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Whilst a reasonable harmonic fit to the ESPaDOnS data can be achieved using this period, it does not produce an acceptable phasing of all available 〈 B z 〉 measurements. Figure 1. Photometric (top) and magnetic 〈 B z 〉 (bottom) measurements, phased with periods determined from (left to right) K2 photometry, all 〈 B z 〉... | {
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comparison once the angular positions of the satellites are randomized around this point. From this tensor we compute its eigenvalues, λ 1 > λ 2 > λ 3, and corresponding eigenvectors,,,. We define the size of the three ellipsoidal axis as a = λ 1, b = λ 2, and c = λ 3. We also define as the vector perpendicular to the ... | {
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ACKNOWLEDGEMENTS The authors thank an anonymous reviewer for comments and suggestions that strengthened our manuscript. NWCL gratefully acknowledges support from the American Museum of Natural History and the Richard Guilder Graduate School, specifically the Kalbfleisch Fellowship Program, as well as support from a Nat... | {
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BDM gratefully acknowledges support from NASA Fermi grant NNX14AQ68G, NSF grant AST-1410950, and the Alfred P. Sloan Foundation. We thank the anonymous reviewer for several helpful suggestions and for emphasizing the applicability of our results to Type IIn supernovae. | {
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ACKNOWLEDGEMENTS We thank Dougal Mackey, Adrian Price-Whelan, David Hogg, Gurtina Besla, David Schiminovich, Alis Deason, and Sergey Koposov for illuminating discussions. The research leading to these results has received funding from the European Research Council under the European Union’s Seventh Framework Programme ... | {
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I thank Duncan Galloway, Zac Johnston, and Hendrik Schatz for useful discussions, and acknowledge the instructive tutorials from Ed Brown, Andrew Cumming, and Rob Farmer located on the MESA Marketplace (http://cococubed.asu.edu/mesa_market/) that helped at the beginning stages of this work. Relevant MESA inputs for thi... | {
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Lasota (2007) have updated this work, for a sample of ten CVs. The importance of this test was revived by Schreiber Gänsicke (2002), who pointed out that the HST FGS parallax distance of SS Cyg, the archetypal dwarf nova, led to a revised mass transfer rate that placed this outbursting system in the stable region of th... | {
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an antenna with cos 2 beam would have a maximum temperature at the LST when the Galactic center is at zenith. This also corresponds to the spectrum having the largest rms residual among the various mock spectra considered here. For various large-area samplings of the sky, we have thus demonstrated that the foreground c... | {
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origin. Our findings from this Section for the radial metallicity distribution of red and blue GCs in massive ETGs are summarized in a schematic way in Fig. 2. This representative diagram shows the same radial metallicity gradient for the red (metal-rich) GCs and the blue (metal-poor) GCs, only offset by 1 dex in metal... | {
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of the CSM density profile and the forward shock evolution together determine the temporal behavior of the optically thin radio flux density. For s = 0 and, the flux density rises with time as once, the flux density evolution steepens to (visible as a kink in the model light curve of Figure 1 with cm −3 around 100 days... | {
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We first thank M.S. Ruderman for helpful comments. A.H. thanks the School of Mathematics and Statistics, University of Sheffield (UK) for the support received. R.E. is thankful to the NSF, Hungary (OTKA, Ref. No. K83133) and is grateful to STFC (UK) for the awarded Consolidated Grant, and, The Royal Society for the sup... | {
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where and are two cylindrical coordinates; is the axial ratio, is a structure parameter, and is a function of, such that becomes the density at radius, which defines a volume containing half of the total mass of the component (for details, see Tamm et al. 2012 ). The gravitational potential derivative of a component, n... | {
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version of the full table is available. Table 3 The Spectral Parameters Associated with the H β Emission Line Note. Column information is as follows: Column [1]: 4FGL name; Column [2]: redshift; Column [3]: log-scale continuum luminosity at 5100 Å; Column [4]: FWHM of H β line, in km s −1; and Column [5]: log-scale H β... | {
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ACKNOWLEDGEMENTS It is a pleasure to thank Frdric Arenou for helpful comments. HL and JB received support from the Natural Sciences and Engineering Research Council of Canada (NSERC; funding reference number RGPIN-2015-05235) and from an Ontario Early Researcher Award (ER16-12-061). JB also received partial support fro... | {
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identified toward these positions. Column densities of this species are presented in Table 3. Figure 5. Detected transitions of CH 3 NHCHO in the spectrum toward position MM1-nmf. The observed spectrum is plotted in black, with the synthetic spectrum overplotted in blue and the rest-frequency center of the transition i... | {
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core. Figure 12 shows that such a quiescent gas environment barely affects the line ratios, as the difference in the line ratios calculated at the turbulence 0 and 150 km s −1 is very small. Figure 12. Line intensity ratio relative to w vs. log of hydrogen column density. Solid: no turbulence. Dashed: turbulence 150 km... | {
