Appendix II. Publications
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FY08 Technical Papers by GSMTPO Staff
AURA/NOAO ANNUAL REPORT FY 2008 Submitted to the National Science Foundation July 23, 2008 Revised as Complete and Submitted December 23, 2008 NGC 660, ~13 Mpc from the Earth, is a peculiar, polar ring galaxy that resulted from two galaxies colliding. It consists of a nearly edge-on disk and a strongly warped outer disk. Image Credit: T.A. Rector/University of Alaska, Anchorage NATIONAL OPTICAL ASTRONOMY OBSERVATORY NOAO ANNUAL REPORT FY 2008 Submitted to the National Science Foundation December 23, 2008 TABLE OF CONTENTS EXECUTIVE SUMMARY ............................................................................................................................. 1 1 SCIENTIFIC ACTIVITIES AND FINDINGS ..................................................................................... 2 1.1 Cerro Tololo Inter-American Observatory...................................................................................... 2 The Once and Future Supernova η Carinae...................................................................................................... 2 A Stellar Merger and a Missing White Dwarf.................................................................................................. 3 Imaging the COSMOS...................................................................................................................................... 3 The Hubble Constant from a Gravitational Lens.............................................................................................. 4 A New Dwarf Nova in the Period Gap............................................................................................................ -
CARMENES Input Catalogue of M Dwarfs IV. New Rotation Periods from Photometric Time Series
Astronomy & Astrophysics manuscript no. pk30 c ESO 2018 October 9, 2018 CARMENES input catalogue of M dwarfs IV. New rotation periods from photometric time series E. D´ıezAlonso1;2;3, J. A. Caballero4, D. Montes1, F. J. de Cos Juez2, S. Dreizler5, F. Dubois6, S. V. Jeffers5, S. Lalitha5, R. Naves7, A. Reiners5, I. Ribas8;9, S. Vanaverbeke10;6, P. J. Amado11, V. J. S. B´ejar12;13, M. Cort´es-Contreras4, E. Herrero8;9, D. Hidalgo12;13;1, M. K¨urster14, L. Logie6, A. Quirrenbach15, S. Rau6, W. Seifert15, P. Sch¨ofer5, and L. Tal-Or5;16 1 Departamento de Astrof´ısicay Ciencias de la Atm´osfera, Facultad de Ciencias F´ısicas,Universidad Complutense de Madrid, E-280140 Madrid, Spain; e-mail: [email protected] 2 Departamento de Explotaci´ony Prospecci´onde Minas, Escuela de Minas, Energ´ıay Materiales, Universidad de Oviedo, E-33003 Oviedo, Asturias, Spain 3 Observatorio Astron´omicoCarda, Villaviciosa, Asturias, Spain (MPC Z76) 4 Centro de Astrobiolog´ıa(CSIC-INTA), Campus ESAC, Camino Bajo del Castillo s/n, E-28692 Villanueva de la Ca~nada,Madrid, Spain 5 Institut f¨ur Astrophysik, Georg-August-Universit¨at G¨ottingen, Friedrich-Hund-Platz 1, D-37077 G¨ottingen, Germany 6 AstroLAB IRIS, Provinciaal Domein \De Palingbeek", Verbrandemolenstraat 5, B-8902 Zillebeke, Ieper, Belgium 7 Observatorio Astron´omicoNaves, Cabrils, Barcelona, Spain (MPC 213) 8 Institut de Ci`enciesde l'Espai (CSIC-IEEC), Campus UAB, c/ de Can Magrans s/n, E-08193 Bellaterra, Barcelona, Spain 9 Institut d'Estudis Espacials de Catalunya (IEEC), E-08034 Barcelona, Spain 10 -
NASA's Goddard Space Flight Center Laboratory for High Energy
