A Guide to Video Astrometry
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ESO's VLT Sphere and DAMIT
ESO’s VLT Sphere and DAMIT ESO’s VLT SPHERE (using adaptive optics) and Joseph Durech (DAMIT) have a program to observe asteroids and collect light curve data to develop rotating 3D models with respect to time. Up till now, due to the limitations of modelling software, only convex profiles were produced. The aim is to reconstruct reliable nonconvex models of about 40 asteroids. Below is a list of targets that will be observed by SPHERE, for which detailed nonconvex shapes will be constructed. Special request by Joseph Durech: “If some of these asteroids have in next let's say two years some favourable occultations, it would be nice to combine the occultation chords with AO and light curves to improve the models.” 2 Pallas, 7 Iris, 8 Flora, 10 Hygiea, 11 Parthenope, 13 Egeria, 15 Eunomia, 16 Psyche, 18 Melpomene, 19 Fortuna, 20 Massalia, 22 Kalliope, 24 Themis, 29 Amphitrite, 31 Euphrosyne, 40 Harmonia, 41 Daphne, 51 Nemausa, 52 Europa, 59 Elpis, 65 Cybele, 87 Sylvia, 88 Thisbe, 89 Julia, 96 Aegle, 105 Artemis, 128 Nemesis, 145 Adeona, 187 Lamberta, 211 Isolda, 324 Bamberga, 354 Eleonora, 451 Patientia, 476 Hedwig, 511 Davida, 532 Herculina, 596 Scheila, 704 Interamnia Occultation Event: Asteroid 10 Hygiea – Sun 26th Feb 16h37m UT The magnitude 11 asteroid 10 Hygiea is expected to occult the magnitude 12.5 star 2UCAC 21608371 on Sunday 26th Feb 16h37m UT (= Mon 3:37am). Magnitude drop of 0.24 will require video. DAMIT asteroid model of 10 Hygiea - Astronomy Institute of the Charles University: Josef Ďurech, Vojtěch Sidorin Hygiea is the fourth-largest asteroid (largest is Ceres ~ 945kms) in the Solar System by volume and mass, and it is located in the asteroid belt about 400 million kms away. -
The Impact Crater at the Origin of the Julia Family Detected with VLT/SPHERE??,?? P
A&A 618, A154 (2018) Astronomy https://doi.org/10.1051/0004-6361/201833477 & © ESO 2018 Astrophysics The impact crater at the origin of the Julia family detected with VLT/SPHERE??,?? P. Vernazza1, M. Brož2, A. Drouard1, J. Hanuš2, M. Viikinkoski3, M. Marsset4, L. Jorda1, R. Fetick1, B. Carry5, F. Marchis6, M. Birlan7, T. Fusco1, T. Santana-Ros8, E. Podlewska-Gaca8,9, E. Jehin10, M. Ferrais10, P. Bartczak8, G. Dudzinski´ 8, J. Berthier7, J. Castillo-Rogez11, F. Cipriani12, F. Colas7, C. Dumas13, J. Durechˇ 2, M. Kaasalainen3, A. Kryszczynska8, P. Lamy1, H. Le Coroller1, A. Marciniak8, T. Michalowski8, P. Michel5, M. Pajuelo7,14, P. Tanga5, F. Vachier7, A. Vigan1, B. Warner15, O. Witasse12, B. Yang16, E. Asphaug17, D. C. Richardson18, P. Ševecekˇ 2, M. Gillon10, and Z. Benkhaldoun19 1 Aix-Marseille Université, CNRS, LAM (Laboratoire d’Astrophysique de Marseille), Marseille, France e-mail: [email protected] 2 Institute of Astronomy, Charles University, Prague, V Holešovickᡠch 2, 18000, Prague 8, Czech Republic 3 Department of Mathematics, Tampere University of Technology, PO Box 553, 33101 Tampere, Finland 4 Astrophysics Research Centre, Queen’s University Belfast, BT7 1NN, UK 5 Université Côte d’Azur, Observatoire de la Côte d’Azur, CNRS, Laboratoire Lagrange, 06304 Nice Cedex 4, France 6 SETI Institute, Carl Sagan Center, 189 Bernado Avenue, Mountain View CA 94043, USA 7 IMCCE, Observatoire de Paris, 77 avenue Denfert-Rochereau, 75014 Paris Cedex, France 8 Astronomical Observatory Institute, Faculty of Physics, Adam Mickiewicz University, -
The Minor Planet Bulletin
