Mission Update: June 2017

Total Page:16

File Type:pdf, Size:1020Kb

Mission Update: June 2017 Mission Update: June 2017 Lucy Lim Assistant Project Scientist NASA/Goddard Space Flight Center Small Bodies Assessment Group 2017 June Powered On – Nominal ■ Powered Off – Nominal ■ SPACECRAFT SNAPSHOT STATUS Not powered since launch ■ 6-June-2017 Suspect ■ Issue ■ C&DH ■■ Thermal ■ IMU ■■ EPS ■ RWAs ■■■■ Solar Panels ■ LIDARs ■■ SATAGs ■ Star Trackers ■■ Propulsion ■ TAGSAM ■ SRC ■ SPACECRAFT ■ OLA ■ O – SamCam ■ O – PolyCam ■ O – MapCam ■ LGA -X ■ REXIS ■ MGA ■ T – NavCam ■ LGA +X* ■ T – StowCam ■ HGA* ■ *HGA/TWTA-1 in OTES ■ SDST ■■ contact, +X LGA/TWTA- OVIRS ■ TWTA* ■■ 2 carrier only PAYLOADS TELECOM Navigation Status Current Orbit Diagram As of June 07, 2017, Launch+271 days: Earth Range = 0.53 AU (↓) Sun Range = 1.23 AU (↑) Sun-Probe-Earth Angle = 54 deg (↓) One Way Light Time = 04:20 mm:ss (↓) Round Trip Light Time = 08:40 mm:ss (↓) 3 Recent and Upcoming Mission Activities • First science activity: Earth Trojan Asteroid Search, Feb. 2017 • Participating Scientist Program (Asteroid Operations) Step-2 due 11 July 2017 • Launch + 10-month Calibrations • 2017-07-26 through 2017-08-03: OVIRS, OCAMS calibrations; OTES, OLA, REXIS checkouts • 2017-08-13 through 2017-08-16: REXIS Solar X-ray Monitor (“SXM”) calibration • Earth Gravity Assist (“EGA”), 22 Sept. 2017 • Observations on EGA+1d, +3d, +6d, contingency +10d • Asteroid Arrival at (101955) Bennu, Fall 2018 4 Goals of OSIRIS-REx Earth Trojan Asteroid Search • Observing geometry for L4 region was superior to that from Earth • Closer to objects • Lower phase angle OSIRIS-REx on Feb 9 • One disadvantage: OCAMS MapCam has small aperture (1.5”) so brighter limiting magnitude than Earth-based systems • Operational test of OSIRIS-REx • First science observations by mission • Test of spacecraft and OCAMS instrument performance OSIRIS-REx on L4 on Feb 9 • Test of J-Asteroid science planning and commanding Feb 20 tool • Test of astronomical software and data reduction processes • Dry run of 10-cm natural satellite searches to be conducted at Bennu • Dry run of OpNav image planning and reductions L4 on Feb 20 (Jupiter as target) • Lessons learned during the Earth Trojan search are already influencing planning of near-Bennu observations Earth Trojan Asteroid Search: Feb. 9-20, 2017 • Daily mosaic of 3x3 MapCam fields visited 5 times over ~4.2 hours (~51 min between visits) • Each visit consisted of 1 10-s and 2 30-s Pan images • Total of 90 fields and 1350 images as part of ETAS science observations • Estimate of what we could have detected at a MapCam limiting magnitude of 14.0 in 30s exposures: • On Feb 9: • for phase angle of 0°, range of 0.04 au • H = 20.9 = diameter of 180 to 400m • On Feb 18: • for phase angle of 0°, range of 0.01 au • H = 23.6 = diameter of 50 to 110m • cf. PanSTARRS, Catalina limit of H~19 for L4 objects (Tricarico 2015) Earth Trojan Asteroid Search: What we found • Zero Earth Trojan asteroids • 17 Main belt asteroids were detected • 12 Victoria V=10.4 Feb 11/12 • 36 Atalante V=13.3 Feb 11/12 • 47 Aglaja V=12.0 Feb 13/14/17 • 55 Pandora V=12.0 Feb 19/20 • 112 Iphigenia V=13.4 Feb 14 • 144 Vibilia V=12.5 Feb 13 • 172 Baucis V=12.3 Feb 11/12 • 230 Athamantis V=10.5 Feb 11/12 • 245 Vera V=13.0 Feb 14/17 • 247 Eukrate V=12.6 Feb 11/12 • 248 Lameia V=13.2 Feb 20 • 250 Bettina V=12.2 Feb 19/20 • 258 Tyche V=12.9 Feb 13/14/17/18 • 327 Columbia V=13.8 Feb 10 • 332 Siri V=13.7 Feb 09 • 720 Bohlinia V=13.6 Feb 09 • 1013 Tombecka V=13.1 Feb 13/14/17/18 • Also detected one planet (Jupiter) and four natural satellites (Europa, Io, Ganymede, Callisto) • Catalina Sky Survey (CSS) asteroid detection software • Ongoing analysis by Saverio Cambioni and Renu Malhotra Earth Gravity Assist: 2017-09-22 Earth Gravity Assist: 2017-09-22 Earth Gravity Assist: Earth Range (km) and Earth/Moon Phase Angles • Sept. 22, 2017 16:53 UTC • Time of Closest Approach • EGA @ range of 25k km 3500000 180 Earth Range 170 160 Earth Phase Angle Moon Range 150 2625000 140 Moon Phase Angle Lockheed Blackout 130 120 Lockheed Blackout Instrument Observation Window 110 100 1750000 Instrument Observation Window 90 Range (km) 80 70 60 875000 Phase Angle (degrees) 50 40 30 20 10 0 -96. -71.6 -47.2 -22.8 1.6 26. 50.4 74.8 99.2 123.6 148. 0 -96. -71.6 -47.2 -22.8 1.6 26. 50.4 74.8 99.2 123.6 148. Time until Closest Approach (hours) Time until closest approach (hours) EGA: Instrument FOVs Relative to Earth NavCam SamCam MapCam PolyCam OTES OVIRS EGA + 6 d EGA + 9 h EGA + 3 d EGA + 4 h EGA + 1 day • Flat Field Check (NavCam1) OVIRS FOV in light blue • OpNav Rehearsal of Bennu & 4th Magnitude Star OTES FOV in purple Imaging • Earth stands-in for Bennu and its calculated position with respect to background stars will be used to estimate OpNav uncertainty. • Extended Object Radiometry Check (NavCam1 & NavCam2) • OTES/OVIRS Earth Observations (Spectral Calibration / Alignment between OTES/OVIRS/OCAMS) • Observation Type: Rasterscan Slews (8 N-S, 8 E-W) • Instruments: OVIRS, OTES, MapCam (during N-S slews), PolyCam (during E-W slews), SamCam (during E-W slews) • Earth Diameter: 80 to 70 mrad • OCAMS Absolute Responsivity (Earth and Moon) • Moon Limb Imaging (NavCam1) EGA + 3 days • OTES/OVIRS Moon Observations (Spectral Calibration / Alignment between OVIRS FOV OTES/OVIRS/OCAMS) • Sep 25, 2017 – 00:20 – 01:20 UT • Target: Moon • Observation Type: Rasterscan Slews (4 N-S, 4 E-W) • Instrument: OVIRS, OTES, MapCam (during N-S slews), PolyCam (during E-W slews), SamCam (during E-W slews) • Moon Diameter: 3 mrad • Moon Limb Imaging (NavCam1 & NavCam2) • OCAMS Absolute Responsivity (Earth and Moon) • OTES/OVIRS Earth Observations (Spectral Calibration / Alignment between OTES/OVIRS/OCAMS) • Sep 25, 2017 – 03:40 – 04:40 UT • Target: Earth • Observation Type: Rasterscan Slews (4 N-S, 4 E-W) • Instrument: OVIRS, OTES EGA + 6 Days • Similar to EGA + 3 days Sep 28, 2017 – 01:40 – 02:00 UT Target: Earth • Sep 28, 2017 – 00:00 UT Observation Type: Point and Stare Mosaic (5x1 mosaic) • Science Observation Window Start Instrument: PolyCam Pan filter • Sep 28, 2017 – 00:00 – 00:20 UT Focus @ infinity (17371) • Slew to first target 10 light + 6 dark exposures Repeat MapCam and