DOCSLIB.ORG

Perspectives of the Radial Velocity Method: Physical Modeling of the Wavelength Solution & Exoplanetary Detections Around Giant Stars

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text
Perspectives of the Radial Velocity Method: Physical Modeling of the Wavelength Solution & Exoplanetary Detections Around Giant Stars RUPRECHT-KARLS-UNIVERSITÄT HEIDELBERG DOCTORAL THESIS Perspectives of the Radial Velocity Method: Physical Modeling of the Wavelength Solution & Exoplanetary Detections around Giant Stars Author: Supervisor: Marcelo Said TALA PINTO Prof. Dr. Andreas QUIRRENBACH Second Referee: Prof. Dr. Thomas HENNING Thesis submitted in fulfillment of the requirements for the degree of Doctor of Natural Sciences in the Extrasolar Planet Research Group Landessternwarte Königstuhl June 4, 2019 ii iii Dissertation in Astronomy submitted to the Combined Faculties of the Natural Sciences and Mathematics of the Ruperto-Carola-University of Heidelberg, Germany for the degree of Doctor of Natural Sciences M.Sc. Marcelo Said Tala Pinto Born in Antofagasta, Chile Oral Examination: 16.07.2019 iv v Perspectives of the Radial Velocity Method: Physical Modeling of the Wavelength Solution & Exoplanetary Detections around Giant Stars Referees: Prof. Dr. Andreas Quirrenbach Prof. Dr. Thomas Henning vi vii “Even if all life on our planet is destroyed, there must be other life somewhere which we know nothing of. It is impossible that ours is the only world; there must be world after world unseen by us, in some region or dimension that we simply do not perceive. Even though I can’t prove that, even though it isn’t logical - I believe it, he said to himself ” The Man in the High Castle - Philip K. Dick, 1962 viii ix Abstract First, I present the design and construction of the Front-end of the Waltz Spectro- graph. I designed upgrades in the system to optimize its mechanical stability and light coupling efficiency. To improve the instrument performance, I changed the original spectrograph fiber for one with slightly larger core and better focal ratio degradation, providing a spectral resolving power of 60.000, a mean spectral sam- pling of 2.6 pixels and only 5 % losses due to focal ratio degradation. In the second part I present a ray tracing software that calculates the optical path of individual rays through an echelle spectrograph from the slit to the detector. By including the effects of the environment on the physical properties of the optical elements that compose the spectrograph, I am able to reproduce some of the trends observed in the time series of the spectral line positions of the calibration data. Finally, I report the discovery of two planets orbiting the stars HD 25723 and 17 Sco and two planet candidates orbiting 3 Cnc and 44 Uma. Also, I investigate the planet occurrence rates as a function of evolutionary stage for two surveys, Lick and EXPRESS, concluding that there is no strong effect of stellar evolution in planet occurrence rates. Zusammenfassung Als erstes präsentiere ich das Design und die Konstruktion des Waltz Spektro- grafen Frontends. Ich entwarf Verbesserungen im System seine mechanische Sta- bilität und Lichtkopplungseffizienz zu optimieren. Mit dem Ziel die Leistung des Instruments zu erhöhen, habe ich die ursprüngliche Glasfaser des Spektrografen gegen eine mit einer geringeren Degradierung des Fokusverhältnisses und einem etwas größeren Kern ausgetauscht. Das neue Design erreicht eine spektrale Au- flösung von 60.000, eine spektrale Abtastrate von durchschnittlich 2.6 Pixeln sowie lediglich 5% Verlust durch die Degradierung des Fokusverhältnisses. Im zweiten Teil präsentiere ich eine Lichtstrahlverfolgungssoftware, welche den Weg einzelner Lichtstrahlen durch einen Gitterspektrografen vom Spalt bis zum Detektor berechnet. Indem ich die Umwelteinflüsse auf die physikalischen Eigen- schaften der optischen Elemente des Spektrografen miteinbeziehe, kann ein ein paar der