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Non-Principal Axis Rotation (Tumbling) Asteroids
NON-PRINCIPAL AXIS ROTATION (TUMBLING) ASTEROIDS Asteroid PAR Per1 Amp1 Per2 Amp2 Reference 244 Sita T0 129.51 0.82 0 129.51 0.82 Brinsfield, 09 253 Mathilde T 417.7 0.50 –3 417.7 0.45 250. Mottola, 95 –3 418. 0.5 250. Pravec, 05 288 Glauke T 1170. 0.9 –1 1200. 0.9 Harris, 99 0 Pravec, 14 –2 1170. 0.37 740. Pilcher, 15 299∗ Thora T– 272.9 0.50 0 274. 0.39 Pilcher, 14 +2 272.9 0.47 Pilcher, 17 319∗ Leona T 430. 0.5 –2 430. 0.5 1084. Pilcher, 17 341∗ California T 318. 0.92 –2 318. 0.9 250. Pilcher, 17 –2 317.0 0.54 Polakis, 17 –1 317.0 0.92 Polakis, 17 408 Fama T0 202.1 0.58 0 202.1 0.58 Stephens, 08 470 Kilia T0 290. 0.26 0 290. 0.26 Stephens, 09 0 Stephens, 09 496∗ Gryphia T 1072. 1.25 –2 1072. 1.25 Pilcher, 17 571 Dulcinea T 126.3 0.50 –2 126.3 0.50 Stephens, 11 630 Euphemia T0 350. 0.45 0 350. 0.45 Warner, 11 703∗ No¨emi T? 200. 0.78 –1 201.7 0.78 Noschese, 17 0 115.108 0.28 Sada, 17 –2 200. 0.62 Franco, 17 707 Ste¨ına T0 414. 1.00 0 Pravec, 14 763∗ Cupido T 151.5 0.45 –1 151.1 0.24 Polakis, 18 –2 151.5 0.45 101. Pilcher, 18 823 Sisigambis T0 146. -
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. -
The L3 Exhibitions Catalogue 2010-2014
The L3 Exhibitions Catalogue 2010-2014 Leonardo da Vinci overview Leonardo da Vinci is a universal genius. He What the public knows about Leonardo is bare- was, of course, an Italian, but he belongs to a ly the tip of the iceberg. His manuscripts con- past that is part of the cultural heritage of every tinue to hide secrets and are worthy of inquiry person and every nation. He is a singular exam- and presentation in new, innovative ways. L3 ple throughout history of a man who possessed explores, discovers and reveals the “unknown an enormous talent and excelled not only as a Leonardo” in order to spark the hidden genius scientist, but also as an artist. Most of the inven- that lies within us all. tions and machines that he designed can in fact be considered works of art. On the same note, Leonardo3 (L3) is the world leader in exclu- his artistic works are both the creations of a sive exhibitions and publications on da Vinci’s master artist and the products of a formidable genius. Each of our exhibitions is the result of scientific brain. work carried out by our own team of researchers who investigate and develop never-seen-before Just as his paintings deserve the kind of investi- machines for each event. gation to which only today’s technology can do justice, so the full extent of his scientific work Our exhibitions are “dynamic” rather than “stat- has yet to be revealed to the public. ic”. We make extensive use of 3D animations, physical models and interactive software to of- fer the public a unique level of interaction and a hands-on “edu-tainment” experience. -
4 from the Herschel-VVDS-CFHTLS-D1 Field
A&A 572, A90 (2014) Astronomy DOI: 10.1051/0004-6361/201323089 & c ESO 2014 Astrophysics Hidden starbursts and active galactic nuclei at 0 < z < 4 from the Herschel-VVDS-CFHTLS-D1 field: Inferences on coevolution and feedback B. C. Lemaux1,E.LeFloc’h2,O.LeFèvre1,O.Ilbert1, L. Tresse1,L.M.Lubin3, G. Zamorani4,R.R.Gal5, P. Ciliegi4, P. Cassata1,9,D.D.Kocevski6,7,E.J.McGrath7,S.Bardelli4, E. Zucca4, and G. K. Squires8 1 Aix-Marseille Université, CNRS, LAM (Laboratoire d’Astrophysique de Marseille) UMR 7326, 13388 Marseille, France e-mail: [email protected] 2 Laboratoire AIM-Paris-Saclay, CEA/DSM/Irfu – CNRS – Université Paris Diderot, CE-Saclay, pt courrier 131, 91191 Gif-sur-Yvette, France 3 Department of Physics, University of California, Davis, 1 Shields Avenue, Davis, CA 