adsabs/WIESP2022-NER huggingface dataset:
Paper: 2017ApJ...846..106L (acknowledgments)
This work was supported by a grant from the US Air Force Office of Scientific Research in the Basic Research Initiative “Understanding the Interaction of CMEs with the Solar–Terrestrial Environment,” and by an STFC consortium grant to the universities of Dundee and Durham. The authors thank C. Prior, M. Weinzierl, P. Wyper, and T. Whitbread for useful discussions concerning the development of this work, which made use of the Hamilton HPC Service of Durham University. SOLIS data used here are produced cooperatively by NSF/NOAO and NASA/LWS. Facility: SOLIS. Software: Python, SunPy (SunPy Community et al. 2015 ), SciPy (Jones et al. 2001 ), NumPy (van der Walt et al. 2011 ), Mayavi (Varoquaux Ramachandran 2011 ), Matplotlib (Hunter 2007 ), FRoDO (Lowder 2017 , https://github.com/lowderchris/FRoDO ).
Paper: 2017ApJ...842...97L (acknowledgments)
This work uses data obtained through the Telescope Access Program (TAP), which is funded by the National Astronomical Observatories of China, the Chinese Academy of Sciences (the Strategic Priority Research Program, “The Emergence of Cosmological Structures” Grant No. XDB09000000), and the Special Fund for Astronomy from the Ministry of Finance. The observations reported in this study were obtained at the MMT Observatory, a joint facility of the Smithsonian Institution and the University of Arizona. This research has made use of the NASA/IPAC Extragalactic Database (NED), which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. This work is supported by the National Basic Research Program of China (973 Program)(2015CB857004), and the National Natural Science Foundation of China (NSFC, Nos. 1320101002, 11433005, 11421303, and 11673004), and the Yunnan Applied Basic Research Projects (2014FB155). E.W. was supported by the Youth Innovation Fund by the University of Science and Technology of China (No. WK2030220019). Facility: MMT. Software: SExtractor (Bertin Arnouts 1996 ), xfitfibs, HSRED, STARLIGHT (Cid Fernandes et al. 2005 ), MPFIT (Markwardt 2009 ), PyNeb (Luridiana et al. 2015 ).
Paper: 2018ApJ...861...52K (acknowledgments)
We thank Lydia Heck and James Willis for their assistance with computational challenges. We thank the anonymous referee for their helpful comments. This work was supported by the Science and Technology Facilities Council (STFC) grants ST/P000541/1 and ST/L00075X/1, and used the DiRAC Data Centric system at Durham University, operated by the Institute for Computational Cosmology on behalf of the STFC DiRAC HPC Facility ( www.dirac.ac.uk ). This equipment was funded by BIS National E-infrastructure capital grant ST/K00042X/1, STFC capital grants ST/H008519/1 and ST/K00087X/1, STFC DiRAC Operations grant ST/K003267/1 and Durham University. DiRAC is part of the National E-Infrastructure. J.A.K. is funded by STFC grant ST/N50404X/1. V.R.E. acknowledges support from STFC grant ST/P000541/1. R.J.M. acknowledges the support of a Royal Society University Research Fellowship. L.F.A.T. and D.G.K. acknowledge support from NASA Outer Planets Research program award NNX13AK99G. L.F.A.T., D.C.C., D.G.K., and K.J.Z. acknowledge support from NASA Planetary Atmospheres grant NNX14AJ45G. C.L.F. was funded in part under the auspices of the U.S. Dept. of Energy, and supported by its contract W-7405-ENG-36 to Los Alamos National Laboratory.
Paper: 2016A&A...594A..69D (acknowledgments)
This work is partly supported by the European Research Council under the European Community’s Seventh Framework Programme (FP7/2007-2013 Grant Agreement No. 247060-PEPS and grant No. 320478-TOFU). B.D. thanks the University of Exeter for support through a Ph.D. studentship. D.S.A. acknowledges support from the NASA Astrobiology Program through the Nexus for Exoplanet System Science. N.J.M. and J.G.’s contributions were in part funded by a Leverhulme Trust Research Project Grant, and in part by a University of Exeter College of Engineering, Mathematics and Physical Sciences studentship. This work used the DiRAC Complexity system, operated by the University of Leicester IT Services, which forms part of the STFC DiRAC HPC Facility. This equipment is funded by BIS National E-Infrastructure capital grant ST/K000373/1 and STFC DiRAC Operations grant ST/K0003259/1. DiRAC is part of the National E-Infrastructure. This work also used the University of Exeter Supercomputer, a DiRAC Facility jointly funded by STFC, the Large Facilities Capital Fund of BIS and the University of Exeter.
