Spectroscopy of B-Type Asteroids: Subgroups and Meteorite Analogs
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Asteroid Shape and Spin Statistics from Convex Models J
Asteroid shape and spin statistics from convex models J. Torppa, V.-P. Hentunen, P. Pääkkönen, P. Kehusmaa, K. Muinonen To cite this version: J. Torppa, V.-P. Hentunen, P. Pääkkönen, P. Kehusmaa, K. Muinonen. Asteroid shape and spin statistics from convex models. Icarus, Elsevier, 2008, 198 (1), pp.91. 10.1016/j.icarus.2008.07.014. hal-00499092 HAL Id: hal-00499092 https://hal.archives-ouvertes.fr/hal-00499092 Submitted on 9 Jul 2010 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 Asteroid shape and spin statistics from convex models J. Torppa, V.-P. Hentunen, P. Pääkkönen, P. Kehusmaa, K. Muinonen PII: S0019-1035(08)00283-2 DOI: 10.1016/j.icarus.2008.07.014 Reference: YICAR 8734 To appear in: Icarus Received date: 18 September 2007 Revised date: 3 July 2008 Accepted date: 7 July 2008 Please cite this article as: J. Torppa, V.-P. Hentunen, P. Pääkkönen, P. Kehusmaa, K. Muinonen, Asteroid shape and spin statistics from convex models, Icarus (2008), doi: 10.1016/j.icarus.2008.07.014 This is a PDF file of an unedited manuscript that has been accepted for publication. -
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. -
PACS Sky Fields and Double Sources for Photometer Spatial Calibration
Document: PACS-ME-TN-035 PACS Date: 27th July 2009 Herschel Version: 2.7 Fields and Double Sources for Spatial Calibration Page 1 PACS Sky Fields and Double Sources for Photometer Spatial Calibration M. Nielbock1, D. Lutz2, B. Ali3, T. M¨uller2, U. Klaas1 1Max{Planck{Institut f¨urAstronomie, K¨onigstuhl17, D-69117 Heidelberg, Germany 2Max{Planck{Institut f¨urExtraterrestrische Physik, Giessenbachstraße, D-85748 Garching, Germany 3NHSC, IPAC, California Institute of Technology, Pasadena, CA 91125, USA Document: PACS-ME-TN-035 PACS Date: 27th July 2009 Herschel Version: 2.7 Fields and Double Sources for Spatial Calibration Page 2 Contents 1 Scope and Assumptions 4 2 Applicable and Reference Documents 4 3 Stars 4 3.1 Optical Star Clusters . .4 3.2 Bright Binaries (V -band search) . .5 3.3 Bright Binaries (K-band search) . .5 3.4 Retrieval from PACS Pointing Calibration Target List . .5 3.5 Other stellar sources . 13 3.5.1 Herbig Ae/Be stars observed with ISOPHOT . 13 4 Galactic ISOCAM fields 13 5 Galaxies 13 5.1 Quasars and AGN from the Veron catalogue . 13 5.2 Galaxy pairs . 14 5.2.1 Galaxy pairs from the IRAS Bright Galaxy Sample with VLA radio observations 14 6 Solar system objects 18 6.1 Asteroid conjunctions . 18 6.2 Conjunctions of asteroids with pointing stars . 22 6.3 Planetary satellites . 24 Appendices 26 A 2MASS images of fields with suitable double stars from the K-band 26 B HIRES/2MASS overlays for double stars from the K-band search 32 C FIR/NIR overlays for double galaxies 38 C.1 HIRES/2MASS overlays for double galaxies . -
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. -
A Spectral Comparison of (379) Huenna and Its Satellite ⇑ Francesca E
Icarus 212 (2011) 677–681 Contents lists available at ScienceDirect Icarus journal homepage: www.elsevier.com/locate/icarus A spectral comparison of (379) Huenna and its satellite ⇑ Francesca E. DeMeo a,b, ,1, Benoît Carry c,b,d, Franck Marchis e, Mirel Birlan f,1, Richard P. Binzel a,f, Schelte J. Bus g, Pascal Descamps f, Alin Nedelcu f,h,1, Michael Busch i, Hervé Bouy c a Department of Earth, Atmospheric, and Planetary Sciences, Massachusetts Institute of Technology, 77 Massachusetts Avenue, Cambridge, MA 02139, USA b LESIA, Observatoire de Paris, 5 Place Jules Janssen, 92195 Meudon Principal Cedex, France c European Space Astronomy Centre, ESA, P.O. Box 78, 28691 Villanueva de la Cañada, Madrid, Spain d Université Paris 7 Denis-Diderot, 5 rue Thomas Mann, 75205 Paris Cedex, France e University of California at Berkeley, Dept. Of Astronomy, 601 Campbell Hall, Berkeley, CA 94720, USA f IMCCE, UMR8028 