THE MINOR PLANET BULLETIN OF THE MINOR PLANETS SECTION OF THE BULLETIN ASSOCIATION OF LUNAR AND PLANETARY OBSERVERS VOLUME 36, NUMBER 3, A.D. 2009 JULY-SEPTEMBER 77. PHOTOMETRIC MEASUREMENTS OF 343 OSTARA Our data can be obtained from http://www.uwec.edu/physics/ AND OTHER ASTEROIDS AT HOBBS OBSERVATORY asteroid/. Lyle Ford, George Stecher, Kayla Lorenzen, and Cole Cook Acknowledgements Department of Physics and Astronomy University of Wisconsin-Eau Claire We thank the Theodore Dunham Fund for Astrophysics, the Eau Claire, WI 54702-4004 National Science Foundation (award number 0519006), the [email protected] University of Wisconsin-Eau Claire Office of Research and Sponsored Programs, and the University of Wisconsin-Eau Claire (Received: 2009 Feb 11) Blugold Fellow and McNair programs for financial support. References We observed 343 Ostara on 2008 October 4 and obtained R and V standard magnitudes. The period was Binzel, R.P. (1987). “A Photoelectric Survey of 130 Asteroids”, found to be significantly greater than the previously Icarus 72, 135-208. reported value of 6.42 hours. Measurements of 2660 Wasserman and (17010) 1999 CQ72 made on 2008 Stecher, G.J., Ford, L.A., and Elbert, J.D. (1999). “Equipping a March 25 are also reported. 0.6 Meter Alt-Azimuth Telescope for Photometry”, IAPPP Comm, 76, 68-74. We made R band and V band photometric measurements of 343 Warner, B.D. (2006). A Practical Guide to Lightcurve Photometry Ostara on 2008 October 4 using the 0.6 m “Air Force” Telescope and Analysis. Springer, New York, NY. located at Hobbs Observatory (MPC code 750) near Fall Creek, Wisconsin. -
Earth and Planetary Science Letters 490 (2018) 122–131
Earth and Planetary Science Letters 490 (2018) 122–131 Contents lists available at ScienceDirect Earth and Planetary Science Letters www.elsevier.com/locate/epsl Cosmic history and a candidate parent asteroid for the quasicrystal-bearing meteorite Khatyrka ∗ Matthias M.M. Meier a, , Luca Bindi b,c, Philipp R. Heck d, April I. Neander e, Nicole H. Spring f,g, My E.I. Riebe a,1, Colin Maden a, Heinrich Baur a, Paul J. Steinhardt h, Rainer Wieler a, Henner Busemann a a Institute of Geochemistry and Petrology, ETH Zurich, Zurich, Switzerland b Dipartimento di Scienze della Terra, Università di Firenze, Florence, Italy c CNR-Istituto di Geoscienze e Georisorse, Sezione di Firenze, Florence, Italy d Robert A. Pritzker Center for Meteoritics and Polar Studies, Field Museum of Natural History, Chicago, USA e Department of Organismal Biology and Anatomy, University of Chicago, Chicago, USA f School of Earth and Environmental Sciences, University of Manchester, Manchester, UK g Department of Earth and Atmospheric Sciences, University of Alberta, Edmonton, Canada h Department of Physics, and Princeton Center for Theoretical Science, Princeton University, Princeton, USA a r t i c l e i n f o a b s t r a c t Article history: The unique CV-type meteorite Khatyrka is the only natural sample in which “quasicrystals” and associated Received 6 October 2017 crystalline Cu, Al-alloys, including khatyrkite and cupalite, have been found. They are suspected to Received in revised form 11 March 2018 have formed in the early Solar System. To better understand the origin of these exotic phases, and Accepted 13 March 2018 the relationship of Khatyrka to other CV chondrites, we have measured He and Ne in six individual, Available online 22 March 2018 ∼40–μm-sized olivine grains from Khatyrka. -
The Orbital Evolution of Asteroid 367943 Duende (2012 Da14) Under Yarkovsky Effect Influence and Its Implications for Collision with the Earth
