Ground-Based Surveys and the Asteroidfinder Mission
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Spacewalch Discovery of Near-Earth Asteroids Tom Gehrele Lunar End
N9 Spacewalch Discovery of Near-Earth Asteroids Tom Gehrele Lunar end Planetary Laboratory The University of Arizona Our overall scientific goal is to survey the solar system to completion -- that is, to find the various populations and to study their statistics, interrelations, and origins. The practical benefit to SERC is that we are finding Earth-approaching asteroids that are accessible for mining. Our system can detect Earth-approachers In the 1-km size range even when they are far away, and can detect smaller objects when they are moving rapidly past Earth. Until Spacewatch, the size range of 6 - 300 meters in diameter for the near-Earth asteroids was unexplored. This important region represents the transition between the meteorites and the larger observed near-Earth asteroids (Rabinowitz 1992). One of our Spacewatch discoveries, 1991 VG, may be representative of a new orbital class of object. If it is really a natural object, and not man-made, its orbital parameters are closer to those of the Earth than we have seen before; its delta V is the lowest of all objects known thus far (J. S. Lewis, personal communication 1992). We may expect new discoveries as we continue our surveying, with fine-tuning of the techniques. III-12 Introduction The data accumulated in the following tables are the result of continuing observation conducted as a part of the Spacewatch program. T. Gehrels is the Principal Investigator and also one of the three observers, with J.V. Scotti and D.L Rabinowitz, each observing six nights per month. R.S. McMillan has been Co-Principal Investigator of our CCD-scanning since its inception; he coordinates optical, mechanical, and electronic upgrades. -
The Catalina Sky Survey
The Catalina Sky Survey Current Operaons and Future CapabiliKes Eric J. Christensen A. Boani, A. R. Gibbs, A. D. Grauer, R. E. Hill, J. A. Johnson, R. A. Kowalski, S. M. Larson, F. C. Shelly IAWN Steering CommiJee MeeKng. MPC, Boston, MA. Jan. 13-14 2014 Catalina Sky Survey • Supported by NASA NEOO Program • Based at the University of Arizona’s Lunar and Planetary Laboratory in Tucson, Arizona • Leader of the NEO discovery effort since 2004, responsible for ~65% of new discoveries (~46% of all NEO discoveries). Currently discovering NEOs at a rate of ~600/year. • 2 survey telescopes run by a staff of 8 (observers, socware developers, engineering support, PI) Current FaciliKes Mt. Bigelow, AZ Mt. Lemmon, AZ 0.7-m Schmidt 1.5-m reflector 8.2 sq. deg. FOV 1.2 sq. deg. FOV Vlim ~ 19.5 Vlim ~ 21.3 ~250 NEOs/year ~350 NEOs/year ReKred FaciliKes Siding Spring Observatory, Australia 0.5-m Uppsala Schmidt 4.2 sq. deg. FOV Vlim ~ 19.0 2004 – 2013 ~50 NEOs/year Was the only full-Kme NEO survey located in the Southern Hemisphere Notable discoveries include Great Comet McNaught (C/2006 P1), rediscovery of Apophis Upcoming FaciliKes Mt. Lemmon, AZ 1.0-m reflector 0.3 sq. deg. FOV 1.0 arcsec/pixel Operaonal 2014 – currently in commissioning Will be primarily used for confirmaon and follow-up of newly- discovered NEOs Will remove follow-up burden from CSS survey telescopes, increasing available survey Kme by 10-20% Increased FOV for both CSS survey telescopes 5.0 deg2 1.2 ~1,100/ G96 deg2 night 19.4 deg2 2 703 8.2 deg 2 ~4,300 deg per night New 10k x 10k cameras will increase the FOV of both survey telescopes by factors of 4x and 2.4x. -
Naming the Extrasolar Planets
