adsabs/WIESP2022-NER huggingface dataset:
Paper: 2019MNRAS.489.2505M (fulltext)
of position and velocity or momentum, and that are conserved throughout the orbit. There are three action coordinates: radial action ( J R ), vertical action ( J Z ), and angular momentum ( L z ). By providing all three action coordinates, one can perfectly describe an entire orbit at any point in time or space. Traditionally, actions were incredibly difficult to calculate. In fact, they can only be analytically solved for a small subset of convenient galactic potentials. As computers became more advanced, astronomers developed ways to numerically approximate action coordinates. Sanders Das ( 2018 ) used the Stäckel Fudge method for approximating actions (Binney 2012 ), which interpolates on a distribution of phase-space coordinates generated from an axisymmetric potential. Resulting errors on the actions are propagated through from errors on parallax, proper motion, and radial velocity. We use the vertical actions calculated by Sanders Das ( 2018 ) to determine whether stars in our sample are members of the thick or thin disc (see Section 3.2 ). 2.4 Cross-matching and quality cuts In order to compare the motions of our planet host and stellar samples, we used Megan Bedell’s catalogue of data cross-matched between Gaia DR2 and Kepler DR25 with a 1 arcsecond search radius, downloaded on 2019 January 9. The two catalogues were matched using the RA and Dec coordinates of every star. The final cross-matched catalogue contains 197 090 stars, 1647 of which are confirmed planet hosts. We make the following quality cuts on both our planet host and field star samples: We removed stars with negative parallax values. This left our planet host sample with 1637 members and our field star sample with 195 545. We removed giants as well as massive and very-low mass dwarfs from our data by discarding stars with logg 4 and effective temperatures 4000 or >8000. We did this because Kepler was optimized for finding planets around FGK stars and therefore has a lower completeness for giants (Sliski Kipping 2014 ). This left our planet host sample with 1477 stars and our field star sample with 148 860 stars. We removed stars with relative errors in the total velocity (see Section 3 ) >10 per cent to minimize the error propagated through our analysis. Much of the error in the velocity calculation comes from uncertainties in the parallax, so making this 10 per cent cut ensures that we are only using stars with small parallax uncertainties and therefore reliable distances consistent with those in Bailer–Jones et al. ( 2018 ). This left us with two final samples of Kepler FGK dwarfs with reliable galactocentric velocities: a planet host sample with 1437 members and a field star sample with 140 918 members. Fig. 1 shows the galactocentric X-Y positions of the stars in the cross matched catalog, color-coded by how far they got in the sample selection process. Our field star sample is shown in black points and our planet host sample is shown in blue. Figure 1. Face-on view
Paper: 2015MNRAS.453.3257L (acknowledgments)
The authors thank the anonymous reviewer for a very prompt and helpful set of comments. HNL is partially funded by STFC grant ST/L000636/1. SF acknowledges funding from the European Research Council under the European Union's Seventh Framework Programme (FP7/2007-2013)/ERC Grant agreement n258729.
Paper: 2019A&A...631A..69M (acknowledgments)
Acknowledgements The authors wish to thank Richard Booth, Antonella Natta, Karin Öberg, and Jennifer Bergner for insightful comments and interesting discussions. A.M. and S.F. acknowledge an ESO Fellowship. This project has received funding from the European Union’s Horizon 2020 research and innovation programme under the Marie Sklodowska-Curie grant agreement No 823823, (RISE DUSTBUSTERS). This work was funded by the Deutsche Forschungsgemeinschaft (DFG, German Research Foundation) – Ref no. FOR 2634/1 ER685/11-1. This paper makes use of the following ALMA data: ADS/JAO.ALMA#2016.1.00459.S. ALMA is a partnership of ESO (representing its member states), NSF (USA) and NINS (Japan), together with 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 ESO, AUI/NRAO and NAOJ.
