to tens of thousands of nuclear reactions.
Geant4 options, models, and simulation runs The neutron interaction databases for the different semiconductor materials listed in Table  1  have been computed in this work using Geant4 version 4. 9. 4 patch 01. The list of physical processes employed in simulation is based on the standard package of physics lists QGSP_ BIC_HP  [10]. Concerning the hadronic interactions, in QGSP group of physics lists, the quark gluon string model is applied for high-energy (above ~12 GeV) interactions of protons, neutrons, pions, kaons, and nuclei. The high-energy interaction creates an excited nucleus, which is passed to the precompound model describing the nuclear de-excitation. Nuclear capture of negative particles is simulated within the chiral invariant phase space (CHIPS) model. QGSP_BIC_HP list includes binary cascade for primary protons and neutrons with energies below ~10 GeV and also uses binary light ion cascade for inelastic interaction of ions up to few GeV/nucleons with matter.
The complete list of the Geant4 classes that we considered for our neutron simulations is summarized in Table  2. For each semiconductor target, a simulation run consists in the generation of 100 millions (10 8 ) of primary incident neutrons on a 20-μm-thick material layer perpendicular to its surface (1 cm 2 ). All particles characterized by tiny (i. e. , insignificant) ionizing properties and thus negligible impact on electronics in terms of electron-pair generation and single events have been excluded from the simulation. Consequently, the computed databases exclude electrons, positrons, gamma photons, pions, and mesons and only contain protons, alpha particles, and ionizing products with Z > 2. The target dimensions have been chosen to match the typical dimensions of the sensitive volume of an integrated circuit.
Main characteristics of the databases An example of the computed databases is given in Table  3  for a target composed of GaAs material and subjected to atmospheric neutron irradiation. As illustrated in this sample composed of nine events, each neutron-interaction event is described in two or several successive lines: the first line gives the event number, the energy of the incident neutron at the origin of the event, the Cartesian coordinates of the reaction vertex, and the number of secondary products generated; the following lines give for each secondary product the nature of this product, its mass and atomic numbers, its initial energy just after emission/production, and the Cartesian coordinates of its momentum. In the first line of the database sample shown in Table  3 , the event #11369 corresponds to a neutron elastic interaction with an As nucleus of the semiconductor lattice, giving a recoil As with an energy of 58 keV.
Also shown in Figure  5 , beryllium (Z = 4) is the less produced product for silicon target, lithium (Z = 3) for diamond, and fluor (Z = 9) for SiC. Finally, note that in Figure  6 , an axis-break has been introduced because no secondary product is created between Z = 3 and 19 for Ge, between Z = 4 and 22 (except Z = 16 and 19) for GaAs, and between Z = 7 and 21 for GaN. For these large Z elements (31 for Ga, 32 for Ge, and 33 for As), the absence of fragments in these ranges of Z comes from the limited number of high-energy incident neutrons, due to the 1/E nature of the spectrum of Figure  1  and to the finite value of the high-energy limit (10 5 MeV) considered for simulation; certain reaction channels being not present in the computed databases.
Consequences in terms of electron-hole pair generation and single events This last paragraph examines the consequences of neutron interactions in the different targets in terms of electron-hole pair generation and fundamental mechanism at the origin of single events in electronics. From the computed databases, we calculated in Figure  11  the total energy deposited by all the secondary products in the different target materials. Although it is a purely theoretical value, this total amount of deposited energy by ionization process is in the range of 10 11 eV for 100 million incident neutrons, which gives an average value in the range of keV per incident neutron, more precisely 1. 7 keV for Si, 2. 85 keV for Ge, 3. 07 keV for C, 2. 33 keV for SiC, 2. 6 keV for GaAs, and 3. 74 keV for GaN. This quantity is found to be minimum for the silicon target and maximum for GaN (Figure  11 ).
We report spatially-resolved [C II]λ158 µm observations of HE 0433-1028, which is the first detection of a nearby luminous AGN (redshift 0. 0355) with FIFI-LS onboard the airborne observatory SOFIA. We compare the spatially-resolved star formation tracers [C II], as provided by our SOFIA observations, and Hα from MUSE optical integral-field spectroscopy. We find that the [C II] emission is mainly matching the extended star formation as traced by the extinction-corrected Hα line emission but some additional flux is present. While a larger sample is needed to statistically confirm our findings and investigate possible dependencies on AGN luminosity and star formation rate, our study underlines the necessity of collecting a spatially-resolved optical-FIR dataset for nearby AGNs, and shows that it is technically feasible to collect such datasets with FIFI-LS onboard SOFIA.
