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The Cosmic Evolution Survey (Cosmos): Overview1 N
The Astrophysical Journal Supplement Series, 172:1Y8, 2007 September # 2007. The American Astronomical Society. All rights reserved. Printed in U.S.A. THE COSMIC EVOLUTION SURVEY (COSMOS): OVERVIEW1 N. Scoville,2,3 H. Aussel,4 M. Brusa,5 P. Capak,2 C. M. Carollo,6 M. Elvis,7 M. Giavalisco,8 L. Guzzo,9 G. Hasinger,5 C. Impey,10 J.-P. Kneib,11 O. LeFevre,11 S. J. Lilly,6 B. Mobasher,8 A. Renzini,12,13 R. M. Rich,14 D. B. Sanders,15 E. Schinnerer,16,17 D. Schminovich,18 P. Shopbell,2 Y. Taniguchi,19 and N. D. Tyson20 Received 2006 April 25; accepted 2006 June 28 ABSTRACT The Cosmic Evolution Survey (COSMOS) is designed to probe the correlated evolution of galaxies, star formation, active galactic nuclei (AGNs), and dark matter (DM) with large-scale structure (LSS) over the redshift range z > 0:5Y6. The survey includes multiwavelength imaging and spectroscopy from X-rayYtoYradio wavelengths covering a 2 deg2 area, including HST imaging. Given the very high sensitivity and resolution of these data sets, COSMOS also provides unprecedented samples of objects at high redshift with greatly reduced cosmic variance, compared to earlier surveys. Here we provide a brief overview of the survey strategy, the characteristics of the major COSMOS data sets, and a summary the science goals. Subject headinggs: cosmology: observations — dark matter — galaxies: evolution — galaxies: formation — large-scale structure of universe — surveys 1. INTRODUCTION multiband imaging and spectroscopy provide redshifts and hence cosmic ages for these populations. Most briefly, the early universe Our understanding of the formation and evolution of galaxies and their large-scale structures (LSSs) has advanced enormously galaxies were more irregular/interacting than at present and the overall cosmic star formation rate probably peaked at z 1Y3 over the last decade—a result of a phenomenal synergy between with 10Y30 times the current rates (Lilly et al. -
Gaia and WEAVE/Wxes: Supporting the PLATO Exoplanet Hunter Nicholas Walton Institute of Astronomy University of Cambridge
Gaia and WEAVE/WxES: supporting The PLATO Exoplanet Hunter Nicholas Walton Institute of Astronomy University of Cambridge WEAVE – Gaia – PLATO a winning planet hunter combo • Gaia releases its first all sky astrometric catalogues late 2017 • WEAVE begins on sky operations in 2018 • PLATO begins its planet hunt in 2024 • Why are these events linked? • Finding and characterising extra solar planets requires a detailed knowledge of the host stars • And it helps to know your target stars before you observe them 6 March 2015 Nic Walton - WEAVE/Plato @ MOS ING - La Palma 2 PLATO set for 2024 6 March 2015 Nic Walton - WEAVE/Plato @ MOS ING - La Palma 3 … but first … Gaia’s role in planets Recall Carme Jordi’s talk earlier this week 6 March 2015 Nic Walton - WEAVE/Plato @ MOS ING - La Palma 4 Gaia launched 19 Dec 2013 a powerful complement to PLATO NGC 1818 in LMC 212x212 arcsec2 (~1% of AF FoV) 2.85s integration time 6 March 2015 Nic Walton - WEAVE/Plato @ MOS ING - La Palma 5 Gaia End-of-Mission Parallax Errors Apply factors of ~ 0.7 and ~ 0.5 for positions and proper motions Figure from http://www.rssd.esa.int/index.php?project=GAIA&page=Science_Performance Non-uniformity over the sky: 2 70% – 116% 1 PLATO stars 1. bright-star regime (calibration errors, CCD saturation) 2. photon-noise regime, with sky-background noise and electronic noise setting in around G ~ 20 mag (equivalent to V = 20 to 22) 6 March 2015 Nic Walton - WEAVE/Plato @ MOS ING - La Palma 6 Gaia Performance (at IOCR) http://www.cosmos.esa.int/web/gaia/science-performance Typical -
Precollimator for X-Ray Telescope (Stray-Light Baffle) Mindrum Precision, Inc Kurt Ponsor Mirror Tech/SBIR Workshop Wednesday, Nov 2017
