STTR) Program Proposals Selected for Negotiation of STTR Phase I Contracts Sorted by Company and Proposal Number
Total Page:16
File Type:pdf, Size:1020Kb
Load more
Recommended publications
-
Target Selection for the SUNS and DEBRIS Surveys for Debris Discs in the Solar Neighbourhood
Mon. Not. R. Astron. Soc. 000, 1–?? (2009) Printed 18 November 2009 (MN LATEX style file v2.2) Target selection for the SUNS and DEBRIS surveys for debris discs in the solar neighbourhood N. M. Phillips1, J. S. Greaves2, W. R. F. Dent3, B. C. Matthews4 W. S. Holland3, M. C. Wyatt5, B. Sibthorpe3 1Institute for Astronomy (IfA), Royal Observatory Edinburgh, Blackford Hill, Edinburgh, EH9 3HJ 2School of Physics and Astronomy, University of St. Andrews, North Haugh, St. Andrews, Fife, KY16 9SS 3UK Astronomy Technology Centre (UKATC), Royal Observatory Edinburgh, Blackford Hill, Edinburgh, EH9 3HJ 4Herzberg Institute of Astrophysics (HIA), National Research Council of Canada, Victoria, BC, Canada 5Institute of Astronomy (IoA), University of Cambridge, Madingley Road, Cambridge, CB3 0HA Accepted 2009 September 2. Received 2009 July 27; in original form 2009 March 31 ABSTRACT Debris discs – analogous to the Asteroid and Kuiper-Edgeworth belts in the Solar system – have so far mostly been identified and studied in thermal emission shortward of 100 µm. The Herschel space observatory and the SCUBA-2 camera on the James Clerk Maxwell Telescope will allow efficient photometric surveying at 70 to 850 µm, which allow for the detection of cooler discs not yet discovered, and the measurement of disc masses and temperatures when combined with shorter wavelength photometry. The SCUBA-2 Unbiased Nearby Stars (SUNS) survey and the DEBRIS Herschel Open Time Key Project are complimentary legacy surveys observing samples of ∼500 nearby stellar systems. To maximise the legacy value of these surveys, great care has gone into the target selection process. This paper describes the target selection process and presents the target lists of these two surveys. -
New Debris Disks Around Nearby Main-Sequence Stars: Impact on the Direct Detection of Planets C
The Astrophysical Journal, 652:1674Y1693, 2006 December 1 # 2006. The American Astronomical Society. All rights reserved. Printed in U.S.A. NEW DEBRIS DISKS AROUND NEARBY MAIN-SEQUENCE STARS: IMPACT ON THE DIRECT DETECTION OF PLANETS C. A. Beichman,1 G. Bryden,2 K. R. Stapelfeldt,2 T. N. Gautier,2 K. Grogan,2 M. Shao,2 T. Velusamy,2 S. M. Lawler,1 M. Blaylock,3 G. H. Rieke,3 J. I. Lunine,3 D. A. Fischer,4 G. W. Marcy,5 J. S. Greaves,6 M. C. Wyatt,7 W. S. Holland,8 and W. R. F. Dent8 Received 2006 April 17; accepted 2006 July 28 ABSTRACT Using the MIPS instrument on Spitzer, we have searched for infrared excesses around a sample of 82 stars, mostly F, G, and K main-sequence field stars, along with a small number of nearby M stars. These stars were selected for their suitability for future observations by a variety of planet-finding techniques. These observations provide information on the asteroidal and cometary material orbiting these stars, data that can be correlated with any planets that may even- tually be found. We have found significant excess 70 m emission toward 12 stars. Combined with an earlier study, we find an overall 70 m excess detection rate of 13% Æ 3% for mature cool stars. Unlike the trend for planets to be found preferentially toward stars with high metallicity, the incidence of debris disks is uncorrelated with metallicity. By newly identifying four of these stars as having weak 24 mexcesses(fluxes10% above the stellar photosphere), we confirm a trend found in earlier studies wherein a weak 24 m excess is associated with a strong 70 m excess. -