Journal of Engineering Science and Technology Special Issue on AASEC’2016, October (2017) 42 - 52 © School of Engineering, Taylor’s University THE ORBITAL EVOLUTION OF ASTEROID 367943 DUENDE (2012 DA14) UNDER YARKOVSKY EFFECT INFLUENCE AND ITS IMPLICATIONS FOR COLLISION WITH THE EARTH JUDHISTIRA ARIA UTAMA1,2,*, TAUFIQ HIDAYAT3, UMAR FAUZI4 1Astronomy Post Graduate Study Program, Institut Teknologi Bandung, Jl. Ganesha 10, Bandung 40132, Indonesia 2Physics Education Department, Universitas Pendidikan Indonesia, Jl. Dr. Setiabudhi 229, Bandung, 40154, Indonesia 3Astronomy Research Division, Institut Teknologi Bandung, Jl. Ganesha 10, Bandung 40132, Indonesia 4Geophysics & Complex System Research Division, Institut Teknologi Bandung, Jl. Ganesha 10, Bandung 40132, Indonesia *Corresponding Author: [email protected] Abstract Asteroid 367943 Duende (2012 DA14) holds the record as the one of Aten subpopulation with H 24 that had experienced deep close encounter event to the Earth (0.09x Earth-Moon distance) as informed in NASA website. In this work, we studied the orbital evolution of 120 asteroid clones and the nominal up to 5 Megayears (Myr) in the future using Swift integrator package with and without the Yarkovsky effect inclusion. At the end of orbital integration with both integrators, we found as many as 17 asteroid clones end their lives as Earth impactor. The prediction of maximum semimajor axis drift for this subkilometer-sized asteroid from diurnal and seasonal variants of Yarkovsky effect was 9.0×10-3 AU/Myr and 2.6×10-4 AU/Myr, respectively. By using the MOID (Minimum Orbital Intersection Distance) data set calculated from our integrators of entire clones and nominal asteroids, we obtained the value of impact rate with the Earth of 2.35×10-7 per year (with Yarkovsky effect) and 2.37×10-7 per year (without Yarkovsky effect), which corresponds to a mean lifetime of 4.25 Myr and 4.22 Myr, respectively. -
Aqueous Alteration on Main Belt Primitive Asteroids: Results from Visible Spectroscopy1
Aqueous alteration on main belt primitive asteroids: results from visible spectroscopy1 S. Fornasier1,2, C. Lantz1,2, M.A. Barucci1, M. Lazzarin3 1 LESIA, Observatoire de Paris, CNRS, UPMC Univ Paris 06, Univ. Paris Diderot, 5 Place J. Janssen, 92195 Meudon Pricipal Cedex, France 2 Univ. Paris Diderot, Sorbonne Paris Cit´e, 4 rue Elsa Morante, 75205 Paris Cedex 13 3 Department of Physics and Astronomy of the University of Padova, Via Marzolo 8 35131 Padova, Italy Submitted to Icarus: November 2013, accepted on 28 January 2014 e-mail: [email protected]; fax: +33145077144; phone: +33145077746 Manuscript pages: 38; Figures: 13 ; Tables: 5 Running head: Aqueous alteration on primitive asteroids Send correspondence to: Sonia Fornasier LESIA-Observatoire de Paris arXiv:1402.0175v1 [astro-ph.EP] 2 Feb 2014 Batiment 17 5, Place Jules Janssen 92195 Meudon Cedex France e-mail: [email protected] 1Based on observations carried out at the European Southern Observatory (ESO), La Silla, Chile, ESO proposals 062.S-0173 and 064.S-0205 (PI M. Lazzarin) Preprint submitted to Elsevier September 27, 2018 fax: +33145077144 phone: +33145077746 2 Aqueous alteration on main belt primitive asteroids: results from visible spectroscopy1 S. Fornasier1,2, C. Lantz1,2, M.A. Barucci1, M. Lazzarin3 Abstract This work focuses on the study of the aqueous alteration process which acted in the main belt and produced hydrated minerals on the altered asteroids. Hydrated minerals have been found mainly on Mars surface, on main belt primitive asteroids and possibly also on few TNOs. These materials have been produced by hydration of pristine anhydrous silicates during the aqueous alteration process, that, to be active, needed the presence of liquid water under low temperature conditions (below 320 K) to chemically alter the minerals. -
Cosmic History and a Candidate Parent Asteroid for the Quasicrystal-Bearing Meteorite Khatyrka
