The Detectability of Transit Signals from a Microlensed Source Star with Euclid
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Index Abulfeda crater chain (Moon), 97 Aphrodite Terra (Venus), 142, 143, 144, 145, 146 Acheron Fossae (Mars), 165 Apohele asteroids, 353–354 Achilles asteroids, 351 Apollinaris Patera (Mars), 168 achondrite meteorites, 360 Apollo asteroids, 346, 353, 354, 361, 371 Acidalia Planitia (Mars), 164 Apollo program, 86, 96, 97, 101, 102, 108–109, 110, 361 Adams, John Couch, 298 Apollo 8, 96 Adonis, 371 Apollo 11, 94, 110 Adrastea, 238, 241 Apollo 12, 96, 110 Aegaeon, 263 Apollo 14, 93, 110 Africa, 63, 73, 143 Apollo 15, 100, 103, 104, 110 Akatsuki spacecraft (see Venus Climate Orbiter) Apollo 16, 59, 96, 102, 103, 110 Akna Montes (Venus), 142 Apollo 17, 95, 99, 100, 102, 103, 110 Alabama, 62 Apollodorus crater (Mercury), 127 Alba Patera (Mars), 167 Apollo Lunar Surface Experiments Package (ALSEP), 110 Aldrin, Edwin (Buzz), 94 Apophis, 354, 355 Alexandria, 69 Appalachian mountains (Earth), 74, 270 Alfvén, Hannes, 35 Aqua, 56 Alfvén waves, 35–36, 43, 49 Arabia Terra (Mars), 177, 191, 200 Algeria, 358 arachnoids (see Venus) ALH 84001, 201, 204–205 Archimedes crater (Moon), 93, 106 Allan Hills, 109, 201 Arctic, 62, 67, 84, 186, 229 Allende meteorite, 359, 360 Arden Corona (Miranda), 291 Allen Telescope Array, 409 Arecibo Observatory, 114, 144, 341, 379, 380, 408, 409 Alpha Regio (Venus), 144, 148, 149 Ares Vallis (Mars), 179, 180, 199 Alphonsus crater (Moon), 99, 102 Argentina, 408 Alps (Moon), 93 Argyre Basin (Mars), 161, 162, 163, 166, 186 Amalthea, 236–237, 238, 239, 241 Ariadaeus Rille (Moon), 100, 102 Amazonis Planitia (Mars), 161 COPYRIGHTED -
Arxiv:Astro-Ph/0609369 V2 15 Sep 2006 Ahntnd,54 Ra Rnhr.N,Wsigo DC, Washington NW, Rd
Draft version September 18, 2006 – VERSION Accepted for publication in ApJ A Preprint typeset using LTEX style emulateapj v. 12/14/05 HAT-P-1b: A LARGE-RADIUS, LOW-DENSITY EXOPLANET TRANSITING ONE MEMBER OF A STELLAR BINARY† ⋆ G. A.´ Bakos1,2, R. W. Noyes1, G. Kovacs´ 3, D. W. Latham1, D. D. Sasselov1, G. Torres1, D. A. Fischer6, R. P. Stefanik1, B. Sato7, J. A. Johnson8, A. Pal´ 4,1, G. W. Marcy8, R. P. Butler9, G. A. Esquerdo1, K. Z. Stanek10, J. Laz´ ar´ 5, I. Papp5, P. Sari´ 5 & B. Sipocz˝ 4,1 Draft version September 18, 2006 – VERSION Accepted for publication in ApJ ABSTRACT Using small automated telescopes in Arizona and Hawaii, the HATNet project has detected an object transiting one member of the double star system ADS 16402. This system is a pair of G0 main-sequence stars with age about 3 Gyr at a distance of ∼139 pc and projected separation of ∼1550 AU. The transit signal has a period of 4.46529 days and depth of 0.015 mag. From follow-up photometry and spectroscopy, we find that the object is a “hot Jupiter” planet with mass about 0.53 MJ and radius ∼1.36 RJ traveling in an orbit with semimajor axis 0.055 AU and inclination about 85◦.9, thus transiting the star at impact parameter 0.74 of the stellar radius. Based on a data set spanning three years, ephemerides for the transit center are: TC = 2453984.397+ Ntr ∗ 4.46529. The planet, designated HAT-P-1b, appears to be at least as large in radius, and smaller in mean density, than any previously-known planet. -
Gaianir Combining Optical and Near-Infra-Red (NIR) Capabilities with Time-Delay-Integration (TDI) Sensors for a Future Gaia-Like Mission
