Pole Coordinates and Shape of 30 Asteroids
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ESO's VLT Sphere and DAMIT
ESO’s VLT Sphere and DAMIT ESO’s VLT SPHERE (using adaptive optics) and Joseph Durech (DAMIT) have a program to observe asteroids and collect light curve data to develop rotating 3D models with respect to time. Up till now, due to the limitations of modelling software, only convex profiles were produced. The aim is to reconstruct reliable nonconvex models of about 40 asteroids. Below is a list of targets that will be observed by SPHERE, for which detailed nonconvex shapes will be constructed. Special request by Joseph Durech: “If some of these asteroids have in next let's say two years some favourable occultations, it would be nice to combine the occultation chords with AO and light curves to improve the models.” 2 Pallas, 7 Iris, 8 Flora, 10 Hygiea, 11 Parthenope, 13 Egeria, 15 Eunomia, 16 Psyche, 18 Melpomene, 19 Fortuna, 20 Massalia, 22 Kalliope, 24 Themis, 29 Amphitrite, 31 Euphrosyne, 40 Harmonia, 41 Daphne, 51 Nemausa, 52 Europa, 59 Elpis, 65 Cybele, 87 Sylvia, 88 Thisbe, 89 Julia, 96 Aegle, 105 Artemis, 128 Nemesis, 145 Adeona, 187 Lamberta, 211 Isolda, 324 Bamberga, 354 Eleonora, 451 Patientia, 476 Hedwig, 511 Davida, 532 Herculina, 596 Scheila, 704 Interamnia Occultation Event: Asteroid 10 Hygiea – Sun 26th Feb 16h37m UT The magnitude 11 asteroid 10 Hygiea is expected to occult the magnitude 12.5 star 2UCAC 21608371 on Sunday 26th Feb 16h37m UT (= Mon 3:37am). Magnitude drop of 0.24 will require video. DAMIT asteroid model of 10 Hygiea - Astronomy Institute of the Charles University: Josef Ďurech, Vojtěch Sidorin Hygiea is the fourth-largest asteroid (largest is Ceres ~ 945kms) in the Solar System by volume and mass, and it is located in the asteroid belt about 400 million kms away. -
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. -
Occultation Newsletter Volume 8, Number 4
Volume 12, Number 1 January 2005 $5.00 North Am./$6.25 Other International Occultation Timing Association, Inc. (IOTA) In this Issue Article Page The Largest Members Of Our Solar System – 2005 . 4 Resources Page What to Send to Whom . 3 Membership and Subscription Information . 3 IOTA Publications. 3 The Offices and Officers of IOTA . .11 IOTA European Section (IOTA/ES) . .11 IOTA on the World Wide Web. Back Cover ON THE COVER: Steve Preston posted a prediction for the occultation of a 10.8-magnitude star in Orion, about 3° from Betelgeuse, by the asteroid (238) Hypatia, which had an expected diameter of 148 km. The predicted path passed over the San Francisco Bay area, and that turned out to be quite accurate, with only a small shift towards the north, enough to leave Richard Nolthenius, observing visually from the coast northwest of Santa Cruz, to have a miss. But farther north, three other observers video recorded the occultation from their homes, and they were fortuitously located to define three well- spaced chords across the asteroid to accurately measure its shape and location relative to the star, as shown in the figure. The dashed lines show the axes of the fitted ellipse, produced by Dave Herald’s WinOccult program. This demonstrates the good results that can be obtained by a few dedicated observers with a relatively faint star; a bright star and/or many observers are not always necessary to obtain solid useful observations. – David Dunham Publication Date for this issue: July 2005 Please note: The date shown on the cover is for subscription purposes only and does not reflect the actual publication date. -
Observations from Orbiting Platforms 219