COSMIC HISTORY AND A CANDIDATE PARENT ASTEROID FOR THE QUASICRYSTAL-BEARING METEORITE KHATYRKA Matthias M. M. Meier1*, Luca Bindi2,3, Philipp R. Heck4, April I. Neander5, Nicole H. Spring6,7, My E. I. Riebe1,8, Colin Maden1, Heinrich Baur1, Paul J. Steinhardt9, Rainer Wieler1 and Henner Busemann1 1Institute of Geochemistry and Petrology, ETH Zurich, Zurich, Switzerland. 2Dipartimento di Scienze della Terra, Università di Firenze, Florence, Italy. 3CNR-Istituto di Geoscienze e Georisorse, Sezione di Firenze, Florence, Italy. 4Robert A. Pritzker Center for Meteoritics and Polar Studies, Field Museum of Natural History, Chicago, USA. 5De- partment of Organismal Biology and Anatomy, University of Chicago, Chicago, USA. 6School of Earth and Environ- mental Sciences, University of Manchester, Manchester, UK. 7Department of Earth and Atmospheric Sciences, Uni- versity of Alberta, Edmonton, Canada. 8Current address: Department of Terrestrial Magnetism, Carnegie Institution of Washington, Washington, USA. 9Department of Physics, and Princeton Center for Theoretical Science, Princeton University, Princeton, USA. *corresponding author: [email protected]; (office phone: +41 44 632 64 53) Submitted to Earth and Planetary Science Letters. Abstract The unique CV-type meteorite Khatyrka is the only natural sample in which “quasicrystals” and associated crystalline Cu,Al-alloys, including khatyrkite and cupalite, have been found. They are suspected to have formed in the early Solar System. To better understand the origin of these ex- otic phases, and the relationship of Khatyrka to other CV chondrites, we have measured He and Ne in six individual, ~40-μm-sized olivine grains from Khatyrka. We find a cosmic-ray exposure age of about 2-4 Ma (if the meteoroid was <3 m in diameter, more if it was larger). -
(2000) Forging Asteroid-Meteorite Relationships Through Reflectance
Forging Asteroid-Meteorite Relationships through Reflectance Spectroscopy by Thomas H. Burbine Jr. B.S. Physics Rensselaer Polytechnic Institute, 1988 M.S. Geology and Planetary Science University of Pittsburgh, 1991 SUBMITTED TO THE DEPARTMENT OF EARTH, ATMOSPHERIC, AND PLANETARY SCIENCES IN PARTIAL FULFILLMENT OF THE REQUIREMENTS FOR THE DEGREE OF DOCTOR OF PHILOSOPHY IN PLANETARY SCIENCES AT THE MASSACHUSETTS INSTITUTE OF TECHNOLOGY FEBRUARY 2000 © 2000 Massachusetts Institute of Technology. All rights reserved. Signature of Author: Department of Earth, Atmospheric, and Planetary Sciences December 30, 1999 Certified by: Richard P. Binzel Professor of Earth, Atmospheric, and Planetary Sciences Thesis Supervisor Accepted by: Ronald G. Prinn MASSACHUSES INSTMUTE Professor of Earth, Atmospheric, and Planetary Sciences Department Head JA N 0 1 2000 ARCHIVES LIBRARIES I 3 Forging Asteroid-Meteorite Relationships through Reflectance Spectroscopy by Thomas H. Burbine Jr. Submitted to the Department of Earth, Atmospheric, and Planetary Sciences on December 30, 1999 in Partial Fulfillment of the Requirements for the Degree of Doctor of Philosophy in Planetary Sciences ABSTRACT Near-infrared spectra (-0.90 to ~1.65 microns) were obtained for 196 main-belt and near-Earth asteroids to determine plausible meteorite parent bodies. These spectra, when coupled with previously obtained visible data, allow for a better determination of asteroid mineralogies. Over half of the observed objects have estimated diameters less than 20 k-m. Many important results were obtained concerning the compositional structure of the asteroid belt. A number of small objects near asteroid 4 Vesta were found to have near-infrared spectra similar to the eucrite and howardite meteorites, which are believed to be derived from Vesta. -
Hered in These Proceedings with the Aim to Keep Track of These Very Interesting Days