Paper: 2017ApJ...834..108L (acknowledgments)
An anonymous referee’s comments and suggestions are gratefully acknowledged.
Paper: 2020ApJ...890....6S (fulltext)
frequency of the observed maser transition. We use A = 5.570 × 10 −8 s −1 , the highest Einstein coefficient in Lankhaar et al. ( 2018 ) for the ν = 24959.079 × 10 6 Hz CH 3 OH maser transition, and T b = 10 6 –10 7 K, ΔΩ ≃ 0.03–0.003 for the 25 GHz maser line (Leurini et al. 2016 ). Using these values in Equation ( 2 ), we obtain R ≤ 3 ×10 −3 s −1 . Meanwhile, g Ω ≈ 170 s −1 in our observations of OMC-1. This means that R ≪ g Ω, and thus it is unlikely that a rotation of the axis of symmetry for the molecular quantum states is responsible for the shape of the Stokes V profile. Finally, Houde ( 2014 ) found that maser radiation scattering off foreground molecules can increase the antisymmetry in the Stokes V spectral profile of SiO masers. Consequently, if the Stokes V profile were ascribed to the Zeeman effect, one would obtain a much larger value for the magnetic field traced by these SiO masers. While we cannot rule out this effect in our 25 GHz CH 3 OH maser observations, our values are not orders of magnitude higher than the fields expected in such regions, unlike in SiO masers. We will discuss this in more detail in the next subsection. 4.3. Magnetic Fields and Densities If the observed Stokes V profile is caused by a magnetic field in the source, and is not due to any instrumental effects or other non-Zeeman causes discussed in Section 4.2 , then we have a magnetic field from our 25 GHz Class I CH 3 OH maser observation of OMC-1 that is three to four times larger (depending on which hyperfine is responsible for the maser) than the highest magnetic field we have detected to date in Class I CH 3 OH masers at 44 GHz (Momjian Sarma 2017 ). Such a value is not implausible, however; if we assume that the fields are amplified in proportion to the density in the shocked regions where these masers occur, thenwhere B pre and B post are the magnetic fields in the pre- and post-shock regions respectively, and n pre and n post are the densities in these regions. We can use Equation ( 3 ) to calculate B pre and compare it to magnetic fields calculated from other observations. Since our measured fields are in the range 171–214 mG depending on which hyperfine is responsible for the maser transition (Table 3 ), we will use = 171 mG in our calculations; this is convenient because values corresponding to = 214 mG can then be found by multiplying our results by a factor of 1.25. Leurini et al. ( 2016 ) have found that bright Class I methanol masers likely occur in regions with densities in the range 10 7–8 cm −3 , so we will calculate corresponding to both n post = 10 7 and 10 8 cm −3 . For densities in the pre-shocked gas we draw upon the work of Kwan et al. ( 1977 ), who found that a minimum pre-shock density of 10 5 cm −3 is required to produce the observed intensities in the H 2 ν = 1−0 emission lines in OMC-1. Thus, densities in the pre-shocked material of interest are likely of the order of 10 5 cm −3 or higher, but unlikely to be as high as, or
Paper: 2019ApJ...883..101R (acknowledgments)
We thank E. Zirnstein and P. Mostafavi for helpful discussions about PUI pressures and densities, shocks, and wave speeds in the heliosheath. We are grateful to both the Voyager and IBEX teams. This work was supported by NASA Grant 80NSSC18K0237 and by the IBEX mission, which is part of NASA’s Explorer Program. J.D.R. was supported under NASA contract 959203 from the Jet Propulsion Laboratory to the Massachusetts Institute of Technology.
