adsabs/WIESP2022-NER huggingface dataset:
Paper: 2021ApJ...913L...2M (fulltext)
all remaining isomers are located among the second peak nuclei, the most notable of which include 125,127 Te. Finally, we identify the particularly interesting isomer in 129 Te. It remains important across all epochs of our simulation, from 0.01 days to 1 year, reflecting a complex interplay between the β -decay feeding parent, thermal excitation, and de-excitation. We identify 195 Pt as the dominant astromer located in the third r- process peak (green). In contrast with the conventional assumption that this isotope is stable upon population via the ground state β decay of 195 Ir, our calculations show that the isomer of 195 Pt may be populated directly from the β decay of the isomer of 195 Ir. The 195 Pt isomer de-excites on a timescale of ∼4 days, which is relevant to the study of electromagnetic signals associated with the r process. In the interest of readability, Figure 2 shows only those astromers that rank in the top five by AIR. When we expand our enumeration of r -process astromers to include the top 10, we identify only 11 additional astromers. This highlights the effectiveness of AIR as a filter for distinguishing astromers from the broader population of isomers: the list of isomers identified as influential astromers is relatively insensitive to the particular choice of AIR top- N . We summarize our expanded (top 10) list of astromers in Table 1 . Table 1 Astromer Importance Rating (AIR) Top 10 Selected at Each Time Point t ≳ 15 Minutes Notes. We use g and m to indicate the ground state and isomer, respectively. The isomer energy is E m , and the J π are the spin and parity of the respective levels (parentheses denote uncertain J π ). The half-lives ( T 1/2 ) and β -decay branching for the isomer ( B m β ) are as measured in the laboratory; B m β is the percent of isomer decays, which are β decays rather than internal transitions to another nuclear state. T pop is the approximate timescale on which the isotope is populated, and the Notes column gives some brief comments on the nucleus. a EM signals (detectable x -rays and γ -rays) are possible, but we do not study them carefully here. b Nearly all parent β decay feeds the isomer, effectively bypassing the longer-lived ground state. c To explore the 195 Pt isomer population, we assume all 195 Os β decay feeds the 195 Ir isomer (actual feeding unknown). Notably, there are three species in Table 1 that do not appear in Figure 1 : 93,95 Nb and 131 Xe. This is because while the isomers might not be heavily populated relative to the ground state (low R ), they have comparatively high activities a and large thermal population imbalances I . The astromers identified in Table 1 that change β -decay rates will affect r -process heating. Some (e.g., 115 Cd, 127,129,131 Te) will defer heating by delaying decay, while others (e.g., 85 Kr, 128,130 Sb) partially counteract this trend by accelerating decay. Furthermore, astromers may generate identifiable x -ray or γ -ray signals either directly
Paper: 2016MNRAS.462.4038Y (fulltext)
ranges as Lohfink et al. ( 2012b ), we obtained a reduced χ 2 value of 1.099 (null hypothesis probability of 0.065). Considering the fact that our data selection criteria and extraction regions for XIS source and background data are not completely identical, we conclude that our blurred reflection fit results are consistent with those of Lohfink et al. ( 2012b ). The blurred reflection model fitted by Lohfink et al. ( 2012b ) and the MYTORUS model fit (see Table 2 ) give reduced χ 2 values that are comparable, which indicates that the two model fits are statistically similar to each other. In our blurred reflection model fit described above, the value of C PIN: XIS was fixed at 1.16, as was in Lohfink et al. ( 2012b ). When we allowed C PIN: XIS to be a free parameter, the value of χ 2 dropped by only 1.6, and we obtained , which encompasses the value of 1.16. Figure 5. A comparison, in the 4–8 keV band, of the best-fitting baseline face-on MYTORUS fit with a ‘blurred reflection’ model, similar to that fitted by Lohfink et al. ( 2012b ), showing how the MYTORUS model can eliminate the need for a relativistically broadened Fe Kα line. Both models include narrow Fe xxv and Fe xxvi Lyα emission lines from distant ionized material (but the fitted Fe xxv flux for the blurred reflection model is negligible). (a) Unfolded photon spectrum (black) overlaid with the total MYTORUS model (red; see Table 2 , column 2). The Compton-scattered continuum from the MYTORUS model shown in blue is able to account for excess emission in the Fe K band instead of a relativistically broadened Fe Kα line. (b) Unfolded photon spectrum (black) overlaid with the total multi-component Lohfink et al. ( 2012b ) disc-reflection and Comptonization model in red (see the text for details). The blurred reflection component is shown in blue. Above the blue wing of the relativistic Fe Kα line, the reflection continuum drops by more than an order of magnitude but rises again at high energies. Note that in this model fit, the narrow Fe Kα is unresolved because Lohfink et al. ( 2012b ) did not include any broadening for this component. Panels (c) and (d) show the data-to-model ratios corresponding to (a) and (b), respectively, showing that both models give good fits to the data. Note that, although the MYTORUS component and blurred reflection component (shown in blue in panels (a) and (b), respectively) appear to be markedly different from each other, smearing due to the limited CCD detector energy resolution has a considerable impact on the ability of the data to distinguish between the two models. This is illustrated in Fig. 6 . The model components in blue in Figs 5(a) and (b) show how the Compton-scattered continuum from the MYTORUS model and the relativistically broadened Fe Kα line with blurred disc continuum respectively provide very different solutions to the same data. At a disc inclination angle of 48°, the relativistic line has significant emission in the blue wing but it
