DOCSLIB.ORG

Infrared Excesses in Stars with and Without Planets

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text
Infrared Excesses in Stars with and Without Planets Infrared Excesses in stars with and without planets by Ra´ulFelipe Maldonado S´anchez Thesis submitted in partial fulfillment of the requirements for the degree of MASTER OF SCIENCE IN ASTROPHYSICS at the Instituto Nacional de Astrof´ısica, Optica´ y Electr´onica August 2015 Tonantzintla, Puebla Under the supervision of: Ph.D. Miguel Ch´avez Dagostino (INAOE) Ph.D. Emanuele Bertone (INAOE) c INAOE, 2015 The author hereby grants to INAOE permission to reproduce and to distribute publicly paper and electronic copies of this thesis document in whole or in part. To my family and friends iii Acknowledgments I would like to offer my special thanks to my advisors Ph.D. Miguel Ch´avez Dagostino and Ph.D. Emanuele Bertone for all their support, advice and patience since the be- ginning of the project until the successful conclusion of this work, for helping me to improve this thesis and sharing me the necessary knowledge to do this research work. My special thanks are extended to Ph.D. Olga Vega, Ph.D. Alicia Porras and Ph.D. Abraham Luna for being examiners of this thesis and giving me the advices and com- ments to improve this research work. I am particularly grateful with all my classmates and friends: Eric, Carlos, Leticia, Emanuel, Ana, Gisela and Alan. They have shown me the meaning of a true friendship. The let me know that the study and learning in a perfect work team is easier and much funnier. I hope we still be friends for a long time and even collaborate in future projects. I would like to express my very great appreciation to my colleague and friend Rodrigo Pineda, for his friendship and all his support through the master studies and during the development of this thesis, for encouraging me to continue in difficult times and showing me the importance of the study everyday. I also want to thank Msc. Fernando Cruz S´aenzde Miera for his help in the develop- ment of this work. I give my special thanks to my mom, sisters, brothers in law, nephews and nice, who are showing me their care and love everyday. The accomplishment of all my goals is because of their emotional support. I really appreciate the knowledge acquired from all the teachers in the master, for their teachings in the classroom. Finally, I thank CONACYT for the financial support in the master studies. v List of Figures 1.1 Spectral energy distributions of Vega, Fomalhaut, Eridani and β Pictoris.2 1.2 Diagram of the evolution of a typical circumstellar disk..........3 1.3 Spectral Energy Distribution of the Herbig Ae star AB Aurigae.....4 1.4 Two parameter debris disk model......................6 1.5 Spectral Energy Distributions of stars with prominent 22 µm excesses..9 1.6 Evolution of 24 µm excesses around Sun-like stars............ 11 1.7 β Pictoris coronagraphic images....................... 13 1.8 Dust emission around Eridani at a wavelength of 850 µm........ 13 2.1 WISE satellite in its mapping configuration................ 16 2.2 Fit photometry profile differences between AllWISE and WISE All-Sky 17 2.3 Comparison of a real and spurious detection in WISE images...... 22 2.4 Spectral type distributions of stars with and without planets....... 23 2.5 Distance distribution of stars with and without planets......... 24 2.6 V magnitude distributions of stars with and without planets...... 24 2.7 Metallicity distributions of stars with and without planets....... 25 3.1 Color vs spectral type of stars with and without planets samples.... 28 3.2 Color excess distribution of the stars with and without planets sample. 29 3.3 Comparison between ATLAS9 and NEXTGEN synthetic spectra.... 33 3.4 Comparison of synthetic spectra with same Teff , surface gravity but different metallicity.............................. 35 3.5 Johnson, 2MASS and WISE filter response curves............ 36 3.6 Best fit of the Synthetic Spectral Energy Distribution for the star HD108874 using ATLAS9 models........................... 37 2 3.7 χν distribution for the stars with and without planets.......... 37 3.8 WISE vs Tycho-2 B-V color-diagrams................... 41 4.1 Distribution of uncertainties in the flux ratio W4/W3 in dependence of W4 flux.................................... 47 4.2 Distribution of total uncertainties propagated in the different IR-detection methods.................................... 