HIPPARCHOSHIPPARCHOS the Hellenic Astronomical Society Newsletter Volume 2, Issue 11
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Astronomie in Theorie Und Praxis 8. Auflage in Zwei Bänden Erik Wischnewski
Astronomie in Theorie und Praxis 8. Auflage in zwei Bänden Erik Wischnewski Inhaltsverzeichnis 1 Beobachtungen mit bloßem Auge 37 Motivation 37 Hilfsmittel 38 Drehbare Sternkarte Bücher und Atlanten Kataloge Planetariumssoftware Elektronischer Almanach Sternkarten 39 2 Atmosphäre der Erde 49 Aufbau 49 Atmosphärische Fenster 51 Warum der Himmel blau ist? 52 Extinktion 52 Extinktionsgleichung Photometrie Refraktion 55 Szintillationsrauschen 56 Angaben zur Beobachtung 57 Durchsicht Himmelshelligkeit Luftunruhe Beispiel einer Notiz Taupunkt 59 Solar-terrestrische Beziehungen 60 Klassifizierung der Flares Korrelation zur Fleckenrelativzahl Luftleuchten 62 Polarlichter 63 Nachtleuchtende Wolken 64 Haloerscheinungen 67 Formen Häufigkeit Beobachtung Photographie Grüner Strahl 69 Zodiakallicht 71 Dämmerung 72 Definition Purpurlicht Gegendämmerung Venusgürtel Erdschattenbogen 3 Optische Teleskope 75 Fernrohrtypen 76 Refraktoren Reflektoren Fokus Optische Fehler 82 Farbfehler Kugelgestaltsfehler Bildfeldwölbung Koma Astigmatismus Verzeichnung Bildverzerrungen Helligkeitsinhomogenität Objektive 86 Linsenobjektive Spiegelobjektive Vergütung Optische Qualitätsprüfung RC-Wert RGB-Chromasietest Okulare 97 Zusatzoptiken 100 Barlow-Linse Shapley-Linse Flattener Spezialokulare Spektroskopie Herschel-Prisma Fabry-Pérot-Interferometer Vergrößerung 103 Welche Vergrößerung ist die Beste? Blickfeld 105 Lichtstärke 106 Kontrast Dämmerungszahl Auflösungsvermögen 108 Strehl-Zahl Luftunruhe (Seeing) 112 Tubusseeing Kuppelseeing Gebäudeseeing Montierungen 113 Nachführfehler -
![Arxiv:2105.11583V2 [Astro-Ph.EP] 2 Jul 2021 Keck-HIRES, APF-Levy, and Lick-Hamilton Spectrographs](https://docslib.b-cdn.net/cover/4203/arxiv-2105-11583v2-astro-ph-ep-2-jul-2021-keck-hires-apf-levy-and-lick-hamilton-spectrographs-364203.webp)
Arxiv:2105.11583V2 [Astro-Ph.EP] 2 Jul 2021 Keck-HIRES, APF-Levy, and Lick-Hamilton Spectrographs
Draft version July 6, 2021 Typeset using LATEX twocolumn style in AASTeX63 The California Legacy Survey I. A Catalog of 178 Planets from Precision Radial Velocity Monitoring of 719 Nearby Stars over Three Decades Lee J. Rosenthal,1 Benjamin J. Fulton,1, 2 Lea A. Hirsch,3 Howard T. Isaacson,4 Andrew W. Howard,1 Cayla M. Dedrick,5, 6 Ilya A. Sherstyuk,1 Sarah C. Blunt,1, 7 Erik A. Petigura,8 Heather A. Knutson,9 Aida Behmard,9, 7 Ashley Chontos,10, 7 Justin R. Crepp,11 Ian J. M. Crossfield,12 Paul A. Dalba,13, 14 Debra A. Fischer,15 Gregory W. Henry,16 Stephen R. Kane,13 Molly Kosiarek,17, 7 Geoffrey W. Marcy,1, 7 Ryan A. Rubenzahl,1, 7 Lauren M. Weiss,10 and Jason T. Wright18, 19, 20 1Cahill Center for Astronomy & Astrophysics, California Institute of Technology, Pasadena, CA 91125, USA 2IPAC-NASA Exoplanet Science Institute, Pasadena, CA 91125, USA 3Kavli Institute for Particle Astrophysics and Cosmology, Stanford University, Stanford, CA 94305, USA 4Department of Astronomy, University of California Berkeley, Berkeley, CA 94720, USA 5Cahill Center for Astronomy & Astrophysics, California Institute of Technology, Pasadena, CA 91125, USA 6Department of Astronomy & Astrophysics, The Pennsylvania State University, 525 Davey Lab, University Park, PA 16802, USA 7NSF Graduate Research Fellow 8Department of Physics & Astronomy, University of California Los Angeles, Los Angeles, CA 90095, USA 9Division of Geological and Planetary Sciences, California Institute of Technology, Pasadena, CA 91125, USA 10Institute for Astronomy, University of Hawai`i, -