Paper: 2017MNRAS.464.2249H (fulltext)
for the independent frequencies are also quoted. Formal errors on the amplitudes are ± 0.3 mmag in u and ± 0.2 mmag in v , y , B , and R . These formal errors are known to underestimate the real errors by about a factor of 2 (Handler et al. 2000 ; JHS ). The S/N quoted is for the data set used to create Fig. 3 . The detected signals are separated in groups of independent pressure and mixed modes (numerical subscripts), gravity modes (letter subscripts), as well as first-, second-, and third-order combination frequencies, respectively. The residuals from this solution were searched for other signals that may be intrinsic to the star. We analysed the amplitude-scaled residuals in the different filters (whereby the u data were divided by 1.5, the v and B data are divided by 1.05, and the R data are multiplied by 1.05 to scale them to amplitudes similar to that in the y filter), and using different combinations of data sets. Even though some interesting possibilities for further intrinsic pulsation frequencies offered themselves, we prefer to err on the side of caution and stop the frequency search at this point. Nevertheless, it is interesting to note that the residual scatter in the light curves (6.4 mmag per point in u , 5.2 mmag per point in v , 4.5 mmag per point in y , 5.5 mmag per orbit in B , and 4.2 mmag per orbit in R ) is larger than the precision of the observations. This may be partly explicable by data reduction imperfections, but residual intrinsic stellar variability is also likely involved. 4 MODE IDENTIFICATION BRITE-Constellation was designed to obtain multicolour time series photometry specifically to provide identifications of the spherical degree l of the modes of pulsating stars (Weiss et al. 2014 ). Daszyńska-Daszkiewicz ( 2008 ) provided diagnostic diagrams to perform such mode identifications from a comparison of the amplitude ratios and phase shifts between the two BRITE passbands. The four strongest modes of ν Eri are, both spectroscopically and photometrically, uniquely identified (De Ridder et al. 2004 ; Handler et al. 2004 ; Daszyńska-Daszkiewicz Walczak 2010 ): the strongest mode is radial (spherical degree l = 0) and the high-amplitude triplet consists of dipole modes ( l = 1). In Fig. 4 , the observed uvyBR amplitude ratios are compared to theoretical predictions for the used Strömgren and BRITE passbands for these four modes. Figure 4. Identification of the spherical degree of the four strongest pulsation modes of ν Eri. The filled circles with error bars are the observed amplitude ratios, in order of increasing wavelength u / u , v / u , B / u , y / u , and R / u . The full lines are theoretical predictions for radial modes, the dashed lines for dipole modes, the dashed–dotted lines for quadrupole modes, the dotted lines for l = 3 modes, and the dashed–dot–dot–dotted lines are for l = 4. The thin error bars delineate the uncertainties in the theoretical amplitude ratios. The theoretical amplitude ratios were
Paper: 2017ApJ...849L..15E (fulltext)
Matthaeus et al. 2007 ), but which for the purposes of comparison has the benefit of having been used in previous electron modulation studies, as well as providing results not vastly different from those derived using a more realistic spectral form (Engelbrecht Burger 2013a ). Expressions for derived using different energy-containing range spectral indices can be found in Shalchi et al. ( 2010 ) as well as Engelbrecht Burger ( 2015 ). The results of this calculation are shown in the right panel of Figure 2 . The solutions where PUI effects have been neglected are considerably smaller than the corresponding values, with a less steep rigidity dependence, in contrast with what is usually assumed in cosmic-ray modulation studies. A decrease in dynamical effects leads to larger perpendicular MFPs due to their dependence on . When , the PUI-affected solutions are very small relative to when PUI effects are ignored, as expected, but now assume values larger than the corresponding parallel MFPs. This is a consequence of the dependence in Equation ( 10 ). Choosing leads to perpendicular MFPs smaller than the corresponding at 50 and 100 au, and larger at 10 au. Figure 1. Wavelike energies (top panel) and parallel correlation scales (middle panel) yielded by the Oughton et al. ( 2011 ) TTM model both with (blue lines) and without (red lines) PUI driving. Bottom panel shows (Equation ( 9 )) at 1 MeV as function of μ at 10 au using inputs from the abovementioned TTM. Figure 2. Parallel mean free paths at various radial distances taking into account PUI effects (red lines) and neglecting them (blue lines; Equation ( 6 )), as a function of rigidity for full dynamical effects (; top panels) and reduced dynamical effects (; bottom panels). To study the effects of PUI-driven waves on the electron drift coefficients, an expression for the turbulence-reduced drift coefficient proposed by Engelbrecht et al. ( 2017 ) is employed, where the lengthscale corresponding to the drift coefficient is given bywhere denotes the total transverse variance. This expression reduces to the weak scattering, full drift lengthscale in the absence of turbulence. Figure 3 shows this drift lengthscale as function of rigidity for and at various radial distances, including the PUI-affected perpendicular MFPs from Figure 2 for the purposes of comparison. Note that this figure is plotted on a different scale to that of Figure 2 , for the purpose of clarity. Solutions computed without PUI effects (blue lines) decrease sharply from the weak scattering values (black lines) at the lowest rigidities, due to the larger values of at these rigidities, and remain well below the calculated assuming no PUI effects for both values of α . When PUI effects are included, though, the drift lengthscale at 10 au also drops below the weak scattering value for both values of α , and remains below the corresponding . At 50 and 100 au, however, the PUI-influenced drift coefficient becomes very similar to the
Paper: 2015MNRAS.448.2530Z (acknowledgments)
DZ's work is supported by a Research Excellence Scholarship from the University of Nottingham and the China Scholarship Council. AAS and CJC acknowledge financial support from the UK Science and Technology Facilities Council. This paper is partially based on SDSS data. 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 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.