The Close AGN Reference Survey  (CARS, www. cars-survey. org, Husemann et al. 2017 ) comprises a spatially-resolved multiwavelength dataset of nearby (0. 01 < z < 0. 06) luminous AGNs that are ideal as a bridge between the well-studied local AGN population and more distant quasi-stellar objects (QSOs,  Bertram et al. 2007; Busch et al. 2016). It therefore provides a reference data set for high-redshift galaxies and also offers a range of AGN luminosities (L bol ∼ 10 43 -10 45. 5 erg s -1 ) that allows for a statistical analysis of possible deviations from the [C II]-SFR relation as a function of the AGN luminosity. In this letter, we report the first spatially-resolved detection of [C II] line emission in a nearby luminous AGN with the airborne Stratospheric Observatory For Infrared Astronomy (SOFIA,  Young et al.
1. The fitted [C II] line has a signal-to-noise of ∼18. The line width is FWHM≈ 380 km s -1 (290 km s -1 after correcting for instrumental resolution) and the peak velocity of the [C II] emission coincides with that of the Hα line within 30 km s -1. This demonstrates FIFI-LS ability to detect extragalactic sources, and extends SOFIA's scope from sources in the immediate Galactic neighborhood to nearby galaxies and AGNs. Optical integral-field spectroscopy with the Multi-Unit Spectroscopic Explorer (MUSE;  Bacon et al. 2010 ) is available from CARS. HE 0433-1028 was observed in December 2014 with a total on-source integration time of 600 seconds. The reduction with the standard ESO pipeline  Weilbacher et al. (2012)  results in a data cube with a large field-of-view (FOV) of 1 × 1 which matches the FIFI-LS FOV.
MODELING THE [C II] EMISSION With the available FIFI-LS data we can spatially distinguish between the central region that might be influenced by the AGN and the star formation along the bar. In Fig. 3 , fourth panel, we show the flux distribution of the [C II] line, which we derive by summing up the spectra on a spaxel-by-spaxel basis between 163. 2 µm and 163. 43 µm. The first value was chosen based on the Hα spectrum and the fit described in Sect. 2. 1 2 , the latter value was chosen to avoid the atmospheric absorption 2 We confirmed that changing the starting value to e. g. 163. 1 µm leads to the same results within the uncertainties. feature (see Fig. 1 ). We correct for missing flux in this wing by applying a correction factor of 1. 5 which was derived from the integrated spectrum by comparing the total flux in the Gaussian with the flux derived when summing only in the mentioned interval.
5). This corresponds to reaching the so-called "extreme AO" regime where phase-mask coronagraphs such as the vortex can exponentially converge to their design null depth for unaberrated on-axis starlight. The paper is structured as follows: first, a brief reminder of the vector vortex technology is provided, with further details in the Appendix section. Second, pupil stop design considerations are exposed, and expected vortex raw contrast performances for the Subaru/SCExAO optical configuration are numerically-simulated. Third, the SCExAO near-infrared coronagraphic beam train is described, followed by the measured null depth and throughput performance using the SCExAO internal calibration source. Finally, a few examples of on-sky results during recent observing runs are presented, including raw coronagraphic images as well as ADI-only reduced datasets, for "median observing conditions" on Maunakea and total exposure times on target of about 600 s.
Further examination of the high-framerate non-coronagraphic PSF dataset (3,000 frames at 20 µs integration time) on Procyon, revealed a residual tip/tilt jitter at this frequency, in the order of 0. 25 λ/D tip/tilt rms (10 mas rms). This seems consistent with the "bump" observed around 200 Hz  (Lozi et al. 2016) , as this frequency is also outside the ~ 100 Hz bandwidth of the LLOWFS used during this on-sky calibration sequence. Poor tip/tilt jitter residuals as an explanation for the limited null depth is further reinforced by investigating the evolution of the instantaneous attenuation in time, within the high-speed Procyon coronagraphic time series (3,000 frames at 1 ms integration time), exhibiting instantaneous peak-to-peak attenuation numbers as high as APTP ~ 35, while the mean attenuation remains limited to <APTP> ~ 18.
1 degrees East of North. As seen on Figure  6 , a basic ADI contrast (5-sigma) of about 8•10 -5 is reached at 0''. 3, and 10 -5 is achieved past 0''. 7 (see Table  3 ). Another one to two magnitudes ALOCI contrast gain can be obtained on deeper exposure ADI datasets with larger parallactic angle rotation (see e. g. Currie et al. 2017).
