adsabs/WIESP2022-NER huggingface dataset:
Paper: 2017MNRAS.468.4822L (acknowledgments)
Acknowledgments This work was partially supported by the Consejo Nacional de Investigaciones Cientficas y Tcnicas (CONICET), and the Secretara de Ciencia y Tecnologa, Universidad Nacional de Crdoba, Argentina. Plots were made using r software and post-processed with inkscape . This research has made use of NASAs Astrophysics Data System. The authors would like to thank the anonymous reviewer for their valuable suggestions. Funding for the SDSS and SDSS-II has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, the US Department of Energy, the National Aeronautics and Space Administration, the Japanese Monbukagakusho, the Max Planck Society and the Higher Education Funding Council for England. The SDSS web site is http://www.sdss.org/ . The SDSS is managed by the Astrophysical Research Consortium for the Participating Institutions. The Participating Institutions are the American Museum of Natural History, Astrophysical Institute Potsdam, University of Basel, University of Cambridge, Case Western Reserve University, University of Chicago, Drexel University, Fermilab, the Institute for Advanced Study, the Japan Participation Group, Johns Hopkins University, the Joint Institute for Nuclear Astrophysics, the Kavli Institute for Particle Astrophysics and Cosmology, the Korean Scientist Group, the Chinese Academy of Sciences (LAMOST), Los Alamos National Laboratory, the Max-Planck-Institute for Astronomy (MPIA), the Max-Planck-Institute for Astrophysics (MPA), New Mexico State University, the Ohio State University, the University of Pittsburgh, the University of Portsmouth, Princeton University, the United States Naval Observatory and the University of Washington.
Paper: 2016ApJ...821....1J (acknowledgments)
The authors appreciate the enlightening suggestions from the anonymous referee, which helped to improve the quality of this paper. This work is supported by National Basic Research Program of China (973 Program, grant No. 2015CB857005, grant No. 2013CB834905), the NSFC grant (grant No. 11233002, 11203022, 11421303, 11473025, 11033007), and the SOC program (CHINARE2015-02-03). Funding for SDSS-III has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, and the U.S. Department of Energy Office of Science. The SDSS-III web site 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: 2019MNRAS.483.4742C (acknowledgments)
ACKNOWLEDGEMENTS Parts of this research are supported by the Australian Research Council Centre of Excellence for Gravitational Wave Discovery (OzGrav) (project number CE170100004).
Paper: 2016A&A...587A..64S (fulltext)
sets of transits were found in the Kepler light curve of the target star KOI-1574: one giant-planet candidate at 114 days ( Borucki et al. 2011b , KOI-1574.01), one Saturn-size candidate at 574 days ( Burke et al. 2014 , KOI-1574.02), and two Earth-size candidates at 5.8d and 9d (KOI-1574.03 and KOI-1574.04, respectively; Rowe et al. 2015 ). Only the EGP at 114 days is within our selection criteria. The two large and long-orbital periods objects have already been confirmed thanks to the transiting timing variation analysis performed by Ofir et al. (2014) . However, they reported a different 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
Paper: 2019MNRAS.484.3831B (acknowledgments)
ACKNOWLEDGEMENTS The authors HB, DB, MM, AK, SBP, and PW acknowledges support through the National Research Foundation of South Africa. AK acknowledges the Russian Science Foundation (project no. 14-50-00043). VL and EG acknowledges support of the Development Program of M.V. Lomonosov Moscow State University and the Russian Science Foundation 16-12-00085. MASTER-SAAO is supported by the Russian Foundation for Basic Research (RFBR) 17-52-80133. Some observations reported in this paper were obtained with the South African Large Telescope under programme 2014-2-DDT-002. We thank Prof. Jules Halpern of Columbia University, who kindly obtained a short time series in 2017 March from MDM. We also thank the students of the 2015 Dartmouth Astronomy Foreign Study Program for assistance at the telescope; they are MacKenzie Carlson, Z. Edrei Chua, Robert Cueva, Natalie Drozdoff, John French, Emma Garcia, Zoe Guttendorf, Rachel McKee, Krystyna Miles, Jack Neustadt, Samuel Rosen, Marie Schwalbe, and Nicholas Suntzeff, and graduate assistants Erek Alper and MacKenzie Jones. Finally, we thank the anonymous referee, whose comments and suggestions have lead to greater understanding, and significantly improved the quality of this work.
