Corot 223992193: a New, Low-Mass, Pre-Main Sequence Eclipsing Binary with Evidence of a Circumbinary Disk⋆
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Asteroseismology with Corot, Kepler, K2 and TESS: Impact on Galactic Archaeology Talk Miglio’S
Asteroseismology with CoRoT, Kepler, K2 and TESS: impact on Galactic Archaeology talk Miglio’s CRISTINA CHIAPPINI Leibniz-Institut fuer Astrophysik Potsdam PLATO PIC, Padova 09/2019 AsteroseismologyPlato as it is : a Legacy with CoRoT Mission, Kepler for Galactic, K2 and TESS: impactArchaeology on Galactic Archaeology talk Miglio’s CRISTINA CHIAPPINI Leibniz-Institut fuer Astrophysik Potsdam PLATO PIC, Padova 09/2019 Galactic Archaeology strives to reconstruct the past history of the Milky Way from the present day kinematical and chemical information. Why is it Challenging ? • Complex mix of populations with large overlaps in parameter space (such as Velocities, Metallicities, and Ages) & small volume sampled by current data • Stars move away from their birth places (migrate radially, or even vertically via mergers/interactions of the MW with other Galaxies). • Many are the sources of migration! • Most of information was confined to a small volume Miglio, Chiappini et al. 2017 Key: VOLUME COVERAGE & AGES Chiappini et al. 2018 IAU 334 Quantifying the impact of radial migration The Rbirth mix ! Stars that today (R_now) are in the green bins, came from different R0=birth Radial Migration Sources = bar/spirals + mergers + Inside-out formation (gas accretion) GalacJc Center Z Sun R Outer Disk R = distance from GC Minchev, Chiappini, MarJg 2013, 2014 - MCM I + II A&A A&A 558 id A09, A&A 572, id A92 Two ways to expand volume for GA • Gaia + complementary photometric information (but no ages for far away stars) – also useful for PIC! • Asteroseismology of RGs (with ages!) - also useful for core science PLATO (miglio’s talk) The properties at different places in the disk: AMR CoRoT, Gaia+, K2 + APOGEE Kepler, TESS, K2, Gaia CoRoT, Gaia+, K2 + APOGEE PLATO + 4MOST? Predicon: AMR Scatter increases towards outer regions Age scatter increasestowars outer regions ExtracGng the best froM GaiaDR2 - Anders et al. -
Spring Semester 2021 (F21) 1 January 2021 Until 30 June 2021
Centro Astronomico´ Hispano-Aleman´ (CAHA) Call for proposals at the Calar Alto 2.2 & 3.5 meter telescopes Spring semester 2021 (F21) 1 January 2021 until 30 June 2021 DEADLINE: October 15th, 2020 23h59m59s (CEST) at the latest Earliest date for submission: September 17th, 2020 Calar Alto, September 16th, 2020. Contact: [email protected] Contents 1 Applications for observing time at Calar Alto4 1.1 General information...........................4 1.2 Spanish open time at the CAHA 2.2- and 3.5-m telescopes......4 1.3 Proposals from PIs in Europe but out of Spain.............4 1.4 Proposals from non-European PIs...................4 1.5 Visitor and service observing modes..................5 1.5.1 Visitor mode..........................5 1.5.2 Service mode..........................5 1.6 Ongoing surveys............................6 1.6.1 On the 3.5-m telescope.....................6 1.6.2 On the 2.2-m telescope.....................6 2 Important to notice6 2.1 No visits during the COVID-19 pandemic...............6 2.2 CAFE´ ..................................7 2.3 PANIC..................................7 3 How to write a proposal7 3.1 Calar Alto instrument pages......................8 3.1.1 Instruments offered on the 3.5-m telescope..........8 3.1.2 Instruments offered on the 2.2-m telescope..........8 3.2 Science categories of proposals.....................9 3.3 Types of proposal............................9 3.3.1 Re-submitted applications...................9 3.3.2 PhD thesis projects....................... 10 3.3.3 Long term or large projects................... 10 3.3.4 Testing new instruments.................... 10 3.3.5 Visitor instruments....................... 11 3.3.6 Multiple-instrument proposals................ -