Arxiv:Astro-Ph/0611682V1 21 Nov 2006 )Sho Fpyisadatooy Nvriyo T Andrew St
New Debris Disks Around Nearby Main Sequence Stars: Impact on The Direct Detection of Planets C. A. Beichman1, G. Bryden2, K. R. Stapelfeldt2, T. N. Gautier2, K. Grogan2, M. Shao2, T. Velusamy2, S. M. Lawler1, M. Blaylock3, G. H. Rieke3, J. I. Lunine3, D. A. Fischer4, G. W. Marcy5, J. S. Greaves6, M. C. Wyatt7, W. S. Holland8, & W. R. F. Dent8 1) Michelson Science Center, California Institute of Technology, Pasadena, CA 91125 2) Jet Propulsion Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 3) Steward Observatory, University of Arizona, 933 North Cherry Ave, Tucson, AZ 85721 4) Department of Physics and Astronomy, San Francisco State University, San Francisco, CA 94132 5) Department of Astronomy, University of California, Berkeley, CA 94720 6) School of Physics and Astronomy, University of St. Andrews, North Haugh, St. Andrews KY16 9SS, UK 7) Institute of Astronomy, University of Cambridge, Cambridge, CB3 0HA, UK 8) UK Astronomy Technology Centre, Royal Observatory, Edinburgh EH9 3HJ, UK ABSTRACT Using the MIPS instrument on the Spitzer telescope, we have searched for infrared excesses around a sample of 82 stars, mostly F, G, and K main-sequence arXiv:astro-ph/0611682v1 21 Nov 2006 field stars, along with a small number of nearby M stars. These stars were selected for their suitability for future observations by a variety of planet-finding tech- niques. These observations provide information on the asteroidal and cometary material orbiting these stars - data that can be correlated with any planets that may eventually be found. We have found significant excess 70 µm emission to- ward 12 stars. -
Collocato In
Collocato in: http://digilander.libero.it/occultazioni/ I/149A Fifth Fundamental Catalogue (FK5) Part I (Fricke+, 1988) ================================================================================ Fifth Fundamental Catalogue (FK5) Part I Fricke W., Schwan H., Lederle T. (in collaboration with Bastian U., Bien R., Burkhardt G., du Mont B., Hering R., Jaehrling R., Jahreiss H., Roeser S., Schwerdtfeger H.M., Walter H.G.) <Veroeff. Astron. Rechen-Institut Heidelb. No. 32 (1988)> =1988VeARI..32....1F ================================================================================ ADC_Keywords: Proper motions ; Positional data Abstract: The Basic Fifth Fundamental Catalogue (FK5) Part I provides improved mean positions and proper motions for the 1535 classical fundamental stars that had been included in the FK3 and FK4 catalogs. The machine version of the catalog contains the positions and proper motions of the Basic FK5 stars for the epochs and equinoxes J2000.0 and B1950.0, the mean epochs of individual observed right ascensions and declinations used to determine the final positions, the mean errors of the final positions and proper motions for the reported epochs, and ancillary data such as magnitudes, spectral types, parallaxes, radial velocities, and cross identifications to other catalog designations. Introduction: The Basic FK5 is the successor to the FK4 (Fricke & Kopff 1963) and contains the 1535 classical fundamental stars used to define the latter system. It represents a revision of the FK4 and results from the determination of systematic and individual corrections to the mean positions and proper motions of the FK4, the elimination of the error in the FK4 equinox, and the introduction of the IAU (1976) system of astronomical constants. About 300 catalogs providing star positions obtained from throughout the world are included in the FK5. -
The ROSAT All-Sky Survey Catalogue of Optically Bright Main-Sequence Stars and Subgiant Stars?