Proposal title: GaiaNIR Combining optical and Near-Infra-Red (NIR) capabilities with Time-Delay-Integration (TDI) sensors for a future Gaia-like mission. PI: Dr. David Hobbs, Lund Observatory, Box 43, SE-221 00 Lund, Sweden. Email: [email protected]. Tel.: +46-46-22 21573 Core team members: The following minimum team is needed to initiate the project. D. Hobbs Lund Observatory, Sweden. A. Brown Leiden Observatory, Holland. A. Mora Aurora Technology B.V., Spain. C. Crowley HE Space Operations B.V., Spain. N. Hambly University of Edinburgh, UK. J. Portell Institut de Ciències del Cosmos, ICCUB-IEEC, Spain. C. Fabricius Institut de Ciències del Cosmos, ICCUB-IEEC, Spain. M. Davidson University of Edinburgh, UK. Proposal writers: See Appendix A. Other supporting scientists: See Appendix B and Appendix C. Senior science advisors: E. Høg Copenhagen University (Retired), Denmark. L. Lindegren Lund Observatory, Sweden. C. Jordi Institut de Ciències del Cosmos, ICCUB-IEEC, Spain. S. Klioner Lohrmann Observatory, Germany. F. Mignard Observatoire de la Côte d’Azur, France. arXiv:1609.07325v2 [astro-ph.IM] 22 May 2020 Fig. 1: Left is an IR image from the Two Micron All-Sky Survey (image G. Kopan, R. Hurt) while on the right an artist’s concept of the Gaia mission superimposed on an optical image, (Image ESA). Images not to scale. 1 1. Executive summary ESA recently called for new “Science Ideas” to be investigated in terms of feasibility and technological developments – for tech- nologies not yet sufficiently mature. These ideas may in the future become candidates for M or L class missions within the ESA Science Program. -
Astrophysics with New Horizons: Making the Most of a Generational Opportunity
Draft version October 3, 2018 Typeset using LATEX twocolumn style in AASTeX62 Astrophysics with New Horizons: Making the Most of a Generational Opportunity Michael Zemcov,1, 2 Iair Arcavi,3, 4 Richard Arendt,5 Etienne Bachelet,6 Ranga Ram Chary,7 Asantha Cooray,8 Diana Dragomir,9 Richard Conn Henry,10 Carey Lisse,11 Shuji Matsuura,12, 13 Jayant Murthy,14 Chi Nguyen,1 Andrew R. Poppe,15 Rachel Street,6 and Michael Werner16 1Center for Detectors, School of Physics and Astronomy, Rochester Institute of Technology, Rochester, NY 14623, USA 2Jet Propulsion Laboratory, 4800 Oak Grove Drive, Pasadena, CA 91109, USA 3Einstein Fellow at the Department of Physics, University of California, Santa Barbara, CA 93106-9530, USA 4Las Cumbres Observatory, 6740 Cortona Drive, Suite 102, Goleta, CA 93117-5575, USA 5CRESST II/UMBC Observational Cosmology Laboratory, Code 665, Goddard Space Flight Center, 8800 Greenbelt Road, Greenbelt, MD 20771, USA 6Las Cumbres Observatory, 6740 Cortona Dr Ste 102, Goleta, CA 93117-5575, USA 7U. S. Planck Data Center, California Institute of Technology, 1200 East California Boulevard, Pasadena, CA 91125, USA 8Department of Physics and Astronomy, University of California, Irvine, CA 92697, USA 9NASA Hubble Fellow, Massachusetts Institute of Technology, Cambridge, MA 02139, USA 10Henry A. Rowland Department of Physics and Astronomy, The Johns Hopkins University, Baltimore, MD 21218, USA 11Planetary Exploration Group, Space Department, Johns Hopkins University Applied Physics Laboratory, 11100 Johns Hopkins Road, Laurel, MD -
EUCLID Mission Assessment Study
EUCLID Mission Assessment Study Executive Summary ESA Contract. No. 5856/08/F/VS September 2009 EUCLID– Mapping the Dark Universe EUCLID is a mission to study geometry and nature of the dark universe. It is a medium-class mission candidate within ESA's Cosmic Vision 2015– 2025 Plan for launch around 2017. EUCLID has been derived by ESA from DUNE and SPACE, two complementary Cosmic Vision proposals addressing questions on the origin and the constitution of the Universe. 70% Dark Energy The observational methods applied by EUCLID are shape and redshift measure- ments of galaxies and clusters of galaxies. To 4% Baryonic Matter this end EUCLID is equipped with 3 scientific instruments: 26% Dark Matter • Visible Imager (VIS) • Near-Infrared Photometer (NIP) • Near-Infrared Spectrograph (NIS) The EUCLID Mission Assessment Study is the industrial part of the EUCLID assessment phase. The study has been performed by Astrium from September 2008 to September 2009 and is intended for space segment definition and programmatic evaluation. The prime