Paper: 2018A&A...615A.175B (fulltext)
The low-mass inner planets of the 11 archival solar system analogues discussed in Sect. 1 are shown as white circles. It is therefore clear that to achieve higher detection frequencies for terrestrial and super-terrestrial planet at all periods, expecially shorter ones, it is necessary to obtain a higher number of observations per target star and ensure a higher-density sampling. Our observing programme, as noted in Sect. 3 , originally foresaw about 40 measurements per star, a much higher number than the average 27 per star we actually obtained; it can be argued that a number of observations closer to the one originally proposed could push the survey’s detection limits to lower planetary masses, ensuring a better coverage and higher detection frequencies for terrestrial and super-terrestrial additional planets. In fact, analytical expressions for close-in low-mass exoplanets detection threshold found in Narayan et al. (2005) show such a dependence on the number of radial velocity measurements. It will also be important in the near future comparing our results with the similarly produced detection map for the parallel HARPS-N survey mentioned in Sect. 1 . From the overall survey detection map one can finally obtain an estimate for the planetary occurence frequency f p in the presence of a giant outer planet; the probability of obtaining m detection out of a sample of size N is given by the binomial distribution: The choice of distribution is dictated by the small size of our sample (at most N = 20) and has been originally justified in Burgasser et al. (2003) and successfully used in Sozzetti et al. (2009) and Faria et al. (2016) , to name a few. During the analysis of our sample, as detailed in Sect. 4 , we found a single new candidate planet, namely the gas giant HD 50499 c, which due to its estimated minimum orbital period P ≥ 8265.51 days lies outside our considered period range of P ≥ 1 yr. Following a section of the analysis reported in the work of Mayor et al. (2011) , in which the authors estimated the occurrence frequency of stars with at leats one planet in given regions of orbital period and planetary mass, we focus our interest on sub-giant planets with orbital period less than 150 days and M sin i between 10 and 30 M ⊕ , a region for which we are conservatively sensitive to only 50% of our 20-stars sample. Having found no candidate planet falling within this mass-period space, we can only obtain a lower limit of 1− γ for the occurence frequency of low-mass planets in the presence of a known outer giant planet of f p 9.84%, a value we note to be much lower than the 38.8 ± 7.1% reported in Mayor et al. (2011) for stars hosting at least one planet in the same period-mass region. 6. Summary and discussion In this work we report the results of an intense observational campaign conducted using the high-precision HARPS spectrograph on 20 stars, obtaining an average of 27 datapoints per star. The stars in the sample were selected in
Paper: 2016A&A...586A..49B (fulltext)
Table A.1 Linelists for the synthesis of Sr. Notes. The lists include atomic data for Sr from Bautista et al. (2002) and additional lines nearby. Columns represent element line, wavelength, and log() values. Table A.2 Linelists for the synthesis of Zr. Notes. The lists include atomic data for Zr from Ljung et al. (2006) and additional lines nearby. Columns represent element line, wavelength, and log() values. Table A.3 Linelists for the synthesis of La. Notes. The lists include the hfs (when available) of the La in question taken from Ivans et al. (2006) and additional lines nearby. Columns represent element line, wavelength, and log() values. Table A.4 Linelists for the synthesis of Ce. Notes. The lists include atomic data for Ce from Lawler et al. (2009) and additional lines nearby. Columns represent element line, wavelength, and log() values. Table A.5 Linelists for the synthesis of Nd. Notes. The lists include the hfs (when available) of the Nd in question taken from Roederer et al. (2008) and additional lines nearby. Columns represent element line, wavelength, and log() values. Table A.6 Linelists for the synthesis of Sm. Notes. The lists include the hfs (when available) of the Sm in question taken from Lawler et al. (2006) and Roederer et al. (2008) , as well as additional lines nearby. Columns represent element line, wavelength, and log() values. Table A.7 Linelists for the synthesis of Eu ii . Notes. The lists include the hfs of the Eu ii in question taken from Lawler et al. (2001) and additional lines nearby. Columns represent element line, wavelength, and log() values. Appendix B: Solar abundance plots Figures B.1 – B.5 show the synthesis for all the lines analyzed in this work for the solar spectrum from Vesta observed at Magellan in January 2006. Each plot shows (in the bigger panel) the line fitting with the best fit to the observed one and the different abundances in steps of 0.04 dex. In the lower panel, the differences between the observed spectrum and the synthetic one are shown, with the difference with the best fit highlighted. In the small square panel, the values for the different abundances are represented, with the red dot representing the minimum, hence the best fit value for the elemental abundance. Fig. B.1 Solar spectrum taken using asteroid Vesta during the run at Magellan in January 2006. Spectral lines are listed in order of element and wavelength. Chemical elements with all the hfs lines are indicated inside the lines. The different colored lines represent the different synthetic spectra with different abundances in steps of 0.04 dex, while the dots are the observed spectra. The lower panels show the values of differences between the real and synthetic spectra for the synthetic spectra plotted above. The red lines represent the best fit derived from un-normalized , visible in the small plot as a red dot. Here the fits for the Sr line and the five Zr lines are shown. Fig. B.2 As in Fig. B.1 but for the four
Paper: 2015ApJ...806...13M (acknowledgments)
We thank the Wind/ WAVES, SDO /AIA, and STEREO /SECCHI teams for providing data. This research was done as part of the LWS Focused Science Topic, “SEP Variability” supported by NASA grants NNX10AL50A and NNG11PL10A. SOHO is a project of international cooperation between ESA and NASA. The authors thank the anonymous referee for helpful comments.