Paper: 2019A&A...626A..20M (fulltext)
6′′ of the central source detected by M98 and compare it with the current number (including objects from the WDS catalog, Gaia DR2, and companions detected in this paper, see below) the number has grown from 12 to 28, an equally impressive advancement. As we will show in future papers, there is still room for significant improvements in the case of new spectroscopic orbits. The same should be true for the discovery of new astrometric companions, not only using lucky imaging but also more sophisticated techniques such as the ones used in the southern hemisphere by the SMaSH+ survey ( Sana et al. 2014 ). The value of our results lies mostly in the updated detailed information, such as the homogeneous revision of the spectral classification of the sample applying the criteria we have developed for GOSSS, that can be used for future global analyses of the multiplicity in O stars. We indeed plan to do such analyses in future papers ourselves but it is also worthy to point out some results for individual systems in this work. We present first-time O-type GOSSS spectral classifications for 17 objects: HD 170 097 A, QR Ser, BD − 13 4923, HD 190 967, HD 193 611, HDE 228 989, HDE 229 234, Cyg OB2-3 A, ALS 15 133, ALS 15 148, Cyg OB2-1, ALS 15 131, Cyg OB2-20, Cyg OB2-15, ALS 12 502, DN Cas, and IU Aur AB. For another six objects we present their first-time B-type GOSSS spectral classifications: HD 193 322 B, Cyg OB2-3 B, HD 15 558 B, HD 16 429 C, MY Cam B, and LY Aur B. We have identified one eclipsing system as SB2 for the first time, HD 170 097 A, and derived its separate spectral classifications. To that one we can add a second eclipsing system in the sample, ALS 12 688, that was identified as having double absorption lines for the first time in GOSSS III. For another eclipsing binary, V747 Cep, we detect moving lines (SB1) for the first time using our LiLiMaRlin spectra. For two systems that have published SB1 orbits, BD − 16 4826 and θ 2 Ori A, we publish the first spectrograms with double lines (SB2) and derive their first true separate spectral classifications. For HD 168 112 AB we also publish the first SB2 spectrograms and separate spectral classification. We have also detected nine new astrometric components, one each around HD 190 967, ALS 15 133, Cyg OB2-A11, Cyg OB2-1, ALS 12 502, DN Cas, and MY Cam A and two around IU Aur AB. The results of this paper will be added to GOSC at the time of publication, which will reach version 4.2. With them, GOSC will contain a total of 655 objects: 611 in the main catalog (Galactic O stars), 32 in supplement 2 (Galactic early-type stars), and 12 in supplement 3 (Galactic late-type stars). It is not possible to do a full multiplicity analysis based on our 92 stars for two reasons: the sample is too small and is biased. The most obvious bias is that we selected our stars from systems that had spectroscopic orbits previously published, so no single targets are included. Note, however, that several SB1?