Multiple Star Systems Observed with Corot and Kepler
Multiple star systems observed with CoRoT and Kepler John Southworth Astrophysics Group, Keele University, Staffordshire, ST5 5BG, UK Abstract. The CoRoT and Kepler satellites were the first space platforms designed to perform high-precision photometry for a large number of stars. Multiple systems dis- play a wide variety of photometric variability, making them natural benefactors of these missions. I review the work arising from CoRoT and Kepler observations of multiple sys- tems, with particular emphasis on eclipsing binaries containing giant stars, pulsators, triple eclipses and/or low-mass stars. Many more results remain untapped in the data archives of these missions, and the future holds the promise of K2, TESS and PLATO. 1 Introduction The CoRoT and Kepler satellites represent the first generation of astronomical space missions capable of large-scale photometric surveys. The large quantity – and exquisite quality – of the data they pro- vided is in the process of revolutionising stellar and planetary astrophysics. In this review I highlight the immense variety of the scientific results from these concurrent missions, as well as the context provided by their precursors and implications for their successors. CoRoT was led by CNES and ESA, launched on 2006/12/27,and retired in June 2013 after an irre- trievable computer failure in November 2012. It performed 24 observing runs, each lasting between 21 and 152days, with a field of viewof 2×1.3◦ ×1.3◦, obtaining light curves of 163000 stars [42]. Kepler was a NASA mission, launched on 2009/03/07and suffering a critical pointing failure on 2013/05/11. It observed the same 105deg2 sky area for its full mission duration, obtaining high-precision light curves of approximately 191000 stars. -
Data Mining in the Spanish Virtual Observatory. Applications to Corot and Gaia
Highlights of Spanish Astrophysics VI, Proceedings of the IX Scientific Meeting of the Spanish Astronomical Society held on September 13 - 17, 2010, in Madrid, Spain. M. R. Zapatero Osorio et al. (eds.) Data mining in the Spanish Virtual Observatory. Applications to Corot and Gaia. Mauro L´opez del Fresno1, Enrique Solano M´arquez1, and Luis Manuel Sarro Baro2 1 Spanish VO. Dep. Astrof´ısica. CAB (INTA-CSIC). P.O. Box 78, 28691 Villanueva de la Ca´nada, Madrid (Spain) 2 Departamento de Inteligencia Artificial. ETSI Inform´atica.UNED. Spain Abstract Manual methods for handling data are impractical for modern space missions due to the huge amount of data they provide to the scientific community. Data mining, understood as a set of methods and algorithms that allows us to recover automatically non trivial knowledge from datasets, are required. Gaia and Corot are just a two examples of actual missions that benefits the use of data mining. In this article we present a brief summary of some data mining methods and the main results obtained for Corot, as well as a description of the future variable star classification system that it is being developed for the Gaia mission. 1 Introduction Data in Astronomy is growing almost exponentially. Whereas projects like VISTA are pro- viding more than 100 terabytes of data per year, future initiatives like LSST (to be operative in 2014) and SKY (foreseen for 2024) will reach the petabyte level. It is, thus, impossible a manual approach to process the data returned by these surveys. It is impossible a manual approach to process the data returned by these surveys. -