Naming the extrasolar planets W. Lyra Max Planck Institute for Astronomy, K¨onigstuhl 17, 69177, Heidelberg, Germany [email protected] Abstract and OGLE-TR-182 b, which does not help educators convey the message that these planets are quite similar to Jupiter. Extrasolar planets are not named and are referred to only In stark contrast, the sentence“planet Apollo is a gas giant by their assigned scientific designation. The reason given like Jupiter” is heavily - yet invisibly - coated with Coper- by the IAU to not name the planets is that it is consid- nicanism. ered impractical as planets are expected to be common. I One reason given by the IAU for not considering naming advance some reasons as to why this logic is flawed, and sug- the extrasolar planets is that it is a task deemed impractical. gest names for the 403 extrasolar planet candidates known One source is quoted as having said “if planets are found to as of Oct 2009. The names follow a scheme of association occur very frequently in the Universe, a system of individual with the constellation that the host star pertains to, and names for planets might well rapidly be found equally im- therefore are mostly drawn from Roman-Greek mythology. practicable as it is for stars, as planet discoveries progress.” Other mythologies may also be used given that a suitable 1. This leads to a second argument. It is indeed impractical association is established. to name all stars. But some stars are named nonetheless. In fact, all other classes of astronomical bodies are named. -
Staircase of Vienna Observatory (Institut Für Astronomie Der Universität Wien)
Figure 15.1: Staircase of Vienna Observatory (Institut für Astronomie der Universität Wien) 142 15. The University Observatory Vienna Anneliese Schnell (Vienna, Austria) 15.1 Introduction should prefer non-German instrument makers (E. Weiss 1873). In spring of 2008 the new Vienna Observatory was th commemorating its 125 anniversary, it was officially During a couple of years Vienna Observatory was edit- opened by Emperor Franz Joseph in 1883. Regular ob- ing an astronomical calendar. In the 1874 edition K. L. servations had started in 1880. Viennese astronomers Littrow wrote a contribution about the new observatory had planned that observatory for a long time. Already th in which he defined the instrumental needs: Karl von Littrow’s father had plans early in the 19 “für Topographie des Himmels ein mächtiges parallakti- century (at that time according to a letter from Joseph sches Fernrohr, ein dioptrisches Instrument von 25 Zoll Johann Littrow to Gauß from December 1, 1823 the Öffnung. Da sich aber ein Werkzeug von solcher Grö- observatory of Turku was taken as model) (Reich 2008), ße für laufende Beobachtungen (Ortsbestimmung neu- but it lasted until 1867 when it was decided to build a er Planeten und Kometen, fortgesetzte Doppelsternmes- new main building of the university of Vienna and also sungen, etc.) nicht eignet, ein zweites, kleineres, daher a new observatory. Viennese astronomers at that time leichter zu handhabendes, aber zur Beobachtung licht- had an excellent training in mathematics, they mostly schwacher Objekte immer noch hinreichendes Teleskop worked on positional astronomy and celestial mechanics. von etwa 10 Zoll Öffnung, und ein Meridiankreis er- They believed in F. -
March 21–25, 2016
FORTY-SEVENTH LUNAR AND PLANETARY SCIENCE CONFERENCE PROGRAM OF TECHNICAL SESSIONS MARCH 21–25, 2016 The Woodlands Waterway Marriott Hotel and Convention Center The Woodlands, Texas INSTITUTIONAL SUPPORT Universities Space Research Association Lunar and Planetary Institute National Aeronautics and Space Administration CONFERENCE CO-CHAIRS Stephen Mackwell, Lunar and Planetary Institute Eileen Stansbery, NASA Johnson Space Center PROGRAM COMMITTEE CHAIRS David Draper, NASA Johnson Space Center Walter Kiefer, Lunar and Planetary Institute PROGRAM COMMITTEE P. Doug Archer, NASA Johnson Space Center Nicolas LeCorvec, Lunar and Planetary Institute Katherine Bermingham, University of Maryland Yo Matsubara, Smithsonian Institute Janice Bishop, SETI and NASA Ames Research Center Francis McCubbin, NASA Johnson Space Center Jeremy Boyce, University of California, Los Angeles Andrew Needham, Carnegie Institution of Washington Lisa Danielson, NASA Johnson Space Center Lan-Anh Nguyen, NASA Johnson Space Center Deepak Dhingra, University of Idaho Paul Niles, NASA Johnson Space Center Stephen Elardo, Carnegie Institution of Washington Dorothy Oehler, NASA Johnson Space Center Marc Fries, NASA Johnson Space Center D. Alex Patthoff, Jet Propulsion Laboratory Cyrena Goodrich, Lunar and Planetary Institute Elizabeth Rampe, Aerodyne Industries, Jacobs JETS at John Gruener, NASA Johnson Space Center NASA Johnson Space Center Justin Hagerty, U.S. Geological Survey Carol Raymond, Jet Propulsion Laboratory Lindsay Hays, Jet Propulsion Laboratory Paul Schenk, -