Paper: 2017A&A...601A..56T (acknowledgments)
Based on data products from observations made with ESO Telescopes at the La Silla Paranal Observatory under programme ID 188.B-3002. These data products have been processed by the Cambridge Astronomy Survey Unit (CASU) at the Institute of Astronomy, University of Cambridge, and by the FLAMES/UVES reduction team at INAF/Osservatorio Astrofisico di Arcetri. These data have been obtained from the Gaia -ESO Survey Data Archive, prepared and hosted by the Wide Field Astronomy Unit, Institute for Astronomy, University of Edinburgh, which is funded by the UK Science and Technology Facilities Council. This work was partly supported by the European Union FP7 programme through ERC grant number 320360 and by the Leverhulme Trust through grant RPG-2012-541. We acknowledge the support from INAF and Ministero dell’ Istruzione, dell’ Università e della Ricerca (MIUR) in the form of the grant “Premiale VLT 2012”. The results presented here benefit from discussions held during the Gaia -ESO workshops and conferences supported by the ESF (European Science Foundation) through the GREAT Research Network Programme. We thank the anonymous referee for insightful comments. D.G., S.V., and B.T. gratefully acknowledges support from the Chilean BASAL Centro de Excelencia en Astrofísica y Tecnologías Afines (CATA) grant PFB-06/2007. C.M. acknowledges support from CONICYT-PCHA/Doctorado Nacional/2014-21141057. R.E.C. acknowledges funding from Gemini-CONICYT for Project 32140007. F.M. gratefully acknowledges the support provided by Fondecyt for project 314017. This work was partly supported (A.R.C.) by the European Union FP7 programme through grant number 320360. This work was partly supported (A.D., G.T., R.Ž.) by the grant from the Research Council of Lithuania (MIP-082/2015). S.G.S. acknowledges the support from FCT through Investigador FCT contract of reference IF/00028/2014 and the support from FCT through the project PTDC/FIS-AST/7073/2014. C.L. gratefully acknowledges financial support from the European Research Council (ERC-CoG-646928, Multi-Pop, PI: N. Bastian). V.A. acknowledges the support from the FCT (Portugal) in the form of the grant SFRH/BPD/70574/2010, the support by FCT through national funds (Refs. PTDC/FIS-AST/7073/2014 and PTDC/FIS-AST/1526/2014) and by FEDER through COMPETE2020 (Refs. POCI-01-0145-FEDER-016880 and POCI-01-0145-FEDER-016886).
Paper: 2017MNRAS.467..179G (fulltext)
and magnetic fields, and has been shown to produce realistic galaxy populations in large-scale cosmological boxes (Vogelsberger etal. 2013 ; Genel etal. 2014 ). The most novel aspects of the simulations, with respect to previous studies, are the large simulation sample, high resolution, the inclusion of magnetic fields that are seeded, grown and evolved in a fully cosmological context, and the BH model that has been used in only one simulation set previous to this study (Marinacci etal. 2014a ). The suite comprises 30 simulations with typical baryonic mass resolution of around 510 4 M , three of which have higher resolution counterparts with eight times better mass resolution. The sample size, resolution and galaxy formation model make these simulations some of the most advanced and comprehensive found in the literature. We analysed the properties of the stellar components of these simulations, and found that they lie on the expected stellar masshalo mass relation, and are consistent with other key observables such as flat rotation curves, the massmetallicity relation and present-day SFRs. The simulated galaxies are, on average, slightly too massive in the stellar component, particularly at earlier times such as z 3. This may indicate the need for early stellar feedback (see e.g. Aumer etal. 2013 ; Stinson etal. 2013a ). Such feedback may bring down the stellar masses of our simulations and reduce the number of compact galaxies (see Fig. 5 ), which we will investigate in future work. The mass distributions of our simulated galaxies are realistic and produce rotationally supported discs: most of our simulations have flat rotation curves, with velocities that match the TullyFisher relation for Milky Way-mass galaxies. We note that in the past, it has proven to be difficult to reproduce flat circular velocity curves for galaxy discs in haloes in the virial mass range 1210 12 M (see for example, Stinson etal. 2010 ; Mollitor, Nezri Teyssier 2015 ; Wang etal. 2015 ), although a variety of recent models have achieved some success (Aumer etal. 2013 ; Stinson etal. 2013a ; Marinacci etal. 2014a ; Schaller etal. 2015a ; Colin etal. 2016 ). The circularity distributions indicate that at least two-thirds of the simulations have well-defined, rotationally supported disc components, with disc-total mass ratios of up to 0.60.7 for the most disc-dominated simulations. These are among the highest disc-total mass ratios in the literature, along with Aumer etal. ( 2013 ). The vertical structure of our simulated discs appears to be somewhat thicker than expected from observations in the Milky Way, which may be related to energy from stellar feedback that acts to puff up the gas disc (see Marinacci etal. 2016 ). Rokar etal. ( 2014 ) reported a similar conclusion, although their feedback recipe included radiation feedback that destroyed the morphology of their disc in addition to thickening it. However, the inner discs of our simulations show some consistency
Paper: 2016MNRAS.457.3678P (acknowledgments)
We are grateful to the referee, Professor M.A. Dopita, for his constructive comments. LSP and EKG acknowledge support in the framework of Sonderforschungsbereich SFB 881 on ‘The Milky Way System’ (especially subproject A5), which is funded by the German Research Foundation (DFG). LSP thanks for the hospitality of the Astronomisches Rechen-Institut at Heidelberg University where part of this investigation was carried out. This work was partly funded by the subsidy allocated to Kazan Federal University for the state assignment in the sphere of scientific activities (LSP).