Proceedings of GAIA-FUN-SSO 2014 Third “Gaia Follow-up Network for Solar System Objects” Workshop held at IMCCE/Paris Observatory 2014, November 24 – 26 Institut de mécanique céleste et de calcul des éphémérides Observatoire de Paris Legal Deposite – June 2015 ISBN 2-910015-73-4 Foreword The observation of Solar System Objects (SSO) by the Gaia space astrometry mission will be constrained by a scanning law. Much detection of interesting objects may occur with no possibility of further observations by the probe. These objects will then require complementary ground-based observations. Among them, previously unknown Near- Earth Objects, fast moving towards the Earth or going away from it could be found. Several objects discovered by Gaia could also be Inner-Earth Objects, as the probe will observe at rather low Solar elongations. In order to confirm from the ground the discoveries made in space and to follow interesting targets, a dedicated network is organized, the Gaia Follow-Up Network. This task is performed in the frame of the Coordination Unit 4 of the Gaia Data Processing and Analysis Consortium (DPAC), devoted to data processing of specific objects. The goal of the network is to improve the knowledge of the orbit of poorly observed targets by astrometric observations on alert. This activity is coordinated by a central node interacting with the Gaia data reduction pipeline all along the mission. In 2010 and 2012, we had organized the first two workshops in order to initiate the network and to meet the participants. In 2014, almost one year after the launch of Gaia, we organize the third Gaia-FUN-SSO workshop in Paris in order to discuss further the coordination of the network of observing stations, to discuss the prelaunch training observations which have been performed and to prepare the network for the operating phase of the alert mode which must begin in 2015. -
Astrometry and Spectra Classification of Near Earth Asteroids with Lijiang
Astronomy and Astrophysics in the Gaia sky Proceedings IAU Symposium No. 330, 2017 A. Recio-Blanco, P. de Laverny, A.G.A. Brown c International Astronomical Union 2018 & T. Prusti, eds. doi:10.1017/S174392131700624X Astrometry and Spectra Classification of Near Earth Asteroids with Lijiang 2.4m Telescope† X. L. Zhang1,2,B.Yang1,2, and J. M. Bai1,2 1 Yunnan Observatories, Chinese Academy of Sciences, Kunming 650011, China email: [email protected] 2 Key Laboratory of the Structure and Evolution of Celestial Objects, Chinese Academy of Sciences, Kunming 650011, China Abstract. The Lijiang 2.4m telescope of Yunnan Observatories is located at longitude E100◦0151, latitude N26◦4232 and height 3250m above sea level (IAU code O44). Because of low latitude of the site, long-focus system and planetary tracking mode of telescope, high accuracy posi- tioning and spectral classification of the near Earth objects (NEAs) especially in the Southern Hemisphere can be studied with the Lijiang 2.4m telescope. As a set of observational campaigns organized by the GAIA-FUN-SSO, astrometry of several near Earth asteroids including (367943) Duende and (99942) Apophis were made with Lijiang 2.4m telescope during 2013. From Decem- ber 12, 2015, spectra of three near earth asteroids were also observed with the YFOSC terminal attached to the Lijiang 2.4m telescope. This paper will give the detailed introduction of Lijiaing 2.4m telescope and observational results of near Earth asteroids obtained with it. Keywords. methods: observational, techniques: astrometry, spectrum classification. 1. Introduction Knowledge of asteroids and comets, the relic of planet building blocks, directly sheds light on the formation of terrestrial planets, and the origin and evolution of the Solar System. -
An Innovative Solution to NASA's NEO Impact Threat Mitigation Grand
