adsabs/WIESP2022-NER huggingface dataset:
Paper: 2019MNRAS.484.5608D (acknowledgments)
ACKNOWLEDGEMENTS This publication was made possible by grants NPRP-X-019-1-006 and NPRP-09-476-1-78 from the Qatar National Research Fund (a member of Qatar Foundation). GD acknowledges Regione Campania for support from POR-FSE Campania 2014-2020. MPGH acknowledges support from the Villum Foundation. Work by C.H. was supported by the grant (2017R1A4A1015178) of National Research Foundation of Korea. This work makes use of observations from the LCOGT network, which includes three ‘SUPAscopes’ owned by the University of St Andrews. The RoboNet programme is an LCOGT Key Project using time allocations from the University of St Andrews, LCOGT and the University of Heidelberg together with time on the Liverpool Telescope through the Science and Technology Facilities Council (STFC), UK. This research has made use of the LCOGT Archive, which is operated by the California Institute of Technology, under contract with the LCO. OGLE Team thanks Profs. M. Kubiak and G. Pietrzyński, former members of the OGLE team, for their contribution to the collection of the OGLE photometric data over the past years. The OGLE project has received funding from the National Science Centre, Poland, grant MAESTRO 2014/14/A/ST9/00121 to AU. LM acknowledges support from the Italian Ministry of Instruction, University and Research (MIUR) through FFABR 2017 fund. LM acknowledges support from the University of Rome Tor Vergata through ‘Mission: Sustainability 2016’ fund. KH acknowledges support from STFC grant ST/R000824/1.
Paper: 2015ApJ...813...96S (acknowledgments)
We are grateful to Ewine van Dishoeck for suggesting this study and we thank her, Simon Bruderer, and François Lique for valuable discussions. We thank the computer and communication department (CCZ) of the Faculty of Science of the Radboud University for computer resources and technical support. The work is supported by The Netherlands Organisation for Scientific Research, NWO, through the Dutch Astrochemistry Network, and in part by the National Science Foundation under grant No. NSF PHY11-25915. N.B. is supported in part by NSF grant PHY-1505557. K.M.W. and P.C.S. acknowledge support from NASA grants NNX12AF42G and NNX13AF42G. I.K. and W.F.T. acknowledge funding from the European Union Seventh Framework Programme FP7-2011 under grant agreement no. 284405.
Paper: 2016MNRAS.458L..54M (fulltext)
in an unbroken sequence lasting for 9.45 h which is slightly longer than Ceres rotational period of 9.074 h. On August 26, we took a second sequence of 29 exposures of 900 s each. The observations started on August 26 at 23:36 ut at the beginning of the night and ended at the set of Ceres on August 27 at 06:49 UT ut (MJD 2457260.9878–2457261.2840) in an uninterrupted sequence lasting 7.25 h, i.e. a bit shorter than a complete rotation. Five exposures were also taken at the end of the night on August 27, when we could shortly open the dome during a pause of bad weather. The journal of the observations together with the relevant quantities are given in Table 1 which is available online. Table 1. Journal of July observations. 1 st column is the time of the start of the exposure in UT. 2 nd column is the time in MJD. 3 rd column is the radial velocity computed by the HARPS pipeline. 4 th column is the radial velocity corrected from the instrumental drift. 5 th column is the BERV of the HARPS pipeline. 6 th column is the exposure time in seconds. 7 th column is the flux weighted mid exposure fraction. 8 th column is the effective mid exposure time. 9 th column is the radial velocity of Ceres with respect to the Sun. 10 th is the radial velocity of the observer relative to Ceres. The full table is available online. Ceres had an APmag of ≈7.5 mag, an angular dimension of 0.69 arcsec and was observable during most of the night. The observations were performed at phase angles of 4.4 and 12.3 in July and August, respectively. At opposition, Ceres becomes slightly brighter due to the Opposition Surge effect, but no radial velocity variations are expected within a single rotational period (Molaro et al. 2015 ). Inspection of the solar activity through the Solar Dynamic Observatory revealed no significant change in the solar activity to induce an important radial velocity change. The solar activity measured from the total sunspot area changed slightly from ≈500 to ≈1250 millionths of solar hemisphere between July 31 July and August 27. However, note that these will introduce a radial velocity offset between the two nights but not a change within one epoch. We used HARPS pipeline to obtain the radial velocities from sunlight spectra which are reported in the third column of online Table 1 . In the HARPS spectrograph, a second fibre supplies simultaneous ThAr spectra that are used to correct for instrumental radial velocity drifts occurring over the night due to residual temperature, pressure or mechanical changes. The radial velocity differences with respect to the previous calibration provide the instrumental drifts of the spectrograph. We are considering the values RV c corrected for instrumental drift and reported in the column 4 of online Table 1 but note that corrections are always below 0.5 m s −1 and do not affect the results. Single observations have S/N ≥ 100 and the error in the radial velocity measurement is lower than 1 m s −1 .
