Near-Earth Asteroid Is Really a Comet 10 September 2013

Total Page:16

File Type:pdf, Size:1020Kb

Near-Earth Asteroid Is Really a Comet 10 September 2013 Near-Earth asteroid is really a comet 10 September 2013 asteroid's, which tend to be more circular—so people thought it was one that had shed all its ice deposits." Using the Spitzer Space Telescope operated by the Jet Propulsion Laboratory at the California Institute of Technology under contract with NASA, the team—led by Michael Mommert of Northern Arizona University—reexamined images of Don Quixote from 2009 when it was in the part of its orbit closest to the Sun, and found it had a coma and a faint tail. Emery also reexamined images from 2004, when it The image displays Don Quixote's orbit. Credit: Josh was at its farthest distance from the sun, and Emery determined that the surface is composed of silicate dust, which is similar to comet dust. He also determined that Don Quixote did not have a coma or tail at this distance, which is common for comets Some things are not always what they seem—even because they need the sun's radiation to form the in space. For 30 years, scientists believed a large coma and the sun's charged particles to form the near-Earth object was an asteroid. Now, an tail. The researchers also confirmed Don Quixote's international team including Joshua Emery, size and the low, comet-like reflectivity of its assistant professor of earth and planetary sciences surface. at the University of Tennessee, Knoxville, has discovered it is actually a comet. Called 3552 Don Quixote, the body is the third largest near-Earth object—mostly rocky bodies, or asteroids, that orbit the Sun in the vicinity of Earth. About 5 percent of near-Earth objects are thought to be "dead" comets that have shed all the water and carbon dioxide in the form of ice that give them their coma—a cloud surrounding the comet nucleus—and tail. The team found that Don Quixote is neither. It is, in fact, an active comet, thus likely containing water ice and not just rocks. The finding will be presented at the European Planetary Science Congress 2013 in London today, Sept. 10. The discovery could hold implications for the origin of water on Earth. "Don Quixote has always been recognized as an This is Don Quixote's coma and tail (left) as seen in oddball," said Emery. "Its orbit brings it close to infrared light by NASA's Spitzer Space Telescope. In after-image processing (right), the tail is more apparent. Earth, but also takes it way out past Jupiter. Such Credit: NASA/JPL-Caltech/DLR/NAU a vast orbit is similar to a comet's, not an 1 / 2 "The power of the Spitzer telescope allowed us to spot the coma and tail, which was not possible using optical telescopes on the ground," said Emery. "We now think this body contains a lot of ice, including carbon dioxide and/or carbon monoxide ice, rather than just being rocky." This discovery implies that carbon dioxide and water ice might be present within other near-Earth asteroids, as well. It also may have implications for the origins of water on Earth as comets may be the source of at least some of it, and the amount on Don Quixote represents about 100 billion tons of water—roughly the same amount that can be found in Lake Tahoe, California's. Provided by University of Tennessee at Knoxville APA citation: Near-Earth asteroid is really a comet (2013, September 10) retrieved 23 September 2021 from https://phys.org/news/2013-09-near-earth-asteroid-comet.html This document is subject to copyright. Apart from any fair dealing for the purpose of private study or research, no part may be reproduced without the written permission. The content is provided for information purposes only. 2 / 2 Powered by TCPDF (www.tcpdf.org).
Recommended publications
  • Phobos and Deimos: Planetary Protection Knowledge Gaps for Human Missions
    Planetary Protection Knowledge Gaps for Human Extraterrestrial Missions (2015) 1007.pdf PHOBOS AND DEIMOS: PLANETARY PROTECTION KNOWLEDGE GAPS FOR HUMAN MISSIONS. Pascal Lee1,2,3 and Kira Lorber1,4, 1Mars Institute, NASA Ames Research Center, MS 245-3, Moffett Field, CA 94035-1000, USA, [email protected], 2SETI Institute, 3NASA ARC, 4University of Cincinnati.. Summary: Phobos and Deimos, Mars’ two moons, are associated with significant planetary protection knowledge gaps for human missions, that may be filled by a low cost robotic reconnaissance mission focused on elucidating their origin and volatile content. Introduction: Phobos and Deimos are currently considered to be potentially worthwhile destinations Figure 1: Deimos (left) and Phobos (right), to scale. for early human missions to Mars orbit, and possibly in Deimos is 15 km long, and Phobos, 27 km long. Both the context of longer term human Mars exploration moons have, to first order, a D-type spectrum: they are strategies as well [1] (Fig. 1). Until recently, it was very dark (albedo ~ 0.07) and very red. (NASA MRO). widely considered that planetary protection (PP) con- cerns associated with the exploration of Phobos and Extinct Comet Hypothesis. As a variant of the Deimos would be fundamentally no different from “captured small body from the outer main belt” hy- those associated with the exploration of primitive pothesis, it has long been suggested that Phobos and/or NEAs [2], as the preponderance of scientific evidence Deimos might be captured comet nuclei. (now inactive suggested that 1) there was never liquid water on Pho- or extinct). Consistent with this idea, some grooves on bos and Deimos, except possibly very early in their Phobos (those resembling crater chains, or catenas) are history; 2) there is no metabolically useful energy interpreted as fissures lined with vents through which source except near their heavily irradiated surface; 3) volatiles were once outgassed [3] (Fig.