Final Technical Report of a NIAC Phase 2 Study December 9, 2014 NASA Grant and Cooperative Agreement Number: NNX12AQ60G NIAC Phase 2 Study Period: 09/10/2012 – 09/09/2014 An Innovative Solution to NASA’s NEO Impact Threat Mitigation Grand Challenge and Flight Validation Mission Architecture Development PI: Dr. Bong Wie, Vance Coffman Endowed Chair Professor Asteroid Deflection Research Center Department of Aerospace Engineering Iowa State University, Ames, IA 50011 email: [email protected] (515) 294-3124 Co-I: Brent Barbee, Flight Dynamics Engineer Navigation and Mission Design Branch (Code 595) NASA Goddard Space Flight Center Greenbelt, MD 20771 email: [email protected] (301) 286-1837 Graduate Research Assistants: Alan Pitz (M.S. 2012), Brian Kaplinger (Ph.D. 2013), Matt Hawkins (Ph.D. 2013), Tim Winkler (M.S. 2013), Pavithra Premaratne (M.S. 2014), Sam Wagner (Ph.D. 2014), George Vardaxis, Joshua Lyzhoft, and Ben Zimmerman NIAC Program Executive: Dr. John (Jay) Falker NIAC Program Manager: Jason Derleth NIAC Senior Science Advisor: Dr. Ronald Turner NIAC Strategic Partnerships Manager: Katherine Reilly Contents 1 Hypervelocity Asteroid Intercept Vehicle (HAIV) Mission Concept 2 1.1 Introduction ...................................... 2 1.2 Overview of the HAIV Mission Concept ....................... 6 1.3 Enabling Space Technologies for the HAIV Mission . 12 1.3.1 Two-Body HAIV Configuration Design Tradeoffs . 12 1.3.2 Terminal Guidance Sensors/Algorithms . 13 1.3.3 Thermal Protection and Shield Issues . 14 1.3.4 Nuclear Fuzing Mechanisms ......................... 15 2 Planetary Defense Flight Validation (PDFV) Mission Design 17 2.1 The Need for a PDFV Mission ............................ 17 2.2 Preliminary PDFV Mission Design by the MDL of NASA GSFC . -
Observational Investigation of the 2013 Near-Earth Encounter By
Observational Investigation of the 2013 Near-Earth Encounter by Asteroid (367943) Duende Nicholas A. Moskovitz a, Conor James Benson b, Daniel Scheeres b, Thomas Endicott c, David Polishook d, Richard Binzel e, Francesca DeMeo e, William Ryan f, Eileen Ryan f, Mark Willman g, Carl Hergenrother h, Arie Verveer i, Tim Lister j, Peter Birtwhistle k, Amanda Sickafoose `;e;o, Takahiro Nagayama m, Alan Gilmore n, Pam Kilmartin n, Susan Bennechi o, Scott Sheppard p, Franck Marchis q, Thomas Augusteijn r, Olesja Smirnova r aLowell Observatory, 1400 West Mars Hill Road, Flagstaff, AZ 86001 (U.S.A) bUniversity of Colorado Boulder, Boulder, CO 80305 cUniversity of Massachusetts Boston, Boston, MA 02125 dWeizmann Institute of Science, 234 Herzl St. Rehovot 7610001, Israel arXiv:1911.00609v1 [astro-ph.EP] 1 Nov 2019 eMassachusetts Institute of Technology, EAPS, Cambridge, MA 02139 f New Mexico Institute of Mining and Technology, Socorro, NM 87801 gInstitute for Astronomy, University of Hawaii, Hilo, HI 96720 hUniversity of Arizona, LPL, Tucson, AZ 85721 iPerth Observatory, Bickley, WA 6076 (Australia) Preprint submitted to Icarus 5 November 2019 jLas Cumbres Observatory Global Telescope Network, Goleta, CA 93117 kGreat Shefford Observatory, Berkshire (England) `South African Astronomical Observatory (South Africa) mKagoshima University (Japan) nUniversity of Canterbury, Mt John University Observatory, Lake Tekapo (New Zealand) oPlanetary Science Institute, 1700 E. Fort Lowell Rd., Tucson, AZ 85719 pDepartment of Terrestrial Magnetism, Carnegie Institution for Science, Washington, DC 20015 qSETI Institute, Carl Sagan Center, 189 Bernardo Ave., Mountain View CA 94043 rNordic Optical Telescope, La Palma (Spain) Copyright c 2019 Nicholas A. Moskovitz Number of pages: 50 Number of tables: 5 Number of figures: 12 2 Proposed Running Head: The 2013 Near-Earth Encounter of Asteroid Duende Please send Editorial Correspondence to: Nicholas A.