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C M Y K www.newssun.com EWS UN NHighlands County’s Hometown-S Newspaper Since 1927 Rivalry rout Deadly wreck in Polk Harris leads Lake 20-year-old woman from Lake Placid to shutout of AP Placid killed in Polk crash SPORTS, B1 PAGE A2 PAGE B14 Friday-Saturday, March 22-23, 2013 www.newssun.com Volume 94/Number 35 | 50 cents Forecast Fire destroys Partly sunny and portable at Fred pleasant High Low Wild Elementary Fire alarms “Myself, Mr. (Wally) 81 62 Cox and other administra- Complete Forecast went off at 2:40 tors were all called about PAGE A14 a.m. Wednesday 3 a.m.,” Waldron said Wednesday morning. Online By SAMANTHA GHOLAR Upon Waldron’s arrival, [email protected] the Sebring Fire SEBRING — Department along with Investigations into a fire DeSoto City Fire early Wednesday morning Department, West Sebring on the Fred Wild Volunteer Fire Department Question: Do you Elementary School cam- and Sebring Police pus are under way. Department were all on think the U.S. govern- The school’s fire alarms the scene. ment would ever News-Sun photo by KATARA SIMMONS Rhoda Ross reads to youngsters Linda Saraniti (from left), Chyanne Carroll and Camdon began going off at approx- State Fire Marshal seize money from pri- Carroll on Wednesday afternoon at the Lake Placid Public Library. Ross was reading from imately 2:40 a.m. and con- investigator Raymond vate bank accounts a children’s book she wrote and illustrated called ‘A Wildflower for all Seasons.’ tinued until about 3 a.m., Miles Davis was on the like is being consid- according to FWE scene for a large part of ered in Cyprus? Principal Laura Waldron. -
March 21–25, 2016
FORTY-SEVENTH LUNAR AND PLANETARY SCIENCE CONFERENCE PROGRAM OF TECHNICAL SESSIONS MARCH 21–25, 2016 The Woodlands Waterway Marriott Hotel and Convention Center The Woodlands, Texas INSTITUTIONAL SUPPORT Universities Space Research Association Lunar and Planetary Institute National Aeronautics and Space Administration CONFERENCE CO-CHAIRS Stephen Mackwell, Lunar and Planetary Institute Eileen Stansbery, NASA Johnson Space Center PROGRAM COMMITTEE CHAIRS David Draper, NASA Johnson Space Center Walter Kiefer, Lunar and Planetary Institute PROGRAM COMMITTEE P. Doug Archer, NASA Johnson Space Center Nicolas LeCorvec, Lunar and Planetary Institute Katherine Bermingham, University of Maryland Yo Matsubara, Smithsonian Institute Janice Bishop, SETI and NASA Ames Research Center Francis McCubbin, NASA Johnson Space Center Jeremy Boyce, University of California, Los Angeles Andrew Needham, Carnegie Institution of Washington Lisa Danielson, NASA Johnson Space Center Lan-Anh Nguyen, NASA Johnson Space Center Deepak Dhingra, University of Idaho Paul Niles, NASA Johnson Space Center Stephen Elardo, Carnegie Institution of Washington Dorothy Oehler, NASA Johnson Space Center Marc Fries, NASA Johnson Space Center D. Alex Patthoff, Jet Propulsion Laboratory Cyrena Goodrich, Lunar and Planetary Institute Elizabeth Rampe, Aerodyne Industries, Jacobs JETS at John Gruener, NASA Johnson Space Center NASA Johnson Space Center Justin Hagerty, U.S. Geological Survey Carol Raymond, Jet Propulsion Laboratory Lindsay Hays, Jet Propulsion Laboratory Paul Schenk, -
Nova Report 2006-2007
NOVA REPORTNOVA 2006 - 2007 NOVA REPORT 2006-2007 Illustration on the front cover The cover image shows a composite image of the supernova remnant Cassiopeia A (Cas A). This object is the brightest radio source in the sky, and has been created by a supernova explosion about 330 year ago. The star itself had a mass of around 20 times the mass of the sun, but by the time it exploded it must have lost most of the outer layers. The red and green colors in the image are obtained from a million second observation of Cas A with the Chandra X-ray Observatory. The blue image is obtained with the Very Large Array at a wavelength of 21.7 cm. The emission is caused by very high energy electrons swirling around in a magnetic field. The red image is based on the ratio of line emission of Si XIII over Mg XI, which brings out the