An Early Warning System for Asteroid Impact
An Early Warning System for Asteroid Impact John L. Tonry(1) ABSTRACT Earth is bombarded by meteors, occasionally by one large enough to cause a significant explosion and possible loss of life. It is not possible to detect all hazardous asteroids, and the efforts to detect them years before they strike are only advancing slowly. Similarly, ideas for mitigation of the danger from an impact by moving the asteroid are in their infancy. Although the odds of a deadly asteroid strike in the next century are low, the most likely impact is by a relatively small asteroid, and we suggest that the best mitigation strategy in the near term is simply to move people out of the way. With enough warning, a small asteroid impact should not cause loss of life, and even portable property might be preserved. We describe an \early warning" system that could provide a week's notice of most sizeable asteroids or comets on track to hit the Earth. This may be all the mitigation needed or desired for small asteroids, and it can be implemented immediately for relatively low cost. This system, dubbed \Asteroid Terrestrial-impact Last Alert System" (AT- LAS), comprises two observatories separated by about 100 km that simulta- neously scan the visible sky twice a night. Software automatically registers a comparison with the unchanging sky and identifies everything which has moved or changed. Communications between the observatories lock down the orbits of anything approaching the Earth, within one night if its arrival is less than a week. The sensitivity of the system permits detection of 140 m asteroids (100 Mton impact energy) three weeks before impact, and 50 m asteroids a week be- fore arrival. -
The Orbital Distribution of Near-Earth Objects Inside Earth’S Orbit
Icarus 217 (2012) 355–366 Contents lists available at SciVerse ScienceDirect Icarus journal homepage: www.elsevier.com/locate/icarus The orbital distribution of Near-Earth Objects inside Earth’s orbit ⇑ Sarah Greenstreet a, , Henry Ngo a,b, Brett Gladman a a Department of Physics & Astronomy, 6224 Agricultural Road, University of British Columbia, Vancouver, British Columbia, Canada b Department of Physics, Engineering Physics, and Astronomy, 99 University Avenue, Queen’s University, Kingston, Ontario, Canada article info abstract Article history: Canada’s Near-Earth Object Surveillance Satellite (NEOSSat), set to launch in early 2012, will search for Received 17 August 2011 and track Near-Earth Objects (NEOs), tuning its search to best detect objects with a < 1.0 AU. In order Revised 8 November 2011 to construct an optimal pointing strategy for NEOSSat, we needed more detailed information in the Accepted 9 November 2011 a < 1.0 AU region than the best current model (Bottke, W.F., Morbidelli, A., Jedicke, R., Petit, J.M., Levison, Available online 28 November 2011 H.F., Michel, P., Metcalfe, T.S. [2002]. Icarus 156, 399–433) provides. We present here the NEOSSat-1.0 NEO orbital distribution model with larger statistics that permit finer resolution and less uncertainty, Keywords: especially in the a < 1.0 AU region. We find that Amors = 30.1 ± 0.8%, Apollos = 63.3 ± 0.4%, Atens = Near-Earth Objects 5.0 ± 0.3%, Atiras (0.718 < Q < 0.983 AU) = 1.38 ± 0.04%, and Vatiras (0.307 < Q < 0.718 AU) = 0.22 ± 0.03% Celestial mechanics Impact processes of the steady-state NEO population. -
The Minor Planets