ASTRONOMY & ASTROPHYSICS OCTOBER II 1998, PAGE 155 SUPPLEMENT SERIES Astron. Astrophys. Suppl. Ser. 132, 155–171 (1998) The ROSAT all-sky survey catalogue of optically bright main-sequence stars and subgiant stars? M. H¨unsch1,3, J.H.M.M. Schmitt2,3, and W. Voges3 1 Institut f¨ur Theoretische Physik und Astrophysik, Universit¨at Kiel, Olshausenstrasse 40, 24118 Kiel, Germany 2 Hamburger Sternwarte, Universit¨at Hamburg, Gojenbergsweg 112, 21029 Hamburg, Germany 3 Max-Planck-Institut f¨ur Extraterrestrische Physik, Giessenbachstrasse, 85740 Garching, Germany Received February 18; accepted April 14, 1998 Abstract. We present X-ray data for all main-sequence In principle, any late-type star should be able to sus- and subgiant stars of spectral types A, F, G, and K and tain a corona, and henceforth, be an X-ray source. Indeed, luminosity classes IV and V listed in the Bright Star already the Einstein Observatory detected X-ray emission Catalogue that have been detected as X-ray sources in from a large number of late-type stars (cf. Vaiana et al. the ROSAT all-sky survey; several stars without luminos- 1981; Maggio et al. 1987). Detailed studies of the im- ity class are also included. The catalogue contains 980 mediate solar environment (Schmitt et al. 1995; Schmitt entries yielding an average detection rate of 32 percent. 1997) revealed that virtually every late-type dwarf star In addition to count rates, source detection parameters, with spectral type later than A7 can be detected as an hardness ratios, and X-ray fluxes we also list X-ray lumi- X-ray source given data of sufficient sensitivity; Schmitt nosities derived from Hipparcos parallaxes. -
Updating Multiplicity of Solar-Type Stars Within 22 Parsecs
Georgia State University ScholarWorks @ Georgia State University Physics and Astronomy Dissertations Department of Physics and Astronomy 11-18-2008 The Separated Fringe Packet Survey: Updating Multiplicity of Solar-Type Stars within 22 Parsecs Christopher Donald Farrington Follow this and additional works at: https://scholarworks.gsu.edu/phy_astr_diss Part of the Astrophysics and Astronomy Commons, and the Physics Commons Recommended Citation Farrington, Christopher Donald, "The Separated Fringe Packet Survey: Updating Multiplicity of Solar-Type Stars within 22 Parsecs." Dissertation, Georgia State University, 2008. https://scholarworks.gsu.edu/phy_astr_diss/26 This Dissertation is brought to you for free and open access by the Department of Physics and Astronomy at ScholarWorks @ Georgia State University. It has been accepted for inclusion in Physics and Astronomy Dissertations by an authorized administrator of ScholarWorks @ Georgia State University. For more information, please contact [email protected]. The Separated Fringe Packet Survey: Updating Multiplicity of Solar-Type Stars within 22 Parsecs by CHRISTOPHER FARRINGTON Under the Direction of Harold A. McAlister Abstract Over the past half century, multiplicity studies have provided a foundation for the theories of stellar formation and evolution through understanding how likely it is that stars form alone or with companions. If spectroscopic orbits are combined with techniques that can determine visual orbits, we can access the most fundamental parameter of stellar evolution, stellar mass. This dissertation is composed of two main sections. The ¯rst involves the investigation of the seminal multiplicity study of Duquennoy et al. (1991) which has been the \gold standard" for solar-type stars for nearly 20 years. Improvements in technology in the intervening years have improved the measurement accuracy for radial velocities and distances on which the study was based. -
Arxiv:0909.0058V1
