Super Earth Explorer: a Coronagraphic Off-Axis Space Telescope
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Planetas Extrasolares
Local Extrasolar Planets Universidad Andres Bello ESO Vitacura 4 June 2015 Foto: Dante Joyce Minniti Pullen The big picture 1. Increase human resources and networks for national Astronomy 2. Develop new areas of research and do quality science 3. Promote science in Chile Universidad Andres Bello ESO Vitacura 4 June 2015 Dante Minniti The Pioneers Wolfgang Gieren Maria Teresa Ruiz Grzegorz Pietrzynski Dante Minniti School on Extrasolar Planets and Brown Dwarfs Santiago, 2003 Invited Lecturers: Michel Mayor, Scott Tremaine, Gill Knapp, France Allard Universidad Andres Bello ESO Vitacura 4 June 2015 Dante Minniti It is all about time... Telescope time is the most precious... Universidad Andres Bello ESO Vitacura 4 June 2015 Dante Minniti The Pioneers Wolfgang Gieren Maria Teresa Ruiz Grzegorz Pietrzynski Dante Minniti The first exoplanet for us: M. Konacki, G. Torres, D. D. Sasselov, G. Pietrzynski, A. Udalski, S. Jha, M. T. Ruiz, W. Gieren, & D. Minniti, “A Transiting Extrasolar Giant Planet Around the Star OGLE-TR-113'', 2004, ApJ, 609, L37” Universidad Andres Bello ESO Vitacura 4 June 2015 Dante Minniti The Pioneers Paul Butler Debra Fischer Dante Minniti The First Planets from the N2K Consortium Fischer et al., ``A Hot Saturn Planet Orbiting HD 88133, from the N2K Consortium", 2005, The Astrophysical Journal, 620, 481 Sato, et al., ``The N2K Consortium. II. A Transiting Hot Saturn around HD 149026 with a Large Dense Core", 2005, The Astrophysical Journal, 633, 465 Universidad Andres Bello ESO Vitacura 4 June 2015 Dante Minniti The Pioneers -
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. -
Miniature Exoplanet Radial Velocity Array I: Design, Commissioning, and Early Photometric Results
Miniature Exoplanet Radial Velocity Array I: design, commissioning, and early photometric results Jonathan J. Swift Steven R. Gibson Michael Bottom Brian Lin John A. Johnson Ming Zhao Jason T. Wright Paul Gardner Nate McCrady Emilio Falco Robert A. Wittenmyer Stephen Criswell Peter Plavchan Chantanelle Nava Reed Riddle Connor Robinson Philip S. Muirhead David H. Sliski Erich Herzig Richard Hedrick Justin Myles Kevin Ivarsen Cullen H. Blake Annie Hjelstrom Jason Eastman Jon de Vera Thomas G. Beatty Andrew Szentgyorgyi Stuart I. Barnes Downloaded From: http://astronomicaltelescopes.spiedigitallibrary.org/ on 05/21/2017 Terms of Use: http://spiedigitallibrary.org/ss/termsofuse.aspx Journal of Astronomical Telescopes, Instruments, and Systems 1(2), 027002 (Apr–Jun 2015) Miniature Exoplanet Radial Velocity Array I: design, commissioning, and early photometric results Jonathan J. Swift,a,*,† Michael Bottom,a John A. Johnson,b Jason T. Wright,c Nate McCrady,d Robert A. Wittenmyer,e Peter Plavchan,f Reed Riddle,a Philip S. Muirhead,g Erich Herzig,a Justin Myles,h Cullen H. Blake,i Jason Eastman,b Thomas G. Beatty,c Stuart I. Barnes,j,‡ Steven R. Gibson,k,§ Brian Lin,a Ming Zhao,c Paul Gardner,a Emilio Falco,l Stephen Criswell,l Chantanelle Nava,d Connor Robinson,d David H. Sliski,i Richard Hedrick,m Kevin Ivarsen,m Annie Hjelstrom,n Jon de Vera,n and Andrew Szentgyorgyil aCalifornia Institute of Technology, Departments of Astronomy and Planetary Science, 1200 E. California Boulevard, Pasadena, California 91125, United States bHarvard-Smithsonian Center for Astrophysics, Cambridge, Massachusetts 02138, United States cThe Pennsylvania State University, Department of Astronomy and Astrophysics, Center for Exoplanets and Habitable Worlds, 525 Davey Laboratory, University Park, Pennsylvania 16802, United States dUniversity of Montana, Department of Physics and Astronomy, 32 Campus Drive, No. -
A GROUND-BASED ALBEDO UPPER LIMIT for HD 189733B from POLARIMETRY Sloane J