The Minor Planets Swinburne Astronomy Online 3D PDF c SAO 2012 The Minor Planets c Swinburne Astronomy Online 2012 1 Description 1.1 Minor planets Our view of the Solar System has changed dramatically over the past 15 years with the discovery of new classes of small bodies. Mi- nor planets are another name for asteroids, or celestial bodies that orbit the Sun that are not otherwise classed as planets or comets. Generally, minor planets are relatively small rocky bodies, while comets are icy bodies that become active when their orbits carry them close to the Sun. (An \active" comet exhibits a large coma and a long tail.) The minor planets can be classified by their orbital characteristics. In this 3D PDF, we have included 5 classes of minor planets: (1) the Near Earth Asteroids (NEAs), (2) the main belt asteroids, (3) the Trojan asteroids of Jupiter, (4) the Centaurs, and (5) the Trans-Neptunian Objects (TNOs). The dataset used comes from the Minor Planets Centre. As of 19 November 2012, there were 9,346 NEAs (comprising 732 Atens, 4686 Apollos and 3928 Amors); 581,613 main belt asteroids; 5,407 jovian Trojans; 330 Centaurs; and 1,150 TNOs. (Note than in this 3D PDF, we have only included 11,678 main belt asteroids.) • The Near Earth Asteroids have perihelion distances of less than 1.3 AU, and include the following sub-classes: { Atens have aphelion distances greater than 0.983 AU, and semi-major axes less than 1 AU { Apollos have perihelion distances less than 1.017 AU, and semi-major axes greater than 1 AU { Amors have perihelion distances between 1.017 and 1.3 AU and semi-major axes greater than 1 AU • The main belt asteroids reside between the orbits of Mars and Jupiter, with most of the asteroids orbiting between about 2.1 AU and 3.3 AU. -
Orbital Stability Zones About Asteroids
ICARUS 92, 118-131 (1991) Orbital Stability Zones about Asteroids DOUGLAS P. HAMILTON AND JOSEPH A. BURNS Cornell University, Ithaca, New York, 14853-6801 Received October 5, 1990; revised March 1, 1991 exploration program should be remedied when the Galileo We have numerically investigated a three-body problem con- spacecraft, launched in October 1989, encounters the as- sisting of the Sun, an asteroid, and an infinitesimal particle initially teroid 951 Gaspra on October 29, 1991. It is expected placed about the asteroid. We assume that the asteroid has the that the asteroid's surroundings will be almost devoid of following properties: a circular heliocentric orbit at R -- 2.55 AU, material and therefore benign since, in the analogous case an asteroid/Sun mass ratio of/~ -- 5 x 10-12, and a spherical of the satellites of the giant planets, significant debris has shape with radius R A -- 100 km; these values are close to those of never been detected. The analogy is imperfect, however, the minor planet 29 Amphitrite. In order to describe the zone in and so the possibility that interplanetary debris may be which circum-asteroidal debris could be stably trapped, we pay particular attention to the orbits of particles that are on the verge enhanced in the gravitational well of the asteroid must be of escape. We consider particles to be stable or trapped if they considered. If this is the case, the danger of collision with remain in the asteroid's vicinity for at least 5 asteroid orbits about orbiting debris may increase as the asteroid is approached. -
Arxiv:1406.5253V1 [Astro-Ph.EP] 20 Jun 2014
Physical Properties of Near-Earth Asteroid 2011 MD M. Mommert Department of Physics and Astronomy, Northern Arizona University, PO Box 6010, Flagstaff, AZ 86011, USA D. Farnocchia Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109, USA J. L. Hora Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, MS 65, Cambridge, MA 02138-1516, USA S. R. Chesley Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109, USA D. E. Trilling Department of Physics and Astronomy, Northern Arizona University, PO Box 6010, Flagstaff, AZ 86011, USA P. W. Chodas Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109, USA arXiv:1406.5253v1 [astro-ph.EP] 20 Jun 2014 M. Mueller SRON Netherlands Institute for Space Research, Postbus 800, 9700 AV, Groningen, The Netherlands A. W. Harris DLR Institute of Planetary Research, Rutherfordstrasse 2, 12489 Berlin, Germany H. A. Smith –2– Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, MS 65, Cambridge, MA 02138-1516, USA and G. G. Fazio Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, MS 65, Cambridge, MA 02138-1516, USA Received ; accepted accepted by ApJL –3– ABSTRACT We report on observations of near-Earth asteroid 2011 MD with the Spitzer Space Telescope. We have spent 19.9 h of observing time with channel 2 (4.5 µm) of the Infrared Array Camera and detected the target within the 2σ positional uncertainty ellipse. Using an asteroid thermophysical model and a model of non- gravitational forces acting upon the object we constrain the physical properties of 2011 MD, based on the measured flux density and available astrometry data. -
