adsabs/WIESP2022-NER huggingface dataset:
Paper: 2016A&A...588A.106W (fulltext)
1966 ) and the effect on measured image quality was seen by the smaller FWHM of star images at redder wavelengths compared to 4900 Å in the MUSE cubes. Given that the wave feature of the extinction maps occurs where the surface brightness decreases by a factor 2 over a distance of a few spaxels (0.5), then the effect of the different image FWHM between the wavelengths of the H Balmer lines would modulate the ratio image which forms the basis of the extinction determination. For example for a step function across the shell, the ratio map H/H would be expected to show a trough, since the image FWHM at H is lower than at H. On the 10 s MUSE cube the measured FWHM of the central star varies from 0.53 to 0.50 between H and H. In order to determine if this effect could be responsible for the observed wave-trough appearance across the inner shell, the H image was convolved with a Gaussian to the same measured FWHM as the H image and the extinction map redetermined. The strength of the trough is slightly decreased, by 0.02 in , and the wave increased by a lesser amount, but the features remain. A repeat of this test but with the 120 s H map showed a similar result. Having rejected instrumental or seeing effects as causing the pattern in extinction, astrophysical effects are now examined. 3.4. Balmer v. Paschen line ratios The He II Pickering series 6g-4f 6560.10 Å line is within 2.7 Å of the H line and at the resolution of the MUSE spectra, and given the very large flux ratio (100), will be included in the flux of the fitted H line. Thus the H flux needs to be corrected for the contamination of the He II line (1% of the H surface brightness in the bright He II core of the nebula). The He II Pickering 7g-4f 5411.52 Å line was measured in all the cubes and from the Case B ratio 6560.1/5411.5 Å ratio, the 6560.1 Å observed line flux was computed using Storey Hummer (1995) and a reddening map. The observed value of the He II 6560.10 Å line of 0.0338 F(H) tabulated by Fang Liu (2011) appears to be too large (the theoretical ratio 6560.1/5411.5 Å is 1.75 at 10 K whilst Fang Liu 2011 have a dereddened ratio of 2.92). Similarly the Pickering He II 8g-4f 4859.32 Å line is blended with H at the MUSE resolution, so its contamination of the measured H flux should also be corrected (similarly 1% of H in the core). The theoretical ratio of 4859.3 Å to 5411.5 Å was again used. Applying both these corrections to the H and H flux maps, the derived extinction map was re-computed. The He II line is indeed only strong inside the inner rim and is very weakly present outside the rim, so the effect of the correction to H and H fluxes for He II is insignificant where the strongest features of the extinction are present. Inside the inner rim, where the He II is brightest, the effect on the extinction map is small, . The Paschen lines higher than P9 (9229.0 Å) are also available for extinction determination. These lines also have the advantage that the contaminating He II
Paper: 2018MNRAS.481.1786F (acknowledgments)
ACKNOWLEDGEMENTS We thank the MDM Observatory staff for their assistance and rapid instrument re-configuration, and Ronald Downes and Debra Wallace for help in constructing an H α survey of the Cygnus Loop. This research was made possible in part by funds from NASA’s SpaceGrant, the Guarini School of Graduate and Advanced Studies at Dartmouth, and is part of RAF’s Archangel Research Program. We have made use of data from the European Space Agency (ESA) mission Gaia ( https://www.cosmos.esa.int/gaia ), processed by the Gaia Data Processing and Analysis Consortium (DPAC, https://www.cosmos.esa.int/web/gaia/dpac/consortium ). Funding for the DPAC has been provided by national institutions, in particular the institutions participating in the Gaia Multilateral Agreement. This research has also made use of the SIMBAD data base, operated at CDS, Strasbourg, France.