The Astrophysical Journal, 813:48 (11pp), 2015 November 1 doi:10.1088/0004-637X/813/1/48 © 2015. The American Astronomical Society. All rights reserved. A GROUND-BASED ALBEDO UPPER LIMIT FOR HD 189733b FROM POLARIMETRY Sloane J. Wiktorowicz1,2, Larissa A. Nofi3,1, Daniel Jontof-Hutter4,5, Pushkar Kopparla6, Gregory P. Laughlin1, Ninos Hermis1, Yuk L. Yung6, and Mark R. Swain7 1 Department of Astronomy and Astrophysics, University of California, Santa Cruz, CA 95064, USA; [email protected] 2 Remote Sensing Department, The Aerospace Corporation, El Segundo, CA 90245, USA 3 Institute for Astronomy, University of Hawaii, Honolulu, HI 96822, USA 4 Department of Astronomy, Davey Laboratory, Pennsylvania State University, University Park, PA 16802, USA 5 NASA Ames Research Center, Moffett Field, CA 94035, USA 6 Division of Geological and Planetary Sciences, California Institute of Technology, Pasadena, CA 91125, USA 7 Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena, CA 91109, USA Received 2015 July 13; accepted 2015 September 29; published 2015 October 27 ABSTRACT We present 50 nights of polarimetric observations of HD 189733 in the B band using the POLISH2 aperture- integrated polarimeter at the Lick Observatory Shane 3-m telescope. This instrument, commissioned in 2011, is designed to search for Rayleigh scattering from short-period exoplanets due to the polarized nature of scattered light. Since these planets are spatially unresolvable from their host stars, the relative contribution of the planet-to- total system polarization is expected to vary with an amplitude of the order of 10 parts per million (ppm) over the course of the orbit. -
Simulating (Sub)Millimeter Observations of Exoplanet Atmospheres in Search of Water
University of Groningen Kapteyn Astronomical Institute Simulating (Sub)Millimeter Observations of Exoplanet Atmospheres in Search of Water September 5, 2018 Author: N.O. Oberg Supervisor: Prof. Dr. F.F.S. van der Tak Abstract Context: Spectroscopic characterization of exoplanetary atmospheres is a field still in its in- fancy. The detection of molecular spectral features in the atmosphere of several hot-Jupiters and hot-Neptunes has led to the preliminary identification of atmospheric H2O. The Atacama Large Millimiter/Submillimeter Array is particularly well suited in the search for extraterrestrial water, considering its wavelength coverage, sensitivity, resolving power and spectral resolution. Aims: Our aim is to determine the detectability of various spectroscopic signatures of H2O in the (sub)millimeter by a range of current and future observatories and the suitability of (sub)millimeter astronomy for the detection and characterization of exoplanets. Methods: We have created an atmospheric modeling framework based on the HAPI radiative transfer code. We have generated planetary spectra in the (sub)millimeter regime, covering a wide variety of possible exoplanet properties and atmospheric compositions. We have set limits on the detectability of these spectral features and of the planets themselves with emphasis on ALMA. We estimate the capabilities required to study exoplanet atmospheres directly in the (sub)millimeter by using a custom sensitivity calculator. Results: Even trace abundances of atmospheric water vapor can cause high-contrast spectral ab- sorption features in (sub)millimeter transmission spectra of exoplanets, however stellar (sub) millime- ter brightness is insufficient for transit spectroscopy with modern instruments. Excess stellar (sub) millimeter emission due to activity is unlikely to significantly enhance the detectability of planets in transit except in select pre-main-sequence stars. -
Report by the ESA–ESO Working Group on Extra-Solar Planets
