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A&A 583, A85 (2015) Astronomy DOI: 10.1051/0004-6361/201526795 & c ESO 2015 Astrophysics Reaching the boundary between stellar kinematic groups and very wide binaries III. Sixteen new stars and eight new wide systems in the β Pictoris moving group F. J. Alonso-Floriano1, J. A. Caballero2, M. Cortés-Contreras1,E.Solano2,3, and D. Montes1 1 Departamento de Astrofísica y Ciencias de la Atmósfera, Facultad de Ciencias Físicas, Universidad Complutense de Madrid, 28040 Madrid, Spain e-mail: [email protected] 2 Centro de Astrobiología (CSIC-INTA), ESAC PO box 78, 28691 Villanueva de la Cañada, Madrid, Spain 3 Spanish Virtual Observatory, ESAC PO box 78, 28691 Villanueva de la Cañada, Madrid, Spain Received 19 June 2015 / Accepted 8 August 2015 ABSTRACT Aims. We look for common proper motion companions to stars of the nearby young β Pictoris moving group. Methods. First, we compiled a list of 185 β Pictoris members and candidate members from 35 representative works. Next, we used the Aladin and STILTS virtual observatory tools and the PPMXL proper motion and Washington Double Star catalogues to look for companion candidates. The resulting potential companions were subjects of a dedicated astro-photometric follow-up using public data from all-sky surveys. After discarding 67 sources by proper motion and 31 by colour-magnitude diagrams, we obtained a final list of 36 common proper motion systems. The binding energy of two of them is perhaps too small to be considered physically bound. Results. Of the 36 pairs and multiple systems, eight are new, 16 have only one stellar component previously classified as a β Pictoris member, and three have secondaries at or below the hydrogen-burning limit. -
Asteroid Family Identification 613
Bendjoya and Zappalà: Asteroid Family Identification 613 Asteroid Family Identification Ph. Bendjoya University of Nice V. Zappalà Astronomical Observatory of Torino Asteroid families have long been known to exist, although only recently has the availability of new reliable statistical techniques made it possible to identify a number of very “robust” groupings. These results have laid the foundation for modern physical studies of families, thought to be the direct result of energetic collisional events. A short summary of the current state of affairs in the field of family identification is given, including a list of the most reliable families currently known. Some likely future developments are also discussed. 1. INTRODUCTION calibrate new identification methods. According to the origi- nal papers published in the literature, Brouwer (1951) used The term “asteroid families” is historically linked to the a fairly subjective criterion to subdivide the Flora family name of the Japanese researcher Kiyotsugu Hirayama, who delineated by Hirayama. Arnold (1969) assumed that the was the first to use the concept of orbital proper elements to asteroids are dispersed in the proper-element space in a identify groupings of asteroids characterized by nearly iden- Poisson distribution. Lindblad and Southworth (1971) cali- tical orbits (Hirayama, 1918, 1928, 1933). In interpreting brated their method in such a way as to find good agree- these results, Hirayama made the hypothesis that such a ment with Brouwer’s results. Carusi and Massaro (1978) proximity could not be due to chance and proposed a com- adjusted their method in order to again find the classical mon origin for the members of these groupings. -
Research Paper in Nature
Draft version November 1, 2017 Typeset using LATEX twocolumn style in AASTeX61 DISCOVERY AND CHARACTERIZATION OF THE FIRST KNOWN INTERSTELLAR OBJECT Karen J. Meech,1 Robert Weryk,1 Marco Micheli,2, 3 Jan T. Kleyna,1 Olivier Hainaut,4 Robert Jedicke,1 Richard J. Wainscoat,1 Kenneth C. Chambers,1 Jacqueline V. Keane,1 Andreea Petric,1 Larry Denneau,1 Eugene Magnier,1 Mark E. Huber,1 Heather Flewelling,1 Chris Waters,1 Eva Schunova-Lilly,1 and Serge Chastel1 1Institute for Astronomy, 2680 Woodlawn Drive, Honolulu, HI 96822, USA 2ESA SSA-NEO Coordination Centre, Largo Galileo Galilei, 1, 00044 Frascati (RM), Italy 3INAF - Osservatorio Astronomico di Roma, Via Frascati, 33, 00040 Monte Porzio Catone (RM), Italy 4European Southern Observatory, Karl-Schwarzschild-Strasse 2, D-85748 Garching bei M¨unchen,Germany (Received November 1, 2017; Revised TBD, 2017; Accepted TBD, 2017) Submitted to Nature ABSTRACT Nature Letters have no abstracts. Keywords: asteroids: individual (A/2017 