Photometry of Be Stars in the Vicinity of COROT Primary Targets for Asteroseismology
Comm. in Asteroseismology Vol. 143, 2003 Photometry of Be stars in the vicinity of COROT primary targets for asteroseismology J. Guti´errez-Soto1, J. Fabregat1, J. Suso2, A.M. Hubert3, M. Floquet3 and R. Garrido4 1 Observatori Astron`omic, Universitat de Val`encia 2 Instituto Ciencia de los Materiales, Universitat de Val`encia 3GEPI, Observatoire de Paris-Meudon 4Instituto de Astrof´ısica de Andaluc´ıa Abstract We present differential photometry of Be stars close to potential COROT pri- mary targets for asteroseismology. Several stars are found to be short pe- riod variables. We propose them to be considered as secondary targets in the COROT asteroseismology fields. Introduction The observation of classical Be stars by COROT will provide important keys to understand the physics of these objects and the nature of the Be phenomenon. In particular, the detection of photospheric multiperiodicity will confirm the presence of non radial pulsations (nrp) as the origin of the short term variability. COROT observations will allow the study of the beat phenomenon of nrp modes and its relation with recurrent outbursts and the building of the circumstellar disc. Our group is proposing the observation of Be stars as secondary targets for the asteroseismology fields. A sample of stars in the vicinity of the main target candidates is under study for this purpose. Hubert et al. (2001, 2003) presented the selected objects and performed a study of their short term variability using Hipparcos photometric data. We have obtained new ground based photometry with a more suitable time sampling to further characterize their variability. 2 Photometry of Be stars in the vicinity of COROT primary targets for asteroseismology Observations and data analysis Observations were done at the 0.9 m telescope of the Observatorio de Sierra Nevada (Granada, Spain). -
2014 Science with the Hubble Space
Beyond HST: The Universe in High-Definition – UVOIR Space Astronomy in 2030 Julianne Dalcanton & Marc Postman Science with HST IV Meeting Rome, Italy March 18, 2014 Long History of Large Space UVOIR Telescope Concepts • VLST – 10m-16m concept (ca. 1989) • SUVO – 4m concept (ca. 1998-1999) • Workshop on 10m - 30m VLST (2003) • MUST – 10m concept (ca. 2004-2005) • ATLAST – 8m-16m concepts (ca. 2008-2010) • EUVO – European 8m concept (ca. 2013) • Modular Assembled 20m concept (ca. 2013) Scientifically compelling for over 2 decades! (Average Aperture Diameter – 13.5 meters) “Can we find another planet like Earth orbiting a nearby star? To find such a planet would complete the revolution, started by Copernicus nearly 500 years ago, that displaced the Earth as the center of the universe… The observational challenge is great but armed with new technologies… astronomers are poised to rise to it.” - U.S. 2010 Astronomy Decadal Review This is a question whose answer is sought by all of humanity and the search will demand international cooperation. The path has been laid ! for characterizing Earth 2.0 Kepler Hubble Spitzer CoRoT Ground-based Coronagraphs Gaia WFIRST 30-m class telescopes TESS JWST PLATO !"