48 4.3 Excess significance distribution of stars with and without planets.... 49 vii 4.4 Comparison between W4 and W3 observed and synthetic photometry as a function of W4 flux for each star in the combined samples of stars with and without planets.......................... 50 4.5 Comparison between W4, W3 and W2 observed and synthetic photom- etry in dependence of W4 flux for each star in the combined samples of stars with and without planets....................... 51 4.6 Flux comparison of the WISE bands between the WISE catalogues avail- able in the literature............................. 53 4.7 Spectral energy distribution of HD 106906................. 55 4.8 Spectral energy distribution of V342Peg (HR 8799)............ 56 4.9 Spectral energy distribution of BD-10 3166................ 57 4.10 Spectral energy distribution of CD-301812................. 58 4.11 WISE W4 pixel intensity distribution of CD-301812........... 58 4.12 WISE W2, W3 and W4 images of CD-301812............... 59 4.13 Spectral energy distribution of HD107146................. 60 4.14 Spectral energy distribution of HD85301.................. 61 4.15 Spectral energy distribution of HD 136544................. 62 A.1 Empirically determined WISE vs. B-V photospheric color-color trends for all six WISE colors............................ 69 B.1 Spectral energy distributions of HD106906 & HR7899.......... 71 B.2 Spectral energy distributions of HD45184 & HD113337.......... 72 B.3 Spectral energy distributions of HD114729A & HR6907.......... 72 B.4 Spectral energy distributions of HD11506 & HD224693.......... 72 B.5 Spectral energy distributions of HD130322 & HD98649.......... 73 B.6 Spectral energy distributions of HD168443 & HD33643.......... 73 B.7 Spectral energy distribution of HD4113.................. 73 B.8 Spectral energy distributions of HD107146 & HD85301......... 74 B.9 Spectral energy distributions of HD60491 & HD125040.......... 74 B.10 Spectral energy distributions of AFLep & HD136544........... 75 B.11 Spectral energy distributions of HD29137 & HD34745.......... 75 B.12 Spectral energy distributions of HD8907 & LQHya............ 75 B.13 Spectral energy distributions of HD96418 & HR1981........... 76 B.14 Spectral energy distributions of HD205294 & HD44821.......... 76 B.15 Spectral energy distributions of HD85638 & HD209253.......... 76 List of Tables 3.1 Zero magnitude flux density for B, V, J, H, KS, W1, W2, W3, W4 bands. 30 3.2 Extinction law coefficients as a function of wavelength.......... 30 3.3 Color corrections............................... 32 3.4 Flux ratio comparison among the WISE bands in ATLAS9 synthetic spectra with different stellar parameters.................. 34 4.1 Number and percentage of IR excesses (E) in stars with and without planets.................................... 43 C.1 Stellar parameters of the sample of stars with planets........... 77 C.2 Stellar parameters of the sample of stars without planets......... 81 D.1 Observed fluxes for stars with planets................... 100 D.2 Observed fluxes for stars without planets.................. 106 ix Contents Acknowledgmentsv 1 Introduction1 1.1 Circumstellar Disks.............................1 1.1.1 Protoplanetary Disks........................4 1.1.2 Debris Disks.............................5 1.2 Observing Debris Disks at IR wavelengths................7 1.3 Mid-IR observations: Warm debris disks.................8 1.4 Planet interaction and disks........................ 12 1.5 Aims of this work.............................. 14 2 The sample selection 15 2.1 IR Surveys.................................. 15 2.1.1 Wide-field Infrared Survey Explorer (WISE)........... 15 2.1.2 Two Micron All Sky Survey (2MASS)............... 18 2.2 The sample................................. 19 2.2.1 Stars with planets.......................... 19 2.2.2 Stars without planets........................ 20 2.3 Optical and Infrared photometry..................... 21 2.3.1 Comparison of both samples.................... 22 3 Methodology 27 3.1 Correction for extinction and magnitude to flux conversion....... 27 3.2 Photosphere fitting and synthetic photometry.............. 32 3.3 Searching for Infrared Excesses....................... 38 3.3.1 Method 1 (This work)....................... 38 3.3.2 Method 2: Cruz-Saenz de Miera et al.(2014)........... 39 3.3.3 Method 3: Kennedy & Wyatt(2012)............... 