adsabs/WIESP2022-NER huggingface dataset:
Paper: 2017MNRAS.465.3185O (fulltext)
used in Barro etal. ( 2013 ) and van Dokkum etal. ( 2015 ) plotted for reference in addition to the van der Wel z 0.75 relation with its intrinsic scatter. Also plotted are the red nugget populations from Taylor etal. ( 2010 ), Damjanov etal. ( 2009 ) and van Dokkum etal. ( 2008 ), which suggest an evolution towards increasing size at lower redshifts. Our source galaxies are much more consistent with this trend within the red nugget populations, whereas the lens galaxies are consistent with the global population (though they span a very small range in stellar mass). Table 5. Inference on the sizemass relation for the source galaxy population, for 1C and 2C models. The parameters correspond to those defined in equations ( 3 ) and ( 4 ); we model the sources as following the linear relation log( R e /kpc) SM log( M /10 11 M ) SM with an intrinsic scatter SM in the log R e direction, and allowing the masses to be drawn from an underlying Gaussian distribution . It can be seen from Fig. 2 that the EELs sources are compact. We also plot the fits to the sizemass relation from van der Wel etal. ( 2014 ) both at z 0.25 and 0.75, which are chosen to bracket the redshifts of the EELs sources in the left-hand panel. Nearly all the sources lie distinctly below these lines. For comparison, the lens galaxy sample straddles the z 0.25 sizemass relation, as might be expected given their average redshift . In the right-hand panel, we show the EELs lenses and sources alongside the red nugget populations from van Dokkum etal. ( 2008 ), Damjanov etal. ( 2009 ) and Taylor etal. ( 2010 ), which span redshifts between z 2 and z 0, in addition to the compactness criteria for classifying high-redshift nuggets used by Barro etal. ( 2013 ) and van Dokkum etal. ( 2015 ) and the global z 0.75 sizemass relation of van der Wel etal. ( 2014 ), along with its intrinsic scatter. Seen in this context, the EELs source population appears to occupy a region closer to the red nuggets rather than normal ETGs. We note, however, that the relations shown on this plot are meant to define some sort of boundary between compact and non-compact objects, with the former all lying below it; our EELs sources are instead scattered above and below these lines. Specifically, 9 out of the 13 systems would be classed as compact according to Barro etal. ( 2013 )s criterion, whereas van Dokkum etal. ( 2015 )s slightly stricter definition reduces this to 7 though, due to differences in the two criteria at high and low masses, these two subsamples do not completely overlap. Given the distinct position in sizemass space of our sources, in addition to the diversity of conflicting compactness definitions that exist, we do not think it is valuable to classify our sources in this way. Rather, we simply note that they seem to be quite massive and significantly more compact than the majority of ETGs at similar redshifts, and may be better associated with the red nugget population. For instance, they may
Paper: 2017ApJ...848..119L (acknowledgments)
The authors thank Jamie Kennea and Phil Evans of the Swift team for their help with the analysis of the Swift /XRT follow-up observations; Kevin Hurley and the IPN team for their efforts to triangulate GRB 160530A, which helped plan the Swift /XRT observations; Varun Bhalerao and Dipankar Bhattacharya with the Astrosat team for helping cross-calibrate COSI’s timing performance with Astrosat; the NASA Columbia Scientific Ballooning Facility team for successfully flying (and landing) COSI and making this work possible. COSI is funded by NASA grant NNX14AC81G-APRA. The Swift Guest Observer analysis is supported through NASA grant NNH15ZDA001N-SWIFT. This work is also supported in part by CNES. Software: GEANT4 (Agostinelli et al. 2003 ), MINUIT (James Roos 1975 ), MEGAlib (Zoglauer et al. 2006 ), ROOT (Brun Rademakers 1997 ).
Paper: 2018A&A...615A.171M (acknowledgments)
The author would like to thank René W. Goosmann for his comments on the text, Ariane Lançon for her advises on galaxy structures and physics, and Mari Kolehmainen for proof-reading this paper. This work was supported by the Centre national d’études spatiales (CNES) who funded this project through to the post-doctoral grant “Probing the geometry and physics of active galactic nuclei with ultraviolet and X-ray polarized radiative transfer”.