15 λ/D) have been derived by  Huby et al. 2015  (see also  Serabyn et al. 2017)  in the case of an unobstructed aperture: 2 2 ( ) 8 t N t π  (1) for a charge-2 vortex, with t being the tip/tilt offset in units of λ/D, and 4 4 ( ) 32 t N t π  (2) in the case of a charge-4 vortex  (Jenkins et al. 2008). In Figure  A1 , we present a few simulated examples, using our IDL software code: the cases of charge-2 and charge-4 vortices for unobstructed apertures, but also for the actual SCExAO pupil configuration, using the Lyot stop configuration as in Table  2. The IWA is defined as the angular separation at which a point source experiences a transmission of 0. 5, and it corresponds to 1. 7 λ/D for the charge-2 vortex currently equipping SCExAO. In Fig. A1 , we can also notice a "shoulder" or "plateau" in terms of throughput for both the charge-2 and charge-4 vortex when dealing with the Subaru pupil: this can be explained by the interplay between the donut shaped PSF (stronger Airy rings) and the 25-µm sized metallic dot masking the central defect of the vortices.
f. Supplementary Note 3). However, our data on the YbT 2 Si 2 series demonstrate that once the system enters from the strongly mixed-valent into the Kondo regime, T v stops to decrease and stays within a factor of two at a universal value, even when T K drops by four orders of magnitude. We note that this effect is also clearly visible on recent X-ray absorption spectroscopy (XAS) data on YbNi 3 Ga 9 under pressure  33. When the pressure is increased from p = 0 to p = 16. 1 GPa, the valence at low T < 10 K increases continuously from v = 2. 6 to v = 2. 88, but the T scale on which v is increasing towards 3+ does not change significantly (Fig. 2  in Ref. 33). Our findings are summarized in Fig. 4  where we plot for each Kondo lattice compound the experimentally measured low temperature deviation from the trivalent Yb state, i.
ACKNOWLEDGMENTS We thank  L. Simonelli  for assistance during the experiments at the  ESRF. This work was supported by the  German Research Foundation (DFG)  (grants  VY64/1-3 ,  GE602/2-1 ,  GE602/4-1 ,  KR3831/5-1 ,  Fermi-NEst ,  GRK1621  and  SFB1143 ) and  Saint-Petersburg State University  under Research Grant  15. 61. 202. 2015.
Acknowledgements: We thank  Jan de Boer ,  Billy Cottrel ,  Óscar Dias ,  Monica Guicȃ ,  David Kutasov ,  Finn Larsen ,  Oleg Lunin ,  Emil Martinec ,  Miguel Paulos ,  Ioannis Papadimitriou ,  Andrea Puhm ,  Rodolfo Russo ,  Kostas Skenderis ,  Marika Taylor  and  Nick Warner  for useful discussions. This work was supported in part by the  ANR  grant  Black-dS-String   ANR-16-CE31-0004-01. The work of PH is supported by an  ENS   Lyon grant. The work of DT is supported by a  Royal Society Tata University Research Fellowship.
B. X-ray diffraction The lattice parameters and the phase constitution were determined by using the Rietveld refinement software MAUD  15. The phase diagram  14  shows two equilibrium phases depending on the proportions of Mn and Al atoms : β-phase and γ 2 -phase. The phase is stable at high temperature but can be obtained in non-equilibrium conditions. The τ metastable phase is obtained after annealing the quenched -phase. From X-ray diffraction, the as prepared powder is a pure -phase. As shown in Fig. 1  and Table II, the material is almost fully in τ -phase, but the sintering process produces the precipitation of few % of β-phase. A higher proportion of τ -phase for the same sintering temperature and pressure is obtained by decreasing the milling velocity compared to ref. 4.
This feature, as trivial as it might appear, imposes additional restrictions on FIMP dark matter model-building. As simple as the freeze-in idea might be, in practice calculations can get fairly cumbersome if a large number of processes contribute to dark matter production. As we will see in the following Sections Clockwork FIMP scenarios do, indeed, tend to involve a large number of BSM fields and processes through which dark matter particles can be produced. In order to account for all of them, we employ the latest version of the micrOMEGAs dark matter code  [44]  which has been recently upgraded in order to compute the abundance of FIMP dark matter candidates in freeze-in scenarios. The implementation of all models in micrOMEGAs5. 0 has been performed through the FeynRules package  [45].