Report by the ESA–ESO Working Group on Extra-Solar Planets 4 March 2005 Summary Various techniques are being used to search for extra-solar planetary signatures, including accurate measurement of radial velocity and positional (astrometric) dis- placements, gravitational microlensing, and photometric transits. Planned space experiments promise a considerable increase in the detections and statistical know- ledge arising especially from transit and astrometric measurements over the years 2005–15, with some hundreds of terrestrial-type planets expected from transit mea- surements, and many thousands of Jupiter-mass planets expected from astrometric measurements. Beyond 2015, very ambitious space (Darwin/TPF) and ground (OWL) experiments are targeting direct detection of nearby Earth-mass planets in the habitable zone and the measurement of their spectral characteristics. Beyond these, ‘Life Finder’ (aiming to produce confirmatory evidence of the presence of life) and ‘Earth Imager’ (some massive interferometric array providing resolved images of a distant Earth) arXiv:astro-ph/0506163v1 8 Jun 2005 appear as distant visions. This report, to ESA and ESO, summarises the direction of exo-planet research that can be expected over the next 10 years or so, identifies the roles of the major facilities of the two organisations in the field, and concludes with some recommendations which may assist development of the field. The report has been compiled by the Working Group members and experts (page iii) over the period June–December 2004. Introduction & Background Following an agreement to cooperate on science planning issues, the executives of the European Southern Observatory (ESO) and the European Space Agency (ESA) Science Programme and representatives of their science advisory structures have met to share information and to identify potential synergies within their future projects. -
Looking for New Earth in the Coming Decade
Detection of Earth-like Planets with NWO With discoveries like methane on Mars (Mumma et al. 2009) and super-Earth planets orbiting nearby stars (Howard et al. 2009), the fields of exobiology and exoplanetary science are breaking new ground on almost a weekly basis. These two fields will one day merge, with the high goal of discovering Earth-like planets orbiting nearby stars and the subsequent search for signs of life on those planets. The Kepler mission will soon place clear bounds on the frequency of terrestrial-sized planets (Basri et al. 2008). Beyond that, the great challenge is to determine their true natures. Are terrestrial exoplanets anything like Earth, with life forms able to thrive even on the surface? What is the range of conditions under which Earth-like and other habitable worlds can arise? Every stellar system in the solar neighborhood is entirely unique, and it is almost certain that anything that can happen, will. With current and near-term technology, we can make great strides in finding and characterizing planets in the habitable zones of nearby stars. Given reasonable mission specifications for the New Worlds Observer, the layout of the stars in the solar neighborhood, and their variable characteristics (especially exozodiacal dust) a direct imaging mission can detect and characterize dozens of Earths. Not only does direct imaging achieve detection of planets in a single visit, but photometry, spectroscopy, polarimetry and time-variability in those signals place strong constraints on how those planets compare to our own, including plausible ranges in planet mass and atmospheric and internal structure. -
Link 1. JA Acosta-Pulido, I. Agudo, R. Barrena
