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SPECIAL Comet Shoemaker-Levy 9 Collides with Jupiter
SL-9/JUPITER ENCOUNTER - SPECIAL Comet Shoemaker-Levy 9 Collides with Jupiter THE CONTINUATION OF A UNIQUE EXPERIENCE R.M. WEST, ESO-Garching After the Storm Six Hectic Days in July eration during the first nights and, as in other places, an extremely rich data The recent demise of comet Shoe ESO was but one of many profes material was secured. It quickly became maker-Levy 9, for simplicity often re sional observatories where observations evident that infrared observations, es ferred to as "SL-9", was indeed spectac had been planned long before the critical pecially imaging with the far-IR instru ular. The dramatic collision of its many period of the "SL-9" event, July 16-22, ment TIMMI at the 3.6-metre telescope, fragments with the giant planet Jupiter 1994. It is now clear that practically all were perfectly feasible also during day during six hectic days in July 1994 will major observatories in the world were in time, and in the end more than 120,000 pass into the annals of astronomy as volved in some way, via their telescopes, images were obtained with this facility. one of the most incredible events ever their scientists or both. The only excep The programmes at most of the other predicted and witnessed by members of tions may have been a few observing La Silla telescopes were also successful, this profession. And never before has a sites at the northernmost latitudes where and many more Gigabytes of data were remote astronomical event been so ac the bright summer nights and the very recorded with them. -
KAREN J. MEECH February 7, 2019 Astronomer
BIOGRAPHICAL SKETCH – KAREN J. MEECH February 7, 2019 Astronomer Institute for Astronomy Tel: 1-808-956-6828 2680 Woodlawn Drive Fax: 1-808-956-4532 Honolulu, HI 96822-1839 [email protected] PROFESSIONAL PREPARATION Rice University Space Physics B.A. 1981 Massachusetts Institute of Tech. Planetary Astronomy Ph.D. 1987 APPOINTMENTS 2018 – present Graduate Chair 2000 – present Astronomer, Institute for Astronomy, University of Hawaii 1992-2000 Associate Astronomer, Institute for Astronomy, University of Hawaii 1987-1992 Assistant Astronomer, Institute for Astronomy, University of Hawaii 1982-1987 Graduate Research & Teaching Assistant, Massachusetts Inst. Tech. 1981-1982 Research Specialist, AAVSO and Massachusetts Institute of Technology AWARDS 2018 ARCs Scientist of the Year 2015 University of Hawai’i Regent’s Medal for Research Excellence 2013 Director’s Research Excellence Award 2011 NASA Group Achievement Award for the EPOXI Project Team 2011 NASA Group Achievement Award for EPOXI & Stardust-NExT Missions 2009 William Tylor Olcott Distinguished Service Award of the American Association of Variable Star Observers 2006-8 National Academy of Science/Kavli Foundation Fellow 2005 NASA Group Achievement Award for the Stardust Flight Team 1996 Asteroid 4367 named Meech 1994 American Astronomical Society / DPS Harold C. Urey Prize 1988 Annie Jump Cannon Award 1981 Heaps Physics Prize RESEARCH FIELD AND ACTIVITIES • Developed a Discovery mission concept to explore the origin of Earth’s water. • Co-Investigator on the Deep Impact, Stardust-NeXT and EPOXI missions, leading the Earth-based observing campaigns for all three. • Leads the UH Astrobiology Research interdisciplinary program, overseeing ~30 postdocs and coordinating the research with ~20 local faculty and international partners. -
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. -
Early Observations of the Interstellar Comet 2I/Borisov