Verläufe reproduzieren, welche in Zeitreihen der Spektrallinienpositionen der CARMENES Kalibrationsdaten vorhanden sind. Zuletzt gebe ich die Entdeckung zweier Planeten um die Sterne HD 25723 und 17 Sco sowie zweier Planetenkandidaten um 3 Cnc und 44 UMa bekannt. Zusät- zlich untersuche ich die Planetenhäufigkeit in Abhängigkeit des evolutionären Sta- tus zweier Beobachtungsprogramme: Lick und EXPRESS. Mittels der abgeleiteten Planetenhäufigkeit kann ich schlussfolgern, dass die Evolutionsphase des Sterns keinen starken Einfluss auf die Planetenhäufigkeit hat. xiii Acknowledgements Long time ago, when my mother took me to the Paranal Observatory, close to my home city Antofagasta, I never thought that I was going to end up doing my PhD in the observatory that built the first optical instrument for the VLT1. Learning Astron- omy at the Landessternwarte Königstuhl is one of the greatest treasures of my life, and I will always be thankful to my supervisors, Prof. Dr. Andreas Quirrenbach and Priv.-Doz. Sabine Reffert, for giving the opportunity to pursue my doctoral studies in such a rich scientific environment. Just in the LSW it would have been possible to become the best astronomer I can be, and this is mostly because of your support and the freedom you gave me to explore the nature of my scientific work. I would like to thank to all the people who contributed with their work to the completion of this thesis: Anantha Chanumolu who guided me through the con- struction of the RAMSES code by giving me parts of her code and providing feed- back during the course of this investigation, Lutz Geuer and Ludwig Schäffner for their excellent work at the LSW Workshop building the parts for the Waltz and for the excellent feedback provided when I had to improve my mechanical designs, Wal- ter Seifert and Conchi Cárdenas for providing the optical designs of the CARMENES VIS and NIR spectrographs as built, Otmar Stahl for the discussions about the envi- ronment control system of CARMENES and for solving all most my IT issues dur- ing the last four years, Julian Stürmer and Christian Schwab for the discussions that helped improving the original design of the Waltz Spectrograph, and Matthias Zech- meister and Florian Bauer for providing the data I used to analyze the behaviour of CARMENES and for all the fruitful discussions that helped me understand what really a wavelength solution is. The progress in science has never been a task of one, as the cornerstone of a succesful learning process is the exchange of knowledge and ideas with our friends and colleagues. As far as I am from home now, curiously, home never really felt far away and this is thanks to the Exoplanets and Astrophotonics Research Groups at the LSW: Theodorus Anagnos, Paz Bluhm, Stefan Brems, Robert Harris, Paul Heeren, Philip Hottinger, Adrian Kaminski, Jonas Kemmer, Sepideh Sadegi, Dane Späth, Stephan Stock, Thomas Stuber, Trifon Trifonov, Vera Wolthoff and Steffi Yen. A special tribute deserves Steffi and Rob, as we started our respective science trips in Heidelberg more or less at the same time and have played an important role in my doctoral studies, but also in the quality of the english of this thesis. Without their friendship the days in Heidelberg would have not been so colorful. A special tribute goes to Vera and Stefan for their contribution in the german translation of the abstract. It is the time to put the final points to this thesis. Before doing so I must em- phasize that most of what I am as a scientist and human being was learned from 1Appenzeller et al. 1998, "Successful commissioning of FORS1 - the first optical instrument on the VLT." xiv my family, my mother Ana María Pinto Castillo and my brothers, Maximiliano Tala Pinto and Marco Tala Pinto. Even though none of them is a scientist, they planted in me the seed of curiosity, but more important, the seed of honesty and kindness. And those are, in my opinion, the three qualities that a good scientist must have. To be curious, to be honest, and to be kind. To you, who are reading these words now. Thank you. xv Contents Abstract ix Zusammenfassung xi Acknowledgements xiii 1 Introduction1 1.1 Exoplanets...................................1 1.2 The Radial Velocity Method.........................3 1.2.1 High Resolution Spectroscopy for Precise Radial Velocities...5 1.2.2 The Iodine Cell Technique......................9 1.2.3 The Simultaneous Calibration Technique............. 