Sky Notes: 2013 August & September
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A Temperate Rocky Super-Earth Transiting a Nearby Cool Star Jason A
LETTER doi:10.1038/nature22055 A temperate rocky super-Earth transiting a nearby cool star Jason A. Dittmann1, Jonathan M. Irwin1, David Charbonneau1, Xavier Bonfils2,3, Nicola Astudillo-Defru4, Raphaëlle D. Haywood1, Zachory K. Berta-Thompson5, Elisabeth R. Newton6, Joseph E. Rodriguez1, Jennifer G. Winters1, Thiam-Guan Tan7, Jose-Manuel Almenara2,3,4, François Bouchy8, Xavier Delfosse2,3, Thierry Forveille2,3, Christophe Lovis4, Felipe Murgas2,3,9, Francesco Pepe4, Nuno C. Santos10,11, Stephane Udry4, Anaël Wünsche2,3, Gilbert A. Esquerdo1, David W. Latham1 & Courtney D. Dressing12 15 16,17 M dwarf stars, which have masses less than 60 per cent that of Ks magnitude and empirically determined stellar relationships , the Sun, make up 75 per cent of the population of the stars in the we estimate the stellar mass to be 14.6% that of the Sun and the stellar Galaxy1. The atmospheres of orbiting Earth-sized planets are radius to be 18.6% that of the Sun. We estimate the metal content of the observationally accessible via transmission spectroscopy when star to be approximately half that of the Sun ([Fe/H] = −0.24 ± 0.10; the planets pass in front of these stars2,3. Statistical results suggest 1σ error), and we measure the rotational period of the star to be that the nearest transiting Earth-sized planet in the liquid-water, 131 days from our long-term photometric monitoring (see Methods). habitable zone of an M dwarf star is probably around 10.5 parsecs On 15 September 2014 ut, MEarth-South identified a potential away4. A temperate planet has been discovered orbiting Proxima transit in progress around LHS 1140, and automatically commenced Centauri, the closest M dwarf5, but it probably does not transit and high-cadence follow-up observations (see Extended Data Fig. -
Observer's Handbook 1974
the OBSERVER’S HANDBOOK 1974 sixty- sixth year of publication the ROYAL ASTRONOMICAL SOCIETY of CANADA THE ROYAL ASTRONOMICAL SOCIETY OF CANADA Incorporated 1890 Federally Incorporated 1968 The National Office of the Society is located at 252 College Street, Toronto 130, Ontario; the business office, reading room and astronomical library are housed here. Membership is open to anyone interested in astronomy and applicants may affiliate with one of the eighteen Centres across Canada established in St. John’s, Halifax, Quebec, Montreal, Ottawa, Kingston, Hamilton, Niagara Falls, London, Windsor, Winnipeg, Saskatoon, Edmonton, Calgary, Vancouver, Victoria and Toronto, or join the National Society direct. Publications of the Society are free to members, and include the Jo u r n a l (6 issues per year) and the O bserver’s H a n d b o o k (published annually in November). Annual fees of $12.50 ($7.50 for full-time students) are payable October 1 and include the publications for the following calendar year. VISITING HOURS AT SOME CANADIAN OBSERVATORIES Burke-Gaffney Observatory, Saint Mary’s University, Halifax, Nova Scotia. October-April: Saturday evenings 7:00 p.m. May-September: Saturday evenings 9:00 p.m. David Dunlap Observatory, Richmond Hill, Ontario. Wednesday mornings throughout the year, 10:00 a.m. Saturday evenings, April through October (by reservations, tel. 884-2112). Dominion Astrophysical Observatory, Victoria, B.C. May-August: Daily, 9:15 a.m.-4:30 p.m. (Guide, Monday to Friday). Sept.-April: Monday to Friday, 9:15 a.m.-4:30 p.m. Public observing, Saturday evenings, April-October, inclusive. -
FY13 High-Level Deliverables
National Optical Astronomy Observatory Fiscal Year Annual Report for FY 2013 (1 October 2012 – 30 September 2013) Submitted to the National Science Foundation Pursuant to Cooperative Support Agreement No. AST-0950945 13 December 2013 Revised 18 September 2014 Contents NOAO MISSION PROFILE .................................................................................................... 1 1 EXECUTIVE SUMMARY ................................................................................................ 2 2 NOAO ACCOMPLISHMENTS ....................................................................................... 