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This work is based on observations made with the NASA/ESA Hubble Space Telescope, obtained at the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 526555. These observations are associated with program #13364. R.C. acknowled... | {
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We are grateful to Francisco Prada, Risa Wechsler, Chiaki Hikage, and Surhud More for useful discussions. We acknowledge Yu Lu and Andrew Benson for useful discussions related to SAMs. This work was supported by World Premier International Research Center Initiative (WPI Initiative), MEXT, Japan. Numerical computations... | {
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We are indebted to Jimmy Irwin, Matthieu Roman, Jean-Baptiste Melin, Adam Mantz, Nabila Aghanim, Maxim Markevich, Erwin Lau and Daisuke Nagai for valuable comments. AM gratefully acknowledges the hospitality of the Harvard-Smithsonian Center for Astrophysics and of the NASA's Goddard Space Flight Center. We acknowledge... | {
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This work was supported by INFN and ASI under ASI-INFN Agreement No.2014-037-R.0. M.S.P. and E.E.V. acknowledge partial financial support from the the South African National Research Foundation (NRF) under their Research Cooperation Programme. E.E.V. thanks the Space Science Division of the South African Space Agency (... | {
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shells, with secondary typical scales as small as (0.5–1) × 10 9 cm. The slope of the VSH power spectra stays consistent over time regardless of the presence or absence of rotation. In all cases we find nearly circular shapes for the characteristic convective elements. In terms of the 2D convective flow properties, our... | {
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drops (to 30%) in the lowest redshift bin. This decline may not be reliable for two reasons. First, the size of the star-forming sample at 0.5 z 1.0 is very small (only 10 objects), and therefore the sample proportions are not statistically significant. Second, the H -band images for the low- z objects are missing the ... | {
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This material is based upon work supported by the National Science Foundation under grant No. AST-1109683. Any opinions, findings, and conclusions or recommendations expressed in this material are those of the author(s) and do not necessarily reflect the views of the National Science Foundation Based on observations (G... | {
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from stellar activity). The likelihood function is given by where i indexes the observations acquired with the I th instrument, is the nominal uncertainty of each RV measurement, and s I are the zero-point and extra noise parameters (also called jitter) of each instrument, and the Doppler signal from a companion on the... | {
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and planets with little Ly absorption but strong emission can be used to distinguish between these two classes of thermospheres. Based on the predicted strong absorption signals, WASP-80 b and GJ 3470 b are the most promising targets among our sample in the search for yet undetected escaping atmospheres. Appendix A: Ca... | {
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conditions requires equilibrium total pressure balance across each interface. This demands that the total (gas plus magnetic) pressure is constant:where μ is the permeability of free space. The sound speed in each region can be expressed as for. Here, γ is the adiabatic index, which is uniform across every domain, unde... | {
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Swift Observatory short GRBs suggests that of those with an X-ray afterglow, >30% have evidence for additional energy input at later times, most commonly in the form of a long-lived plateau, persisting at bright levels for hundreds to thousands of seconds (with the majority at the shorter end), or in the form of X-ray ... | {
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We thank Ralf-Dieter Scholz for constructive conversations during the preparation stage and the anonymous referee for indicating revisions that have improved our analysis and results. We also thank the Cambridge Astronomy Survey Unit (CASU) and the Wide Field Astronomy Unit (WFAU) in Edinburgh for providing calibrated ... | {
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would either require a larger sample of observed dwarf galaxies with smaller error bars and systematic errors of (a difficult prospect) or obtaining spatially resolved rotation curves for 400 pc (within the half-light radii) in small dwarfs, where Fig. 9 shows that CDM/WDM and SIDM/SIWDM could be differentiated. While ... | {
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all but one observation the exposure time was particularly low (i.e. 0.5–1 ks). We estimated the Bayesian 95 per cent upper limit (Kraft et al. (1991) to the source count rate from the observation with the longer exposure (4.2 ks, n. 4, obs ID 00087498001). It was equal to 0.0025 count s −1. Using WebPIMMS, it converts... | {
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component to the width. Dynamical studies of galaxies typically use Newton’s gravity. However, it has been argued that once galactic masses are considered, relativistic effects arising from large masses (rather than large velocities) may become important (Deur 2009, 2017, 2019 ). Their physical origin is that in genera... | {