bi-polar, jet-like, structure. The green image is the Si XIII line emission itself, showing that most X-ray emission comes from a shell of stellar debris. Faintly visible in green in the center is a point-like source, which is presumably the neutron star, created just prior to the supernova explosion. Image credits: Creation/compilation: Jacco Vink. The data were obtained from: NASA Chandra X-ray observatory and Very Large Array (downloaded from Astronomy Digital Image Library http://adil.ncsa.uiuc. edu). Related scientific publications: Hwang, Vink, et al., 2004, Astrophys. J. 615, L117; Helder and Vink, 2008, Astrophys. J. in press. -
18Th Meeting of the Venus Exploration Analysis Group (Vexag)
18TH MEETING OF THE VENUS EXPLORATION ANALYSIS GROUP (VEXAG) Program and Abstracts LPI Contribution No. 2356 18th Meeting of the Venus Exploration Analysis Group November 16–17, 2020 Institutional Support Lunar and Planetary Institute Universities Space Research Association Convener Noam Izenberg Johns Hopkins Applied Physics Laboratory Darby Dyar Mount Holyoke College Science Organizing Committee Darby Dyar Planetary Science Institute, Mount Holyoke College Noam Izenberg JHU Applied Physics Laboratory Megan Andsell NASA Headquarters Natasha Johnson NASA Goddard Jennifer Jackson California Institute of Technology Jim Cutts Jet Propulsion Laboratory Tommy Thompson Jet Propulsion Laboratory Lunar and Planetary Institute 3600 Bay Area Boulevard Houston TX 77058-1113 Compiled in 2020 by Meeting and Publication Services Lunar and Planetary Institute USRA Houston 3600 Bay Area Boulevard, Houston TX 77058-1113 This material is based upon work supported by NASA under Award No. 80NSSC20M0173. Any opinions, findings, and conclusions or recommendations expressed in this volume are those of the author(s) and do not necessarily reflect the views of the National Aeronautics and Space Administration. The Lunar and Planetary Institute is operated by the Universities Space Research Association under a cooperative agreement with the Science Mission Directorate of the National Aeronautics and Space Administration. Material in this volume may be copied without restraint for library, abstract service, education, or personal research purposes; however, republication of any paper or portion thereof requires the written permission of the authors as well as the appropriate acknowledgment of this publication. ISSN No. 0161-5297 Abstracts for this meeting are available via the meeting website at https://www.hou.usra.edu/meetings/vexag2020/ Abstracts can be cited as Author A. -
Astrophysical Studies of Extrasolar Planetary Systems Using Infrared Interferometric Techniques Olivier Absil
Astrophysical studies of extrasolar planetary systems using infrared interferometric techniques Olivier Absil To cite this version: Olivier Absil. Astrophysical studies of extrasolar planetary systems using infrared interferometric techniques. Astrophysics [astro-ph]. Université de Liège, 2006. English. tel-00124720 HAL Id: tel-00124720 https://tel.archives-ouvertes.fr/tel-00124720 Submitted on 15 Jan 2007 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. Facult´edes Sciences D´epartement d’Astrophysique, G´eophysique et Oc´eanographie Astrophysical studies of extrasolar planetary systems using infrared interferometric techniques THESE` pr´esent´eepour l’obtention du diplˆomede Docteur en Sciences par Olivier Absil Soutenue publiquement le 17 mars 2006 devant le Jury compos´ede : Pr´esident: Pr. Jean-Pierre Swings Directeur de th`ese: Pr. Jean Surdej Examinateurs : Dr. Vincent Coude´ du Foresto Dr. Philippe Gondoin Pr. Jacques Henrard Pr. Claude Jamar Dr. Fabien Malbet Institut d’Astrophysique et de G´eophysique de Li`ege Mis en page avec la classe thloria. i Acknowledgments First and foremost, I want to express my deepest gratitude to my advisor, Professor Jean Surdej. I am forever indebted to him for striking my interest in interferometry back in my undergraduate student years; for introducing me to the world of scientific research and fostering so many international collaborations; for helping me put this work in perspective when I needed it most; and for guiding my steps, from the supervision of diploma thesis to the conclusion of my PhD studies. -