Paper: 2019ApJ...884..132K (acknowledgments)
We thank the anonymous referee for careful reading and offering constructive comments for improving the paper. S.K. thanks Masanori Nakamura and Keiichi Asada for helpful comments and encouragement. This paper is based on observations carried out with the VLBA. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. This work made use of the Swinburne University of Technology software correlator (Deller et al. 2011 ), developed as part of the Australian Major National Research Facilities Programme and operated under license. This work was done with the contribution of the Italian Ministry of Foreign Affairs and University and Research for the collaboration project between Italy and Japan. This work is partially supported by JSPS KAKENHI grant Nos. 18K03656 (M.K.), 18H03721 (K.N., M.K., K.H.), 24340042 (A.D.), and 25120007 (M.H., K.H., K.A.). K.A. is a Jansky Fellow of the National Radio Astronomy Observatory. The Black Hole Initiative at Harvard University is financially supported by a grant from the John Templeton Foundation. K.A. is financially supported in part by a grant from the National Science Foundation (AST-1614868). G.Y.Z is supported by the Korea Research Fellowship Program through the National Research Foundation of Korea (NRF) funded by the Ministry of Science and ICT (NRF-2015H1D3A1066561). Facility: VLBA.
Paper: 2020ApJ...889..184W (acknowledgments)
Support for this work was provided by NASA grant NNX15AW31G. R.M.W. acknowledges support from NASA grants NNX15AW31G and 80NSSC19K0914, and NSF grant AGS1622352. N.L. acknowledges support from NASA grants NNX15AB87G and NNX13AP52G. C.J.F. was partially supported by the NASA STEREO Quadrature grant. C.L.J., M.A.A., and L.P. acknowledge support from the Natural Sciences and Engineering Research Council of Canada. We would like to thank the STEREO PLASTIC PI for the STEREO He/H data provided for this study. All the data analyzed in this study are publicly available. MESSENGER data are available on the Planetary Data System ( https://pds.jpl.nasa.gov ), while STEREO data are available on the Space Physics Data Facility’s Coordinated Data Analysis Web ( https://cdaweb.sci.gsfc.nasa.gov ).
Paper: 2020A&A...635A..31M (acknowledgments)
Acknowledgements We acknowledge Cloud Academy I 2018 at the Les Houches School of Physics, France, during which this project was kicked off. We thank Maria Steinrueck for the constructive discussions and contribution. Part of this work was supported by the German Deutsche Forschungsgemeinschaft, DFG project number Ts 17/2–1. We are grateful to the anonymous referee for helpful comments and constructive criticism of the manuscript.
Paper: 2015ApJ...811..106H (acknowledgments)
This research was supported by the European Commission funded Research Training Network SOLAIRE. It was also supported by the Research Council of Norway through grants of computing time from the Norwegian Programme for Supercomputing and by the Swiss National Science Foundation under grant No. 153302. The research leading to these results has received funding from the European Research Council under the European Union’s Seventh Framework Programme (FP7/2007-2013)/ERC grant agreement No. 291058 and support by NASA grants NNX08AH45G, NNX08BA99G, NNX11AN98G, NNM07AA01C ( Hinode ), and NNG09FA40C ( IRIS ). To analyze the data we have used IDL and Vapor ( http://www.vapor.ucar.edu ).