11 1.3 The Lick Survey of Giant Planets around Giant Stars........... 13 1.4 CARMENES: a search for Super-Earths around M-dwarfs........ 14 1.5 Objectives and Outline............................ 17 2 Front-end opto-mechanical design of the Waltz Telescope 19 2.1 Introduction.................................. 19 2.2 Instrument description............................ 20 2.2.1 Spectrograph optical design..................... 20 2.2.2 Calibration Unit............................ 22 2.3 FN-system and Spectrograph Fiber upgrade............... 23 2.3.1 FN-system............................... 24 2.3.2 Focal Ratio Degradation....................... 26 Experimental setup.......................... 26 Measurement procedure....................... 26 Results................................. 28 2.3.3 Final spectrograph optical design.................. 28 2.4 Waltz Front-end................................ 29 2.4.1 Preliminary design.......................... 30 Early results.............................. 32 2.4.2 Waltz Telescope F/#......................... 34 Experimental procedure and results................ 34 2.4.3 Final Waltz Front-end Opto-mechanical Design......... 36 Calibration Fiber........................... 36 Fiber Aperture on-sky and Mirror Pinhole............ 36 xvi Fiber Feeding Unit.......................... 38 Final Design.............................. 40 2.4.4 Front-end control........................... 42 2.5 Summary.................................... 43 3 RAMSES and the CARMENES wavelength
Load more

Recommended publications
  • Mathématiques Et Espace
    Atelier disciplinaire AD 5 Mathématiques et Espace Anne-Cécile DHERS, Education Nationale (mathématiques) Peggy THILLET, Education Nationale (mathématiques) Yann BARSAMIAN, Education Nationale (mathématiques) Olivier BONNETON, Sciences - U (mathématiques) Cahier d'activités Activité 1 : L'HORIZON TERRESTRE ET SPATIAL Activité 2 : DENOMBREMENT D'ETOILES DANS LE CIEL ET L'UNIVERS Activité 3 : D'HIPPARCOS A BENFORD Activité 4 : OBSERVATION STATISTIQUE DES CRATERES LUNAIRES Activité 5 : DIAMETRE DES CRATERES D'IMPACT Activité 6 : LOI DE TITIUS-BODE Activité 7 : MODELISER UNE CONSTELLATION EN 3D Crédits photo : NASA / CNES L'HORIZON TERRESTRE ET SPATIAL (3 ème / 2 nde ) __________________________________________________ OBJECTIF : Détermination de la ligne d'horizon à une altitude donnée. COMPETENCES : ● Utilisation du théorème de Pythagore ● Utilisation de Google Earth pour évaluer des distances à vol d'oiseau ● Recherche personnelle de données REALISATION : Il s'agit ici de mettre en application le théorème de Pythagore mais avec une vision terrestre dans un premier temps suite à un questionnement de l'élève puis dans un second temps de réutiliser la même démarche dans le cadre spatial de la visibilité d'un satellite. Fiche élève ____________________________________________________________________________ 1. Victor Hugo a écrit dans Les Châtiments : "Les horizons aux horizons succèdent […] : on avance toujours, on n’arrive jamais ". Face à la mer, vous voyez l'horizon à perte de vue. Mais "est-ce loin, l'horizon ?". D'après toi, jusqu'à quelle distance peux-tu voir si le temps est clair ? Réponse 1 : " Sans instrument, je peux voir jusqu'à .................. km " Réponse 2 : " Avec une paire de jumelles, je peux voir jusqu'à ............... km " 2. Nous allons maintenant calculer à l'aide du théorème de Pythagore la ligne d'horizon pour une hauteur H donnée.