Paper: 2021ApJ...910...96M (fulltext)
case, we use the HS(DD2) EOS described within the extended nuclear statistical equilibrium (NSE) model of Hempel Schaffner-Bielich ( 2010 ). It is expected that hyperons and/or (anti)kaons would not appear at low densities and low temperatures. In this situation, we compare the free energy per baryon at fixed n B , T , and Y q of the data of our uniform EOS table with those of the HS(DD2) EOS table. If the free energy of the HS(DD2) table is less than that of our EOS table, we replace the corresponding data of the latter with those of the former to get the final EOS table with Λ-hyperons and (anti)kaons. Furthermore, we impose the condition that hyperons and (anti)kaons are considered only when their fractions are > 10 −5 to avoid unphysical situations and ensure a smooth transition between low and high densities. Henceforth we call this merged EOS table 4 4 https://universe.bits-pilani.ac.in/Hyderabad/sbanik/EoS with Λ-hyperon and K − the BHBΛ K − φ EOS. Incidentally, we generated a similar EOS table (BHBΛ φ ) with Λ-hyperons following a similar procedure (Banik et al. 2014 ). 2.5. Accuracy and Consistency of the EOS Table The following consistency checks on the EOS table are performed. Thermodynamic consistency is achieved by the conditionwhere . The modulus of the relative thermodynamic accuracy in this EOS table is given byThe sum rule of particle fractions ( X i ) is satisfied by the EOS table given byFinally, the EOS table fulfills the thermodynamic stability criteria: 3. Results and Discussion The EOS table with thermal (anti)kaons and K − condensate is generated using the DD2 parameter set and for baryon densities ( n B = 10 −12 to ∼1 fm −3 ), temperatures ( T = 0.1–158.48 MeV), and positive charge fractions Y q ( n B ) = n p − n K ( Y q = 0.01–0.60). Grid spacing for baryon density is for temperature, ; and for positive charge fraction, Δ Y q = 0.01. The EOS table consists of 301 baryon density points, 81 temperatures, and 60 positive charge fractions, i.e., a total of 1 million data points. Before describing the thermodynamic quantities in the BHBΛ K − φ EOS table, we discuss the β -equilibrated matter relevant to cold NSs. We generate the EOS of NSs by imposing charge neutrality with the inclusion of electrons and the β -equilibrium condition without neutrinos at temperature T = 0. In Figure 1 (a), various particle fractions are plotted as a function of baryon number density. The NS core contains a high neutron fraction. The proton fraction increases monotonically as baryon density increases. The positive charges of protons are balanced by negative charges of electrons. Λ-hyperons appear at ∼2.2 n B followed by the K − condensate. The early appearance of Λ-hyperons makes the EOS softer, delaying the appearance of the antikaon condensate. The K − fraction in the condensate abundance reaches a considerable fraction at 3.5 n B . As soon as K − appears, the e − fraction drops and the charge neutrality is totally taken care of by the
Paper: 2017A&A...608A..63P (acknowledgments)
We are grateful to Guillem Anglada-Escudé for the HARPS-N TERRA code and the Likelihood-ratio diagrams. M.P., I.R., J.C.M., A.R., E.H, and M.L. acknowledge support from the Spanish Ministry of Economy and Competitiveness (MINECO) and the Fondo Europeo de Desarrollo Regional (FEDER) through grant ESP2016-80435-C2-1-R, as well as the support of the Generalitat de Catalunya/CERCA program. L.A. and G.M. acknowledge support from the Ariel ASI-INAF agreement No. 2015-038-R.0. A.S.M., J.I.G.H., R.R.L., and B.T.P. acknowledge financial support from the Spanish Ministry project MINECO AYA2014-56359-P. J.I.G.H. also acknowledges financial support from the Spanish MINECO under the 2013 Ramón y Cajal program MINECO RYC-2013-14875. GAPS acknowledges support from INAF through the “Progetti Premiali” funding scheme of the Italian Ministry of Education, University, and Research. The research leading to these results has received funding from the European Union Seventh Framework Programme (FP7/2007-2013) under Grant Agreement No. 313014 (ETAEARTH). The HARPS-N Project is a collaboration between the Astronomical Observatory of the Geneva University (lead), the CfA in Cambridge, the Universities of St. Andrews and Edinburgh, the Queen’s University of Belfast, and the TNG-INAF Observatory. This paper makes use of data from the first public release of the WASP data as provided by the WASP consortium and services at the NASA Exoplanet Archive, which is operated by the California Institute of Technology, under contract with the National Aeronautics and Space Administration under the Exoplanet Exploration Program. This work has made further 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 ). Funding for the DPAC has been provided by national institutions, in particular the institutions participating in the Gaia Multilateral Agreement.