Mindrum.com Precollimator for X-Ray Telescope (stray-light baffle) Mindrum Precision, Inc Kurt Ponsor Mirror Tech/SBIR Workshop Wednesday, Nov 2017 1 Overview Mindrum.com Precollimator •Past •Present •Future 2 Past Mindrum.com • Space X-Ray Telescopes (XRT) • Basic Structure • Effectiveness • Past Construction 3 Space X-Ray Telescopes Mindrum.com • XMM-Newton 1999 • Chandra 1999 • HETE-2 2000-07 • INTEGRAL 2002 4 ESA/NASA Space X-Ray Telescopes Mindrum.com • Swift 2004 • Suzaku 2005-2015 • AGILE 2007 • NuSTAR 2012 5 NASA/JPL/ASI/JAXA Space X-Ray Telescopes Mindrum.com • Astrosat 2015 • Hitomi (ASTRO-H) 2016-2016 • NICER (ISS) 2017 • HXMT/Insight 慧眼 2017 6 NASA/JPL/CNSA Space X-Ray Telescopes Mindrum.com NASA/JPL-Caltech Harrison, F.A. et al. (2013; ApJ, 770, 103) 7 doi:10.1088/0004-637X/770/2/103 Basic Structure XRT Mindrum.com Grazing Incidence 8 NASA/JPL-Caltech Basic Structure: NuSTAR Mirrors Mindrum.com 9 NASA/JPL-Caltech Basic Structure XRT Mindrum.com • XMM Newton XRT 10 ESA Basic Structure XRT Mindrum.com • XMM-Newton mirrors D. de Chambure, XMM Project (ESTEC)/ESA 11 Basic Structure XRT Mindrum.com • Thermal Precollimator on ROSAT 12 http://www.xray.mpe.mpg.de/ Basic Structure XRT Mindrum.com • AGILE Precollimator 13 http://agile.asdc.asi.it Basic Structure Mindrum.com • Spektr-RG 2018 14 MPE Basic Structure: Stray X-Rays Mindrum.com 15 NASA/JPL-Caltech Basic Structure: Grazing Mindrum.com 16 NASA X-Ray Effectiveness: Straylight Mindrum.com • Correct Reflection • Secondary Only • Backside Reflection • Primary Only 17 X-Ray Effectiveness Mindrum.com • The Crab Nebula by: ROSAT (1990) Chandra 18 S. -
HD 97658 and Its Super-Earth Spitzer & MOST Transit Analysis and Seismic Modeling of the Host Star
The space photometry revolution CoRoT3-KASC7 joint meeting HD 97658 and its super-Earth Spitzer & MOST transit analysis and seismic modeling of the host star Valerie Van Grootel (University of Liege, Belgium) M. Gillon (U. Liege), D. Valencia (U. Toronto), N. Madhusudhan (U. Cambridge), D. Dragomir (UC Santa Barbara), and the Spitzer team 1. Introducing HD 97658 and its super-Earth The second brightest star harboring a transiting super-Earth HD 97658 (V=7.7, K=5.7) HD 97658 b, a transiting super-Earth • • Teff = 5170 ± 50 K (Howard et al. 2011) Discovery by Howard et al. (2011) from Keck- Hires RVs: • [Fe/H] = -0.23 ± 0.03 ~ Z - M sin i = 8.2 ± 1.2 M • d = 21.11 ± 0.33 pc ; from Hipparcos P earth - P = 9.494 ± 0.005 d (Van Leeuwen 2007) orb • Transits discovered by Dragomir et al. (2013) with MOST: RP = 2.34 ± 0.18 Rearth From Howard et al. (2011) From Dragomir et al. (2013) Valerie Van Grootel – CoRoT/Kepler July 2014, Toulouse 2 2. Modeling the host star HD 97658 Rp α R* 2/3 Mp α M* Radial velocities Transits + the age of the star is the best proxy for the age of its planets (Sun: 4.57 Gyr, Earth: 4.54 Gyr) • With Asteroseismology: T. Campante, V. Van Eylen’s talks • Without Asteroseismology: stellar evolution modeling Valerie Van Grootel – CoRoT/Kepler July 2014, Toulouse 3 2. Modeling the host star HD 97658 • d = 21.11 ± 0.33 pc, V = 7.7 L* = 0.355 ± 0.018 Lsun • +Teff from spectroscopy: R* = 0.74 ± 0.03 Rsun • Stellar evolution code CLES (Scuflaire et al. -
X-Ray Telescope
Early results of the Hitomi satellite Hiro Matsumoto Ux group & KMI Nagoya Univ.1 Outline •Hitomi instruments •Early scientific results –DM in Perseus –Turbulence in Perseus –others 2 Japanese history of X-ray satellites Launch, Feb. 17, 2016 Weight Suzaku Ginga ASCA Hitomi Tenma Hakucho Rocket 3 International collaboration More than 160 scientists from Japan/USA/Europe 4 Attitude anomaly Loss of communication (Mar. 26, 2016) spinning Gave up recovery (Apr. 28, 2016)5 Hitomi Obs. List Target Date Perseus Cluster of galaxies Feb. 25—27, 2016 Mar. 4—8, 2016 N132D Supernova remnants Mar. 8—11, 2016 IGR J16318-4848 Pulsar wind nebula Mar. 11—15, 2016 RXJ 1856-3754 Neutron star Mar. 17—19, 2016 Mar. 23—25, 2016 G21.5-0.9 Pulsar wind nebula Mar. 19—23, 2016 Crab Pulsar wind nebula Mar. 25, 2016 6 Scienfitic Instruments 7 4 systems Name X-Ray Telescope SXS Soft Micro-calorimeter (E<10keV) SXI Soft CCD (E<10keV) HXI Hard Si/CdTe (E<80keV) SGD --- Si/CdTe (Compton) 8 Wide energy range (0.3—600keV) HXT 1keV∼ 107K SXT SGD SXI HXI SXS 9 SXT + SXS (0.3—12keV) Soft X-ray Telescope Soft X-ray Spectrometer (X-ray micro-calorimeter) f=5.6m 10 Soft X-ray Spectrometer (SXS) FOV: 3′ × 3′ Δ푇 ∝ ℎ휈 6 × 6 pix 11 Energy Resolution Hitomi SXS Suzaku CCD Δ퐸 = 5 푒푉@ 6푘푒푉 (cf. CCD Δ퐸 = 130 푒푉)12 Before Hitomi: gratings Point source Extended Not good for extended objects 13 X-ray microcalorimeter Extended Non-dispersive type. Spatial extension doesn’t matter. -
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. -
Technology Development for Future Sparse Aperture Telescopes and Interferometers in Space
