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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. -
(704) Interamnia from Its Occultations and Lightcurves
International Journal of Astronomy and Astrophysics, 2014, 4, 91-118 Published Online March 2014 in SciRes. http://www.scirp.org/journal/ijaa http://dx.doi.org/10.4236/ijaa.2014.41010 A 3-D Shape Model of (704) Interamnia from Its Occultations and Lightcurves Isao Satō1*, Marc Buie2, Paul D. Maley3, Hiromi Hamanowa4, Akira Tsuchikawa5, David W. Dunham6 1Astronomical Society of Japan, Yamagata, Japan 2Southwest Research Institute, Boulder, USA 3International Occultation Timing Association, Houston, USA 4Hamanowa Astronomical Observatory, Fukushima, Japan 5Yanagida Astronomical Observatory, Ishikawa, Japan 6International Occultation Timing Association, Greenbelt, USA Email: *[email protected], [email protected], [email protected], [email protected], [email protected], [email protected] Received 9 November 2013; revised 9 December 2013; accepted 17 December 2013 Copyright © 2014 by authors and Scientific Research Publishing Inc. This work is licensed under the Creative Commons Attribution International License (CC BY). http://creativecommons.org/licenses/by/4.0/ Abstract A 3-D shape model of the sixth largest of the main belt asteroids, (704) Interamnia, is presented. The model is reproduced from its two stellar occultation observations and six lightcurves between 1969 and 2011. The first stellar occultation was the occultation of TYC 234500183 on 1996 De- cember 17 observed from 13 sites in the USA. An elliptical cross section of (344.6 ± 9.6 km) × (306.2 ± 9.1 km), for position angle P = 73.4 ± 12.5˚ was fitted. The lightcurve around the occulta- tion shows that the peak-to-peak amplitude was 0.04 mag. and the occultation phase was just be- fore the minimum. -
In Pursuit of the GENUINE CHRISTIAN IMAGE
In Pursuit of THE GENUINE CHRISTIAN IMAGE Erland Forsberg as a Lutheran Producer of Icons in the Fields of Culture and Religion Juha Malmisalo Academic dissertation To be publicly discussed, by permission of the Faculty of Theology of the University of Helsinki, in Auditorium XII in the Main Building of the University, on May 14, 2005, at 10 am. Helsinki 2005 1 In Pursuit of THE GENUINE CHRISTIAN IMAGE Erland Forsberg as a Lutheran Producer of Icons in the Fields of Culture and Religion Juha Malmisalo Helsinki 2005 2 ISBN 952-91-8539-1 (nid.) ISBN 952-10-2414-3 (PDF) University Printing House Helsinki 2005 3 Contents Abbreviations .......................................................................................................... 4 Abstract ................................................................................................................... 6 Preface ..................................................................................................................... 7 1. Encountering Peripheral Cultural Phenomena ......................................... 9 1.1. Forsberg’s Icon Painting in Art Sociological Analysis: Conceptual Issues and Selected Perspectives ............................................................ 9 1.2. An Adaptation of Bourdieu’s Theory of Cultural Fields .......................... 18 1.3. The Pictorial Source Material: Questions of Accessibility and Method .. 23 2. Attempts at a Field-Constitution ................................................................ 30 2.1. Educational, Social, and -
New Double Stars from Asteroidal Occultations, 1971 - 2008
Vol. 6 No. 1 January 1, 2010 Journal of Double Star Observations Page 88 New Double Stars from Asteroidal Occultations, 1971 - 2008 Dave Herald, Canberra, Australia International Occultation Timing Association (IOTA) Robert Boyle, Carlisle, Pennsylvania, USA Dickinson College David Dunham, Greenbelt, Maryland, USA; Toshio Hirose, Tokyo, Japan; Paul Maley, Houston, Texas, USA; Bradley Timerson, Newark, New York, USA International Occultation Timing Association (IOTA) Tim Farris, Gallatin, Tennessee, USA Volunteer State Community College Eric Frappa and Jean Lecacheux, Paris, France Observatoire de Paris Tsutomu Hayamizu, Kagoshima, Japan Sendai Space Hall Marek Kozubal, Brookline, Massachusetts, USA Clay Center Richard Nolthenius, Aptos, California, USA Cabrillo College and IOTA Lewis C. Roberts, Jr., Pasadena, California, USA California Institute of Technology/Jet Propulsion Laboratory David Tholen, Honolulu, Hawaii, USA University of Hawaii E-mail: [email protected] Abstract: Observations of occultations by asteroids and planetary moons can detect double stars with separations in the range of about 0.3” to 0.001”. This paper lists all double stars detected in asteroidal occultations up to the end of 2008. It also provides a general explanation of the observational method and analysis. The incidence of double stars with a separation in the range 0.001” to 0.1” with a magnitude difference less than 2 is estimated to be about 1%. Vol. 6 No. 1 January 1, 2010 Journal of Double Star Observations Page 89 New Double Stars from Asteroidal Occultations, 1971 - 2008 tions. More detail about the method of analysis is set Introduction out in the Appendix. Asteroids and planetary moons will naturally oc- cult many stars as they move through the sky. -