    [Show full text]
  • Three-Year Follow up of the Phase 3 Pollux Study of Daratumumab Plus
    This is a repository copy of Three-Year Follow up of the Phase 3 Pollux Study of Daratumumab Plus Lenalidomide and Dexamethasone (D-Rd) Versus Lenalidomide and Dexamethasone (Rd) Alone in Relapsed or Refractory Multiple Myeloma (RRMM). White Rose Research Online URL for this paper: http://eprints.whiterose.ac.uk/157106/ Version: Accepted Version Proceedings Paper: Bahlis, N, Dimopoulos, MA, White, DJ et al. (14 more authors) (2018) Three-Year Follow up of the Phase 3 Pollux Study of Daratumumab Plus Lenalidomide and Dexamethasone (D-Rd) Versus Lenalidomide and Dexamethasone (Rd) Alone in Relapsed or Refractory Multiple Myeloma (RRMM). In: Blood. ASH 2018 – 60th American Society of Hematology Annual Meeting and Exposition, 01-04 Dec 2018, San Diego, CA. American Society of Hematology . https://doi.org/10.1182/blood-2018-99-112697 © 2018 by The American Society of Hematology. This is an author produced version of a conference abstract published in Blood. Uploaded in accordance with the publisher's self-archiving policy. Reuse Items deposited in White Rose Research Online are protected by copyright, with all rights reserved unless indicated otherwise. They may be downloaded and/or printed for private study, or other acts as permitted by national copyright laws. The publisher or other rights holders may allow further reproduction and re-use of the full text version. This is indicated by the licence information on the White Rose Research Online record for the item. Takedown If you consider content in White Rose Research Online to be in breach of UK law, please notify us by emailing [email protected] including the URL of the record and the reason for the withdrawal request.
    [Show full text]
  • 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.
    [Show full text]
  • Winter Observing Notes
    Wynyard Planetarium & Observatory Winter Observing Notes Wynyard Planetarium & Observatory PUBLIC OBSERVING – Winter Tour of the Sky with the Naked Eye NGC 457 CASSIOPEIA eta Cas Look for Notice how the constellations 5 the ‘W’ swing around Polaris during shape the night Is Dubhe yellowish compared 2 Polaris to Merak? Dubhe 3 Merak URSA MINOR Kochab 1 Is Kochab orange Pherkad compared to Polaris? THE PLOUGH 4 Mizar Alcor Figure 1: Sketch of the northern sky in winter. North 1. On leaving the planetarium, turn around and look northwards over the roof of the building. To your right is a group of stars like the outline of a saucepan standing up on it’s handle. This is the Plough (also called the Big Dipper) and is part of the constellation Ursa Major, the Great Bear. The top two stars are called the Pointers. Check with binoculars. Not all stars are white. The colour shows that Dubhe is cooler than Merak in the same way that red-hot is cooler than white-hot. 2. Use the Pointers to guide you to the left, to the next bright star. This is Polaris, the Pole (or North) Star. Note that it is not the brightest star in the sky, a common misconception. Below and to the right are two prominent but fainter stars. These are Kochab and Pherkad, the Guardians of the Pole. Look carefully and you will notice that Kochab is slightly orange when compared to Polaris. Check with binoculars. © Rob Peeling, CaDAS, 2007 version 2.0 Wynyard Planetarium & Observatory PUBLIC OBSERVING – Winter Polaris, Kochab and Pherkad mark the constellation Ursa Minor, the Little Bear.
