Observational Constraints on the Optical and Near-Infrared Emission from the Neutron Star–Black Hole Binary Merger Candidate S190814bv? K
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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. -
Assa Handbook-1993
ASTRONOMICAL HANDBOOK FOR SOUTHERN AFRICA 1 published by the Astronomical Society of Southern Africa 5 A MUSEUM QUEEN VICTORIA STREET (3 61 CAPE TOWN 8000 (021)243330 o PUBLIC SHOWS o MONTHLY SKY UPDATES 0 ASTRONOMY COURSES O MUSIC CONCERTS o ASTRONOMY WEEK 0 SCHOOL SHOWS ° CLUB BOOKINGS ° CORPORATE LAUNCH VENUE FOR MORE INFO PHONE 243330 ASTRONOMICAL HANDBOOK FOR SOUTHERN AFRICA 1993 This booklet is intended both as an introduction to observational astronomy for the interested layman - even if hie interest is only a passing one - and as a handbook for the established amateur or professional astronomer. Front cover The telescope of Ds G. de Beer (right) of the Ladismith Astronomical Society. He, Dr M. Schreuder (left) and the late Mr Ron Dale of the Natal Midlands Centre, are viewing Siriu3 in the daytime with the aid of setting circles. Photograph Mr J. Watson ® t h e Astronomical Society of Southern Africa, Cape Town. 1992 ISSN 0571-7191 CONTENTS ASTRONOMY IN SOUTHERN AFRICA...................... 1 DIARY................................................................. 6 THE SUN............................................................... 8 THE MOON............................................................. 11 THE PLANETS.......................................................... 17 THE MOONS OF JUPITER ................................................ 24 THE MOONS OF SATURN....................................... 28 COMETS AND METEORS............................ 29 THE STARS........................................................... -
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. -
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. -
Combining Asteroid Models Derived by Lightcurve Inversion with Asteroidal Occultation Silhouettes
Combining asteroid models derived by lightcurve inversion with asteroidal occultation silhouettes Josef Durechˇ a,∗, Mikko Kaasalainenb, David Heraldc, David Dunhamd, Brad Timersone, Josef Hanuˇsa, Eric Frappaf, John Talbotg, Tsutomu Hayamizuh, Brian D. Warneri, Frederick Pilcherj, Adri´an Gal´adk,l aAstronomical Institute, Faculty of Mathematics and Physics, Charles University in Prague, V Holeˇsoviˇck´ach 2, CZ-18000 Prague, Czech Republic bDepartment of Mathematics, Tampere University of Technology, P.O. Box 553, 33101 Tampere, Finland c3 Lupin Pl, Murrumbateman, NSW, Australia dInternational Occultation Timing Association (IOTA) and KinetX, Inc., 7913 Kara Ct., Greenbelt, MD 20770, USA eInternational Occultation Timing Association (IOTA), 623 Bell Rd., Newark, NY, USA f1 bis cours Jovin Bouchard 42000 Saint-Etienne, France gOccultation Section, Royal Astronomical Society of New Zealand, P.O. Box 3181, Wellington, New Zealand hJapan Occultation Information Network (JOIN), Sendai Space Hall, 2133-6 Nagatoshi, Kagoshima pref, Japan iPalmer Divide Observatory, 17955 Bakers Farm Rd., Colorado Springs, CO 80908, USA j4438 Organ Mesa Loop, Las Cruces, NM 88011, USA kModra Observatory, FMFI Comenius University, 842 48 Bratislava, Slovakia lOndˇrejov Observatory, AV CR,ˇ 251 65 Ondˇrejov, Czech Republic Abstract Asteroid sizes can be directly measured by observing occultations of stars by asteroids. When there are enough observations across the path of the shadow, the asteroid’s projected silhouette can be reconstructed. Asteroid shape models derived from photometry by the lightcurve inversion method enable us to predict the orientation of an asteroid for the time of occultation. By scaling the shape model to fit the occultation chords, we can determine the asteroid size with a relative accuracy of typically ∼ 10%. -