95616, USA 4 INAF – Osservatorio Astronomico di Bologna, via Ranzani 1, 40127 Bologna, Italy 5 University of Hawai’i, Institute for Astronomy, 2680 Woodlawn Drive, Honolulu, HI 96822, USA 6 Department of Physics and Astronomy, University of Kentucky, Lexington, KY 40506-0055, USA 7 Department of Physics and Astronomy, Colby College, Waterville, ME 04901, USA 8 Spitzer Science Center, California Institute of Technology, M/S 220-6, 1200 E. California Blvd., Pasadena, CA 91125, USA 9 Instituto de Fisica y Astronomía, Facultad de Ciencias, Universidad de Valparaíso, Gran Breta˜na 1111, Casilla 5030, Playa Ancha, Valparaíso, Chile Received 20 November 2013 / Accepted 17 September 2014 ABSTRACT We investigate of the properties of ∼2000 Herschel/SPIRE far-infrared-selected galaxies from 0 < z < 4intheCFHTLS-D1field. Using a combination of extensive spectroscopy from the VVDS and ORELSE surveys, deep multiwavelength imaging from CFHT, VLA, Spitzer, XMM-Newton,andHerschel, and well-calibrated spectral energy distribution fitting, Herschel-bright galaxies are com- pared to optically-selected galaxies at a variety of redshifts. -
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. -
Uranus, Neptune, Pluto, and the Outer Solar System Linda T
Uranus, Neptune, Pluto, and the Outer Solar System Linda T. Elkins-Tanton Uranus, Neptune, Pluto, and the Outer Solar System Copyright © 2006 by Linda T.Elkins-Tanton All rights reserved. No part of this book may be reproduced or utilized in any form or by any means, electronic or mechani- cal, including photocopying, recording, or by any information storage or retrieval systems, without permission in writing from the publisher. For information contact: Chelsea House An imprint of Infobase Publishing 132 West 31st Street New York NY 10001 Library of Congress Cataloging-in-Publication Data Elkins-Tanton, Linda T. Uranus, Neptune, Pluto, and the outer solar system / Linda T.Elkins-Tanton. p. cm. — (The Solar system) Includes bibliographical references and index. ISBN 0-8160-5197-6 (acid-free paper) 1. Uranus (Planet)—Popular works. 2. Neptune (Planet)—Popular works. 3. Pluto (Planet)—Popular works. 4. Solar system—Popular works. I.Title. QB681.E45 2006 523.47—dc22 2005014801 Chelsea House books are available at special discounts when purchased in bulk quantities for businesses, associations, institu- tions, or sales promotions. Please call our Special Sales Department in New York at (212) 967-8800 or (800) 322-8755. You can find Chelsea House on the World Wide Web at http://www.chelseahouse.com Text and cover design by Dorothy M. Preston Illustrations by Richard Garratt Printed in the United States of America VB Hermitage 10 9 8 7 6 5 4 3 2 1 This book is printed on acid-free paper. In memory of my brother Thomas Turner Elkins, who, when I was 10 years old, taught me about the Oort cloud, and together we named our pet mouse Oort. -
The Minor Planet Bulletin
THE MINOR PLANET BULLETIN OF THE MINOR PLANETS SECTION OF THE BULLETIN ASSOCIATION OF LUNAR AND PLANETARY OBSERVERS VOLUME 38, NUMBER 2, A.D. 2011 APRIL-JUNE 71. LIGHTCURVES OF 10452 ZUEV, (14657) 1998 YU27, AND (15700) 1987 QD Gary A. Vander Haagen Stonegate Observatory, 825 Stonegate Road Ann Arbor, MI 48103 [email protected] (Received: 28 October) Lightcurve observations and analysis revealed the following periods and amplitudes for three asteroids: 10452 Zuev, 9.724 ± 0.002 h, 0.38 ± 0.03 mag; (14657) 1998 YU27, 15.43 ± 0.03 h, 0.21 ± 0.05 mag; and (15700) 1987 QD, 9.71 ± 0.02 h, 0.16 ± 0.05 mag. Photometric data of three asteroids were collected using a 0.43- meter PlaneWave f/6.8 corrected Dall-Kirkham astrograph, a