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The Composition of M-Type Asteroids II: Synthesis of Spectroscopic and Radar Observations ⇑ J.R
Icarus 238 (2014) 37–50 Contents lists available at ScienceDirect Icarus journal homepage: www.elsevier.com/locate/icarus The composition of M-type asteroids II: Synthesis of spectroscopic and radar observations ⇑ J.R. Neeley a,b,1, , B.E. Clark a,1, M.E. Ockert-Bell a,1, M.K. Shepard c,2, J. Conklin d, E.A. Cloutis e, S. Fornasier f, S.J. Bus g a Department of Physics, Ithaca College, Ithaca, NY 14850, United States b Department of Physics, Iowa State University, Ames, IA 50011, United States c Department of Geography and Geosciences, Bloomsburg University, Bloomsburg, PA 17815, United States d Department of Mathematics, Ithaca College, Ithaca, NY 14850, United States e Department of Geography, University of Winnipeg, Winnipeg, MB R3B 2E9, Canada f LESIA, Observatoire de Paris, 5 Place Jules Janssen, F-92195 Meudon Principal Cedex, France g Institute for Astronomy, 2680 Woodlawn Dr., Honolulu, HI 96822, United States article info abstract Article history: This work updates and expands on results of our long-term radar-driven observational campaign of Received 7 February 2012 main-belt asteroids (MBAs) focused on Bus–DeMeo Xc- and Xk-type objects (Tholen X and M class Revised 7 May 2014 asteroids) using the Arecibo radar and NASA Infrared Telescope Facilities (Ockert-Bell, M.E., Clark, B.E., Accepted 9 May 2014 Shepard, M.K., Rivkin, A.S., Binzel, R.P., Thomas, C.A., DeMeo, F.E., Bus, S.J., Shah, S. [2008]. Icarus 195, Available online 16 May 2014 206–219; Ockert-Bell, M.E., Clark, B.E., Shepard, M.K., Issacs, R.A., Cloutis, E.A., Fornasier, S., Bus, S.J. -
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. -
Alactic Observer Gjohn J
alactic Observer GJohn J. McCarthy Observatory Volume 5, No. 2 February 2012 Belly of the Beast At the center of the Milky Way galaxy, a gas cloud is on a perilous journey into a supermassive black hole. As the cloud stretches and accelerates, it gives away the location of its silent predator. For more information , see page 9 inside, or go to http://www.nasa.gov/ centers/goddard/news/topstory/2008/ blackhole_slumber.html. Credit: NASA/CXC/MIT/Frederick K. Baganoff et al. The John J. McCarthy Observatory Galactic Observvvererer New Milford High School Editorial Committee 388 Danbury Road Managing Editor New Milford, CT 06776 Bill Cloutier Phone/Voice: (860) 210-4117 Production & Design Phone/Fax: (860) 354-1595 Allan Ostergren www.mccarthyobservatory.org Website Development John Gebauer JJMO Staff Marc Polansky It is through their efforts that the McCarthy Observatory has Josh Reynolds established itself as a significant educational and recreational Technical Support resource within the western Connecticut community. Bob Lambert Steve Barone Allan Ostergren Dr. Parker Moreland Colin Campbell Cecilia Page Dennis Cartolano Joe Privitera Mike Chiarella Bruno Ranchy Jeff Chodak Josh Reynolds Route Bill Cloutier Barbara Richards Charles Copple Monty Robson Randy Fender Don Ross John Gebauer Ned Sheehey Elaine Green Gene Schilling Tina Hartzell Diana Shervinskie Tom Heydenburg Katie Shusdock Phil Imbrogno Jon Wallace Bob Lambert Bob Willaum Dr. Parker Moreland Paul Woodell Amy Ziffer In This Issue THE YEAR OF THE SOLAR SYSTEM ................................ 4 SUNRISE AND SUNSET .................................................. 11 OUT THE WINDOW ON YOUR LEFT ............................... 5 ASTRONOMICAL AND HISTORICAL EVENTS ...................... 11 FRA MAURA ................................................................ 5 REFERENCES ON DISTANCES ....................................... -