TRUE MASSES of RADIAL-VELOCITY EXOPLANETS Robert A
APP Template V1.01 Article id: apj513330 Typesetter: MPS Date received by MPS: 19/05/2015 PE: CE : LE: UNCORRECTED PROOF The Astrophysical Journal, 00:000000 (28pp), 2015 Month Day © 2015. The American Astronomical Society. All rights reserved. TRUE MASSES OF RADIAL-VELOCITY EXOPLANETS Robert A. Brown Space Telescope Science Institute, USA; [email protected] Received 2015 January 12; accepted 2015 April 14; published 2015 MM DD ABSTRACT We study the task of estimating the true masses of known radial-velocity (RV) exoplanets by means of direct astrometry on coronagraphic images to measure the apparent separation between exoplanet and host star. Initially, we assume perfect knowledge of the RV orbital parameters and that all errors are due to photon statistics. We construct design reference missions for four missions currently under study at NASA: EXO-S and WFIRST-S, with external star shades for starlight suppression, EXO-C and WFIRST-C, with internal coronagraphs. These DRMs reveal extreme scheduling constraints due to the combination of solar and anti-solar pointing restrictions, photometric and obscurational completeness, image blurring due to orbital motion, and the “nodal effect,” which is the independence of apparent separation and inclination when the planet crosses the plane of the sky through the host star. Next, we address the issue of nonzero uncertainties in RV orbital parameters by investigating their impact on the observations of 21 single-planet systems. Except for two—GJ 676 A b and 16 Cyg B b, which are observable only by the star-shade missions—we find that current uncertainties in orbital parameters generally prevent accurate, unbiased estimation of true planetary mass. -
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. -
I N S I D E T H I S I S S
February / février 2008 Volume/volume 102 Number/numéro 1 [728] This Issue's Winning Astrophoto! FEATURING A FULL COLOUR SECTION! The Journal of the Royal Astronomical Society of Canada Cassiopeia Rising Over the Plaskett by Charles Banville, Victoria Centre. This is a montage of two pictures I took using a Canon 20Da and a Canon EF 17-40mm f/4L lens. The foreground image was acquired at the Dominion Astrophysical Observatory in Victoria on 2007 July 26. That evening the Plaskett Dome was illuminated by a bright 12-day-old Moon. The star trails were created using 87 light frames of 1 minute each taken from Cattle Point on 2007 August 8. Le Journal de la Société royale d’astronomie du Canada [Editor’s Note: The two-member team of Dietmar Kupke and Paul Mortfield of the Toronto Centre selected this late-entry image from among the 30 or so entries to the “Own the Back Cover” con- test. Thanks to all the submitters. We welcome further entries, so don’t delay – send in yours now! INSIDE THIS ISSUE Watch the back cover of the April issue for the next winner.] One Hundred Editions of the Observer's Handbook · Seriously Seeking Ceres! Mont-Mégantic Dark-Sky Reserve Conference, 2007 September 19-21 Duplicity of ZC1042: My First Double-Star Discovery In Memory of Gertrude Jean Southam Building for the International Year of Astronomy (IYA2009) THE ROYAL ASTRONOMICAL SOCIETY OF CANADA February / février 2008 NATIONAL OFFICERS AND COUNCIL FOR 2007-2008/CONSEIL ET ADMINISTRATEURS NATIONAUX Honorary President Robert Garrison, Ph.D., Toronto President Scott Young, B.Sc., Winnipeg Vol. -