    [Show full text]
  • Cvetoje- Vic, Anthony Cheetham, Frantz Martinache, Barnaby Norris, Peter Tuthill
    Dr Benjamin Pope Lecturer in Astrophysics and DECRA Fellow Advisor: Prof. David Hogg Affiliation: School of Mathematics & Physics University of Queensland, St Lucia, QLD 4072, Australia and Centre for Astrophysics University of Southern Queensland, West Street, Toowoomba, QLD 4350, Australia Homepage: benjaminpope.github.io email: [email protected] orcid: 0000-0003-2595-9114 Education and Previous Positions 2017-2020 NASA Sagan Fellow, New York University Advisor: Prof. David Hogg 2017 Postdoctoral Research Associate, University of Sydney Advisor: Prof. Peter Tuthill 2013-2017 Doctor of Philosophy in Astrophysics, University of Oxford Thesis: “Observing Bright Stars and their Planets from the Earth and from Space” Balliol College | Supervisors: Prof. Suzanne Aigrain, Prof. Patrick Roche 2013-14 Master of Science in Astrophysics, University of Sydney Thesis: “Vision and Revision: Wavefront Sensing from the Image Domain” Supervisor: Prof. Peter Tuthill 2012 Bachelor of Science (Advanced) with Honours in Physics, University of Sydney First Class Honours, with the University Medal Thesis: “Dancing in the Dark: Kernel Phase Interferometry of Ultracool Dwarfs” Supervisors: Prof. Peter Tuthill, Dr. Frantz Martinache 2010-2011 Study Abroad at the University of California, Berkeley Research project with Prof. Charles H. Townes, Infrared Spatial Interferometer. Grants ARC Discovery Early Career Research Award (DECRA) AUD $444,075.00 NASA TESS Cycle 3 Guest Investigator USD $50,000 TESS Cycle 2 Guest Investigator USD $50,000 Balliol Balliol Interdisciplinary Institute Research Grant College GBP £3,000 Teaching 2021 Extragalactic Astrophysics & Cosmology, University of Queensland 2019 Master of Data Science Guest Lecturer, NYU Center for Data Science 2017 Bayesian Reasoning Honours Lecturer, University of Sydney 2017 Honours Project Supervisor, University of Sydney Supervised Alison Wong and Matthew Edwards, both to First Class Honours and PhD acceptance.
    [Show full text]
  • A Basic Requirement for Studying the Heavens Is Determining Where In
    Abasic requirement for studying the heavens is determining where in the sky things are. To specify sky positions, astronomers have developed several coordinate systems. Each uses a coordinate grid projected on to the celestial sphere, in analogy to the geographic coordinate system used on the surface of the Earth. The coordinate systems differ only in their choice of the fundamental plane, which divides the sky into two equal hemispheres along a great circle (the fundamental plane of the geographic system is the Earth's equator) . Each coordinate system is named for its choice of fundamental plane. The equatorial coordinate system is probably the most widely used celestial coordinate system. It is also the one most closely related to the geographic coordinate system, because they use the same fun­ damental plane and the same poles. The projection of the Earth's equator onto the celestial sphere is called the celestial equator. Similarly, projecting the geographic poles on to the celest ial sphere defines the north and south celestial poles. However, there is an important difference between the equatorial and geographic coordinate systems: the geographic system is fixed to the Earth; it rotates as the Earth does . The equatorial system is fixed to the stars, so it appears to rotate across the sky with the stars, but of course it's really the Earth rotating under the fixed sky. The latitudinal (latitude-like) angle of the equatorial system is called declination (Dec for short) . It measures the angle of an object above or below the celestial equator. The longitud inal angle is called the right ascension (RA for short).