The VAST Survey – IV. a Wide Brown Dwarf Companion to the A3V Star Ζ Delphini
MNRAS 445, 3694–3705 (2014) doi:10.1093/mnras/stu2018 The VAST Survey – IV. A wide brown dwarf companion to the A3V star ζ Delphini R. J. De Rosa,1,2† J. Patience,1 K. Ward-Duong,1 A. Vigan,3 C. Marois,4 I. Song,5 B. Macintosh,6,7 J. R. Graham,8 R. Doyon,9 M. S. Bessell,10 O. Lai,11,12 D. W. McCarthy13 and C. Kulesa13 1School of Earth and Space Exploration, Arizona State University, PO Box 871404, Tempe, AZ 85287, USA 2School of Physics, College of Engineering, Mathematics and Physical Sciences, University of Exeter, Stocker Road, Exeter EX4 4QL, UK 3Aix Marseille Universite,´ CNRS, LAM (Laboratoire d’Astrophysique de Marseille) UMR 7326, F-13388 Marseille, France 4NRC Herzberg Astronomy and Astrophysics, 5071 West Saanich Road, Victoria, BC V9E 2E7, Canada 5Physics and Astronomy, University of Georgia, 240 Physics, Athens, GA 30602, USA Downloaded from 6Kavli Institute for Particle Astrophysics and Cosmology, Stanford University, Stanford, CA 94305, USA 7Institute of Geophysics and Planetary Physics, Lawrence Livermore National Laboratory, 7000 East Ave, Livermore, CA 94550, USA 8Department of Astronomy, University of California at Berkeley, Berkeley, CA 94720, USA 9Dept´ de Physique, Universite´ de Montreal,´ C.P. 6128, Succ. Centre-Ville, Montreal,´ QC H3C 3J7, Canada 10Research School of Astronomy and Astrophysics, Mount Stromlo Observatory, The Australian National University, ACT 2611, Australia 11Gemini Observatory, 670 N. A’ohoku Place, Hilo, HI 96720, USA http://mnras.oxfordjournals.org/ 12National Astronomical Observatory of Japan, 650 North A’ohoku Place, Hilo, HI 96720, USA 13Steward Observatory, University of Arizona, 933 N. -
DIRECT IMAGING DISCOVERY of a “SUPER-JUPITER” AROUND the LATE B-TYPE STAR Κ And∗
The Astrophysical Journal Letters, 763:L32 (6pp), 2013 February 1 doi:10.1088/2041-8205/763/2/L32 C 2013. The American Astronomical Society. All rights reserved. Printed in the U.S.A. DIRECT IMAGING DISCOVERY OF A “SUPER-JUPITER” AROUND THE LATE B-TYPE STAR κ And∗ J. Carson1,2, C. Thalmann2,3,M.Janson4, T. Kozakis1, M. Bonnefoy2, B. Biller2, J. Schlieder2,T.Currie5, M. McElwain5, M. Goto6, T. Henning2, W. Brandner2, M. Feldt2, R. Kandori7, M. Kuzuhara7,8, L. Stevens1,P.Wong1, K. Gainey1, M. Fukagawa9, Y. Kuwada9, T. Brandt4, J. Kwon7,L.Abe10,S.Egner11, C. Grady5,O.Guyon11, J. Hashimoto7, Y. Hayano11, M. Hayashi7, S. Hayashi11, K. Hodapp12,M.Ishii11,M.Iye7, G. Knapp4,T.Kudo11, N. Kusakabe7,T.Matsuo13,S.Miyama14,J.Morino7, A. Moro-Martin15, T. Nishimura11,T.Pyo11, E. Serabyn16, H. Suto7, R. Suzuki7, M. Takami17, N. Takato11, H. Terada11, D. Tomono11, E. Turner4,18, M. Watanabe19, J. Wisniewski20, T. Yamada21, H. Takami7,T.Usuda11, and M. Tamura7 1 Department of Physics & Astronomy, College of Charleston, 58 Coming Street, Charleston, SC 29424, USA 2 Max-Planck-Institut fur¨ Astronomie, Konigstuhl¨ 17, D-69117 Heidelberg, Germany 3 Astronomical Institute “Anton Pannekoek,” University of Amsterdam, Science Park 904, 1098-XH Amsterdam, The Netherlands 4 Department of Astrophysical Sciences, Princeton University, NJ 08544, USA 5 ExoPlanets and Stellar Astrophysics Laboratory, Code 667, Goddard Space Flight Center, Greenbelt, MD 20771, USA 6 Young Stars and Star Formation Universitats-Sternwarte¨ Munchen,¨ Ludwig-Maximilians-Universitat,¨ D-81679 -
Reach Your Ideal Chemistry Candidate in Print, Online and on Social Media