1 NASA’s Goddard Space Flight Center Laboratory for High Energy Astrophysics Greenbelt, Maryland 20771 @S0002-7537~99!00301-7# This report covers the period from July 1, 1997 to June 30, Toshiaki Takeshima, Jane Turner, Ken Watanabe, Laura 1998. Whitlock, and Tahir Yaqoob. This Laboratory’s scientific research is directed toward The following investigators are University of Maryland experimental and theoretical research in the areas of X-ray, Scientists: Drs. Keith Arnaud, Manuel Bautista, Wan Chen, gamma-ray, and cosmic-ray astrophysics. The range of inter- Fred Finkbeiner, Keith Gendreau, Una Hwang, Michael Loe- ests of the scientists includes the Sun and the solar system, wenstein, Greg Madejski, F. Scott Porter, Ian Richardson, stellar objects, binary systems, neutron stars, black holes, the Caleb Scharf, Michael Stark, and Azita Valinia. interstellar medium, normal and active galaxies, galaxy clus- Visiting scientists from other institutions: Drs. Vadim ters, cosmic-ray particles, and the extragalactic background Arefiev ~IKI!, Hilary Cane ~U. Tasmania!, Peter Gonthier radiation. Scientists and engineers in the Laboratory also ~Hope College!, Thomas Hams ~U. Seigen!, Donald Kniffen serve the scientific community, including project support ~Hampden-Sydney College!, Benzion Kozlovsky ~U. Tel such as acting as project scientists and providing technical Aviv!, Richard Kroeger ~NRL!, Hideyo Kunieda ~Nagoya assistance to various space missions. Also at any one time, U.!, Eugene Loh ~U. Utah!, Masaki Mori ~Miyagi U.!, Rob- there are typically between twelve and eighteen graduate stu- ert Nemiroff ~Mich. Tech. U.!, Hagai Netzer ~U. Tel Aviv!, dents involved in Ph.D. research work in this Laboratory. Yasushi Ogasaka ~JSPS!, Lev Titarchuk ~George Mason U.!, Currently these are graduate students from Catholic U., Stan- Alan Tylka ~NRL!, Robert Warwick ~U. -
Naming the Extrasolar Planets
Naming the extrasolar planets W. Lyra Max Planck Institute for Astronomy, K¨onigstuhl 17, 69177, Heidelberg, Germany [email protected] Abstract and OGLE-TR-182 b, which does not help educators convey the message that these planets are quite similar to Jupiter. Extrasolar planets are not named and are referred to only In stark contrast, the sentence“planet Apollo is a gas giant by their assigned scientific designation. The reason given like Jupiter” is heavily - yet invisibly - coated with Coper- by the IAU to not name the planets is that it is consid- nicanism. ered impractical as planets are expected to be common. I One reason given by the IAU for not considering naming advance some reasons as to why this logic is flawed, and sug- the extrasolar planets is that it is a task deemed impractical. gest names for the 403 extrasolar planet candidates known One source is quoted as having said “if planets are found to as of Oct 2009. The names follow a scheme of association occur very frequently in the Universe, a system of individual with the constellation that the host star pertains to, and names for planets might well rapidly be found equally im- therefore are mostly drawn from Roman-Greek mythology. practicable as it is for stars, as planet discoveries progress.” Other mythologies may also be used given that a suitable 1. This leads to a second argument. It is indeed impractical association is established. to name all stars. But some stars are named nonetheless. In fact, all other classes of astronomical bodies are named. -
Stargazer Vice President: James Bielaga (425) 337-4384 Jamesbielaga at Aol.Com P.O