Explorations Beyond the Snow Line: Spitzer/IRS Spectra of Debris Disks Around Solar-Type Stars S. M. Lawler1,2,3, C. A. Beichman2, G. Bryden4, D. R. Ciardi2, A. M. Tanner4, K. Y. L. Su5, K. R. Stapelfeldt4, C. M. Lisse6, D. E. Harker7 1) Astronomy Department, Wesleyan University, Middletown, CT 06459 2) NASA Exoplanet Science Institute, California Institute of Technology, Pasadena, CA 91125 3) present address: University of British Columbia, Department of Physics and Astronomy, 6244 Agricultural Road, Vancouver, BC V6T 1Z1 Canada 4) Jet Propulsion Laboratory, 4800 Oak Grove Drive, Pasadena, CA 91109 5) Steward Observatory, University of Arizona, 933 North Cherry Avenue, Tucson, AZ 85721 6) Johns Hopkins University - Applied Physics Laboratory, SD/SRE, MP3-W155, 7707 Montpelier Road, Laurel, MD 20723 7) Center for Astrophysics and Space Sciences, University of California, San Diego, 9500 Gilman Drive, La Jolla, CA 92093-0424 ABSTRACT We have observed 152 nearby solar-type stars with the Infrared Spectrometer (IRS) on the Spitzer Space Telescope. Including stars that met our criteria but were observed in other surveys, we get an overall success rate for finding excesses arXiv:0909.0058v1 [astro-ph.SR] 1 Sep 2009 in the long wavelength IRS band (30–34 µm) of 11.8% ± 2.4%. The success rate for excesses in the short wavelength band (8.5–12 µm) is ∼1% including sources from other surveys. For stars with no excess at 8.5–12 µm, the IRS data set 3σ limits of around 1,000 times the level of zodiacal emission present in our solar system, while at 30–34 µm set limits of around 100 times the level of our solar system. -
Carolina Chavero
Ministerio´ de Cienciaˆ e Tecnologia Observatorio´ Nacional EVOLUC¸ AO˜ DE DISCOS CIRCUNSTELARES EM ESTRELAS DE BAIXA MASSA Carolina Chavero Tese realizada sob a orientac¸ao˜ do Prof. Dr. Ra- miro de la Reza e apresentada a` Divisao˜ de Pro- gramas de Pos-graduac¸´ ao˜ do Observatorio´ Nacional como requisito para a obtenc¸ao˜ do t´ıtulo de Doutor em Astronomia. Rio de Janeiro, Abril de 2009 Livros Grátis http://www.livrosgratis.com.br Milhares de livros grátis para download. ... Este trabalho ´ededicado especialmente para minha familia, que ´eminha base e meu maior orgulho, e tamb´em para todos aqueles que compartilham comigo o entusiasmo pela Astronomia. Conteudo´ Agradecimentos v Resumo ix Abstract xi Lista de Tabelas xiii Lista de Figuras xix 1 Motivac¸ao˜ 1 1.1 Contextohist´orico............................ 1 2 Discosdotipo debris 5 2.1 Descobertas............................... 5 2.2 M´etododedetecc¸˜ao. 6 2.2.1 Excessosinfravermelhos . 6 2.2.2 Imagensdiretas ........................ 8 2.2.3 Algumasimagens. .. .. .. .. .. .. 12 2.3 Buscas.................................. 15 2.4 Luminosidade: Fator fd ......................... 16 2.4.1 Evoluc¸˜ao temporal dos discos debris ............. 17 2.5 Tempodevidadodiscovs.massaestelar . 20 3 Estrelas com planetas extra-solares 23 3.1 Contextohist´orico. .. .. .. .. .. .. .. 23 3.2 T´ecnicasdedetecc¸˜ao . 25 3.2.1 T´ecnica espectrosc´opica: Velocidade radial (VR) ou Doppler 26 3.2.2 T´ecnica fotom´etrica: Trˆansito planet´ario . ....... 28 3.3 Propriedades dos planetas extra-solares e de suas estrelashospedeiras 29 3.3.1 Distribuic¸˜aodemassase´orbitas . 30 i ii 3.3.2 Metalicidade .......................... 32 3.4 Migrac¸˜aoplanet´aria. 35 4 Evoluc¸ao˜ de discos debris emvoltadeestrelasdebaixamassa 39 4.1 Introduc¸˜aoemotivac¸˜ao . -
Spitzer Approved Warm Mission Abstracts
Printed by SSC Jan 29, 20 19:21 Spitzer Approved Warm Mission Abstracts Page 1/750 Jan 29, 20 19:21 Spitzer Approved Warm Mission Abstracts Page 2/750 Spitzer Space Telescope − Directors Discretionary Time Proposal #13159 Spitzer Space Telescope − General Observer Proposal #60167 Variability at the edge: highly accreting objects in Taurus Disk tomography and dynamics: a time−dependent study of known mid−infrared Principal Investigator: Peter Abraham variable young stellar objects Institution: Konkoly Observatory Principal Investigator: Peter Abraham Technical Contact: Peter Abraham, Konkoly Observatory Institution: Konkoly Observatory of the Hungarian Academy of Science Co−Investigators: Technical Contact: Peter Abraham, Konkoly Observatory of the Hungarian Agnes Kospal, Konkoly Observatory Academy of Science Robert Szabo, Konkoly Observatory Co−Investigators: Science Category: YSOs Jose Acosta−Pulido, Instituto