Introduction to the European Activities in Electric Propulsion *
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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. -
LISA, the Gravitational Wave Observatory
The ESA Science Programme Cosmic Vision 2015 – 25 Christian Erd Planetary Exploration Studies, Advanced Studies & Technology Preparations Division 04-10-2010 1 ESAESA spacespace sciencescience timelinetimeline JWSTJWST BepiColomboBepiColombo GaiaGaia LISALISA PathfinderPathfinder Proba-2Proba-2 PlanckPlanck HerschelHerschel CoRoTCoRoT HinodeHinode AkariAkari VenusVenus ExpressExpress SuzakuSuzaku RosettaRosetta DoubleDouble StarStar MarsMars ExpressExpress INTEGRALINTEGRAL ClusterCluster XMM-NewtonXMM-Newton CassiniCassini-H-Huygensuygens SOHOSOHO ImplementationImplementation HubbleHubble OperationalOperational 19901990 19941994 19981998 20022002 20062006 20102010 20142014 20182018 20222022 XMM-Newton • X-ray observatory, launched in Dec 1999 • Fully operational (lost 3 out of 44 X-ray CCD early in mission) • No significant loss of performances expected before 2018 • Ranked #1 at last extension review in 2008 (with HST & SOHO) • 320 refereed articles per year, with 38% in the top 10% most cited • Observing time over- subscribed by factor ~8 • 2,400 registered users • Largest X-ray catalogue (263,000 sources) • Best sensitivity in 0.2-12 keV range • Long uninterrupted obs. • Follow-up of SZ clusters 04-10-2010 3 INTEGRAL • γ-ray observatory, launched in Oct 2002 • Imager + Spectrograph (E/ΔE = 500) + X- ray monitor + Optical camera • Coded mask telescope → 12' resolution • 72 hours elliptical orbit → low background • P/L ~ nominal (lost 4 out 19 SPI detectors) • No serious degradation before 2016 • ~ 90 refereed articles per year • Obs -
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. -
ESO Call for Proposals – P109 Proposal Deadline: 23 September 2021, 12:00 Noon CEST * Call for Proposals
ESO Call for Proposals – P109 Proposal Deadline: 23 September 2021, 12:00 noon CEST * Call for Proposals ESO Period 109 Proposal Deadline: 23 September 2021, 12:00 noon Central European Summer Time Issued 26 August 2021 * Preparation of the ESO Call for Proposals is the responsibility of the ESO Observing Programmes Office (OPO). For questions regarding preparation and submission of proposals to ESO telescopes, please submit your enquiries through the ESO Helpdesk. The ESO Call for Proposals document is a fully linked pdf file with bookmarks that can be viewed with Adobe Acrobat Reader 4.0 or higher. Internal document links appear in red and external links appear in blue. Links are clickable and will navigate the reader through the document (internal links) or will open a web browser (external links). ESO Call for Proposals Editor: Dimitri A. Gadotti Approved: Xavier Barcons Director General v Contents I Phase 1 Instructions1 1 ESO Proposals Invited1 1.1 Important recent changes (since Periods 107 and 108)..................2 1.1.1 General.......................................2 1.1.2 Paranal.......................................3 1.1.3 La Silla.......................................5 1.1.4 Chajnantor.....................................5 1.2 Important reminders....................................6 1.2.1 General.......................................6 1.2.2 Paranal.......................................7 1.2.3 La Silla.......................................9 1.2.4 Chajnantor.....................................9 1.3 Changes foreseen in the upcoming Periods........................ 10 2 Getting Started 10 2.1 Support for VLTI programmes.............................. 11 2.2 Exposure Time Calculators................................ 11 2.3 The p1 proposal submission tool............................. 11 2.3.1 Important notes.................................. 12 2.4 Proposal Submission.................................... 13 3 Visitor Instruments 13 II Proposal Types, Policies, and Procedures 14 4 Proposal Types 14 4.1 Normal Programmes................................... -
The GAIA/CHEOPS Synergy