geosciences Article Early Observations of the Interstellar Comet 2I/Borisov Chien-Hsiu Lee NSF’s National Optical-Infrared Astronomy Research Laboratory, Tucson, AZ 85719, USA; [email protected]; Tel.: +1-520-318-8368 Received: 26 November 2019; Accepted: 11 December 2019; Published: 17 December 2019 Abstract: 2I/Borisov is the second ever interstellar object (ISO). It is very different from the first ISO ’Oumuamua by showing cometary activities, and hence provides a unique opportunity to study comets that are formed around other stars. Here we present early imaging and spectroscopic follow-ups to study its properties, which reveal an (up to) 5.9 km comet with an extended coma and a short tail. Our spectroscopic data do not reveal any emission lines between 4000–9000 Angstrom; nevertheless, we are able to put an upper limit on the flux of the C2 emission line, suggesting modest cometary activities at early epochs. These properties are similar to comets in the solar system, and suggest that 2I/Borisov—while from another star—is not too different from its solar siblings. Keywords: comets: general; comets: individual (2I/Borisov); solar system: formation 1. Introduction 2I/Borisov was first seen by Gennady Borisov on 30 August 2019. As more observations were conducted in the next few days, there was growing evidence that this might be an interstellar object (ISO), especially its large orbital eccentricity. However, the first astrometric measurements do not have enough timespan and are not of same quality, hence the high eccentricity is yet to be confirmed. This had all changed by 11 September; where more than 100 astrometric measurements over 12 days, Ref [1] pinned down the orbit elements of 2I/Borisov, with an eccentricity of 3.15 ± 0.13, hence confirming the interstellar nature. -
Interstellar Comet 2I/Borisov
Interstellar comet 2I/Borisov Piotr Guzik1*, Michał Drahus1*, Krzysztof Rusek2, Wacław Waniak1, Giacomo Cannizzaro3,4, Inés Pastor-Marazuela5,6 1 Astronomical Observatory, Jagiellonian University, ul. Orla 171, 30-244 Kraków, Poland 2 AGH University of Science and Technology, al. Mickiewicza 30, Kraków 30-059, Poland 3 SRON, Netherlands Institute for Space Research, Sorbonnelaan, 2, NL-3584CA Utrecht, the Netherlands 4 Department of Astrophysics/IMAPP, Radboud University, P.O. Box 9010, 6500 GL Nijmegen, the Netherlands 5 Anton Pannekoek Institute for Astronomy, University of Amsterdam, Science Park 904, 1098 XH Amsterdam, The Netherlands 6 ASTRON, Netherlands Institute for Radio Astronomy, Oude Hoogeveensedijk 4, 7991 PD Dwingeloo, The Netherlands * These authors contributed equally to this work. Interstellar comets penetrating through the Solar System were anticipated for decades1,2. The discovery of non-cometary 1I/‘Oumuamua by Pan-STARRS was therefore a huge surprise and puzzle. Furthermore, its physical properties turned out to be impossible to reconcile with Solar System objects3-5, which radically changed our view on interstellar minor bodies. Here, we report the identification of a new interstellar object which has an evidently cometary appearance. The body was identified by our data mining code in publicly available astrometric data. The data clearly show significant systematic deviation from what is expected for a parabolic orbit and are consistent with an enormous orbital eccentricity of 3.14 ± 0.14. Images taken by the William Herschel Telescope and Gemini North telescope show an extended coma and a faint, broad tail – the canonical signatures of cometary activity. The observed g’ and r’ magnitudes are equal to 19.32 ± 0.02 and 18.69 ± 0.02, respectively, implying g’-r’ color index of 0.63 ± 0.03, essentially the same as measured for the native Solar System comets. -
Initial Characterization of Interstellar Comet 2I/Borisov
Initial characterization of interstellar comet 2I/Borisov Piotr Guzik1*, Michał Drahus1*, Krzysztof Rusek2, Wacław Waniak1, Giacomo Cannizzaro3,4, Inés Pastor-Marazuela5,6 1 Astronomical Observatory, Jagiellonian University, Kraków, Poland 2 AGH University of Science and Technology, Kraków, Poland 3 SRON, Netherlands Institute for Space Research, Utrecht, the Netherlands 4 Department of Astrophysics/IMAPP, Radboud University, Nijmegen, the Netherlands 5 Anton Pannekoek Institute for Astronomy, University of Amsterdam, Amsterdam, the Netherlands 6 ASTRON, Netherlands Institute for Radio Astronomy, Dwingeloo, the Netherlands * These authors contributed equally to this work; email: [email protected], [email