Paper: 2015MNRAS.452..986S (acknowledgments)
The authors would like to thank the anonymous referee who provided useful suggestions that improved this manuscript. RCS gratefully acknowledges support through a grant from the STScI JDF. This research has made use of the Fabry Perot data base, operated at CeSAM/LAM, Marseille, France. The authors also acknowledge NSF grants AST 95- 29098 and 00- 71198 to UC Santa Cruz. RCS would like to thank A. Dutton for helpful comments. We wish to extend thanks to those of Hawaiian ancestry on whose sacred mountain we are privileged guests.
Paper: 2017MNRAS.469.4504M (acknowledgments)
Acknowledgments The authors thank the referee for the comments and suggestions in their helpful report. Computer time for the simulations performed with GENESIS was provided by HPC resources of Cines under the allocation A0010406957 made by GENCI (Grand Equipement National de Calcul Intensif). Those performed with FARGO utilized: Queen Mary's MidPlus computational facilities, supported by QMUL Research-IT and funded by EPSRC grant EP/K000128/1; and the DiRAC Complexity system, operated by the University of Leicester IT Services, which forms part of the STFC DiRAC HPC Facility ( www.dirac.ac.uk ). This equipment is funded by BIS National E-Infrastructure capital grant ST/K000373/1 and STFC DiRAC Operations grant ST/K0003259/1. DiRAC is part of the National E-Infrastructure. This research was also supported in part by the National Science Foundation under Grant No. NSF PHY-1125915.
Paper: 2018MNRAS.473.1570Y (acknowledgments)
Acknowledgements We are grateful to Dr. H. Shimabukuro for helpful comments on a draft version of this manuscript. This work is supported by Grant-in-Aid from the Ministry of Education, Culture, Sports, Science and Technology (MEXT) of Japan, Nos. 24340048, 26610048, 15H05896, 16H05999, 17H01110 (KT) and 16J01585 (SY), and Bilateral Joint Research Projects of JSPS (KT).
Paper: 2017ApJ...849...15W (acknowledgments)
This work was supported in part through the Air Force Office for Scientific Research, FA9550-15-1-0213, by Ministerio de Economía y Competitividad of Spain, CTQ2014-58617-R, and by Xunta de Galicia through project GRC2014/032. The authors also thank “Centro de Supercomputación de Galicia (CESGA)” for the use of their computational facilities.
Paper: 2018MNRAS.479.3952B (acknowledgments)
ACKNOWLEDGEMENTS This material is based on work supported by the National Science Foundation Graduate Research Fellowship under Grant No. DGE-1329626. The authors would also like to acknowledge the aid of both anonymous referees, Lars Hernquist, Brent Tully, and Larissa Nofi in preparing this document for publication.
Paper: 2015A&A...583A..53L (acknowledgments)
The contributions by P. Bergman, including the interesting discussions, are highly appreciated. We also thank the Swedish APEX team and the APEX staff on site for their help with the observations. As part of our Odin and Herschel work, this research has been supported by the Swedish National Space Board (SNSB).