#$%&'('$)*+%&'($,)(%&$+-%$%&'('./$ Thick Atmosphere Methane Oxygen Fraction with terrestrial planets = !Earth FractionWater with detectable biosignature = fBio OpticalIf : ! Near-Infrared $ f ~ 1 then D ~ 4m Earth Bio0'12'($('#-2%#$ 8-meterTel 16-meter The signature of life is encoded inf the < 1 then D 8m spectrum! Earthof the Earth$ Bio $ tel ~ 70 !Earth $ fBio << 1 then DTel ~ 16m a > 12 Earths $ 60 50 40 30 # 4 Earths 20 4-meter 10 of total integration time of total integration time 0 Above: Distribution of all FGK stars within 45 pc of the Sun Number of Exo-Earths in 1 year 2-m 4-m 8-m 16-m where a R=70 spectrum of an Earth-twin could be acquired Telescope Size in <500 ksec shown as a function of telescope aperture. -
Effective Aperture 3.6–4.9 M) 4.7 M 186″ Segmented, MMT (6×1.8 M) F
Effective Effective Mirror type Name Site Built aperture aperture (m) (in) 10.4 m 409″ Segmented, Gran Telescopio Roque de los Muchachos 2006/9 36 Canarias (GTC) Obs., Canary Islands, Spain 10 m 394″ Segmented, Keck 1 Mauna Kea Observatories, 1993 36 Hawaii, USA 10 m 394″ Segmented, Keck 2 Mauna Kea Observatories, 1996 36 Hawaii, USA 9.8 m 386″ Segmented, Southern African South African Astronomical 2005 91 Large Telescope Obs., Northern Cape, South (SALT) Africa 9.2 m 362″ Segmented, Hobby-Eberly McDonald Observatory, 1997 91 Telescope (HET) Texas, USA (11 m × 9.8 m mirror) 8.4 m×2 330″×2 Multiple Large Binocular Mount Graham 2004 (can use mirror, 2 Telescope (LBT) Internationals Obs., Phased- Arizona array optics for combined 11.9 m[2]) 8.2 m 323″ Single Subaru (JNLT) Mauna Kea Observatories, 1999 Hawaii, USA 8.2 m 323″ Single VLT UT1 (Antu) Paranal Observatory, 1998 Antofagasta Region, Chile 8.2 m 323″ Single VLT UT2 (Kueyen) Paranal Observatory, 1999 Antofagasta Region, Chile 8.2 m 323″ Single VLT UT3 (Melipal) Paranal Observatory, 2000 Antofagasta Region, Chile 8.2 m 323″ Single VLT UT4 (Yepun) Paranal Observatory, 2001 Antofagasta Region, Chile 8.1 m 318″ Single Gemini North Mauna Kea Observatories, 1999 (Gillett) Hawaii, USA 8.1 m 318″ Single Gemini South Cerro Pachón (CTIO), 2001 Coquimbo Region, Chile 6.5 m 256″ Honeycomb Magellan 1 Las Campanas Obs., 2000 (Walter Baade) Coquimbo Region, Chile 6.5 m 256″ Honeycomb Magellan 2 Las Campanas Obs., 2002 (Landon Clay) Coquimbo Region, Chile 6.5 m 256″ Single MMT (1 x 6.5 M1) F. -
Advanced Technologies for Future Space Telescopes and Instruments
Advanced Technologies for Future Space Telescopes and Instruments - A sample of upcoming astronomy missions - Interferometry in space (Darwin) - Very large telescopes in orbit (XEUS) - Future space telescope concepts (TPF) Dr. Ph. Gondoin (ESA) IR and visible astronomy missions (ESA Cosmic Vision – NASA Origin programs) DARWIN TPF GAIA SIM Herschel SIRTF Planck Eddington Kepler JWST Corot 1 GAIA Science Objective: Understanding the structure and evolution of the Galaxy PayloadGAIA payload • 2 astrometric telescopes: • Separated by 106o • SiC mirrors (1.4 m × 0.5 m) • Large focal plane (TDI operating CCDs) • 1 additional telescope equipped with: • Medium-band photometer • Radial-velocity spectrometer 2 Technology requirements for GAIA (applicable to many future space missions) • Large focal plane assemblies: – 250 CCDs per astrometry field, 3 side buttable, small pixel (9 µm), high perf. CCDs ( large CTE, low-noise, wide size, high QE), TDI operation • Ultra-stable telescope structure and optical bench: • Light weight mirror elements: – SiC mirrors (highly aspherized for good off-axis performance) Large SiC mirror for space telescopes (Boostec) ESA Herschell telescope: 1.35 m prototype 3.5 m brazed flight model (12 petals) 3 James Webb Space Telescope (JWST) Mirror Actuators Beryllium Mirrors Mirror System AMSD SBMD Wavefront Sensing and Control, Mirror Phasing Secondary mirror uses six actuators In a hexapod configuration Primary mirror segments attached to backplane using actuators in a three-point kinematic mount NIRSpec: a Multi-object -
