Interferometric Observations of the Multiple Stellar System Delta Velorum
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'.';King Navigation
1980012912 -' JPL PUBLICATION 78-38 '.';king Navigation W. J. O'Neil, R. P. Rudd, D. L. Farless, C. E. Hildebrand, R. T. Mitchell, K. H. Rourke, et al. Jet Propulsion Laboratory E. A. Euler Martin Marietta Aerospace (N,%SA-C[_-l_,2517) VIklt_G ._AVIGA'IION (Jet t, u0-213_-_ : Pcopulsio[, L,_c.) 322 p _lC Alq/MF A01 _:d[,U CSCL Z2.t; hd0-_|4dj •_ [J_;c ]. a_ GJ/15 l,t7 5 'JJ ± November 15, 1979 _',r:.'> ;Y/l&_',,/I_cC7.'/',_/, : < X* ",t ,'" t National Aeronautics and Space Administration Jet Propulsion Laboratory California Institute of Technology Pasadena, California # 1980012912-002 JPL PUBLICATION 78-38 Viking Navigation W. J. O'Neil, R. P. Rudd, D. L. Farless, C. E. Hildebrand, R. T. Mitchell, K. H. Rourke, et al. Jet Propulsion Laboratory E. A. Euler Martin Marietta Aerospace November 15, 1979 National Aeronautics and Space Administration Jet Propulsion Laboratory : California Institute of Technology Pasadena, California 1980012912-003 The research descnbed bnth_s pubhcat_onwas camed out by the Jet Propulsion Laboratory, Cahforn_aInstitute of Technology, under NASA Contract No NAS7-100 i 1980012912-004 Abstract NASA soft-landed two Viking spacecraft on Mars in the summer t,f 1976. These were the free world's first landings on another planet. This report provides a final, comprehensive description of the navigation of the Viking spacecraft throughout their flight from Earth launch to Mars landing. The flight path design, actual int]lght control, and postflight reconstruction ale discussed in detail. The report Is comprised of an introductory chapter followed by five Olapters which essenually correspond to the organization of the Viking navigation operations, namely, Trajectory Descriptton, Interplanetary Orbit Determination, Satellite Orbit Determination, ._haneuver Analysis, and Lander Flight Path Analysis. -
Assessing Time Scales of Atmospheric Turbulence at Observatory Sites Aglae Kellerer
Assessing time scales of atmospheric turbulence at observatory sites Aglae Kellerer To cite this version: Aglae Kellerer. Assessing time scales of atmospheric turbulence at observatory sites. Astrophysics [astro-ph]. Université Paris-Diderot - Paris VII, 2007. English. tel-00171277 HAL Id: tel-00171277 https://tel.archives-ouvertes.fr/tel-00171277 Submitted on 12 Sep 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. U´ D D P 7 ` pr´esent´ee pour obtenir le grade de Docteur de l’Universit´eParis VII Specialit´ e:´ Astrophysique et Instrumentations Associ´ees A´ K Assessing time scales of atmospheric turbulence at observatory sites Soutenue le 7 Septembre 2007 devant la Commission d’examen : Pr´esident : Pr. G´erard Rousset Directeurs de th`ese : Dr. Vincent Coud´edu Foresto Dr. Monika Petr-Gotzens Rapporteurs : Dr. Tony Travouillon Dr. Jean Vernin Examinateurs : Dr. Thierry Fusco Dr. Marc Sarazin 2 The worst moment for the atheist is when he is really thankful and has nobody to thank. Dante Gabriel Rossetti (1828-1882) For me – as a really thankful atheist – it is a pleasure to have many people to thank, and first of all, my family. -
Evolved Stars
Evolved Stars Planets orbiting the other stellar systems: Giant Stars White Dwarfs??? No. 1, 2010 RETIRED A STARS AND THEIR COMPANIONS. III. 397 Table 1 Planetary-Mass Companions to Evolved Intermediate-Mass Stars with M > 1.5 M ∗ " Star M SpT R MP sin i aeReference ∗ ∗ (M )(R )(MJup)(AU) " " HD 13189 2–6 K2 II 8–20 1.5–2.2 0.27 (0.06) 1, 2 ··· ! Tau 2.7(0.1) K0III 13.7(0.6) 7.6(0.2) 1.93(0.03) 0.151(0.023) 3 NGC 2423 No. 3 2.4 (0.2) 10.6 2.10 0.21 (0.07) 4 ··· ··· 81 Cet 2.4 (2.0–2.5) G5 III: 11 (10–13) 5.3 2.5 0.206 (0.029) 5 HD 104985 2.3 G9 III 11 8.3 0.95 0.090 (0.009) 6, 7 18 Del 2.3 G6 III 8.5 10.3 2.6 0.08 (0.01) 6 HD 17092 2.3 (0.3) K0 III 10.9 (2.8) 4.6 (0.3) 1.29 (0.05) 0.166 (0.052) 8 ξ Aql 2.2 K0 III 12 2.8 0.68 0.0 (fixed) 6 14 And 2.2 (2.0–2.3) K0 III 11 (10–12) 4.8 0.83 0.0 (fixed) 5 HD 81688 2.1 K0III-IV 13 2.7 0.81 0.0 (fixed) 6 HD 173416 2.0 (0.3) G8 III 13.5 (0.9) 2.7 (0.3) 1.16 (0.06) 0.21 (0.04) 9 HD 11977 1.91 (0.21) G5 III 10.09 (0.32) 6.54 1.93 0.40 (0.07) 10, 11 HD 102272 1.9 (0.3) K0 III 10.1 (4.6) 