39 3.3.4 Method 4: Morales et al.(2012).................. 40 3.3.5 Method 5: Patel et al.(2014)................... 40 4 Results 43 4.1 Comparing the two stellar samples.................... 44 xi 4.2 Comparison among the methods...................... 45 4.2.1 This work vs. Cruz-Saenz de Miera et al.(2014)......... 45 4.2.2 Kennedy & Wyatt(2012) vs. Morales et al.(2012)....... 45 4.2.3 Patel et al.(2014) vs. Morales et al.(2012)............ 46 4.3 Explaining differences among the methods................ 46 4.3.1 So, which is the best method?................... 51 4.4 Comparison between WISE data releases................. 52 4.5 Comments on some stars with planets................... 54 4.5.1 HD106906.............................. 54 4.5.2 V342Peg (HR 8799)........................ 55 4.5.3 BD-10 3166............................. 56 4.5.4 CD-301812 (WASP-79)....................... 57 4.6 Comments
Load more

Recommended publications
  • Lurking in the Shadows: Wide-Separation Gas Giants As Tracers of Planet Formation
    Lurking in the Shadows: Wide-Separation Gas Giants as Tracers of Planet Formation Thesis by Marta Levesque Bryan In Partial Fulfillment of the Requirements for the Degree of Doctor of Philosophy CALIFORNIA INSTITUTE OF TECHNOLOGY Pasadena, California 2018 Defended May 1, 2018 ii © 2018 Marta Levesque Bryan ORCID: [0000-0002-6076-5967] All rights reserved iii ACKNOWLEDGEMENTS First and foremost I would like to thank Heather Knutson, who I had the great privilege of working with as my thesis advisor. Her encouragement, guidance, and perspective helped me navigate many a challenging problem, and my conversations with her were a consistent source of positivity and learning throughout my time at Caltech. I leave graduate school a better scientist and person for having her as a role model. Heather fostered a wonderfully positive and supportive environment for her students, giving us the space to explore and grow - I could not have asked for a better advisor or research experience. I would also like to thank Konstantin Batygin for enthusiastic and illuminating discussions that always left me more excited to explore the result at hand. Thank you as well to Dimitri Mawet for providing both expertise and contagious optimism for some of my latest direct imaging endeavors. Thank you to the rest of my thesis committee, namely Geoff Blake, Evan Kirby, and Chuck Steidel for their support, helpful conversations, and insightful questions. I am grateful to have had the opportunity to collaborate with Brendan Bowler. His talk at Caltech my second year of graduate school introduced me to an unexpected population of massive wide-separation planetary-mass companions, and lead to a long-running collaboration from which several of my thesis projects were born.
    [Show full text]
  • Where Are the Distant Worlds? Star Maps
    W here Are the Distant Worlds? Star Maps Abo ut the Activity Whe re are the distant worlds in the night sky? Use a star map to find constellations and to identify stars with extrasolar planets. (Northern Hemisphere only, naked eye) Topics Covered • How to find Constellations • Where we have found planets around other stars Participants Adults, teens, families with children 8 years and up If a school/youth group, 10 years and older 1 to 4 participants per map Materials Needed Location and Timing • Current month's Star Map for the Use this activity at a star party on a public (included) dark, clear night. Timing depends only • At least one set Planetary on how long you want to observe. Postcards with Key (included) • A small (red) flashlight • (Optional) Print list of Visible Stars with Planets (included) Included in This Packet Page Detailed Activity Description 2 Helpful Hints 4 Background Information 5 Planetary Postcards 7 Key Planetary Postcards 9 Star Maps 20 Visible Stars With Planets 33 © 2008 Astronomical Society of the Pacific www.astrosociety.org Copies for educational purposes are permitted. Additional astronomy activities can be found here: http://nightsky.jpl.nasa.gov Detailed Activity Description Leader’s Role Participants’ Roles (Anticipated) Introduction: To Ask: Who has heard that scientists have found planets around stars other than our own Sun? How many of these stars might you think have been found? Anyone ever see a star that has planets around it? (our own Sun, some may know of other stars) We can’t see the planets around other stars, but we can see the star.
