Author
Radek Poleski
Other affiliations: University of Warsaw
Bio: Radek Poleski is an academic researcher from Ohio State University. The author has contributed to research in topics: Gravitational microlensing & Planet. The author has an hindex of 18, co-authored 72 publications receiving 1335 citations. Previous affiliations of Radek Poleski include University of Warsaw.
Papers
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University of Notre Dame1, Massey University2, Goddard Space Flight Center3, Massachusetts Institute of Technology4, 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, Queen Mary University of London30, Las Cumbres Observatory Global Telescope Network31, 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
TL;DR: In this article, the first example of binary microlensing for which the parameter measurements can be verified (or contradicted) by future Doppler observations is presented, made possible by a confluence of two relatively unusual circumstances.
Abstract: We present the first example of binary microlensing for which the parameter measurements can be verified (or contradicted) by future Doppler observations. This test is made possible by a confluence of two relatively unusual circumstances. First, the binary lens is bright enough (I=15.6) to permit Doppler measurements. Second, we measure not only the usual 7 binary-lens parameters, but also the 'microlens parallax' (which yields the binary mass) and two components of the instantaneous orbital velocity. Thus we measure, effectively, 6 'Kepler+1' parameters (two instantaneous positions, two instantaneous velocities, the binary total mass, and the mass ratio). Since Doppler observations of the brighter binary component determine 5 Kepler parameters (period, velocity amplitude, eccentricity, phase, and position of periapsis), while the same spectroscopy yields the mass of the primary, the combined Doppler + microlensing observations would be overconstrained by 6 + (5 + 1) - (7 + 1) = 4 degrees of freedom. This makes possible an extremely strong test of the microlensing solution. We also introduce a uniform microlensing notation for single and binary lenses, we define conventions, summarize all known microlensing degeneracies and extend a set of parameters to describe full Keplerian motion of the binary lenses.
149 citations
Posted Content•
California Institute of Technology1, Las Cumbres Observatory Global Telescope Network2, Goddard Space Flight Center3, Space Telescope Science Institute4, University of Maryland, College Park5, University of Salerno6, Ohio State University7, University of Groningen8, Carnegie Institution for Science9, University of Arizona10, University of California, Berkeley11, University of Texas at Austin12, University of California, Santa Cruz13, University of California, Los Angeles14, Johns Hopkins University Applied Physics Laboratory15, Princeton University16, University of Toronto17, Max Planck Society18, Arizona State University19, Rutgers University20, University of Minnesota21, Gordon and Betty Moore Foundation22, Cornell University23, Stanford University24, University of Cambridge25, University of South Carolina26, Duke University27, University of Utah28, Vanderbilt University29, Johns Hopkins University30, Search for extraterrestrial intelligence31, Stony Brook University32, University of Washington33, Harvard University34
TL;DR: The Wide Field Infrared Survey Telescope (WFIRST) as discussed by the authors is a 2.4m space telescope with a 0.281 deg^2 field of view for near-IR imaging and slitless spectroscopy and a coronagraph designed for > 10^8 starlight suppresion.
Abstract: The Wide Field Infrared Survey Telescope (WFIRST) is a 2.4m space telescope with a 0.281 deg^2 field of view for near-IR imaging and slitless spectroscopy and a coronagraph designed for > 10^8 starlight suppresion. As background information for Astro2020 white papers, this article summarizes the current design and anticipated performance of WFIRST. While WFIRST does not have the UV imaging/spectroscopic capabilities of the Hubble Space Telescope, for wide field near-IR surveys WFIRST is hundreds of times more efficient. Some of the most ambitious multi-cycle HST Treasury programs could be executed as routine General Observer (GO) programs on WFIRST. The large area and time-domain surveys planned for the cosmology and exoplanet microlensing programs will produce extraordinarily rich data sets that enable an enormous range of Archival Research (AR) investigations. Requirements for the coronagraph are defined based on its status as a technology demonstration, but its expected performance will enable unprecedented observations of nearby giant exoplanets and circumstellar disks. WFIRST is currently in the Preliminary Design and Technology Completion phase (Phase B), on schedule for launch in 2025, with several of its critical components already in production.