Paper: 2016MNRAS.461.2461M (acknowledgments)
We thank Sebastian Lopez for initial discussions about using Zn and Cr ii to measure Δα/α, and Julija Bagdonaite and Jonathan Whitmore for assistance with Fig. 15 . MTM thanks the Australian Research Council for Discovery Projects grant DP110100866 which supported this work. Some of the data presented herein were obtained at the W.M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California and the National Aeronautics and Space Administration. The Observatory was made possible by the generous financial support of the W.M. Keck Foundation. We wish to recognize and acknowledge the very significant cultural role and reverence that the summit of Maunakea has always had within the indigenous Hawaiian community. We are most fortunate to have the opportunity to conduct observations from this mountain. Other data presented herein were based on observations made with ESO Telescopes at the La Silla Paranal Observatory under programme IDs 65.O-0158, 67.A-0022, 072.A-0346, 074.A-0201, 079.A-0600, 082.A-0682, 082.A-0569, 083.A-0874 and 084.A-0136.
Paper: 2018MNRAS.480.1676Q (acknowledgments)
ACKNOWLEDGEMENTS PQM gratefully acknowledge the financial support of CONICYT/Becas Chile. This work was also supported by the Portuguese Science foundation (FCT) through national funds (Investigador contract of reference IF/00894/2012 and UID/FIS/04434/2013) and POPH/FSE (EC) by FEDER through COMPETE2020 (POCI-01-0145-FEDER-030389 and POCI-01-0145- FEDER-007672). Funds were also provided by the project FCT/CNRS: PICS 2014. OK acknowledges financial support from the Knut and Alice Wallenberg Foundation, the Swedish Research Council, and the Swedish National Space Board.
Paper: 2016A&A...591A..41P (fulltext)
in two distinct emission regions. We used compTT plus compPS , or two compTB . The dominant emission results, by the Comptonization, in a disk geometry of seed photons at 0.1 keV by a plasma with keV and optical depth 3. This emission can be interpreted as arising in a region above the accretion disk and contributes to the 70 of the total flux. We call this component hard Comptonization. In addition, a secondary emission component, described by a spherical geometry, is due to seed photons at 0.8 keV Comptonized by a plasma with keV and optical depth 8 using a compTT model or with keV using a compTB . This emission can be interpreted as originating from a region closer to the neutron star around the boundary layer and contributes about 30 of the total flux. We call this component soft Comptonization. The persistent emission spectrum of the LMXB GS 1826-23, observed jointly by Chandra and RXTE, has been described by Thompson et al. ( 2005 ) with a similar model. This model uses dual Comptonization of 0.3 keV soft photons by a plasma with keV and , which is interpreted as emission from accretion disk corona, plus Comptonization of hotter 0.8 keV photons by a 6.8 keV plasma, which is interpreted as emission from the boundary layer. The parameters are therefore very similar to those reported here for 4U 1705-44. Moreover, a dual Comptonization model was successfully applied to the broadband spectra of the low/hard state of the black hole candidate Cyg X-1 by Makishima et al. ( 2008 ) with Suzaku data, by Di Salvo et al. ( 2001 ) and Frontera et al. ( 2001 ) with Beppo SAX data, and by Gierliski et al. (2007) and Ibragimov et al. ( 2005 ), who used simultaneous Ginga, RXTE and GRO/OSSE data. Takahashi et al. ( 2008 ) modeled the spectra of GRO J1655–40 taken with Suzaku in a similar way. Recently, the two compTB model was applied to six neutron star LMXBs (see Seifina et al. 2015 ). This model describes a scenario in which the Keplerian disk is connected to the neutron star by the transition layer (see Titarchuk et al. 1998 ), where the hot electrons scatter off the soft photons from the neutron star photosphere of temperature and the soft disk photons of temperature giving rise to two Comptonized components. We stress that no reflection component is needed in the two scenarios described above. 5.2. Banana states and high energy tail The absorbed Comptonized component with reflection does not describe the soft/high state spectrum. In addition to a dominating Comptonized emission, the continuum broadband spectrum of the source during the soft state requires a blackbody component at lower energies and a hard component to model the hard tail or excess. The dual Comptonization scenario successfully describes the broadband spectra of the banana state in that it models the soft dominating emission and the hard tail well. Contrary to the island state, the dominating Comptonization emission is soft and is expected to originate in the hot plasma