protected] Interstellar comets penetrating through the Solar System had been anticipated for decades1,2. The discovery of asteroidal-looking ‘Oumuamua3,4 was thus a huge surprise and a puzzle. Furthermore, the physical properties of the ‘first scout’ turned out to be impossible to reconcile with Solar System objects4–6, challenging our view of interstellar minor bodies7,8. Here, we report the identification and early characterization of a new interstellar object, which has an evidently cometary appearance. The body was discovered by Gennady Borisov on 30 August 2019 UT and subsequently identified as hyperbolic by our data mining code in publicly available astrometric data. The initial orbital solution implies a very high hyperbolic excess speed of ~32 km s−1, consistent with ‘Oumuamua9 and theoretical predictions2,7. Images taken on 10 and 13 September 2019 UT with the William Herschel Telescope and Gemini North Telescope show an extended coma and a faint, broad tail. We measure a slightly reddish colour with a g′–r′ colour index of 0.66 ± 0.01 mag, compatible with Solar System comets. -
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. -
Carbon Monoxide in Jupiter After Comet Shoemaker-Levy 9
ICARUS 126, 324±335 (1997) ARTICLE NO. IS965655 Carbon Monoxide in Jupiter after Comet Shoemaker±Levy 9 1 1 KEITH S. NOLL AND DIANE GILMORE Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, Maryland 21218 E-mail: [email protected] 1 ROGER F. KNACKE AND MARIA WOMACK Pennsylvania State University, Erie, Pennsylvania 16563 1 CAITLIN A. GRIFFITH Northern Arizona University, Flagstaff, Arizona 86011 AND 1 GLENN ORTON Jet Propulsion Laboratory, Pasadena, California 91109 Received February 5, 1996; revised November 5, 1996 for roughly half the mass. In high-temperature shocks, Observations of the carbon monoxide fundamental vibra- most of the O is converted to CO (Zahnle and MacLow tion±rotation band near 4.7 mm before and after the impacts 1995), making CO one of the more abundant products of of the fragments of Comet Shoemaker±Levy 9 showed no de- a large impact. tectable changes in the R5 and R7 lines, with one possible By contrast, oxygen is a rare element in Jupiter's upper exception. Observations of the G-impact site 21 hr after impact atmosphere. The principal reservoir of oxygen in Jupiter's do not show CO emission, indicating that the heated portions atmosphere is water. The Galileo Probe Mass Spectrome- of the stratosphere had cooled by that time. The large abun- ter found a mixing ratio of H OtoH of X(H O) # 3.7 3 dances of CO detected at the millibar pressure level by millime- 2 2 2 24 P et al. ter wave observations did not extend deeper in Jupiter's atmo- 10 at P 11 bars (Niemann 1996). -
The Physical Characterization of the Potentially-‐Hazardous
The Physical Characterization of the Potentially-Hazardous Asteroid 2004 BL86: A Fragment of a Differentiated Asteroid Vishnu Reddy1 Planetary Science Institute, 1700 East Fort Lowell Road, Tucson, AZ 85719, USA Email: [email protected] Bruce L. Gary Hereford Arizona Observatory, Hereford, AZ 85615, USA Juan A. Sanchez1 Planetary Science Institute, 1700 East Fort Lowell Road, Tucson, AZ 85719, USA Driss Takir1 Planetary Science Institute, 1700 East Fort Lowell Road, Tucson, AZ 85719, USA Cristina A. Thomas1 NASA Goddard Spaceflight Center, Greenbelt, MD 20771, USA Paul S. Hardersen1 Department of Space Studies, University of North Dakota, Grand Forks, ND 58202, USA Yenal Ogmen Green Island Observatory, Geçitkale, Mağusa, via Mersin 10 Turkey, North Cyprus Paul Benni Acton Sky Portal, 3 Concetta Circle, Acton, MA 01720, USA Thomas G. Kaye Raemor Vista Observatory, Sierra Vista, AZ 85650 Joao Gregorio Atalaia Group, Crow Observatory (Portalegre) Travessa da Cidreira, 2 rc D, 2645- 039 Alcabideche, Portugal Joe Garlitz 1155 Hartford St., Elgin, OR 97827, USA David Polishook1 Weizmann Institute of Science, Herzl Street 234, Rehovot, 7610001, Israel Lucille Le Corre1 Planetary Science Institute, 1700 East Fort Lowell Road, Tucson, AZ 85719, USA Andreas