    [Show full text]
  • A Deep Search for Emission From" Rock Comet"(3200) Phaethon at 1 AU
    Draft version November 23, 2020 Typeset using LATEX preprint style in AASTeX63 A Deep Search for Emission From \Rock Comet" (3200) Phaethon At 1 AU Quanzhi Ye (叶泉志),1 Matthew M. Knight,2, 1 Michael S. P. Kelley,1 Nicholas A. Moskovitz,3 Annika Gustafsson,4 and David Schleicher3 1Department of Astronomy, University of Maryland, College Park, MD 20742, USA 2Department of Physics, United States Naval Academy, 572C Holloway Rd, Annapolis, MD 21402, USA 3Lowell Observatory, 1400 W Mars Hill Road, Flagstaff, AZ 86001, USA 4Department of Astronomy and Planetary Science, P.O. Box 6010, Northern Arizona University, Flagstaff, AZ 86011, USA (Received -; Revised -; Accepted -) Submitted to PSJ ABSTRACT We present a deep imaging and spectroscopic search for emission from (3200) Phaethon, a large near-Earth asteroid that appears to be the parent of the strong Geminid meteoroid stream, using the 4.3 m Lowell Discovery Telescope. Observations were conducted on 2017 December 14{18 when Phaethon passed only 0.07 au from the Earth. We determine the 3σ upper level of dust and CN production rates to be 0.007{0.2 kg s−1 and 2:3 1022 molecule s−1 through narrowband imaging. A search × in broadband images taken through the SDSS r' filter shows no 100-m-class fragments in Phaethon's vicinity. A deeper, but star-contaminated search also shows no sign of fragments down to 15 m. Optical spectroscopy of Phaethon and comet C/2017 O1 (ASASSN) as comparison confirms the absence of cometary emission lines from 24 25 −1 Phaethon and yields 3σ upper levels of CN, C2 and C3 of 10 {10 molecule s , 2 orders of magnitude higher than the CN constraint placed∼ by narrowband imaging, due to the much narrower on-sky aperture of the spectrographic slit.
    [Show full text]
  • Callhorizons Documentation Release 1.0.5
    callHORIZONS Documentation Release 1.0.5 Michael Mommert Jul 19, 2018 Contents 1 Installation 3 1.1 PIP....................................................3 1.2 GitHub..................................................3 2 How to Use It? 5 3 Examples 9 4 callhorizons 11 4.1 callhorizons module........................................... 11 5 Indices and tables 17 Python Module Index 19 i ii callHORIZONS Documentation, Release 1.0.5 CALLHORIZONS is a Python interface to access JPL HORIZONS ephemerides and orbital elements of Solar System bodies. Please note that CALLHORIZONS is not maintained anymore. Please use astroquery.jplhorizons instead, which will be maintained in the future and offers additional functionality. I apologize for any inconvenience. Contents 1 callHORIZONS Documentation, Release 1.0.5 2 Contents CHAPTER 1 Installation Please note that CALLHORIZONS is not maintained anymore. Please use [astroquery.jplhorizons](http:// astroquery.readthedocs.io/en/latest/jplhorizons/jplhorizons.html) instead, which will be maintained in the future and offers additional functionality. I apologize for any inconvenience. 1.1 PIP Using PIP, simply call: pip install callhorizons 1.2 GitHub Using git, simply clone the code from GitHub: git clone https://github.com/mommermi/callhorizons or, download and unpack the zip file with all the files from GitHub and then run from the callhorizons directory: python setup.py install 3 callHORIZONS Documentation, Release 1.0.5 4 Chapter 1. Installation CHAPTER 2 How to Use It? Please note that CALLHORIZONS is not maintained anymore. Please use [astroquery.jplhorizons](http:// astroquery.readthedocs.io/en/latest/jplhorizons/jplhorizons.html) instead, which will be maintained in the future and offers additional functionality. I apologize for any inconvenience.