Dotto et al.: Observations from Orbiting Platforms 219 Observations from Orbiting Platforms E. Dotto Istituto Nazionale di Astrofisica Osservatorio Astronomico di Torino M. A. Barucci Observatoire de Paris T. G. Müller Max-Planck-Institut für Extraterrestrische Physik and ISO Data Centre A. D. Storrs Towson University P. Tanga Istituto Nazionale di Astrofisica Osservatorio Astronomico di Torino and Observatoire de Nice Orbiting platforms provide the opportunity to observe asteroids without limitation by Earth’s atmosphere. Several Earth-orbiting observatories have been successfully operated in the last decade, obtaining unique results on asteroid physical properties. These include the high-resolu- tion mapping of the surface of 4 Vesta and the first spectra of asteroids in the far-infrared wave- length range. In the near future other space platforms and orbiting observatories are planned. Some of them are particularly promising for asteroid science and should considerably improve our knowledge of the dynamical and physical properties of asteroids. 1. INTRODUCTION 1800 asteroids. The results have been widely presented and discussed in the IRAS Minor Planet Survey (Tedesco et al., In the last few decades the use of space platforms has 1992) and the Supplemental IRAS Minor Planet Survey opened up new frontiers in the study of physical properties (Tedesco et al., 2002). This survey has been very important of asteroids by overcoming the limits imposed by Earth’s in the new assessment of the asteroid population: The aster- atmosphere and taking advantage of the use of new tech- oid taxonomy by Barucci et al. (1987), its recent extension nologies. (Fulchignoni et al., 2000), and an extended study of the size Earth-orbiting satellites have the advantage of observing distribution of main-belt asteroids (Cellino et al., 1991) are out of the terrestrial atmosphere; this allows them to be in just a few examples of the impact factor of this survey. -
Guide to the Extended Versions of MPC Data Files Based on the MPCORB Format
Guide to the Extended Versions of MPC Data Files Based on the MPCORB Format Last updated: 2016/04/19 by J.L. Galache Introduction The Minor Planet Center (MPC) has been providing the orbits of minor planets in the form of a file, MPCORB.DAT, since the mid '90s (1990s, not 1890s). Back then there were only a few thousand known asteroids, compared to the several hundred thousand of today, so a flat text file was the appropriate way to circulate these data. It was also a time when most orbit computations were programmed in Fortran, which ingested data no other way. MPCORB.DAT has therefore always been, and continues to be, a fixed-width file (see Table 1 for the current format description1). In fact, all original data files available on the MPC website are flat text files (even the orbits files provided for planetarium-type/sky simulation software packages are simply text files of varying format2). In the early years of the 2010s, possibly due to the rising popularity of the scripting language Python amongst astronomers, and an increased interest from developers wanting to write asteroid-themed tools, requests were received to provide data in other, easier to parse formats, e.g., JSON, CSV, SQL, etc. At the same time, astronomers and developers alike wanted more information than was currently been provided in MPCORB.DAT; information that did exist on the MPC website in other, often hard to find, files. Here was an opportunity to add some new data to existing files, while also making them available in other formats. -
~XECKDING PAGE BLANK WT FIL,,Q
1,. ,-- ,-- ~XECKDING PAGE BLANK WT FIL,,q DYNAMICAL EVIDENCE REGARDING THE RELATIONSHIP BETWEEN ASTEROIDS AND METEORITES GEORGE W. WETHERILL Department of Temcltricrl kgnetism ~amregie~mtittition of Washington Washington, D. C. 20025 Meteorites are fragments of small solar system bodies (comets, asteroids and Apollo objects). Therefore they may be expected to provide valuable information regarding these bodies. How- ever, the identification of particular classes of meteorites with particular small bodies or classes of small bodies is at present uncertain. It is very unlikely that any significant quantity of meteoritic material is obtained from typical ac- tive comets. Relatively we1 1-studied dynamical mechanisms exist