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. -
Observer's Handbook 1986
OBSERVER’S HANDBOOK 1986 EDITOR: ROY L. BISHOP THE ROYAL ASTRONOMICAL SOCIETY OF CANADA CONTRIBUTORS AND ADVISORS A l a n H. B a t t e n , Dominion Astrophysical Observatory, 5071 W. Saanich Road, Victoria, BC, Canada V8X 4M6 (The Nearest Stars). L a r r y D. B o g a n , Department of Physics, Acadia University, Wolfville, NS, Canada B0P 1X0 (Configurations of Saturn’s Satellites). Terence Dickinson, R.R. 3, Odessa, ON, Canada K0H 2H0 (The Planets). David W. Dunham, International Occultation Timing Association, P.O. Box 7488, Silver Spring, MD 20907, U.S.A. (Lunar and Planetary Occultations). Alan Dyer, Queen Elizabeth Planetarium, 10004-104 Ave., Edmonton, AB, Canada T5J 0K1 (Messier Catalogue, Deep-Sky Objects). Fred Espenak, Planetary Systems Branch, NASA-Goddard Space Flight Centre, Greenbelt, MD, U.S.A. 20771 (Eclipses and Transits). M arie Fidler, The Royal Astronomical Society of Canada, 136 Dupont St., Toronto, ON, Canada M5R 1V2 (Observatories and Planetaria). Victor Gaizauskas, Herzberg Institute of Astrophysics, National Research Council, Ottawa, ON, Canada K1A 0R6 (Solar Activity). R o b e r t F. G a r r is o n , David Dunlap Observatory, University of Toronto, Box 360, Richmond Hill, ON, Canada L4C 4Y6 (The Brightest Stars). Ian H alliday, Herzberg Institute of Astrophysics, National Research Council, Ottawa, ON, Canada K1A 0R6 (Miscellaneous Astronomical Data). W illiam Herbst, Van Vleck Observatory, Wesleyan University, Middletown, CT, U.S.A. 06457 (Galactic Nebulae). H e l e n S. H o g g , David Dunlap Observatory, University of Toronto, Box 360, Richmond Hill, ON, Canada L4C 4Y6 (Foreword). -
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. -
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. -
Legends of the Madonna by Mrs. Jameson</H1>
Legends of the Madonna by Mrs. Jameson Legends of the Madonna by Mrs. Jameson Produced by Charles Aldarondo, Keren Vergon, William Flis, and the Online Distributed Proofreading Team. LEGENDS OF THE MADONNA, AS REPRESENTED IN THE FINE ARTS. BY MRS. JAMESON. CORRECTED AND ENLARGED EDITION. page 1 / 503 BOSTON: HOUGHTON, MIFFLIN AND COMPANY. The Riverside Press, Cambridge. 1881. NOTE BY THE PUBLISHERS. Some months since Mrs. Jameson kindly consented to prepare for this Edition of her writings the series of _Sacred and Legendary Art_, but dying before she had time to fulfil her promise, the arrangement has been intrusted to other hands. The text of the whole series will be an exact reprint of the last English Edition. TICKNOR & FIELDS. BOSTON, Oct. 1st, 1860. CONTENTS. PREFACE INTRODUCTION-- Origin of the Worship of the Madonna. page 2 / 503 Earliest artistic Representations. Origin of the Group of the Virgin and Child in the Fifth Century. The First Council at Ephesus. The Iconoclasts. First Appearance of the Effigy of the Virgin on Coins. Period of Charlemagne. Period of the Crusades. Revival of Art in the Thirteenth Century. The Fourteenth Century. Influence of Dante. The Fifteenth Century. The Council of Constance and the Hussite Wars. The Sixteenth Century. The Luxury of Church Pictures. The Influence of Classical Literature on the Representations of the Virgin. The Seventeenth Century. Theological Art. Spanish Art. Influence of Jesuitism on Art. Authorities followed by Painters in the earliest Times. Legend of St. Luke. Character of the Virgin Mary as drawn in the Gospels. Early Descriptions of her Person; how far attended to by the Painters. -
The V-Band Photometry of Asteroids from ASAS-SN