de Astrofisica de Canarias Observing Modes: IRAC Post−Cryo Mapping Cornelis P. Dullemond, Max−Planck−Institut fur Astronomie Hours Approved: 9.3 Carol A. Grady, Eureka Sci/NASA Goddard Thomas Henning, Max−Planck−Institut fur Astronomie Abstract: Attila Juhasz, Max−Planck−Institut fur Astronomie In Kepler K2, Campaign 13, we will obtain 80−days−long optical light curves of Csaba Kiss, Konkoly Observatory seven highly accreting T Tauri stars in the benchmark Taurus star forming Agnes Kospal, Leiden Observatory region. Here we propose to monitor our sample simultaneously with Kepler and Maria Kun, Konkoly Observatory Spitzer, to -
New Measurements of Rotation and Differential Rotation in AF Stars
A&A 542, A116 (2012) Astronomy DOI: 10.1051/0004-6361/201118724 & c ESO 2012 Astrophysics New measurements of rotation and differential rotation in A-F stars: are there two populations of differentially rotating stars? ,, M. Ammler-von Eiff1,2,3 and A. Reiners2 1 Thüringer Landessternwarte Tautenburg, Sternwarte 5, 07778 Tautenburg, Germany e-mail: [email protected] 2 Institut für Astrophysik, Georg-August-Universität Göttingen, Friedrich-Hund-Platz 1, 37077 Göttingen, Germany e-mail: [email protected] 3 Max Planck Institute for Solar System Research, Max-Planck-Straße 2, 37191 Katlenburg-Lindau, Germany Received 22 December 2011 / Accepted 25 March 2012 ABSTRACT Context. The Sun displays differential rotation that is intimately connected to the solar dynamo and hence related to solar activity, the solar cycle, and the solar wind. Considering the detectability and habitability of planets around other stars it is important to understand theroleofdifferential rotation in other stars. Aims. We present projected rotational velocities and new measurements of the rotational profile of some 180 nearby stars with spectral types A-F. The results are consolidated by a homogeneous compilation of basic stellar data from photometry and the identification of multiple stellar systems. New and previous measurements of rotation by line profile analysis are compiled and made available. Methods. The overall broadening profile is derived analysing spectral line shape from hundreds of spectral lines by the method of least-squares deconvolution, reducing spectral noise to a minimum. The effect of differential rotation on the broadening profile is best measured in inverse wavelength space by the first two zeros of its Fourier transform. -
Antennas and Propagation Society: Linda P.B
NATIONAL ACADEMIES OF SCIENCES AND ENGINEERING NATIONAL RESEARCH COUNCIL of the UNITED STATES OF AMERICA UNITED STATES NATIONAL COMMITTEE International Union of Radio Science National Radio Science Meeting 5 - 8 January 2004 Sponsored by USNC/URSI University of Colorado at Boulder Boulder, Colorado USA I ( ·r____________ _ '--------------------------~ United States National Committee International Union of Radio Science ABSTRACTS National Radio Science Meeting 5-8 January 2004 University of Colorado at Boulder Sponsored by USNC/URSI Table of Contents Session Page No. Session Page No. Membership Information ...... iii Gl ...................... 185 Description of URSI ......... iv 02 ...................... 197 Plenary Session ............. vii 03 ...................... 207 Al ........................ 1 04 ...................... 219 A2 ........................ 7 GS ...................... 229 Bl ....................... 13 G/Hl .................... 237 B2 ....................... 25 G/H2 .................... 249 B3 ....................... 35 Hl ...................... 259 B4 ....................... 47 H2 ...................... 271 BS ....................... 53 H3 ...................... 279 B6 ....................... 61 H4 ...................... 293 Cl ....................... 73 HS ...................... 305 C2 ....................... 81 H6 ...................... 319 Dl ....................... 93 Jl ....................... 329 D2 ...................... 103 J2 ....................... 341 D/Bl .................... 109 J3 ...................... -