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Continuum reverberation mapping of the accretion disks in two Seyfert 1 galaxies

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arXiv 2018年

作者： Fausnaugh, M.M. Starkey, D.A. Horne, Keith Kochanek, C.S. Peterson, B.M. Bentz, M.C. Denney, K.D. Grier, C.J. Grupe, D. Pogge, R.W. Rosa, G.D.E. Adams, S.M. Barth, A.J. Beatty, Thomas G. Bhattacharjee, A. Borman, G.A. Boroson, T.A. Bottorff, M.C. Brown, Jacob E. Brown, Jonathan S. Brotherton, M.S. Coker, C.T. Crawford, S.M. Croxall, K.V. Eftekharzadeh, Sarah Eracleous, Michael Joner, M.D. Henderson, C.B. Holoien, T.W.-S. Hutchison, T. Kaspi, Shai Kim, S. King, Anthea L. Miao, L.I. Lochhaas, Cassandra Zhiyuan, M.A. Macinnis, F. Manne-Nicholas, E.R. Mason, M. Montuori, Carmen Mosquera, Ana Mudd, Dale Musso, R. Nazarov, S.V. Nguyen, M.L. Okhmat, D.N. Onken, Christopher A. Ou-Yang, B. Pancoast, A. Pei, L. Penny, Matthew T. Poleski, Radoslaw Rafter, Stephen Romero-Colmenero, E. Runnoe, Jessie Sand, David J. Schimoia, Jaderson S. Sergeev, S.G. Shappee, B.J. Simonian, Gregory V. Somers, Garrett Spencer, M. Stevens, Daniel J. Tayar, Jamie Treu, T. Valenti, Stefano van Saders, J. Villanueva, S. Villforth, C. Weiss, Yaniv Winkler, H. Zhu, W. Department of Astronomy Ohio State University 140 W 18th Ave ColumbusOH43210 United States MIT Kavli Institute for Astrophysics and Space Research 77 Massachusetts Avenue 37-241 CambridgeMA02139 United States SUPA Physics and Astronomy University of St. Andrews FifeKY16 9SS Scotland United Kingdom Center for Cosmology and AstroParticle Physics Ohio State University 191 West Woodruff Ave ColumbusOH43210 United States Space Telescope Science Institute 3700 San Martin Drive BaltimoreMD21218 United States Department of Physics and Astronomy Georgia State University AtlantaGA30303 United States Illumination Works LLC. 5650 Blazer Parkway Suite 152 DublinOH43017 Department of Astronomy & Astrophysics Pennsylvania State University 525 Davey Laboratory University ParkPA16802 United States Institute for Gravitation and the Cosmos Pennsylvania State University University ParkPA16802 United States Department of Earth and Space Sciences Morehead State University MoreheadKY United States Cahill Center for Astrophysics California Institute of Technology PasadenaCA91125 United States Department of Physics and Astronomy 4129 Frederick Reines Hall University of California IrvineCA92697 United States Center for Exoplanets and Habitable Worlds Pennsylvania State University 525 Davey Lab University ParkPA16802 United States Department of Physics and Astronomy University of Wyoming 1000 E. University Ave LaramieWY United States Department of Biology Geology and Physical Sciences Sul Ross State University WSB 216 Box-64 AlpineTX79832 United States Crimean Astrophysical Observatory P/O Nauchny Crimea298409 Russia Las Cumbres Global Telescope Network 6740 Cortona Drive Suite 102 Santa BarbaraCA93117 United States Fountainwood Observatory Department of Physics FJS 149 Southwestern University 1011 E. University Ave. GeorgetownTX78626 United States Department of Physics and Astronomy University of Missouri Columbia United States South Afr