Reach your ideal chemistry candidate in print, online and on social media. Visit newscientistjobs.com and connect with thousands of chemistry professionals the easy way Contact us on 617-283-3213 or [email protected] STUPID ECONOMICS Why we’re hardwired to misunderstand finance PEA MILK, ANYONE? The non-dairy dairy explosion DITCHING DNA A brand new molecule for life WEEKLY September 22 – 28, 2018 THE MYSTERY OF THE UNIVERSE IN 10 OBJECTS Understand them, and we’ll understand everything Supermassive black holes Polystyrene planets Big bang afterglow Exploding dwarfs Superfast flashes Naked galaxies Monster stars No3196 US$6.99 CAN$6.99 38 and more... Science and technology news www.newscientist.com 0 72440 30690 5 US jobs in science THE WEIRDEST DINOSAUR Almost a bird, almost a whale – meet Spinosaurus PLUS NEW SCIENTIST ASKS THE PUBLIC: Our exclusive survey of attitudes to science Headlines grab attention, but only details inform. For over 28 years, that’s how Orbis has invested. By digging deep into a company’s fundamentals, we find value others miss. And by ignoring short-term market distractions, we’ve remained focused on long-term performance. For more details, ask your financial adviser or visit Orbis.com As with all investing, your capital is at risk. Past performance is not a reliable indicator of future results. Avoid distracting headlines Orbis Investments (U.K.) Limited is authorised and regulated by the Financial Conduct Authority SUBSCRIPTION OFFER More ideas... more discoveries... and now even more value SAVE 77% AND GET A FREE BOOK WORTH $35 “A beautifully produced book which gives an excellent overview of just what makes us tick” Subscribe today PRINT + APP + WEB HOW TO BE HUMAN Weekly magazine delivered to your door + Take a tour around the human body and brain + full digital access to the app and web in the ultimate guide to your amazing existence. -
Why Do Hydrogen and Helium Migrate from Some Planets and Smaller
Why do Hydrogen and Helium Migrate from Some Planets and Smaller Objects? Author Weitter Duckss Independent Researcher, Zadar, Croatia mail: [email protected] Project: https://www.svemir-ipaksevrti.com/ Abstract This article analyzes the processes through measuring the material incoming from the outer space onto Earth, through migrating of hydrogen and helium from our atmosphere and from other objects and through inability to detect the radioactive effects on stars and objects with melted interiorities. Habitable periods on such objects are determined through the processes. 1. Introduction The goal of the article is to give arguments, based on the existing data bases, that a constant growth of space objects, as well as their rotation and tidal forces, cause their warming up and radiation emissions, therefore making radioactive processes of fission and fusion – which are not detected on stars and other objects anyway – unnecessary. The article gives evidence of hydrogen and helium migrating towards the objects that have more mass and of temperature levels of stars being directly related to their chemical compositions and the objects in their orbits. The argumentation to support a habitable period will be derived from the natural processes of constant growth and matter gathering. 2. Why there is no radioactive emission, derived from the processes of fission and fusion, inside stars? All data bases indicate that astronomic research (or, evidence) support the existence of a constant (monotonous), omnipresent, slow gathering of matter. The processes are "more accelerated" in such part of the Universe where there is more matter gathered (in the form of nebulae, molecular clouds, etc.) during a long period of time, but gathering takes place constantly in the whole volume of the Universe as well. -
A COMPREHENSIVE STUDY of SUPERNOVAE MODELING By