U1) | comets: interstellar Corresponding author: Karen J. Meech [email protected] 2 Meech et al. 1. SUMMARY 22 confirmed that this object is unique, with the highest 29 Until very recently, all ∼750 000 known aster- known hyperbolic eccentricity of 1:188 ± 0:016 . Data oids and comets originated in our own solar sys- obtained by our team and other researchers between Oc- tem. These small bodies are made of primor- tober 14{29 refined its orbital eccentricity to a level of dial material, and knowledge of their composi- precision that confirms the hyperbolic nature at ∼ 300σ. tion, size distribution, and orbital dynamics is Designated as A/2017 U1, this object is clearly from essential for understanding the origin and evo- outside our solar system (Figure2). -
11–6–03 Vol. 68 No. 215 Thursday Nov. 6, 2003 Pages 62731–63010
11–6–03 Thursday Vol. 68 No. 215 Nov. 6, 2003 Pages 62731–63010 VerDate jul 14 2003 19:08 Nov 05, 2003 Jkt 203001 PO 00000 Frm 00001 Fmt 4710 Sfmt 4710 E:\FR\FM\06NOWS.LOC 06NOWS 1 II Federal Register / Vol. 68, No. 215 / Thursday, November 6, 2003 The FEDERAL REGISTER (ISSN 0097–6326) is published daily, SUBSCRIPTIONS AND COPIES Monday through Friday, except official holidays, by the Office of the Federal Register, National Archives and Records PUBLIC Administration, Washington, DC 20408, under the Federal Register Subscriptions: Act (44 U.S.C. Ch. 15) and the regulations of the Administrative Paper or fiche 202–512–1800 Committee of the Federal Register (1 CFR Ch. I). The Assistance with public subscriptions 202–512–1806 Superintendent of Documents, U.S. Government Printing Office, Washington, DC 20402 is the exclusive distributor of the official General online information 202–512–1530; 1–888–293–6498 edition. Periodicals postage is paid at Washington, DC. Single copies/back copies: The FEDERAL REGISTER provides a uniform system for making Paper or fiche 202–512–1800 available to the public regulations and legal notices issued by Assistance with public single copies 1–866–512–1800 Federal agencies. These include Presidential proclamations and (Toll-Free) Executive Orders, Federal agency documents having general FEDERAL AGENCIES applicability and legal effect, documents required to be published by act of Congress, and other Federal agency documents of public Subscriptions: interest. Paper or fiche 202–741–6005 Documents are on file for public inspection in the Office of the Assistance with Federal agency subscriptions 202–741–6005 Federal Register the day before they are published, unless the issuing agency requests earlier filing. -
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. -
Orders of Magnitude (Length) - Wikipedia
03/08/2018 Orders of magnitude (length) - Wikipedia Orders of magnitude (length) The following are examples of orders of magnitude for different lengths. Contents Overview Detailed list Subatomic Atomic to cellular Cellular to human scale Human to astronomical scale Astronomical less than 10 yoctometres 10 yoctometres 100 yoctometres 1 zeptometre 10 zeptometres 100 zeptometres 1 attometre 10 attometres 100 attometres 1 femtometre 10 femtometres 100 femtometres 1 picometre 10 picometres 100 picometres 1 nanometre 10 nanometres 100 nanometres 1 micrometre 10 micrometres 100 micrometres 1 millimetre 1 centimetre 1 decimetre Conversions Wavelengths Human-defined scales and structures Nature Astronomical 1 metre Conversions https://en.wikipedia.org/wiki/Orders_of_magnitude_(length) 1/44 03/08/2018 Orders of magnitude (length) - Wikipedia Human-defined scales and structures Sports Nature Astronomical 1 decametre Conversions Human-defined scales and structures Sports Nature Astronomical 1 hectometre Conversions Human-defined scales and structures Sports Nature Astronomical 1 kilometre Conversions Human-defined scales and structures Geographical Astronomical 10 kilometres Conversions Sports Human-defined scales and structures Geographical Astronomical 100 kilometres Conversions Human-defined scales and structures Geographical Astronomical 1 megametre Conversions Human-defined scales and structures Sports Geographical Astronomical 10 megametres Conversions Human-defined scales and structures Geographical Astronomical 100 megametres 1 gigametre -
(2000) Forging Asteroid-Meteorite Relationships Through Reflectance