Making the Invisible Visible: a History of the Spitzer Infrared Telescope Facility (1971–2003)/ by Renee M
MAKING THE INVISIBLE A History of the Spitzer Infrared Telescope Facility (1971–2003) MONOGRAPHS IN AEROSPACE HISTORY, NO. 47 Renee M. Rottner MAKING THE INVISIBLE VISIBLE A History of the Spitzer Infrared Telescope Facility (1971–2003) MONOGRAPHS IN AEROSPACE HISTORY, NO. 47 Renee M. Rottner National Aeronautics and Space Administration Office of Communications NASA History Division Washington, DC 20546 NASA SP-2017-4547 Library of Congress Cataloging-in-Publication Data Names: Rottner, Renee M., 1967– Title: Making the invisible visible: a history of the Spitzer Infrared Telescope Facility (1971–2003)/ by Renee M. Rottner. Other titles: History of the Spitzer Infrared Telescope Facility (1971–2003) Description: | Series: Monographs in aerospace history; #47 | Series: NASA SP; 2017-4547 | Includes bibliographical references. Identifiers: LCCN 2012013847 Subjects: LCSH: Spitzer Space Telescope (Spacecraft) | Infrared astronomy. | Orbiting astronomical observatories. | Space telescopes. Classification: LCC QB470 .R68 2012 | DDC 522/.2919—dc23 LC record available at https://lccn.loc.gov/2012013847 ON THE COVER Front: Giant star Zeta Ophiuchi and its effects on the surrounding dust clouds Back (top left to bottom right): Orion, the Whirlpool Galaxy, galaxy NGC 1292, RCW 49 nebula, the center of the Milky Way Galaxy, “yellow balls” in the W33 Star forming region, Helix Nebula, spiral galaxy NGC 2841 This publication is available as a free download at http://www.nasa.gov/ebooks. ISBN 9781626830363 90000 > 9 781626 830363 Contents v Acknowledgments -
Vénus Les Transits De Vénus L’Exploration De Vénus Par Les Sondes Iconographie, Photos Et Additifs
VVÉÉNUSNUS Introduction - Généralités Les caractéristiques de Vénus Les transits de Vénus L’exploration de Vénus par les sondes Iconographie, photos et additifs GAP 47 • Olivier Sabbagh • Février 2015 Vénus I Introduction – Généralités Vénus est la deuxième des huit planètes du Système solaire en partant du Soleil, et la sixième par masse ou par taille décroissantes. La planète Vénus a été baptisée du nom de la déesse Vénus de la mythologie romaine. Symbolisme La planète Vénus doit son nom à la déesse de l'amour et de la beauté dans la mythologie romaine, Vénus, qui a pour équivalent Aphrodite dans la mythologie grecque. Cythère étant une épiclèse homérique d'Aphrodite, l'adjectif « cythérien » ou « cythéréen » est parfois utilisé en astronomie (notamment dans astéroïde cythérocroiseur) ou en science-fiction (les Cythériens, une race de Star Trek). Par extension, on parle d'un Vénus à propos d'une très belle femme; de manière générale, il existe en français un lexique très développé mêlant Vénus au thème de l'amour ou du plaisir charnel. L'adjectif « vénusien » a remplacé « vénérien » qui a une connotation moderne péjorative, d'origine médicale. Les cultures chinoise, coréenne, japonaise et vietnamienne désignent Vénus sous le nom d'« étoile d'or », et utilisent les mêmes caractères (jīnxīng en hanyu, pinyin en hiragana, kinsei en romaji, geumseong en hangeul), selon la « théorie » des cinq éléments. Vénus était connue des civilisations mésoaméricaines; elle occupait une place importante dans leur conception du cosmos et du temps. Les Nahuas l'assimilaient au dieu Quetzalcoatl, et, plus précisément, à Tlahuizcalpantecuhtli (« étoile du matin »), dans sa phase ascendante et à Xolotl (« étoile du soir »), dans sa phase descendante. -
A Astronomical Terminology