A COMPREHENSIVE STUDY OF SUPERNOVAE MODELING by Chengdong Li BS, University of Science and Technology of China, 2006 MS, University of Pittsburgh, 2007 Submitted to the Graduate Faculty of the Dietrich School of Arts and Sciences in partial fulfillment of the requirements for the degree of Doctor of Philosophy University of Pittsburgh 2013 UNIVERSITY OF PITTSBURGH PHYSICS AND ASTRONOMY DEPARTMENT This dissertation was presented by Chengdong Li It was defended on January 22nd 2013 and approved by John Hillier, Professor, Department of Physics and Astronomy Rupert Croft, Associate Professor, Department of Physics Steven Dytman, Professor, Department of Physics and Astronomy Michael Wood-Vasey, Assistant Professor, Department of Physics and Astronomy Andrew Zentner, Associate Professor, Department of Physics and Astronomy Dissertation Director: John Hillier, Professor, Department of Physics and Astronomy ii Copyright ⃝c by Chengdong Li 2013 iii A COMPREHENSIVE STUDY OF SUPERNOVAE MODELING Chengdong Li, PhD University of Pittsburgh, 2013 The evolution of massive stars, as well as their endpoints as supernovae (SNe), is important both in astrophysics and cosmology. While tremendous progress towards an understanding of SNe has been made, there are still many unanswered questions. The goal of this thesis is to study the evolution of massive stars, both before and after explosion. In the case of SNe, we synthesize supernova light curves and spectra by relaxing two assumptions made in previous investigations with the the radiative transfer code cmfgen, and explore the effects of these two assumptions. Previous studies with cmfgen assumed γ-rays from radioactive decay deposit all energy into heating. However, some of the energy excites and ionizes the medium. -
Download This Article in PDF Format
A&A 593, A75 (2016) Astronomy DOI: 10.1051/0004-6361/201526326 & c ESO 2016 Astrophysics Direct Imaging discovery of a second planet candidate around the possibly transiting planet host CVSO 30? T. O. B. Schmidt1; 2, R. Neuhäuser2, C. Briceño3, N. Vogt4, St. Raetz5, A. Seifahrt6, C. Ginski7, M. Mugrauer2, S. Buder2; 8, C. Adam2, P. Hauschildt1, S. Witte1, Ch. Helling9, and J. H. M. M. Schmitt1 1 Hamburger Sternwarte, Gojenbergsweg 112, 21029 Hamburg, Germany e-mail: [email protected] 2 Astrophysikalisches Institut und Universitäts-Sternwarte, Universität Jena, Schillergäßchen 2-3, 07745 Jena, Germany 3 Cerro Tololo Inter-American Observatory CTIO/AURA/NOAO, Colina El Pino s/n. Casilla 603, 1700000 La Serena, Chile 4 Instituto de Física y Astronomía, Universidad de Valparaíso, Avenida Gran Bretaña 1111, 2340000 Valparaíso, Chile 5 European Space Agency ESA, ESTEC, SRE-S, Keplerlaan 1, 2201 AZ Noordwijk, The Netherlands 6 Department of Astronomy and Astrophysics, University of Chicago, 5640 S. Ellis Ave., Chicago, IL 60637, USA 7 Sterrewacht Leiden, PO Box 9513, Niels Bohrweg 2, 2300 RA Leiden, The Netherlands 8 Max-Planck-Institute for Astronomy, Königstuhl 17, 69117 Heidelberg, Germany 9 School of Physics and Astronomy SUPA, University of St. Andrews, North Haugh, St. Andrews, KY16 9SS, UK Received 16 April 2015 / Accepted 14 March 2016 ABSTRACT Context. Direct imaging has developed into a very successful technique for the detection of exoplanets in wide orbits, especially around young stars. Directly imaged planets can be both followed astrometrically on their orbits and observed spectroscopically and thus provide an essential tool for our understanding of the early solar system. -
Supernova 2007Bi As a Pair-Instability Explosion
