The Detached Dust Shells of AQ Andromedae, U Antliae, and TT Cygni ,
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Annual Report 2017
Koninklijke Sterrenwacht van België Observatoire royal de Belgique Royal Observatory of Belgium Jaarverslag 2017 Rapport Annuel 2017 Annual Report 2017 Cover illustration: Above: One billion star map of our galaxy created with the optical telescope of the satellite Gaia (Credit: ESA/Gaia/DPAC). Below: Three armillary spheres designed by Jérôme de Lalande in 1775. Left: the spherical sphere; in the centre: the geocentric model of our solar system (with the Earth in the centre); right: the heliocentric model of our solar system (with the Sun in the centre). Royal Observatory of Belgium - Annual Report 2017 2 De activiteiten beschreven in dit verslag werden ondersteund door Les activités décrites dans ce rapport ont été soutenues par The activities described in this report were supported by De POD Wetenschapsbeleid De Nationale Loterij Le SPP Politique Scientifique La Loterie Nationale The Belgian Science Policy The National Lottery Het Europees Ruimtevaartagentschap De Europese Gemeenschap L’Agence Spatiale Européenne La Communauté Européenne The European Space Agency The European Community Het Fonds voor Wetenschappelijk Onderzoek – Le Fonds de la Recherche Scientifique Vlaanderen Royal Observatory of Belgium - Annual Report 2017 3 Table of contents Preface .................................................................................................................................................... 6 Reference Systems and Planetology ...................................................................................................... -
U Antliae — a Dying Carbon Star
THE BIGGEST, BADDEST, COOLEST STARS ASP Conference Series, Vol. 412, c 2009 Donald G. Luttermoser, Beverly J. Smith, and Robert E. Stencel, eds. U Antliae — A Dying Carbon Star William P. Bidelman,1 Charles R. Cowley,2 and Donald G. Luttermoser3 Abstract. U Antliae is one of the brightest carbon stars in the southern sky. It is classified as an N0 carbon star and an Lb irregular variable. This star has a very unique spectrum and is thought to be in a transition stage from an asymptotic giant branch star to a planetary nebula. This paper discusses possi- ble atomic and molecular line identifications for features seen in high-dispersion spectra of this star at wavelengths from 4975 A˚ through 8780 A.˚ 1. Introduction U Antliae (U Ant = HR 4153 = HD 91793) is classified as an N0 carbon star with a visual magnitude of 5.38 and B−V of +2.88 (Hoffleit 1982). It also is classified as an Lb irregular variable with small scale light variations. Scattered light optical images for U Ant have been made and these observations are consistent the existence of a geometrically thin (∼3 arcsec) spherically symmetric shell of radius ∼43 arcsec. The size of this shell agrees very well with that of the detached shell seen in CO radio line emission. These observations also show the presence of at least one, possibly two, shells inside the 43 arcsec shell (Gonz´alez Delgado et al. 2001). In this paper, absorption lines in the optical spectrum of U Ant are tentatively identified for this bright cool carbon star. -
Eao Submillimetre Futures Paper Series, 2019
EAO SUBMILLIMETRE FUTURES PAPER SERIES, 2019 The East Asian Observatory∗ James Clerk Maxwell Telescope 660 N. A‘ohok¯ u¯ Place, Hilo, Hawai‘i, USA, 96720 1 About This Series Submillimetre astronomy is an active and burgeoning field that is poised to answer some of the most pressing open questions about the universe. The James Clerk Maxwell Telescope, operated by the East Asian Observatory, is at the forefront of discovery as it is the largest single-dish submillimetre telescope in the world. Situated at an altitude of 4,092 metres on Maunakea, Hawai‘i, USA, the facility capitalises on the 850 µm observing window that offers crucial insights into the cold dust that forms stars and galaxies. In 1997, the Submillimetre Common User Bolometer Array (SCUBA) was commissioned, allowing astronomers to detect the furthest galaxies ever recorded (so-called SCUBA galaxies) and develop our understanding of the earliest stages of star formation. Since 2011, its successor, SCUBA-2, has revolutionised submillimetre wavelength surveys by mapping the sky hundreds of times faster than SCUBA. The extensive data collected spans a wealth of astronomy sub-fields and has inspired world-wide collaborations and innovative analysis methods for nearly a decade. Building on the successes of these instruments, the East Asian Observatory is constructing a third generation 850 µm wide-field camera with intrinsic polarisation capabilities for deployment on the James Clerk Maxwell Telescope. In May, 2019, the “EAO Submillimetre Futures” meeting was held in Nanjing, China to discuss the science drivers of future instrumentation and the needs of the submillimetre astronomy community. A central focus of the meeting was the new 850 µm camera. -
Magisterarbeit
MAGISTERARBEIT Titel der Magisterarbeit “Imaging and photometry of U Antliae and AQ Andromedae using the Herschel space telescope” Verfasser Bernhard Baumann, Bakk.rer.nat. angestrebter akademischer Grad Magister der Naturwissenschaften (Mag.rer.nat.) Wien, 2012 Studienkennzahl lt. Studienblatt: A 066 861 Studienrichtung lt. Studienblatt: Magisterstudium Astronomie Betreuer: A. Univ. Prof. Dr. Franz Kerschbaum Danksagung Die hier vorgestellte Magisterarbeit wurde in Zusammenarbeit mit dem MESS Konsor- tium (http://www.univie.ac.at/space/MESS/) und dem Institut f¨ur Astronomie in Wien (http://astro.univie.ac.at/) erstellt. Ich bedanke mich bei Franz Kerschbaum, dass ich bei diesen internationalen Projekten, Herschel Space Telescope und MESS, mitarbeiten durfte und f¨ur die Betreuung der Ar- beit. Mein herzlicher Dank gilt der AGB-Arbeitsgruppe (http://www.univie.ac.at/agb/), besonders Roland Ottensamer f¨ur die vielen wertvollen Diskussionen, Anregungen und Korrekturen sowie Marko Mecina f¨ur die gute Zusammenarbeit als Studienkollege. Weiteren Korrekturlesern wie Verena Baumgartner und meinem Bruder Michael gilt mein Dank. Zu guter Letzt m¨ochte ich mich bei meinen Eltern sowie meinem Bruder Michael f¨ur die Unterst¨utzung und Motivation w¨ahrend meines Studiums bedanken. Wien, im M¨arz 2012. Zusammenfassung Die vorliegende Magisterarbeit beinhaltet die Beobachtungsauswertung und die Datenre- duktion zweier Asymptotic Giant Branch (AGB) Sterne, U Ant und AQ And, welche mithilfe des Herschel Weltraumteleskops aufgezeichnet wurden. Die Ergebnisse dieser Datenreduktion werden mit der Modellierung in DUSTY verglichen, welche den Strah- lungstransport in staubigen Umgebungen rund um Sterne simuliert. Mit den Ergebnis- sen ist es m¨oglich, R¨uckschl¨usse ¨uber die aktuelle und anschließende Entwicklung der Sterne zu ziehen. -
Reduced Maximum Mass-Loss Rate of OH/IR Stars Due to Overlooked Binary Interaction
The University of Manchester Research Reduced maximum mass-loss rate of OH/IR stars due to overlooked binary interaction DOI: 10.1038/s41550-019-0703-5 Document Version Accepted author manuscript Link to publication record in Manchester Research Explorer Citation for published version (APA): Decin, L., Homan, W., Danilovich, T., de Koter, A., Engels, D., Waters, L. B. F. M., Muller, S., Gielen, C., Garca- Hernandez, D. A., Stancliffe, R., Van de Sande, M., Molenberghs, G., Kerschbaum, F., Zijlstra, A., & El Mellah, I. (2019). Reduced maximum mass-loss rate of OH/IR stars due to overlooked binary interaction. Nature Astronomy, 3(5), 408-415. https://doi.org/10.1038/s41550-019-0703-5 Published in: Nature Astronomy Citing this paper Please note that where the full-text provided on Manchester Research Explorer is the Author Accepted Manuscript or Proof version this may differ from the final Published version. If citing, it is advised that you check and use the publisher's definitive version. General rights Copyright and moral rights for the publications made accessible in the Research Explorer are retained by the authors and/or other copyright owners and it is a condition of accessing publications that users recognise and abide by the legal requirements associated with these rights. Takedown policy If you believe that this document breaches copyright please refer to the University of Manchester’s Takedown Procedures [http://man.ac.uk/04Y6Bo] or contact [email protected] providing relevant details, so we can investigate your claim. Download date:08. Oct. 2021 Reduced maximum mass-loss rate of OH/IR stars due to overlooked binary interaction L. -