CNRS, Observatoire de Paris, 77 avenue Denfert-Rochereau, 75014 Paris Cedex, France g Institute for Astronomy, 640 N. Aohoku Place, Hilo, HI 96720, USA h Astronomical Institute of the Romanian Academy, 5 Cutßitul de Argint, RO-75212 Bucharest, Romania i Department of Earth and Space Sciences, University of California Los Angeles, 595 Charles Young Dr. E., Los Angeles, CA 90095, USA article info abstract Article history: We present near-infrared spectral measurements of Themis family Asteroid (379) Huenna (D 98 km) Received 17 June 2010 and its 6 km satellite using SpeX on the NASA IRTF. The companion was farther than 1.500 from the pri- Revised 2 February 2011 mary at the time of observations and was approximately 5 magnitudes dimmer. -
Clasificación Taxonómica De Asteroides
Clasificación Taxonómica de Asteroides Cercanos a la Tierra por Ana Victoria Ojeda Vera Tesis sometida como requisito parcial para obtener el grado de MAESTRO EN CIENCIAS EN CIENCIA Y TECNOLOGÍA DEL ESPACIO en el Instituto Nacional de Astrofísica, Óptica y Electrónica Agosto 2019 Tonantzintla, Puebla Bajo la supervisión de: Dr. José Ramón Valdés Parra Investigador Titular INAOE Dr. José Silviano Guichard Romero Investigador Titular INAOE c INAOE 2019 El autor otorga al INAOE el permiso de reproducir y distribuir copias parcial o totalmente de esta tesis. II Dedicatoria A mi familia, con gran cariño. A mis sobrinos Ian y Nahil, y a mi pequeña Lia. III Agradecimientos Gracias a mi familia por su apoyo incondicional. A mi mamá Tere, por enseñarme a ser perseverante y dedicada, y por sus miles de muestras de afecto. A mi hermana Fernanda, por darme el tiempo, consejos y cariño que necesitaba. A mi pareja Odi, por su amor y cariño estos tres años, por su apoyo, paciencia y muchas horas de ayuda en la maestría, pero sobre todo por darme el mejor regalo del mundo, nuestra pequeña Lia. Gracias a mis asesores Dr. José R. Valdés y Dr. José S. Guichard, promotores de esta tesis, por su paciencia, consejos y supervisión, y por enseñarme con sus clases divertidas y motivadoras todo lo que se refiere a este trabajo. A los miembros del comité, Dra. Raquel Díaz, Dr. Raúl Mújica y Dr. Sergio Camacho, por tomarse el tiempo de revisar y evaluar mi trabajo. Estoy muy agradecida con todos por sus críticas constructivas y sugerencias. -
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. -
2011 HP: a Potentially Water-Rich Near-Earth Asteroid. Teague, S.1, Hicks, M.2
2011 HP: A Potentially Water-Rich Near-Earth Asteroid. Teague, S.1, Hicks, M.2 1-Victor Valley College 2-Jet Propulsion Laboratory, California Institute of Technology Abstract Broadband photometry was obtained to provide data on 2011 HP, a Near-Earth Object (NEO) discovered April 24, 2011. Our data was collected over a series of three nights using the 0.6 m telescope located at Table Mountain Observatory (TMO) in Wrightwood, California. The data was used to construct a solar phase curve for the object which, along with our measured broadband colors, allowed us to determine that the object most likely has a low albedo and a surface composition similar to the carbonaceous chondrite meteorites, which tend to be water-rich. 2011 HP appears to have a Xc type spectral classification, determined by comparison of our rotationally averaged colors (B-R=1.110+/-0.031 mag; V-R=0.393+/-0.030 mag; R-I=0.367+/-0.045 mag) against the 1341 asteroid spectra in the SMASS II database. We assumed a double-peaked lightcurve and were able to determine a period of 3.95+/-0.01 hr. Assuming a low albedo as suggested by the solar phase curve, we estimate the diameter of the object to be ~250 meters, and given that the minimum orbital intersection distance (MOID) equals 0.0274 AU, we recommend that this particular meteorite be re-classified as a Potentially Hazardous Asteroid by the Minor Planet Center. Introduction Asteroid impact craters dot the surface of our Earth as a visual reminder of the ever-present possibility of collisions of space debris with our home planet. -