Paper: 2020ApJ...897L...1G (fulltext)
large SEP events (e.g., Gopalswamy 2018 ). SEP events need to be magnetically connected to the observer in order to be detected; type II bursts do not have such a requirement. Only 2 of the 44 cycle-23 limb halos are not associated with DH type II bursts; they are slow (800 km s −1 on 2000 October 24; 896 km s −1 on 2002 January 4) compared to the average speed of CMEs associated with cycle-23 DH type II bursts (1219 km s −1 ). The 2002 January 4 CME is associated with a metric type II burst, while the 2000 October 24 CME is radio-quiet. Nine cycle-24 halos have no DH type II association (see Table 1 ): five have metric type II bursts, three are quiescent filament-eruption events (which are only occasionally associated with DH type II bursts, Gopalswamy et al. 2015a ), and the slowest cycle-24 halo (2012 February 23). The four radio-quiet halos are slow (505 to 919 km s −1 ) compared CMEs associated with cycle-24 DH type II bursts (1059 km s −1 ). Thus, an overwhelming majority of limb halos (cycle 23: 98%; cycle 24: 90%) have type II bursts indicative of electron acceleration. 4. Discussion and Summary We analyzed large samples of limb-halo CMEs observed in cycles 23 and 24. We found that cycle-24 halos are slower than the cycle-23 ones. The limb CMEs that revealed wider width in cycle 24 did not show the speed difference (Gopalswamy et al. 2014a ). We introduced a new parameter—the height at halo time is readily determined for limb halos, but not for disk halos (the CME nose is hidden by the occulting disk of the coronagraph). The cycle-24 halo heights are significantly smaller. Combined with the result that cycle-24 halos are slower, we conclude that halos form at shorter heliocentric distances at lower speeds. Furthermore, we ruled out the possibility that the difference in CME properties is due to solar-source characteristics represented by soft X-ray flare size. Thus, we can pin down the heliospheric state as the main cause of the anomalous CME expansion in cycle 24. The number of limb halos (44) in cycle 23 is only slightly larger than the number (38) in cycle 24. This corresponds to a drop of only 14% in cycle 24. There was a 4 month SOHO data gap in cycle 23 (3 month in 1998 and one month in 1999). Assuming that the limb halos occurred at the cycle-averaged monthly rate (0.3 per month), we expect only one additional CME during the data gap. Then the drop is only 16%. This is much smaller than the 40% drop in the cycle-averaged total SSN from 81 to 49. Normalizing to SSN, we see that there are ∼42% more limb halos per SSN in cycle 24. This result was previously obtained by considering all LASCO halos in the first half of the two cycles (Gopalswamy et al. 2015b ). The effect of the heliospheric state on CMEs has important implications for space weather: lower geoeffectiveness is expected in SC 24 because lower speed and weaker CME magnetic field (due to expansion) result in a weaker storm. Furthermore, milder space weather is
Paper: 2019A&A...628A...9C (acknowledgments)
Acknowledgements The authors would like to thank Dr Sven Buder for his useful comments and discussion about Na abundances. Based on observations made with the Italian Telescopio Nazionale Galileo (TNG) operated on the island of La Palma by the Fundación Galileo Galilei of the INAF (Istituto Nazionale di Astrofisica) at the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias. CARMENES is an instrument for the Centro Astronómico Hispano-Alemán de Calar Alto (CAHA, Almería, Spain) funded by the German Max-Planck-Gesellschaft (MPG), the Spanish Consejo Superior de Investigaciones Científicas (CSIC), the European Union through FEDER/ERF FICTS-2011-02 funds, and the members of the CARMENES Consortium. This work is partly financed by the Spanish Ministry of Economics and Competitiveness through project ESP2016-80 435-C2-2-R. G.C. acknowledges the support by the National Natural Science Foundation of China (Grant No. 11503088, 11573073, 11573075) and by the project “Technology of Space Telescope Detecting Exoplanet and Life” from National Defense Science and Engineering Bureau civil spaceflight advanced research project (D030201). F.Y. acknowledges the support of the DFG priority programme SPP 1992 “Exploring the Diversity of Extrasolar Planets (RE 1664/16-1)”. A.F. acknowledges the support from JSPS KAKENHI Grant Number JP17H04574. This work is partly supported by JSPS KAKENHI Grant Numbers JP18H01265 and 18H05439, and JST PRESTO Grant Number JPMJPR1775. This article is based on observations made with the MuSCAT2 instrument, developed by ABC, at Telescopio Carlos Sánchez operated on the island of Tenerife by the IAC in the Spanish Observatorio del Teide. This work made use of PyAstronomy and of the VALD database, operated at Uppsala University, the Institute of Astronomy RAS in Moscow, and the University of Vienna.