Modelling and Scaling Neglected Asteroids
Asteroid studies via lightcurves Selection effects TPM Shape models vs. occultations Summary Modelling and scaling neglected asteroids A. Marciniak1 with V. Alí-Lagoa, T. Müller, P. Bartczak, R. Behrend, M. Butkiewicz-B ˛ak, G. Dudzinski,´ R. Duffard, K. Dziadura, S. Fauvaud, M. Ferrais, S. Geier, J. Grice, R. Hirsch, J. Horbowicz, K. Kaminski,´ P. Kankiewicz, D.-H. Kim, M.-J. Kim, I. Konstanciak, V. Kudak, L. Molnár, F. Monteiro, W. Ogłoza, D. Oszkiewicz, A. Pál, N. Parley, F. Pilcher, E. Podlewska - Gaca, T. Polakis, J. J. Sanabria, T. Santana-Ros, B. Skiff, K. Sobkowiak, R. Szakáts, S. Urakawa, M. Zejmo,˙ K. Zukowski˙ 1. Astronomical Observatory Institute, Faculty of Physics, A. Mickiewicz University, Poznan,´ Poland ESOP XXXIX, 29 August 2020 Asteroid studies via lightcurves Selection effects TPM Shape models vs. occultations Summary Asteroid lightcurves (219) Thusnelda P = 59.74 h 487 Venetia P = 13.355h 2014 -2,1 Oct 11.1 Suhora 2012/2013 -2,2 Oct 12.1 Suhora Oct 29.0 Bor Oct 24.1 Bor. -2,05 Nov 10.2 Suh Oct 28.1 Bor. Nov 11.1 Suh CCCCCC Nov 4.0 Bor. CCCCCCCCC CC C C Nov 7.4 Organ M. Dec 28.8 Bor C Mar 2.8 Bor C Nov 8.4 Organ M. AAAA -2 Mar 3.8 Bor AAAAAA C Nov 13.4 Organ M. AAAA C CCC Nov 14.4 Organ M. A -2,1 AAA CCC A Nov 15.4 Organ M. A AA Nov 21.4 Winer -1,95 Dec 2.1 OAdM Dec 3.0 OAdM Dec 5.0 Bor. -
Deliverable H2020 COMPET-05-2015 Project "Small
Deliverable H2020 COMPET-05-2015 project "Small Bodies: Near And Far (SBNAF)" Topic: COMPET-05-2015 - Scientific exploitation of astrophysics, comets, and planetary data Project Title: Small Bodies Near and Far (SBNAF) Proposal No: 687378 - SBNAF - RIA Duration: Apr 1, 2016 - Mar 31, 2019 WP WP5 Del.No D5.3 Title Occultation candidates for 2018 Lead Beneficiary CSIC Nature Report Dissemination Level Public Est. Del. Date 20 Dec 2017 Version 1.0 Date 20 Dec 2017 Lead Author Pablo Santos-Sanz, Instituto de Astrofísica de Andalucía-CSIC, [email protected] WP5 Ground based observations Objectives: The main objective of WP5 is to execute observations from ground- based telescopes with the goal to acquire more data on the SBNAF targets. One of the scheduled observations is the occultation of a star by a Main Belt Asteroid (MBA), a Centaur or a Trans-Neptunian Object (TNO). For this particular stellar occultation technique the main tasks are: i) to predict the stellar occultation, ii) to coordinate the observations, and iii) to produce results on physical parameters of the MBAs, Centaurs and TNOs (i.e. sizes, shapes, albedos, densities, etc). Description of deliverable D5.3 The potential occultation candidates for 2018 are presented. This deliverable follows deliverables D5.1 and D5.2, and is related to milestones MS5 “Occultation predictions with 10 mas accuracy”, and MS12 “25 successful TNO occultation measurements”. In this document, we first give a short state of the art of the stellar occultation technique (Section 1), then we discuss about the expected goal to reach ~10 mas accuracy in the prediction of stellar occultations by TNOs (Section 2). -
Aqueous Alteration on Main Belt Primitive Asteroids: Results from Visible Spectroscopy1