    [Show full text]
  • Meeting Announcement Upcoming Star Parties And
    CVAS Executive Committee Pres – Bruce Horrocks Night Sky Network Coordinator – [email protected] Garrett Smith – [email protected] Vice Pres- James Somers Past President – Dell Vance (435) 938-8328 [email protected] [email protected] Treasurer- Janice Bradshaw Public Relations – Lyle Johnson - [email protected] [email protected] Secretary – Wendell Waters (435) 213-9230 Webmaster, Librarian – Tom Westre [email protected] [email protected] Vol. 7 Number 6 February 2020 www.cvas-utahskies.org The President’s Corner Meeting Announcement By Bruce Horrocks – CVAS President Our next meeting will be held on Wed. I don’t know about most of you, but I for February 26th at 7 pm in the Lake Bonneville Room one would be glad to at least see a bit of sun and of the Logan City Library. Our presenter will be clear skies at least once this winter. I believe there Wendell Waters, and his presentation is called was just a couple of nights in the last 2 months that “Charles Messier and the ‘Not-Comet’ Catalogue”. I was able to get out and do some observing and so I The meeting is free and open to the public. am hoping to see some clear skies this spring. I Light refreshments will be served. COME AND have watched all the documentaries I can stand on JOIN US!! Netflix, so I am running out of other nighttime activities to do and I really want to get out and test my new little 72mm telescope. Upcoming Star Parties and CVAS Events We made a change to our club fees at our last meeting and if you happened to have missed We have four STEM Nights coming up in that I will just quickly explain it to you now.
    [Show full text]
  • Staff, Visiting Scientists and Graduate Students at the Pescara Center December 2012 2
    Staff, Visiting Scientists and Graduate Students at the Pescara Center December 2012 2 Contents ICRANet Faculty Staff……………………………………………………………………. p. 17 Adjunct Professors of the Faculty .……………………………………………………… p. 36 Lecturers…………………………………………………………………………………… p. 64 Research Scientists ……………………………………………………………………….. p. 76 Visiting Scientists ………………………………………………………………………... p. 86 IRAP Ph. D. Students ……………………………………………………………………. p. 103 IRAP Ph. D. Erasmus Mundus Students………………………………………………. p. 123 Administrative and Secretarial Staff …………………………………………………… p. 135 3 4 ICRANet Faculty Staff Belinski Vladimir ICRANet Bianco Carlo Luciano University of Rome “Sapienza” and ICRANet Einasto Jaan Tartu Observatory, Estonia Novello Mario Cesare Lattes-ICRANet Chair CBPF, Rio de Janeiro, Brasil Rueda Jorge A. University of Rome “Sapienza” and ICRANet Ruffini Remo University of Rome “Sapienza” and ICRANet Vereshchagin Gregory ICRANet Xue She-Sheng ICRANet 5 Adjunct Professors Of The Faculty Aharonian Felix Albert Benjamin Jegischewitsch Markarjan Chair Dublin Institute for Advanced Studies, Dublin, Ireland Max-Planck-Institut für Kernphysis, Heidelberg, Germany Amati Lorenzo Istituto di Astrofisica Spaziale e Fisica Cosmica, Italy Arnett David Subramanyan Chandrasektar- ICRANet Chair University of Arizona, Tucson, USA Chakrabarti Sandip P. Centre for Space Physics, India Chardonnet Pascal Université de la Savoie, France Chechetkin Valeri Mstislav Vsevolodich Keldysh-ICRANet Chair Keldysh institute for Applied Mathematics Moscow, Russia Damour Thibault Joseph-Louis