The GAIA/CHEOPS synergy Valerio Nascimbeni (INAF-OAPD) and the CHEOPS A1 working group CHEOPS Science workshop #3, Madrid 2015 Jun 17-19 Introduction GAIA is the most accurate (~10 μas) astrometric survey ever; it was launched in 2013 and is performing well (though some technical issues) Final catalog is expected in ≥2022, with a few intermediate releases starting from 2016 What planets (or planetary candidates) can GAIA provide to CHEOPS? This was investigated within the CHEOPS A1 WG, designed to 1) build an overview of available targets, 2) monitor present and future planet-search surveys, 3) establishing selection criteria for CHEOPS, 4) and proposing strategies to build the target list. CHEOPS Science workshop #3, Madrid 2015 Jun 17-19 The GAIA/CHEOPS synergy We started reviewing some recent works about the GAIA planet yield: ▶ Casertano+ 2008, A&A 482, 699. “Double-blind test program for astrometric planet detection with GAIA” ▶ Perryman+ 2014, Apj 797, 14. “Astrometric Exoplanet Detection with GAIA” ▶ Dzigan & Zucker 2012, ApJ 753, 1. “Detection of Transiting Jovian Exoplanets by GAIA Photometry” ▶ Sozzetti+ 2014, MNRAS 437, 497, “Astrometric detection of giant planets around nearby M dwarfs: the GAIA potential” ▶ Lucy 2014, A&A 571, 86. “Analysing weak orbital signals in GAIA data” ▶ Sahlmann+ 2015, MNRAS 447, 287. “GAIA's potential for the discovery of circumbinary planets” CHEOPS Science workshop #3, Madrid 2015 Jun 17-19 “Photometric” planets Challenges of GAIA planets discovered by photometry: ▶ GAIA's photometric detection of transiting planets will be limited by precision (1 mmag) and especially by the sparse sampling of the scanning law (Dzigan & Zucker 2012) ▶ Nearly all those planets will be VHJ (P < 3 d); only ~40 of them will be robustly detected and bright enough for CHEOPS (G < 12). -
ARIEL – 13Th Appleton Space Conference PLANETS ARE UBIQUITOUS
Background image credit NASA ARIEL – 13th Appleton Space Conference PLANETS ARE UBIQUITOUS OUR GALAXY IS MADE OF GAS, STARS & PLANETS There are at least as many planets as stars Cassan et al, 2012; Batalha et al., 2015; ARIEL – 13th Appleton Space Conference 2 EXOPLANETS TODAY: HUGE DIVERSITY 3700+ PLANETS, 2700 PLANETARY SYSTEMS KNOWN IN OUR GALAXY ARIEL – 13th Appleton Space Conference 3 HUGE DIVERSITY: WHY? FORMATION & EVOLUTION PROCESSES? MIGRATION? INTERACTION WITH STAR? Accretion Gaseous planets form here Interaction with star Planet migration Ices, dust, gas ARIEL – 13th Appleton Space Conference 4 STAR & PLANET FORMATION/EVOLUTION WHAT WE KNOW: CONSTRAINTS FROM OBSERVATIONS – HERSCHEL, ALMA, SOLAR SYSTEM Measured elements in Solar system ? Image credit ESA-Herschel, ALMA (ESO/NAOJ/NRAO), Marty et al, 2016; André, 2012; ARIEL – 13th Appleton Space Conference 5 THE SUN’S PLANETS ARE COLD SOME KEY O, C, N, S MOLECULES ARE NOT IN GAS FORM T ~ 150 K Image credit NASA Juno mission, NASA Galileo ARIEL – 13th Appleton Space Conference 6 WARM/HOT EXOPLANETS O, C, N, S (TI, VO, SI) MOLECULES ARE IN GAS FORM Atmospheric pressure 0.01Bar H2O gas CO2 gas CO gas CH4 gas HCN gas TiO gas T ~ 500-2500 K Condensates VO gas H2S gas 1 Bar Gases from interior ARIEL – 13th Appleton Space Conference 7 CHEMICAL MEASUREMENTS TODAY SPECTROSCOPIC OBSERVATIONS WITH CURRENT INSTRUMENTS (HUBBLE, SPITZER,SPHERE,GPI) • Precision of 20 ppm can be reached today by Hubble-WFC3 • Current data are sparse, instruments not absolutely calibrated • ~ 40 planets analysed -
The Evolution of the Milky Way's Radial Metallicity Gradient As Seen By
Astronomy in Focus - XXX Proceedings IAU Symposium No. XXX, 2018 c International Astronomical Union 2020 M. T. Lago, ed. doi:10.1017/S174392131900423X The evolution of the Milky Way’s radial metallicity gradient as seen by APOGEE, CoRoT, and Gaia Friedrich Anders, Ivan Minchev and Cristina Chiappini Leibniz-Institut f¨ur Astrophysik Potsdam (AIP), An der Sternwarte 16, 14482 Potsdam, Germany Abstract. The time evolution of the radial metallicity gradient is one of the most important constraints for Milky Way chemical and chemo-dynamical models. In this talk we reviewed the status of the observational debate and presented a new measurement of the age dependence of the radial abundance gradients, using combined asteroseismic and spectroscopic observations of red giant stars. We compared our results to state-of-the-art chemo-dynamical Milky Way models and recent literature results obtained with open clusters and planetary nebulae, and propose a new method to infer the past history of the Galactic radial abundance profile. Keywords. stars: asteroseismology, stars: late-type, stars: abundances, stars: distances, stars: ages, Galaxy: stellar content, Galaxy: evolution In Anders et al. (2017), we used combined asteroseismic CoRoT and spectroscopic APOGEE observations of 418 red giants located close to the Galactic disc plane (6 kpc <RGal < 13 kpc) to derive the age dependence of the Milky Way’s radial metallic- ity gradient. The radial iron gradient traced by the youngest red-giant population (−0.058 ± 0.008 ± 0.003 dex/kpc) reproduces the results obtained with young Cepheids and HII regions, while for the 1-4 Gyr population we obtain a slightly steeper gradient (−0.066 ± 0.007 ± 0.002 dex/kpc). -