Paper: 2020ApJ...902...85M (fulltext)
LIGO-Virgo network (1200 yr −1 detections at design sensitivity) under this model variation of Mandel de Mink ( 2016 ) and de Mink Mandel ( 2016 ). 6. Summary and Conclusion We have created and analyzed models of thermal winds from twin-star close binaries in circular orbits. Each of our models adopts q = 1, and we set the binary components surface based on a factor times the potential at the L 1 Lagrange point, f Φ . The wind initial sound speed is set based on a hydrodynamic escape parameter, λ . We examine the emergent wind distributions in each model, as well as the fluxes of mass and angular momentum carried away from the binary by the wind. Some key findings of our study are: 1. The acceleration of winds from about the binary components leads to a symmetric outflow traced by spiral density waves in the plane of the orbit (Figure 1 ). The subsonic acceleration region can surround either the individual binary components, or the entire binary, when f Φ ≲ λ /2 (Figure 2 ). The resulting outflow is largely similar to that of a spherical wind, with the addition of density and velocity waves in the equatorial plane due to the binary’s motion (Figure 1 ). 2. Eventual wind radial velocities are related to the surface sound speeds. At low sound speeds, radial velocities exceed that of a single-object wind model, implying that orbital motion imparts additional kinetic energy to the wind (Figures 3 and 4 ). 3. Mass loss rates from the binary are enhanced relative to the estimated superposition of two single-object winds. This effect is best modeled as a function of wind velocity, as shown in Figure 5 , and approximated by Equation ( 29 ). 4. The specific angular momentum carried by the wind depends primarily on the wind velocity as well (Figure 7 ). It is enhanced well beyond the binary’s specific angular momentum for the slower winds, which circulate around the binary before escaping near the outer Lagrange points (Figure 8 ), and we provide an approximating formula in Equation ( 32 ). The dependence of wind mass loss rate and specific angular momentum on wind velocity, as modeled by Equations ( 29 ) and ( 32 ) may have implications for models of massive, near-contact twin binaries undergoing chemically homogeneous evolution due to rotationally enhanced mixing. In particular, Mandel de Mink ( 2016 ) and de Mink Mandel ( 2016 ) argue that the model is sensitive to both the mass and angular momentum carried by winds. Our results suggest that for contact systems with low-velocity winds, mass loss rates and angular momentum loss rates will both be enhanced. Comparison to the model variations of Mandel de Mink ( 2016 ) and de Mink Mandel ( 2016 ) suggest that the high angular momentum loss rates may indicate an enhancement in the portion of binaries that undergo chemically homogeneous evolution that leave binary black hole remnants that can merge in a Hubble time. Productive avenues for future study include modeling twin-star winds that are radiatively,
Paper: 2015ApJ...805...59I (acknowledgments)
The authors acknowledge Malcolm Walmsley for critical reading of the manuscript and helpful comments. A.V. and P.C. acknowledge support from the European Research Council (ERC, project PALs 320620).
Paper: 2019MNRAS.487.2742D (fulltext)
the stability of the orbits in the sense of keeping them within a well-defined section of the available orbital parameter space, Fig. 1 indicates that the eccentricity may eventually reach values that lead the aphelion closer to the Earth–Moon system, perhaps triggering an impact or an ejection from NEA parameter space. Conversely, a larger value of the eccentricity may lead to a shorter perihelion and an eventual collision with the Sun or an ejection from the Solar system or into its outskirts. In our case, the value of the aphelion distance, that oscillates between those of the semimajor axes of Venus and the Earth, can become as high as 1.02 au (see Fig. 6 , right-hand panel), opening the door to eventual impacts on our planet if one of the nodes reaches aphelion (see also Ribeiro et al. 2016 ). Members of the Atira population can eventually become impactors as a result of the complex orbital evolution discussed here and in the event of an impact, they will most probably come from out of the Sun’s glare. 