VII. ACKNOWLDGEMENTS We would like to aknowledge enightening discussions with Geneviève Belanger, Cédric Delaunay, R. Sekhar Chivukula, Ashwani Kushwaha and Alexander Pukhov, whom we would also like to thank for support with micrOMEGAs5. 0. A. G. was supported by the Labex We now further define two sequences h = {0, 1, 0,. }, and x = {x, 0, 0,. , }, and use the Cauchy convolution theorem for the product of two sequences, a = {a} ∞ i=0 , b = {b} ∞ i=0 , as ab = ∞ i=0 c i , where c i = i l=0 a l b i-l , to rewrite the recursion relation by convolution of Eq. (A4) with h 2 as 13 X = (f + cx 1 )h ah 2 + (b -λ)h + c. (A5) The denominator of this equation has two roots, which can be written as γ ± = -(b -λ) ± √ ω 2a , with ω = (b -λ) 2 -4ac; γ ± , ω ∈ C. ( A6 ) Let γ = p ± iq, such that γ + γ -= p 2 + q 2 = c/a, and γ + + γ -= 2p = (λ-b) a.
ILP (reference  ANR-10-LABX-63 ) part of the Idex SUPER, and received financial state aid managed by the  Agence Nationale de la Recherche , as part of the  programme Investissements d'avenir  under the reference  ANR-11-IDEX-0004-02. The work of D. S and K. M. is supported by the  National Science Foundation, U. S. A  under Grant No. 1519045. A. G. and D. S. would like to thank the organisers of the 2017 Les Houches -Physics at TeV Collders workshop where this project was initiated for their warm hospitality. D. S acknowledges  LPTHE-Paris  for hospitality during the completion of part of this work. K. M. acknowledges LAPTh, Annecy for hospitality where part of this work was carried out. This work was supported in part by  Michigan State University  through computational resources provided by the  Institute for Cyber-Enabled Research.
The data points of figure 2 of  Nieuwenhuizen (2017)  are estimates, and partly upper estimates, for the acceleration in theories, such as MOG, where light moves in the gravitational potential  (Nieuwenhuizen 2017). The vanishing of the MZH acceleration at small radii in their figure  1  is perfectly physical while consistent with the finite value of their upper bound. Third, MZH employ A1689 parameters from our paper  Nieuwenhuizen (2017) , in particular from 2 runs of X-ray data by the Chandra satellite that were introduced by us in  Nieuwenhuizen & Morandi (2011). Below we present here the final A1689 Chandra data for the X-ray gas, and notice a calibration error in analysing the previous data sets. Hence the gas fits must be redone; the implication for MOG will be presented below. We also present new gas and strong lensing data for a second, well relaxed cluster, A1835, and analyse them in a similar fashion.
Data for the X-ray gas We present the final data of the CHANDRA X-ray Observatory. The data reduction was carried out using the CIAO 4. 8. 1 and Heasoft 6. 19 software suites, in conjunction with the Chandra calibration database (CALDB) version 4. 7. 2. Figure  1  exhibits the resulting 56 data CHANDRA points at radii between 7. 7 and 963 kpc. Let us recall some properties of the X-ray gas. We adopt a typical Z = 0. 3 solar metallicity for A1689, so that to a good approximation np = 11 nα. With elements heavier than He neglected and 25% of the gas weight in He, this implies that ne = (13/11)np. The particle density is ne + np + nα = (25/13)ne and hence the thermal pressure pg = (25/13)nekBTg. The mass density reads ρg = mN np + 4mN nα = (15/11)mN np, so ρg = mN ne with mN = (15/13)mN = 1. 154 mN.
The mean molecular weight in p = ρgkBT /µmN is µ = 3/5. These factors agree within a per mille with ne + nion = 1. 9254 ne and µ = 0. 5996 from the solar abundance tables of  Asplund et al. (2009). Further data for ne have been obtained from the ROSAT satellite with its Position Sensitive Proportional Counters (PSPC) camera  Eckert et al. (2012a). A resulting set of 50 "parametric" data points for np is publicly available  (Eckert et al. 2012a,b). As ri-values we take the mids of their bins. As seen in figures 1 and 2, the Chandra and PR data sets overlap within their error bars for radii between 268 and 872 kpc (except for the outlying last Chandra point).
Strong lensing in A1689 The strong lensing (SL) data arise from background galaxies lensed by the cluster. While a full Einstein ring does not occur, galaxies not-too-far from the sightline to the cluster centre are observed as an arclet or a set of n ≤ 7 arclets in A1689. Its SL mass model was first derived in Limousin et al. (2007). From the arclets the computer code Lenstool, presented by  Jullo et al. (2007)  and  Kneib et al. (2011) , has now produced candidate maps for the 2d mass distribution; this being an underdetermined problem, a set of maps, labeled by µ = 1, • • • , N , can be generated. In total N = 1001 solutions ("samples") have been achieved. These maps are integrated over circles around the centre to yield the 2d mass M M 2d (rn) πr 2 n = 1 N µ Σ (µ) n , (n = 1, • • • , 149), (8) In shells without arclets, the Lenstool program produces constant values for M 2d , of which only the one at smallest r provides physical information.