Paper: 2017MNRAS.464.1591P (fulltext)
g ′) and Δμ( r ′ − i ′), with the maximum at only ρ = 0.30 and p = 0.08. The only exception is for the PAS profiles from the r ′ − i ′ breaks sub-sample, where there is a correlation of ρ = 0.49 and p = 0.02. This correlation is due to the same points as the correlation of h 0 with Δ h 0 ( r ′ − i ′0) in the PAS. 4.4.4 Correlations with absolute magnitude, maximum rotation and specific angular momentum Martín-Navarro et al. ( 2012 ) found that the truncation radius of a galaxy is strongly correlated with the maximum rotational velocity v rot of a galaxy, having a correlation of ρ truncation = 0.81. The breaks in their sample were correlated at only ρ break = 0.50. In contrast, Pohlen Trujillo ( 2006 ) report no correlation with rotation. They do report a weak correlation of the brightness at the feature with the absolute magnitude M B,abs . We explore possible correlations of the feature radii R f , surface brightness at the feature μ and differences in brightness between bands at the feature μΔ with absolute magnitude M abs and maximum rotation v rot in Table 7 . We find only one weak correlation in the difference between the g ′ and r ′ surface brightness at the feature radius, as measured with the EP method, with the rotation velocity v rot . The correlation strength is ρ = 0.36 and p = 0.03. Martín-Navarro et al. ( 2012 ) also perform a correlation test of the break and truncation radii with the specific angular momentum j , calculated using the empirical expression by Navarro Steinmetz ( 2000 ), 4 As this is a rescaling of v rot , the correlation remains the same. They find that the feature radius only correlates well beyond r b = 8 kpc. For a smaller disc with v rot 100 kms −1 , r break and v rot are essentially unlinked. When examining the full radii range, we also do not find a statistically significant correlation. The same holds when limiting ourselves to all features beyond r > 8. 4.4.5 Effect of inclination In Section 4.4.2 , we found that the PAS profiles typically tend to have sharper breaks than the ellipse-fit profiles and EP. As the PAS projects data as if it was edge-on, it is also interesting to compare the effect of inclinations in this. To this end, we have tested the correlation of a / b (major axis over minor axis) with scalelengths h 0 and h f , h 0 / h f and R f / h f , in Table 7 . The results are also visualized in Fig. 12 . Figure 12. Correlation of various parameters with inclination (expressed as a / b ). Top row shows with scalelength h 0 (left) and h f (right). Bottom row has the h 0 / h f (right) and R f / h f (left) correlations. The statistical correlation tests are plotted in each panel. Boxes represent the PAS points, while circles represent the EP points. Open markers represent truncations, while filled markers represent boxes. We find no significant correlation between a / b and inner scalelength h 0 . There may be a negative trend visible in the truncation-only sample, as both the EP and PAS profiles
Paper: 2018A&A...613A..74P (acknowledgments)
Acknowledgements A. P. acknowledges support from CONACyT 238631. G. B. acknowledges financial support under the INTEGRAL ASI-INAF agreement 2013-025.R01. This research has made use of the NASA/IPAC Extragalactic Database (NED), which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. This research has made use of data from the MOJAVE database that is maintained by the MOJAVE team ( Lister et al. 2009 ). This work was supported by UNAM-PAPIIT IA101214 and IA102816. We thank Prof. Robert Antonucci for his careful revision of the paper and useful comments.
Paper: 2020MNRAS.492..177C (acknowledgments)
ACKNOWLEDGEMENTS This work was supported by the ERC Consolidator Grant CMBSPEC (No. 725456) as part of the European Union’s Horizon 2020 research and innovation programme. JC was supported by the Royal Society as a Royal Society URF at the University of Manchester, UK.
Paper: 2019MNRAS.484.3491T (acknowledgments)
ACKNOWLEDGEMENTS We thank Nir Shaviv and Reetanjali Moharana for helpful discussions. The research was supported by an ERC advanced grant TReX and by the CHE-ISF I-CORE center for excellence.