    [Show full text]
  • Exoplanet.Eu Catalog Page 1 # Name Mass Star Name
    exoplanet.eu_catalog # name mass star_name star_distance star_mass OGLE-2016-BLG-1469L b 13.6 OGLE-2016-BLG-1469L 4500.0 0.048 11 Com b 19.4 11 Com 110.6 2.7 11 Oph b 21 11 Oph 145.0 0.0162 11 UMi b 10.5 11 UMi 119.5 1.8 14 And b 5.33 14 And 76.4 2.2 14 Her b 4.64 14 Her 18.1 0.9 16 Cyg B b 1.68 16 Cyg B 21.4 1.01 18 Del b 10.3 18 Del 73.1 2.3 1RXS 1609 b 14 1RXS1609 145.0 0.73 1SWASP J1407 b 20 1SWASP J1407 133.0 0.9 24 Sex b 1.99 24 Sex 74.8 1.54 24 Sex c 0.86 24 Sex 74.8 1.54 2M 0103-55 (AB) b 13 2M 0103-55 (AB) 47.2 0.4 2M 0122-24 b 20 2M 0122-24 36.0 0.4 2M 0219-39 b 13.9 2M 0219-39 39.4 0.11 2M 0441+23 b 7.5 2M 0441+23 140.0 0.02 2M 0746+20 b 30 2M 0746+20 12.2 0.12 2M 1207-39 24 2M 1207-39 52.4 0.025 2M 1207-39 b 4 2M 1207-39 52.4 0.025 2M 1938+46 b 1.9 2M 1938+46 0.6 2M 2140+16 b 20 2M 2140+16 25.0 0.08 2M 2206-20 b 30 2M 2206-20 26.7 0.13 2M 2236+4751 b 12.5 2M 2236+4751 63.0 0.6 2M J2126-81 b 13.3 TYC 9486-927-1 24.8 0.4 2MASS J11193254 AB 3.7 2MASS J11193254 AB 2MASS J1450-7841 A 40 2MASS J1450-7841 A 75.0 0.04 2MASS J1450-7841 B 40 2MASS J1450-7841 B 75.0 0.04 2MASS J2250+2325 b 30 2MASS J2250+2325 41.5 30 Ari B b 9.88 30 Ari B 39.4 1.22 38 Vir b 4.51 38 Vir 1.18 4 Uma b 7.1 4 Uma 78.5 1.234 42 Dra b 3.88 42 Dra 97.3 0.98 47 Uma b 2.53 47 Uma 14.0 1.03 47 Uma c 0.54 47 Uma 14.0 1.03 47 Uma d 1.64 47 Uma 14.0 1.03 51 Eri b 9.1 51 Eri 29.4 1.75 51 Peg b 0.47 51 Peg 14.7 1.11 55 Cnc b 0.84 55 Cnc 12.3 0.905 55 Cnc c 0.1784 55 Cnc 12.3 0.905 55 Cnc d 3.86 55 Cnc 12.3 0.905 55 Cnc e 0.02547 55 Cnc 12.3 0.905 55 Cnc f 0.1479 55
    [Show full text]
  • List of Easy Double Stars for Winter and Spring  = Easy  = Not Too Difficult  = Difficult but Possible
    List of Easy Double Stars for Winter and Spring = easy = not too difficult = difficult but possible 1. Sigma Cassiopeiae (STF 3049). 23 hr 59.0 min +55 deg 45 min This system is tight but very beautiful. Use a high magnification (150x or more). Primary: 5.2, yellow or white Seconary: 7.2 (3.0″), blue 2. Eta Cassiopeiae (Achird, STF 60). 00 hr 49.1 min +57 deg 49 min This is a multiple system with many stars, but I will restrict myself to the brightest one here. Primary: 3.5, yellow. Secondary: 7.4 (13.2″), purple or brown 3. 65 Piscium (STF 61). 00 hr 49.9 min +27 deg 43 min Primary: 6.3, yellow Secondary: 6.3 (4.1″), yellow 4. Psi-1 Piscium (STF 88). 01 hr 05.7 min +21 deg 28 min This double forms a T-shaped asterism with Psi-2, Psi-3 and Chi Piscium. Psi-1 is the uppermost of the four. Primary: 5.3, yellow or white Secondary: 5.5 (29.7), yellow or white 5. Zeta Piscium (STF 100). 01 hr 13.7 min +07 deg 35 min Primary: 5.2, white or yellow Secondary: 6.3, white or lilac (or blue) 6. Gamma Arietis (Mesarthim, STF 180). 01 hr 53.5 min +19 deg 18 min “The Ram’s Eyes” Primary: 4.5, white Secondary: 4.6 (7.5″), white 7. Lambda Arietis (H 5 12). 01 hr 57.9 min +23 deg 36 min Primary: 4.8, white or yellow Secondary: 6.7 (37.1″), silver-white or blue 8.