Stellar Life Cycle
1 23 45 6 789 10 11 12 13 14 15 16 17 18 19 20 21 22 23 24 25 26 27 28 29 30 31 32 33 34 Stellar Cycles Post Assessment Activity - Image Descriptions The name and type of object and/or artist illustration for each of the images is listed below. The stage of stellar evolution is indicated by the bold type. The URL for each of the deep sky objects is listed. For more specific information concerning the sequencing or selection of the images please refer to the Teacher Guide and Answer Key. 1. The Sun is a mid-sized main sequence star. 9. The Sagittarius A black hole in the center of the Milky Way Galaxy. [Solar and Heliospheric Observatory (SOHO) image] NOTE: This image is included for a specific reason, to address a http://antwrp.gsfc.nasa.gov/apod/ap981212.html common misconception that all black holes are the end result of the collapse of a massive star. Sagittarius A is the massive black 2. Sirius B (dim object in the background) is a white dwarf in a hole at the center of the Milky Way Galaxy. This type of black hole binary system with Sirius A (bright object in the foreground) - is not involved with stellar evolution. You can use this image as an a 2 solar mass main sequence star. assessment of student understanding of different types of black [McDonald Observatory image] holes, or simply for discussion. http://antwrp.gsfc.nasa.gov/apod/ap960902.html [Chandra X-Ray Observatory image] http://chandra.harvard.edu/photo/2003/0203long/more.html 3. -
Reduced Maximum Mass-Loss Rate of OH-IR Stars Ariv
UvA-DARE (Digital Academic Repository) Reduction of the maximum mass-loss rate of OH/IR stars due to unnoticed binary interaction Decin, L.; Homan, W.; Danilovich, T.; de Koter, A.; Engels, D.; Waters, L.B.F.M.; Muller, S.; Gielen, C.; García-Hernández, D.A.; Stancliffe, R.J.; Van de Sande, M.; Molenberghs, G.; Kerschbaum, F.; Zijlstra, A.A.; El Mellah, I. DOI 10.1038/s41550-019-0703-5 Publication date 2019 Document Version Submitted manuscript Published in Nature Astronomy Link to publication Citation for published version (APA): Decin, L., Homan, W., Danilovich, T., de Koter, A., Engels, D., Waters, L. B. F. M., Muller, S., Gielen, C., García-Hernández, D. A., Stancliffe, R. J., Van de Sande, M., Molenberghs, G., Kerschbaum, F., Zijlstra, A. A., & El Mellah, I. (2019). Reduction of the maximum mass-loss rate of OH/IR stars due to unnoticed binary interaction. Nature Astronomy, 3, 408-415. https://doi.org/10.1038/s41550-019-0703-5 General rights It is not permitted to download or to forward/distribute the text or part of it without the consent of the author(s) and/or copyright holder(s), other than for strictly personal, individual use, unless the work is under an open content license (like Creative Commons). Disclaimer/Complaints regulations If you believe that digital publication of certain material infringes any of your rights or (privacy) interests, please let the Library know, stating your reasons. In case of a legitimate complaint, the Library will make the material inaccessible and/or remove it from the website. Please Ask the Library: https://uba.uva.nl/en/contact, or a letter to: Library of the University of Amsterdam, Secretariat, Singel 425, 1012 WP Amsterdam, The Netherlands. -
Mira (Omicron Ceti)