Neofixer a Broker for Near Earth Asteroid Follow-Up Rob Seaman & Eric Christensen Catalina Sky Survey
NEOFIXER A BROKER FOR NEAR EARTH ASTEROID FOLLOW-UP ROB SEAMAN & ERIC CHRISTENSEN CATALINA SKY SURVEY Building the Infrastructure for Time-Domain Alert Science in the LSST Era • May 22-25, 2017 • Tucson CATALINA SKY SURVEY • LPL runs 2 NEO projects, CSS and SpacewatcH • Talk to Eric or me about CSS, Bob McMillan for SW • CSS demo at 3:30 pm CONGRESSIONAL MANDATE • Spaceguard goal: 1 km Near EartH Objects ✔ • George E Brown Act to find > 140m (H < 22) NEOs • 90% complete by 2020 ✘ (2017: ~ 30%) • ROSES 2017 language is > 100m • Chelyabinsk was ~20m (H ~ 25.8) or ~400 kiloton (few per century likeliHood) SUMMARY • Near EartH Asteroid inventory is “retail Big Data” • NEOfixer will be NEO-optimized targeting broker • No one broker will address all use cases • Will benefit LSST as well as current surveys • LSST not tasked to study NEOs, but ratHer tHe Solar System (slower objects and fartHer away) • What is tHe most valuable NEO observation a particular telescope can make at a particular time? CHESLEY & VERES (1705.06209) • 55 ± 5.0% for LSST baseline operating alone • But 42% of NEOs witH H < 22 will be discovered before 2022 • And witHout LSST, current surveys would discover 61% of the catalog by 2032 • Completion CH<22 will be 77% combined LSST will add 16% to CH<22 Can targeted follow-up increase this? CHESLEY & VERES (CAVEATS) • Lots of details worth reading • CH<22 degrades by ~1.8% for every 0.1 mag loss in sensitivity • Issues of linking efficiency including: • Efficiency down to H < 25 is lower • 4% false MBA-MBA links ASTROMETRIC -
Detecting the Yarkovsky Effect Among Near-Earth Asteroids From
Detecting the Yarkovsky effect among near-Earth asteroids from astrometric data Alessio Del Vignaa,b, Laura Faggiolid, Andrea Milania, Federica Spotoc, Davide Farnocchiae, Benoit Carryf aDipartimento di Matematica, Universit`adi Pisa, Largo Bruno Pontecorvo 5, Pisa, Italy bSpace Dynamics Services s.r.l., via Mario Giuntini, Navacchio di Cascina, Pisa, Italy cIMCCE, Observatoire de Paris, PSL Research University, CNRS, Sorbonne Universits, UPMC Univ. Paris 06, Univ. Lille, 77 av. Denfert-Rochereau F-75014 Paris, France dESA SSA-NEO Coordination Centre, Largo Galileo Galilei, 1, 00044 Frascati (RM), Italy eJet Propulsion Laboratory/California Institute of Technology, 4800 Oak Grove Drive, Pasadena, 91109 CA, USA fUniversit´eCˆote d’Azur, Observatoire de la Cˆote d’Azur, CNRS, Laboratoire Lagrange, Boulevard de l’Observatoire, Nice, France Abstract We present an updated set of near-Earth asteroids with a Yarkovsky-related semi- major axis drift detected from the orbital fit to the astrometry. We find 87 reliable detections after filtering for the signal-to-noise ratio of the Yarkovsky drift esti- mate and making sure the estimate is compatible with the physical properties of the analyzed object. Furthermore, we find a list of 24 marginally significant detec- tions, for which future astrometry could result in a Yarkovsky detection. A further outcome of the filtering procedure is a list of detections that we consider spurious because unrealistic or not explicable with the Yarkovsky effect. Among the smallest asteroids of our sample, we determined four detections of solar radiation pressure, in addition to the Yarkovsky effect. As the data volume increases in the near fu- ture, our goal is to develop methods to generate very long lists of asteroids with reliably detected Yarkovsky effect, with limited amounts of case by case specific adjustments.