Kepler Press
National Aeronautics and Space Administration PRESS KIT/FEBRUARY 2009 Kepler: NASA’s First Mission Capable of Finding Earth-Size Planets www.nasa.gov Media Contacts J.D. Harrington Policy/Program Management 202-358-5241 NASA Headquarters [email protected] Washington 202-262-7048 (cell) Michael Mewhinney Science 650-604-3937 NASA Ames Research Center [email protected] Moffett Field, Calif. 650-207-1323 (cell) Whitney Clavin Spacecraft/Project Management 818-354-4673 Jet Propulsion Laboratory [email protected] Pasadena, Calif. 818-458-9008 (cell) George Diller Launch Operations 321-867-2468 Kennedy Space Center, Fla. [email protected] 321-431-4908 (cell) Roz Brown Spacecraft 303-533-6059. Ball Aerospace & Technologies Corp. [email protected] Boulder, Colo. 720-581-3135 (cell) Mike Rein Delta II Launch Vehicle 321-730-5646 United Launch Alliance [email protected] Cape Canaveral Air Force Station, Fla. 321-693-6250 (cell) Contents Media Services Information .......................................................................................................................... 5 Quick Facts ................................................................................................................................................... 7 NASA’s Search for Habitable Planets ............................................................................................................ 8 Scientific Goals and Objectives ................................................................................................................. -
A Tale of Two Exoplanets: the Inflated Atmospheres of the Hot Jupiters HD 189733 B and Corot-2 B
A Tale of Two Exoplanets: the Inflated Atmospheres of the Hot Jupiters HD 189733 b and CoRoT-2 b K. Poppenhaeger1,3, S.J. Wolk1, J.H.M.M. Schmitt2 1Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA 2Hamburger Sternwarte, Gojenbergsweg 112, 21029 Hamburg, Germany 3NASA Sagan Fellow Abstract. Planets in close orbits around their host stars are subject to strong irradiation. High-energy irradiation, originating from the stellar corona and chromosphere, is mainly responsible for the evaporation of exoplanetary atmospheres. We have conducted mul- tiple X-ray observations of transiting exoplanets in short orbits to determine the extent and heating of their outer planetary atmospheres. In the case of HD 189733 b, we find a surprisingly deep transit profile in X-rays, indicating an atmosphere extending out to 1.75 optical planetary radii. The X-ray opacity of those high-altitude layers points towards large densities or high metallicity. We preliminarily report on observations of the Hot Jupiter CoRoT-2 b from our Large Program with XMM-Newton, which was conducted recently. In addition, we present results on how exoplanets may alter the evolution of stellar activity through tidal interaction. 1. Exoplanetary transits in X-rays Close-in exoplanets are expected to harbor extended atmospheres and in some cases lose mass through atmospheric evaporation, driven by X-ray and extreme UV emission from the host star (Lecavelier des Etangs et al. 2004; Murray-Clay et al. 2009, for exmaple). Direct observational evidence for such extended atmospheres has been collected at UV wavelengths (Vidal-Madjar et al. -
Lessons from COROT, M. Ollivier