# Author Year Title Journal Vol. Page [Count Tel. (Instrument) Link ry] 1. J. A. Acosta‐pulido, I. Agudo, R. Barrena, C. Ramos Almeida, A. 2010 The redshift and broad‐band spectral energy distribution of A&A 519 A5 [ES] WHT (LIRIS) http://www.aanda.org/index.php?op Manchado and P. Rodríguez‐Gil NRAO 150 tion=com_article&access=standard&I temid=129&url=/articles/aa/full_htm l/2010/11/aa13953‐09/aa13953‐ 09.html 2. R. Alonso, H. J. Deeg, P. Kabath and M. Rabus 2010 Ground‐based Near‐infrared Observations of the Secondary AJ 139 1481 [CH] WHT (LIRIS) http://iopscience.iop.org/1538‐ Eclipse of CoRoT‐2b 3881/139/4/1481/fulltext 3. J. P. Anderson, R. A. Covarrubias, P. A. James, M. Hamuy and S. 2010 Observational constraints on the progenitor metallicities of MNRAS 407 2660 [CL] WHT (ISIS) http://onlinelibrary.wiley.com/doi/10 M. Habergham core‐collapse supernovae .1111/j.1365‐2966.2010.17118.x/full 4. Iair Arcavi, Avishay Gal‐Yam, Mansi M. Kasliwal, Robert M. 2010 Core‐collapse Supernovae from the Palomar Transient ApJ 721 777 [IL] WHT (ISIS) http://iopscience.iop.org/0004‐ Quimby, Eran O. Ofek, Shrinivas R. Kulkarni, Peter E. Nugent, S. Factory: Indications for a Different Population in Dwarf 637X/721/1/777/fulltext Bradley Cenko, Joshua S. Bloom, Mark Sullivan, D. Andrew Galaxies Howell, Dovi Poznanski, Alexei V. Filippenko, Nicholas Law, Isobel Hook, Jakob Jönsson, Sarah Blake, Jeff Cooke, Richard Dekany, Gustavo Rahmer, David Hale, Roger Smith, Jeff Zolkower, Viswa Velur, Richard Walters, John Henning, Kahnh Bui, Dan McKenna and Janet Jacobsen 5. -
Mètodes De Detecció I Anàlisi D'exoplanetes
MÈTODES DE DETECCIÓ I ANÀLISI D’EXOPLANETES Rubén Soussé Villa 2n de Batxillerat Tutora: Dolors Romero IES XXV Olimpíada 13/1/2011 Mètodes de detecció i anàlisi d’exoplanetes . Índex - Introducció ............................................................................................. 5 [ Marc Teòric ] 1. L’Univers ............................................................................................... 6 1.1 Les estrelles .................................................................................. 6 1.1.1 Vida de les estrelles .............................................................. 7 1.1.2 Classes espectrals .................................................................9 1.1.3 Magnitud ........................................................................... 9 1.2 Sistemes planetaris: El Sistema Solar .............................................. 10 1.2.1 Formació ......................................................................... 11 1.2.2 Planetes .......................................................................... 13 2. Planetes extrasolars ............................................................................ 19 2.1 Denominació .............................................................................. 19 2.2 Història dels exoplanetes .............................................................. 20 2.3 Mètodes per detectar-los i saber-ne les característiques ..................... 26 2.3.1 Oscil·lació Doppler ........................................................... 27 2.3.2 Trànsits -
Super Earth Explorer: a Coronagraphic Off-Axis Space Telescope
DRAFT Super Earth Explorer: A Coronagraphic Off-Axis Space Telescope Schneider J.a, Boccaletti A.b, Mawet D.e Baudoz P.b, Beuzit J.-L.c, Doyon R.d Marley M.e, Stam D g., Tinetti Gh. Traub W. f, Trauger J.f, Aylward A.h, Cho J. Y-K. i , Keller C.-U. J , Udry S.k, and the SEE-COAST Team 1 a LUTH, Paris Observatory; b LESIA, Paris Observatory; c LAOG; d U. Montreal, e NASA/Ames, f Jet Propulsion Laboratory, California Institute of Technology; g SRON; hUCL, ; i Queen Mary, U. London, J U. Utrecht,, k Geneva Observatory jean.schneider.obspm.fr keywords: exoplanets, coronagraphy Accepted in “Experimental Astronomy” 1 Full list at the end of the paper 1 Abstract: The Super-Earth Explorer is an Off-Axis Space Telescope (SEE-COAST) designed for high contrast imaging. Its scientific objective is to make the physico-chemical characterization of exoplanets possibly down to 2 Earth radii . For that purpose it will analyze the spectral and polarimetric properties of the parent starlight reflected by the planets, in the wavelength range 400-1250 nm 1. Scientific Objectives The currently known planetary systems from indirect detection show a huge diversity in the orbits (semi-major axis and eccentricity), masses, and, in a few cases, radii of their planets. If we add to this the observation that the planets in our Solar System differ strongly from each other, there is no doubt that more information on the physical characteristics of exoplanets will reveal not only new and unexpected scenarios but also answers and a better understanding. -
