adsabs/WIESP2022-NER huggingface dataset:
Paper: 2018MNRAS.477.1970Z (acknowledgments)
ACKNOWLEDGEMENTS We have used NASA’s ADS Bibliographic Services. Most of the computations that made possible this work were performed with NASA NAIF SPICE Software (Acton 1996 and Jon D. Giorgini), Python 2.7 , and their related tools and libraries, iPython (Pérez Granger 2007 ), Matplotlib (Hunter et al. 2007 ), scipy , and numpy (Van Der Walt, Colbert Varoquaux 2011 ). Special thanks to the reviewers that through their criticism significantly contributed to improve the paper. In particular, we thank Steve Chesley for his in-depth initial review of this work; his comments and observations contributed to improve significantly the quality of the manuscript with respect to its initial versions. We appreciate the assistance of Jon D. Giorgini, senior analyst of the JPL Solar system Dynamics Group. We also thank Professor Ignacio Ferrin and Professor David Asher for useful comments and insightful discussions about this topic. We also thank the organizers of Meteoroid 2016 conference for allowing us to present the initial versions of this work to the meteor and asteroid scientific community. This work is supported by Vicerrectoria de Docencia-UdeA and the Estrategia de Sostenibilidad 2014-2015 de la Universidad de Antioquia . MS is supported by Colciencias, Doctorado Nacional - 647 programme. We thank Universidad Pontificia Bolivariana (UPB-Medellin) and DELL for allowing us to run most of our simulations in their data centres.
Paper: 2017MNRAS.465.1699M (acknowledgments)
Acknowledgments We gratefully acknowledge the fine support at the MMT Observatory, and the Local Group Galaxy Survey conducted at NOAO by Phil Massey and collaborators. This research has made use of the VizieR catalogue access tool, operated at CDS, Strasbourg, France. This study has been supported in part by the Polish National Science Centre grant DEC-2013/10/M/ST9/00086. KI has been also financed by the Polish Ministry of Science and Higher Education Diamond Grant Programme via grant 0136/DIA/2014/43.
Paper: 2017ApJ...846...69R (acknowledgments)
I thank Miles for significantly delaying this publication (by being born and so completely disrupting my life). I would not have it any other way. I thank the anonymous referee for constructive comments that helped to improve and clarify this manuscript. This research was supported by NASA Astrophysics Theory Program grant NNX17AG25G and made use of 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.
Paper: 2016A&A...586A..59G (acknowledgments)
This work is based on observations with the Gran Telescopio Canarias (GTC), installed in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofísica de Canarias on the island of La Palma. This work has been funded by the Spanish Ministry of Economy and Competitiveness (MINECO) under the grant AYA2011-22614 and also received partial support from the DGAPA-UNAM, Mexico under grant PAPIIT IN109614. We thank the referee, G. Stasińska, for her valuable comments that helped to improve the quality of the paper. JGR acknowledges support from the Severo Ochoa excellence programme (SEV-2011-0187) postdoctoral fellowship. We are very grateful to Dr. P. Ventura for providing the tables with the surface abundances of his AGB models, and to Dr. C. Morisset for his invaluable help and comments related to the 3Mdb. We also are grateful to A. Karakas from providing the detailed numbers of the models by Fishlock et al. (2014) . We acknowledge fruitful discussions with D. A. García-Hernández, A. Karakas, and M. Lugaro.
Paper: 2018MNRAS.477.1760C (fulltext)
in green, candidate members in light grey, members in red, and members with measured radial velocity in black. Figure 4. Differences between structural parameters obtained from Sérsic fits and isophotal ones. (a) Difference between r e calculated by Calderón et al. ( 2015 ) fitting a Sérsic model and the ‘isophotal’ ∼27 mag arcsec −2 ones, versus absolute and apparent T 1 magnitudes (top and bottom axes), respectively. (b) Same as plot (a) but for the difference in effective surface brightness. It is important to remark that for the two brightest galaxies ( mag), the effective radius results underestimated when using a single component profile (for NGC 3268 the difference is even larger than 1 kpc). A similar (although milder) tendency is present for S0s and cEs. It can be