Paper: 2016MNRAS.461.4182M (fulltext)
mass profiles are extrapolated based on the best-fitting temperature profile model beyond the extent of the temperature profile. The median extent of the temperature profiles is 1.25 R 500 . Profiles of the mass ratios beyond that point are less robust. In Fig. 4 , the ratio of the hydrostatic to caustic masses at the radius R 500 determined from the hydrostatic mass profile is shown for each cluster. Again, the ratios are computed as . At this radius, the two mass estimators agree well, with κ = 0.080 ± 0.046, corresponding to . The intrinsic scatter between the hydrostatic and caustic mass estimators at this radius is , corresponding to an intrinsic scatter of . The RCC and NRCC subsamples show consistent results, albeit with weaker constraints. Figure 4. Ratio of hydrostatic to caustic masses at the hydrostatic R 500 for each cluster (computed as ). Points are coloured to indicate RCC (blue triangles) and NRCC (red circles) clusters. The solid line and shaded band show the mean bias between the hydrostatic and caustic masses and its uncertainty. These summary statistics are captured in Table 3 , along with the same quantities derived in a fixed aperture of for each cluster. The parameter values are insensitive to the choice of aperture, demonstrating that our results are not significantly influenced by scaling the caustic profiles to the hydrostatic estimate of R 500 . Table 3. Summary statistics of the ratio of the mean bias between hydrostatic and caustic masses, measured in the hydrostatic estimate of R 500 and in a fixed aperture of . The second column gives the subset being considered and the third column gives the mean bias. The mean bias is expressed as the mean ratio of masses in column four, and the intrinsic scatter between the mass estimators (converted to a percentage) is given in column five. Note that the quantities in columns four and five are summaries of a lognormal distribution using a median and percentiles as described in Section 3.3 . 5 DISCUSSION 5.1 Biases in hydrostatic and caustic masses We have performed one of the first comparisons between mass profiles of galaxy clusters determined from their hot gas via hydrostatic assumptions, and the dynamics of their galaxies via the caustic method. These two methods are completely independent, and are subject to different assumptions and systematics. We found that, while significant scatter is present between the two estimators, the average agreement is good. As demonstrated in Fig. 2 , the masses agree to better than ≈20 per cent on average over the full radial range sampled by both techniques. Importantly, neither of the mass measurement techniques assumed a functional form for the mass profile (although the hydrostatic analysis did use parametric temperature and density profiles). The agreement we find is not a consequence of a common parametrization of the mass profile. This good average agreement is somewhat surprising given that various observational and
Paper: 2019MNRAS.486.5853D (acknowledgments)
ACKNOWLEDGEMENTS We are grateful to the anonymous referee for her/his very useful comments and suggestions that helped us to clarify and improve this work. OLD and ACK are grateful to FAPESP and CNPq. AFM is grateful to CAPES. MVC and GFH are grateful to CONICET. OLD is grateful to Dr. Sameshima and Dr. Miller for making their BLR metallicity estimations and α ox values available, respectively.