3.3.2 Vatira evolution The evolution of 2019 AQ 3 shown in Fig. 1 initially leads to brief periods (in thick red/grey) in which the aphelion distance of 2019 AQ 3 , Q 0.718 au i.e. 2019 AQ 3 , an Atira, becomes a transient Vatira. This opens the door to transitions between the two dynamical classes. In fact, the dynamical context that keeps 2019 AQ 3 in a chaotic but relatively stable state may be effective in enabling a dynamical pathway to go from the Atira orbital realm into the Vatira one as shown by the evolution after about 3.5 Myr into the future. The progressive reduction in the value of the semimajor axis eventually leads to a transition from the Atira population into the Vatiras that avoid encounters with Venus altogether. Fig. 6 shows that transitions to and from the Vatira orbital realm are also possible well away from the nominal orbit. Our calculations show that a combination of secular evolution and eventual close encounters with Venus triggers the transitions. Atiras do not cross the orbit of the Earth–Moon system and Vatiras do not cross the orbit of Venus; both Atiras and Vatiras define disjoint subsets. Atiras can impact on Venus, Vatiras cannot; therefore and although the members of both dynamical classes interact with Venus, they do it quite differently. We may now argue that the distinctive dynamical property of putative, long-term stable Vatiras is that they must be virtually and dynamically detached from Venus. This implies a robust difference between the dynamical behaviour of hypothetically stable Atiras, such as those discussed by Ribeiro et al. ( 2016 ), and stable Vatiras. In general, Atiras may still experience close encounters with Venus, Vatiras cannot. When the Lidov–Kozai resonance is at work, in addition to avoiding close encounters with Venus at aphelion, close encounters with Mercury at perihelion are also reduced, but the orbit of Mercury is far more eccentric (0.21) and inclined (70) than that of
Paper: 2016ApJ...822...86M (acknowledgments)
T.D.M. acknowledges support from the Kepler Participating Scientist Program (NNX14AE11G). We thank the anonymous referee, Daniel Huber, Jack Lissauer, Juna Kollmeier, and David Hogg for providing helpful suggestions that improved both the analysis and the presentation herein. This paper includes data collected by the Kepler mission. Funding for the Kepler mission is provided by the NASA Science Mission directorate. The authors acknowledge the efforts of the Kepler Mission team for obtaining the light curve products used in this publication, which were generated by the Kepler Mission science pipeline through the efforts of the Kepler Science Operations Center and Science Office. The Kepler Mission is led by the project office at NASA Ames Research Center. Ball Aerospace built the Kepler photometer and spacecraft, which is operated by the mission operations center at LASP. These data products are archived at the NASA Exoplanet Science Institute, which is operated by the California Institute of Technology, under contract with the National Aeronautics and Space Administration under the Exoplanet Exploration Program. This research has made use of NASA’s Astrophysics Data System.
Paper: 2021ApJ...907...64L (fulltext)
fluid with a special cooling function (Lin Youdin 2017 ; Lovascio Paardekooper 2019 ). Dropping the subscript “c” for clarity, our one-fluid model equations in the local shearing box to O ( t s ) are (Laibe Price 2014 ; Lin Youdin 2017 ; Lovascio Paardekooper 2019 ; Chen Lin 2020 ; Paardekooper et al. 2020 ), where f d ≡ ρ d / ρ is the dust fraction. Note that for the isothermal gas we consider, so . The second term on the rhs of Equation ( B5 ) vanishes in a particle disk where ρ g → 0, because solids do not feel pressure gradients. Conversely, for a dust-free gas disk ( ρ g / ρ → 1), we recover the full pressure support from the global disk. The second term in the parentheses on the rhs of Equation ( B6 ) arises from the contribution to the terminal velocity approximation from the large-scale radial pressure gradient in Equation ( B3 ). B.1. Approximate Equilibria As in the two-fluid model, we seek steady, horizontally uniform solutions. The mass, energy, and vertical momentum equations are then where in Equation ( B8 ) we ignore the term a posteriori for consistency with the small t s approximation used to derive the one-fluid model. These equations may then be solved for constant τ s = t s / f g = St/Ω to yield From here, it is clear that v z = O (St), so it is self-consistent to ignore the term. Equations ( B10 )–( B12 ) are in fact the same solutions as in the full two-fluid model in the limit St ≪ 1 (see Equations ( 19 )–( 21 ); recall β → St for St → 0 and note v z = f d v d z ). The horizontal momentum equations are where we ignore the quadratic term in Equation ( B13 ) to obtainThis is expected on physical grounds for tightly coupled dust (St → 0). In this limit, the mixture behaves close to a single fluid with orbital velocity depending on the level of dust enrichment. For ε → 0, we have a pressure-supported gas disk at sub-Keplerian velocity (assuming η > 0), while ε → ∞ corresponds to a particle disk on exactly Keplerian orbits, because then