Arxiv:2007.10189V2 [Astro-Ph.SR] 26 Jul 2020
Astronomy & Astrophysics manuscript no. worley_k2ges c ESO 2020 July 28, 2020 The Gaia-ESO Survey: Spectroscopic-asteroseismic analysis of K2 stars in Gaia-ESO The K2 Galactic Caps Project C. C. Worley1, P. Jofré2, B. Rendle3, A. Miglio3, L. Magrini4, D. Feuillet5;12, A. Gavel6, R. Smiljanic7, K. Lind5;6;21, A. Korn6, G. Gilmore1, S. Randich4, A. Hourihane1, A. Gonneau1, P. Francois8, J. Lewis1, G. Sacco4, A. Bragaglia11, U. Heiter6, S. Feltzing12, T. Bensby12, M. Irwin1, E. Gonzalez Solares1, D. Murphy1, A. Bayo19;22, L. Sbordone17, T. Zwitter18, A. C. Lanzafame10, N. Walton1, S. Zaggia9, E. J. Alfaro13, L. Morbidelli4, S. Sousa14, L. Monaco15, G. Carraro16, and C. Lardo20 (Affiliations can be found after the references) Received ; accepted ABSTRACT Context. The extensive stellar spectroscopic datasets that are available for studies in Galactic Archeaology thanks to, for example, the Gaia-ESO Survey, now benefit from having a significant number of targets that overlap with asteroseismology projects such as Kepler, K2, and CoRoT. Combining the measurements from spectroscopy and asteroseismology allows us to attain greater accuracy with regard to the stellar parameters needed to characterise the stellar populations of the Milky Way. Aims. The aim of this Gaia-ESO Survey special project is to produce a catalogue of self-consistent stellar parameters by combining measurements from high-resolution spectroscopy and precision asteroseismology. Methods. We carried out an iterative analysis of 90 K2@Gaia-ESO red giants. The spectroscopic values of Teff were used as input in the seismic analysis to obtain log g values. The seismic estimates of log g were then used to re-determine the spectroscopic values of Teff and [Fe/H]. -
ESA's Gaia Mission: a Billion Stars with a Billion Pixels
FOCUS I PHOTONIC TECHNIQUES AND TECHNOLOGIES ESA’S GAIA MISSION: a billion stars with a billion pixels Jos DE BRUIJNE 1 Astrometry is the astronomical discipline of measuring the positions, 2 Matthias ERDMANN and changes therein, of celestial bodies. Accurate astrometry from 1 Directorate of Science, European Space Agency, ESA/ESTEC, the ground is limited by the blurring effects induced by the Earth’s The Netherlands atmosphere. Since decades, Europe has been at the forefront of 2 Directorate of Earth Observation, making astrometric measurements from space. The European Space European Space Agency, ESA/ ESTEC, The Netherlands Agency (ESA) launched the first satellite dedicated to astrometry, [email protected] named Hipparcos, in 1989, culminating in the release of the Hipparcos Catalogue containing astrometric data for 117 955 stars in 1997. Since mid 2014, Hipparcos’ successor, Gaia, has been collecting astrometric data, with a 100 times improved precision, for 10 000 times as many stars. lthough astrometry sounds revolves around the sun – and of pro- the telescope in 1608, the first reliable boring, it is of fundamental per motion – the continuous, true parallax measurement of a star other Aimportance to many branches displacement of a star on the sky as than the sun was only made in 1838. of astronomy and astrophysics. The a result of its velocity in space relative The reason for this late success is the reason for this is that astrometry can to the sun. Measuring the distances fact that stars are located at extremely determine -
ARIEL Payload Design Description