Paper: 2017MNRAS.469.3424M (fulltext)
a low-order tunable filter will be described. We present Fabry–Perot data cubes for the large-diameter expanding structures around a giant H ii region, the centre of the 30 Doradus starburst (or 30 Doradus giant star-forming region), also called the Tarantula Nebula, in the Large Magellanic Cloud (LMC). The study of shells and bubbles, due to stellar winds and supernova explosions, within giant H ii regions is crucial for understanding the processes of mass and energy transfer from the stellar component to the interstellar medium and the processes of triggering of star formation. Although kinematic studies of supergiant shells and superbubbles in giant H ii regions are common in the literature, carried out both with long-slit and, more recently, with 3D spectroscopy, they have not had the necessary coverage and spatial resolution to answer a few key questions. Even the origin of the supersonic motions present in these regions is still a matter of debate (Melnick et al. 1999 ). Moreover, it is still not understood if the kinematics of giant H ii regions are due to an underlying diffuse component or to superposed multiple kinematic components. Having high spatial and spectral resolution velocity maps, as those delivered by SAM-FP, is crucial to tackle these problems. A few authors have studied the kinematics of the ionized gas in the 30 Doradus nebula, e.g. Chu Kennicutt ( 1994 ), Melnick et al. ( 1999 ), Redman et al. ( 2003 ), Torres-Flores et al. ( 2013 ), and references therein. All of these studies reported broad and possibly multiple components widespread in the nebula, which indicate a complex structure. These studies were either performed (i) with long-slit echelle spectroscopy (e.g. Chu Kennicutt 1994 ; Melnick et al. 1999 ), probing motions and physical conditions in small (parsec) and larger (tens of parsecs) scales but covering only a limited number of lines of sight; or (ii) with fibres, as the work of Torres-Flores et al. ( 2013 ), with a somewhat larger field of view, but probing the nebula in a sparse manner (every 5 × 5 pc 2 , with a filling factor of 0.0028). The advantage of this study is that it combines 3D spectroscopy information with continuous coverage of the field over a fairly large field of view, with a pixel size (binned 4 × 4) of 0.18 × 0.18 arcsec 2 (or 0.045 × 0.045 pc 2 ). These data show that the kinematic profiles change on scales of a tenth of a parsec over the whole field. The wealth of details seen in Hubble Space Telescope ( HST ) images of nearby giant H ii regions can now be investigated using similar-quality kinematic data taken with SAM-FP with a laser guide star. The main purpose of this paper is to highlight the potential of Fabry–Perot maps obtained with adaptive optics in the study of 30 Doradus and similar giant H ii regions. A high-order Fabry–Perot was used to observe the ionized gas within 30 Doradus, in its strongest optical line: Hα. In Section 2 , we first describe the new mode of SAM with a
Paper: 2016A&A...590A...8P (acknowledgments)
The authors thank Cecilia Ceccarelli, Daniele Galli, and Vincent Tatischeff for valuable discussions. We acknowledge the financial support of the Agence National pour la Recherche (ANR) through the COSMIS project. This work has been carried out thanks to 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 programme managed by the ANR. M.P. and A.M. also acknowledge the support of the CNRS-INAF PICS project “Pulsar wind nebulae, supernova remnants and the origin of cosmic rays”.
Paper: 2018ApJ...857...31T (acknowledgments)
The authors gratefully acknowledge the anonymous referee for a careful reading of the manuscript and very helpful comments. We are deeply thankful to Dr. Mark G Rawlings for supporting our observations with SCUBA-2. We also appreciate Dr. Manolis Rovilos, Dr. Elisabete da Cunha, and Dr. Stéphanie Juneau for their helpful comments on SEABASs and MAGPHYS . The Submillimeter Array is a joint project between the Smithsonian Astrophysical Observatory and the Academia Sinica Institute of Astronomy and Astrophysics and is funded by the Smithsonian Institution and the Academia Sinica. The James Clerk Maxwell Telescope has historically been operated by the Joint Astronomy Centre on behalf of the Science and Technology Facilities Council of the United Kingdom, the National Research Council of Canada and the Netherlands Organisation for Scientific Research. Additional funds for the construction of SCUBA-2 were provided by the Canada Foundation for Innovation. Funding for SDSS-III has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, and the U.S. Department of Energy Office of Science. The SDSS-III website 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 publication makes use of data products from the Wide-field Infrared Survey Explorer , which is a joint project of the University of California, Los Angeles, and the Jet Propulsion Laboratory/California Institute of Technology, funded by the National Aeronautics and Space Administration. This research is based on observations with AKARI, a JAXA project with the participation of ESA. Y.T., W.H.W., C.F.L., and Y.Y.C. acknowledge the support from the Ministry of Science and Technology of Taiwan ( MOST 105-2112-M-001-029-MY3). T.N. is financially supported by the Japan Society for the Promotion of Science (JSPS) KAKENHI (16H01101 and 16H03958).