Das Projekt ALMA Mater* Teil 3: Eine Beobachtung, die es in sich hat: kosmischer Baustofftransport *Wir verwenden die Bezeichnung Alma Mater als Synonym für eine Universität. Seinen Ursprung hat das Doppelwort im Lateinischen (alma: nähren, mater: Mutter). Im übertragenen Sinne ernährt die (mütterliche) Universität ihre Studenten mit Wissen. Und weiter gesponnen ernährt das Projekt ALMA auch die Schüler und Studenten mit Anreizen für das Lernen. (Zudem bedeutet das spanische Wort ‚Alma‘: Seele.) In Bezug zum Beitrag „Rote Riesen und das größte Radioteleskop der Welt“ in der Zeitschrift „Sterne und Weltraum“ (SuW) 3/2015, unter der Kategorie »Blick in die Forschung: Kurzberichte«, WIS-ID: 1285851 Olaf Fischer Schon die ersten Beobachtungen mit ALMA zeigen, welch enormer Zuwachs an Wissen möglich wird. Im Folgenden steht der Massenabfluss von solchen Sternen im Blickpunkt, die sich in einer späten Lebensphase befinden, welche sich entsprechend ihrer Zustandswerte im HRD im AGB-Gebiet (Asymp- totic Giant Branch) befinden. Diese Sterne stellen die wichtigste Quelle für die Anreicherung des inter- stellaren Mediums mit schweren Elementen dar (bedeutender als Supernovae). Folglich muss man den Massenabfluss, sozusagen einen kosmischen Baustofftransport, studieren, um etwas über die Bildung folgender Sterngenerationen samt ihrer Planeten und vielleicht sogar möglichen Lebewesen zu lernen. Im folgenden WIS-Beitrag steht ein aktuelles Forschungsergebnis von ALMA im Brennpunkt – die Entdeckung einer Spiralstruktur im Massenabfluss des AGB-Sterns R Sculptoris (R Scl). Ausgehend von der Veröffentlichung dieser Entdeckung in der Zeitschrift „Nature“ wird eine Brücke zur Schule gebaut. Wir wollen dabei den Gedankengängen der Autoren folgen und dies anhand der unten aufgeführten Fragen tun. Es wird gezeigt, dass man mit dem Schulwissen etliche Aspekte des Nature-Beitrags (Begriffe, Aussagen Abbildungen) verstehen kann. -
Monthly Newsletter of the Durban Centre - November 2017
Page 1 Monthly Newsletter of the Durban Centre - November 2017 Page 2 Table of Contents Chairman’s Chatter …...…………………………….………..….…… 3 Carbon Stars ……………………………………...………………….... 5 At the Eye Piece …..……………...……….….………………..….…. 9 The Cover Image - NGC 246 (Skull Nebula) ………..………..….. 11 Bits and Pieces ………..…...………………………..….….…...….... 12 Mystery of a New Star …..……………………………..…..………... 14 Shape Shifting Bacteria …….…………….…………….….……….. 16 Members Moments ………………………….…..………….….…..... 21 The Month Ahead …..…………………...….…….……………..…… 24 Minutes of the Meeting ………………………………………..…….. 25 Facts about the SMC and LMC …………………………………….. 26 Public Viewing Roster …………………………….……….…..……. 27 Pre-loved Telescope Equipment …………………………..……… 28 ASSA Symposium 2018 ………………………...…………......…… 29 Member Submissions Disclaimer: The views expressed in ‘nDaba are solely those of the writer and are not necessarily the views of the Durban Centre, nor the Editor. All images and content is the work of the respective copyright owner Page 3 Chairman’s Chatter By Mike Hadlow Dear Members, Already November! The year is almost over and we have definitely entered into the rainy season, with floods having recently been experienced, and significant cloud cover virtually every evening. This has resulted in us having to cancel both of our last public viewings. The society has nevertheless been busy during October with a number of activities; including, having a stand at Hobby X from the 6 to 8 of October. Thanks to those of you who assisted in setting up the stand, representing our society to the many visitors, selling raffle tickets, selling the last of our starter kits and attracting a few new members to the society. Unfortunately, due to activities at the school, we had to cancel the proposed braai, telescope workshop and the short media liaison course that Logan was to present at the school on the afternoon of 21 October. -
Information Bulletin on Variable Stars
COMMISSIONS AND OF THE I A U INFORMATION BULLETIN ON VARIABLE STARS Nos March November EDITORS L SZABADOS K OLAH TECHNICAL EDITOR A HOLL TYPESETTING K ORI ADMINISTRATION Zs KOVARI EDITORIAL BOARD L A BALONA M BREGER E BUDDING M deGROOT E GUINAN D S HALL P HARMANEC M JERZYKIEWICZ K C LEUNG M RODONO N N SAMUS J SMAK C STERKEN H BUDAPEST XI I Box HUNGARY HU ISSN COPYRIGHT NOTICE IBVS is published on b ehalf of the th and nd Commissions of the IAU by the Konkoly Observatory Budap est Hungary Individual issues could b e downloaded for scientic and educational purp oses free of charge Bibliographic information of the recent issues could b e entered to indexing sys tems No IBVS issues may b e stored in a public