4 2.1 Achievements ..................................................................................................... 4 2.2 Status of Vision and Goals ................................................................................. 5 2.2.1 Status of FY13 High-Level Deliverables ............................................ 5 2.2.2 FY13 Planned vs. Actual Spending and Revenues .............................. 8 2.3 Challenges and Their Impacts ............................................................................ 9 3 SCIENTIFIC ACTIVITIES AND FINDINGS .............................................................. 11 3.1 Cerro Tololo Inter-American Observatory ....................................................... 11 3.2 Kitt Peak National Observatory ....................................................................... 14 3.3 Gemini Observatory ........................................................................................ -
Abstracts of Extreme Solar Systems 4 (Reykjavik, Iceland)
Abstracts of Extreme Solar Systems 4 (Reykjavik, Iceland) American Astronomical Society August, 2019 100 — New Discoveries scope (JWST), as well as other large ground-based and space-based telescopes coming online in the next 100.01 — Review of TESS’s First Year Survey and two decades. Future Plans The status of the TESS mission as it completes its first year of survey operations in July 2019 will bere- George Ricker1 viewed. The opportunities enabled by TESS’s unique 1 Kavli Institute, MIT (Cambridge, Massachusetts, United States) lunar-resonant orbit for an extended mission lasting more than a decade will also be presented. Successfully launched in April 2018, NASA’s Tran- siting Exoplanet Survey Satellite (TESS) is well on its way to discovering thousands of exoplanets in orbit 100.02 — The Gemini Planet Imager Exoplanet Sur- around the brightest stars in the sky. During its ini- vey: Giant Planet and Brown Dwarf Demographics tial two-year survey mission, TESS will monitor more from 10-100 AU than 200,000 bright stars in the solar neighborhood at Eric Nielsen1; Robert De Rosa1; Bruce Macintosh1; a two minute cadence for drops in brightness caused Jason Wang2; Jean-Baptiste Ruffio1; Eugene Chiang3; by planetary transits. This first-ever spaceborne all- Mark Marley4; Didier Saumon5; Dmitry Savransky6; sky transit survey is identifying planets ranging in Daniel Fabrycky7; Quinn Konopacky8; Jennifer size from Earth-sized to gas giants, orbiting a wide Patience9; Vanessa Bailey10 variety of host stars, from cool M dwarfs to hot O/B 1 KIPAC, Stanford University (Stanford, California, United States) giants. 2 Jet Propulsion Laboratory, California Institute of Technology TESS stars are typically 30–100 times brighter than (Pasadena, California, United States) those surveyed by the Kepler satellite; thus, TESS 3 Astronomy, California Institute of Technology (Pasadena, Califor- planets are proving far easier to characterize with nia, United States) follow-up observations than those from prior mis- 4 Astronomy, U.C. -
SIAC Newsletter October 2013
SOUTHEASTERN IOWA ASTRONOMY CLUB THE SIDEREAL TIMES OCTOBER 2013 A M EMBER SOCIETY OF THE ASTRONOMICAL LEAGUE CLUB OFFICERS : MINUTES SEPTEMBER 20, 2013 President Jim Hilkin called the meeting to is meeting night. Jim Hilkin gave an up- Executive Committee order with the following members in attend- date on the following maintenance President Jim Hilkin items: some additional dirt was added to Vice President Libby Snipes ance: Judy Smithson, Libby Snipes, Jim Treasurer Vicki Philabaum Wilt, Ray Reineke, Duane Gerling, Claus the east end of the berm to help block Secretary David Philabaum Benninghoven, Dave Philabaum, John Ton- headlights from cars coming from the Chief Observer David Philabaum ey, and Paul Sly. Vicki Philabaum conduct- beach and area E; the viburnum bushes Members-at-Large Claus Benninghoven ed a tour of the facility for a group from on the north side of the classroom were Duane Gerling Great River Christian School during the removed as they were getting too big for Blake Stumpf meeting. Libby moved to approve the the space; Jim has installed cabinet Board of Directors minutes as published, seconded by Jim Wilt, doors and created a storage area in the Chair Judy Hilkin motion passed. Jim Hilkin read the Treasur- Stone-Kelly dome; the new doors for Vice Chair Ray Reineke er's report from Vicki. Checks were written the Prugh-Carver Observatory are in, Secretary David Philabaum for the phone bill and to Ray for the new but there has been no word from SCC Members-at-Large David Martin about painting them so Barngrover's will Blake Stumpf motor for the Fecker telescope. -
