adsabs/WIESP2022-NER huggingface dataset:
Paper: 2018ApJ...864L...9Y (fulltext)
May 2 (chosen arbitrarily) and are integrated using a Bulirsch–Stoer integrator, considering the gravitational perturbations from the eight major planets (with the Earth–Moon system represented by a single point mass at the barycenter of the two bodies), relativistic effects, and β = 0.001 particles, radiation pressure, and Poynting–Robertson drag. The particle representing Phaethon and all other dust particles are considered to be massless and do not interact with each other. We find that it only takes about 250 years (∼200 orbits) for particles to spread to the entire orbit of Phaethon (Figure 1 , left panel). The timescale is much shorter (∼30 years) for β = 0.001 particles under cometary ejection. The definition adopted here is the “encircling limit” described in Ye et al. ( 2016 , Section 3): meteoroids have spread to most of the orbit of the parent when the standard deviation of their mean anomalies σ ( M ) has reached 60°. The mathematical consideration is that 99.7% of the meteoroids have spread to half-orbit, or 180° in mean anomaly, assuming a Gaussian distribution along the orbit. (One may wonder why we do not choose 360° in mean anomaly instead of 180°. The reason is that σ ( M ) becomes highly sensitive to regional overdensities when meteoroids are quasi-evenly distributed along the orbit or , as reflected in the figure, and is no longer a good indicator of the dispersion of meteoroids along the orbit.) Figure 1. Evolution of particles ejected under different ejection mechanisms, cometary or gravitational escape. Left panel: standard deviation of mean anomalies of simulated particles, σ ( M ); the encircling limit at σ ( M ) = 60° follows the definition in Ye et al. ( 2016 ) (described in the main text). Right panel: along-orbit distance of the center of the particles (represented by the mean of the mean anomaly, ) to Phaethon. Regardless of the driving mechanism and size ( β ) of the particle, it only takes a small number of orbits for the bulk of the ejecta to spread to significant distances from Phaethon (∼0.1 au). This means that if any materials larger than typical meteor sizes (see below for more on meteor-sized particles) were recently ejected, they could be closer to the Earth than Phaethon itself during their late 2017 approach to the Earth and are potentially detectable using existing facilities. Examination of the existence of such ejecta will therefore provide a useful diagnosis as to recent activity of Phaethon that is otherwise irretrievable. This will also provide useful information for the design of any Phaethon-bound spacecraft like DESTINY + . We find that β = 0.001 particles quickly drift away from Phaethon (Figure 1 , right panel). This radiation-driven process is very fast due to the extreme orbit of Phaethon, with the along-orbit recession rate being approximately 0.1 au yr −1 . This means that it takes less than an orbit for small particles to drift to different locations of the orbit and effectively
Paper: 2019MNRAS.482.1485P (acknowledgments)
ACKNOWLEDGEMENTS AP is grateful for research support from the Gates Cambridge Trust. NM, SG, and RM acknowledge support from the Science and Technology Facilities Council (STFC), UK. We thank the reviewer for useful comments that have helped improve the manuscript. This research has made use of the SVO Filter Profile Service supported from the Spanish MINECO through grant AyA2014-55216. We thank the contributors of the Python Software Foundation, the Open Science Framework, and NASA’s Astrophysics Data System.