responsibility is with Astrium GmbH (Friedrichshafen, Germany) with support from Astrium SAS (Toulouse, France) and Astrium Ltd (Stevenage, UK). EUCLID Mission EUCLID shall observe 20.000 deg2 of the extragalactic sky at galactic latitudes |b|>30 deg. The sky is sampled in step & b>30° stare mode with instantaneous fields of about 0.5 deg2 . Nominally a strip of about 20 deg in latitude is scanned per day (corresponding to about 1 deg in longitude). galactic plane step 1 b<30° step 2 step 3 The sky is nominally observed along great circles in planes perpendicular to the Sun- spacecraft axis (SAA=0). -
Using the Microlensing Technique, Astronomers Discover an Earth-Like Planet Outside Our Solar System
S&TR July/August 2006 11 Using the microlensing technique, astronomers discover an Earth-like planet outside our solar system. OOKING out to the vastness of the L night sky, stargazers often ponder questions about the universe, many wondering if planets like ours can be found somewhere out there. But teasing out the details in astronomical data that point to a possible Earth-like planet is exceedingly difficult. To find an extrasolar planet—a planet that circles a star other than the Sun— astrophysicists have in the past searched for Doppler shifts, changes in the wavelength emitted by an object because of its motion. When an astronomical object moves toward an observer on Earth, the light it emits becomes higher in frequency and shifts to the blue end of the spectrum. When the object moves away from the observer, its light becomes lower in frequency and shifts to the red end. By measuring these changes in wavelength, astrophysicists can precisely calculate how quickly objects are moving toward or away from Earth. When This artist’s rendition shows the Earth-like extrasolar planet discovered in 2005. (Reprinted courtesy of the European Southern Observatory.) Lawrence Livermore National Laboratory 12 An Earth-Like Extrasolar Planet S&TR July/August 2006 a giant planet orbits a star, the planet’s About the New Planet we consider the number of stars out there,” gravitational pull on the star produces a According to Livermore astrophysicist Cook says, “the fact that we stumbled on small (meters-per-second) back-and-forth Kem Cook, OGLE-2005-BLG-290-Lb is a one small planet means that thousands Doppler shift in the star’s light. -
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. -
Joint UV Survey Telescope
S. Basa, Laboratoire d’Astrophysique de Marseille, France distant sample of SMBHs, which in turn, hold the greatest promise of extending the existing M-σ relation beyond current limitations by revealing dormant SMBHs in galactic nuclei [15,16]. Finally is the class of unknown transients for which we currently lack both predictions and detections. This class represents a significant area of discovery space that only a wide-field The transientand sensitivesky X-ray transient “machine” can uniquely explore. In the sections below, we outline the importance of extending our knowledge of known, predicted, and unknown X-ray transients, on par with the on-going ground-based technological efforts to advance our understanding of the dynamic sky at optical (LSST) and radio (SKA pathfinders) wavelengths. Sky is intrinsically variable!! • Hard X-ray monitoring instruments show a restless X-ray sky (Swift-BAT, INTEGRAL, MAXI).! ! distant sample of SMBHs, which in turn, hold the greatest promise of extending the existing ! M-σ relation beyond current limitations by revealing dormant SMBHs in galactic nuclei [15,16]. Finally is the class of unknown transients for which we currently lack both predictions and Time domain astronomy still in its infancy, but detections. This class represents a significant area of discovery space that only a wide-field and sensitive X-ray transient “machine” can uniquely explore. In the sections below, we outline theSoderberg et al. 2009 importance of extending our knowledge of known, predicted, and unknown X-ray should quickly evolve especially at optical (PTF, transients, on par with the on-going ground-based technological efforts to advance our understanding of the dynamic sky at optical (LSST) and radio (SKA pathfinders)EXPLORING wavelengths. -