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t b to be 23.0. Figure 3. Multi-band light-curve fitting of SN 2013dy using Equation (1) for estimating t 0. The value of is fixed to be 1.90 and t b is fixed to be 23.0 during the fitting procedure. Diamond-shaped data points are included in the fitting, while cross-shaped ones are excluded. After applying the t 0 fit... | {
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The project was partially supported by National Science Centre, Poland, grant no. 2017/26/A/ST9/00756 (Maestro 9). V.K. acknowledges Czech Science Foundation no. 17-16287S. | {
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ACKNOWLEDGEMENTS This work is based upon observations obtained with the Georgia State University (GSU) Center for High Angular Resolution Astronomy (CHARA) Array at Mount Wilson Observatory, and the University of Hawai‘i 2.2-m telescope on Maunakea. The authors wish to recognize and acknowledge the very significant cul... | {
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This work has made use of data from the European Space Agency (ESA) mission Gaia (https://www.cosmos.esa.int/gaia ), processed by the Gaia Data Processing and Analysis Consortium (DPAC, https://www.cosmos.esa.int/web/gaia/dpac/consortium ); data from the Two Micron All Sky Survey, which is a joint project of the Univer... | {
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sample of SNe included in this data release, our adopted classifications and dates of peak brightness (if available), and the values we used to perform redshift and dust-reddening corrections. Table 3 provides a description of the spectra included in our sample. Our research group utilizes a database of observations an... | {
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Acknowledgements The authors would like to thank the referee Francisco-Shu Kitaura and Stefan Gottlöber for providing comments that helped clarified the paper as well as Sergey Pilipenko for very useful discussions. JS acknowledges support from the Astronomy ESFRI and Research Infrastructure Cluster ASTERICS project, f... | {
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in their targets. Hence, we can conclude that in stars belonging to the transitional branch, the cycle length and the rotation period are uncorrelated. 5.2. Relationship between <italic>P</italic><inline-formula specific-use="simple-math"><sub>cyc</sub></inline-formula> and global stellar parameters We investigated how... | {
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x -axis in all the panels are the observation wavelength. The horizontal dashed line in the lower right panel shows where τ obs = 0.6. On the other hand, we caution that the DSHARP opacity adopted here is for compact spheres without porosity, and that the mixture of different compositions are handled with the Bruggeman... | {
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of the mean pitch angle remains similar over the whole energy range. However, evolution timescales and peak amplitudes change as expected. Next, the influence of the amplitude of the magnetic field of the plasma wave has been studied (Section 5 ). Again, simulation results and analytic predictions have been compared. S... | {
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outward flux is not conserved; its losses are a source for the photon angular momentum flux (Fig. 4 ). But in the model solution, the disc can only supply the flux from the relatively small amount of material within the ISCO, because just outside the ISCO the disc velocity is outward: it is not accreting! This cannot g... | {
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becomes more and more noisy toward higher frequencies and therefore the de-convolved power spectrum will be more and more uncertain toward higher and higher frequencies. Figure 15. (a) Simulated red-noise light curve (a = 2), containing 1000 data points with a sampling interval of one day (blue open circles), along wit... | {
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are quite discrepant (0.2 dex and 0.8 dex in our two stars, respectively). The 4215.5 Å line of the star S11–97 is affected by the CN molecular band in this region. Spectral synthesis taking into account the carbon abundance derived in the CH band led to an abundance that agrees better with the 4077.7 Å line. Yttrium. ... | {
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"text": "λ 5853 Å)",
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"text": "... | [] |
We are grateful to the referee, Brent Groves, for very constructive comments that helped to improve the manuscript. We thank Stefanie Komossa (MPIfR), Pavel Kroupa (University of Bonn), Thomas Krichbaum (MPIfR), Madeleine Yttergren (University of Cologne), Bozena Czerny (CFT PAN), Mary Loli Martinez-Aldama (CFT PAN), a... | {
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"text": "Brent Groves,",
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{
"text": "Pavel Kroupa",
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to account for the radiative recombination continuum and lines, a cutoff power-law model to account for the off-nuclear X-ray sources, in addition to the AGN-related emission, which is parametrized by two different MYTorus scattered and line components, in addition to the transmitted one described by the zeroth-order c... | {
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"text": "2–10 keV",
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"text": "6.... | [] |
We are grateful to the STScI staff members for help in scheduling the intricate STIS observations. We thank the Paranal Observatory for conducting the UVES observations. Stony Brook’s continuing involvement in the SMARTS Consortium is made possible by generous support from the Provost of Stony Brook University. A.M. wa... | {
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"text": "STScI",