    [Show full text]
  • Introduction to the Special Issue: Exploration of the Activity of Asteroid (101955) Bennu
    INTRODUCTION TO Introduction to the Special Issue: Exploration of the A SPECIAL SECTION Activity of Asteroid (101955) Bennu 10.1029/2020JE006549 C. W. Hergenrother1 , C. D. Adam2 , S. R. Chesley3 , and D. S. Lauretta1 Key Points: 1 2 • Novel and classical methods were Lunar and Planetary Laboratory, University of Arizona, Tucson, AZ, USA, KinetX Aerospace, Simi Valley, CA, USA, applied to detect and characterize 3Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA, USA particles ejected from near‐Earth asteroid Bennu • Of the mechanisms investigated, Abstract Near‐Earth asteroid (101955) Bennu is an active asteroid experiencing mass loss. The activity meteoroid impacts, thermal ‐ ‐ fracturing, and ricochet are manifests itself in the form of ejection events emitting up to hundreds of millimeter to centimeter scale consistent with observations particles. The Origins, Spectral Interpretation, Resource Identification, and Security‐Regolith Explorer • Some ejected particles escape or spacecraft monitored particle activity for a 10‐month period that included Bennu's perihelion and aphelion. temporarily orbit and most reimpact, with implications for Novel and classical methods were utilized to detect the particles and characterize their orbital and Bennu's geophysics and surface physical properties. Roughly 30% of the observed particle mass escaped to heliocentric orbit. A majority properties of particles fell back onto the surface of Bennu after ejection, with the longest‐lived particle surviving for 6 days on a temporary orbit. Particle ejection events appear to preferentially take place in the afternoon and evening and from low latitudes, although they can occur at any time or latitude. The reaccumulation of Correspondence to: material is biased toward low latitudes resulting in the possible in‐fill of craters and growth of Bennu's C.
    [Show full text]
  • Planetary Science Update
    Planetary Science Update David Schurr Deputy Director Planetary Science July 23, 2014 Outline • Planetary upcoming mission events • Recent accomplishments • Use of Astrophysics Telescopes • R&A status Planetary Science Missions Events as of July 15, 2014 2014 July – Mars 2020 Rover instrument selection announcement August 6 – 2nd Year Anniversary of Curiosity Landing on Mars Fall - Curiosity arrives at Mt. Sharp September 21 - MAVEN inserted in Mars orbit October 19 – Comet Siding Spring encounters Mars November 11 – ESA’s Rosetta mission lands on Comet Churyumov–Gerasimenko 2015 March - MESSENGER spacecraft impacts Mercury Late March – Dawn inserted into orbit at dwarf planet Ceres April - Europa instrument Step 1 selection June - Discovery 2014 Step 1 selection July 14 – New Horizons flies through the Pluto system 2016 March – Launch of Mars missions InSight and ESA’s ExoMars Trace Gas Orbiter April - Europa instrument step 2 selection July - Juno inserted in Jupiter orbit July – ESA’s Bepi Columbo launch to Mercury August - Discovery 2014 Step 2 selection September - InSight Mars landing September – Launch of Asteroid mission OSIRIS – REx September - Cassini begins to orbit between Saturn’s rings & planet Recent Accomplishments • Release of draft Discovery AO – July 2, 2014 – Comments were due July 16, 2014 – AO release planned by first week in October – Step-1 proposals will be due late in CY2014. • Release of Europa Instrument AO – July 15, 2014 – Proposals due October 17, 2014 • 2014 Senior Review completed – includes Cassini Off-Earth
    [Show full text]
  • Endogenous Surface Processes on Asteroids, Comets, and Meteorite
    Lunar and Planetary Science XXIX 1203.pdf ENDOGENOUS SURFACE PROCESSES ON ASTEROIDS, COMETS AND METEORITE PARENT BODIES. Derek W. G. Sears, Cosmochemistry Group, Department of Chemistry and Biochemistry, University of Arkansas, Fayetteville, Arkansas 72701, USA. It is known that (i) almost half of the known asteroids are CI- or CM-like, and these meteorites are 10-20% water; (ii) many asteroids have water on their surfaces despite impact heating and evaporative drying; (iii) many asteroids, including Apollo-Amor asteroids that have been linked to the ordinary chondrites, are possibly related to comets. It is therefore suggested that endogenous processes involving the mobilization and loss of water and other volatile compounds on meteorite parent bodies should be considered