NASA Program & Budget Update
NASA Update AAAC Meeting | June 15, 2020 Paul Hertz Director, Astrophysics Division Science Mission Directorate @PHertzNASA Outline • Celebrate Accomplishments § Science Highlights § Mission Milestones • Committed to Improving § Inspiring Future Leaders, Fellowships § R&A Initiative: Dual Anonymous Peer Review • Research Program Update § Research & Analysis § ROSES-2020 Updates, including COVID-19 impacts • Missions Program Update § COVID-19 impact § Operating Missions § Webb, Roman, Explorers • Planning for the Future § FY21 Budget Request § Project Artemis § Creating the Future 2 NASA Astrophysics Celebrate Accomplishments 3 SCIENCE Exoplanet Apparently Disappears HIGHLIGHT in the Latest Hubble Observations Released: April 20, 2020 • What do astronomers do when a planet they are studying suddenly seems to disappear from sight? o A team of researchers believe a full-grown planet never existed in the first place. o The missing-in-action planet was last seen orbiting the star Fomalhaut, just 25 light-years away. • Instead, researchers concluded that the Hubble Space Telescope was looking at an expanding cloud of very fine dust particles from two icy bodies that smashed into each other. • Hubble came along too late to witness the suspected collision, but may have captured its aftermath. o This happened in 2008, when astronomers announced that Hubble took its first image of a planet orbiting another star. Caption o The diminutive-looking object appeared as a dot next to a vast ring of icy debris encircling Fomalhaut. • Unlike other directly imaged exoplanets, however, nagging Credit: NASA, ESA, and A. Gáspár and G. Rieke (University of Arizona) puzzles arose with Fomalhaut b early on. Caption: This diagram simulates what astronomers, studying Hubble Space o The object was unusually bright in visible light, but did not Telescope observations, taken over several years, consider evidence for the have any detectable infrared heat signature. -
Meeting Program
A A S MEETING PROGRAM 211TH MEETING OF THE AMERICAN ASTRONOMICAL SOCIETY WITH THE HIGH ENERGY ASTROPHYSICS DIVISION (HEAD) AND THE HISTORICAL ASTRONOMY DIVISION (HAD) 7-11 JANUARY 2008 AUSTIN, TX All scientific session will be held at the: Austin Convention Center COUNCIL .......................... 2 500 East Cesar Chavez St. Austin, TX 78701 EXHIBITS ........................... 4 FURTHER IN GRATITUDE INFORMATION ............... 6 AAS Paper Sorters SCHEDULE ....................... 7 Rachel Akeson, David Bartlett, Elizabeth Barton, SUNDAY ........................17 Joan Centrella, Jun Cui, Susana Deustua, Tapasi Ghosh, Jennifer Grier, Joe Hahn, Hugh Harris, MONDAY .......................21 Chryssa Kouveliotou, John Martin, Kevin Marvel, Kristen Menou, Brian Patten, Robert Quimby, Chris Springob, Joe Tenn, Dirk Terrell, Dave TUESDAY .......................25 Thompson, Liese van Zee, and Amy Winebarger WEDNESDAY ................77 We would like to thank the THURSDAY ................. 143 following sponsors: FRIDAY ......................... 203 Elsevier Northrop Grumman SATURDAY .................. 241 Lockheed Martin The TABASGO Foundation AUTHOR INDEX ........ 242 AAS COUNCIL J. Craig Wheeler Univ. of Texas President (6/2006-6/2008) John P. Huchra Harvard-Smithsonian, President-Elect CfA (6/2007-6/2008) Paul Vanden Bout NRAO Vice-President (6/2005-6/2008) Robert W. O’Connell Univ. of Virginia Vice-President (6/2006-6/2009) Lee W. Hartman Univ. of Michigan Vice-President (6/2007-6/2010) John Graham CIW Secretary (6/2004-6/2010) OFFICERS Hervey (Peter) STScI Treasurer Stockman (6/2005-6/2008) Timothy F. Slater Univ. of Arizona Education Officer (6/2006-6/2009) Mike A’Hearn Univ. of Maryland Pub. Board Chair (6/2005-6/2008) Kevin Marvel AAS Executive Officer (6/2006-Present) Gary J. Ferland Univ. of Kentucky (6/2007-6/2008) Suzanne Hawley Univ. -