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. -
The British Astronomical Association Handbook 2014
THE HANDBOOK OF THE BRITISH ASTRONOMICAL ASSOCIATION 2015 2014 October ISSN 0068–130–X CONTENTS CALENDAR 2015 . 2 PREFACE . 3 HIGHLIGHTS FOR 2015 . 4 SKY DIARY . .. 5 VISIBILITY OF PLANETS . 6 RISING AND SETTING OF THE PLANETS IN LATITUDES 52°N AND 35°S . 7-8 ECLIPSES . 9-14 TIME . 15-16 EARTH AND SUN . 17-19 LUNAR LIBRATION . 20 MOON . 21 MOONRISE AND MOONSET . 21-25 SUN’S SELENOGRAPHIC COLONGITUDE . 26 LUNAR OCCULTATIONS . 27-33 GRAZING LUNAR OCCULTATIONS . 34-35 APPEARANCE OF PLANETS . 36 MERCURY . 37-38 VENUS . 39 MARS . 40-41 ASTEROIDS . 42 ASTEROID EPHEMERIDES . 43-47 ASTEROID OCCULTATIONS .. 48-50 NEO CLOSE APPROACHES TO EARTH . 51 ASTEROIDS: FAVOURABLE OBSERVING OPPORTUNITIES . 52-54 JUPITER . 55-59 SATELLITES OF JUPITER . 59-63 JUPITER ECLIPSES, OCCULTATIONS AND TRANSITS . 64-73 SATURN . 74-77 SATELLITES OF SATURN . 78-81 URANUS . 82 NEPTUNE . 83 TRANS–NEPTUNIAN & SCATTERED DISK OBJECTS . 84 DWARF PLANETS . 85-88 COMETS . 89-96 METEOR DIARY . 97-99 VARIABLE STARS (RZ Cassiopeiae; Algol; λ Tauri) . 100-101 MIRA STARS . 102 VARIABLE STAR OF THE YEAR (V Bootis) . 103-105 EPHEMERIDES OF DOUBLE STARS . 106-107 BRIGHT STARS . 108 ACTIVE GALAXIES . 109 PLANETS – EXPLANATION OF TABLES . 110 ELEMENTS OF PLANETARY ORBITS . 111 ASTRONOMICAL AND PHYSICAL CONSTANTS . 111-112 INTERNET RESOURCES . 113-114 GREEK ALPHABET . 115 ACKNOWLEDGEMENTS . 116 ERRATA . 116 Front Cover: The Moon at perigee and apogee – highlighting the clear size difference when the Moon is closest and farthest away from the Earth. Perigee on 2009/11/08 at 23:24UT, distance -
Astrometric Asteroid Masses: a Simultaneous Determination
A&A 565, A56 (2014) Astronomy DOI: 10.1051/0004-6361/201322766 & c ESO 2014 Astrophysics Astrometric asteroid masses: a simultaneous determination Edwin Goffin Aartselaarstraat 14, 2660 Hoboken, Belgium e-mail: [email protected] Received 27 September 2013 / Accepted 18 March 2014 ABSTRACT Using over 89 million astrometric observations of 349 737 numbered minor planets, an attempt was made to determine the masses of 230 of them by simultaneously solving for corrections to all orbital elements and the masses. For 132 minor planets an acceptable result was obtained, 49 of which appear to be new. Key words. astrometry – celestial mechanics – minor planets, asteroids: general 1. Introduction substantial number of test asteroids (349 737). Section 2 explains the basic principles and problems of simultaneous asteroid mass The astrometric determination of asteroid masses is the tech- determination and in Sect. 3 the details of the actual calculations nique of calculating the mass of asteroids (hereafter called “per- are given. Section 4 briefly deals with the observations used and turbing asteroids” or “perturbers”) from the gravitational pertur- explains the statistical analysis of the residuals that was used to bations they exert on the motion of other asteroids (called “test assign weights to, or reject observations. In Sect. 5 the results asteroids”). are presented and Sect. 6 discusses them. The usual procedure to calculate the mass of one aster- Throughout this paper, asteroid masses are expressed in units oid is, first, to identify potential test asteroids by searching −10 of 10 solar masses (M) and generally given to 3 decimal for close approaches with the perturbing asteroids and then places. -
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) ..................