Aqueous alteration on main belt primitive asteroids: results from visible spectroscopy1 S. Fornasier1,2, C. Lantz1,2, M.A. Barucci1, M. Lazzarin3 1 LESIA, Observatoire de Paris, CNRS, UPMC Univ Paris 06, Univ. Paris Diderot, 5 Place J. Janssen, 92195 Meudon Pricipal Cedex, France 2 Univ. Paris Diderot, Sorbonne Paris Cit´e, 4 rue Elsa Morante, 75205 Paris Cedex 13 3 Department of Physics and Astronomy of the University of Padova, Via Marzolo 8 35131 Padova, Italy Submitted to Icarus: November 2013, accepted on 28 January 2014 e-mail: [email protected]; fax: +33145077144; phone: +33145077746 Manuscript pages: 38; Figures: 13 ; Tables: 5 Running head: Aqueous alteration on primitive asteroids Send correspondence to: Sonia Fornasier LESIA-Observatoire de Paris arXiv:1402.0175v1 [astro-ph.EP] 2 Feb 2014 Batiment 17 5, Place Jules Janssen 92195 Meudon Cedex France e-mail: [email protected] 1Based on observations carried out at the European Southern Observatory (ESO), La Silla, Chile, ESO proposals 062.S-0173 and 064.S-0205 (PI M. Lazzarin) Preprint submitted to Elsevier September 27, 2018 fax: +33145077144 phone: +33145077746 2 Aqueous alteration on main belt primitive asteroids: results from visible spectroscopy1 S. Fornasier1,2, C. Lantz1,2, M.A. Barucci1, M. Lazzarin3 Abstract This work focuses on the study of the aqueous alteration process which acted in the main belt and produced hydrated minerals on the altered asteroids. Hydrated minerals have been found mainly on Mars surface, on main belt primitive asteroids and possibly also on few TNOs. These materials have been produced by hydration of pristine anhydrous silicates during the aqueous alteration process, that, to be active, needed the presence of liquid water under low temperature conditions (below 320 K) to chemically alter the minerals. -
The Minor Planet Bulletin 37 (2010) 45 Classification for 244 Sita
THE MINOR PLANET BULLETIN OF THE MINOR PLANETS SECTION OF THE BULLETIN ASSOCIATION OF LUNAR AND PLANETARY OBSERVERS VOLUME 37, NUMBER 2, A.D. 2010 APRIL-JUNE 41. LIGHTCURVE AND PHASE CURVE OF 1130 SKULD Robinson (2009) from his data taken in 2002. There is no evidence of any change of (V-R) color with asteroid rotation. Robert K. Buchheim Altimira Observatory As a result of the relatively short period of this lightcurve, every 18 Altimira, Coto de Caza, CA 92679 (USA) night provided at least one minimum and maximum of the [email protected] lightcurve. The phase curve was determined by polling both the maximum and minimum points of each night’s lightcurve. Since (Received: 29 December) The lightcurve period of asteroid 1130 Skuld is confirmed to be P = 4.807 ± 0.002 h. Its phase curve is well-matched by a slope parameter G = 0.25 ±0.01 The 2009 October-November apparition of asteroid 1130 Skuld presented an excellent opportunity to measure its phase curve to very small solar phase angles. I devoted 13 nights over a two- month period to gathering photometric data on the object, over which time the solar phase angle ranged from α = 0.3 deg to α = 17.6 deg. All observations used Altimira Observatory’s 0.28-m Schmidt-Cassegrain telescope (SCT) working at f/6.3, SBIG ST- 8XE NABG CCD camera, and photometric V- and R-band filters. Exposure durations were 3 or 4 minutes with the SNR > 100 in all images, which were reduced with flat and dark frames. -
Spectroscopic Survey of X-Type Asteroids S