PDF (Full Thesis)
Unambiguous Black Hole Mass from Polarimetry and Application to Hot Jupiters Dissertation by Sloane J. Wiktorowicz In Partial Fulfillment of the Requirements for the Degree of Doctor of Philosophy California Institute of Technology Pasadena, California 2009 (Defended July 28, 2008) ii c 2009 Sloane J. Wiktorowicz All Rights Reserved iii This dissertation is dedicated to my wife Sharon, who has stood by my side and supported me while writing. I also dedicate this work to my family, who have encouraged me to pursue my love of the stars and whose advice and support through the years have been essential. iv v Acknowledgements Many thanks go to Keith Matthews, whose help and advice have been essential in construction of my instrument. I would like to thank Michael Ireland and Ian McEwan for valuable discussions on instrumentation, polarimetry, and signal processing. I appreciate the help of the Palomar Obser- vatory staff, especially Bruce Baker, Karl Dunscombe, John Henning, Greg van Idsinga, and Steve Kunsman. Without their help, this instrument would literally not have gotten off the ground. I thank Shri Kulkarni, who inspired me to pursue instrumentation. I acknowledge David Stevenson for a valuable debate regarding condensation in a water-hydrogen mixture and Conner Wiktorowicz for his help in determining uncertainty along the photospheric adiabat. I would like to acknowledge funding from the Moore Foundation. This research has made use of the SIMBAD database, operated at CDS, Strasbourg, France. vi vii Abstract A novel technique for detecting light scattered by extrasolar planets is presented that has the poten- tial to constrain orbital inclination and planet mass. -
Spectropolarimetric Signatures of Earth-Like Extrasolar Planets
A&A 482, 989–1007 (2008) Astronomy DOI: 10.1051/0004-6361:20078358 & c ESO 2008 Astrophysics Spectropolarimetric signatures of Earth-like extrasolar planets D. M. Stam Aerospace Engineering Department, Technical University Delft, Kluyverweg 1, 2629 HS, Delft, The Netherlands SRON Netherlands Institute for Space Research, Sorbonnelaan 2, 3584 CA Utrecht, The Netherlands e-mail: [email protected] Received 26 July 2007 / Accepted 29 December 2007 ABSTRACT We present results of numerical simulations of flux F and degree of polarization P of light that is reflected by Earth–like extrasolar planets orbiting solar type stars. Our results are presented as functions of the wavelength (from 0.3 to 1.0 µm, with 0.001 µm spectral resolution) and as functions of the planetary phase angle. We use different surface coverages for our model planets, including vegeta- tion and a Fresnel reflecting ocean, and clear and cloudy atmospheres. Our adding-doubling radiative transfer algorithm, which fully includes multiple scattering and polarization, only handles horizontally homogeneous planets, so we simulate fluxes and polarization of horizontally inhomogeneous planets by weighting results obtained for homogeneous planets. Like F, P of the reflected starlight is shown to depend strongly on the phase angle, on the composition and structure of the planetary atmosphere, on the reflective properties of the underlying surface, and on the wavelength, in particular in wavelength regions with gaseous absorption bands. The sensitivity of P to a planet’s physical properties appears to be different than that of F. Combining flux with polarization observations thus makes for a strong tool for characterizing extrasolar planets.