Paper: 2017A&A...597A..46S (fulltext)
transform Fig. A.4 Illustration of the backward interpolation. Interpolation is performed for inertial knots (bottom line) on intervals between comoving knots (top line). Interpolation weights are indicated on sloped lines connecting corresponding knots between the frames. Linear interpolation is used for internal inertial knots that lie on the internal comoving intervals with l.h.s. (solid) and r.h.s. (dotted) weights. Weights are named with respect to the comoving frame so that the line slopes are opposite to those in the forward interpolation. Constant extrapolation with unity weights is used for inertial knots exactly matching comoving knots , or for inertial knots that lie on the or intervals. Both end cases are given in gray color. Once has been fully accumulated, we compute the comoving profile ratio and keep it in memory for all frequency knots simultaneously. This makes the backward transform much easier than the forward one, because we can employ a standard interpolation. The backward transform can be directly evaluated because it is just an interpolation from the comoving frame to the inertial frame (see green notations in Fig. A.2 ): As follows from Fig. A.4 , each depends on either one or two comoving knots . It depends on two knots if the inertial knot lies on the comoving interval , where both and are internal knots (), that is, . In this case we do linear interpolation: For the backward transform, knots and weights are always denoted by and with no superscript to tell them from knots and weights for the forward transform. It depends on one knot if the inertial knot matches the comoving knot , that is, . It also depends on one knot if the inertial knot lies on intervals before or after , which means or , because we use constant extrapolation. Therefore, in those three cases: Appendix A.2: General interpolation One can perform the searches and interpolations described in Sects. A.1.4 – A.1.5 on the fly. This does not require any additional storage, and can be used for a frequency grid of arbitrary spacing, but the algorithm is slow. We call this algorithm general interpolation. Appendix A.2.1: General forward transform We search for all comoving knots that lie on the intervals and , that is, whose comoving frequencies are either between and , or between and . We take the current inertial knot and its left neighbor and right neighbor . We use and to keep the neighbors within the frequency grid range . For these knots we compute their frequencies in the comoving frame, which we denote by Therefore, the comoving knots related to the inertial knot are those whose frequencies belong to the or intervals. The knots lie either on the left or on the right side of , and they might fall outside the frequency coverage of the line. We thus have four different cases to test for and apply Eqs. ( A.15 )–(A.16). Algorithm 1 shows the forward transform in detail. Appendix A.2.2: General backward transform Algorithm 2 gives the backward transform,
Paper: 2020A&A...641A.160M (fulltext)
to be robust as they are obtained without any assumptions. Table 3. Ro-vibrational partition function values computed at different temperatures. Notes. (a) Includes all states up to 400 cm −1 : the ground, v 11 = 1, v 18 = 1, and v 17 = 1 states. (b) Includes all states up to 1600 cm −1 . To compute the ro-vibrational partition function of the manifold containing all states up to 1600 cm −1 (referred to as “Manifold 2” in Table 3 ), we have applied a vibrational correction to our new ground state partition function values. The correction factor was calculated at each temperature summing up the contribution of all the vibrational states below 1600 cm −1 . Since we have no direct information about the vibrational energies of the states between 400 and 1600 cm −1 , they were either estimated under the harmonic approximation or taken from low-resolution measurements ( Bak et al. 1975 ). Higher energy levels were not considered in the calculation because they do not contribute significantly to Q even at 300 K. The vibration-rotation partition functions of the three manifolds of aminoacetonitrile, computed at temperatures between 2.725 and 300 K, are listed in Table 3 . Based on our results, we prepared new catalog entries for aminoacetonitrile in the ground and excited states. The line intensity of each transition was calculated using the partition function values from Col. 4 of Table 3 (“Manifold 2”), while the permanent dipole moment values μ a = 2.577(7) D and μ b = 0.575(1) D were taken from Pickett (1973) and assumed not to change upon the vibrational states. 