PolyCam observations three times • OTES/OVIRS Earth Observations (Spectral Calibration / Alignment between OTES/OVIRS/OCAMS) • Sep 28, 2017 – 00:20 – 01:20 UT Moon Limb Imaging • Target: Earth Sep 25, 2017 – 03:40 – 04:40 UT • Observation Type: Rasterscan Slews (4 N-S, 4 E-W) Target: Moon • Instrument: OVIRS, OTES, MapCam (during N-S slews), PolyCam Observation Type: Point and Stare Mosaic (1x3 mosaic) (during E-W slews) Instrument: NavCam1 and NavCam2 • OVIRS/OTES Deep Space and Internal Calibrations before and after 27 + 18 = 45 light exposures slews (5 min before and after) • OVIRS Solar Calibrator after slews (10 minutes) • MapCam 10 light + 16 dark exposures Sep 28, 2017 – 04:40 UT • PolyCam 40 light + 4 dark exposures Slew back to s/c nominal position • Absolute Responsivity (Earth and Moon) Sep 28, 2017 – 05:00 UT • Sep 28, 2017 – 01:20 – 01:40 UT Science Observation Window end • Target: Earth Earth • Observation Type: Point and Stare Mosaic (5x1 mosaic) • Instrument: MapCam • Pan, b’, v, w, x filters • 50 light + 16 dark exposures JOIN THE MISSION ON THE WEB! 15 Backup 16 .
Recommended publications
  • CAPTURE of TRANS-NEPTUNIAN PLANETESIMALS in the MAIN ASTEROID BELT David Vokrouhlický1, William F
    The Astronomical Journal, 152:39 (20pp), 2016 August doi:10.3847/0004-6256/152/2/39 © 2016. The American Astronomical Society. All rights reserved. CAPTURE OF TRANS-NEPTUNIAN PLANETESIMALS IN THE MAIN ASTEROID BELT David Vokrouhlický1, William F. Bottke2, and David Nesvorný2 1 Institute of Astronomy, Charles University, V Holešovičkách 2, CZ–18000 Prague 8, Czech Republic; [email protected] 2 Department of Space Studies, Southwest Research Institute, 1050 Walnut Street, Suite 300, Boulder, CO 80302; [email protected], [email protected] Received 2016 February 9; accepted 2016 April 21; published 2016 July 26 ABSTRACT The orbital evolution of the giant planets after nebular gas was eliminated from the Solar System but before the planets reached their final configuration was driven by interactions with a vast sea of leftover planetesimals. Several variants of planetary migration with this kind of system architecture have been proposed. Here, we focus on a highly successful case, which assumes that there were once five planets in the outer Solar System in a stable configuration: Jupiter, Saturn, Uranus, Neptune, and a Neptune-like body. Beyond these planets existed a primordial disk containing thousands of Pluto-sized bodies, ∼50 million D > 100 km bodies, and a multitude of smaller bodies. This system eventually went through a dynamical instability that scattered the planetesimals and allowed the planets to encounter one another. The extra Neptune-like body was ejected via a Jupiter encounter, but not before it helped to populate stable niches with disk planetesimals across the Solar System. Here, we investigate how interactions between the fifth giant planet, Jupiter, and disk planetesimals helped to capture disk planetesimals into both the asteroid belt and first-order mean-motion resonances with Jupiter.
    [Show full text]
  • 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.