Paper: 2020A&A...637A..78S (fulltext)
the main object, respectively, and Na 1, Na 2, Ne 1, and Ne 2 are factors that take place in eccentric orbits and are defined by 5.2 General relativistic effect The important effect derived from General Relativity theory (GRT) on the dynamic of planetary systems is the precession of ω ( Einstein 1916 ). In our case, we considered that only the main object contributes with relevant corrections. As we worked in the reference frame of the star, the associated correction in the acceleration of the embryo is with c the speed of light. Eq. ( 19 ) was proposed by Anderson et al. (1975) , who worked under the parameterize post-Newtonian theories. The authors obtained a relative correction associated with two parameters β and γ , which are equal to unity in the GRT case. This expression has been used in several works that included relativistic corrections (e.g., Quinn et al. 1991 ; Shahid-Saless Yeomans 1994 ; Varadi et al. 2003 ; Benitez Gallardo 2008 ; Zanardi et al. 2018 ). The timescale associated with the precession of the longitude of periastron is given by 5.3 Test simulations We made a set of N -body simulations in order to test the agreement between the external forces that we incorporated in the M ERCURY code and the timescale associated with them. To test the precession of ω , we developed two simulations: one that included the tidal distortion term, and another that included the GR correction. In Fig. 5 we show the apsidal precession timescale of a planet with 1 M ⊕ orbiting a 1 Myr substellar object of 0.08 M ⊙ with initial values a = 0.01 au and e = 0.1 for the two simulations we made. Our results show that the apsidal precession of 360° is completed in 14 750 and 3060 yr, respectively, which agrees with the time predicted by the timescales associated with each correction term in Eqs. ( 20 ) and ( 8 ). These timescale values depend on the physical parameters of the protoplanetary embryos and the substellar object, as well as on the initial orbital elements. For instance, if the protoplanets are smaller than Earth in mass and radius, then the relativistic effect is more relevant than the tidal distortion regarding the precession of ω . Fig. 5 Apsidal precession due to tidal distortion (solid red line) and GR effects (dotted blue line) in a system composed of a 1 M ⊕ planet around a 0.08 M ⊙ BD with initial a = 0.01 au and e = 0.1. In this example, the argument of periastron completes an orbit in ~14 750 yr when is affected by GR and in ~3060 yr when is affected by tidal distortion. Fig. 6 Evolution of e , a , and the pseudo-synchronization period of a 1 M ⊕ around a 0.04 M ⊙ BD. Solid lines indicates the results considering the initial orbital elements from Bolmont et al. (2011) . The dashed lines indicate the evolution of r corot ( middle panel ) and the rotational period of the BD, P ⋆ ( bottom panel ). To test the analytic expressions for the tidal dissipation with the timescales of e and a decay, we developed a N -body simulation
Paper: 2018A&A...620A.192C (fulltext)
scaled-down AGN jet model based on equipartition assumptions and applied it to observationally well defined samples of galactic and extragalactic sources. They find that the jet powers of their studied sources were comparable to their accretion disk luminosities providing evidence for a disk-jet coupling holding from stellar mass BHs to low-luminosity AGN. Merloni Heinz (2008) present a synthesis model for the AGN evolution where they studied how SMBHs grow and evolve through the age of the Universe. In this model, AGN with high Eddington ratios may display either only radiative feedback (high-radiative mode, HR) or both radiative and kinetic feedback (high-kinetic mode, HK). In this context, HLAGN with low radio AGN fractions ( f AGN 0.5) would be those which display mostly radiative feedback, while those with high radio AGN fractions ( f AGN ≥ 0.5) also produce kinetic feedback in the form of radio-detectable features, such as cores, jets and lobes. Radiative feedback is expected to arise in galaxies hosting rapidly accreting SMBHs, where the energy released by the growth of the SMBH can influence the properties of the hosts (e.g., see a review by Fabian 2012 ). The models of galaxy evolution usually find the AGN bolometric luminosity density to increase from the local redshift out to a peak around z ∼ 2 − 3, followed by a decrease toward higher redshifts (e.g., Croton et al. 2006 ; Merloni Heinz 2008 ). For the ∼38% of HLAGN for which we estimated a radio luminosity arising from AGN emission (Sect. 3.2 ) we compare the radiative luminosity density to literature expectations (e.g., Croton et al. 2006 ; Merloni Heinz 2008 ). We binned the radiative luminosities derived from the SED-fitting decomposition (see Delvecchio et al. 2017 ) into nine redshift bins, finding typical values of bolometric luminosity density to be 1% of those found from the literature for all radiatively efficient AGN. This confirms that X-ray and MIR selected AGN detected in radio are not the dominant contribution to the total bolometric output expected for radiatively efficient AGN. In the following sections, we describe how the number and luminosity densities of HLAGN change through cosmic time. By scaling the 1.4 GHz AGN luminosity into kinetic luminosity, we calculate the kinetic luminosity density and compare it to semi-analytic model predictions. 6.2. Cosmic evolution of radio AGN To calculate the number and luminosity density, we use where Φ( L 1.4 GHz ) is the redshift evolved luminosity function, using both best-fit evolution parameters derived from the redshift binned and continuous fitting. Here we take the lower and upper limits of the integral to be L 1.4 GHz = 10 22 WHz −1 and L 1.4 GHz = 10 28 WHz −1 , respectively. The normalizations of the number and luminosity density evolution curves are affected by the chosen limits of integration. For example, a decrease of the lower limit to L 1.4 GHz = 10 21 WHz −1 would produce a number density higher by a factor
Paper: 2017MNRAS.467.3447L (acknowledgments)
Acknowledgments DLK was supported by National Science Foundation grant AST-1412421. TM acknowledges the support of the Australian Research Council through grant FT150100099. This scientific work makes use of the Murchison Radio-astronomy Observatory, operated by CSIRO. We acknowledge the Wajarri Yamatji people as the traditional owners of the Observatory site. Support for the operation of the MWA is provided by the Australian Government (NCRIS), under a contract to Curtin University administered by Astronomy Australia Limited. We acknowledge the Pawsey Supercomputing Centre that is supported by the Western Australian and Australian Governments.This research was conducted by the Australian Research Council Centre of Excellence for All-sky Astrophysics (CAASTRO), through project number CE110001020. Special thanks to the anonymous referee whose comments greatly improved this manuscript.