Mein Erstes Teleskop 4
www.vds-astro.de ISSN 1615-0880 IV/2012 Nr. 43 Zeitschrift der Vereinigung der Sternfreunde e.V. Schwerpunktthema Mein erstes Sturm, Schnee und gute Laune Kometenbahn selbst bestimmt Sternwarten im Porträt Seite 40 Seite 65 Seite 100 Teleskop Editorial 1 Liebe Mitglieder, liebe Sternfreunde, zu unserem Schwerpunktthema in diesem Journal hätte jeder Sternfreund etwas beitragen können. Wer erinnert sich nicht an sein erstes (eigenes) Teleskop oder sogar an seine ersten Geh-(Seh-)versuche am gestirnten Himmel? Besonders das erste selbstgebaute Fernrohr wird immer einen herausragenden Platz beim Titelbild: Erbauer einnehmen. Lesen Sie, wie es anderen Sternguckern ergangen ist ... Jupiter und Ganymed am 26.09.2011 um 00:40 UT, aufgenommen am In ganz Deutschland konnten die Sternschnuppen des Perseiden-Stroms bei 20-Zoll-Newton (f/4) aus der Garten- bestem Wetter beobachtet werden. Zufällig traf sich der VdS-Vorstand fast voll- sternwarte der Familie Winterer in zählig genau zum Maximums-Wochende zu einer Sitzung und durfte so das Meitingen. Zur Bildgewinnung kam eine schöne Himmelsspektakel unter dem herrlichen Himmel der Lüneburger Heide DMK 21 AU618 von TheImagingSource anschauen, wunderbar und beindruckend! Schicken Sie uns doch Ihre Bilder der und ein Astronomik-RGB-Filtersatz II diesjährigen Perseiden zur Veröffentlichung im Journal für Astronomie! zum Einsatz. Die Bildsequenzen wurden mit FireCapture aufgenommen. Die Betreuung der Mitglieds-Sternwarten und -Vereine geht weiter, auch in Die Effek tivbrennweite lag bei 8.270 diesem Journal stellen sich wieder vier von ihnen vor. Überzeugen Sie sich selbst mm. Die Summenbilder der Kanäle von deren Angebot und planen Sie doch mal einen Besuch. Ab Spätherbst kann Rot, Grün und Blau wurden jeweils sich zusätzlich jeder Mitgliedsverein über eine Deutschlandkarte auf der VdS- einzeln mit AviStack gemittelt, für die Website vorstellen. -
Theia: Faint Objects in Motion Or the New Astrometry Frontier
Theia: Faint objects in motion or the new astrometry frontier The Theia Collaboration ∗ July 6, 2017 Abstract In the context of the ESA M5 (medium mission) call we proposed a new satellite mission, Theia, based on rel- ative astrometry and extreme precision to study the motion of very faint objects in the Universe. Theia is primarily designed to study the local dark matter properties, the existence of Earth-like exoplanets in our nearest star systems and the physics of compact objects. Furthermore, about 15 % of the mission time was dedicated to an open obser- vatory for the wider community to propose complementary science cases. With its unique metrology system and “point and stare” strategy, Theia’s precision would have reached the sub micro-arcsecond level. This is about 1000 times better than ESA/Gaia’s accuracy for the brightest objects and represents a factor 10-30 improvement for the faintest stars (depending on the exact observational program). In the version submitted to ESA, we proposed an optical (350-1000nm) on-axis TMA telescope. Due to ESA Technology readiness level, the camera’s focal plane would have been made of CCD detectors but we anticipated an upgrade with CMOS detectors. Photometric mea- surements would have been performed during slew time and stabilisation phases needed for reaching the required astrometric precision. Authors Management team: Céline Boehm (PI, Durham University - Ogden Centre, UK), Alberto Krone-Martins (co-PI, Universidade de Lisboa - CENTRA/SIM, Portugal) and, in alphabetical order, António Amorim -
Ephemerides Astronomicae. Anni...Ad Meridianum Mediolanensem