A Astronomical Terminology A:1 Introduction When we discover a new type of astronomical entity on an optical image of the sky or in a radio-astronomical record, we refer to it as a new object. It need not be a star. It might be a galaxy, a planet, or perhaps a cloud of interstellar matter. The word “object” is convenient because it allows us to discuss the entity before its true character is established. Astronomy seeks to provide an accurate description of all natural objects beyond the Earth’s atmosphere. From time to time the brightness of an object may change, or its color might become altered, or else it might go through some other kind of transition. We then talk about the occurrence of an event. Astrophysics attempts to explain the sequence of events that mark the evolution of astronomical objects. A great variety of different objects populate the Universe. Three of these concern us most immediately in everyday life: the Sun that lights our atmosphere during the day and establishes the moderate temperatures needed for the existence of life, the Earth that forms our habitat, and the Moon that occasionally lights the night sky. Fainter, but far more numerous, are the stars that we can only see after the Sun has set. The objects nearest to us in space comprise the Solar System. They form a grav- itationally bound group orbiting a common center of mass. The Sun is the one star that we can study in great detail and at close range. Ultimately it may reveal pre- cisely what nuclear processes take place in its center and just how a star derives its energy. -
Improved Distances and Structure of Several Galactic Star-Forming Elds
Mem. S.A.It. Vol. 86, 344 c SAIt 2015 Memorie della Improved distances and structure of several Galactic star-forming elds N. Kaltcheva1 and V. Golev2 1 Department of Physics and Astronomy, University of Wisconsin Oshkosh, 800 Algoma Blvd., Oshkosh, WI 54901, USA; e-mail: [email protected] 2 Department of Astronomy, Faculty of Physics, St Kliment Ohridski University of Sofia, 5 James Bourchier Blvd., BG-1164 Sofia, Bulgaria; e-mail: [email protected] Abstract. We summarize results of precision photometry studies of prominent Galactic star-forming regions. The reliable uvbyβ photometry-based parallaxes we utilize for our purpose not only provide a significant revision of the OB-star distribution, but also help to identify previously undetected OB-groups. Key words. Stars: distances – Stars: OB groups – Galaxy: star-forming regions 1. Introduction much as 1.5 mag and thus to overestimate the distance to the Galactic star-forming fields. Optical observations of Galactic young clus- ters and OB associations provide reliable dis- 2. Findings tances for these objects, and thus structural de- tails in the overall study of the Galactic recent 2.1. Northern Monoceros star-formation sites. The distance estimates of the young Galactic groups are usually based Toward the Rosette Nebula and the Monoceros on spectroscopic or photometric parallaxes of Loop SNR, we identify a new OB-group of at individual members. Among the wide variety least 12 members at a distance of 1:26 ± 0:2 of photometric system, the uvbyβ photometry kpc. The group is possibly connected to the (Stromgren¨ 1966; Crawford & Mander 1966) Loop (Kaltcheva & Golev 2011). -
In This Issue: a to K, Please Bring a Main Dish 1
The Rosette Gazette Volume 21,, IssueIssue 1 Newsletter of the Rose CityCity AstronomersAstronomers January, 2009 RCA JANUARY 19 HOLIDAY POTLUCK! As weather prevented the December holiday meeting from taking place the January meeting of the Rose City Astronomers will be a holiday potluck and social gathering for all family members to be held in the OMSI Cafeteria. Each member is asked to bring a dish to serve 10-12 people. If your last name begins with . In This Issue: A to K, please bring a main dish 1 .. General Meeting 2 .. Club Officers L to Q, please bring an appetizer or side dish .... Magazines .... RCA Library R to Z, please bring a dessert 3 .. The Observer’s Corner Plates, silverware, and beverages/ice will be supplied by the club. Just bring your dish 7 .. Southern Galaxies along with a serving utensil and enjoy the holiday spirit of the RCA membership. 