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 Veritas and Themis Asteroid Families: 5-14Μm Spectra with The
Icarus 269 (2016) 62–74 Contents lists available at ScienceDirect Icarus journal homepage: www.elsevier.com/locate/icarus The Veritas and Themis asteroid families: 5–14 μm spectra with the Spitzer Space Telescope Zoe A. Landsman a,∗, Javier Licandro b,c, Humberto Campins a, Julie Ziffer d, Mario de Prá e, Dale P. Cruikshank f a Department of Physics, University of Central Florida, 4111 Libra Drive, PS 430, Orlando, FL 32826, United States b Instituto de Astrofísica de Canarias, C/Vía Láctea s/n, 38205, La Laguna, Tenerife, Spain c Departamento de Astrofísica, Universidad de La Laguna, E-38205, La Laguna, Tenerife, Spain d Department of Physics, University of Southern Maine, 96 Falmouth St, Portland, ME 04103, United States e Observatório Nacional, R. General José Cristino, 77 - Imperial de São Cristóvão, Rio de Janeiro, RJ 20921-400, Brazil f NASA Ames Research Center, MS 245-6, Moffett Field, CA 94035, United States article info abstract Article history: Spectroscopic investigations of primitive asteroid families constrain family evolution and composition and Received 18 October 2015 conditions in the solar nebula, and reveal information about past and present distributions of volatiles in Revised 30 December 2015 the solar system. Visible and near-infrared studies of primitive asteroid families have shown spectral di- Accepted 8 January 2016 versity between and within families. Here, we aim to better understand the composition and physical Available online 14 January 2016 properties of two primitive families with vastly different ages: ancient Themis (∼2.5 Gyr) and young Ver- Keywords: itas (∼8 Myr). We analyzed the 5 – 14 μm Spitzer Space Telescope spectra of 11 Themis-family asteroids, Asteroids including eight previously studied by Licandro et al. -
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. -
Asteroid Photometric and Polarimetric Phase Curves: Joint Linear-Exponential Modeling
Meteoritics & Planetary Science 44, Nr 12, 1937–1946 (2009) Abstract available online at http://meteoritics.org Asteroid photometric and polarimetric phase curves: Joint linear-exponential modeling K. MUINONEN1, 2, A. PENTTILÄ1, A. CELLINO3, I. N. BELSKAYA4, M. DELBÒ5, A. C. LEVASSEUR-REGOURD6, and E. F. TEDESCO7 1University of Helsinki, Observatory, Kopernikuksentie 1, P.O. BOX 14, FI-00014 U. Helsinki, Finland 2Finnish Geodetic Institute, Geodeetinrinne 2, P.O. Box 15, FI-02431 Masala, Finland 3INAF-Osservatorio Astronomico di Torino, strada Osservatorio 20, 10025 Pino Torinese, Italy 4Astronomical Institute of Kharkiv National University, 35 Sumska Street, 61035 Kharkiv, Ukraine 5IUMR 6202 Laboratoire Cassiopée, Observatoire de la Côte d’Azur, BP 4229, 06304 Nice, Cedex 4, France 6UPMC Univ. Paris 06, UMR 7620, BP3, 91371 Verrières, France 7Planetary Science Institute, 1700 E. Ft. Lowell Road, Tucson, Arizona 85719, USA *Corresponding author. E-mail: [email protected] (Received 01 April, 2009; revision accepted 18 August 2009) Abstract–We present Markov-Chain Monte-Carlo methods (MCMC) for the derivation of empirical model parameters for photometric and polarimetric phase curves of asteroids. Here we model the two phase curves jointly at phase angles գ25° using a linear-exponential model, accounting for the opposition effect in disk-integrated brightness and the negative branch in the degree of linear polarization. We apply the MCMC methods to V-band phase curves of asteroids 419 Aurelia (taxonomic class F), 24 Themis (C), 1 Ceres (G), 20 Massalia (S), 55 Pandora (M), and 64 Angelina (E). We show that the photometric and polarimetric phase curves can be described using a common nonlinear parameter for the angular widths of the opposition effect and negative-polarization branch, thus supporting the hypothesis of common physical mechanisms being responsible for the phenomena.