Informazioni su questo libro Si tratta della copia digitale di un libro che per generazioni è stato conservata negli scaffali di una biblioteca prima di essere digitalizzato da Google nell’ambito del progetto volto a rendere disponibili online i libri di tutto il mondo. Ha sopravvissuto abbastanza per non essere più protetto dai diritti di copyright e diventare di pubblico dominio. Un libro di pubblico dominio è un libro che non è mai stato protetto dal copyright o i cui termini legali di copyright sono scaduti. La classificazione di un libro come di pubblico dominio può variare da paese a paese. I libri di pubblico dominio sono l’anello di congiunzione con il passato, rappresentano un patrimonio storico, culturale e di conoscenza spesso difficile da scoprire. Commenti, note e altre annotazioni a margine presenti nel volume originale compariranno in questo file, come testimonianza del lungo viaggio percorso dal libro, dall’editore originale alla biblioteca, per giungere fino a te. Linee guide per l’utilizzo Google è orgoglioso di essere il partner delle biblioteche per digitalizzare i materiali di pubblico dominio e renderli universalmente disponibili. I libri di pubblico dominio appartengono al pubblico e noi ne siamo solamente i custodi. Tuttavia questo lavoro è oneroso, pertanto, per poter continuare ad offrire questo servizio abbiamo preso alcune iniziative per impedire l’utilizzo illecito da parte di soggetti commerciali, compresa l’imposizione di restrizioni sull’invio di query automatizzate. Inoltre ti chiediamo di: + Non fare un uso commerciale di questi file Abbiamo concepito Google Ricerca Libri per l’uso da parte dei singoli utenti privati e ti chiediamo di utilizzare questi file per uso personale e non a fini commerciali. -
Planet Searching from Ground and Space
Planet Searching from Ground and Space Olivier Guyon Japanese Astrobiology Center, National Institutes for Natural Sciences (NINS) Subaru Telescope, National Astronomical Observatory of Japan (NINS) University of Arizona Breakthrough Watch committee chair June 8, 2017 Perspectives on O/IR Astronomy in the Mid-2020s Outline 1. Current status of exoplanet research 2. Finding the nearest habitable planets 3. Characterizing exoplanets 4. Breakthrough Watch and Starshot initiatives 5. Subaru Telescope instrumentation, Japan/US collaboration toward TMT 6. Recommendations 1. Current Status of Exoplanet Research 1. Current Status of Exoplanet Research 3,500 confirmed planets (as of June 2017) Most identified by Jupiter two techniques: Radial Velocity with Earth ground-based telescopes Transit (most with NASA Kepler mission) Strong observational bias towards short period and high mass (lower right corner) 1. Current Status of Exoplanet Research Key statistical findings Hot Jupiters, P < 10 day, M > 0.1 Jupiter Planetary systems are common occurrence rate ~1% 23 systems with > 5 planets Most frequent around F, G stars (no analog in our solar system) credits: NASA/CXC/M. Weiss 7-planet Trappist-1 system, credit: NASA-JPL Earth-size rocky planets are ~10% of Sun-like stars and ~50% abundant of M-type stars have potentially habitable planets credits: NASA Ames/SETI Institute/JPL-Caltech Dressing & Charbonneau 2013 1. Current Status of Exoplanet Research Spectacular discoveries around M stars Trappist-1 system 7 planets ~3 in hab zone likely rocky 40 ly away Proxima Cen b planet Possibly habitable Closest star to our solar system Faint red M-type star 1. Current Status of Exoplanet Research Spectroscopic characterization limited to Giant young planets or close-in planets For most planets, only Mass, radius and orbit are constrained HR 8799 d planet (direct imaging) Currie, Burrows et al. -
Physics of Stellar Coronae
Physics of Stellar Coronae Manuel G¨udel Paul Scherrer Institut, W¨urenlingen and Villigen, CH-5232 Villigen PSI, Switzerland [email protected] 1 Introduction For the plasma physicist, the solar corona offers an outstanding example of a space plasma, and surely one that deserves a lifetime of study. Not only can we observe the solar corona on scales of a few hundred kilometers and monitor its changes in the course of seconds to minutes, we also have a wide range of detailed diagnostics at our disposal that provide immediate access to the prevalent physical processes. Yet, solar physics offers a rich field of unsolved plasma-physical problems. How is the coronal plasma continuously heated to > 106 K? How and where are high-energy particles episodically accelerated? What is the internal dy- namics of plasma in magnetic loops? What is the initial trigger of a coronal flare? How does the corona link to the solar wind, and