seen that, as expected, the confirmed dEs show mostly positive differences, while the new galaxies (mainly candidates) are the ones showing more negative differences. This effect is less noticeable if we consider a similar difference but for the effective surface brightness (Fig. 4b ). In this case, the confirmed dEs are evenly distributed about zero. 6.2 Geometrical parameters at different galactocentric radii In this section, we analyse the geometrical parameters obtained from the ellipse output for the whole sample, considering the four radial ranges (regions 1 to 4) defined in Section 4 . Fig. 5 shows the distribution of the intensity-weighted average ellipticity 〈ε〉 for the four regions, with a cross-hatched (red) histogram for faint galaxies (dEs and dSph) and an open one for the whole sample. We note that the morphological classification was done by visual inspection of each galaxy, following the criteria used in FS90. That is why we do not establish a magnitude limit (usually set around M B = −18 mag); an overlap in luminosity between bright and dwarf ellipticals can thus be seen. Figure 5. Histograms of the mean weighted ellipticity distributions, cross-hatched in red for dE and dSph and open for the whole sample. Number of galaxies in each region is indicated in parentheses. The histograms of mean ellipticity show flatter (although slightly less extended) distributions, as compared to those obtained by Chaware et al. ( 2014 ) and Hao et al. ( 2006 ), where a main peak at 〈ε〉 ∼0.1 → 0.16 is evident in regions 1 to 4, implying a dominant fraction of nearly round galaxies. Besides a similar low 〈ε〉 peak, a second peak at 〈ε〉 ≈0.3 is also evident in region 1 of our sample. This reflects the fact that most of the brighter galaxies in Antlia are lenticulars (S0), while dwarfs also tend to exhibit relatively large flattenings, despite most of them being classified as dE (dS0s are found only among the brighter dwarfs.). Figs 6 and 7 show the distributions of the weighted mean values of the Fourier coefficients 〈 a 3 / a 〉 and 〈 a 4 / a 〉. As usual, they are reasonably fitted with a single Gaussian centred at zero, except in the outermost region, where the
Paper: 2019A&A...622A..42A (acknowledgments)
We thank Kevin Luhman, Eric Mamajek, and Mark Pecaut for helpful draft comments. We wish to emphasize the pivotal cultural role and reverence that the summit of Maunakea has always had within the indigenous Hawaiian community. We are most fortunate to have the privilege to conduct scientific observations from this mountain. R.A.-T. and M.J. gratefully acknowledge funding from the Knut and Alice Wallenberg foundation. S.D. acknowledges support from the “Progetti Premiali” funding scheme of the Italian Ministry of Education, University, and Research. E. A. is supported by MEXT/JSPS KAKENHI grant No. 17K05399. M.T. is supported by MEXT/JSPS KAKENHI grant Nos. 18H05442, 15H02063, and 22000005.M. H. is supported by the Grant-in-Aid for Scientific Research on Innovative Areas (2302, 23103002) under the Ministry of Education, Culture, Sports, Science and Technology (MEXT) of Japan. This research has benefited from the Montreal Brown Dwarf and Exoplanet Spectral Library, maintained by Jonathan Gagne. This work has 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.
Paper: 2016A&A...589A.107M (acknowledgments)
We are grateful to Javier Manzano-Santamaría for his support on the experiments. Special thanks go to Marcelino Agúndez for useful discussions. This research was financed by the Spanish MINECO under projects AYA2011-29375 and AYA2014-60585-P. R.M.D. benefited from a FPI grant from Spanish MINECO.
Paper: 2016MNRAS.457....2G (acknowledgments)
We are grateful to F. Paresce for carefully reading the paper and useful comments, which improved the final version. We thank the referee for constructive comments and suggestions on the manuscript. This research made use of the NASA/IPAC Infrared Science Archive and Extragalactic Database, which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. Part of this work is based on archival data, software or online services provided by the Scientific Data Center of the Italian Space Agency.
Paper: 2017A&A...601L...5R (acknowledgments)
This work is part of the VIALACTEA Project, a Collaborative Project under Framework Programme 7 of the European Union, funded under Contract # 607380 that is hereby acknowledged.