Paper: 2020MNRAS.497.2529E (fulltext)
To compute the cross-covariance matrix more accurately, we compute the BFD moments for each image of empty sky. Using the BFD software enables us to properly account for the differing PSFs and world coordinate systems (i.e. registration) of each image. We then compute the empirical cross-covariance matrix of BFD moments, : where ( i, j ) are indexes of the moment element of the covariance matrix, and α and β index are the exposures of this sky patch. The summation is performed over all combinations of images where α ≠ β . We combine data from all 39 Balrog-variant tiles to compute a global cross-covariance matrix for the DES data from empty sky regions. Finally, we test how using the new cross-covariance matrix affects the noise tests described in Section 2.4 . Analogous to χ M , we now define χ MX , which is now calculated using the sum of the shot/read-noise covariance and : where σ M is from the shot/read-noise covariance matrix and σ X is from the cross-covariance matrix . Generalizing to the χ 2 test using arbitrary moments, we have For these tests, we combine moments from all 48 Balrog-injection tiles, and compute the μ and σ of the normalized histogram (as in Fig. 1 ) for each band. We have subtracted the local sky estimate for each postage stamp and included the variance due to that local sky in the flux moment variance term of . In Fig. 6 , we show the σ value for each band/moment combination using and using + . We find general improvement using our globally defined cross-covariance term, with σ lowering from ∼1.12 to ∼1.01 for the flux moment, and dropping to similar levels for the other moments ( σ = 1.026 in the worst case). We report the σ and μ values for all bands in Table 1 . Figure 6. σ of χ M distribution (blue) and χ MX distribution (red) for each BFD moment from all 48 Balrog-injection tiles. Including the cross-covariance matrix brings the σ of the distribution closer to the expected value of 1. The values of σ for each band/moment combination are given in Table 1 . Furthermore, in Fig. 7 , we show the full χ 2 test for M F only and for all four moments of a given band across all 48 Balrog tiles and we report the value in Table 2 . In all bands, we find that when including the cross-covariance matrix that characterizes the US noise, the CDF of the data more closely approaches the χ 2 distribution with the appropriate number of degrees of freedom. The values also reflect the improvement, as they approach the expected value of 1 for M F only and 4 when looking at the vector of four moments. Figure 7. CDF of (blue/light blue) and (red/pink) for the single BFD M F moment and for the four M F , M R , M 1 , and M 2 moments for each band over all 48 Balrog-injection tiles. The χ 2 CDFs with 1 (black dotted line) and 4 degrees of freedom (black dashed line) are plotted for reference. Again, we show that including the cross-covariance term brings the moment distribution closer to expectations. Mean χ 2 values for each
Paper: 2016ApJ...819..129O (acknowledgments)
We thank the anonymous referee for a helpful report, which greatly improved this manuscript. The primary data for this work were obtained with the Hubble Space Telescope operated by AURA, Inc. for NASA under contract NAS5-26555. Furthermore, this work is based in part on observations made with the Spitzer Space Telescope , which is operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. This work is supported by NASA grant HST-GO-13871. Facilities: HST (ACS, WFC3), Spitzer (IRAC).
Paper: 2019MNRAS.490.4382L (acknowledgments)
ACKNOWLEDGEMENTS This work was supported by the National Natural Science Foundation of China (Grant Nos. 11873026, 11703008, 11273014), the Joint Research Fund in Astronomy (Grant No. U1431227) under cooperative agreement between the National Natural Science Foundation of China (NSFC) and Chinese Academy Sciences (CAS), and partly by the Fundamental Research Funds for the Central Universities. The authors thank the chief scientist Qian S. B. of the 1-m telescope and his working group for their kind support and help. 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: 2017A&A...606A..34D (acknowledgments)
The authors would like to thank Vasilis Archontis for his insightful comments and the referee for their comments and suggestions. S.D. acknowledges STFC for support via her studentship. L.v.D.G. is partially funded under STFC consolidated grant number ST/H00260X/1 and the Hungarian Research grant OTKA K-109276. J.E.L. and M.G.L. were funded by NASA’s Heliophysics Supporting Research and Living With a Star Program, and the Chief of Naval Research’s 6.1 program. The cylindrical flux rope simulations we analysed were performed with a grant of computational time from the DoD’s High Performance Computing Program.
Paper: 2017MNRAS.464.4008P (acknowledgments)
We thank Tirthankar Roy Choudhury, Adam Amara, Phil Bull, Girish Kulkarni, Supratik Pal, Sebastian Seehars and Ali Rahmati for useful discussions and comments on the manuscript, and Joel Akeret for help and support with the cosmohammer package. We thank the anonymous referee for a detailed and helpful report that improved the content and presentation. The research of HP is supported by the Tomalla Foundation.