    [Show full text]
  • The Brightest Stars Seite 1 Von 9
    The Brightest Stars Seite 1 von 9 The Brightest Stars This is a list of the 300 brightest stars made using data from the Hipparcos catalogue. The stellar distances are only fairly accurate for stars well within 1000 light years. 1 2 3 4 5 6 7 8 9 10 11 12 13 No. Star Names Equatorial Galactic Spectral Vis Abs Prllx Err Dist Coordinates Coordinates Type Mag Mag ly RA Dec l° b° 1. Alpha Canis Majoris Sirius 06 45 -16.7 227.2 -8.9 A1V -1.44 1.45 379.21 1.58 9 2. Alpha Carinae Canopus 06 24 -52.7 261.2 -25.3 F0Ib -0.62 -5.53 10.43 0.53 310 3. Alpha Centauri Rigil Kentaurus 14 40 -60.8 315.8 -0.7 G2V+K1V -0.27 4.08 742.12 1.40 4 4. Alpha Boötis Arcturus 14 16 +19.2 15.2 +69.0 K2III -0.05 -0.31 88.85 0.74 37 5. Alpha Lyrae Vega 18 37 +38.8 67.5 +19.2 A0V 0.03 0.58 128.93 0.55 25 6. Alpha Aurigae Capella 05 17 +46.0 162.6 +4.6 G5III+G0III 0.08 -0.48 77.29 0.89 42 7. Beta Orionis Rigel 05 15 -8.2 209.3 -25.1 B8Ia 0.18 -6.69 4.22 0.81 770 8. Alpha Canis Minoris Procyon 07 39 +5.2 213.7 +13.0 F5IV-V 0.40 2.68 285.93 0.88 11 9. Alpha Eridani Achernar 01 38 -57.2 290.7 -58.8 B3V 0.45 -2.77 22.68 0.57 144 10.
    [Show full text]
  • The Observer's Handbook for 1915
    T he O b s e r v e r ’s H a n d b o o k FOR 1915 PUBLISHED BY The Royal Astronomical Society Of Canada E d i t e d b y C . A. CHANT SEVENTH YEAR OF PUBLICATION TORONTO 198 C o l l e g e S t r e e t Pr in t e d f o r t h e S o c ie t y CALENDAR 1915 T he O bserver' s H andbook FOR 1915 PUBLISHED BY The Royal Astronomical Society Of Canada E d i t e d b y C. A. CHANT SEVENTH YEAR OF PUBLICATION TORONTO 198 C o l l e g e S t r e e t Pr in t e d f o r t h e S o c ie t y 1915 CONTENTS Preface - - - - - - 3 Anniversaries and Festivals - - - - - 3 Symbols and Abbreviations - - - - -4 Solar and Sidereal Time - - - - 5 Ephemeris of the Sun - - - - 6 Occultation of Fixed Stars by the Moon - - 8 Times of Sunrise and Sunset - - - - 8 The Sky and Astronomical Phenomena for each Month - 22 Eclipses, etc., of Jupiter’s Satellites - - - - 46 Ephemeris for Physical Observations of the Sun - - 48 Meteors and Shooting Stars - - - - - 50 Elements of the Solar System - - - - 51 Satellites of the Solar System - - - - 52 Eclipses of Sun and Moon in 1915 - - - - 53 List of Double Stars - - - - - 53 List of Variable Stars- - - - - - 55 The Stars, their Magnitude, Velocity, etc. - - - 56 The Constellations - - - - - - 64 Comets of 1914 - - - - - 76 PREFACE The H a n d b o o k for 1915 differs from that for last year chiefly in the omission of the brief review of astronomical pro­ gress, and the addition of (1) a table of double stars, (2) a table of variable stars, and (3) a table containing 272 stars and 5 nebulae.