We present optical continuum lags for two Seyfert 1 galaxies, MCG+08-11-011 and NGC 2617, using monitoring data from a reverberation mapping campaign carried out in 2014. Our light curves span the ugriz filters over four months, with median cadences of 1.0 and 0.6 days for MCG+08-11-011 and NGC 2617, respectively, combined with roughly daily X-ray and near-UV data from Swift for NGC 2617. We find lags consistent with geometrically thin accretion-disk models that predict a lag-wavelength relation of τ ∝ λ4/3. However, the observed lags are larger than predictions based on standard thin-disk theory by factors of 3.3 for MCG+08-11-011 and 2.3 for NGC 2617. These differences can be explained if the mass accretion rates are larger than inferred from the optical luminosity by a factor of 4.3 in MCG+08-11-011 and a factor of 1.3 in NGC 2617, although uncertainty in the SMBH masses determines the significance of this result. While the X-ray variability in NGC 2617 precedes the UV/optical variability, the long 2.6 day lag is problematic for coronal reprocessing models. Copyright © 2018, The Authors. All rights reserved.

关键词： Galaxies

Research and development for HI intensity mapping

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arXiv 2019年

作者： Timbie, Peter Ahmed, Zeeshan Alonso, David Amin, Mustafa A. Ansari, Réza Arena, Evan J. Bandura, Kevin Beardsley, Adam Bull, Philip Castorina, Emanuele Chang, Tzu-Ching Davé, Romeel van Engelen, Alexander Ewall-Wice, Aaron Ferraro, Simone Foreman, Simon Frisch, Josef Green, Daniel Holder, Gilbert Jacobs, Daniel Dillon, Joshua S. Karagiannis, Dionysios Kaurov, Alexander A. Knox, Lloyd Kuhn, Emily Liu, Adrian Ma, Yin-Zhe Masui, Kiyoshi W. McClintock, Thomas Moodley, Kavilan Münchmeyer, Moritz Newburgh, Laura B. Nomerotski, Andrei O'Connor, Paul Obuljen, Andrej Padmanabhan, Hamsa Parkinson, David Perdereau, Olivier Rapetti, David Saliwanchik, Benjamin Sehgal, Neelima Shaw, J. Richard Sheehy, Chris Sheldon, Erin Shirley, Raphael Silverstein, Eva Slatyer, Tracy Slosar, Anže Stankus, Paul Stebbins, Albert Timbie, Peter T. Tucker, Gregory S. Tyndall, William Villaescusa-Navarro, Francisco Wulf, Dallas UW-Madison SLAC National Accelerator Laboratory Menlo ParkCA94025 United States University of Oxford OxfordOX1 3RH United Kingdom Department of Physics & Astronomy Rice University HoustonTX77005 United States Université Paris-Sud LAL UMR 8607 Orsay CedexF-91898 France CNRS/IN2P3 OrsayF-91405 France Brookhaven National Laboratory UptonNY11973 United States Drexel University PhiladelphiaPA19104 United States CSEE West Virginia University MorgantownWV26505 United States Center for Gravitational Waves and Cosmology West Virginia University MorgantownWV26505 United States Arizona State University TempeAZ85287 United States Queen Mary University of London Mile End Road LondonE1 4NS United Kingdom Department of Physics & Astronomy University of the Western Cape Cape Town7535 South Africa Department of Physics University of California Berkeley BerkeleyCA94720 United States Jet Propulsion Laboratory California Institute of Technology PasadenaCA United States University of Edinburgh EdinburghEH8 9YL United Kingdom Canadian Institute for Theoretical Astrophysics University of Toronto TorontoONM5S 3H8 Canada Lawrence Berkeley National Laboratory BerkeleyCA94720 United States University of California San Diego La JollaCA92093 United States Department of Physics University of Illinois at Urbana-Champaign UrbanaIL61801 United States Department of Astronomy University of California Berkeley BerkeleyCA94720 United States Dipartimento di Fisica e Astronomia "G. Galilei" Università degli Studi di Padova via Marzolo 8 PadovaI-35131 Italy Istituto Nazionale di Fisica Nucleare Sezione di Padova via Marzolo 8 PadovaI-35131 Italy Institute for Advanced Study PrincetonNJ08540 United States University of California at Davis DavisCA95616 United States Department of Physics Yale University New HavenCT06520 United States McGill University MontrealQCH3A 2T8 Canada Astrophysics and Cosmology Research Unit School of Chemistry and Phy