SBIG ST-10XME camera, and V-filter at Stonegate Observatory. The camera was binned 2x2 with a resulting image scale of 0.95 arc- seconds per pixel. Image exposures were 120 seconds at –15C. Candidates for analysis were selected using the MPO2011 Asteroid Viewing Guide and all photometric data were obtained and analyzed using MPO Canopus (Bdw Publishing, 2010). Published asteroid lightcurve data were reviewed in the Asteroid Lightcurve Database (LCDB; Warner et al., 2009). The magnitudes in the plots (Y-axis) are not sky (catalog) values but differentials from the average sky magnitude of the set of comparisons. The value in the Y-axis label, “alpha”, is the solar phase angle at the time of the first set of observations. All data were corrected to this phase angle using G = 0.15, unless otherwise stated. -
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. -
Non-Principal Axis Rotation (Tumbling) Asteroids
NON-PRINCIPAL AXIS ROTATION (TUMBLING) ASTEROIDS Asteroid PAR Per1 Amp1 Per2 Amp2 Reference 244 Sita T0 129.51 0.82 0 129.51 0.82 Brinsfield, 09 253 Mathilde T 417.7 0.50 –3 417.7 0.45 250. Mottola, 95 –3 418. 0.5 250. Pravec, 05 288 Glauke T 1170. 0.9 –1 1200. 0.9 Harris, 99 0 Pravec, 14 –2 1170. 0.37 740. Pilcher, 15 299 Thora T0 274. 0.39 0 274. 0.39 Pilcher, 14 408 Fama T0 202.1 0.58 0 202.1 0.58 Stephens, 08 470 Kilia T0 290. 0.26 0 290. 0.26 Stephens, 09 0 Stephens, 09 571 Dulcinea T 126.3 0.50 –2 126.3 0.50 Stephens, 11 630 Euphemia T0 350. 0.45 0 350. 0.45 Warner, 11 707 Ste¨ına T0 414. 1.00 0 Pravec, 14 823 Sisigambis T0 146. 0.7 0 Pravec, 14 824 Anastasia T– 250. 1.20 +2 250. 1.20 Stephens, 10 +2 Pravec, 14 846 Lipperta T0 1641. 0.30 0 1641. 0.30 Buchheim, 11 887 Alinda T0 73.97 0.35 0 Pravec, 14 912 Maritima T0 1332. 0.18 0 Pravec, 14 950 Ahrensa T0 202. 0.40 0 Pravec, 14 989 Schwassmannia T0 107.85 0.39 0 107.85 0.35 Benishek, 14 0 120.3 0.39 Stephens, 14 1042 Amazone T0 540. 0.25 0 Pravec, 14 1183 Jutta T0 212.5 0.10 0 212.5 0.10 Stephens, 11 1235 Schorria T0 1265. -
Hidden Starbursts and Active Galactic Nuclei at 0< Z< 4 from the Herschel-VVDS-CFHTLS-D1 Field: Inferences on Coevolution and Feedback
Astronomy & Astrophysics manuscript no. AA/2013/23089 c ESO 2014 March 3, 2018 Hidden starbursts and active galactic nuclei at 0 < z < 4 from the Herschel⋆-VVDS-CFHTLS-D1 field: Inferences on coevolution and feedback⋆⋆ B. C. Lemaux1, E. Le Floc’h2, O. Le Fèvre1, O. Ilbert1, L. Tresse1, L. M. Lubin3, G. Zamorani4, R. R. Gal5, P. Ciliegi4, P. Cassata1, 9, D. D. Kocevski6, E. J. McGrath7, S. Bardelli4, E. Zucca4, and G. K. Squires8 1 Aix Marseille Université, CNRS, LAM (Laboratoire d’Astrophysique de Marseille) UMR 7326, 13388, Marseille, France e-mail: [email protected] 2 Laboratoire AIM-Paris-Saclay, CEA/DSM/Irfu - CNRS - Université Paris Diderot, CE-Saclay, pt courrier 131, F-91191 Gif-sur- Yvette, France 3 Department of Physics, University of California, Davis, 1 Shields Avenue, Davis, CA 95616, USA 4 INAF - Osservatorio Astronomico di Bologna, via Ranzani 1, 40127 Bologna, Italy 5 University of Hawai’i, Institute for Astronomy, 2680 Woodlawn Drive, Honolulu, HI 96822, USA 6 Department of Physics and Astronomy, University of Kentucky, Lexington, KY 40506-0055, USA 7 Department of Physics and Astronomy, Colby College, Waterville, ME 04901, USA 8 Spitzer Science Center, California Institute of Technology, M/S 220-6, 1200 E. California Blvd., Pasadena, CA 91125, USA 9 Instituto de Fisica y Astronomía, Facultad de Ciencias, Universidad de Valparaíso, Gran Breta˜na 1111, Playa Ancha, Valparaíso Chile Received November 19th, 2013 / Accepted September 17th, 2014 ABSTRACT We investigate of the properties of 2000 Herschel/SPIRE far-infrared-selected galaxies from 0 < z < 4 in the CFHTLS-D1 field. -