    [Show full text]
  • 107 Minor Planet Bulletin 37(2010) LIGHTCURVE PHOTOMETRY of 112 IPHIGENIA Stefan Cikota Physik-Institut, Universität Zürich, W
    107 LIGHTCURVE PHOTOMETRY OF 112 IPHIGENIA Stefan Cikota Physik-Institut, Universität Zürich, Winterthurerstrasse 190, CH-8057 Zürich, SWITZERLAND and Observatorio Astronomico de Mallorca 07144 Costitx, Mallorca, Illes Balears, SPAIN [email protected] Aleksandar Cikota Physik-Institut, Universität Zürich, CH-8057 Zürich, SWITZERLAND and Observatorio Astronomico de Mallorca MINOR PLANET LIGHTCURVE ANALYSIS OF 07144 Costitx, Mallorca, Illes Balears, SPAIN 347 PARIANA AND 6560 PRAVDO (Received: 19 March) Peter Caspari BDI Observatory PO Box 194 Regents Park The main-belt asteroid 112 Iphigenia was observed over NSW 2143, AUSTRALIA 6 nights between 2007 December 9 and December 14 at [email protected] the Observatorio Astronomico de Mallorca (620). From the resulting data, we determined a synodic rotation (Received: 15 January Revised: 22 February) period of 31.385 ± 0.006 h and lightcurve amplitude of 0.30 ± 0.02 mag. Minor planet 347 Pariana was observed in 2009 July and again in 2009 August and September resulting in two 122 Iphigenia was tracked over 6 nights between 2007 December complete lightcurves both with a rotational period 9 and December 14 with one, and sometimes two, identical estimate of 4.052 ± 0.002 h and amplitude of 0.5 mag. telescopes (0.30-m f/9 Schmidt-Cassegrain) located at the These data were combined with data from previous Observatorio Astronomico de Mallorca in Spain. Both were apparitions to produce estimates for a sidereal period, equipped with an SBIG STL-1001E CCD camera. Image spin axis, and shape model. Minor planet 6560 Pravdo acquisition and calibration were performed using Maxim DL. All was observed over nine nights in 2009 June and July 1593 images were unfiltered and had exposures of 60 seconds.
    [Show full text]
  • CURRICULUM VITAE, ALAN W. HARRIS Personal: Born
    CURRICULUM VITAE, ALAN W. HARRIS Personal: Born: August 3, 1944, Portland, OR Married: August 22, 1970, Rose Marie Children: W. Donald (b. 1974), David (b. 1976), Catherine (b 1981) Education: B.S. (1966) Caltech, Geophysics M.S. (1967) UCLA, Earth and Space Science PhD. (1975) UCLA, Earth and Space Science Dissertation: Dynamical Studies of Satellite Origin. Advisor: W.M. Kaula Employment: 1966-1967 Graduate Research Assistant, UCLA 1968-1970 Member of Tech. Staff, Space Division Rockwell International 1970-1971 Physics instructor, Santa Monica College 1970-1973 Physics Teacher, Immaculate Heart High School, Hollywood, CA 1973-1975 Graduate Research Assistant, UCLA 1974-1991 Member of Technical Staff, Jet Propulsion Laboratory 1991-1998 Senior Member of Technical Staff, Jet Propulsion Laboratory 1998-2002 Senior Research Scientist, Jet Propulsion Laboratory 2002-present Senior Research Scientist, Space Science Institute Appointments: 1976 Member of Faculty of NATO Advanced Study Institute on Origin of the Solar System, Newcastle upon Tyne 1977-1978 Guest Investigator, Hale Observatories 1978 Visiting Assoc. Prof. of Physics, University of Calif. at Santa Barbara 1978-1980 Executive Committee, Division on Dynamical Astronomy of AAS 1979 Visiting Assoc. Prof. of Earth and Space Science, UCLA 1980 Guest Investigator, Hale Observatories 1983-1984 Guest Investigator, Lowell Observatory 1983-1985 Lunar and Planetary Review Panel (NASA) 1983-1992 Supervisor, Earth and Planetary Physics Group, JPL 1984 Science W.G. for Voyager II Uranus/Neptune Encounters (JPL/NASA) 1984-present Advisor of students in Caltech Summer Undergraduate Research Fellowship Program 1984-1985 ESA/NASA Science Advisory Group for Primitive Bodies Missions 1985-1993 ESA/NASA Comet Nucleus Sample Return Science Definition Team (Deputy Chairman, U.S.