Development of the hardware, data analysis, and simulation techniques for large compact radio arrays dedicated to mapping the 21 cm line of neutral hydrogen gas has proven to be more difficult than imagined twenty years ago when such telescopes were first proposed. Despite tremendous technical and methodological advances, there are several outstanding questions on how to optimally calibrate and analyze such data. On the positive side, it has become clear that the outstanding issues are purely technical in nature and can be solved with sufficient development activity. Such activity will enable science across redshifts, from early galaxy evolution in the pre-reionization era to dark energy evolution at low redshift. Copyright © 2019, The Authors. All rights reserved.

关键词： Mapping

Search for gamma-ray emission from Galactic novae with the fermi -LAT

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arXiv 2017年

作者： Franckowiak, A. Jean, P. Wood, M. Cheung, C.C. Buson, S. Deutsches Elektronen Synchrotron DESY ZeuthenD-15738 Germany CNRS IRAP Toulouse Cedex 4F-31028 France GAHEC Université de Toulouse UPS-OMP IRAP Toulouse France W. W. Hansen Experimental Physics Laboratory Kavli Institute for Particle Astrophysics and Cosmology Department of Physics SLAC National Accelerator Laboratory Stanford University StanfordCA94305 United States Space Science Division Naval Research Laboratory WashingtonDC20375-5352 United States NASA Goddard Space Flight Center GreenbeltMD20771 United States NASA Postdoctoral Program Fellow United States

Context. A number of novae have been found to emit high-energy gamma rays (> 100 MeV). However, the origin of this emission is not yet understood. We report on the search for gamma-ray emission from 75 optically-detected Galactic novae in the first 7.4 years of operation of the Fermi Large Area Telescope using the Pass 8 data set. Aims. We compile an optical nova catalog including light curves from various resources and estimate the optical peak time and optical peak magnitude in order to search for gamma-ray emission to test if all novae are gamma-ray emitters. Methods. We repeat the analysis of the six novae previously identified as gamma-ray sources and develop a unified analysis strategy which we then apply to all novae in our catalog. We search for emission in a 15-day time window in two-day steps ranging from 20 days before to 20 days after the optical peak time. We perform a population study with Monte Carlo simulations to set constraints on the properties of the gamma-ray emission of novae. Results. Two new novae candidates have been found at ∼ 2σ global significance. Although these two novae candidates were not detected at a significant level individually, taking them together with the other non-detected novae, we found a sub-threshold nova population with a cumulative 3σ significance. We report the measured gamma-ray flux for detected sources and flux upper limits for novae without significant detection. Our results can be reproduced by several gamma-ray emissivity models (e.g. a power-law distribution with a slope of 2), while a constant emissivity model (i.e. assuming novae are standard candles) can be rejected. Copyright © 2017, The Authors. All rights reserved.

关键词： Gamma rays

Fermi GBM Observations of GRB 150101B: A Second Nearby Event with a Short Hard Spike and a Soft Tail