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component of Fe K α emission (log ξ = 0). A very similar result is reached by performing the same test on the 2014 mean EPIC-pn + NuSTAR spectrum (Δ χ 2 = 52), resulting in a modest reflection strength, R ∼ 0.6, while the photon index and Fe abundance remain unchanged: Γ ∼ 1.8; A Fe ∼ 3. The remaining key parameters in... | {
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"wavelength": [
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"text": "Fe K α",
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"text": "Fe K band,",
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{
"text": "hard X-ray",
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],
"formula":... | [] |
other words, the PDFs are equal, because the system self-adjusts, not because glitch sizes are correlated with forward waiting times, as in the α ≪ α c (β) regime in Section 4. The explanation for the qualitative behaviour seen in Fig. 20 is the same as for Fig. 13. Figure 20. Correlation between sizes and forward/back... | {
"entities": {
"formula": [
{
"text": "α ≪ α c (β)",
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"end": 155
},
{
"text": "φ( x) = x δ",
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{
"text": "N = 10 6",
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{
"text... | [] |
where the rise speed of the flux tube at a depth of 20 Mm is more than about 150 m s −1 produce preemergence diverging flows that are not consistent with the observations. Norton et al. (2017) found from HMI vector magnetograms that the surface magnetic flux increases during the emergence process more slowly than predi... | {
"entities": {
"citation": [
{
"text": "Norton et al. (2017)",
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"end": 192
},
{
"text": "Norton et al. (2017)",
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},
{
"text": "Kosovichev et al. (2018)",
"start": 632,
"end":... | [] |
This is well in the range of those measured for UCXBs. 4.2. The nature of the accretor Determining the nature of the compact object in an unclassified LMXB is often challenging. It can be assessed based either on a dynamical measurement of the mass of the compact object (via optical and near infrared spectroscopy durin... | {
"entities": {
"wavelength": [
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"text": "UCXBs.",
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"text": "LMXB",
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{
"text": "optical",
"start": 276,
"end": 283
},
{
"text": "near inf... | [] |
Acknowledgements I would like to thank the anonymous referee for valuable comments that improved this work. The author is supported by the Grants-in-Aid for Scientific Research of the Japan Society for the Promotion of Science (16H07413, 17H02864). | {
"entities": {
"grant": [
{
"text": "Grants-in-Aid for Scientific Research",
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{
"text": "(16H07413,",
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"end": 237
},
{
"text": "17H02864).",
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... | [] |
velocity distribution of the gas within the velocity range from 495 to 495kms 1 (1kms 1 steps). The emission for one square degree centred on the SMCNOD exhibits two main peaks: 94 and 186kms 1 (which are shown in Figs 8 and 9, respectively). These velocities agree with the velocity field related to the MS at the SMCNO... | {
"entities": {
"celestialobjectregion": [
{
"text": "SMCNOD",
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"text": "SMCNOD",
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{
"text": "SMCNOD",
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"end": 844
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{
"te... | [] |
ACKNOWLEDGEMENTS We are very grateful to the constructive and detailed review carried out by our anonymous referee. His/her numerous and wise comments have helped to significantly improve this paper. We thank Manuel Peimbert, Jairo Méndez-Abreu, Leticia Carigi, and Rolf Kudritzki for their useful comments. This paper i... | {
"entities": {
"person": [
{
"text": "Manuel Peimbert,",
"start": 209,
"end": 225
},
{
"text": "Jairo Méndez-Abreu,",
"start": 226,
"end": 245
},
{
"text": "Leticia Carigi,",
"start": 246,
"end": 261
},
... | [] |
the stepwise trajectories of incident CH ions within Titan’s upper atmosphere, all starting at an energy of 50 keV under normal incidence. Three different cases are indicated in the upper panel. For each incident ion, the portion of its trajectory between two consecutive collisions is displayed as the projection to the... | {
"entities": {
"celestialobject": [
{
"text": "Titan’s",
"start": 53,
"end": 60
},
{
"text": "Titan’s",
"start": 1616,
"end": 1623
}
],
"citation": [
{
"text": "Backes et al. 2005",
"start": 880,
"end": ... | [] |
The authors thank the referee for useful feedback which helped improve the final manuscript. This research has made use of data obtained with the NuSTAR mission, a project led by the California Institute of Technology (Caltech), managed by the Jet Propulsion Laboratory (JPL) and funded by NASA, and with XMM-Newton, an ... | {
"entities": {
"telescope": [
{
"text": "NuSTAR",
"start": 146,
"end": 152
},
{
"text": "XMM-Newton",
"start": 305,
"end": 315
}
],
"organization": [
{
"text": "California Institute of Technology (Caltech),",
"s... | [] |
The present work was funded by STFC (UK) through the University of Cambridge DAMTP astrophysics grant and the University of Strathclyde UK APAP network grant ST/J000892/1. | {
"entities": {
"organization": [
{
"text": "STFC",
"start": 31,
"end": 35
},
{
"text": "University of Cambridge",
"start": 53,
"end": 76
},
{
"text": "University of Strathclyde",
"start": 110,
"end": 135
}... | [] |
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