Nathues Max-Planck Institute for Solar System Research, Justus-von-Liebig-Weg 3, 37077 Göttingen, Germany 1Visiting Astronomer at the Infrared Telescope Facility, which is operated by the University of Hawaii under Cooperative Agreement no. NNX-08AE38A with the National Aeronautics and Space Administration, Science Mission Directorate, Planetary Astronomy Program. Pages: 27 Figures: 8 Tables: 4 Proposed Running Head: 2004 BL86: Fragment of Vesta Editorial correspondence to: Vishnu Reddy Planetary Science Institute 1700 East Fort Lowell Road, Suite 106 Tucson 85719 (808) 342-8932 (voice) [email protected] Abstract The physical characterization of potentially hazardous asteroids (PHAs) is important for impact hazard assessment and evaluating mitigation options. -
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 -
Newsletter December 2016
Current NEO statistics A refinement of the method used for analysing the asteroid hazard led to an increase in the number of objects in the risk list. Known NEOs: 15 271 asteroids and 106 comets NEOs in risk list*: 576 New NEO discoveries since last month: 161 NEOs discovered since 1 January 2016: 1750 Focus on Whenever a new set of observations for an object is published, our Impact Monitoring routines perform a new search for possibly impacting orbits compatible with such set of observations. The system is capable of detecting all possibly impacting orbits down to an impact probability threshold, named “generic completeness level”. The search begins by investigating a set of initial conditions taken along a specific line of parameters, called Line of Variations (LoV), inside the orbit uncertainty region. The NEODyS impact monitoring system was recently switched to a new method to sample the LoV, which decreased the generic completeness level from 4×10-7 to 10-7 (i.e. a factor of four better than the previous approach). The whole risk list has been updated with the outcome of the new method, and it is now available on both the NEODyS and the NEOCC risk pages. Upcoming interesting close approaches To date no known object is expected to come closer than one lunar distance to our planet in December, thus deserving special attention. New discoveries likely will. The closest known approach will be 2016 WQ3 at 1.5 lunar distances on 1 December. Recent interesting close approaches Four new objects came closer than the Moon in November. -
Detection of Exocometary CO Within the 440 Myr Old Fomalhaut Belt: a Similar CO+CO2 Ice Abundance in Exocomets and Solar System Comets
UCLA UCLA Previously Published Works Title Detection of Exocometary CO within the 440 Myr Old Fomalhaut Belt: A Similar CO+CO2 Ice Abundance in Exocomets and Solar System Comets Permalink https://escholarship.org/uc/item/1zf7t4qn Journal Astrophysical Journal, 842(1) ISSN 0004-637X Authors Matra, L MacGregor, MA Kalas, P et al. Publication Date 2017-06-10 DOI 10.3847/1538-4357/aa71b4 Peer reviewed eScholarship.org Powered by the California Digital Library University of California The Astrophysical Journal, 842:9 (15pp), 2017 June 10 https://doi.org/10.3847/1538-4357/aa71b4 © 2017. The American Astronomical Society. All rights reserved. Detection of Exocometary CO within the 440 Myr Old Fomalhaut Belt: A Similar CO+CO2 Ice Abundance in Exocomets and Solar System Comets L. Matrà1, M. A. MacGregor2, P. Kalas3,4, M. C. Wyatt1, G. M. Kennedy1, D. J. Wilner2, G. Duchene3,5, A. M. Hughes6, M. Pan7, A. Shannon1,8,9, M. Clampin10, M. P. Fitzgerald11, J. R. Graham3, W. S. Holland12, O. Panić13, and K. Y. L. Su14 1 Institute of Astronomy, University of Cambridge, Madingley Road, Cambridge CB3 0HA, UK; [email protected] 2 Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA 3 Astronomy Department, University of California, Berkeley CA 94720-3411, USA 4 SETI Institute, Mountain View, CA 94043, USA 5 Univ. Grenoble Alpes/CNRS, IPAG, F-38000 Grenoble, France 6 Department of Astronomy, Van Vleck Observatory, Wesleyan University, 96 Foss Hill Dr., Middletown, CT 06459, USA 7 MIT Department of Earth, Atmospheric, and