    [Show full text]
  • The Minor Planet Bulletin 44 (2017) 142
    THE MINOR PLANET BULLETIN OF THE MINOR PLANETS SECTION OF THE BULLETIN ASSOCIATION OF LUNAR AND PLANETARY OBSERVERS VOLUME 44, NUMBER 2, A.D. 2017 APRIL-JUNE 87. 319 LEONA AND 341 CALIFORNIA – Lightcurves from all sessions are then composited with no TWO VERY SLOWLY ROTATING ASTEROIDS adjustment of instrumental magnitudes. A search should be made for possible tumbling behavior. This is revealed whenever Frederick Pilcher successive rotational cycles show significant variation, and Organ Mesa Observatory (G50) quantified with simultaneous 2 period software. In addition, it is 4438 Organ Mesa Loop useful to obtain a small number of all-night sessions for each Las Cruces, NM 88011 USA object near opposition to look for possible small amplitude short [email protected] period variations. Lorenzo Franco Observations to obtain the data used in this paper were made at the Balzaretto Observatory (A81) Organ Mesa Observatory with a 0.35-meter Meade LX200 GPS Rome, ITALY Schmidt-Cassegrain (SCT) and SBIG STL-1001E CCD. Exposures were 60 seconds, unguided, with a clear filter. All Petr Pravec measurements were calibrated from CMC15 r’ values to Cousins Astronomical Institute R magnitudes for solar colored field stars. Photometric Academy of Sciences of the Czech Republic measurement is with MPO Canopus software. To reduce the Fricova 1, CZ-25165 number of points on the lightcurves and make them easier to read, Ondrejov, CZECH REPUBLIC data points on all lightcurves constructed with MPO Canopus software have been binned in sets of 3 with a maximum time (Received: 2016 Dec 20) difference of 5 minutes between points in each bin.
    [Show full text]
  • Asteroid Regolith Weathering: a Large-Scale Observational Investigation
    University of Tennessee, Knoxville TRACE: Tennessee Research and Creative Exchange Doctoral Dissertations Graduate School 5-2019 Asteroid Regolith Weathering: A Large-Scale Observational Investigation Eric Michael MacLennan University of Tennessee, [email protected] Follow this and additional works at: https://trace.tennessee.edu/utk_graddiss Recommended Citation MacLennan, Eric Michael, "Asteroid Regolith Weathering: A Large-Scale Observational Investigation. " PhD diss., University of Tennessee, 2019. https://trace.tennessee.edu/utk_graddiss/5467 This Dissertation is brought to you for free and open access by the Graduate School at TRACE: Tennessee Research and Creative Exchange. It has been accepted for inclusion in Doctoral Dissertations by an authorized administrator of TRACE: Tennessee Research and Creative Exchange. For more information, please contact [email protected]. To the Graduate Council: I am submitting herewith a dissertation written by Eric Michael MacLennan entitled "Asteroid Regolith Weathering: A Large-Scale Observational Investigation." I have examined the final electronic copy of this dissertation for form and content and recommend that it be accepted in partial fulfillment of the equirr ements for the degree of Doctor of Philosophy, with a major in Geology. Joshua P. Emery, Major Professor We have read this dissertation and recommend its acceptance: Jeffrey E. Moersch, Harry Y. McSween Jr., Liem T. Tran Accepted for the Council: Dixie L. Thompson Vice Provost and Dean of the Graduate School (Original signatures are on file with official studentecor r ds.) Asteroid Regolith Weathering: A Large-Scale Observational Investigation A Dissertation Presented for the Doctor of Philosophy Degree The University of Tennessee, Knoxville Eric Michael MacLennan May 2019 © by Eric Michael MacLennan, 2019 All Rights Reserved.