Forging Asteroid-Meteorite Relationships through Reflectance Spectroscopy by Thomas H. Burbine Jr. B.S. Physics Rensselaer Polytechnic Institute, 1988 M.S. Geology and Planetary Science University of Pittsburgh, 1991 SUBMITTED TO THE DEPARTMENT OF EARTH, ATMOSPHERIC, AND PLANETARY SCIENCES IN PARTIAL FULFILLMENT OF THE REQUIREMENTS FOR THE DEGREE OF DOCTOR OF PHILOSOPHY IN PLANETARY SCIENCES AT THE MASSACHUSETTS INSTITUTE OF TECHNOLOGY FEBRUARY 2000 © 2000 Massachusetts Institute of Technology. All rights reserved. Signature of Author: Department of Earth, Atmospheric, and Planetary Sciences December 30, 1999 Certified by: Richard P. Binzel Professor of Earth, Atmospheric, and Planetary Sciences Thesis Supervisor Accepted by: Ronald G. Prinn MASSACHUSES INSTMUTE Professor of Earth, Atmospheric, and Planetary Sciences Department Head JA N 0 1 2000 ARCHIVES LIBRARIES I 3 Forging Asteroid-Meteorite Relationships through Reflectance Spectroscopy by Thomas H. Burbine Jr. Submitted to the Department of Earth, Atmospheric, and Planetary Sciences on December 30, 1999 in Partial Fulfillment of the Requirements for the Degree of Doctor of Philosophy in Planetary Sciences ABSTRACT Near-infrared spectra (-0.90 to ~1.65 microns) were obtained for 196 main-belt and near-Earth asteroids to determine plausible meteorite parent bodies. These spectra, when coupled with previously obtained visible data, allow for a better determination of asteroid mineralogies. Over half of the observed objects have estimated diameters less than 20 k-m. Many important results were obtained concerning the compositional structure of the asteroid belt. A number of small objects near asteroid 4 Vesta were found to have near-infrared spectra similar to the eucrite and howardite meteorites, which are believed to be derived from Vesta. -
Results Astronomical Observations
R E S U L T S I RVAT ASTRONOM CAL OBSE IONS, MADE A T THE OBSERVATORY OF THE I E UN V RSITY, D U R H A M , N 184-6 TO UL 1848 FROMJA UARY, , J Y, , UN DEB THE DI RECTI O N O F L B . H E V . L L F T R . R E D . s TE M P E C H EV A I ER, , A _ PRO F B SO B O E A N D A STRO N O I Y I N THE UN I V ERS I TY O F DURHA M . R EV . N H N B . A . THE ROBERTA CHORT OMPSO , O BS ERV ER I N THE UN I V ERS I TY. D U R H A M PRIN D P HUMBLE. TED BY THE E! EC UTO RS O F E W . IN TRODUCTION . HE servat r of the niversi of Durham was built in 1841 rin T Ob oy U t , ci all y p p y h ubscri tion . The servati ns un er t e eneral su erint n byprivate s p Ob o , d g p e den ce of the r fess r of at ematics and str n m are c n uc e an O server P o o M h A oo y, od tdby b , Th f ll win a es c ntain the results resident at the Observatory . e oo gpg o of O bser ns ma e et ween anuar 1846 and ul 1848 . -
VSSC159 Mar 2014 Corrected CHART.Pmd
British Astronomical Association VARIABLE STAR SECTION CIRCULAR No 159, March 2014 Contents V391/V393 Cassiopeiae Chart - J. Toone ................................ inside front cover From the Director - R. Pickard ........................................................................... 3 Nova Del 2013 (V339 Del)-The First 100 days - G. Poyner ............................. 4 Supernova SN2014J in M82 - D. Boyd ............................................................. 6 Eclipsing Binary News - D. Loughney .............................................................. 8 Why Continue to Observe the Eclipsing Binary OO Aql - L. Corp ................ 10 Online Submission of Observations - A. Wilson .............................................. 16 SS Cephei - M. Taylor ..................................................................................... 19 A ‘Secondary’ Challenge for Observers of Eclipsing Binaries -T. Markham ... 20 Spectrum of the T Tauri star BP Tauri - D. Boyd ........................................... 24 Recent Observations of some Eclipsing Binaries with the Bradford Robotic Telescope - D. Conner ..................................... 26 2013 the year that R Sct switched to Mira mode - J. Toone ........................... 29 Binocular Programme - M. Taylor ................................................................... 31 Eclipsing Binary Predictions – Where to Find Them - D. Loughney .............. 34 Charges for Section Publications .............................................. inside back cover Guidelines -
The Universe Contents 3 HD 149026 B