Paper: 2017MNRAS.467.2517S (acknowledgments)
Acknowledgments The work of A.F. Seleznev and the science leave of G. Carraro in Ekaterinburg was supported by Act 211 Government of the Russian Federation, contract No. 02.A03.21.0006 and by the ESO DGDF programme. G. Baume acknowledges support from CONICET (PIP 112-201101-00301) and financial support from the ESO visitor programme that allowed a visit to ESO premises in Chile, where part of this work was done. This publication also made use of data 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. We thank the Centre de Donnes Astronomiques de Strasbourg (CDS), the US Naval Observatory and NASA for the use of their electronic facilities, especially SIMBAD, ViZier and ADS, and the WEBDA data base. This work was based on observations obtained at the Cerro Tololo Inter-American Observatory, Chile, and at ESO Paranal Observatory under programme 292.D-5043.
Paper: 2016A&A...587A..64S (fulltext)
period for the outermost planet of 192 d, i.e. one third of the period found by Burke et al. (2014) . They reported planetary masses for the two giant objects of and . We secured five observations of KOI-1574 with SOPHIE HE. The data have a rms of 12 m s which is compatible with the uncertainties. The bisector and FWHM have rms of 44 m s and 38 m s, respectively. We fitted four circular orbits to the data fixing the orbital ephemeris to the transit ones. For KOI-1574.02, we choose the period of 572 days. We detect a hint of variation for the EGP at 114 days, with an amplitude of m s, and an upper limit of m s within the 99% confidence interval. For the other planets, we find upper limits at the 99% level on their amplitudes of m s, m s, and m s. Assuming a stellar host mass of ( Ofir et al. 2014 ), it gives a mass constraint for the EGP in our sample of ( at the 99% level). This value is fully compatible with the one derived by the transit timing analysis of Ofir et al. (2014) . For the other planet candidates, we find upper limits on the mass at the 99% level of , , and . Assuming that KOI-1574.02 orbits with a period of 192 d, as stated by Ofir et al. (2014) , does not change significantly our constraints on the mass of KOI-1574.01. For the other planets, the upper limits at 99% change to , , and . We conclude that none of these transiting candidates is an eclipsing brown dwarf or low-mass star eclipsing the target star. We confirm they have a mass within the planetary range. Appendix A.35: KOI-1645.01 The giant-planet candidate KOI-1645.01 was found by Burke et al. (2014) with an orbital period of 41 days. We observed it twice with SOPHIE HE and find a clear SB2. We fitted the cross-correlation function with a two-Gaussian profile to derive the RV of both stars. We call star A the one with the deepest line profile and star B the one with the shallowest line profile. The variation of both stars is anti-correlated, which gives a mass ratio of 87.6%. The star A exhibits a RV variation in anti-phase with the Kepler ephemeris, revealing that the secondary eclipse was detected in the light-curve. This candidate is not a transiting planet but a secondary-only EB. Appendix A.36: KOI-1783.01 A giant-planet candidate was found to transit the host star KOI-1783 with a period of 134d by Batalha et al. (2013) . We observed it twice with SOPHIE HE and find no significant RV variation. The bisector and FWHM variation are also compatible with their photon noise. By fitting a circular orbit with no drift at the transit ephemeris, we find an upper limit at the 99% level on the RV amplitude of m s. We derived the stellar atmospheric parameters that are reported in Table B.2 . We find a host mass of , a radius of , and an age of Gyr. Combining the two analyses, we derive an upper limit on the mass of this candidate of , within the 99% confidence interval. We can therefore exclude a star or brown dwarf eclipsing the target star, but we can not firmly