doi: 10.1038/nature08579 SUPPLEMENTARY INFORMATION Supplementary Information (1) Technical observational details Photometry: Discovery and follow-up observations of SN 2007bi were obtained using the Palomar- QUEST camera mounted on the 48-inch Oschin Schmidt telescope at Palomar Observa- tory (P48) as part of the SN Factory (SNF) program[31]. These R-band observations were pipeline-reduced by the SNF software, including bias removal, flatfield corrections, and an astrometric solution. Observations using the robotic 60-inch telescope at Palomar Observatory (P60) were pipeline-processed[32], including trimming, bias removal, flatfield corrections, and an as- trometric solution. Observations using the 200-inch Hale telescope at Palomar Observatory (P200) were obtained using the Large Format Camera (LFC) in SDSS r-band and were cross-calibrated onto the standard R band as detailed below. Observations by the Catalina Sky Survey (CSS[15]) were obtained using the CCD cam- era mounted on the 0.7 m Catalina telescope. These unfiltered data were cross-calibrated onto the R-band grid as detailed below. Synthetic photometry was derived from the late-time Keck spectrum using the meth- ods of ref. [33]. Table 3 provides the full list of photometric data. Spectroscopy: Early-time spectroscopy presented in Fig. 1[34] was obtained with the Low Resolution Imaging Spectrometer (LRIS[26]) mounted on the 10 m Keck I telescope on Mauna Kea, Hawaii. The presented spectrum was obtained on Apr. 16, 2007 in long-slit mode. The exposure time was 600 s at airmass 1.08 under clear sky conditions with variable seeing around 2��. The D560 dichroic was used with the 600 line mm−1 grism on the blue side, and the 400 line mm−1 grating blazed at 8500 A˚ on the red side, with the 1.5�� slit oriented at the parallactic angle[35]. -
David Stevenson the Complex Lives of Star Clusters Astronomers’ Universe
David Stevenson The Complex Lives of Star Clusters Astronomers’ Universe More information about this series at http://www.springer.com/series/6960 David Stevenson The Complex Lives of Star Clusters David Stevenson Sherwood , UK ISSN 1614-659X ISSN 2197-6651 (electronic) Astronomers’ Universe ISBN 978-3-319-14233-3 ISBN 978-3-319-14234-0 (eBook) DOI 10.1007/978-3-319-14234-0 Library of Congress Control Number: 2015936043 Springer Cham Heidelberg New York Dordrecht London © Springer International Publishing Switzerland 2015 This work is subject to copyright. All rights are reserved by the Publisher, whether the whole or part of the material is concerned, specifi cally the rights of translation, reprinting, reuse of illustrations, recitation, broadcasting, reproduction on microfi lms or in any other physical way, and transmission or information storage and retrieval, electronic adaptation, computer software, or by similar or dissimilar methodology now known or hereafter developed. The use of general descriptive names, registered names, trademarks, service marks, etc. in this publication does not imply, even in the absence of a specifi c statement, that such names are exempt from the relevant protective laws and regulations and therefore free for general use. The publisher, the authors and the editors are safe to assume that the advice and information in this book are believed to be true and accurate at the date of publication. Neither the publisher nor the authors or the editors give a warranty, express or implied, with respect to the material contained herein or for any errors or omissions that may have been made. Cover photo of the Orion Nebula M42 courtesy of NASA Spitzer Printed on acid-free paper Springer International Publishing AG Switzerland is part of Springer Science+Business Media (www.springer.com) For my late mother, Margaret Weir Smith Stevenson Pref ace Stars are fairly social beasts. -
Cycle 20 Abstract Catalog (Based on Phase I Submissions)