Cosmic Vision and Other Missions for Space Science in Europe 2015-2035
Cosmic Vision and other missions for Space Science in Europe 2015-2035 Athena Coustenis LESIA, Observatoire de Paris-Meudon Chair of the Solar System and Exploration Working Group of ESA Member of the Space Sciences Advisory Committee of ESA Cosmic Vision 2015 - 2025 The call The call for proposals for Cosmic Vision missions was issued in March 2007. This call was intended to find candidates for two medium-sized missions (M1, M2 class, launch around 2017) and one large mission (L1 class, launch around 2020). Fifty mission concept proposals were received in response to the first call. From these, five M-class and three L- class missions were selected by the SPC in October 2007 for assessment or feasibility studies. In July 2010, another call was issued, for a medium-size (M3) mission opportunity for a launch in 2022. Also about 50 proposals were received for M3 and 4 concepts were selected for further study. Folie Cosmic Vision 2015 - 2025 The COSMIC VISION “Grand Themes” 1. What are the conditions for planetary formation and the emergence of life ? 2. How does the Solar System work? 3. What are the physical fundamental laws of the Universe? 4. How did the Universe originate and what is it made of? 4 COSMIC VISION (2015-2025) Step 1 Proposal selection for assessment phase in October 2007 . 3 M missions concepts: Euclid, PLATO, Solar Orbiter . 3 L mission concepts: X-ray astronomy, Jupiter system science, gravitational wave observatory . 1 MoO being considered: European participation to SPICA Selection of Solar Orbiter as M1 and Euclid JUICE as M2 in 2011. -
Gravitational Microlensing by Exoplanets and Exomoons
INTERNATIONAL SPACE SCIENCE INSTITUTE SPATIUM Published by the Association Pro ISSI No. 45, May 2020 Gravitational Microlensing by Exoplanets and Exomoons 200216_Spatium_45_2020_(001_016).indd 1 16.05.20 11:11 Editorial Since Copernicus (1473–1543) was world view abruptly. They seemed not able to measure brightness not to be inhabited as previously Impressum variations of the stars due to Earth’s assumed, and life appeared not to revolutionary motion around the be a matter of course. Astrophys- Sun, he inferred that stars must be ics and interdisciplinary science ISSN 2297–5888 (Print) very far away from Earth. During recognised the very special condi- ISSN 2297–590X (Online) the 16th and 17th Centuries schol- tions required to create life. More- ars began gradually to realise that over, these conditions need to be Spatium the Universe, i.e., the sphere of very selective and restricting, de- Published by the fixed stars enclosing our Solar pending not only on physical and Association Pro ISSI System, might not be finite but chemical parameters but particu- infinite. Philosophical arguments larly on stable and stabilising hab- by Thomas Digges (1546–1595) or itable environments in space and Giordano Bruno (1548–1600) sup- on ground. ported this view. Galileo (1564– Today, the existence of extra-ter- Association Pro ISSI 1642) provided evidence from ob- restrial life seems to be quite likely Hallerstrasse 6, CH-3012 Bern servations of the Milky Way using for statistical reasons. However, it Phone +41 (0)31 631 48 96 his telescope. is very hard to find evidence from see In his Cosmotheoros posthumously bio-markers identified in exoplan- www.issibern.ch/pro-issi.html published in 1698, Christiaan Huy- etary spectra as long as it is not clear for the whole Spatium series gens (1629–1695) estimated the dis- what life actually is.