Paper: 2016A&A...589A..29W (fulltext)
(2013) and Jiménez-Serra et al. (2010) have introduced the possibility of low-velocity shocks, which are most likely an effect of large converging flows, such as cloud collision or interaction between two filaments. Jiménez-Serra et al. (2010) consider this possibility for emissions apart from the high-density structures. This could also be a valid possibility for our region, since the spectra from W43 ( Nguyen-Lu’o’ng et al. 2013 ) are, in view of line width and the velocity shift of the SiO line, comparable to those from IRAS 19410 2336. Additionally, the shift in the line peak in the present data lies with a maximum of 6.1 km s (see Table B.1 ) far below the predicted shock velocity for high-velocity shocks ( km s, Gusdorf et al. 2008a , b ). This could be a hint of low-velocity shocks, but it could, as mentioned, also be an effect of the projection in the observed plane and the acceleration of environmental gas. The main reason for Nguyen-Lu’o’ng et al. (2013) considering low-velocity shocks due to large colliding flows was the fact that they observed large SiO structures with relatively uniform emission over the whole area. Again, this is in contrast to our observation that the whole southern part of IRAS 19410 and 2336 lacks SiO emission. Therefore, a collision of flows could again explain the SiO emission in the middle of the region. Still, it cannot explain the only partially present SiO emission in the south or the differences between SiO and CO data. Furthermore, the detection of H emission as a jet shock indicator in the south without any SiO counterpart could not be explained by this. 5. Conclusion After combining the different results, we found that the SiO emission is most likely caused by high-velocity C-type or CJ-type shocks probably from protostellar jets. This explains the emission in the northern part, as well as the observed line widths. The emission in the middle of the region could be a result of decelerated postshock gas due to two or more colliding outflows. The only part of the observation that does not fit this explanation is the missing SiO emission in the southern region. The observed H emission clearly shows shock activity, and the CO data exhibit several bipolar structures. The most valid explanation for us is that there is ongoing jet and outflow activity in the southern part, which is not visible in the SiO data. The missing SiO emission could be a result of the different excitation properties of the molecules and the shock geometry. When the shocks break out of the densest area, as the H data suggest, the density could be too low for SiO to get excited. However, the opposite explanation that SiO is also not visible owing to densities that are too high in the core has to be considered here. Our final conclusion from this observation is that SiO emission has to be used with some caution, because a lot of effects can have an influence on the emission. This is nicely shown by the observed region, since it can be
Paper: 2019MNRAS.490..440L (acknowledgments)
ACKNOWLEDGEMENTS The authors thank the anonymous referee for many constructive comments. 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. This work was supported by the National Research Foundation of Korea (NRF) grant funded by the Korea government (MSIT)(Grant No: NRF-2019R1C1C1005224), Basic Science Research Program through the NRF funded by the Ministry of Education of Korea(Grant No. NRF-2017R1A6A3A03006413), and BK 21 plus program through the NRF funded by the Ministry of Education of Korea. YN, EG, and GR also acknowledge support by the FNRS and by Belspo through the PRODEX contracts.