    [Show full text]
  • Ground-Based Visible Spectroscopy of Asteroids to Support the Development of an Unsupervised Gaia Asteroid Taxonomy A
    Ground-based visible spectroscopy of asteroids to support the development of an unsupervised Gaia asteroid taxonomy A. Cellino, Ph. Bendjoya, M. Delbo’, Laurent Galluccio, J. Gayon-Markt, P. Tanga, E.F. Tedesco To cite this version: A. Cellino, Ph. Bendjoya, M. Delbo’, Laurent Galluccio, J. Gayon-Markt, et al.. Ground-based visible spectroscopy of asteroids to support the development of an unsupervised Gaia asteroid tax- onomy. Astronomy and Astrophysics - A&A, EDP Sciences, 2020, 10.1051/0004-6361/202038246. hal-02942763 HAL Id: hal-02942763 https://hal.archives-ouvertes.fr/hal-02942763 Submitted on 12 Dec 2020 HAL is a multi-disciplinary open access L’archive ouverte pluridisciplinaire HAL, est archive for the deposit and dissemination of sci- destinée au dépôt et à la diffusion de documents entific research documents, whether they are pub- scientifiques de niveau recherche, publiés ou non, lished or not. The documents may come from émanant des établissements d’enseignement et de teaching and research institutions in France or recherche français ou étrangers, des laboratoires abroad, or from public or private research centers. publics ou privés. Astronomy & Astrophysics manuscript no. TNGspectra2ndrev c ESO 2020 July 28, 2020 Ground-based visible spectroscopy of asteroids to support development of an unsupervised Gaia asteroid taxonomy A. Cellino1, Ph. Bendjoya2, M. Delbo’3, L. Galluccio3, J. Gayon-Markt3, P. Tanga3, and E. F. Tedesco4 1 INAF, Osservatorio Astrofisico di Torino, via Osservatorio 20, 10025 Pino Torinese, Italy e-mail: [email protected] 2 Université de la Côte d’Azur - Observatoire de la Côte d’Azur, CNRS, Laboratoire Lagrange, Campus Valrose Nice, Nice Cedex 4, France e-mail: [email protected] 3 Université Côte d’Azur, Observatoire de la Côte d’Azur, CNRS, Laboratoire Lagrange, Boulevard de l’Observatoire, CS34229, 06304, Nice Cedex 4, France e-mail: [email protected], [email protected], [email protected] 4 Planetary Science Institute, Tucson, AZ, USA e-mail: [email protected] Received ..., 2020; accepted ..., 2020 ABSTRACT Context.
    [Show full text]
  • The Minor Planet Bulletin, Alan W
    THE MINOR PLANET BULLETIN OF THE MINOR PLANETS SECTION OF THE BULLETIN ASSOCIATION OF LUNAR AND PLANETARY OBSERVERS VOLUME 42, NUMBER 2, A.D. 2015 APRIL-JUNE 89. ASTEROID LIGHTCURVE ANALYSIS AT THE OAKLEY SOUTHERN SKY OBSERVATORY: 2014 SEPTEMBER Lucas Bohn, Brianna Hibbler, Gregory Stein, Richard Ditteon Rose-Hulman Institute of Technology, CM 171 5500 Wabash Avenue, Terre Haute, IN 47803, USA [email protected] (Received: 24 November) Photometric data were collected over the course of seven nights in 2014 September for eight asteroids: 1334 Lundmarka, 1904 Massevitch, 2571 Geisei, 2699 Kalinin, 3197 Weissman, 7837 Mutsumi, 14927 Satoshi, and (29769) 1999 CE28. Eight asteroids were remotely observed from the Oakley Southern Sky Observatory in New South Wales, Australia. The observations were made on 2014 September 12-14, 16-19 using a 0.50-m f/8.3 Ritchey-Chretien optical tube assembly on a Paramount ME mount and SBIG STX-16803 CCD camera, binned 3x3, with a luminance filter. Exposure times ranged from 90 to 180 sec depending on the magnitude of the target. The resulting image scale was 1.34 arcseconds per pixel. Raw images were processed in MaxIm DL 6 using twilight flats, bias, and dark frames. MPO Canopus was used to measure the processed images and produce lightcurves. In order to maximize the potential for data collection, target asteroids were selected based upon their position in the sky approximately one hour after sunset. Only asteroids with no previously published results were targeted. Lightcurves were produced for 1334 Lundmarka, 1904 Massevitch, 2571 Geisei, 3197 Weissman, and (29769) 1999 CE28.