CoRoT&in&Brief& • «&Small&»&CNES&Mission&+&Belgium&+&Germany&+& Austria&+&Spain&+&Brasil+&ESA& Lessons&from&CoRoT& • 3rd&PROTEUS&mission&(minisat)& Marc&Ollivier& • DouBle&program&:&asteroseismology&and&search&for& Ins5tut&d’Astrophysique&Spa5ale&d’Orsay& planetary&transits& • Launch&:&27&Dec&2006&:&Soyouz&Starsem&2B&from& LESIA&–&OBservatoire&de&Paris& Baïkonour& & • Circular&polar&orbit&at&896&km&& & • Loss&of&detec5on&chain&2&in&March&2009& • Loss&of&detec5on&chain&1&in&Nov&2012& & • End&of&the&mission&june&2013& • End&of&opera5ons&june&2014& CHEOPS&Workshop&_&Madrid&_&18&june&2015& 2& The&CoRoT&oBservatory& The&CoRoT&satellite& CHEOPS&Workshop&_&Madrid&_&18&june&2015& 3& CHEOPS&Workshop&_&Madrid&_&18&june&2015& 4& &&&&&The&focal&plane& CoRoT&:&OBserva5on&and&orBital& constraints& 1.3 ° secondary targets (≤ 9) * * • faint stars (11-16) main target (≤ 6) * • • * * 12000 targets 10 targets! sampling 8.5 min sampling 1 s * (32 s.) to 32s * • * * • * field of view Seismology field Exoplanet field highly defocussed On focus + bi-prism CHEOPS&Workshop&_&Madrid&_&18&june&2015& 6& CHEOPS&Workshop&_&Madrid&_&18&june&2015& 5& Modeling&of&op5cal&chain& 1st&lesson&:&it&is&necessary&to& understand&as&much&as&possiBle& how&the&instrument&works&and& responds& CHEOPS&Workshop&_&Madrid&_&18&june&2015& 7& CHEOPS&Workshop&_&Madrid&_&18&june&2015& 8& Modeling&of&op5cal&chain& PSFs&Huygens&at&INFA2&point& Measured&PSFs& Computed&PSFs& Defoc¶bole&=& 0mm& Defoc¶bole&=& +10mm& CHEOPS&Workshop&_&Madrid&_&18&june&2015& 9& CHEOPS&Workshop&_&Madrid&_&18&june&2015& -
Distant Ekos: 2007 PS45, 2008 CS190 and 4 New Centaur/SDO Discoveries: 2008 FC76, 2004 VP112, 2005 UN524, 2008 CT190
Issue No. 58 May 2008 s DISTANT EKO di The Kuiper Belt Electronic Newsletter r Edited by: Joel Wm. Parker [email protected] www.boulder.swri.edu/ekonews CONTENTS News & Announcements ................................. 2 Abstracts of 10 Accepted Papers ........................ 3 Titles of 2 Submitted Papers ........................... 9 Conference Information .............................. ....9 Newsletter Information .............................. 10 1 NEWS & ANNOUNCEMENTS There were 2 new TNO discoveries announced since the previous issue of Distant EKOs: 2007 PS45, 2008 CS190 and 4 new Centaur/SDO discoveries: 2008 FC76, 2004 VP112, 2005 UN524, 2008 CT190 Objects recently assigned numbers: 1993 FW = (181708) 1998 WT31 = (181855) 1999 CG119 = (181868) 1999 CO153 = (181871) 1999 CV118 = (181867) 1999 HW11 = (181874) 1999 RD215 = (181902) 2000 YC2 = (182223) 2000 YU1 = (182222) 2001 KU76 = (182294) 2001 QW297 = (182397) 2002 FU6 = (182926) 2002 GJ32 = (182934) 2002 GZ31 = (182933) 2003 TG58 = (183595) 2004 DJ64 = (183963) 2004 DJ71 = (183964) 2004 PB112 = (184212) 2005 EO302 = (184314) Current number of TNOs: 1076 (including Pluto) Current number of Centaurs/SDOs: 227 Current number of Neptune Trojans: 6 Out of a total of 1309 objects: 557 have measurements from only one opposition 536 of those have had no measurements for more than a year 281 of those have arcs shorter than 10 days (for more details, see: http://www.boulder.swri.edu/ekonews/objects/recov_stats.gif) 2 PAPERS ACCEPTED TO JOURNALS A Study of Photometric Variations on the Dwarf Planet (136199) Eris R. Duffard1, J.L. Ortiz1, P. Santos Sanz1, A. Mora2, P.J. Guti´errez1, N. Morales1, and D. Guirado1 1 Instituto de Astrof´ısica de Andaluc´ıa, CSIC, Apt 3004, 18008 Granada, Spain 2 Universidad Aut´onoma de Madrid, Departamento de F´ısica Te´orica C-XI, 28049 Madrid, Spain Eris is the largest dwarf planet currently known in the solar system.