how and where is the latter accelerated? How is plasma transported into the solar corona? Why, then, study stellar coronae that remain spatially unresolved in X- rays and are only marginally resolved at radio wavelengths, objects that require exposure times of several hours before approximate measurements of the ensemble of plasma structures can be obtained? There are many reasons. In the context of the solar-stellar connection, stellar X-ray astronomy has introduced a range of stellar rotation periods, gravities, masses, and ages into the debate on the magnetic dynamo. Coronal magnetic structures and heating mechanisms may vary together with varia- tions of these parameters. -
Faint Objects in Motion: the New Frontier of High Precision Astrometry
White paper for the Voyage 2050 long-term plan in the ESA Science Programme Faint objects in motion: the new frontier of high precision astrometry Contact Scientist: Fabien Malbet Institut de Planétologie et d’Astrophysique de Grenoble (IPAG) Université Grenoble Alpes, CS 40700, F-38058 Grenoble cedex 9, France Email: [email protected], Phone: +33 476 63 58 33 version 20190805 Faint objects in motion : the new frontier of high precision astrometry Faint objects in motion: the new on the most critical questions of cosmology, astron- frontier of high precision astrometry omy and particle physics. Sky survey telescopes and powerful targeted telesco- 1.1 Dark matter pes play complementary roles in astronomy. In order to The current hypothesis of cold dark matter (CDM) ur- investigate the nature and characteristics of the mo- gently needs verification. Dark matter (DM) is essential tions of very faint objects, a flexibly-pointed instrument to the L + CDM cosmological model (LCDM), which suc- capable of high astrometric accuracy is an ideal comple- cessfully describes the large-scale distribution of galax- ment to current astrometric surveys and a unique tool for ies and the angular fluctuations of the Cosmic Microwave precision astrophysics. Such a space-based mission Background, as confirmed by the ESA / Planck mission. will push the frontier of precision astrometry from ev- Dark matter is the dominant form of matter (∼ 85%) in idence of earth-massed habitable worlds around the the Universe, and ensures the formation and stability of nearest starts, and also into distant Milky way objects enmeshed galaxies and clusters of galaxies. -
Gaia FGK Benchmark Stars: Effective Temperatures and Surface Gravities U
Astronomy & Astrophysics manuscript no. Heiter_etal_Benchmarkstars_LE c ESO 2018 September 25, 2018 Gaia FGK benchmark stars: Effective temperatures and surface gravities U. Heiter1, P. Jofré2, B. Gustafsson1; 4, A. J. Korn1, C. Soubiran3, and F. Thévenin5 1 Institutionen för fysik och astronomi, Uppsala universitet, Box 516, 751 20 Uppsala, Sweden e-mail: [email protected] 2 Institute of Astronomy, University of Cambridge, Madingley Rd, Cambridge, CB3 0HA, U.K. 3 Univ. Bordeaux, CNRS, LAB, UMR 5804, 33270, Floirac, France 4 Nordita, Roslagstullsbacken 23, 106 91, Stockholm, Sweden 5 Université de Nice Sophia Antipolis, CNRS (UMR7293), Observatoire de la Côte d’Azur, CS 34229, 06304, Nice Cedex 4, France Received / Accepted ABSTRACT Context. In the era of large Galactic stellar surveys, carefully calibrating and validating the data sets has become an important and integral part of the data analysis. Moreover, new generations of stellar atmosphere models and spectral line formation computations need to be subjected to benchmark tests to assess any progress in predicting stellar properties. Aims. We focus on cool stars and aim at establishing a sample of 34 Gaia FGK benchmark stars with a range of different metallicities. The goal was to determine the effective temperature and the surface gravity independently of spectroscopy and atmospheric models as far as possible. Most of the selected stars have been subjected to frequent spectroscopic investigations in the past, and almost all of them have previously been used as reference, calibration, or test objects. Methods. Fundamental determinations of Teff and log g were obtained in a systematic way from a compilation of angular diameter measurements and bolometric fluxes and from a homogeneous mass determination based on stellar evolution models.