    [Show full text]
  • Acuaua91 T;; I) C9r~Lbaeµ
    acuaua91 t;; I) c9r~lbaeµ Volume 8, Number 2 August 2000 $5.00 North Am./$6.25 Other Revised Edition Occultation of SAO 118158 by (308) Polyxo, 2000 Jan. 10 I 50 , , -p,G,\\hid',",'l:°a"Z"i""""^ Elliptical Fit 2a = 154 ±5 km ,,,,, ,,\NR'¶ 2b = 126 ±4 km ,µj{'" |,'i °'"'—1>,, Xc = -287 ±2 km P d' ,6a,n 'j"\\"yS" " , '.' \ Yc _ +12 +4 km b ,L— ', Ca"\ , ' ;, S,,\otd, SP' "\ PAf = 63° +4° 2 Go\ben, Ok\a· F\ ,N'jgenL " "\ ' J,1-r\ags,a\, p'(\1-""" ""! j.,Aob"n' ,,,/ / , <,4- € _!L >- ~ ,..-- " , -1C|Q 1 X (km) International Occultation Timing Association, Inc. (IOTA) International Occultation Timing Association, Inc. In this Issue Articles Page IOTA News. .4 GPS Time for Occultations. 4 GPS Precision with Selective Availability Off . 6 A Spectacular Naked Eye Asteroid Occultation Over North America . .6 The Tycho-2 Star Catalogue . 7 Beware - Watts Profile Too Low for Northern-Limit Waning Phase Grazing Occultations . 7 1999 Leonid Meteor Impacts on the Moon, The Observing Campaign . 8 Heliga Bode, 1949 March 10 - 2000 June 1 . 8 IOTA’s Role in the Dog Bone Asteroid Discovery . 9 Confirmed Lunar Meteor Impacts From the November 1999 Leonids . 10 The Newly Discovered Binary Star 44 Eta Librae . .12 Asteroid 12753 Povenmire . 12 Occultations of Mercury, the Sun, & Venus seen in 3 Days . 12 New Double Stars . .13 The 1999 IOTA Annual Meeting . .17 Resources Page What to Send to Whom . .3 Membership and Subscription Information . .3 IOTA Publications . .3 The Offices and Officers of IOTA. 22 IOTA European Service (IOTA/ES).
    [Show full text]
  • (K)Cudos at Ψtucson
    (K)CUDOs at ΨTucson Work based on collaborative effort with present/former AZ students: Jeremiah Birrell and Lance Labun with contributions from exchange student from Germany Ch. Dietl. Johann Rafelski (UA-Physics) (K)CUDOS at ΨTucson PSITucson,April11,2013 1/39 1. Introduction 2. Dark Matter (CDM) Generalities 3. Strangeletts 4. Dark Matter (DM) CUDOs 5. CUDO impacts Johann Rafelski (UA-Physics) (K)CUDOS at ΨTucson PSITucson,April11,2013 2/39 kudos (from Greek kyddos, singular) = honor; glory; acclaim; praise kudo = back formation from kudos construed as a plural cud (Polish, pronounced c-ood) = miracle cudo (colloq. Polish) = of surprising and exceptional character CUDO=Compact UltraDense Object: A new opportunity to search for dark matter. Not dark matter in form of elementary particles (all present day searches) but (self) bound dark matter. Either an ultra-compact impactor or/and condensation seed for comets. There is a lot of dark matter around, cosmological abundance limit shown below. Johann Rafelski (UA-Physics) (K)CUDOS at ΨTucson PSITucson,April11,2013 3/39 A new type of meteors What if there are ‘dark’ matter meteor and asteroid-like bodies in the Universe? Could some of them have collided with solar system bodies and the Earth? Are they dressed in visible matter from prior impacts and as condensation seeds? CUDOs’ high density of gravitating matter provides the distinct observable, the surface-penetrating puncture: shot through Only a fraction of the kinetic energy damaging the solid surface. Johann Rafelski (UA-Physics) (K)CUDOS at ΨTucson PSITucson,April11,2013 4/39 Asteroids of high density Fruitful Discussions with Marshall Eubanks lead to these data.