5.9 (0.2) 0.614 (0.001) 0.05 (0.04) 12 ””””2.6(0.4)1.57(0.05)0.68(0.06)12 β Gem 1.86, 1.7 (0.4) K0 III 8.8 (0.1) 2.9 (0.3) 1.69 (0.03) 0.06 (0.04) 13, 14, 15, 16 HD 89744 1.86 (0.18) F7 IV 2.08 (0.06) 7.2 0.88 0.70 (0.02) 17, 18 HD 210702 1.85 (0.13) K1 IV 4.45 (0.07) 1.97 (0.11,0.18) 1.20 (0.02,0.03) 0.036 (<0.106) 19, 20 κ CrB 1.84 (0.13) K0 IV 4.71 (0.08) 2.01 (0.11,0.17) 2.80 (0.07,0.08) 0.044 (<0.123) 21, 20 6Lyn 1.82(0.13) K0IV 5.2(4.9–5.6) 2.21(0.11,0.16) 2.18(0.05,0.06) 0.059(<0.125) 20, 5 HD 167042 1.72 (0.12) K1 IV 4.30 (0.07) 1.70 (0.09,0.12) 1.32 (0.03,0.04) 0.089 (0.028,0.065) 21, 20, 5 HD 192699 1.69 (0.12) G8 IV 3.90 (0.06) 2.40 (0.15,0.21) 1.15 (0.02,0.03) 0.129 (0.029,0.060) 19, 20 HD 175541 1.65 (0.12) G8 IV 3.80 (0.09) 0.70 (0.06,0.08) 1.03 (0.02,0.03) 0.083 (<0.283) 19 HD 5319 1.59 (0.18) G5 IV 3.26 (0.50,0.41) 1.94 1.75 0.12 (0.08) 22 Notes. -
Interferometric Observations of the Multiple Stellar System Δ Velorum (Research Note)
A&A 469, 633–637 (2007) Astronomy DOI: 10.1051/0004-6361:20077079 & c ESO 2007 Astrophysics Interferometric observations of the multiple stellar system δ Velorum (Research Note) A. Kellerer1, M. G. Petr-Gotzens1, P. Kervella2, and V. Coudé du Foresto2 1 European Southern Observatory, Karl-Schwarzschild-Str. 2, 85748 Garching, Germany e-mail: [aglae.kellerer;mpetr]@eso.org 2 LESIA, Paris observatory, France e-mail: [vincent.foresto;pierre.kervella]@obspm.fr Received 10 January 2007 / Accepted 26 March 2007 ABSTRACT Context. The nearby (∼24 pc) triple stellar system δ Velorum contains a close, eclipsing binary (Aa, Ab) discovered in 2000. Multiple systems provide an opportunity to determine the set of fundamental parameters (mass, luminosity, size, chemical composition) of coeval stars. Aims. These parameters can be obtained with particular precision in the case of eclipsing binaries; so we exploited this potential for δ Velorum’s components (Aa, Ab). Methods. We have analysed interferometric observations of the close binary (Aa, Ab), obtained with the VINCI instrument and two VLTI siderostats. The measurements, which resolve the two components for the first time, are fitted onto the simple model of two uniformly bright, spherical stars. Results. The observations suggest that Aa and Ab have larger diameters than expected for stars on the main sequence, hence they must be in a later evolutionary state. Key words. binaries: eclipsing – stars: fundamental parameters – techniques: interferometric – binaries: visual – binaries: spectroscopic 1. Introduction δ Vel C and D were taken to be associated with the pair AB be- cause of seemingly similar proper motion. However, we have not One of the fifty brightest stars on the sky, with a visual mag- = . -
I. VINCI/VLTI Observations of Seven Galactic Cepheids
A&A 416, 941–953 (2004) Astronomy DOI: 10.1051/0004-6361:20031743 & c ESO 2004 Astrophysics Cepheid distances from infrared long-baseline interferometry I. VINCI/VLTI observations of seven Galactic Cepheids P. Kervella1,N.Nardetto2, D. Bersier3, D. Mourard2, and V. Coud´e du Foresto4 1 European Southern Observatory, Alonso de Cordova 3107, Casilla 19001, Vitacura, Santiago 19, Chile 2 D´epartement Fresnel, UMR CNRS 6528, Observatoire de la Cˆote d’Azur, BP 4229, 06304 Nice Cedex 4, France 3 Harvard-Smithsonian Center for Astrophysics, 60 Garden St., Cambridge, MA 02138, USA 4 LESIA, Observatoire de Paris-Meudon, 5 place Jules Janssen, 92195 Meudon Cedex, France Received 19 June 2003 / Accepted 26 November 2003 Abstract. We report the angular diameter measurements of seven classical Cepheids, X Sgr, η Aql, W Sgr, ζ Gem, β Dor, Y Oph and Car that we have obtained with the VINCI instrument, installed at ESO’s VLT Interferometer (VLTI). We also present reprocessed archive data obtained with the FLUOR/IOTA instrument on ζ Gem, in order to improve the phase coverage of our observations. We obtain average limb darkened angular diameter values of θLD[X Sgr] = 1.471 ± 0.033 mas, θLD[η Aql] = 1.839 ± 0.028 mas, θLD[W Sgr] = 1.312 ± 0.029 mas, θLD[β Dor] = 1.891 ± 0.024 mas, θLD[ζ Gem] = 1.747 ± 0.061 mas, θLD[Y Oph] = 1.437±0.040 mas, and θLD[ Car] = 2.988±0.012 mas. For four of these stars, η Aql, W Sgr, β Dor, and Car, we detect the pulsational variation of their angular diameter.