Introductory Astronomy Course at UMD With
Introductory Course at UMD with Remote Observing - “Astronomy in Practice” Dr. Melissa N. Hayes-Gehrke Astronomy Dept., UMD 1 2016 GROWTH Education Workshop Overarching Goal Involve non-astronomy students in real astronomical research so that they develop a better understanding of how astronomy, and thus science overall, really works. 2 Talk Outline ● Course Opportunity and Target Student Population ● Educational Goals ● Course Organization and Structure ● Project Execution ● Results: Projects and Course Success 3 Course Opportunity and Target Student Population ● New “Scholarship in Practice” courses at UMD provided the opportunity to develop this course – our department wanted one because all students are required to take two. ● Asteroids are perfect target objects for student research since the required observations and analysis are straightforward, yet new results are possible because of >100,000 unstudied asteroids. 4 Course Opportunity and Target Student Population Target student population: ● Non-astronomy major, may not be science major ● May have only algebra-level math ● May not have any astronomy background 5 Course Opportunity and Target Student Population Example population from most recent course offering (46 students): ● Mostly sophomore/junior ● 33% URMs (including women) ● 25% female ● average GPA of class: 2.9 ● 43% computer science, 13% undecided, 9% biology, 7% engineering ● Many are (or became) astronomy minors 6 Educational Goals The course satisfies learning goals at multiple levels: ● Instructor's astronomical knowledge goals ● University's goals for Scholarship in Practice courses 7 Educational Goals: Instructor's Goals Students will have: ● An understanding of our place in the solar system and how asteroids fit into the solar system. ● An understanding of how astronomers study asteroids. -
The Minor Planet Bulletin Is Open to Papers on All Aspects of 6500 Kodaira (F) 9 25.5 14.8 + 5 0 Minor Planet Study
THE MINOR PLANET BULLETIN OF THE MINOR PLANETS SECTION OF THE BULLETIN ASSOCIATION OF LUNAR AND PLANETARY OBSERVERS VOLUME 32, NUMBER 3, A.D. 2005 JULY-SEPTEMBER 45. 120 LACHESIS – A VERY SLOW ROTATOR were light-time corrected. Aspect data are listed in Table I, which also shows the (small) percentage of the lightcurve observed each Colin Bembrick night, due to the long period. Period analysis was carried out Mt Tarana Observatory using the “AVE” software (Barbera, 2004). Initial results indicated PO Box 1537, Bathurst, NSW, Australia a period close to 1.95 days and many trial phase stacks further [email protected] refined this to 1.910 days. The composite light curve is shown in Figure 1, where the assumption has been made that the two Bill Allen maxima are of approximately equal brightness. The arbitrary zero Vintage Lane Observatory phase maximum is at JD 2453077.240. 83 Vintage Lane, RD3, Blenheim, New Zealand Due to the long period, even nine nights of observations over two (Received: 17 January Revised: 12 May) weeks (less than 8 rotations) have not enabled us to cover the full phase curve. The period of 45.84 hours is the best fit to the current Minor planet 120 Lachesis appears to belong to the data. Further refinement of the period will require (probably) a group of slow rotators, with a synodic period of 45.84 ± combined effort by multiple observers – preferably at several 0.07 hours. The amplitude of the lightcurve at this longitudes. Asteroids of this size commonly have rotation rates of opposition was just over 0.2 magnitudes.