Paper: 2017MNRAS.466.2242B (acknowledgments)
Acknowledgments FB acknowledges support from the UK Space Agency through grant ST/N00180X/1. Funding for SDSS-III has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, and the US Department of Energy Office of Science. The SDSS-III web site is http://www.sdss3.org/ . SDSS-III is managed by the Astrophysical Research Consortium for the Participating Institutions of the SDSS-III Collaboration including the University of Arizona, the Brazilian Participation Group, Brookhaven National Laboratory, Carnegie Mellon University, University of Florida, the French Participation Group, the German Participation Group, Harvard University, the Instituto de Astrofisica de Canarias, the Michigan State/Notre Dame/JINA Participation Group, Johns Hopkins University, Lawrence Berkeley National Laboratory, Max Planck Institute for Astrophysics, Max Planck Institute for Extraterrestrial Physics, New Mexico State University, New York University, Ohio State University, Pennsylvania State University, University of Portsmouth, Princeton University, the Spanish Participation Group, University of Tokyo, University of Utah, Vanderbilt University, University of Virginia, University of Washington and Yale University. This research used resources of the National Energy Research Scientific Computing Center, which is supported by the Office of Science of the US Department of Energy under Contract no. DE-AC02-05CH11231. This work was supported by World Premier International Research Center Initiative (WPI Initiative), MEXT, Japan. Numerical computations were partly carried out on Cray XC30 at Center for Computational Astrophysics, National Astronomical Observatory of Japan. H-JS is supported by the US Department of Energy, Office of Science, Office of High Energy Physics under Award number DE-SC0014329. C-HC acknowledges support as a MultiDark Fellow. C-HC acknowledges support from the Spanish MICINNs Consolider-Ingenio 2010 Programme under grant MultiDark CSD2009-00064, MINECO Centro de Excelencia Severo Ochoa Programme under grant SEV-2012-0249, and grant AYA2014-60641-C2-1-P. MV is partially supported by Programa de Apoyo a Proyectos de Investigacin e Innovacin Tecnolgica (PAPITT) No IA102516 and Proyecto Conacyt Fronteras No 281.
Paper: 2019MNRAS.487.3288S (acknowledgments)
ACKNOWLEDGEMENTS We thank Kat Volk, Rachel Smullen, Renu Malhotra, and Andrew Youdin for helpful discussions. We thank the reviewer for helpful comments. We gratefully acknowledge support from National Science Foundation Grant no. AAG-1410174 and National Aeronautics and Space Administration Grant no. 17-ATP17-0070.
Paper: 2020A&A...634A..85P (fulltext)
to T bb > 10 5 K, n H 10 12 cm −3 or ξ 0 10 4 . In this region of the parameter space, the properties of the warm corona are mainly driven by χ . However, for smaller T bb or larger density, n H , or ionization parameter, ξ 0 , the radiative and spectral properties of the corona depend significantly on these parameter values. The background colors in Fig. 5 correspond to the Compton-cooling-to-corona-heating ratio p compt / q h , whose color scale is reported on the right of the figure. The dependencies of the corona emission spectral shape on T bb and n H can be explained by the properties of the Comptonization process in an environment in radiative equilibrium. At low density or high disk temperature, our simulations show that the corona emission is dominated by Comptonization. In this case, as long as the heating over cooling of the warm corona remains constant, no significant spectral variability is expected. The corona heating is directly related to the sum of the internal heating Q and the illumination ξ 0 while the cooling is related to . They are all related to one another through the net flux crossing the base of the corona (see Eq. ( 10 )). As long as the illumination is negligible with respect to warm corona internal heating power, a constant χ implies a constant heating-to-cooling ratio and the warm corona temperature is not expected to change. The warm corona optical depth being fixed, the spectral shape of the warm corona emission remains roughly constant. This is very similar to the constancy of the spectral shape of the emission from a hot optically thin corona in radiative equilibrium with the surrounding soft photon field (e.g., Haardt Maraschi 1991 ; Haardt 1993 ; Petrucci et al. 2000 ; Tortosa et al. 2018 ). However, for densities larger than ∼10 12 cm −3 and disk temperatures lower than ∼10 5 K, the dependence on these parameters becomes important. This is due to the fact that in this part of the parameter space, the corona radiative processes are less dominated by Comptonization, either because the soft seed photon flux decreases (at low T bb ) or the free-free and bound-free processes increase (at high density) through their dependence on the density squared. The