111 citations
Las Cumbres Observatory Global Telescope Network1, University of Warsaw2, California Institute of Technology3, University of Salerno4, University of Copenhagen5, Ohio State University6, Harvard University7, Heidelberg University8, University of Notre Dame9, University of St Andrews10, Qatar Foundation11, Istituto Nazionale di Fisica Nucleare12, University of Hamburg13, Institut d'Astrophysique de Paris14, Max Planck Society15, Peking University16, Keele University17, Chinese Academy of Sciences18, Korea Astronomy and Space Science Institute19, European Southern Observatory20, Space Telescope Science Institute21, University of Antofagasta22, Pontifical Catholic University of Chile23, Sharif University of Technology24, Aarhus University25, Open University26, Liverpool John Moores University27, University of Warwick28, Nagoya University29, Massey University30, University of Auckland31, Osaka University32, Kyoto Sangyo University33, Vaughn College of Aeronautics and Technology34, Victoria University of Wellington35, Chungbuk National University36
TL;DR: In this paper, the authors reported the detection of a cold Neptune mplanet = 21 ± 2 M⊕ orbiting a 0.38 m⊙ M dwarf lying 2.5-3.3 kpc toward the Galactic center as part of a campaign combining ground-based and Spitzer observations.
Abstract: We report the detection of a cold Neptune mplanet = 21 ± 2 M⊕ orbiting a 0.38 M⊙ M dwarf lying 2.5–3.3 kpc toward the Galactic center as part of a campaign combining ground-based and Spitzer observations to measure the Galactic distribution of planets. This is the first time that the complex real-time protocols described by Yee et al., which aim to maximize planet sensitivity while maintaining sample integrity, have been carried out in practice. Multiple survey and follow up teams successfully combined their efforts within the framework of these protocols to detect this planet. This is the second planet in the Spitzer Galactic distribution sample. Both are in the near to mid-disk and are clearly not in the Galactic bulge.
103 citations
Ohio State University1, University of Warsaw2, Chungbuk National University3, Harvard University4, University of Cambridge5, University of Concepción6, Auckland University of Technology7, University of Canterbury8, Texas A&M University9, Korea Astronomy and Space Science Institute10, Nagoya University11, University of Notre Dame12, Massey University13, University of Auckland14, Osaka University15, University of British Columbia16, Vaughn College of Aeronautics and Technology17, Victoria University of Wellington18, Kyoto Sangyo University19, Tel Aviv University20
TL;DR: In this paper, a cold terrestrial planet orbiting one member of a binary star system was detected using gravitational microlensing, and the planet has low mass (twice Earth's) and lies projected at ~0.8 astronomical units (AU) from its host star, about the distance between Earth and the Sun.
Abstract: Using gravitational microlensing, we detected a cold terrestrial planet orbiting one member of a binary star system. The planet has low mass (twice Earth’s) and lies projected at ~0.8 astronomical units (AU) from its host star, about the distance between Earth and the Sun. However, the planet’s temperature is much lower,
98 citations
Cited by
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TL;DR: The Astropy project as discussed by the authors is an open-source and openly developed Python packages that provide commonly-needed functionality to the astronomical community, including the core package Astropy, which serves as the foundation for more specialized projects and packages.
Abstract: The Astropy project supports and fosters the development of open-source and openly-developed Python packages that provide commonly-needed functionality to the astronomical community. A key element of the Astropy project is the core package Astropy, which serves as the foundation for more specialized projects and packages. In this article, we provide an overview of the organization of the Astropy project and summarize key features in the core package as of the recent major release, version 2.0. We then describe the project infrastructure designed to facilitate and support development for a broader ecosystem of inter-operable packages. We conclude with a future outlook of planned new features and directions for the broader Astropy project.
2,286 citations
Kavli Institute for Theoretical Physics1, Polish Academy of Sciences2, University of California, Santa Cruz3, University of California, Santa Barbara4, Princeton University5, York University6, Harvard University7, University of Amsterdam8, State University of New York at Oswego9, Northwestern University10, University of Liège11, University of Wisconsin-Madison12, University of Wisconsin–Eau Claire13, Arizona State University14, California Institute of Technology15
TL;DR: In this paper, the capabilities of the open-knowledge software instrument Modules for Experiments in Stellar Astrophysics (MESA) have been updated to improve numerical energy conservation capabilities, including during mass changes.