    [Show full text]
  • Winter Constellations
    Winter Constellations *Orion *Canis Major *Monoceros *Canis Minor *Gemini *Auriga *Taurus *Eradinus *Lepus *Monoceros *Cancer *Lynx *Ursa Major *Ursa Minor *Draco *Camelopardalis *Cassiopeia *Cepheus *Andromeda *Perseus *Lacerta *Pegasus *Triangulum *Aries *Pisces *Cetus *Leo (rising) *Hydra (rising) *Canes Venatici (rising) Orion--Myth: Orion, the great ​ ​ hunter. In one myth, Orion boasted he would kill all the wild animals on the earth. But, the earth goddess Gaia, who was the protector of all animals, produced a gigantic scorpion, whose body was so heavily encased that Orion was unable to pierce through the armour, and was himself stung to death. His companion Artemis was greatly saddened and arranged for Orion to be immortalised among the stars. Scorpius, the scorpion, was placed on the opposite side of the sky so that Orion would never be hurt by it again. To this day, Orion is never seen in the sky at the same time as Scorpius. DSO’s ● ***M42 “Orion Nebula” (Neb) with Trapezium A stellar ​ ​ ​ nursery where new stars are being born, perhaps a thousand stars. These are immense clouds of interstellar gas and dust collapse inward to form stars, mainly of ionized hydrogen which gives off the red glow so dominant, and also ionized greenish oxygen gas. The youngest stars may be less than 300,000 years old, even as young as 10,000 years old (compared to the Sun, 4.6 billion years old). 1300 ly. ​ ​ 1 ● *M43--(Neb) “De Marin’s Nebula” The star-forming ​ “comma-shaped” region connected to the Orion Nebula. ● *M78--(Neb) Hard to see. A star-forming region connected to the ​ Orion Nebula.
    [Show full text]
  • Li Abundances in F Stars: Planets, Rotation, and Galactic Evolution,
    A&A 576, A69 (2015) Astronomy DOI: 10.1051/0004-6361/201425433 & c ESO 2015 Astrophysics Li abundances in F stars: planets, rotation, and Galactic evolution, E. Delgado Mena1,2, S. Bertrán de Lis3,4, V. Zh. Adibekyan1,2,S.G.Sousa1,2,P.Figueira1,2, A. Mortier6, J. I. González Hernández3,4,M.Tsantaki1,2,3, G. Israelian3,4, and N. C. Santos1,2,5 1 Centro de Astrofisica, Universidade do Porto, Rua das Estrelas, 4150-762 Porto, Portugal e-mail: [email protected] 2 Instituto de Astrofísica e Ciências do Espaço, Universidade do Porto, CAUP, Rua das Estrelas, 4150-762 Porto, Portugal 3 Instituto de Astrofísica de Canarias, C/via Lactea, s/n, 38200 La Laguna, Tenerife, Spain 4 Departamento de Astrofísica, Universidad de La Laguna, 38205 La Laguna, Tenerife, Spain 5 Departamento de Física e Astronomía, Faculdade de Ciências, Universidade do Porto, Portugal 6 SUPA, School of Physics and Astronomy, University of St. Andrews, St. Andrews KY16 9SS, UK Received 28 November 2014 / Accepted 14 December 2014 ABSTRACT Aims. We aim, on the one hand, to study the possible differences of Li abundances between planet hosts and stars without detected planets at effective temperatures hotter than the Sun, and on the other hand, to explore the Li dip and the evolution of Li at high metallicities. Methods. We present lithium abundances for 353 main sequence stars with and without planets in the Teff range 5900–7200 K. We observed 265 stars of our sample with HARPS spectrograph during different planets search programs. We observed the remaining targets with a variety of high-resolution spectrographs.