Paper: 2016A&A...587A..19P (fulltext)
different dependencies on the three stellar parameters. We chose the molecular TiO bands around and Å (- and - electronic transitions, respectively) since these oxide bands are very sensitive to effective temperature, but almost insensitive to surface gravity (Fig. 1 ). For cooler stars, as shown here, a dependence on surface gravity is introduced by the increasing micro-turbulent velocities, which enhance the line width towards lower values (see Wende et al. (2009) for FeH as an example). More sensitive to surface gravity are alkali lines (Fig. 1 ), which show large alterations of their line wings that are due to pressure broadening (in case of the K lines it is more pronounced towards cooler temperatures). We chose the K- and Na-line pairs at around Å and Å, respectively. To determine the metallicity, we can use all these regions as well because the -TiO band and the alkali lines are strongly dependent on this quantity (see Fig. 2 ). Rajpurohit et al. (2014) also used the K- and Na-line pairs because of their sensitivity to gravity and metallicity, as well as several TiO-bands for temperature determination. They also illustrated the dependency on the different stellar parameters. The chosen spectral regions are also affected by lines of the Earth’s atmosphere. Especially the K- and Na-line pairs are contaminated by O2 and H2O bands, respectively. We used masks to exclude the atmospheric lines from the fit. The contamination of the TiO bands around and Å is very weak and can be neglected. The degree of sensitivity on a certain parameter for a particular line (band) also varies. In Fig. 3 we show how the width of a -level in a -map changes with varying effective temperature (i.e. the of the synthetic spectrum from which the -map is produced is varied) for a fixed surface gravity of cgs and metallicity of cgs. The change is also measured in terms of discretion elements in the -maps, since this determines the given resolution (left axis). All investigated regions become less gravity sensitive towards higher , which is probably due to the increasing thermal broadening, which becomes stronger than the pressure broadening (see also Sect. 3.3 ). At this point we have to keep in mind that the sensitivity curves only represent the behaviour for the chosen parameter values. They look different for other metallicities or surface gravities, which are not shown in detail here. Nevertheless, it becomes clear that the combined -map of all regions is the best choice for most temperatures and provides the highest sensitivity. Even though the sensitivity of the K lines is better for most temperatures than the combined one, we would not suggest to use only these lines because the results would then only depend on two lines. Experience in fitting real observations showed that the results deduced from the K lines alone can differ from the combined solution where the latter matches the actual parameters to a higher accuracy. 3.2. <inline-formula
Paper: 2018MNRAS.474.5534O (acknowledgments)
Acknowledgements The authors are grateful to the anonymous referee for careful and critical comments, which helped to improve the manuscript substantially. HVŞ acknowledges support from the Scientific and Technological Research Council of Turkey (TÜBİTAK) through the project grant 1001 - 115F033. EI acknowledges support from the Young Scientist Award Programme BAGEP-2016 of the Science Academy, Turkey, and is grateful to T. Reinhold and R. H. Cameron for useful discussions. GAJH would also like to acknowledge the IDEX initiative at Université Fédérale Toulouse Midi-Pyrénées (UFTMiP) for funding the STEPS programme that enabled regular research visits. This work has made use of the VALD data base, operated at Uppsala University, the Institute of Astronomy RAS in Moscow and the University of Vienna.
Paper: 2016MNRAS.462.2486F (acknowledgments)
We would like to thank the reviewer for comments that improved the clarity of the presentation. DF was supported by the DoD SMART Scholarship. TP was partially supported by the NSF grant AST-1109113 and the DOE grant DE-FG52-09NA29548. This research used resources of the National Energy Research Scientific Computing Center, which is supported by the Office of Science of the US Department of Energy under Contract No. DE-AC02-05CH11231, and the Air Force Research Laboratory. The software used in this work was in part developed by the DOE Flash Center at the University of Chicago. The data analysis was performed in part using the yt Project (Turk et al. 2011 ), and VisIt (Childs et al. 2012 ). This research has made use of NASA's Astrophysics Data System Bibliographic Services.