A Technology Whitepaper submitted to the 2010 Decadal Survey Technology Development for Future Sparse Aperture Telescopes and Interferometers in Space 24 March 2009 NASA Centers: GSFC: Kenneth G. Carpenter, Keith Gendreau, Jesse Leitner, Richard Lyon, Eric Stoneking MSFC: H. Philip Stahl Industrial Partners: Aurora Flight Systems: Joe Parrish LMATC: Carolus J. Schrijver, Robert Woodruff NGST – Amy Lo, Chuck Lillie Seabrook Engineering: David Mozurkewich University/Astronomical Institute Partners: College de France: Antoine Labeyrie MIT: David Miller NOAO: Ken Mighell SAO: Margarita Karovska, James Phillips STScI: Ronald J. Allen UCO/Boulder: Webster Cash Abstract We describe the major technology development efforts that need to occur throughout the 2010 decade in order to enable a wide variety of sparse aperture and interferometric missions in the following decade. These missions are critical to achieving the next major revolution in astronomical observations by dramatically increasing the achievable angular resolution by more than 2 orders of magnitude, over wavelengths stretching from the x-ray and ultraviolet into the infrared and sub-mm. These observations can only be provided by long-baseline interferometers or sparse aperture telescopes in space, since the aperture diameters required are in excess of 500m - a regime in which monolithic or segmented designs are not and will not be feasible - and since they require observations at wavelengths not accessible from the ground. The technology developments needed for these missions are challenging, but eminently feasible with a reasonable investment over the next decade to enable flight in the 2025+ timeframe. That investment would enable tremendous gains in our understanding of the structure of the Universe and of its individual components in ways both anticipated and unimaginable today. -
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 -
X-Ray and Gamma-Ray Variability of NGC 1275
galaxies Article X-ray and Gamma-ray Variability of NGC 1275 Varsha Chitnis 1,*,† , Amit Shukla 2,*,† , K. P. Singh 3 , Jayashree Roy 4 , Sudip Bhattacharyya 5, Sunil Chandra 6 and Gordon Stewart 7 1 Department of High Energy Physics, Tata Institute of Fundamental Research, Homi Bhabha Road, Mumbai 400005, India 2 Discipline of Astronomy, Astrophysics and Space Engineering, Indian Institute of Technology Indore, Khandwa Road, Simrol, Indore 453552, India 3 Indian Institute of Science Education and Research Mohali, Knowledge City, Sector 81, SAS Nagar, Manauli 140306, India; [email protected] 4 Inter-University Centre for Astronomy and Astrophysics, Ganeshkhind, Pune 411 007, India; [email protected] 5 Department of Astronomy and Astrophysics, Tata Institute of Fundamental Research, Homi Bhabha Road, Mumbai 400005, India; [email protected] 6 Centre for Space Research, North-West University, Potchefstroom 2520, South Africa; [email protected] 7 Department of Physics and Astronomy, The University of Leicester, University Road, Leicester LE1 7RH, UK; [email protected] * Correspondence: [email protected] (V.C.); [email protected] (A.S.) † These authors contributed equally to this work. Received: 30 June 2020; Accepted: 24 August 2020; Published: 28 August 2020 Abstract: Gamma-ray emission from the bright radio source 3C 84, associated with the Perseus cluster, is ascribed to the radio galaxy NGC 1275 residing at the centre of the cluster. Study of the correlated X-ray/gamma-ray emission from this active galaxy, and investigation of the possible disk-jet connection, are hampered because the X-ray emission, particularly in the soft X-ray band (2–10 keV), is overwhelmed by the cluster emission. -
HEIC0701: for IMMEDIATE RELEASE 19:30 (CET)/01:30 PM EST 7 January, 2007