1 - Volume MMVII. No. 1 January 2007 President: Mark Folkerts (425) 486-9733 folkerts at seanet.com The Stargazer Vice President: James Bielaga (425) 337-4384 jamesbielaga at aol.com P.O. Box 12746 Librarian: Mike Locke (425) 259-5995 mlocke at lionmts.com Everett, WA 98206 Treasurer: Carol Gore (360) 856-5135 janeway7C at aol.com Newsletter co-editor: Bill O’Neil (774) 253-0747 wonastrn at seanet.com Web assistance: Cody Gibson (425) 348-1608 sircody01 at comcast.net See EAS website at: (change ‘at’ to @ to send email) http://members.tripod.com/everett_astronomy nearby Diablo Lake. And then at night, discover the night sky like EAS BUSINESS… you've never seen it before. We hope you'll join us for a great weekend. July 13-15, North Cascades Environmental Learning Center North Cascades National Park. More information NEXT EAS MEETING – SATURDAY JANUARY 27TH including pricing, detailed program, and reservation forms available shortly, so please check back at Pacific Science AT 3:00 PM AT THE EVERETT PUBLIC LIBRARY, IN Center's website. THE AUDITORIUM (DOWNSTAIRS) http://www.pacsci.org/travel/astronomy_weekend.html People should also join and send mail to the mail list THIS MONTH'S MEETING PROGRAM: [email protected] to coordinate spur-of-the- Toby Smith, lecturer from the University of Washington moment observing get-togethers, on nights when the sky Astronomy department, will give a talk featuring a clears. We try to hold informal close-in star parties each month visualization presentation he has prepared called during the spring, summer, and fall months on a weekend near “Solar System Cinema”. -
121012-AAS-221 Program-14-ALL, Page 253 @ Preflight
221ST MEETING OF THE AMERICAN ASTRONOMICAL SOCIETY 6-10 January 2013 LONG BEACH, CALIFORNIA Scientific sessions will be held at the: Long Beach Convention Center 300 E. Ocean Blvd. COUNCIL.......................... 2 Long Beach, CA 90802 AAS Paper Sorters EXHIBITORS..................... 4 Aubra Anthony ATTENDEE Alan Boss SERVICES.......................... 9 Blaise Canzian Joanna Corby SCHEDULE.....................12 Rupert Croft Shantanu Desai SATURDAY.....................28 Rick Fienberg Bernhard Fleck SUNDAY..........................30 Erika Grundstrom Nimish P. Hathi MONDAY........................37 Ann Hornschemeier Suzanne H. Jacoby TUESDAY........................98 Bethany Johns Sebastien Lepine WEDNESDAY.............. 158 Katharina Lodders Kevin Marvel THURSDAY.................. 213 Karen Masters Bryan Miller AUTHOR INDEX ........ 245 Nancy Morrison Judit Ries Michael Rutkowski Allyn Smith Joe Tenn Session Numbering Key 100’s Monday 200’s Tuesday 300’s Wednesday 400’s Thursday Sessions are numbered in the Program Book by day and time. Changes after 27 November 2012 are included only in the online program materials. 1 AAS Officers & Councilors Officers Councilors President (2012-2014) (2009-2012) David J. Helfand Quest Univ. Canada Edward F. Guinan Villanova Univ. [email protected] [email protected] PAST President (2012-2013) Patricia Knezek NOAO/WIYN Observatory Debra Elmegreen Vassar College [email protected] [email protected] Robert Mathieu Univ. of Wisconsin Vice President (2009-2015) [email protected] Paula Szkody University of Washington [email protected] (2011-2014) Bruce Balick Univ. of Washington Vice-President (2010-2013) [email protected] Nicholas B. Suntzeff Texas A&M Univ. suntzeff@aas.org Eileen D. Friel Boston Univ. [email protected] Vice President (2011-2014) Edward B. Churchwell Univ. of Wisconsin Angela Speck Univ. of Missouri [email protected] [email protected] Treasurer (2011-2014) (2012-2015) Hervey (Peter) Stockman STScI Nancy S. -
A Blast Wave from the 1843 Eruption of Eta Carinae