Abstract: We update the capabilities of the open-knowledge software instrument Modules for Experiments in Stellar Astrophysics (MESA). RSP is a new functionality in MESAstar that models the nonlinear radial stellar pulsations that characterize RR Lyrae, Cepheids, and other classes of variable stars. We significantly enhance numerical energy conservation capabilities, including during mass changes. For example, this enables calculations through the He flash that conserve energy to better than 0.001%. To improve the modeling of rotating stars in MESA, we introduce a new approach to modifying the pressure and temperature equations of stellar structure, as well as a formulation of the projection effects of gravity darkening. A new scheme for tracking convective boundaries yields reliable values of the convective core mass and allows the natural emergence of adiabatic semiconvection regions during both core hydrogen- and helium-burning phases. We quantify the parallel performance of MESA on current-generation multicore architectures and demonstrate improvements in the computational efficiency of radiative levitation. We report updates to the equation of state and nuclear reaction physics modules. We briefly discuss the current treatment of fallback in core-collapse supernova models and the thermodynamic evolution of supernova explosions. We close by discussing the new MESA Testhub software infrastructure to enhance source code development.
601 citations
TL;DR: In this article, the fundamental concepts of micro-lensing planet searches and their practical application are discussed and the strengths and peculiarities of the method flow from the basic manner in which planets are discovered.
Abstract: Unlike most other planet-detection techniques, gravitational microlensing does not rely on detection of photons from either the host or the planet. Rather, planets are discovered by their gravitational perturbation of light from a more distant source. I review the fundamental concepts of microlensing planet searches and discuss their practical application. I show how the strengths and peculiarities of the method flow from the basic manner in which planets are discovered. In particular, microlensing is sensitive to very low-mass planets on wide orbits and free-floating planets, and can be used to search for planets orbiting host stars with a broad range of masses and Galactocentric distances. However, microlensing events are rare and cannot be predicted in advance, the majority of the host stars are extremely faint, and the planetary signals typically last less than a day. These strengths motivate microlensing searches as powerful, complementary probes of unexplored parameter space that have already provid...
331 citations
01 Jan 1981
TL;DR: In this article, the authors provide an overview of economic analysis techniques and their applicability to software engineering and management, including the major estimation techniques available, the state of the art in algorithmic cost models, and the outstanding research issues in software cost estimation.
Abstract: This paper summarizes the current state of the art and recent trends in software engineering economics. It provides an overview of economic analysis techniques and their applicability to software engineering and management. It surveys the field of software cost estimation, including the major estimation techniques available, the state of the art in algorithmic cost models, and the outstanding research issues in software cost estimation.
283 citations
Max Planck Society1, Carnegie Institution for Science2, Massachusetts Institute of Technology3, California Institute of Technology4, University of Arizona5, Lawrence Berkeley National Laboratory6, Space Telescope Science Institute7, University of California, Santa Barbara8, University of Hawaii9, Durham University10
TL;DR: In this article, the authors proposed the Cosmic Dawn project, which used the ESO Telescopes at the La Silla Paranal Observatory (ESO-Paral Observatory).
Abstract: ERC grant "Cosmic Dawn"; DFG [1573]; National Aeronautics and Space Administration through the Planetary Science Division of the NASA Science Mission Directorate [NNX08AR22G]; National Science Foundation [AST-1238877]; ESO Telescopes at the La Silla Paranal Observatory [092.A-0339(A), 092.A-0150(A), 092.A-0150(B), 093.A-0863(A), 095.A-9001(A), 095.A-0375(A), 095.A-0535(A), 095.A-0535(B), 096.A-0420(A), 096.A-9001(A), 097.A-9001(A), 097.A-0094(A), 097.A-0094(B)]; Leibniz Prize (DFG grant) [HA 1850/28-1]; W. M. Keck Foundation; NFS [AST-1109915]; NSF Telescope System Instrumentation Program (TSIP); Ohio Board of Regents; Ohio State University Office of Research; NSF [AST-9987045]; INSU/CNRS (France); MPG (Germany); IGN (Spain); National Aeronautics and Space Administration
271 citations