Cycle 20 Abstract Catalog (Based on Phase I Submissions) Proposal Category: AR Scientific Category: STAR FORMATION ID: 12814 Program Title: Signatures of turbulence in directly imaged protoplanetary disks Principal Investigator: Philip Armitage PI Institution: University of Colorado at Boulder HST imaging of the edge-on protoplanetary disk in the HH 30 system has shown that substantial changes to the morphology of the disk occur on time scales much shorter than the local dynamical time. This may be due to time- variable obscuration of starlight by the turbulent inner disk. More recently, mid-infrared variability of protoplanetary disks has been attributed to a similar physical origin. We propose a theoretical investigation that will establish whether the optical and infrared variability is due to turbulent variations in the scale height of dust in the inner disk, and determine what observations of that variability can tell us of the nature of disk turbulence. We will use a new generation of global magnetohydrodynamic simulations to directly model the turbulence in an annulus of the inner disk, extending from the dust destruction radius out to the radius where turbulence is quenched by poor coupling of the gas to magnetic fields. We will use the output of the MHD simulations as input to Monte Carlo radiative transfer calculations of stellar irradiation of the outer disk. We will use these calculations to produce light curves that show how time variable shadowing from the inner disk affects the outer disk observables: scattered light images and the infrared spectral energy distribution. Proposal Category: GO Scientific Category: COOL STARS ID: 12815 Program Title: Photometry of the Coldest Benchmark Brown Dwarf Principal Investigator: Kevin Luhman PI Institution: The Pennsylvania State University In 2011, we used images from the Spitzer Space Telescope to discover the coldest directly imaged companion to a nearby star (300-345 K). -
Gaia FGK Benchmark Stars: Effective Temperatures and Surface Gravities U
Astronomy & Astrophysics manuscript no. Heiter_etal_Benchmarkstars_LE c ESO 2018 September 25, 2018 Gaia FGK benchmark stars: Effective temperatures and surface gravities U. Heiter1, P. Jofré2, B. Gustafsson1; 4, A. J. Korn1, C. Soubiran3, and F. Thévenin5 1 Institutionen för fysik och astronomi, Uppsala universitet, Box 516, 751 20 Uppsala, Sweden e-mail: [email protected] 2 Institute of Astronomy, University of Cambridge, Madingley Rd, Cambridge, CB3 0HA, U.K. 3 Univ. Bordeaux, CNRS, LAB, UMR 5804, 33270, Floirac, France 4 Nordita, Roslagstullsbacken 23, 106 91, Stockholm, Sweden 5 Université de Nice Sophia Antipolis, CNRS (UMR7293), Observatoire de la Côte d’Azur, CS 34229, 06304, Nice Cedex 4, France Received / Accepted ABSTRACT Context. In the era of large Galactic stellar surveys, carefully calibrating and validating the data sets has become an important and integral part of the data analysis. Moreover, new generations of stellar atmosphere models and spectral line formation computations need to be subjected to benchmark tests to assess any progress in predicting stellar properties. Aims. We focus on cool stars and aim at establishing a sample of 34 Gaia FGK benchmark stars with a range of different metallicities. The goal was to determine the effective temperature and the surface gravity independently of spectroscopy and atmospheric models as far as possible. Most of the selected stars have been subjected to frequent spectroscopic investigations in the past, and almost all of them have previously been used as reference, calibration, or test objects. Methods. Fundamental determinations of Teff and log g were obtained in a systematic way from a compilation of angular diameter measurements and bolometric fluxes and from a homogeneous mass determination based on stellar evolution models.