    [Show full text]
  • Redox DAS Artist List for Period: 01.10.2017
    Page: 1 Redox D.A.S. Artist List for period: 01.10.2017 - 31.10.2017 Date time: Number: Title: Artist: Publisher Lang: 01.10.2017 00:02:40 HD 60753 TWO GHOSTS HARRY STYLES ANG 01.10.2017 00:06:22 HD 05631 BANKS OF THE OHIO OLIVIA NEWTON JOHN ANG 01.10.2017 00:09:34 HD 60294 BITE MY TONGUE THE BEACH ANG 01.10.2017 00:13:16 HD 26897 BORN TO RUN SUZY QUATRO ANG 01.10.2017 00:18:12 HD 56309 CIAO CIAO KATARINA MALA SLO 01.10.2017 00:20:55 HD 34821 OCEAN DRIVE LIGHTHOUSE FAMILY ANG 01.10.2017 00:24:41 HD 08562 NISEM JAZ SLAVKO IVANCIC SLO 01.10.2017 00:28:29 HD 59945 LEPE BESEDE PROTEUS SLO 01.10.2017 00:31:20 HD 03206 BLAME IT ON THE WEATHERMAN B WITCHED ANG 01.10.2017 00:34:52 HD 16013 OD TU NAPREJ NAVDIH TABU SLO 01.10.2017 00:38:14 HD 06982 I´M EVERY WOMAN WHITNEY HOUSTON ANG 01.10.2017 00:43:05 HD 05890 CRAZY LITTLE THING CALLED LOVE QUEEN ANG 01.10.2017 00:45:37 HD 57523 WHEN I WAS A BOY JEFF LYNNE (ELO) ANG 01.10.2017 00:48:46 HD 60269 MESTO (FEAT. VESNA ZORNIK) BREST SLO 01.10.2017 00:52:21 HD 06008 DEEPLY DIPPY RIGHT SAID FRED ANG 01.10.2017 00:55:35 HD 06012 UNCHAINED MELODY RIGHTEOUS BROTHERS ANG 01.10.2017 00:59:10 HD 60959 OKNA ORLEK SLO 01.10.2017 01:03:56 HD 59941 SAY SOMETHING LOVING THE XX ANG 01.10.2017 01:07:51 HD 15174 REAL GOOD LOOKING BOY THE WHO ANG 01.10.2017 01:13:37 HD 59654 RECI MI DA MANOUCHE SLO 01.10.2017 01:16:47 HD 60502 SE PREPOZNAS SHEBY SLO 01.10.2017 01:20:35 HD 06413 MARGUERITA TIME STATUS QUO ANG 01.10.2017 01:23:52 HD 06388 MAMA SPICE GIRLS ANG 01.10.2017 01:27:25 HD 02680 HIGHER GROUND ERIC CLAPTON ANG 01.10.2017 01:31:20 HD 59929 NE POZABI, DA SI LEPA LUKA SESEK & PROPER SLO 01.10.2017 01:34:57 HD 02131 BONNIE & CLYDE JAY-Z FEAT.
    [Show full text]
  • Downloads/ Astero2007.Pdf) and by Aerts Et Al (2010)
    This work is protected by copyright and other intellectual property rights and duplication or sale of all or part is not permitted, except that material may be duplicated by you for research, private study, criticism/review or educational purposes. Electronic or print copies are for your own personal, non- commercial use and shall not be passed to any other individual. No quotation may be published without proper acknowledgement. For any other use, or to quote extensively from the work, permission must be obtained from the copyright holder/s. i Fundamental Properties of Solar-Type Eclipsing Binary Stars, and Kinematic Biases of Exoplanet Host Stars Richard J. Hutcheon Submitted in accordance with the requirements for the degree of Doctor of Philosophy. Research Institute: School of Environmental and Physical Sciences and Applied Mathematics. University of Keele June 2015 ii iii Abstract This thesis is in three parts: 1) a kinematical study of exoplanet host stars, 2) a study of the detached eclipsing binary V1094 Tau and 3) and observations of other eclipsing binaries. Part I investigates kinematical biases between two methods of detecting exoplanets; the ground based transit and radial velocity methods. Distances of the host stars from each method lie in almost non-overlapping groups. Samples of host stars from each group are selected. They are compared by means of matching comparison samples of stars not known to have exoplanets. The detection methods are found to introduce a negligible bias into the metallicities of the host stars but the ground based transit method introduces a median age bias of about -2 Gyr.
    [Show full text]