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arXiv 2018年

作者： Burns, E. Veres, P. Connaughton, V. Racusin, J. Briggs, M.S. Christensen, N. Goldstein, A. Hamburg, R. Kocevski, D. McEnery, J. Bissaldi, E. Dal Canton, T. Cleveland, W.H. Gibby, M.H. Hui, C.M. Von Kienlin, A. Mailyan, B. Paciesas, W.S. Roberts, O.J. Siellez, K. Stanbro, M. Wilson-Hodge, C.A. NASA Postdoctoral Program Fellow Goddard Space Flight Center GreenbeltMD20771 United States Center for Space Plasma and Aeronomic Research University of Alabama in Huntsville HuntsvilleAL35899 United States Science and Technology Institute Universities Space Research Association HuntsvilleAL35805 United States NASA Goddard Space Flight Center GreenbeltMD20771 United States Space Science Department University of Alabama in Huntsville HuntsvilleAL35899 United States Physics and Astronomy Carleton College MN55057 United States Artemis Université Côte d'Azur Observatoire Côte d'Azur CNRS CS 34229 Nice Cedex 4F-06304 France Astrophysics Branch ST12 NASA/Marshall Space Flight Center HuntsvilleAL35812 United States Istituto Nazionale di Fisica Nucleare Sezione di Bari BariI-70126 Italy Dipartimento Interateneo di Fisica Politecnico di Bari Via E. Orabona 4 Bari70125 Italy Jacobs Technology Inc. HuntsvilleAL35805 United States Max-Planck-Institut für Extraterrestrische Physik Giessenbachstrasse 1 Garching85748 Germany Center for Relativistic Astrophysics School of Physics Georgia Institute of Technology AtlantaGA30332 United States

In light of the joint multimessenger detection of a binary neutron star merger as the gamma-ray burst GRB 170817A and in gravitational waves as GW170817, we reanalyze the Fermi Gamma-ray Burst Monitor data of one of the closest short gamma-ray bursts: GRB 150101B. We find this burst is composed of a short hard spike followed by a comparatively long soft tail. This apparent two-component nature is phenomenologically similar to that of GRB 170817A. While GRB 170817A was distinct from the previously known population of short gamma-ray bursts in terms of its prompt intrinsic energetics, GRB 150101B is not. Despite these differences, GRB 150101B can be modeled as a more on-axis version of GRB 170817A. Identifying a similar signature in two of the closest short gamma-ray bursts suggests the soft tail is common, but generally undetectable in more distant events. If so, it will be possible to identify nearby short gamma-ray bursts from the prompt gamma-ray emission alone, aiding the search for kilonovae. Copyright © 2018, The Authors. All rights reserved.

关键词： Stars

Electromagnetic chirps from neutron star-black hole mergers

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arXiv 2017年

作者： Schnittman, Jeremy D. Dal Canton, Tito Camp, Jordan Tsang, David Kelly, Bernard J. NASA Goddard Space Flight Center GreenbeltMD20771 United States Joint Space-Science Institute College ParkMD20742 United States NASA Postdoctoral Program Fellow Goddard Space Flight Center GreenbeltMD20771 United States Department of Astronomy University of Maryland College ParkMD20742 United States CRESST NASA Goddard Space Flight Center GreenbeltMD20771 United States Department of Physics University of Maryland Baltimore County BaltimoreMD21250 United States

We calculate the electromagnetic signal of a gamma-ray flare coming from the surface of a neutron star shortly before merger with a black hole companion. Using a new version of the Monte Carlo radiation transport code Pandurata that incorporates dynamic spacetimes, we integrate photon geodesics from the neutron star surface until they reach a distant observer or are captured by the black hole. The gamma-ray light curve is modulated by a number of relativistic effects, including Doppler beaming and gravitational lensing. Because the photons originate from the inspiraling neutron star, the light curve closely resembles the corresponding gravitational waveform: a chirp signal characterized by a steadily increasing frequency and amplitude. We propose to search for these electromagnetic chirps using matched filtering algorithms similar to those used in LIGO data analysis. Copyright © 2017, The Authors. All rights reserved.

关键词： Stars

Full orbital solution for the binary system in the northern Galactic disc microlensing event Gaia16aye ⋆