Doc Ref: ARIEL-RAL-PL-DD-001 ARIEL Payload ARIEL Payload Design Issue: 2.0 Consortium Description Date: 15 February 2017 ARIEL Consortium Phase A Payload Study ARIEL Payload Design Description ARIEL-RAL-PL-DD-001 Issue 2.0 Prepared by: Date: Paul Eccleston (RAL Space) Consortium Project Manager Reviewed by: Date: Kevin Middleton (RAL Space) Payload Systems Engineer Approved & Date: Released by: Giovanna Tinetti (UCL) Consortium PI Page i Doc Ref: ARIEL-RAL-PL-DD-001 ARIEL Payload ARIEL Payload Design Issue: 2.0 Consortium Description Date: 15 February 2017 DOCUMENT CHANGE DETAILS Issue Date Page Description Of Change Comment 0.1 09/05/16 All New document draft created. Document structure and headings defined to request input from consortium. 0.2 24/05/16 All Added input information from consortium as received. 0.3 27/05/16 All Added further input received up to this date from consortium, addition of general architecture and background section in part 4. 0.4 30/05/16 All Further iteration of inputs from consortium and addition of section 3 on science case and driving requirements. 0.5 31/05/16 All Completed all additional sections except 1 (Exec Summary) and 8 (Active Cooler), further updates and iterations from consortium including updated science section. Added new mass budget and data rate tables. 0.6 01/06/16 All Updates from consortium review of final document and addition of section 8 on active cooler (except input on turbo-brayton alternative). Updated mass and power budget table entries for cooler based on latest modelling. 0.7 02/06/16 All Updated figure and table numbering following check. -
When Artemis Talks, Johannes Kepler Listens 27 January 2011
When Artemis talks, Johannes Kepler listens 27 January 2011 be shared between Artemis and NASA's Tracking and Data Relay Satellite System (TDRSS). The first ATV mission was also supported by Artemis, in 2008. Working in parallel with TDRSS, Artemis was used as the main relay while ATV was attached to the Station and provided back up for commands and telemetry during rendezvous, docking, undocking and reentry. Artemis will provide communications between Johannes Kepler and the ATV Control Centre (ATV-CC) in Toulouse, France. Hovering some 36 000 km above the equator at 21.4ºE, Artemis will route telemetry and commands to and from the control centre whenever the satellite sees the International Space Station or ATV. During every ATV-2 orbit, there is close to 40 minutes of continuous contact. Credit: ESA Credits: ESA/J.Huart After Ariane 5 lofts ATV Johannes Kepler into Artemis will again provide dedicated support to ATV space on 15 February, ESA's Artemis data relay throughout the free-flying phase of its mission up to satellite will be ready for action. the docking with the Station. TDRSS is the backup to Artemis during the attached phase, while Artemis Artemis will provide communications between will back up TDRSS during the other phases and in Johannes Kepler and the ATV Control Centre (ATV- emergency situations. CC) in Toulouse, France. Hovering some 36 000 km above the equator at 21.4ºE, Artemis will route Such was the case on 11 September 2008, when telemetry and commands to and from the control the Artemis Mission Control Centre provided centre whenever the satellite sees the International emergency support to ATV-1 after Hurricane Ike Space Station or ATV. -
Envisat and MERIS Status
MERIS US Workshop 14 July 2008 MERIS US Workshop, Silver Spring, July 14th, 2008 MERIS US Workshop Agenda a.m. ENVISAT/MERIS mission status, access to MERIS data 08:10-08:55 H. Laur (ESA) and distribution policy 08:55-09:10 Discussion Examples of the use of MERIS data in marine & land 09:10-09:40 P. Regner (ESA) applications 09:40-10:00 B. Arnone (NRL) Examples of MERIS data use for U.S. applications 10:00-10:20 S. Delwart (ESA) MERIS instrument overview 10:20-10:40 S. Delwart Instrument characterization overview 10:40-10:55 Discussion 10:55-11:10 Coffee break 11:10-11:30 S. Delwart Instrument calibration methods and results 11:30-11:50 Discussion 11:50-13:20 Lunch break MERIS US Workshop, Silver Spring, July 14th, 2008 MERIS US Workshop Agenda p.m. 13:20-13:50 L. Bourg (ACRI) Level 1 processing 13:50-14:10 Discussion 14:10-14:30 S. Delwart Vicarious calibration methods and results 14:30-14:50 Discussion 14:50-15:10 L. Bourg Overview Level 2 products 15:10-15:25 Coffee break 15:25-16:25 L. Bourg Level 2 processing 16:25-17:10 Discussion 17:10-17:25 P. Regner BEAM Toolbox 17:25-17:40 H. Laur Plans and status of the OLCI onboard GMES Sentinel-3 17:40-18:00 Discussion MERIS US Workshop, Silver Spring, July 14th, 2008 MERIS US Workshop, July 14th, 2008, Washington (USA) ENVISAT / MERIS mission status, access to MERIS data and distribution policy Henri LAUR Envisat Mission Manager & Head of EO Missions Management Office MERIS US Workshop, Silver Spring, July 14th, 2008 ESA: the European Space Agency The purpose of ESA: An inter-governmental