Paper: 2015A&A...576A..75T (acknowledgments)
I thank Alexei Butkevich for help in providing me with the relevant chapter in Eddington’s rare 1914 book and for discussions on different aspects of the Malmquist bias. Good remarks by the referee are also acknowledged.
Paper: 2016ApJ...823..102C (acknowledgments)
We thank the referee for his/her constructive comments. We thank Martha Boyer, Jason Kalirai, and Guillermo Torres for generously sharing their data with us and Francis Timmes for his assistance with nuclear reaction networks in MESA. We thank Leo Girardi and Dan Weisz for fruitful conversations and comments on the manuscript. We thank Conny Aerts, Lars Bildsten, Jonathan Bird, Phillip Cargile, Selma de Mink, Falk Herwig, Jessica Lu, Marc Pinsonneault, Philip Rosenfield, and Victor Silva-Aguirre for sharing their expertise. We also thank the entire MESA community for making this work possible, with special thanks to the MESA Council. Finally, we thank the participants of the KITP workshop “Galactic Archaeology and Precision Stellar Astrophysics” for stimulating discussions. This research was supported in part by the National Science Foundation under Grant No. NSF PHY11-25915. J.C. acknowledges support from the National Science Foundation Graduate Research Fellowship Program. A.D. received support from the Australian Research Council under grant FL110100012. C.C. acknowledges support from NASA grant NNX13AI46G, NSF grant AST-1313280, and the Packard Foundation. This work was supported in part by NASA grant NNX15AK14G. The computations in this paper were run on the Odyssey cluster supported by the FAS Division of Science, Research Computing Group at Harvard University.
Paper: 2017MNRAS.470.2007W (acknowledgments)
Acknowledgments Generous allocations of time on the 1m McLennnan Telescope and HERCULES spectrograph at the Mt John University Observatory in support of the Southern Binaries Programme have been made available through its TAC and supported by its Director, Dr K. Pollard and previous Director, Prof. J.B. Hearnshaw. Useful help at the telescope were provided by the MJUO management (N. Frost and previously A. Gilmore and P. Kilmartin). Assistance with the use and development of the hrsp software has been given by its author Dr J. Skuljan. Encouragement and support for this programme has been shown by the School of Chemical and Physical Sciences of the Victoria University of Wellington, as well as the Royal Astronomical Society of New Zealand and its Variable Stars South section ( http://www.variablestarssouth.org ). We thank VSSs former-director Tom Richards for advocating DSLR photometry in support of the Southern Binaries Programme, also the AAVSOnet Telescope Allocation Committee for telescope time in 2014 and 2015. We appreciate the hard work and dedication of AAVSOnet site managers Peter Nelson (BSM South) and Greg Bolt (BSM Berry). Dr P. Mayer kindly sent additional photometric details on QZ Car that were used in the construction of the OC curve. As well, Dr H. Drechsel made very useful comments regarding the effects of radiation pressure on the surficial distortions of very hot close binaries. The astrophysics group at COMU have been supportive of this research.