1 A Blast Wave from the 1843 Eruption of Eta Carinae Nathan Smith* *Astronomy Department, University of California, 601 Campbell Hall, Berkeley, CA 94720-3411 Very massive stars shed much of their mass in violent precursor eruptions [1] as luminous blue variables (LBVs) [2] before reaching their most likely end as supernovae, but the cause of LBV eruptions is unknown. The 19th century eruption of Eta Carinae, the prototype of these events [3], ejected about 12 solar masses at speeds of 650 km/s, with a kinetic energy of almost 1050ergs[4]. Some faster material with speeds up to 1000-2000 km/s had previously been reported [5,6,7,8] but its full distribution was unknown. Here I report observations of much faster material with speeds up to 3500-6000 km/s, reaching farther from the star than the fastest material in earlier reports [5]. This fast material roughly doubles the kinetic energy of the 19th century event, and suggests that it released a blast wave now propagating ahead of the massive ejecta. Thus, Eta Carinae’s outer shell now mimics a low-energy supernova remnant. The eruption has usually been discussed in terms of an extreme wind driven by the star’s luminosity [2,3,9,10], but fast material reported here suggests that it was powered by a deep-seated explosion rivalling a supernova, perhaps triggered by the pulsational pair instability[11]. This may alter interpretations of similar events seen in other galaxies. Eta Carinae [3] is the most luminous and the best studied among LBVs [1,2]. -
Fundamental Properties of Core-Collapse Supernova and GRB Progenitors: Predicting the Look of Massive Stars Before Death
A&A 558, A131 (2013) Astronomy DOI: 10.1051/0004-6361/201321906 & c ESO 2013 Astrophysics Fundamental properties of core-collapse supernova and GRB progenitors: predicting the look of massive stars before death Jose H. Groh1, Georges Meynet1, Cyril Georgy2, and Sylvia Ekström1 1 Geneva Observatory, Geneva University, Chemin des Maillettes 51, 1290 Sauverny, Switzerland e-mail: [email protected] 2 Astrophysics group, EPSAM, Keele University, Lennard-Jones Labs, ST5 5BG Keele, UK Received 16 May 2013 / Accepted 20 August 2013 ABSTRACT We investigate the fundamental properties of core-collapse supernova (SN) progenitors from single stars at solar metallicity. For this purpose, we combine Geneva stellar evolutionary models with initial masses of Mini = 20−120 M with atmospheric and wind models using the radiative transfer code CMFGEN. We provide synthetic photometry and high-resolution spectra of hot stars at the pre-SN stage. For models with Mini = 9−20 M, we supplement our analysis using publicly available MARCS model atmospheres of RSGs to estimate their synthetic photometry. We employ well-established observational criteria of spectroscopic classification and find that, depending on their initial mass and rotation, massive stars end their lives as red supergiants (RSG), yellow hypergiants (YHG), luminous blue variables (LBV), and Wolf-Rayet (WR) stars of the WN and WO spectral types. For rotating models, we obtained the + following types of SN progenitors: WO1–3 (Mini ≥ 32 M), WN10–11 (25 < Mini < 32 M), LBV (20 ≤ Mini ≤ 25 M), G1 Ia (18 < Mini < 20 M), and RSGs (9 ≤ Mini ≤ 18 M). For non-rotating models, we found spectral types WO1–3 (Mini > 40 M), WN7–8 (25 < Mini ≤ 40 M), WN11h/LBV (20 < Mini ≤ 25 M), and RSGs (9 ≤ Mini ≤ 20 M). -
Meeting Program