    [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]
  • Exodata: a Python Package to Handle Large Exoplanet Catalogue Data
    ExoData: A Python package to handle large exoplanet catalogue data Ryan Varley Department of Physics & Astronomy, University College London 132 Hampstead Road, London, NW1 2PS, United Kingdom [email protected] Abstract Exoplanet science often involves using the system parameters of real exoplanets for tasks such as simulations, fitting routines, and target selection for proposals. Several exoplanet catalogues are already well established but often lack a version history and code friendly interfaces. Software that bridges the barrier between the catalogues and code enables users to improve the specific repeatability of results by facilitating the retrieval of exact system parameters used in an arti- cles results along with unifying the equations and software used. As exoplanet science moves towards large data, gone are the days where researchers can recall the current population from memory. An interface able to query the population now becomes invaluable for target selection and population analysis. ExoData is a Python interface and exploratory analysis tool for the Open Exoplanet Cata- logue. It allows the loading of exoplanet systems into Python as objects (Planet, Star, Binary etc) from which common orbital and system equations can be calculated and measured parame- ters retrieved. This allows researchers to use tested code of the common equations they require (with units) and provides a large science input catalogue of planets for easy plotting and use in research. Advanced querying of targets are possible using the database and Python programming language. ExoData is also able to parse spectral types and fill in missing parameters according to programmable specifications and equations. Examples of use cases are integration of equations into data reduction pipelines, selecting planets for observing proposals and as an input catalogue to large scale simulation and analysis of planets.
    [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]
  • 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.
    [Show full text]
  • Exoplanet Community Report
    JPL Publication 09‐3 Exoplanet Community Report Edited by: P. R. Lawson, W. A. Traub and S. C. Unwin National Aeronautics and Space Administration Jet Propulsion Laboratory California Institute of Technology Pasadena, California March 2009 The work described in this publication was performed at a number of organizations, including the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration (NASA). Publication was provided by the Jet Propulsion Laboratory. Compiling and publication support was provided by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. Reference herein to any specific commercial product, process, or service by trade name, trademark, manufacturer, or otherwise, does not constitute or imply its endorsement by the United States Government, or the Jet Propulsion Laboratory, California Institute of Technology. © 2009. All rights reserved. The exoplanet community’s top priority is that a line of probe­class missions for exoplanets be established, leading to a flagship mission at the earliest opportunity. iii Contents 1 EXECUTIVE SUMMARY.................................................................................................................. 1 1.1 INTRODUCTION...............................................................................................................................................1 1.2 EXOPLANET FORUM 2008: THE PROCESS OF CONSENSUS BEGINS.....................................................2
    [Show full text]
  • Sydney Observatory Night Sky Map September 2012 a Map for Each Month of the Year, to Help You Learn About the Night Sky
    Sydney Observatory night sky map September 2012 A map for each month of the year, to help you learn about the night sky www.sydneyobservatory.com This star chart shows the stars and constellations visible in the night sky for Sydney, Melbourne, Brisbane, Canberra, Hobart, Adelaide and Perth for September 2012 at about 7:30 pm (local standard time). For Darwin and similar locations the chart will still apply, but some stars will be lost off the southern edge while extra stars will be visible to the north. Stars down to a brightness or magnitude limit of 4.5 are shown. To use this chart, rotate it so that the direction you are facing (north, south, east or west) is shown at the bottom. The centre of the chart represents the point directly above your head, called the zenith, and the outer circular edge represents the horizon. h t r No Star brightness Moon phase Last quarter: 08th Zero or brighter New Moon: 16th 1st magnitude LACERTA nd Deneb First quarter: 23rd 2 CYGNUS Full Moon: 30th rd N 3 E LYRA th Vega W 4 LYRA N CORONA BOREALIS HERCULES BOOTES VULPECULA SAGITTA PEGASUS DELPHINUS Arcturus Altair EQUULEUS SERPENS AQUILA OPHIUCHUS SCUTUM PISCES Moon on 23rd SERPENS Zubeneschamali AQUARIUS CAPRICORNUS E SAGITTARIUS LIBRA a Saturn Centre of the Galaxy Antares Zubenelgenubi t s Antares VIRGO s t SAGITTARIUS P SCORPIUS P e PISCESMICROSCOPIUM AUSTRINUS SCORPIUS Mars Spica W PISCIS AUSTRINUS CORONA AUSTRALIS Fomalhaut Centre of the Galaxy TELESCOPIUM LUPUS ARA GRUSGRUS INDUS NORMA CORVUS INDUS CETUS SCULPTOR PAVO CIRCINUS CENTAURUS TRIANGULUM
    [Show full text]