HEIC0701: FOR IMMEDIATE RELEASE 19:30 (CET)/01:30 PM EST 7 January, 2007 http://www.spacetelescope.org/news/html/heic0701.html News release: First 3D map of the Universe’s Dark Matter scaffolding 7-January-2007 By analysing the COSMOS survey – the largest ever survey undertaken with Hubble – an international team of scientists has assembled one of the most important results in cosmology: a three-dimensional map that offers a first look at the web-like large-scale distribution of dark matter in the Universe. This historic achievement accurately confirms standard theories of structure formation. For astronomers, the challenge of mapping the Universe has been similar to mapping a city from night-time aerial snapshots showing only streetlights. These pick out a few interesting neighbourhoods, but most of the structure of the city remains obscured. Similarly, we see planets, stars and galaxies in the night sky; but these are constructed from ordinary matter, which accounts in total for only one sixth of the total mass in the Universe. The remainder is a mysterious component - dark matter - that neither emits nor reflects light. An international team of astronomers led by Richard Massey of the California Institute of Technology (Caltech), USA, has made a three-dimensional map that offers a first look at the web-like large-scale distribution of dark matter in the Universe in unprecedented detail. This new map is equivalent to seeing a city, its suburbs and surrounding country roads in daylight for the first time. Major arteries and intersections are revealed and the variety of different neighbourhoods becomes evident. -
Building the Coolest X-Ray Satellite
National Aeronautics and Space Administration Building the Coolest X-ray Satellite 朱雀 Suzaku A Video Guide for Teachers Grades 9-12 Probing the Structure & Evolution of the Cosmos http://suzaku-epo.gsfc.nasa.gov/ www.nasa.gov The Suzaku Learning Center Presents “Building the Coolest X-ray Satellite” Video Guide for Teachers Written by Dr. James Lochner USRA & NASA/GSFC Greenbelt, MD Ms. Sara Mitchell Mr. Patrick Keeney SP Systems & NASA/GSFC Coudersport High School Greenbelt, MD Coudersport, PA This booklet is designed to be used with the “Building the Coolest X-ray Satellite” DVD, available from the Suzaku Learning Center. http://suzaku-epo.gsfc.nasa.gov/ Table of Contents I. Introduction 1. What is Astro-E2 (Suzaku)?....................................................................................... 2 2. “Building the Coolest X-ray Satellite” ....................................................................... 2 3. How to Use This Guide.............................................................................................. 2 4. Contents of the DVD ................................................................................................. 3 5. Post-Launch Information ........................................................................................... 3 6. Pre-requisites............................................................................................................. 4 7. Standards Met by Video and Activities ...................................................................... 4 II. Video Chapter 1 -
Archons (Commanders) [NOTICE: They Are NOT Anlien Parasites], and Then, in a Mirror Image of the Great Emanations of the Pleroma, Hundreds of Lesser Angels
A R C H O N S HIDDEN RULERS THROUGH THE AGES A R C H O N S HIDDEN RULERS THROUGH THE AGES WATCH THIS IMPORTANT VIDEO UFOs, Aliens, and the Question of Contact MUST-SEE THE OCCULT REASON FOR PSYCHOPATHY Organic Portals: Aliens and Psychopaths KNOWLEDGE THROUGH GNOSIS Boris Mouravieff - GNOSIS IN THE BEGINNING ...1 The Gnostic core belief was a strong dualism: that the world of matter was deadening and inferior to a remote nonphysical home, to which an interior divine spark in most humans aspired to return after death. This led them to an absorption with the Jewish creation myths in Genesis, which they obsessively reinterpreted to formulate allegorical explanations of how humans ended up trapped in the world of matter. The basic Gnostic story, which varied in details from teacher to teacher, was this: In the beginning there was an unknowable, immaterial, and invisible God, sometimes called the Father of All and sometimes by other names. “He” was neither male nor female, and was composed of an implicitly finite amount of a living nonphysical substance. Surrounding this God was a great empty region called the Pleroma (the fullness). Beyond the Pleroma lay empty space. The God acted to fill the Pleroma through a series of emanations, a squeezing off of small portions of his/its nonphysical energetic divine material. In most accounts there are thirty emanations in fifteen complementary pairs, each getting slightly less of the divine material and therefore being slightly weaker. The emanations are called Aeons (eternities) and are mostly named personifications in Greek of abstract ideas.