History . 64 Antarctica . 136 Utopia Planitia . 209 Umbriel . 286 Comets . 338 In Popular Culture . 66 Great Barrier Reef . 138 Vastitas Borealis . 210 Oberon . 287 Borrelly . 340 The Amazon Rainforest . 140 Titania . 288 C/1861 G1 Thatcher . 341 Universe Mercury . 68 Ngorongoro Conservation Jupiter . 212 Shepherd Moons . 289 Churyamov- Orientation . 72 Area . 142 Orientation . 216 Gerasimenko . 342 Contents Magnetosphere . 73 Great Wall of China . 144 Atmosphere . .217 Neptune . 290 Hale-Bopp . 343 History . 74 History . 218 Orientation . 294 y Halle . 344 BepiColombo Mission . 76 The Moon . 146 Great Red Spot . 222 Magnetosphere . 295 Hartley 2 . 345 In Popular Culture . 77 Orientation . 150 Ring System . 224 History . 296 ONIS . 346 Caloris Planitia . 79 History . 152 Surface . 225 In Popular Culture . 299 ’Oumuamua . 347 In Popular Culture . 156 Shoemaker-Levy 9 . 348 Foreword . 6 Pantheon Fossae . 80 Clouds . 226 Surface/Atmosphere 301 Raditladi Basin . 81 Apollo 11 . 158 Oceans . 227 s Ring . 302 Swift-Tuttle . 349 Orbital Gateway . 160 Tempel 1 . 350 Introduction to the Rachmaninoff Crater . 82 Magnetosphere . 228 Proteus . 303 Universe . 8 Caloris Montes . 83 Lunar Eclipses . .161 Juno Mission . 230 Triton . 304 Tempel-Tuttle . 351 Scale of the Universe . 10 Sea of Tranquility . 163 Io . 232 Nereid . 306 Wild 2 . 352 Modern Observing Venus . 84 South Pole-Aitken Europa . 234 Other Moons . 308 Crater . 164 Methods . .12 Orientation . 88 Ganymede . 236 Oort Cloud . 353 Copernicus Crater . 165 Today’s Telescopes . 14. Atmosphere . 90 Callisto . 238 Non-Planetary Solar System Montes Apenninus . 166 How to Use This Book 16 History . 91 Objects . 310 Exoplanets . 354 Oceanus Procellarum .167 Naming Conventions . 18 In Popular Culture . -
The Planetary and Lunar Ephemeris DE 421
IPN Progress Report 42-178 • August 15, 2009 The Planetary and Lunar Ephemeris DE 421 William M. Folkner,* James G. Williams,† and Dale H. Boggs† The planetary and lunar ephemeris DE 421 represents updated estimates of the orbits of the Moon and planets. The lunar orbit is known to submeter accuracy through fitting lunar laser ranging data. The orbits of Venus, Earth, and Mars are known to subkilometer accu- racy. Because of perturbations of the orbit of Mars by asteroids, frequent updates are needed to maintain the current accuracy into the future decade. Mercury’s orbit is determined to an accuracy of several kilometers by radar ranging. The orbits of Jupiter and Saturn are determined to accuracies of tens of kilometers as a result of spacecraft tracking and modern ground-based astrometry. The orbits of Uranus, Neptune, and Pluto are not as well deter- mined. Reprocessing of historical observations is expected to lead to improvements in their orbits in the next several years. I. Introduction The planetary and lunar ephemeris DE 421 is a significant advance over earlier ephemeri- des. Compared with DE 418, released in July 2007,1 the DE 421 ephemeris includes addi- tional data, especially range and very long baseline interferometry (VLBI) measurements of Mars spacecraft; range measurements to the European Space Agency’s Venus Express space- craft; and use of current best estimates of planetary masses in the integration process. The lunar orbit is more robust due to an expanded set of lunar geophysical solution parameters, seven additional months of laser ranging data, and complete convergence. -
July 2014 BRAS Newsletter
July, 2014 Next Meeting July 19th, 11:00AM at LIGO The LIGO facility in Livingston Parish, LA What's In This Issue? President's Message Secretary's Summary of June Meeting Astroshort- Not-So-Rare Earths Message from the HRPO Globe At Night EBR Parish Library Children's Reading Program Recent BRAS Forum Entries Observing Notes from John Nagle President's Message WE WILL NOT MEET ON THE SECOND MONDAY NIGHT, AS WE USUALLY DO. Our next meeting will be Saturday, July 19, 2014, 11 AM – 4 PM at LIGO, Livingston. It will be a picnic/star-b-cue and enjoy each other’s company. We will meet under the pavilion by the pond at 11 AM to begin the picnic. BRAS will provide the main course. You can bring a small dish if you wish. At 1 PM, we can join the public for LIGO’s regular Saturday Science day activities. That includes the museum, hands on experiments, a video about LIGO “Einstein’s Messengers”, and a tour of the facility. One new thing we would like to do is set a table aside for anyone who has astronomical equipment they want to sell – telescopes, mounts, accessories, binoculars, cameras, books, etc. The idea is to have an impromptu garage sale (or swap meet). Bring what you have and let’s see if we can move it. LIGO is only open during the day, so the only stargazing we will be able to do will be solar. However, we will demonstrate the 35mm Lundt solar scope BRAS is raffling and sell tickets for the raffle.