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arXiv 2019年

作者： Wyrzykowski, Lukasz Mróz, P. Rybicki, K.A. Gromadzki, M. Kolaczkowski, Z. Zielinski, M. Zielinski, P. Britavskiy, N. Gomboc, A. Sokolovsky, K. Hodgkin, S.T. Abe, L. Aldi, G.F. AlMannaei, A. Altavilla, G. Al Qasim, A. Anupama, G.C. Awiphan, S. Bachelet, E. Bakış, V. Baker, S. Bartlett, S. Bendjoya, P. Benson, K. Bikmaev, I.F. Birenbaum, G. Blagorodnova, N. Blanco-Cuaresma, S. Boeva, S. Bonanos, A.Z. Bozza, V. Bramich, D.M. Bruni, I. Burenin, R.A. Burgaz, U. Butterley, T. Caines, H.E. Caton, D.B. Calchi Novati, S. Carrasco, J.M. Cassan, A. Čepas, V. Cropper, M. Chruslińska, M. Clementini, G. Clerici, A. Conti, D. Conti, M. Cross, S. Cusano, F. Damljanovic, G. Dapergolas, A. D’Ago, G. de Bruijne, J.H.J. Dennefeld, M. Dhillon, V.S. Dominik, M. Dziedzic, J. Erece, O. Eselevich, M.V. Esenoglu, H. Eyer, L. Figuera Jaimes, R. Fossey, S.J. Galeev, A.I. Grebenev, S.A. Gupta, A.C. Gutaev, A.G. Hallakoun, N. Hamanowicz, A. Han, C. Handzlik, B. Haislip, J.B. Hanlon, L. Hardy, L.K. Harrison, D.L. van Heerden, H.J. Hoette, V.L. Horne, K. Hudec, R. Hundertmark, M. Ihanec, N. Irtuganov, E.N. Itoh, R. Iwanek, P. Jovanovic, M.D. Janulis, R. Jelínek, M. Jensen, E. Kaczmarek, Z. Katz, D. Khamitov, I.M. Kilic, Y. Klencki, J. Kolb, U. Kopacki, G. Kouprianov, V.V. Kruszynska, K. Kurowski, S. Latev, G. Lee, C.-H. Leonini, S. Leto, G. Lewis, F. Li, Z. Liakos, A. Littlefair, S.P. Lu, J. Manser, C.J. Mao, S. Maoz, D. Martin-Carrillo, A. Marais, J.P. Maskoliūnas, M. Maund, J.R. Meintjes, P.J. Melnikov, S.S. Ment, K. Mikolajczyk, P. Morrell, M. Mowlavi, N. Moździerski, D. Murphy, D. Nazarov, S. Netzel, H. Nesci, R. Ngeow, C.-C. Norton, A.J. Ofek, E.O. Pakštiene, E. Palaversa, L. Pandey, A. Paraskeva, E. Pawlak, M. Penny, M.T. Penprase, B.E. Piascik, A. Prieto, J.L. Qvam, J.K.T. Ranc, C. Rebassa-Mansergas, A. Reichart, D.E. Reig, P. Rhodes, L. Rivet, J.-P. Rixon, G. Roberts, D. Rosi, P. Russell, D.M. Zanmar Sanchez, R. Scarpetta, G. Seabroke, G. Shappee, B.J. Warsaw University Astronomical Observatory Al. Ujazdowskie 4 Warszawa00-478 Poland Department of Physics Chungbuk National University Cheongju28644 Korea Republic of Sternberg Astronomical Institute Moscow State University Universitetskii pr. 13 Moscow119992 Russia E-38205 La Laguna Tenerife Spain Universidad de La Laguna Dpto. Astrofísica La Laguna TenerifeE-38206 Spain Institute of Astronomy University of Cambridge Madingley Road CambridgeCB3 0HA United Kingdom 00078 Italy Indian Institute of Astrophysics II Block Koramangala Bengaluru560034 India National Astronomical Research Institute of Thailand 260 Moo 4 T. Donkaew A. Mae Rim Chiang Mai50180 Thailand Department of Space Sciences and Technologies Faculty of Science Akdeniz University Antalya07058 Turkey Université Côte d’Azur Observatoire de la Côte d’Azur CNRS Laboratoire Lagrange France School of Physics and Astronomy Tel-Aviv University tel-aviv6997801 Israel Jet Propulsion Laboratory California Institute of Technology 4800 Oak Grove Drive PasadenaCA91109 United States NASA Postdoctoral Program Fellow Harvard-Smithsonian Center for Astrophysics 60 Garden Street CambridgeMA02138 United States Institute of Astronomy and NAO Rozhen BAS 72 Tsarighradsko Shousse Blvd. Sofia1784 Bulgaria National Optical Astronomy Observatory 950 N Cherry Avenue TucsonAZ85719 United States Subaru Telescope National Astronomical Observatory of Japan 650 N Aohoku Place HiloHI96720 United States IAASARS National Observatory of Athens Vas. Pavlou & I. Metaxa Penteli15236 Greece I-84084 Italy Department of Astronomy and Space Sciences Ege University Izmir35100 Turkey Centre for Advanced Instrumentation University of Durham South Road DurhamDH1 3LE United Kingdom c/ Martí i Franquès 1 Barcelona08028 Spain Department of Astrophysics IMAPP Radboud University Nijmegen P.O. Box 9010 Nijmegen6500 GL Netherlands INAF - Osservatorio di Astrofisica e Scienza dello Spazio di Bologna