previous discussion in terms of radiative equilibrium no longer holds. At constant χ , decreasing T bb or increasing n H results in a decrease of the temperature and a steepening of the warm corona spectrum. These conditions are thus less favorable to producing spectra that could reach the soft X-ray band and produce a significant soft X-ray excess. The dependence of the spectral shape and temperature of the warm corona on the ionization parameter ξ 0 is quite different. The spectral shape and temperature are almost independent of ξ 0 unless this latter becomes larger than a few 10 4 erg s −1 cm. While for such values of ξ 0 , the warm corona is dominated by Compton cooling, the spectral shape (photon index and temperature) varies with ξ 0 and the lower the χ
Paper: 2021ApJ...909...76P (fulltext)
as follows. We describe the observations, archival data we used, and data reduction in Section 2 . We present the results of our analysis of jet structure, opacity, collimation, and acceleration in Section 3 . The results are discussed in Section 4 . We summarize our findings and conclude in Section 5 . 2. Observations and Data Reduction 2.1. Multifrequency VLBA Observation We observed NGC 315 with the VLBA on 2020 January 05 at frequencies of 1.548, 2.284, 4.980, 8.416, 15.256, 22.220, and 43.120 GHz. All 10 VLBA stations successfully participated in the observation. The data were recorded in both right- and left-hand circular polarizations with two-bit quantization in eight baseband channels (also often called intermediate frequencies [IFs]), using the polyphase filterbank (PFB) observing system, at a recording rate of 2 Gbps, yielding a total bandwidth of 256 MHz for each polarization. The total observation time is 12 hr. The on-source time on our target is ≈40 minutes at 1.5–8.4 GHz and ≈50, 80, and 100 minutes at 15.3, 22.2, and 43.1 GHz, respectively. The weather conditions were good, and no major technical issue occurred during the observation at all stations. We summarize the basic properties of our data in Table 1 . Table 1 Multifrequency Observations and Data of NGC 315 Note. (a) Major axis, minor axis, and position angle of the synthesized beam under the natural weighting of the data. (b) Map peak intensity in units of Jy per beam. (c) Image rms noise measured in the off-source regions in units of mJy per beam. I rms is relatively high at 2.3 GHz owing to (i) the signals in some IFs being blocked by the filters installed in many stations and (ii) severe radio frequency interference in this band. (d) FWHM of the core modelfit elliptical Gaussian component along the perpendicular direction to the jet axis. (e) FWHM of the core JMFIT elliptical Gaussian component along the perpendicular direction to the jet axis. Statistical and systematic errors in the fitted core sizes in (d) and (e) are noted. 1 Participating stations: the VLBA (except Maunakea station), the Effelsberg 100 m station, the Green Bank Telescope, and the phased-up VLA. We performed a standard data reduction with the NRAO’s Astronomical Image Processing System (AIPS; Greisen 2003 , see, e.g., Section C in the AIPS cookbook 12 12 http://www.aips.nrao.edu/CookHTML/CookBook.html ). We updated the Earth Orientation Parameters using more accurate parameters that are available after the data correlation, taken from NASA CDDIS. We corrected the dispersive delays caused by the ionosphere by using the GPS models of the electron content in the ionosphere using the procedure VLBATECR in AIPS. The sampler voltage offsets were corrected by using the autocorrelation spectra. We removed the instrumental delay residuals and phase offsets between IFs by performing a “manual phase-cal” using a scan of bright calibrators such as 0133+476, 3C 84, and BL Lac. The bandpass shapes of the
Paper: 2018ApJ...860..124D (acknowledgments)
We are grateful to Hui Li for useful discussions, Myriam Benisty for making available the SPHERE image of MWC 758, and an anonymous referee for constructive suggestions that largely improved the quality of the paper. Numerical calculations were performed on the SAVIO cluster provided by the Berkeley Research Computing program, supported by the UC Berkeley Vice Chancellor for Research and the Berkeley Center for Integrative Planetary Science. Y.P. was supported by Russian Science Foundation grant 17-12-01168. This paper makes use of the following ALMA data: 2017.1.00492.S. ALMA is a partnership of the ESO (representing its member states), NSF (USA), and NINS (Japan), together with the NRC (Canada), MOST and ASIAA (Taiwan), and KASI (Republic of Korea), in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated by the ESO, AUI/NRAO, and NAOJ. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. Y.H. is currently supported by the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. This work was supported by NAOJ ALMA Scientific Research Grant Number 2016-02A.