in explaining the properties of ordinary chondrite meteorites. It is suggested that water and other volatile compounds from the interior of the meteorite parent body passing through the unconsolidated surface layers produced many of the major meteorite properties, including the aerodynamic and gravitational sorting of their components, and occasional aqueous alteration. Asteroids are almost certainly the immediate parent bodies of most meteorites (1), and some asteroids could be cometary in origin (2,3). There is considerable uncertainty as to which meteorite properties reflect processes occurring on the meteorite parent body (MPB) and which occurred in interstellar or interplanetary space (e.g. 4,5). The impact history and the formation of regoliths on asteroids (and thus MPB) are often discussed (6,7), but not the possibility of endogenous surface alteration processes. Many asteroids have CI- or CM-like surfaces (8), and these meteorites are 10-20 percent total water (9).
    [Show full text]
  • ALBEDOS of ASTEROIDS in COMET-LIKE ORBITS Yanga R
    The Astronomical Journal, 130:308–318, 2005 July # 2005. The American Astronomical Society. All rights reserved. Printed in U.S.A. ALBEDOS OF ASTEROIDS IN COMET-LIKE ORBITS Yanga R. Ferna´ndez,1 David C. Jewitt,1 and Scott S. Sheppard1,2 Institute for Astronomy, University of Hawai‘i at Manoa,¯ 2680 Woodlawn Drive, Honolulu, HI 96822; [email protected], [email protected], [email protected] Received 2005 January 30; accepted 2005 March 24 ABSTRACT We present the results of a mid-infrared survey of 26 asteroids in comet-like orbits, including six Damocloids and six near-Earth asteroids (NEAs). We define a ‘‘comet-like’’ orbit as one having a Tisserand invariant TJ under 3 (but only including objects that are NEAs or otherwise unusual). Visible-wavelength data were also obtained, so geo- metric albedos (in the Cousins R band) and effective radii are presented for 25 objects (plus one more with 3 ' limits) as derived using the NEA Thermal Model. Nine of our objects were observed at two or more mid-infrared wave- lengths, and in all cases the low-thermal inertia thermal model was found to be applicable, with various values of the beaming parameter. Our work more than quintuples the total number of observationally constrained albedos among TJ < 3 asteroids to 32. Defining the ‘‘comet-like’’ albedos as those below 0.075, we find that 64% 5% of the sample has comet-like albedos. Objects in comet-like orbits with comet-like albedos are candidates forÆbeing dormant or extinct comets. Indeed, one of our targets, 2001 OG108, became active again a few months after our observations.
    [Show full text]
  • Dark Primitive Asteroids Account for a Large Share of K/Pg-Scale Impacts on the Earth
    Dark Primitive Asteroids Account for a Large Share of K/Pg-Scale Impacts on the Earth David Nesvorn´y, William F. Bottke, Simone Marchi Department of Space Studies, Southwest Research Institute, 1050 Walnut St., Suite 300, Boulder, CO 80302, USA ABSTRACT A dynamical model for large near-Earth asteroids (NEAs) is developed here to understand the occurrence rate and nature of Cretaceous-Paleogene (K/Pg) scale impacts on the Earth. We find that 16–32 (2–4) impacts of diameter D > 5 km (D > 10 km) NEAs are expected on the Earth in 1 Gyr, with about a half of impactors being dark primitive asteroids (most of which start with semimajor axis a > 2.5 au). These results explain why the Chicxulub crater, the third largest impact structure found on the Earth (diameter ≃ 180 km), was produced by impact of a carbonaceous chondrite. They suggest, when combined with previously published results for small (D . 1 km) NEAs, a size-dependent sampling of the main belt. We conclude that the impactor that triggered the K/Pg mass extinction ≃ 66 Myr ago was a main belt asteroid that quite likely (≃ 60% probability) originated beyond 2.5 au. Subject headings: Near-Earth objects; Asteroids, dynamics; Impact processes; Cratering; Astrobiology 1. Introduction arXiv:2107.03458v1 [astro-ph.EP] 7 Jul 2021 The Earth impact record accounts for ∼200 recognized crater structures and ∼50 de- posits (Schmieder and Kring, 2020). This collection is largely incomplete and contains severe biases. The impact age distribution, inferred from isotopic and stratigraphic analyses, shows that a great majority of preserved terrestrial craters formed in the last ∼650 Myr (Mazrouei et al., 2019; Keller et al., 2019).