Paper: 2015MNRAS.447.3498H (acknowledgments)
I thank Long Wang for his interest. The status of the initial conditions in the N -body model emerged after a check instigated by an enquiry from him.
Paper: 2015MNRAS.448.2332P (acknowledgments)
We thank Drs D. Koester and R. D. Rohrmann for the enlightening discussions and useful suggestions throughout this work. IP and SO Kepler are supported by CNPq and FAPERGS-Pronex-Brazil.
Paper: 2016ApJ...823..156Z (acknowledgments)
We acknowledge the anonymous referee for helpful comments and suggestions. This work made use of data supplied by the UK Swift Science Data Centre at the University of Leicester. Our study was supported by the National Basic Research Program of China with Grant No. 2014CB845800 and by the National Natural Science Foundation of China with Grants No. 11473012, No. 11475085, and No. 11275097.
Paper: 2018MNRAS.480.2046G (acknowledgments)
ACKNOWLEDGEMENTS We thank the anonymous referee for insightful comments and constructive suggestions. This research has made use of data, software, and/or web tools obtained from NASAs High Energy Astrophysics Science Archive Research Center ( heasarc ), a service of the Goddard Space Flight Center and the Smithsonian Astrophysical Observatory. This research has made use of the XRT Data Analysis Software ( xrtdas ) and the NuSTAR Data Analysis Software ( nustar-das ) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (Caltech, USA). PG would like to thank IUCAA and BARC for their hospitality. RG would like to thank the IUCAA associateship programme and CSIR, New Delhi (03(1412)/17/EMR-II) for the financial support.
Paper: 2015ApJ...813...22B (acknowledgments)
We are grateful to Daisuke Nagai and Fang Peng for giving us a copy of their Fortran code that we used to reproduce the data in their sedimentation model. We are grateful to the anonymous referee for a thoughtful and detailed report. The suggestion to make a more comprehensive comparison between a homogeneous and a heterogeneous ICM inspired us to produce several new figures and helped us to significantly improve the final version of this manuscript. We acknowledge useful discussions with Daisuke Nagai, Matthew Kunz, Prateek Sharma, Ellen Zweibel, and Ian Parrish during the 3rd ICM Theory and Computation Workshopheld at the Niels Bohr Institute in 2014. We also thank Sagar Chakraborty and Henrik Latter for valuable comments. The research leading to these results has received funding from the European Research Council under the European Union's Seventh Framework Programme (FP/2007-2013) under ERC grant agreement 306614. T.B. also acknowledges support provided by a Lørup Scholar Stipend and M.E.P. also acknowledges support from the Young Investigator Programme of the Villum Foundation.
Paper: 2017MNRAS.469S.276O (acknowledgments)
Acknowledgements OSIRIS was built by a consortium led by the Max-Planck-Institut für Sonnensystemforschung, Göttingen, Germany, in collaboration with Centro di Ateneo di Studi ed Attivit'a Spaziali ‘Giuseppe Colombo’ (CISAS), University of Padova, Italy; the Laboratoire d’Astrophysique de Marseille, France; the Instituto de Astrofísica de Andalucia, Consejo Superior de Investigaciones Científicas (CSIC), Granada, Spain; the Science Support Office of the European Space Agency, Noordwijk, the Netherlands; the Instituto Nacional de Técnica Aeroespacial, Madrid, Spain; the Universidad Politéchnica de Madrid, Spain; the Department of Physics and Astronomy of Uppsala University, Sweden and the Institut für Datentechnik und Kommunikationsnetze der Technischen Universität Braunschweig, Germany. Rosetta is an ESA mission with contributions from its member states and NASA. The support of the national funding agencies of Germany (DLR), France (CNES), Italy (ASI), Spain (MEC), Sweden (SNSB) and the ESA Technical Directorate is gratefully acknowledged. We thank the Rosetta Science Ground Segment at ESAC, the Rosetta Mission Operations Centre at ESOC and the Rosetta Project at ESTEC for their outstanding work enabling the science return of the Rosetta Mission.