Astronomy & Astrophysics manuscript no. 40759˙ArXiV © ESO 2021 July 22, 2021 V-band photometry of asteroids from ASAS-SN Finding asteroids with slow spin ? J. Hanusˇ1, O. Pejcha2, B. J. Shappee3, C. S. Kochanek4;5, K. Z. Stanek4;5, and T. W.-S. Holoien6;?? 1 Institute of Astronomy, Faculty of Mathematics and Physics, Charles University, V Holesoviˇ ckˇ ach´ 2, 18000 Prague, Czech Republic 2 Institute of Theoretical Physics, Faculty of Mathematics and Physics, Charles University, V Holesoviˇ ckˇ ach´ 2, 18000 Prague, Czech Republic 3 Institute for Astronomy, University of Hawai’i, 2680 Woodlawn Drive, Honolulu, HI 96822, USA 4 Department of Astronomy, The Ohio State University, 140 West 18th Avenue, Columbus, OH 43210, USA 5 Center for Cosmology and Astroparticle Physics, The Ohio State University, 191 W. Woodruff Avenue, Columbus, OH 43210, USA 6 The Observatories of the Carnegie Institution for Science, 813 Santa Barbara St., Pasadena, CA 91101, USA Received x-x-2021 / Accepted x-x-2021 ABSTRACT We present V-band photometry of the 20,000 brightest asteroids using data from the All-Sky Automated Survey for Supernovae (ASAS-SN) between 2012 and 2018. We were able to apply the convex inversion method to more than 5,000 asteroids with more than 60 good measurements in order to derive their sidereal rotation periods, spin axis orientations, and shape models. We derive unique spin state and shape solutions for 760 asteroids, including 163 new determinations. This corresponds to a success rate of about 15%, which is significantly higher than the success rate previously achieved using photometry from surveys. -
The Minor Planet Bulletin 36, 188-190
THE MINOR PLANET BULLETIN OF THE MINOR PLANETS SECTION OF THE BULLETIN ASSOCIATION OF LUNAR AND PLANETARY OBSERVERS VOLUME 37, NUMBER 3, A.D. 2010 JULY-SEPTEMBER 81. ROTATION PERIOD AND H-G PARAMETERS telescope (SCT) working at f/4 and an SBIG ST-8E CCD. Baker DETERMINATION FOR 1700 ZVEZDARA: A independently initiated observations on 2009 September 18 at COLLABORATIVE PHOTOMETRY PROJECT Indian Hill Observatory using a 0.3-m SCT reduced to f/6.2 coupled with an SBIG ST-402ME CCD and Johnson V filter. Ronald E. Baker Benishek from the Belgrade Astronomical Observatory joined the Indian Hill Observatory (H75) collaboration on 2009 September 24 employing a 0.4-m SCT PO Box 11, Chagrin Falls, OH 44022 USA operating at f/10 with an unguided SBIG ST-10 XME CCD. [email protected] Pilcher at Organ Mesa Observatory carried out observations on 2009 September 30 over more than seven hours using a 0.35-m Vladimir Benishek f/10 SCT and an unguided SBIG STL-1001E CCD. As a result of Belgrade Astronomical Observatory the collaborative effort, a total of 17 time series sessions was Volgina 7, 11060 Belgrade 38 SERBIA obtained from 2009 August 20 until October 19. All observations were unfiltered with the exception of those recorded on September Frederick Pilcher 18. MPO Canopus software (BDW Publishing, 2009a) employing 4438 Organ Mesa Loop differential aperture photometry, was used by all authors for Las Cruces, NM 88011 USA photometric data reduction. The period analysis was performed using the same program. David Higgins Hunter Hill Observatory The data were merged by adjusting instrumental magnitudes and 7 Mawalan Street, Ngunnawal ACT 2913 overlapping characteristic features of the individual lightcurves. -
Cumulative Index to Volumes 1-45
The Minor Planet Bulletin Cumulative Index 1 Table of Contents Tedesco, E. F. “Determination of the Index to Volume 1 (1974) Absolute Magnitude and Phase Index to Volume 1 (1974) ..................... 1 Coefficient of Minor Planet 887 Alinda” Index to Volume 2 (1975) ..................... 1 Chapman, C. R. “The Impossibility of 25-27. Index to Volume 3 (1976) ..................... 1 Observing Asteroid Surfaces” 17. Index to Volume 4 (1977) ..................... 2 Tedesco, E. F. “On the Brightnesses of Index to Volume 5 (1978) ..................... 2 Dunham, D. W. (Letter regarding 1 Ceres Asteroids” 3-9. Index to Volume 6 (1979) ..................... 3 occultation) 35. Index to Volume 7 (1980) ..................... 3 Wallentine, D. and Porter, A. Index to Volume 8 (1981) ..................... 3 Hodgson, R. G. “Useful Work on Minor “Opportunities for Visual Photometry of Index to Volume 9 (1982) ..................... 4 Planets” 1-4. Selected Minor Planets, April - June Index to Volume 10 (1983) ................... 4 1975” 31-33. Index to Volume 11 (1984) ................... 4 Hodgson, R. G. “Implications of Recent Index to Volume 12 (1985) ................... 4 Diameter and Mass Determinations of Welch, D., Binzel, R., and Patterson, J. Comprehensive Index to Volumes 1-12 5 Ceres” 24-28. “The Rotation Period of 18 Melpomene” Index to Volume 13 (1986) ................... 5 20-21. Hodgson, R. G. “Minor Planet Work for Index to Volume 14 (1987) ................... 5 Smaller Observatories” 30-35. Index to Volume 15 (1988) ................... 6 Index to Volume 3 (1976) Index to Volume 16 (1989) ................... 6 Hodgson, R. G. “Observations of 887 Index to Volume 17 (1990) ................... 6 Alinda” 36-37. Chapman, C. R. “Close Approach Index to Volume 18 (1991) ..................