Gaia16aye was a binary microlensing event discovered in the direction towards the northern Galactic disc and was one of the first microlensing events detected and alerted to by the Gaia space mission. Its light curve exhibited five distinct brightening episodes, reaching up to I=12 mag, and it was covered in great detail with almost 25,000 data points gathered by a network of telescopes. We present the photometric and spectroscopic follow-up covering 500 days of the event evolution. We employed a full Keplerian binary orbit microlensing model combined with the motion of Earth and Gaia around the Sun to reproduce the complex light curve. The photometric data allowed us to solve the microlensing event entirely and to derive the complete and unique set of orbital parameters of the binary lensing system. We also report on the detection of the first-ever microlensing space-parallax between the Earth and Gaia located at L2. The properties of the binary system were derived from microlensing parameters, and we found that the system is composed of two main-sequence stars with masses 0.57±0.05 M and 0.36±0.03 M at 780 pc, with an orbital period of 2.88 years and an eccentricity of 0.30. We also predict the astrometric microlensing signal for this binary lens as it will be seen by Gaia as well as the radial velocity curve for the binary system. Events such as Gaia16aye indicate the potential for the microlensing method of probing the mass function of dark objects, including black holes, in directions other than that of the Galactic bulge. This case also emphasises the importance of long-term time-domain coordinated observations that can be made with a network of heterogeneous telescopes. Copyright © 2019, The Authors. All rights reserved.

关键词： Geometrical optics

A new, long-lived, jupiter mesoscale wave observed at visible wavelengths

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arXiv 2018年

作者： Simon, Amy A. Hueso, Ricardo Iñurrigarro, Peio Sánchez-Lavega, Agustín Morales-Juberías, Raúl Cosentino, Richard Fletcher, Leigh N. Wong, Michael H. Hsu, Andrew I. de Pater, Imke Orton, Glenn S. Colas, François Delcroix, Marc Peach, Damian Gómez-Forrellad, Josep-María NASA Goddard Space Flight Center Solar System Exploration Division 8800 Greenbelt Road GreenbeltMD2077 United States Física Aplicada I Escuela de Ingeniería de Bilbao UPV/EHU Bilbao Spain New Mexico Institute of Technology and Mining 801 Leroy Place SocorroNM8780 United States NASA Postdoctoral Program Fellow Department of Physics & Astronomy University of Leicester University Road LeicesterLE1 7RH United Kingdom University of California at Berkeley Astronomy Department BerkeleyCA947200-3411 United States Jet Propulsion Laboratory California Institute of Technology 4800 Oak Grove Drive PasadenaCA91109 United States IMCCE Observatoire de Paris PSL Research University CNRS-UMR 8028 Sorbonne Universités UPMC Univ. Lille 1 ParisF-75014 France Société Astronomique de France Commission des observations planétaires Tournefeuille France British Astronomical Association Burlington House London United Kingdom Fundació Observatori Esteve Duran Barcelona Spain