for transferring material into the vicinity of the Earth from the inner edge of the asteroid belt on an 210~-~year time scale. It seems likely that most iron meteorites are obtained in this way, and a significant yield of complementary differec- tiated meteoritic silicate material may be expected to accom- pany these differentiated iron meteorites. Insofar as data exist, photometric measurements support an association between Apollo objects and chondri tic meteorites. Because Apol lo ob- jects are in orbits which come close to the Earth, and also must be fragmented as they traverse the asteroid belt near aphel ion, there also must be a component of the meteorite flux derived from Apollo objects. Dynamical arguments favor the hypothesis that most Apollo objects are devolatilized comet resiaues. However, plausible dynamical , petrographic, and cosmogonical reasons are known which argue against the simple conclusion of this syllogism, uiz., that chondri tes are of cometary origin. Suggestions are given for future theoretical , observational, experimental investigations directed toward improving our understanding of this puzzling situation. -
Chaotic Diffusion of the Vesta Family Induced by Close Encounters with Massive Asteroids
A&A 540, A118 (2012) Astronomy DOI: 10.1051/0004-6361/201118339 & c ESO 2012 Astrophysics Chaotic diffusion of the Vesta family induced by close encounters with massive asteroids J.-B. Delisle and J. Laskar ASD, IMCCE-CNRS UMR8028, Observatoire de Paris, UPMC, 77 Av. Denfert-Rochereau, 75014 Paris, France e-mail: [email protected] Received 26 October 2011 / Accepted 1 March 2012 ABSTRACT We numerically estimate the semi-major axis chaotic diffusion of the Vesta family asteroids induced by close encounters with 11 mas- sive main-belt asteroids: (1) Ceres, (2) Pallas, (3) Juno, (4) Vesta, (7) Iris, (10) Hygiea, (15) Eunomia, (19) Fortuna, (324) Bamberga, (532) Herculina, (704) Interamnia. We find that most of the diffusion is caused by Ceres and Vesta. By extrapolating our results, we are able to constrain the global effect of close encounters with all main-belt asteroids. A comparison of this drift estimate with the one expected for the Yarkovsky effect shows that for asteroids whose diameter is larger than about 40 km, close encounters dominate the Yarkovsky effect. Overall, our findings confirm the standard scenario for the history of the Vesta family. Key words. celestial mechanics – minor planets, asteroids: general – chaos – methods: numerical 1. Introduction (in terms of the number of asteroids taken into account) con- cerned the Gefion and Adeona families and was conducted by It is now common consent that most of the V-type near-Earth as- Carruba et al. (2003). The authors considered all 682 asteroids teroids (NEAs) and howardite, eucrite, and diogenite (HED) me- of radius larger than 50 km for encounters with members of teorites are fragments of a collision between Vesta and another the families. -
16 Minor Planet Bulletin 40 (2013)
16 bimodal but has some indication of flattening of the maximums. LIGHTCURVES FOR 1394 ALGOA, 3078 HORROCKS, 4874 Burke was observed by Aymani (2012), who obtained a 4724 BROCKEN, AND 6329 HIKONEJYO period of 3.657 ± 0.001 and amplitude A = 0.31 mag. Menzies FROM ETSCORN CAMPUS OBSERVATORY (2012) obtained a period of 3.656 ± 0.001 and an amplitude of 0.23 ± 0.02 mag. Daniel A. Klinglesmith III, Ethan Risley, Janek Turk, Angelica Vargas, Curtis Warren The 115° longitude difference between the Etscorn Campus Etscorn Campus Observatory Observatory and the Bigmuskie Observatory allowed almost an 8 New Mexico Tech hour (~0.3) phase shift for 3948 Bohr. This allowed us to cover the 101 East Road nearly 24-hour sidereal period asteroid completely. This type of Socorro, NM, USA 87801 international collaboration is essential for asteroid with periods [email protected] near 24 hours. The collaboration continued with the observations of 4874 Burke’s 3.657-hour period (Received: 6 September) Between 2012 March and June, four asteroids were observed at the Etscorn Campus Observatory. Synodic periods and amplitudes were determined for all four: 1394 Algoa, P = 2.768 ± 0.001 h, A = 0.21 ± 0.10 mag; 3078 Horrocks, P = 13.620 ± 0.003 h, A = 0.25 ± 0.10 mag; 4724 Brocken, P = 5.912 ± 0.001 h, A = 0.75 ± 0.10 mag; and 6329 Hikonejyo, P = 6.064 ± 0.001 h, A = 0.23 ± 0.10 mag. Continuing with the lightcurve program at Etscorn Campus Observatory, we obtained data for four asteroids using our two Celestron 35.6-cm f/11 Schmidt-Cassegrain telescopes and SBIG STL-1001E CCD cameras with 1024x1024x24-micron pixels. -
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, 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. -
Iso and Asteroids
r bulletin 108 Figure 1. Asteroid Ida and its moon Dactyl in enhanced colour. This colour picture is made from images taken by the Galileo spacecraft just before its closest approach to asteroid 243 Ida on 28 August 1993. The moon Dactyl is visible to the right of the asteroid. The colour is ‘enhanced’ in the sense that the CCD camera is sensitive to near-infrared wavelengths of light beyond human vision; a ‘natural’ colour picture of this asteroid would appear mostly grey. Shadings in the image indicate changes in illumination angle on the many steep slopes of this irregular body, as well as subtle colour variations due to differences in the physical state and composition of the soil (regolith). There are brighter areas, appearing bluish in the picture, around craters on the upper left end of Ida, around the small bright crater near the centre of the asteroid, and near the upper right-hand edge (the limb). This is a combination of more reflected blue light and greater absorption of near-infrared light, suggesting a difference Figure 2. This image mosaic of asteroid 253 Mathilde is in the abundance or constructed from four images acquired by the NEAR spacecraft composition of iron-bearing on 27 June 1997. The part of the asteroid shown is about 59 km minerals in these areas. Ida’s by 47 km. Details as small as 380 m can be discerned. The moon also has a deeper near- surface exhibits many large craters, including the deeply infrared absorption and a shadowed one at the centre, which is estimated to be more than different colour in the violet than any 10 km deep. -
Planck Collaboration: ERCSC the Cosmic Microwave Background (CMB)
Astronomy & Astrophysics manuscript no. 16474ms c ESO 2011 August 15, 2011 Planck Early Results. VII. The Early Release Compact Source Catalogue Planck Collaboration: P. A. R. Ade76, N. Aghanim50, M. Arnaud63, M. Ashdown61,4, J. Aumont50, C. Baccigalupi74, A. Balbi30, A. J. Banday82,8,68, R. B. Barreiro57, J. G. Bartlett3,59, E. Battaner84, K. Benabed51, A. Benoˆıt49, J.-P. Bernard82,8, M. Bersanelli27,43, R. Bhatia5, A. Bonaldi39, L. Bonavera74,6, J. R. Bond7, J. Borrill67,78, F. R. Bouchet51, M. Bucher3, C. Burigana42, R. C. Butler42, P. Cabella30, C. M. Cantalupo67, B. Cappellini43, J.-F. Cardoso64,3,51, P. Carvalho4, A. Catalano3,62, L. Cay´on20, A. Challinor54,61,11, A. Chamballu47, R.-R. Chary48⋆, X. Chen48, L.-Y Chiang53, C. Chiang19, P. R. Christensen71,31, D. L. Clements47, S. Colombi51, F. Couchot66, A. Coulais62, B. P. Crill59,72, F. Cuttaia42, L. Danese74, R. J. Davis60, P. de Bernardis26, A. de Rosa42, G. de Zotti39,74, J. Delabrouille3, J.-M. Delouis51, F.-X. D´esert45, C. Dickinson60, J. M. Diego57, K. Dolag68, H. Dole50, S. Donzelli43,55, O. Dor´e59,9, U. D¨orl68, M. Douspis50, X. Dupac34, G. Efstathiou54, T. A. Enßlin68, H. K. Eriksen55, F. Finelli42, O. Forni82,8, P. Fosalba52, M. Frailis41, E. Franceschi42, S. Galeotta41, K. Ganga3,48, M. Giard82,8, Y. Giraud-H´eraud3, J. Gonz´alez-Nuevo74, K. M. G´orski59,86, S. Gratton61,54, A. Gregorio28, A. Gruppuso42, J. Haissinski66, F. K. Hansen55, D. Harrison54,61, G. Helou9, S. Henrot-Versill´e66, C. Hern´andez-Monteagudo68 , D. Herranz57, S. R. Hildebrandt9,65,56, E.