10. Dec. Board Minutes The Holiday Social is a great event to pick up some excellent holiday deals! Save time to 11. Telescope Workshop shop at the RCA Sales Table for your favorite astronomy gifts. In addition, the Swap .... Astro Imaging SIG Meet will be back by popular demand and there will be ample empty tables around the .... Science Sig .... Downtowners lobby for everyone who is interested in displaying items for the Swap Meet. 12. Calendar There will also be tables provided for interesting celestial displays. If you have taken any astronomy pictures this year and want to share them, this is your ideal opportu- nity. Members also bring their latest inventions and "astro stuff." If you have a fun gadget, item, or tool, please bring it in and show it off to the rest of the membership! Note that January 19 is the THIRD Monday of the month which is the evening of our normal general meeting. -
Annual Report 2007 ESO
ESO European Organisation for Astronomical Research in the Southern Hemisphere Annual Report 2007 ESO European Organisation for Astronomical Research in the Southern Hemisphere Annual Report 2007 presented to the Council by the Director General Prof. Tim de Zeeuw ESO is the pre-eminent intergovernmental science and technology organisation in the field of ground-based astronomy. It is supported by 13 countries: Belgium, the Czech Republic, Denmark, France, Finland, Germany, Italy, the Netherlands, Portugal, Spain, Sweden, Switzerland and the United Kingdom. Further coun- tries have expressed interest in member- ship. Created in 1962, ESO provides state-of- the-art research facilities to European as- tronomers. In pursuit of this task, ESO’s activities cover a wide spectrum including the design and construction of world- class ground-based observational facili- ties for the member-state scientists, large telescope projects, design of inno- vative scientific instruments, developing new and advanced technologies, further- La Silla. ing European cooperation and carrying out European educational programmes. One of the most exciting features of the In 2007, about 1900 proposals were VLT is the possibility to use it as a giant made for the use of ESO telescopes and ESO operates the La Silla Paranal Ob- optical interferometer (VLT Interferometer more than 700 peer-reviewed papers servatory at several sites in the Atacama or VLTI). This is done by combining the based on data from ESO telescopes were Desert region of Chile. The first site is light from several of the telescopes, al- published. La Silla, a 2 400 m high mountain 600 km lowing astronomers to observe up to north of Santiago de Chile. -
The Benefit of Simultaneous Seven-Filter Imaging: 10 Years of Grond Observations
Draft version December 4, 2018 Typeset using LATEX preprint2 style in AASTeX61 THE BENEFIT OF SIMULTANEOUS SEVEN-FILTER IMAGING: 10 YEARS OF GROND OBSERVATIONS J. Greiner1 1Max-Planck-Institut für extraterrestrische Physik, 85740 Garching, Germany ABSTRACT A variety of scientific results have been achieved over the last 10 years with the GROND simul- taneous 7-channel imager at the 2.2m telescope of the Max-Planck Society at ESO/La Silla. While designed primarily for rapid observations of gamma-ray burst afterglows, the combination of si- 0 0 0 0 multaneous imaging in the Sloan g r i z and near-infrared JHKs bands at a medium-sized (2.2 m) telescope and the very flexible scheduling possibility has resulted in an extensive use for many other astrophysical research topics, from exoplanets and accreting binaries to galaxies and quasars. Keywords: instrumentation: detectors, techniques: photometric arXiv:1812.00636v1 [astro-ph.HE] 3 Dec 2018 [email protected] 2 1. INTRODUCTION (5) mapping of galaxies to study their stel- An increasing number of scientific questions lar population; (6) multi-color light curves of require the measurement of spatially and spec- supernovae to, e.g., recognize dust formation trally resolved intensities of radiation from as- (Taubenberger et al. 2006); (7) differentiat- trophysical objects. Over the last decade, tran- ing achromatic microlensing events (Paczyn- sient and time-variable sources are increasingly ski 1986) from other variables with similar moving in the focus of present-day research light curves; (8) identifying objects with pe- (with its separate naming of “time-domain as- culiar SEDs, e.g.