Paper: 2015A&A...575A..87F (acknowledgments)
F.F. and A.P. are grateful to the IRAM-30 m staff for their help with the observations at the IRAM-30 m telescope. G.B. is grateful to Amanda Kepley for her help during the GBT observations and to Jeff Magnum for providing the procedures for converting the GBT spectra from GBTIDL to CLASS format. A.P. acknowledges the financial support from UNAM, and CONACyT, México. G.B. is supported by the Spanish MICINN grant AYA2008–06189–C03–01 (co-funded with FEDER funds) and by the Italian Space Agency (ASI) fellowship under contract number I/005/07/01. P.C. acknowledges the financial support of the European Research Council (ERC; project PALs 320620). A.S.-M. is supported by the Deutsche Forschungsgemeinschaft (DFG) through the collaborative research grant SFB 956 “Conditions and Impact of Star Formation”, project area A6. The research leading to these results has received funding from the European Commission Seventh Framework Programme (FP/2007-2013) under grant agreement Na 283393 (RadioNet3).
Paper: 2018ApJ...854..164S (fulltext)
the protosolar disk. In addition, D/H ratios can readily be modified by non-nebular processes. For example, the D/H ratio of Rumuruti type and ordinary chondrites is higher than that in comets, which Alexander et al. ( 2012 ) attribute to iron oxidation in their parent bodies. 4.5. Water in Chondrites If carbonaceous and non-carbonaceous chondrites formed on opposite sides of the snowline, where Jupiter formed, why do some carbonaceous chondrites have relatively low water and carbon contents like those in some non-carbonaceous chondrites? CM, CI, and CR chondrites have the highest contents of water and carbon among chondrites, but CO and CV have lower amounts that are comparable to those in some of the least metamorphosed ordinary chondrites (Krot et al. 2014 ). Krot et al. ( 2015 ) infer that CI, CM, and CR chondrites were altered under water/rock mass ratios of up to 0.6, whereas CV and CO chondrites were altered at lower water/rock ratios of 0.1–0.2. We do not know the answer to this issue but note that water contents of carbonaceous chondrites are related to matrix contents and that the coarse-grained matrix material likely contained more water than the fine-grained matrix rims. Thus, the low water content of CO and CV chondrites may reflect their low content of coarse-grained matrix material relative to CI, CM, and CR chondrites (Scott Krot 2014 ). We also note that comets can contain more rock than ice (Brownlee 2014 ; Davidsson et al. 2016 ), much less ice than the predicted theoretical water-rock ratio beyond the snowline of 1.2 (Krot et al. 2014 ; Palme et al. 2014 ). 5. How and When Were the Two Isotopic Populations Mixed Together in the Asteroid Belt? The isotopic dichotomy in the solar system lasted until at least 3–4 Myr after CAI formation, the likely accretion time of CR chondrites, which are the least metamorphosed and altered chondrites and have the highest concentration of presolar grains (Zhao et al. 2013 ; Budde et al. 2017 ; Krot Nagashima 2017 ). The two isotopic populations were then intermixed, most likely by the migration of the giant planets before the gas had dissipated in the disk. In the Grand Tack model, once Jupiter and Saturn reached masses of ∼50 M ⊕ , they migrated inward across the asteroid belt so that it was first emptied and then repopulated with S-type asteroids, which formed in the belt, and C-types, which formed outside Jupiter (Walsh et al. 2011 ). Alternatively, planetesimals from the giant planet region may have been scattered into the asteroid belt as a natural side-effect of the growth of giant planets (Kretke et al. 2017 ; Raymond Izidoro 2017 ). Raymond Izidoro ( 2017 ) show that scattering during the rapid growth of the gaseous envelopes of giant planets would have scattered nearby planetesimals in all directions and may have delivered water to the growing Earth. However, the Grand-Tack model has the advantage that it creates a strongly mass-depleted belt with roughly equal masses of S- and
Paper: 2018ApJ...868...17A (acknowledgments)
This research was partially supported by the National Science Foundation under grant NSF PHY-1125915 and by the Polish NCN grants 2014/14/M/ST9/00707, 2015/19/B/ST9/01099, and 2016/22/E/ST9/00037. M.A.A. acknowledges the Czech Science Foundation grant No. 17-16287S, which supported one of his visits to the Paris Observatory. The authors benefited from discussions with Ramesh Narayan, Paweł Haensel, Avi Loeb, Axel Brandenburg, and Krzysztof Belczyński. Some of this work was conducted at the Black Hole Initiative at Harvard University, which is funded through a grant from the John Templeton Foundation.
