Institution
University of Warsaw
Education•Warsaw, Poland•
About: University of Warsaw is a education organization based out in Warsaw, Poland. It is known for research contribution in the topics: Population & Large Hadron Collider. The organization has 20832 authors who have published 56617 publications receiving 1185084 citations. The organization is also known as: Uniwersytet Warszawski & Warsaw University.
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University of Notre Dame1, Massey University2, Massachusetts Institute of Technology3, Goddard Space Flight Center4, Osaka University5, Institut d'Astrophysique de Paris6, University of Warsaw7, Vienna University of Technology8, University of Salerno9, Istituto Nazionale di Fisica Nucleare10, Nagoya University11, University of Auckland12, Vaughn College of Aeronautics and Technology13, Victoria University of Wellington14, University of Canterbury15, University of Toulouse16, European Southern Observatory17, University of Tasmania18, University of Rijeka19, University of St Andrews20, Chungbuk National University21, Space Telescope Science Institute22, Heidelberg University23, Texas A&M University24, Peking University25, Ohio State University26, Korea Astronomy and Space Science Institute27, Harvard University28, University of Concepción29, Las Cumbres Observatory Global Telescope Network30, Queen Mary University of London31, Royal Society32, Qatar Foundation33, Max Planck Society34, Liverpool John Moores University35, Pontifical Catholic University of Chile36, University of Manchester37, University of Hertfordshire38, Centre national de la recherche scientifique39
TL;DR: In this paper, the first microlensing candidate for a free-floating exoplanet-exomoon system, MOA-2011-BLG-262, with a primary lens mass of M host ~ 4 Jupiter masses hosting a sub-Earth mass moon was presented.
Abstract: We present the first microlensing candidate for a free-floating exoplanet-exomoon system, MOA-2011-BLG-262, with a primary lens mass of M host ~ 4 Jupiter masses hosting a sub-Earth mass moon. The argument for an exomoon hinges on the system being relatively close to the Sun. The data constrain the product ML πrel where ML is the lens system mass and πrel is the lens-source relative parallax. If the lens system is nearby (large πrel), then ML is small (a few Jupiter masses) and the companion is a sub-Earth-mass exomoon. The best-fit solution has a large lens-source relative proper motion, μrel = 19.6 ± 1.6 mas yr–1, which would rule out a distant lens system unless the source star has an unusually high proper motion. However, data from the OGLE collaboration nearly rule out a high source proper motion, so the exoplanet+exomoon model is the favored interpretation for the best fit model. However, there is an alternate solution that has a lower proper motion and fits the data almost as well. This solution is compatible with a distant (so stellar) host. A Bayesian analysis does not favor the exoplanet+exomoon interpretation, so Occam's razor favors a lens system in the bulge with host and companion masses of and , at a projected separation of AU. The existence of this degeneracy is an unlucky accident, so current microlensing experiments are in principle sensitive to exomoons. In some circumstances, it will be possible to definitively establish the mass of such lens systems through the microlensing parallax effect. Future experiments will be sensitive to less extreme exomoons.
173 citations
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TL;DR: In this paper, the authors compute the shell correction energy at spherical shape using self-consistent nuclear models: the non-relativistic Skyrme-Hartree-Fock approach and the relativistic mean field model, for a number of parametrizations.
172 citations
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University of Notre Dame1, Lawrence Livermore National Laboratory2, Ohio State University3, University of Warsaw4, Tel Aviv University5, University of Concepción6, University of Cambridge7, Texas A&M University8, Chungbuk National University9, Korea Astronomy and Space Science Institute10, Auckland University of Technology11, Nagoya University12, Massey University13, University of Auckland14, University of Canterbury15, Victoria University of Wellington16, Konan University17, Vaughn College of Aeronautics and Technology18, University of Exeter19, Institut d'Astrophysique de Paris20, European Southern Observatory21, University of Stuttgart22, Ames Research Center23, University of St Andrews24, University of Toulouse25, University of Tasmania26, Liverpool John Moores University27, Las Cumbres Observatory Global Telescope Network28, Dartmouth College29, University of Massachusetts Amherst30
TL;DR: The OGLE-2006-BLG-109Lb,c was the first double planet system discovered with the gravitational microlensing method as mentioned in this paper, which was the only multi-planet system discovered by any method with measured masses for the star and both planets.