Small-scale waves were observed along the boundary between Jupiter’s North Equatorial Belt and North Tropical Zone, ~16.5° N planetographic latitude in Hubble Space Telescope data in 2012 and throughout 2015 to 2018, observable at all wavelengths from the UV to the near IR. At peak visibility, the waves have sufficient contrast (~10%) to be observed from ground-based telescopes. They have a typical wavelength of about 1.2° (1400 km), variable-length wave trains, and westward phase speeds of a few m/s or less. New analysis of Voyager 2 data shows similar wave trains over at least 300 hours. Some waves appear curved when over cyclones and anticyclones, but most are straight, but tilted, shifting in latitude as they pass vortices. Based on their wavelengths, phase speeds, and faint appearance at high-altitude sensitive passbands, the observed NEB waves are consistent with inertia-gravity waves at the 500-mbar pressure level, though formation altitude is not well constrained. Preliminary General Circulation Model simulations generate inertia-gravity waves from vortices interacting with the environment and can reproduce the observed wavelengths and orientations. Several mechanisms can generate these waves, and all may contribute: geostrophic adjustment of cyclones;cyclone/anticyclone interactions;wind interactions with obstructions or heat pulses from convection;or changing vertical wind shear. However, observations also show that the presence of vortices and/or regions of convection are not sufficient by themselves for wave formation, implying that a change in vertical structure may affect their stability, or that changes in haze properties may affect their visibility. Copyright © 2018, The Authors. All rights reserved.

关键词： Storms

Substructures in the Keplerian disc around the O-type (proto)star G17.64+0.16

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arXiv 2019年

作者： Maud, L.T. Cesaroni, R. Kumar, M.S.N. Rivilla, V.M. Ginsburg, A. Klaassen, P.D. Harsono, D. Sánchez-Monge, Á. Ahmadi, A. Allen, V. Beltrán, M.T. Beuther, H. Galván-Madrid, R. Goddi, C. Hoare, M.G. Hogerheijde, M.R. Johnston, K.G. Kuiper, R. Moscadelli, L. Peters, T. Testi, L. van der Tak, F.F.S. de Wit, W.J. European Southern Observatory Karl-Schwarzschild-Str. 2 Garching bei München85748 Germany Leiden Observatory Leiden University PO Box 9513 Leiden2300 RA Netherlands INAF Osservatorio Astrofisico di Arcetri Largo E. Fermi 5 Firenze50125 Italy Instituto de Astrofísica e Ciências do Espa’cco Universidade do Porto CAUP Rua das Estrelas Porto4150–762 Portugal Jansky fellow of the National Radio Astronomy Observatory 1003 Lopezville Road SocorroNM87801 United States UK Astronomy Technology Centre Royal Observatory Edinburgh Blackford Hill EdinburghEH9 3HJ United Kingdom I. Physikalisches Institut der Universität zu Köln Zülpicher Str. 77 Köln50937 Germany Max Planck Institute for Astronomy Königstuhl 17 Heidelberg69117 Germany NASA Postdoctoral Program Fellow NASA Goddard Space Flight Center GreenbeltMD20771 United States Universidad Nacional Autónoma de México Instituto de Radioastronomía y Astrofísica MoreliaMichoacán58089 Mexico Department of Astrophysics IMAPP Radboud University PO Box 9010 Nijmegen6500 GL Netherlands School of Physics and Astronomy University of Leeds LeedsLS2 9JT United Kingdom Anton Pannekoek Institute for Astronomy University of Amsterdam Science Park 904 Amsterdam1098 XH Netherlands Institute of Astronomy and Astrophysics University of Tübingen Auf der Morgenstelle 10 Tübingen72076 Germany Max-Planck-Institut für Astrophysik Karl-Schwarzschild-Str.1 Garching85748 Germany Kapteyn Astronomical Institute University of Groningen Netherlands SRON Landleven 12 Groningen9747 AD Netherlands European Southern Observatory Alónso de Cordova 3107 Vitacura Casilla Santiago de Chile19001 Chile

We present the highest angular resolution (∼20×15 mas - 44×33 au) Atacama Large Millimeter/sub-millimeter Array (ALMA) observations currently possible of the proto-O-star G17.64+0.16 in Band 6. The Cycle 5 observations with baselines out to 16 km probes scales 150 K, this does not preclude that the substructures formed earlier through disc fragmentation. Copyright © 2019, The Authors. All rights reserved.