Paper: 2016MNRAS.455..370E (acknowledgments)
We are grateful to Ho Seong Hwang for providing his catalogues of AKARI and IRAS fluxes for matched SDSS galaxies. SLE acknowledges the receipt of an NSERC Discovery Grant. Funding for the SDSS and SDSS-II has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, the US Department of Energy, the National Aeronautics and Space Administration, the Japanese Monbukagakusho, the Max Planck Society and the Higher Education Funding Council for England. The SDSS Web Site is http://www.sdss.org/ . The SDSS is managed by the Astrophysical Research Consortium for the Participating Institutions. The Participating Institutions are the American Museum of Natural History, Astrophysical Institute Potsdam, University of Basel, University of Cambridge, Case Western Reserve University, University of Chicago, Drexel University, Fermilab, the Institute for Advanced Study, the Japan Participation Group, Johns Hopkins University, the Joint Institute for Nuclear Astrophysics, the Kavli Institute for Particle Astrophysics and Cosmology, the Korean Scientist Group, the Chinese Academy of Sciences (LAMOST), Los Alamos National Laboratory, the Max-Planck-Institute for Astronomy (MPIA), the Max-Planck-Institute for Astrophysics (MPA), New Mexico State University, Ohio State University, University of Pittsburgh, University of Portsmouth, Princeton University, the United States Naval Observatory and the University of Washington.
Paper: 2019MNRAS.488.3541W (acknowledgments)
ACKNOWLEDGEMENTS We thank Brian Batell, Arthur Kosowsky, Rachel Mandelbaum, Dazhuang Mao, Jeffrey Newman, Troy Raen, Li-Cheng Tsai, and Rongpu Zhou for useful discussions. KW, ARZ, and ASV are supported by the US National Science Foundation (NSF) through grant AST 1517563 and by the Pittsburgh Particle Physics Astrophysics and Cosmology Center (PITT PACC). ASV is additionally supported by the Argonne Leadership Computing Facility, which is a Department of Energy (DOE) Office of Science User Facility supported under Contract DE-AC02-06CH11357. YYM is supported by PITT PACC through the Samuel P. Langley Postdoctoral Fellowship. FvdB and JUL are supported by the US National Science Foundation (NSF) through grant AST 1516962. FvdB received additional support from the Klaus Tschira foundation, and from the National Aeronautics and Space Administration through Grant No. 17-ATP17-0028 issued as part of the Astrophysics Theory Program. CMS is supported by NSF through grant DMS 1521786. APH is supported under the DOE contract DE-AC02-06CH11357. DC is supported by a McWilliams Postdoctoral Fellowship. The authors gratefully acknowledge the Gauss Centre for Supercomputing e.V. ( www.gauss-centre.eu ) and the Partnership for Advanced Supercomputing in Europe (PRACE, http://www.prace-ri.eu ) for funding the MultiDark simulation project by providing computing time on the GCS Supercomputer SuperMUC at Leibniz Supercomputing Centre (LRZ, http://www.lrz.de ). The Bolshoi simulations have been performed within the Bolshoi project of the University of California High-Performance AstroComputing Center (UC-HiPACC) and were run at the National Aeronautics and Space Administration (NASA) Ames Research Center. This research made use of python , along with many community-developed or maintained software packages, including ipython (Pérez Granger 2007 ), jupyter ( jupyter.org ), matplotlib (Hunter 2007 ), numpy (van der Walt, Colbert Varoquaux 2011 ), and scipy (Jones et al. 2001 ). This research made use of NASA’s Astrophysics Data System for bibliographic information.
Paper: 2016A&A...592A..70H (acknowledgments)
We would like to thank the referee for constructive comments that helped improved the presentation of this work. We would like to thank A. Casey for discussions that improved this work. K.H. is funded by the British Marshall Scholarship program and the King’s College, Cambridge Studentship. This work was partly supported by the European Union FP7 programme through ERC grant number 320360. U.H. acknowledges support from the Swedish National Space Board (Rymdstyrelsen).