Paper: 2020A&A...644A.143O (fulltext)
in November 2014 (red; Snodgrass et al. 2016 ). 3.2 Dust coma morphology and activity For each cube in our dataset, we extracted maps over the bandpasses of the V , R , and I Johnson-Cousins filters. All maps in the same bandpass were re-centred and then co-added. The resulting co-added maps are displayed in the top part of Fig. 2 . The dust coma morphology is the same for all three bandpasses. It is asymmetrical, likely due to the presence of dust jets. To investigate the presence of jets further, we divided the dust maps by an azimuthal median profile ( Samarasinha et al. 2013 ). Enhanced maps are displayed on the bottom part of Fig. 2 . Here, we can clearly see two jets, which are most likely the cause of the apparent asymmetry of the dust coma. The first jet is located close to the anti-sunward direction, towards the south-west. The second jet is located about 90° away, towards the south-east. Finally, we see a faint feature towards the sunward direction. Those jets are consistent with what was observed on previous passages and what is reported by Knight et al. (2017) and Snodgrass et al. (2017a ) from observations at the same epoch. They are also consistent with the modelling of the pole orientation and active region location done by Vincent et al. (2013) prior to the Rosetta mission. In addition to the two jets mentioned above, we see an enhancement towards the North-West. This corresponds to the dust trail that was reported to be at least two degrees long at that epoch ( Snodgrass et al. 2017a ; Boehnhardt et al. 2016 ; Knight et al. 2017 ). We do not see changes of the coma morphology over the five nights of our observations, nor over a single night. To constrain the comet activity at that time, we compute the Af ρ value, which is a proxy for dust production, as defined by A’Hearn et al. (1984) . We compute the Af ρ for the V , R , and I bands over a 2500 km physical aperture. We use a 2500 km aperture instead of the more commonly used 10 000 km aperture because the comet signal drops significantly at 10 000 km. We obtain values of 65 ± 4 cm, 75 ± 4 cm, and 82 ± 4 cm in the V , R , and I bands, respectively. Those values have not been corrected for the phase angle effect and are consistent with those reported by Boehnhardt et al. (2016) at the same epoch, and they are comparable (even though slightly lower) to those reported by Knight et al. (2017) once the phase angle effect is taken into account. Using the Af ρ values in the different bands, we can also compute the dust reflectivity gradient defined as ( Jewitt Meech 1986 ): where Af ρ x and the corresponding wavelength λ x are expressed in cm and nm, respectively. For the I – V combination, this gives a reflectivity gradient of 7 ± 1%∕100 nm, while it is of 11 ± 2%∕100 nm for the R – V and 7 ± 1%∕100 nm for the I – R combination. This confirms the trend outlined in Sect. 3.1 of higher reflectivity gradient at lower wavelengths. To check for trends with the aperture size, we
Paper: 2017ApJ...839...48V (acknowledgments)
L.D.V., K.G.S., and R.M. acknowledge partial support from NSF PAARE grant AST-1358862. L.D.V. acknowledges the support of the NASA MUREP Harriett G. Jenkins Fellowship. G.E.S. acknowledges the support of the Vanderbilt Office of the Provost through the Vanderbilt Initiative in Data-intensive Astrophysics (VIDA) fellowship. This paper includes data collected by the Kepler mission. Funding for the Kepler mission is provided by the NASA Science Mission directorate. The data was obtained from the Mikulski Archive for Space Telescopes (MAST). STScI is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555. Support for MAST for non- HST data is provided by the NASA Office of Space Science via grant NNX09AF08G and by other grants and contracts. This work has also made use of data from the European Space Agency (ESA) mission Gaia ( http://www.cosmos.esa.int/gaia ), processed by the Gaia Data Processing and Analysis Consortium (DPAC, http://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 publication makes use of data products from the Two Micron All Sky Survey, which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology, funded by the National Aeronautics and Space Administration and the National Science Foundation. 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. Facilities: Gaia , GALEX , Kepler , WISE .
Paper: 2019ApJ...873...41N (fulltext)
of the field at the cusp with respect to the current sheet axis is zero. The analysis of such irregular cusp structures in the literature were performed either analytically (e.g., Vekstein Priest 1992 , 1993 ; Uzdensky Kulsrud 1997 ; Wiegelmann et al. 1998 , 2000 ) or based on numerical simulations (e.g., Karlický Bárta 2007 ). In all of these investigations, the inner structure of the current distribution was neglected. Figure 1. Sketch of a helmet streamer with cusp point and singular current sheet and zoom to the inner cusp point region within the current sheet. The tiny red box inside the zoom defines the domain of our analysis. In this work, we investigate the internal structure of the current sheet at magnetic cusps. We concentrate on regular, mathematical cusp structures with a finite scale of the current distribution, in contrast to the singular current sheets mentioned before. This means that we are considering regular magnetic flux functions in the very close vicinity of the singular magnetic point, here the cusp point, to characterize the topological connections of the involved physical fields and to allow for transverse components of the magnetic field inside the current sheet (right part of Figure 1 ). 2. Objectives and Methodology The investigation of topological properties not only of the magnetic field , but also of the plasma flow and the non-idealness , requires the violation of ideal Ohm’s law, . The reason is that in 2D, the electric field is , where E z = const in the case of stationary translational invariant MHD. If the electric field component in z -direction does not vanish, i.e., , no regular solutions exist for the velocity field at a magnetic null point, meaning that the velocity field diverges. Therefore, one typically has to use nonideal Ohm’s law,to describe flows around a magnetic null point. In the case of resistive MHD, the nonideal term (or total electric field) is given by where η is the resistivity and is the electric current in the 2D case. In the following, we restrict the analysis to stationary flows. More specifically, we concentrate on the investigation of nonideal Ohm’s law, as it reflects magnetic topology and magnetic flux conservation and their violation. Furthermore, we focus on cusp configurations that are structurally unstable but topologically classifiable magnetic singularities. For structurally stable magnetic null points, an indispensable criterion for magnetic reconnection is that the plasma flow can cross magnetic separatrices, where the plasma flow is usually connected to an X-type stagnation-point flow. Cusp structures are thought to result from reconnection processes. However, as in the strict mathematical sense, no magnetic separatrices exist at or near cusps, the question arises how the plasma streams in the vicinity of such structures. To describe such flows, it is necessary to find solutions of the nonideal Ohm’s law, meaning that the plasma flow and the non-idealness are
Paper: 2016MNRAS.461.3599R (acknowledgments)
We warmly thank the Swift PI Neil Gehrels and his team for approving our observations and scheduling them. We acknowledge with thanks the variable star observations from the AAVSO International Database contributed by observers worldwide and used in this research. We also thank François Teyssier for altering us to the many amateur spectroscopic observations which have been made and we acknowledge and thank François Teyssier, Umberto Sollecchia, Joan Guarro Flo, Jacques Montier, Peter Somogyi, Keith Graham and V Bouttard for use of their spectra. Armagh Observatory is supported by the Northern Ireland Government through the Dept of Culture, Arts and Leisure. GJML and NEN acknowledge support from Argentina grant ANPCYT-PICT 0478/14. GJML and NEN are members of the ‘Carrera del Investigador Cientifico (CIC)’ of CONICET. We thank the referee for a helpful and constructive report.