Abstract: We present a new analysis of the Jupiter+Saturn analog system, OGLE-2006-BLG-109Lb,c, which was the first double planet system discovered with the gravitational microlensing method. This is the only multi-planet system discovered by any method with measured masses for the star and both planets. In addition to the signatures of two planets, this event also exhibits a microlensing parallax signature and finite source effects that provide a direct measure of the masses of the star and planets, and the expected brightness of the host star is confirmed by Keck AO imaging, yielding masses of , Mb = 231 ± 19 M ⊕, and Mc = 86 ± 7 M ⊕. The Saturn-analog planet in this system had a planetary light-curve deviation that lasted for 11 days, and as a result, the effects of the orbital motion are visible in the microlensing light curve. We find that four of the six orbital parameters are tightly constrained and that a fifth parameter, the orbital acceleration, is weakly constrained. No orbital information is available for the Jupiter-analog planet, but its presence helps to constrain the orbital motion of the Saturn-analog planet. Assuming co-planar orbits, we find an orbital eccentricity of and an orbital inclination of . The 95% confidence level lower limit on the inclination of i > 49° implies that this planetary system can be detected and studied via radial velocity measurements using a telescope of 30 m aperture.
172 citations
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TL;DR: In this paper, ground-based and Swift photometric and spectroscopic observations of the TDE ASASSN-15oi, discovered at the center of 2MASX J20390918-3045201 ($d\simeq216$ Mpc), were presented.
Abstract: We present ground-based and Swift photometric and spectroscopic observations of the tidal disruption event (TDE) ASASSN-15oi, discovered at the center of 2MASX J20390918-3045201 ($d\simeq216$ Mpc) by the All-Sky Automated Survey for SuperNovae (ASAS-SN). The source peaked at a bolometric luminosity of $L\simeq1.9\times10^{44}$ ergs s$^{-1}$ and radiated a total energy of $E\simeq5.0\times10^{50}$ ergs over the $\sim3.5$ months of observations. The early optical/UV emission of the source can be fit by a blackbody with temperature increasing from $T\sim2\times10^4$ K to $T\sim6\times10^4$ K while the luminosity declines from $L\simeq1.9\times10^{44}$ ergs s$^{-1}$ to $L\simeq2.8\times10^{43}$ ergs s$^{-1}$, requiring the photosphere to be shrinking rapidly. The optical/UV luminosity decline is broadly consistent with an exponential decline, $L\propto e^{-t/t_0}$, with $t_0\simeq35$ days. ASASSN-15oi also exhibits roughly constant soft X-ray emission that is significantly weaker than the optical/UV emission. Spectra of the source show broad helium emission lines and strong blue continuum emission in early epochs, although these features fade rapidly and are not present $\sim3$ months after discovery. The early spectroscopic features and color evolution of ASASSN-15oi are consistent with a TDE, but the rapid spectral evolution is unique among optically-selected TDEs.
172 citations
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TL;DR: How a G protein (transducin) docks on to an oligomeric GPCR (rhodopsin) is described, revealing structural details of this critical interface in the signal transduction process.
Abstract: G protein-coupled receptors (GPCRs) are ubiquitous and essential in modulating virtually all physiological processes. These receptors share a similar structural design consisting of the seven-transmembrane α-helical segments. The active conformations of the receptors are stabilized by an agonist and couple to structurally highly conserved heterotrimeric G proteins. One of the most important unanswered questions is how GPCRs couple to their cognate G proteins. Phototransduction represents an excellent model system for understanding G protein signaling, owing to the high expression of rhodopsin in rod photoreceptors and the multidisciplinary experimental approaches used to study this GPCR. Here, we describe how a G protein (transducin) docks on to an oligomeric GPCR (rhodopsin), revealing structural details of this critical interface in the signal transduction process. This conceptual model takes into account recent structural information on the receptor and G protein, as well as oligomeric states of GPCRs.
172 citations
Authors
Showing all 21191 results
Name | H-index | Papers | Citations |
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Alexander Malakhov | 139 | 1486 | 99556 |
Emmanuelle Perez | 138 | 1550 | 99016 |
Piotr Zalewski | 135 | 1388 | 89976 |
Krzysztof Doroba | 133 | 1440 | 89029 |
Hector F. DeLuca | 133 | 1303 | 69395 |
Krzysztof M. Gorski | 132 | 380 | 105912 |
Igor Golutvin | 131 | 1282 | 88559 |
Jan Krolikowski | 131 | 1289 | 83994 |
Michal Szleper | 130 | 1238 | 82036 |
Anatoli Zarubin | 129 | 1204 | 86435 |
Malgorzata Kazana | 129 | 1175 | 81106 |
Artur Kalinowski | 129 | 1162 | 81906 |
Predrag Milenovic | 129 | 1185 | 81144 |
Marcin Konecki | 128 | 1178 | 79392 |
Karol Bunkowski | 128 | 1192 | 79455 |