4. Astronomical observations 4.1. Observations We used the ReMoCA imaging spectral line survey carried out toward the protostellar cluster Sgr B2(N) with ALMA. Details about the observational setup and data reduction of this survey were reported in Belloche et al. (2019) . In short, the observations covered the frequency range from 84.1 GHz to 114.4 GHz with five tunings, with a spectral resolution of 488 kHz (1.7–1.3 km s −1 ). The angular resolution (HPBW) varied between ∼0.3′′ and ∼0.8′′, with a median value of 0.6′′, which corresponds to ∼4900 au at the distance of Sgr B2. The rms sensitivity ranged from 0.35 mJy beam −1 to 1.1 mJy beam −1 , with a median value of 0.8 mJy beam −1 . The field was centered at ( α , δ ) J2000 = (), a position that is halfway between the two main hot molecular cores, Sgr B2(N1) and Sgr B2(N2), which are separated by 4.9′′ or ∼0.2 pc. Here we analyze the spectrum at the offset position Sgr B2(N1S) defined by Belloche et al. (2019) to reduce the optical depth of the continuum emission, which is partially optically thick toward the peak position of the main hot core Sgr B2(N1). Sgr B2(N1S) is located at ( α , δ ) J2000 = (, ), about 1′′ to the south of Sgr B2(N1). In Belloche et al. (2019) , the continuum and line emission of the ReMoCA survey was separated in the image plane because the hot cores detected in the field of view have different systemic
Paper: 2018MNRAS.479.5385H (acknowledgments)
ACKNOWLEDGEMENTS We would like to thank Ming Sun for providing us with their data. We also thank Helen Russell, Stephen Walker and Elena Rasia for helpful discussions about X-ray data analysis. We are grateful to Volker Springel for making the arepo moving-mesh code available to us and to the Illustris collaboration for their development of the Illustris galaxy formation model on which this work is based. NAH is supported by the Science and Technology Facilities Council (STFC). EP acknowledges support by the Kavli Foundation. DS and SS acknowledge support by the STFC and the European Research Council Starting Grant 638707 ‘Black holes and their host galaxies: co-evolution across cosmic time’. This work made use of the following DiRAC facilities ( www.dirac.ac.uk ): the Data Analytic system at the University of Cambridge [ funded by a BIS National E-infrastructure capital grant (ST/K001590/1), STFC capital grants ST/H008861/1 and ST/H00887X/1, and STFC DiRAC Operations grant ST/K00333X/1] and the COSMA Data Centric system at Durham University (funded by a BIS National E-infrastructure capital grant ST/K00042X/1, STFC capital grant ST/K00087X/1, DiRAC Operations grant ST/K003267/1 and Durham University). DiRAC is part of the National E-Infrastructure.
Paper: 2019ApJ...885...93F (fulltext)
gas is released in the inner region of the disk, a global transonic structure of such a slim disk surrounding a BH is crucial in modeling the observations. In this work, we derive a global solution to a slim accretion disk with outflows accelerated by radiation force of the disk. The calculations can be applied to model the accretion disks surrounding either massive BHs or stellar mass BHs. We describe our model calculations and results in Sections 2 and 3 . The last section contains the discussion of the results. 2. Model A set of equations describing a slim disk with outflows in cylindrical coordinates are summarized in the previous works (see Gu Lu 2007 ; Kato et al. 2008 ). We consider a steady axisymmetric accretion disk in this work, which is described by the momentum equations, energy equation, continuity equation, and the equation of state. The r -component of the momentum equation isAs was done in many previous works, we adopt the pseudo–Newtonian potential,to simulate the gravity of the BH, where M is the BH mass, and is the Schwarzschild radius (Paczyńsky Wiita 1980 ). The continuity equation is We integrate Equation ( 1 ) over z and obtainwhere Equation ( 3 ) is used, Σ is the surface density, Π is the vertically integrated pressure, Ω is the angular velocity of the gas in the disk, and Ω K is the Keplerian angular velocity. The φ -component of the momentum equation iswhere the α -viscosity of t rφ = − αp is adopted. Integrating Equation ( 5 ) over z -direction, we havewhere the velocity of outflow at the disk surface is v H = v z ( H ), as the outflows driven by the radiation force are considered in our model. By integrating Equation ( 3 ) vertically, it becomesThe term 2 ρv H in this equation represents the mass loss rate in outflows from the unit area of the disk surface. If we further integrate Equation ( 7 ) over r -direction, it becomeswhere the integral constant C can be determined with suitable boundary conditions. As the mass loss rate in the outflows from the unit area of the disk surface are , we haveso the mass accretion rate in the disk at radius r isand the total mass loss rate in the outflows driven from the disk region between r and r out is Substituting Equation ( 7 ) into Equation ( 6 ), we haveWe integrate the angular Equation ( 12 ) over r , which leads torespectively, where Equation ( 9 ) is used, is the angular momentum removed by the outflows from the corresponding disk region, is the mass accretion rate swallowed by the BH, and is rate of angular momentum of the accretion gas flowing into the BH ( j in is the specific angular momentum of the accreting gas swallowed by the BH). The vertical integrated equation of state iswhere μ is the mean molecular weight ( μ = 0.62 is used in this work), and T 0 is the temperature at the mid-plane of the disk (see Equations (7.43)–(7.45) in Kato et al. 2008 ). The isothermal sound speed is . The energy equation of the disk iswhere is the gravitational power released