Spectroscopic Survey of X-type Asteroids S. Fornasier, B.E. Clark, E. Dotto To cite this version: S. Fornasier, B.E. Clark, E. Dotto. Spectroscopic Survey of X-type Asteroids. Icarus, Elsevier, 2011, 10.1016/j.icarus.2011.04.022. hal-00768793 HAL Id: hal-00768793 https://hal.archives-ouvertes.fr/hal-00768793 Submitted on 24 Dec 2012 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. Accepted Manuscript Spectroscopic Survey of X-type Asteroids S. Fornasier, B.E. Clark, E. Dotto PII: S0019-1035(11)00157-6 DOI: 10.1016/j.icarus.2011.04.022 Reference: YICAR 9799 To appear in: Icarus Received Date: 26 December 2010 Revised Date: 22 April 2011 Accepted Date: 26 April 2011 Please cite this article as: Fornasier, S., Clark, B.E., Dotto, E., Spectroscopic Survey of X-type Asteroids, Icarus (2011), doi: 10.1016/j.icarus.2011.04.022 This is a PDF file of an unedited manuscript that has been accepted for publication. As a service to our customers we are providing this early version of the manuscript. The manuscript will undergo copyediting, typesetting, and review of the resulting proof before it is published in its final form. -
The Minor Planet Bulletin
THE MINOR PLANET BULLETIN OF THE MINOR PLANETS SECTION OF THE BULLETIN ASSOCIATION OF LUNAR AND PLANETARY OBSERVERS VOLUME 35, NUMBER 3, A.D. 2008 JULY-SEPTEMBER 95. ASTEROID LIGHTCURVE ANALYSIS AT SCT/ST-9E, or 0.35m SCT/STL-1001E. Depending on the THE PALMER DIVIDE OBSERVATORY: binning used, the scale for the images ranged from 1.2-2.5 DECEMBER 2007 – MARCH 2008 arcseconds/pixel. Exposure times were 90–240 s. Most observations were made with no filter. On occasion, e.g., when a Brian D. Warner nearly full moon was present, an R filter was used to decrease the Palmer Divide Observatory/Space Science Institute sky background noise. Guiding was used in almost all cases. 17995 Bakers Farm Rd., Colorado Springs, CO 80908 [email protected] All images were measured using MPO Canopus, which employs differential aperture photometry to determine the values used for (Received: 6 March) analysis. Period analysis was also done using MPO Canopus, which incorporates the Fourier analysis algorithm developed by Harris (1989). Lightcurves for 17 asteroids were obtained at the Palmer Divide Observatory from December 2007 to early The results are summarized in the table below, as are individual March 2008: 793 Arizona, 1092 Lilium, 2093 plots. The data and curves are presented without comment except Genichesk, 3086 Kalbaugh, 4859 Fraknoi, 5806 when warranted. Column 3 gives the full range of dates of Archieroy, 6296 Cleveland, 6310 Jankonke, 6384 observations; column 4 gives the number of data points used in the Kervin, (7283) 1989 TX15, 7560 Spudis, (7579) 1990 analysis. Column 5 gives the range of phase angles. -
RASNZ Occultation Section Circular CN2009/1 April 2013 NOTICES
ISSN 11765038 (Print) RASNZ ISSN 23241853 (Online) OCCULTATION CIRCULAR CN2009/1 April 2013 SECTION Lunar limb Profile produced by Dave Herald's Occult program showing 63 events for the lunar graze of a bright, multiple star ZC2349 (aka Al Niyat, sigma Scorpi) on 31 July 2009 by two teams of observers from Wellington and Christchurch. The lunar profile is drawn using data from the Kaguya lunar surveyor, which became available after this event. The path the star followed across the lunar landscape is shown for one set of observers (Murray Forbes and Frank Andrews) by the trail of white circles. There are several instances where a stepped event was seen, due to the two brightest components disappearing or reappearing. See page 61 for more details. Visit the Occultation Section website at http://www.occultations.org.nz/ Newsletter of the Occultation Section of the Royal Astronomical Society of New Zealand Table of Contents From the Director.............................................................................................................................. 2 Notices................................................................................................................................................. 3 Seventh TransTasman Symposium on Occultations............................................................3 Important Notice re Report File Naming...............................................................................4 Observing Occultations using Video: A Beginner's Guide.................................................. -