    [Show full text]
  • Don Quixote – a Possible Parent Body of a Meteor Shower Regina Rudawska1 and Jérémie Vaubaillon2
    Proceedings of the IMC, Giron, 2014 1 Don Quixote – a possible parent body of a meteor shower Regina Rudawska1 and Jérémie Vaubaillon2 1Faculty of Mathematics, Physics and Informatics, Comenius University, Bratislava, Slovakia [email protected] 2IMCCE – Observatoire de Paris, Paris, France [email protected] Here we are interested in whether the meteoroid stream of (3552) Don Quixote can generate some observed meteor showers. We have showed that particles originating from Don Quixote particles produce two meteor showers at Earth: κ Lyrids and August μ Draconids. 1 (3552) Don Quixote below the conventional threshold value which assumed when establishing orbits similarity, i.e. 0.20 (Babadzhanov The (3552) Don Quixote asteroid was discovered in 1983 et al., 2013). Similarly, the values of DV are below the usual and categorized as Amor asteroid. The Tisserand parameter threshold value of 0.08 (Jopek et al., 2008; Rudawska et al., for the orbit has a value of 2,315 with respect to Jupiter, 2012). which indicates a comet-like orbit. The diameter of the object as calculated from the absolute magnitude is in the range of 12,3 – 24,5 km. This all makes Don Quixote a good candidate for a short-period comet among known NEOs, which has been confirmed by recent observations of some cometary activity (Momment et al., 2014). 2 Methodology We have investigated the orbital evolution of the meteoroid stream originating from Don Quixote. For this purpose, we modelled the generation and evolution of the meteoroid stream in the Solar System. The ejections of meteoroids from the asteroid's surface took place when the asteroid was passing its perihelion between 5000 B.C.
    [Show full text]
  • Near-Earth Objects 400 Years After Galileo: Physical Properties and Internal Structure
    Galileo’s Medicean Moons: their impact on 400 years of discovery Proceedings IAU Symposium No. 269, 2010 c International Astronomical Union 2010 C. Barbieri, S. Chakrabarti, M. Coradini & M. Lazzarin, eds. doi:10.1017/S1743921310007477 Near-Earth Objects 400 Years after Galileo: Physical Properties and Internal Structure Dmitrij Lupishko1 and Zhanna Pozhalova2 1 Institute of Astronomy of Kharkiv V. N. Karazin National University, Sumska str., 35, Kharkiv 61022, Ukraine email: [email protected] 2 Research Institute “Nikolaev Astronomical Observatory”, Observatornaya str. 1, Nikolaev 54030, Ukraine email: [email protected] Abstract. The review contains the most recent data on near-Earth objects such as their sizes and densities, rotation and shapes, taxonomy and mineralogy, optical properties and structure of their surfaces, binary systems among the NEOs and internal structure of asteroids and comets constituted the NEO population. Keywords. Asteroids, near-Earth objects, physical properties, internal structure. 1. Introduction Near-Earth objects (NEOs) are defined as asteroids and comets having orbits with perihelion distances of 1.3 AU or less. About 30% of the entire NEO population may reside in orbits having a Jovian Tisserand parameter <3, and among them roughly half are observed to have comet-like physical properties such as albedos and spectra. Thus, about 10-15% of the NEO population may be comprised by extinct or dormant comets (Lupishko & Lupishko 2001; Binzel & Lupishko 2006; Michel & Bottke 2009). The rest are the near-Earth asteroids, which are traditionally divided into three groups (the relative abundances are estimated by Bottke et al. (2002)): Amor a 1.0 AU 1.017 < q 1.3 AU (32 ± 1%) Apollo a 1.0 AU q < 1.017 AU (62 ± 1%) Aten a < 1.0 AU Q > 0.983 AU (6 ± 1%) Besides, there is an additional group of rather dangerous asteroids whose orbits reside entirely inside of the Earth’s one (Q < 0.983 AU).