v y → 0. Next, we use Equations ( B15 ), ( B14 ), and ( B11 ) to obtainNotice the radial velocity of the dust–gas mixture’s center of mass depends on height. It is only zero at the midplane and for ∣ z ∣ → ∞ where ε → 0. For η > 0, the specific angular momentum decreases with increasing ∣ z ∣: the mixture gains pressure support as it becomes more gas-rich away from the midplane. This means that as a parcel of the mixture settles, it finds itself having an angular-momentum deficit compared to its surrounding; it thus drifts inwards ( v x 0), as indicated by Equation ( B16 ). B.2. Linearized Equations We linearize the one-fluid equations about the above basic state, with nonuniform v x ( z ), v y ( z ), and v z ( z ). As in the main text, we assume axisymmetric perturbations in the form of and similarly for other variables. The linearized equations are whereand recall Q = δ ε / ε and W = δ ρ g / ρ g = δ P / P . B.3. Mode Energetics Following Ishitsu et al. ( 2009 ), we multiply the x , y , and
Paper: 2016A&A...588L...9B (fulltext)
M 87 is likely anchored close to the innermost stable circular orbit (ISCO). Performing such an analysis in other sources is clearly fundamental for testing the variety of possible scenarios. However, while future instruments with improved capabilities (e.g. phased ALMA) will certainly enrich the sample of suitable targets, this is currently quite limited. In this Letter we present, for the first time, a detailed imaging of the jet base in Cygnus A through global VLBI observations at 86 (GMVA). Among the powerful FR II radio galaxies, Cygnus A is one of the very few two-sided sources whose jet launching region can be probed with sufficient sensitivity at high radio frequencies. At the source redshift () 1 and assuming a black hole mass of ( Tadhunter et al. 2003 ), GMVA observations allow scales of the order of to be probed. The large jet viewing angle enables a prominent counter-jet to be detected in this source, which represents a fundamental advantage when investigating the nuclear regions of a jet. In fact, since the transverse width can be determined continuously along the two-sided flow, the assumption-dependent back-extrapolations of the properties of the jet apex can be replaced by actual measurements. The following analysis complements a previous VLBI study at 43 of the jet transverse profile and of the kinematic properties ( Boccardi et al. 2016 , hereafter B1). This revealed the presence of a pronounced transverse stratification, both in flux density (limb brightening) and bulk Lorentz factor (), typical of a flow with spine-sheath structure. Table 1 Log of observations at 86 GHz (3 mm) and characteristics of the clean maps shown in Fig. 1 . Notes. Column 1: Date of observation. Column 2: Array. VLBA_3mm indicates the part of the Very Long Baseline Array (all but the Hancock and St. Croix antennas) which is equipped with 86 GHz receivers; On – Onsala 20 m; Eb – Effelsberg 100-m; PdB – Plateau de Bure Interferometer; PV – IRAM 30-m atop Pico Veleta; Mh – Metsähovi. Column 3: Beam FWHM and position angle for untapered data with uniform weighting. 2. Observations and VLBI images The GMVA data set comprises three epochs from observations in 2009/2010 with a cadence between five and seven months (Table 1 ). The duration of the observations was 1516 h, 8 of which were spent on Cygnus A. This, together with the large number of antennas employed and with the favourable declination of the source, enabled good uv-coverage. Data were recorded in single polarization mode with a recording rate of 512 , which corresponds to an observing bandwidth of 128 . The correlation took place at the MPIfR in Bonn, Germany. The data reduction was carried out in AIPS ( Greisen 1990 ). Aside from the standard calibration procedures, special care was devoted during the fringe fitting. First, as described in Martí-Vidal et al. (2012) , the manual phase calibration was applied. Single sub-band phases and delays were calculated using one or more scans showing
Paper: 2017ApJ...834..197C (acknowledgments)
We thank D. Gurnett for the Voyager wave spectrogram, N. Schwadron for the IBEX Ribbon spectrogram, and J. Harding for preparing Figures 1 , 2 , and 4 . I.H.C. thanks H. Elliott, V. Florinski, D. McComas, D. Melrose, N. Pogorelov, G. Zank, and E. Zirnstein for helpful advice and discussions. He also thanks the University of Sydney for support under its Special Studies Program (SSP), J. LaBelle and G. Zank for hosting his SSP visits to Dartmouth College and the University of Alabama at Huntsville (UAH), respectively, and the staff and colleagues at Dartmouth, UAH, and SwRI for their support and interest during his visits. S.A.F.’s research at SwRI was supported by NASA through the Explorer Program.