Paper: 2017ApJ...846...52G (acknowledgments)
We wish to thank The Astrophysical Journal editor Allen Shafter for his promptness in handling the manuscript, and in particular the referee, Ivan Hubeny, for his short, constructive, and encouraging comments and promptness in delivering a report that helped expedite the article. This work was supported by the National Aeronautics and Space Administration (NASA) under grant numbers NNX17AF36G, NNX13AF11G, and NNX13AF12G issued through the Office of Astrophysics Data Analysis Program (ADAP) and grant number NNX13AJ70G issued through the Astrophysics Division Office ( Swift Cycle 8 Guest Investigator Program), all at Villanova University. We have used some of the online data from the AAVSO, and are thankful to the AAVSO and its members worldwide for making this data public and their constant monitoring of cataclysmic variables.
Paper: 2016MNRAS.456.2290T (fulltext)
of the cores, and as such, our results are limited by our model. We note that spdust does not incorporate some important effects, such as internal thermal fluctuations, impulsive excitation due to high-impact ion collisions, and irregular dust grain shapes, all of which produce an increase in the emissivity of the spinning dust emission. Nevertheless, spdust is the only publicly available spinning dust model, and it has been shown to accurately fit observations of spinning dust emission (e.g. Tibbs et al. 2012 ; Planck Collaboration XV 2014 ; Génova-Santos et al. 2015 ). In addition to the limitations of spdust , we are also dependent on the parametrization of our adopted size distribution. For example, we assume that the size distribution varies only with b C , and that the other parameters, such as a 0, i and σ are fixed. Although Weingartner Draine ( 2001 ) were able to fit extinction curves for a range of R V values with these parameters fixed to the values used in this analysis, it is possible that these parameters will vary. For instance, if grain growth is occurring, then this will likely lead to an increase in a 0, i , which would have an impact on the amplitude of the spinning dust emission. However, in this analysis we follow the example of Weingartner Draine ( 2001 ) in assuming that these parameters are fixed, which enables us to compare our constrained value of b C with the value obtained by Li Draine ( 2001 ) for the diffuse ISM. Additionally, varying the electric dipole moment of the grains will also affect the result. Increasing or decreasing this parameter will result in a corresponding increase or decrease in the spinning dust emission. However, as discussed in Section 3.2 , our adopted dipole moment is rather conservative, and any such increase in this value would result in an increase in the predicted spinning dust curves, which would produce a corresponding decrease in the constrained b C values, therefore not affecting the results of the analysis. Throughout this analysis, we assume that all of the cm emission ( S 1 cm observed ) is due to spinning dust emission. However, as mentioned in Section 3 , it is possible that there may be a contribution from magnetic dipole emission. If this is the case, then this will decrease the contribution of spinning dust emission to the total cm emission, thereby further enhancing the observed deficit of very small grains. Therefore, ignoring magnetic dipole emission throughout this analysis is a conservative approach, and does not impact our results. Finally, we stress that this analysis is the first attempt to use spinning dust emission to characterize the properties of interstellar dust grains, and even with these limitations, this work demonstrates the possibilities of this new method, and as such we hope that it will be included in future studies of interstellar dust. 5 CONCLUSIONS By combining 1 cm CARMA measurements, with far-IR Herschel observations, we have constrained the
Paper: 2017MNRAS.468.2713M (acknowledgments)
Acknowledgments This work has been carried out with the financial support of Basic Research Program of the Presidium of the Russian Academy of Sciences Transitional and Explosive Processes in Astrophysics (P-41) and Russian Foundation for Basic Research (grant 16-02-00954). The author thanks the referee for the very useful comments and corrections and L. B. Potapova for the help with the preparation of the manuscript.