retrieval system in any form or by any means electronic or otherwise without the prior written p ermission of the publishers Prior written p ermission of the publishers is required for entering IBVS issues to an electronic indexing or bibliographic system to o CONTENTS E PAUNZEN G HANDLER Pulsation of HD and HD :::: E PAUNZEN WW WEISS R KUSCHNIG Nonvariability among Bo o Star I ESO and Data :::::::::::::::::::::::::::::::::: PA HECKERT Photometry of SV Camelopardalis :::::::::::::::: M WOLF L SAROUNOVA P MOLIK Period Changes in V Ophiuchi ::::::::::::::::::::::::::::::::::::::::::::::::::: ::::::::::::: RM ROBB MD GLADDERS Optical Observations of the Active Star FF Cancri ::::::::::::::::::::::::::::::::::::::::::::::::::: ::::::: U BASTIAN E BORN F AGERER M DAHM V GROSSMANN V MAKAROV Conrmation of the -
MEMORIA IAC 2010 SUBCOMITES - Finanzas 2 9 - Operación Del Obs
MEMORIA 2010 “INSTITUTO DE ASTROFISICA DE CANARIAS” “INSTITUTO DE ASTROFISICA DE CANARIAS” GABINETE DE DIRECCIÓN INSTITUTO DE ASTROFÍSICA DE CANARIAS (IAC) MAQUETACIÓN: Ana M. Quevedo PORTADA: Gotzon Cañada PREIMPRESIÓN E IMPRESIÓN: Producciones Gráficas S.L. DEPÓSITO LEGAL: TF-1905/94 Indice general 7- PRESENTACIÓN 8- CONSORCIO PÚBLICO IAC 11- LOS OBSERVATORIOS DE CANARIAS 12- - Observatorio del Teide (OT) 13- - Observatorio del Roque de los Muchachos (ORM) 14- COMISIÓN PARA LA ASIGNACIÓN DE TIEMPO (CAT) 18- ACUERDOS 20- Gran Telescopio CANARIAS (GTC) 25- ÁREA DE INVESTIGACIÓN 28- - Estructura del Universo y Cosmología 50- - El Universo Local 88- - Física de las estrellas, Sistemas Planetarios y Medio Interestelar 124- - El Sol y el Sistema Solar 146- - Instrumentación y Espacio 180- - Otros 202- ÁREA DE INSTRUMENTACIÓN 202- - Ingeniería 214- - Producción 222- - Oficina de Transferencia de Resultados de Investigación (OTRI) 234- ÁREA DE ENSEÑANZA 234- - Cursos de doctorado 235- - Seminarios científicos 239- - Coloquios 239- - Becas 241- - XXII Escuela de Invierno: ”Astrosismología” 243- ADMINISTRACIÓN DE SERVICIOS GENERALES 243- - Instituto de Astrofísica 244- - Observatorio del Teide 245- - Observatorio del Roque de los Muchachos 246- - Centro de Astrofísica de la Palma 247- - Oficina Técnica para la Protección de la Calidad del Cielo (OTPC) 249- - Ejecución del Presupuesto 2010 250- GABINETE DE DIRECCIÓN 250- - Ediciones 252- - Comunicación y divulgación 263- - Web 265- - Visitas a las instalaciones del IAC 268- SERVICIOS INFORMÁTICOS -
AST Senior Review Major Recommendations
NSF Division of Astronomical Sciences (AST): AAAC Ralph Gaume Deputy Division Director September 27, 2017 NSF, MPS, Big Ideas • Jim Ulvestad, Acting Assistant Director, Directorate for Mathematical and Physical Sciences • Presentation, Questions 09/27/2017 AAAC-NSF/AST 2 Talk Outline • Highlights • The Move • AST Personnel • AST Grant Program • AST Facilities – Including Divestment • AST Budget (FY 2018) 9/27/2017 AAAC-NSF/AST 3 Some Highlights 9/27/2017 AAAC 4 Continental-America Telescope Eclipse (CATE) • Led by Matt Penn of NSF’s National Solar Observatory • 68 identical telescope sites along the path of totality manned by citizen scientists • Images every 10 seconds with 2 arcsecond resolution • 90+ minutes of eclipse data (coronal movie) 9/27/2017 AAAC-NSF/AST 6 Dark Energy Survey Determines Cosmological Parameters The DES collaboration analyzed the first year of imaging data from the Dark Energy Camera on the NOAO Blanco 4m telescope. Those determinations alone are comparable in accuracy to those of the Planck mission. Credit: C. Chang et al,, arxiv:1708.01535 (2017) Credit: Dark Energy Collaboration, arxiv 1708.01530 (2017 ) . Utilized weak lensing distortion of 26 million source galaxies in four redshift bins (mass map above), and the angular correlation of 650,000 luminous red galaxies for the analysis. Combined with other cosmological measures, they derive values for the density of dark energy and dark matter with ~1% uncertainty, and the equation of state to ~4%. The investigation is supported jointly by NSF and DOE. Two highlights: ALMA and VLA ALMA: Outflows from AGB stars - Thermal CO spectral line data cube of U Antlia.