    [Show full text]
  • Appendix 1 1311 Discoverers in Alphabetical Order
    Appendix 1 1311 Discoverers in Alphabetical Order Abe, H. 28 (8) 1993-1999 Bernstein, G. 1 1998 Abe, M. 1 (1) 1994 Bettelheim, E. 1 (1) 2000 Abraham, M. 3 (3) 1999 Bickel, W. 443 1995-2010 Aikman, G. C. L. 4 1994-1998 Biggs, J. 1 2001 Akiyama, M. 16 (10) 1989-1999 Bigourdan, G. 1 1894 Albitskij, V. A. 10 1923-1925 Billings, G. W. 6 1999 Aldering, G. 4 1982 Binzel, R. P. 3 1987-1990 Alikoski, H. 13 1938-1953 Birkle, K. 8 (8) 1989-1993 Allen, E. J. 1 2004 Birtwhistle, P. 56 2003-2009 Allen, L. 2 2004 Blasco, M. 5 (1) 1996-2000 Alu, J. 24 (13) 1987-1993 Block, A. 1 2000 Amburgey, L. L. 2 1997-2000 Boattini, A. 237 (224) 1977-2006 Andrews, A. D. 1 1965 Boehnhardt, H. 1 (1) 1993 Antal, M. 17 1971-1988 Boeker, A. 1 (1) 2002 Antolini, P. 4 (3) 1994-1996 Boeuf, M. 12 1998-2000 Antonini, P. 35 1997-1999 Boffin, H. M. J. 10 (2) 1999-2001 Aoki, M. 2 1996-1997 Bohrmann, A. 9 1936-1938 Apitzsch, R. 43 2004-2009 Boles, T. 1 2002 Arai, M. 45 (45) 1988-1991 Bonomi, R. 1 (1) 1995 Araki, H. 2 (2) 1994 Borgman, D. 1 (1) 2004 Arend, S. 51 1929-1961 B¨orngen, F. 535 (231) 1961-1995 Armstrong, C. 1 (1) 1997 Borrelly, A. 19 1866-1894 Armstrong, M. 2 (1) 1997-1998 Bourban, G. 1 (1) 2005 Asami, A. 7 1997-1999 Bourgeois, P. 1 1929 Asher, D.
    [Show full text]
  • Tim Cooper, Keynote Address
    The contribution of Southern African Amateur Observations to Professional Astronomical Studies Tim Cooper 1 Serious Amateur Astronomy: Linking with Professionals Observing Sections of ASSA • Comet and Meteor Tim Cooper • Deep Sky Section Auke Slotegraaf • Double Stars Chris Middleton • Occultations Brian Fraser • Solar Jacques van Delft • Variable Stars Brian Fraser 2 Serious Amateur Astronomy: Linking with Professionals Past, Present and Future • Variable Stars • Comets, Meteors, Asteroids 3 Serious Amateur Astronomy: Linking with Professionals Variable Stars • 654000 of 13 million observations – plus 70000 from A W Roberts project • Mattei 2002, ASSA contributions • Henden 2006 – Visual - historical observations 1800’s – Visual - eruptive variables – CCD - fainter variables, smaller amplitude 4 Serious Amateur Astronomy: Linking with Professionals Variable Stars • Intrinsic – Pulsating – Eruptive – Cataclysmic • Extrinsic Around 38,000 – Eclipsing 200 monitored – Rotating 5 Serious Amateur Astronomy: Linking with Professionals Prolific Variable Star observers by era A W Roberts 1891-1932 70,121 J F Skjellerup 1915-1948 6,733 H E Houghton 1926-1942 25,589 R P de Kock 1934-1973 160,777 M D Overbeek 1952-2001 287,150 L A G Monard 1992- +40,000 6 Serious Amateur Astronomy: Linking with Professionals 7 Serious Amateur Astronomy: Linking with Professionals T Pic Blue (at left) = SKQ, J. Skjellerup (1915-1948) Yellow = DK, R. De Kock (1934-1973) Purple = LOA, A. Long (1917-1927) White = OB, D. Overbeek (1952-2001) Green = SMW, W. Smith (1924-1931)
    [Show full text]