A A S MEETING PROGRAM 211TH MEETING OF THE AMERICAN ASTRONOMICAL SOCIETY WITH THE HIGH ENERGY ASTROPHYSICS DIVISION (HEAD) AND THE HISTORICAL ASTRONOMY DIVISION (HAD) 7-11 JANUARY 2008 AUSTIN, TX All scientific session will be held at the: Austin Convention Center COUNCIL .......................... 2 500 East Cesar Chavez St. Austin, TX 78701 EXHIBITS ........................... 4 FURTHER IN GRATITUDE INFORMATION ............... 6 AAS Paper Sorters SCHEDULE ....................... 7 Rachel Akeson, David Bartlett, Elizabeth Barton, SUNDAY ........................17 Joan Centrella, Jun Cui, Susana Deustua, Tapasi Ghosh, Jennifer Grier, Joe Hahn, Hugh Harris, MONDAY .......................21 Chryssa Kouveliotou, John Martin, Kevin Marvel, Kristen Menou, Brian Patten, Robert Quimby, Chris Springob, Joe Tenn, Dirk Terrell, Dave TUESDAY .......................25 Thompson, Liese van Zee, and Amy Winebarger WEDNESDAY ................77 We would like to thank the THURSDAY ................. 143 following sponsors: FRIDAY ......................... 203 Elsevier Northrop Grumman SATURDAY .................. 241 Lockheed Martin The TABASGO Foundation AUTHOR INDEX ........ 242 AAS COUNCIL J. Craig Wheeler Univ. of Texas President (6/2006-6/2008) John P. Huchra Harvard-Smithsonian, President-Elect CfA (6/2007-6/2008) Paul Vanden Bout NRAO Vice-President (6/2005-6/2008) Robert W. O’Connell Univ. of Virginia Vice-President (6/2006-6/2009) Lee W. Hartman Univ. of Michigan Vice-President (6/2007-6/2010) John Graham CIW Secretary (6/2004-6/2010) OFFICERS Hervey (Peter) STScI Treasurer Stockman (6/2005-6/2008) Timothy F. Slater Univ. of Arizona Education Officer (6/2006-6/2009) Mike A’Hearn Univ. of Maryland Pub. Board Chair (6/2005-6/2008) Kevin Marvel AAS Executive Officer (6/2006-Present) Gary J. Ferland Univ. of Kentucky (6/2007-6/2008) Suzanne Hawley Univ. -
The Possible Detection of a Binary Companion to a Type Ibn Supernova Progenitor J
The Astrophysical Journal, 833:128 (6pp), 2016 December 20 doi:10.3847/1538-4357/833/2/128 © 2016. The American Astronomical Society. All rights reserved. THE POSSIBLE DETECTION OF A BINARY COMPANION TO A TYPE IBN SUPERNOVA PROGENITOR J. R. Maund1,7, A. Pastorello2, S. Mattila3,4, K. Itagaki5, and T. Boles6 1 Department of Physics and Astronomy, University of Sheffield, Hicks Building, Hounsfield Road, Sheffield, S3 7RH, UK 2 INAF—Osservatorio Astronomico di Padova. Vicolo Osservatorio 5, I-35122, Padova, Italy 3 Tuorla Observatory, Department of Physics and Astronomy, University of Turku, Väisäläntie 20, FI-21500 Piikkiö, Finland 4 Finnish Centre for Astronomy with ESO (FINCA), University of Turku, Väisäläntie 20, FI-21500 Piikkiö, Finland 5 Itagaki Astronomical Observatory, Teppo-cho, 990-2492 Yamagata, Japan 6 Coddenham Astronomical Observatory, Suffolk IP6 9QY, UK Received 2016 April 28; revised 2016 August 23; accepted 2016 September 20; published 2016 December 13 ABSTRACT We present late-time observations of the site of the Type Ibn supernova (SN) 2006jc, acquired with the Hubble Space Telescope Advanced Camera for Surveys. A faint blue source is recovered at the SN position, with brightness mFW435 =26.76 0.20, mFW555 =26.60 0.23 and mFW625 =26.32 0.19 mag, although there is no detection in a contemporaneous narrow-band Ha image. The spectral energy distribution of the late-time source is well-fit by a stellar-like spectrum (logTeff > 3.7 and log LL > 4), subject to only a small degree of reddening —consistent with that estimated for SN2006jc itself at early-times. The lack of further outbursts after the explosion of SN2006jc suggests that the precursor outburst originated from the progenitor. -
OGLE-2014-SN-131: a Long-Rising Type Ibn Supernova from a Massive Progenitor E