Paper: 2019MNRAS.484.3537F (fulltext)
of equation 33 ). Finally, in Fig. 4 we show the temperature moment itself as given in equation ( 33 ). Figure 2. Kappa function f κ ( v , η(Θ, κ)) for isentropic electron flows for different values of kappa as a function of the particle velocity v in units of U 0 = 100 km s −1 . One can see that different transitions from a Maxwellian core to a power-law distribution are occurring along the heliosheath streamlines at an isentropic electron behaviour. Figure 3. The differential temperature moment of the electrons defined by the integrand of equation ( 33 ) is plotted as a function of the velocity v in units of U 0 = 100 km s −1 for different values of the parameter κ. This shows that for different permitted combinations of the parameters κ and Θ the contributions to the effective temperature are due to the higher electron velocities, the lower are the associated kappa values. Figure 4. The electron temperature, as a velocity-moment of the distribution function given by equation ( 33 ) as a function of the upper velocity border v ∞ in units of U 0 = 100 km s −1 , is shown as a function of the actual kappa value for isentropic electron flows. 4 NON-ISENTROPIC ELECTRON FLOWS AND THE ELECTRON ENTROPY In case that the electron flow along the streamlines, contrary to the assumption in the section before, develops non-isentropically due to the presence of energy sources or sinks, i.e. if the entropy of the electron fluid changes with the flow line element s , then one has to consider the following more complicate relation along streamlines: where d Q according to thermodynamical convention describes energy gains and losses per unit of the streamline element s in the co-moving volume Δ V , and T = T κ ( s ) is the local kappa temperature. Looking at equation ( 34 ), one can already qualitatively say that practically no change of the entropy has to be faced, if the temporal energy change compared to the given energy content Q is negligible, i.e. the latter condition for would lead to a quasi-isentropic behaviour. In order to check on this condition, we may now look into the pressure transport equation (equation 14 ) where one can identify two processes contributing to the change of the energy density Q ( s ) = ε( s ), namely: connected with the process of magnetic cooling (see Section 2 , equation 8 ) which is given by and the process of velocity-space diffusion (see Section 2 , equation 11 ) leading to the following term: Hence one can express the energy change per time by . Since we have already derived the solution for the local pressure P κ ( s ), one thus, based on that, can also obtain the entropy evolution with the following equation (see Section 2 , equation 14 ): where the actual kappa temperature is given by (see Heerikhuisen et al. 2008 ; Scherer et al. 2018 ) The kappa-entropy S κ ( s ) can then be calculated with the above differential equation, using the equation for P κ ( s ) (equation 14 ) derived further above in this paper in
Paper: 2015MNRAS.454..439V (acknowledgments)
Thanks to an anonymous referee for useful comments on the paper. This work has been funded with support from the Spanish Ministerio de Economía y Competitividad through the grant AYA2012-32295. JS acknowledges financial support from the Alexander von Humboldt foundation. CRA is supported by a Marie Curie Intra European Fellowship within the 7th European Community Framework Programme (PIEF-GA-2012-327934). RGD acknowledges support through the grant AYA2010-15081. This work is partially based on data obtained as part of the WHT service programme. The WHT and its service programme are operated on the island of La Palma by the Isaac Newton Group in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofísica de Canarias. We thank the WHT staff for performing the observations. The work is also based on data from Sloan Digital Sky Survey. 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 website 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.485..396V (acknowledgments)
ACKNOWLEDGEMENTS The authors are grateful to the anonymous referee for the useful comments on the manuscript. The Hydrangea simulations were in part performed on the German federal maximum performance computer ‘Hazel Hen’ at the maximum performance computing centre Stuttgart (HLRS), under project GCS-HYDA/ID44067 financed through the large-scale project ‘Hydrangea’ of the Gauss Centre for Supercomputing. Further simulations were performed at the Max Planck Computing and Data Facility in Garching, Germany. This project received funding from the EU Horizon 2020 research and innovation programme under Marie Skłodowska-Curie grant agreement 747645 (ClusterGal). This work used the DiRAC Data Centric system at Durham University, operated by the Institute for Computational Cosmology on behalf of the STFC DiRAC HPC Facility. DiRAC is part of the National E-Infrastructure. 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. This work has furthermore benefitted from the use of Py-SPHViewer (Benitez-Llambay 2015). STK and DJB acknowledge support from STFC through grant ST/L000768/1. RAC is a Royal Society University Research Fellow. CDV acknowledges financial support from the Spanish Ministry of Economy and Competitiveness (MINECO) through grants AYA2014-58308 and RYC-2015-1807.