关键词： Stars

Spitzer opens new path to break classic degeneracy for jupiter-mass microlensing planet OGLE-2017-BLG-1140Lb

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arXiv 2018年

作者： Novati, S. Calchi Skowron, J. Jung, Y.K. Beichman, C. Bryden, G. Carey, S. Gaudi, B.S. Henderson, C.B. Shvartzvald, Y. Yee, J.C. Zhu, W. Udalski, A. Szymanski, M.K. Mroz, P. Poleski, R. Soszinski, I. Kozlowski, S. Pietrukowicz, P. Ulaczyk, K. Pawlak, M. Rybicki, K. Iwanek, P. Albrow, M.D. Chung, S.-J. Gould, A. Han, C. Hwang, K.-H. Ryu, Y.-H. Shin, I.-G. Zang, W. Cha, S.-M. Kim, D.-J. Kim, H.-W. Kim, S.-L. Lee, C.-U. Lee, D.-J. Lee, Y. Park, B.-G. Pogge, R.W. IPAC Caltech Mail Code 100-22 1200 E. California Blvd. PasadenaCA91125 United States Warsaw University Observatory Al. Ujazdowskie 4 Warszawa00-478 Poland Korea Astronomy and Space Science Institute Daejon34055 Korea Republic of NASA Exoplanet Science Institute California Institute of Technology PasadenaCA91125 United States Jet Propulsion Laboratory California Institute of Technology 4800 Oak Grove Drive PasadenaCA91109 United States Spitzer Science Center California Institute of Technology MS 220-6 PasadenaCA United States Department of Astronomy Ohio State University 140 W. 18th Ave. ColumbusOH43210 United States IPAC NExScI Caltech Mail Code 100-22 1200 E. California Blvd. PasadenaCA91125 United States Harvard-Smithsonian Center for Astrophysics 60 Garden St. CambridgeMA02138 United States Canadian Institute for Theoretical Astrophysics University of Toronto 60 St George Street TorontoONM5S3H8 Canada University of Canterbury Department of Physics and Astronomy Private Bag 4800 Christchurch8020 New Zealand Korea University of Science and Technology Daejeon34113 Korea Republic of Max-Planck-Institute for Astronomy Königstuhl 17 Heidelberg69117 Germany Department of Physics Chungbuk National University Cheongju28644 Korea Republic of Physics Department Tsinghua Centre for Astrophysics Tsinghua University Beijing100084 China School of Space Research Kyung Hee University Yongin Kyeonggi17104 Korea Republic of NASA Postdoctoral Program Fellow

We analyze the combined Spitzer and ground-based data for OGLE-2017-BLG-1140 and show that the event was generated by a Jupiter-class (mp 1.6Mjup) planet orbiting a mid-late M dwarf (M 0.2Mo) that lies DLS 1.0 kpc in the foreground of the microlensed, Galactic-bar, source star. The planet-host projected separation is a 1.0AU, i.e., well-beyond the snow line. By measuring the source proper motion μs from ongoing, long-term OGLE imaging, and combining this with the lens-source relative proper motion μrel derived from the microlensing solution, we show that the lens proper motion μl = μrel+μs is consistent with the lens lying in the Galactic disk, although a bulge lens is not ruled out. We show that while the Spitzer and ground-based data are comparably well fitted by planetary (i.e., binary-lens, 2L1S) models and by binary-source (1L2S) models, the combination of Spitzer and ground-based data decisively favor the planetary model. This is a new channel to resolve the 2L1S/1L2S degeneracy, which can be difficult to break in some cases. Copyright © 2018, The Authors. All rights reserved.

关键词： Gravitation