Astronomy & Astrophysics manuscript no. output c ESO 2017 March 8, 2017 OGLE-2014-SN-131: A long-rising Type Ibn supernova from a massive progenitor E. Karamehmetoglu1, F. Taddia1, J. Sollerman1, Ł. Wyrzykowski2, S. Schmidl3, M. Fraser4, C. Fremling1, J. Greiner5; 6, C. Inserra7, Z. Kostrzewa-Rutkowska2; 8; 9, K. Maguire7, S. Smartt7, M. Sullivan10, and D. R. Young7 1 Department of Astronomy, The Oskar Klein Centre, Stockholm University, AlbaNova, 10691 Stockholm, Sweden. e-mail: [email protected] 2 Warsaw University Astronomical Observatory, Al. Ujazdowskie 4, 00-478 Warszawa, Poland. 3 Thüringer Landessternwarte Tautenburg, Sternwarte 5, 07778 Tautenburg, Germany. 4 Institute of Astronomy, University of Cambridge, Madingley Road, Cambridge CB3 0HA, UK. 5 Max-Planck-Institut für Extraterrestrische Physik, Giessenbachstrasse 1, 85748 Garching, Germany. 6 Excellence Cluster Universe, Technische Universität München, Boltzmannstrasse 2, 85748 Garching, Germany. 7 Astrophysics Research Centre, School of Mathematics and Physics, Queens University Belfast, Belfast BT7 1NN, UK. 8 SRON Netherlands Institute for Space Research, Sorbonnelaan 2, 3584 CA Utrecht, the Netherlands. 9 Department of Astrophysics/IMAPP, Radboud University Nijmegen, P.O. Box 9010, 6500 GL Nijmegen, the Netherlands. 10 Department of Physics and Astronomy, University of Southampton, Southampton, SO17 1BJ, UK. Received date / Accepted date ABSTRACT Context. Type Ibn supernovae (SNe Ibn) are thought to be the core-collapse explosions of massive stars whose ejecta interact with He-rich circumstellar material (CSM). Aims. We report the discovery of a SN Ibn, with the longest rise-time ever observed, OGLE-2014-SN-131. We discuss the potential powering mechanisms and the progenitor nature of this peculiar stripped-envelope (SE), circumstellar-interacting SN. -
Download a PDF of the Abstracts Booklet
TALKS SN2016 ABSTRACTS BOOKLET 2 1.- SESSION: Cultural NAME: Cristian Moreno Pakarati AFFILIATION: Ahirenga Research TITTLE: A new proposal for a division of Easter Island's history ABSTRACT: This paper presents an original interpretation of the long-term history of the island, dividing it in three main periods. By this, it pretends to contribute a new vision on a topic long abandoned by the growingly specialized archaeology that focuses more and more on the smallest of details. The scheme is as follows: a first period, as an era of open ocean navigation and relatively frequent contact with other Polynesian people; a second period, as an era of extreme isolation where the Rapanui culture developed many of its unique traits within the Polynesian and World context; and a third period, of contacts with "the West", starting in 1722 with the Dutch expedition of Roggeveen. By this, it pretends to simplify the timeline of events on the island and contextualize better the statue-carving era and the Bird-cult of Easter Island. 2.- SESSION: 01 NAME: Edmundo Edwards AFFILIATION: Pacific Islands Research Institute TITTLE: Archeoastronomy of Eastern Polynesia and Easter Island ABSTRACT: Some 3,500 years ago in a span of about 500 years, the Lapita, the ancestors of the Polynesians, used their knowledge of the stars to settle an area 4,300 km wide in what is considered one of the speediest human expansions of the pre-historic world. Their descendants, the Polynesians, eventually settled hundreds of islands crossing millions of square kilometres of water without navigational instruments, guided by nothing more than complex astronomical observations and an understanding of natural signs.