    [Show full text]
  • Ice& Stone 2020
    Ice & Stone 2020 WEEK 45: NOVEMBER 1-7 Presented by The Earthrise Institute # 45 Authored by Alan Hale This week in history NOVEMBER 1 2 3 4 5 6 7 NOVEMBER 1, 1577: Observers in Peru make the first sighting of the Great Comet of 1577. This comet, a brilliant object which is often referred to as “Tycho Brahe’s Comet” and which is one of the most important scientific comets in history, is next week’s “Comet of the Week.” NOVEMBER 1, 1948: Observers on the ground near Nairobi, Kenya, as well as in a Royal Air Force plane flying at 4000 meters, detect a bright comet near the sun during a total solar eclipse. The Eclipse Comet of 1948 and other “eclipse comets” are the subject of a previous “Special Topics” presentation. NOVEMBER 1, 1975: University of California astronomer Martin Cohen publishes a paper announcing the likely presence of water ice surrounding the young solar-type star HL Tauri. A protoplanetary disk has since been detected surrounding this star. The significance of Cohen’s discovery is discussed in a previous “Special Topics” presentation. The protoplanetary disc surrounding the young star HL Tauri is seen in this sharp image from the Atacama Large Millimeter/submillimeter Array (ALMA) in Chile. It reveal substructures within the disc that have never been seen before and even show the possible positions of planets forming in the dark patches within the system. Courtesy ALMA (ESO/NAOJ/NRAO). NOVEMBER 1, 1998: A team led by William Merline discovers a moon, since named Petit-Prince, around the main-belt asteroid (45) Eugenia with the Canada-France-Hawaii Telescope at Mauna Kea.
    [Show full text]
  • NEAR EARTH ASTEROIDS (Neas) a CHRONOLOGY of MILESTONES 1800 - 2200
    INTERNATIONAL ASTRONOMICAL UNION UNION ASTRONOMIQUE INTERNATIONALE NEAR EARTH ASTEROIDS (NEAs) A CHRONOLOGY OF MILESTONES 1800 - 2200 8 July 2013 – version 41.0 on-line: www.iau.org/public/nea/ (completeness not pretended) INTRODUCTION Asteroids, or minor planets, are small and often irregularly shaped celestial bodies. The known majority of them orbit the Sun in the so-called main asteroid belt, between the orbits of the planets Mars and Jupiter. However, due to gravitational perturbations caused by planets as well as non- gravitational perturbations, a continuous migration brings main-belt asteroids closer to Sun, thus crossing the orbits of Mars, Earth, Venus and Mercury. An asteroid is coined a Near Earth Asteroid (NEA) when its trajectory brings it within 1.3 AU [Astronomical Unit; for units, see below in section Glossary and Units] from the Sun and hence within 0.3 AU of the Earth's orbit. The largest known NEA is 1036 Ganymed (1924 TD, H = 9.45 mag, D = 31.7 km, Po = 4.34 yr). A NEA is said to be a Potentially Hazardous Asteroid (PHA) when its orbit comes to within 0.05 AU (= 19.5 LD [Lunar Distance] = 7.5 million km) of the Earth's orbit, the so-called Earth Minimum Orbit Intersection Distance (MOID), and has an absolute magnitude H < 22 mag (i.e., its diameter D > 140 m). The largest known PHA is 4179 Toutatis (1989 AC, H = 15.3 mag, D = 4.6×2.4×1.9 km, Po = 4.03 yr). As of 3 July 2013: - 903 NEAs (NEOWISE in the IR, 1 February 2011: 911) are known with D > 1000 m (H < 17.75 mag), i.e., 93 ± 4 % of an estimated population of 966 ± 45 NEAs (NEOWISE in the IR, 1 February 2011: 981 ± 19) (see: http://targetneo.jhuapl.edu/pdfs/sessions/TargetNEO-Session2-Harris.pdf, http://adsabs.harvard.edu/abs/2011ApJ...743..156M), including 160 PHAs.
    [Show full text]