Asteroid Observations at Low Phase Angles. IV. Average Parameters for the New H, G1, G2 Magnitude System Vasilij G
Planetary and Space Science ∎ (∎∎∎∎) ∎∎∎–∎∎∎ Contents lists available at ScienceDirect Planetary and Space Science journal homepage: www.elsevier.com/locate/pss Asteroid observations at low phase angles. IV. Average parameters for the new H, G1, G2 magnitude system Vasilij G. Shevchenko a,b,n, Irina N. Belskaya a, Karri Muinonen c,d, Antti Penttilä c, Yurij N. Krugly a, Feodor P. Velichko a, Vasilij G. Chiorny a, Ivan G. Slyusarev a,b, Ninel M. Gaftonyuk e, Igor A. Tereschenko a a Institute of Astronomy of Kharkiv Karazin National University, Sumska str. 35, Kharkiv 61022, Ukraine b Department of Astronomy and Space Informatics of Kharkiv Karazin National University, Svobody sqr. 4, Kharkiv 61022, Ukraine c Department of Physics, University of Helsinki, P.O. Box 64, FI-00014, Finland d Finnish Geospatial Research Institute, P.O. Box 15, Masala, FI-02431, Finland e Crimean Astrophysical Observatory, Crimea, Simeiz 98680, Ukraine article info abstract Article history: We present new observational data for selected main-belt asteroids of different compositional types. The Received 21 January 2015 detailed magnitude–phase dependences including small phase angles (o1°) were obtained for these Received in revised form asteroids, namely: (10) Hygiea (down to the phase angle of 0.3°, C-type), (176) Iduna (0.2°, G-type), (214) 6 September 2015 Aschera (0.2°, E-type), (218) Bianca (0.3°, S-type), (250) Bettina (0.3°, M-type), (419) Aurelia (0.1°, F-type), Accepted 19 November 2015 (596) Scheila (0.2°, D-type), (635) Vundtia (0.2°, B-type), (671) Carnegia (0.2°, P-type), (717) Wisibada (0.1°, T-type), (1021) Flammario (0.6°, B-type), and (1279) Uganda (0.5°, E-type). -
The Ch-‐Class Asteroids
The Ch-class asteroids: Connecting a visible taxonomic class to a 3-µm band shape Andrew S. Rivkin1*, Cristina A. Thomas2+, Ellen S. Howell3*^, Joshua P. Emery4* 1. The Johns Hopkins University Applied Physics Laboratory 2. NASA Goddard Space Flight Center, 3. Arecibo Observatory, USRA 4. University of Tennessee Accepted to The Astronomical Journal 3 November 2015 *Visiting 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. +Currently also at the Planetary Science Institute. Work done while supported by an appointment to the NASA Postdoctoral Program, administered by Oak Ridge Associated Universities through a contract with NASA. ^Currently at Lunar and Planetary Laboratory, University of Arizona, Tucson AZ Abstract Asteroids belonging to the Ch spectral taxonomic class are defined by the presence of an absorption near 0.7 μm, which is interpreted as due to Fe-bearing phyllosilicates. Phyllosilicates also cause strong absorptions in the 3-μm region, as do other hydrated and hydroxylated minerals and H2O ice. Over the past decade, spectral observations have revealed different 3-µm band shapes the asteroid population. Although a formal taxonomy is yet to be fully established, the “Pallas-type” spectral group is most consistent with the presence of phyllosilicates. If Ch class and Pallas type are both indicative of phyllosilicates, then all Ch-class asteroids should also be Pallas-type. In order to test this hypothesis, we obtained 42 observations of 36 Ch-class asteroids in the 2- to 4-µm spectral region.