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LISA, the Gravitational Wave Observatory

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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 time oversubscribed by factor ~4 • Ranked 2nd at 2008 extension review (with MEX, VEX & Cluster) 04-10-2010 4 Rosetta • Comet chaser, launched March 2004 • Rendezvous with, and enter orbit around, comet 67P/Churyumov-Gerasimenko • Asteroid Steins flyby (5 September 2008), Asteroid Lutetia flyby (10 July 2010) • Comet rendezvous manoeuvre: May 2014 • Perform observations of the comet's nucleus and coma • During Rosetta orbit the 67P/Churyumov- Gerasimenko will reach the closest point to the Sun in its orbit (increase in activity) • First ever attempted landing on a comet by Lander named Philae 04-10-2010 5 • Launched in May 2009 rd PlanckPlanck • 3 generation CMB experiment • Performances exceed requirements • Completed 2 sky-surveys 3 • Enough He to operate to Jan 2012 and complete 4 surveys at 0.1 K • Polarisation E-mode detected • Galaxy clusters & cold molecular cores routinely detected • Compact Sources catalogue v1 to be published in Jan 2011 • 1st CMB data release in Nov 2012; final release Nov 2013 st • 1 Planck conference in Paris 10-14 Jan 2011 • 1 year “warm” (20 K) extension will be requested to SPC Gaia Click to edit Master title style Mission Requirements – A Stereoscopic Census of Our Galaxy – Astrometry (V < 20): – completeness to 20 magnitude (on-board detection) → 109 stars – parallax accuracy: 7 μarcsec at ≤10 mag; 12–25 μarcsec at 15 mag; and 100–300 arcsec at 20 mag (depending on spectral type) μ – Photometry (V < 20): – astrophysical diagnostics (low-dispersion photometry) + chromaticity – 8–20 mmag at 15 mag: Teff ~200 K, log g, [Fe/H] to 0.2 dex, extinction – Radial velocity (V < 16.5–17): – third component of space motion, perspective acceleration – <1 km/s at 13-13.5 mag and <15 km/s at 16.5-17 mag SCIENCE AND ROBOTIC EXPLORATION Gaia Design Click to edit Master title style SCIENCE AND ROBOTIC EXPLORATION The Gaia optical bench Click to edit Master title style SCIENCE AND ROBOTIC EXPLORATION Gaia Mission Status Click to edit Master title style – Gaia is being built for launch in 2012 – Currently in the middle of the Spacecraft Critical Design Review – Consolidation of scientific performance estimates with all effects taken into account (including radiation damage & its calibration) Photometry & Radial Velocities comply with requirements Astrometry requirements missed by about 1-2 μas for stars brighter than 10th magnitude at end of mission → Currently exploring avenues for improvements SCIENCE AND ROBOTIC EXPLORATION ESA’sESA’s newnew longlong termterm planplan forfor spacespace sciencescience 04-10-2010 11 Cosmic Vision Process • Plan covers 10 years, starting from 1st launch in 2017 • It is divided in 3 “slices” with a ~1 B€ budget each (2010 EC) • It foresees a “Call for Mission proposals” for each of the 3 slices • First “Call for Missions” was issued in 1st Q 2007 • 50 proposals received by June 2007 deadline (2x than H2000+) • Selection by advisory structure on behalf of scientific community during summer & fall of 2007 → Assessment study (1 year) 04-10-2010 12 Cosmic Vision 2015‐2025 Implementation Assessment Definition Implementation Phase 0/A Phase A/B1 Phase B2/C/D DOI: Declaration of Interest AO: Announcement of Opportunity TRL ≥5 LOE: Letter of Endorsement MLA: Multi-Lateral Agreement Euclid Euclid Plato M1 launch Marco-Polo Plato M2 launch Cross-Scale Solar Orbiter Solar Orbiter M-class missions Instruments DOI AO MLA LOE TRL ≥5 EJSM/Laplace EJSM/Laplace TSSM/Tandem L1 launch Lisa IXO Instruments L-class missions DOI AO MLA LOE 2008 2009 2010 2011 2012 2013 2014 2015 2016 2017 2018 2019 2020 EUCLID, a dark-energy surveyor • To constrain Dark Energy equation of state parameter w to <1% and its evolution w(z) to < 10 % • Uses 2 probes: Weak Lensing & Baryonic Acoustic Oscillations • Imaging & spectroscopic survey of entire extragalactic sky 04-10-2010 14 PLATO, the planet finder • To search & characterise earth-size planets in 1-AU orbit around 20,000 Sun-like stars • Method: occultation technique i.e. measure stellar magnitude to 27 p.p.m. accuracy! • Successor to CoRoT & Kepler … • But emphasis is on bright mv ≤ 11 stars → Also characterise star by astroseismology → star size, mass & age → exoplanet size & age → Easier to characterise with Radial Velocity • Need to monitor many stars for long time →Large 1800 deg2 instantaneous FOV →Many nearly co-aligned small telescopes • May find up to 200 earth analogues, sufficiently nearby for follow-up with future imaging/spectroscopic mission (~Darwin) 04-10-2010 15 Solar Orbiter • To produce images of the Sun at an unprecedented resolution and perform closest ever in-situ measurements • Determine in-situ the properties and dynamics of plasma, fields and particles in the near-Sun heliosphere • Survey the fine detail of the Sun's magnetised atmosphere • Identify the links between activity on the Sun's surface and the resulting evolution of the corona and inner heliosphere, using solar co-rotation passes • Observe and characterise the Sun's polar regions and equatorial corona from high latitudes • Visible, extreme ultra violet, X-rays • Elliptical orbit around the Sun with perihelion as low as 0.23 AU and with increasing inclination up to more than 30° with respect to the solar equator. • 6 years lifetime (nominal) 04-10-2010 17 Cosmic Vision Slice #2 : M3 Mission • Call for M3 Mission (≤ 470 M€) proposals released on 29 July: – 3 December: Proposal deadline – Dec 2010 – Feb 2011: Proposal evaluation by AWG → SSAC – Feb 2011: selection of 3 (TBC) M3 missions for Assessment • 2011-mid 2012: Assessment study of selected M3 mission candidates • End-2012: selection of 2 M3 missions for Definition study (phase A/B1) • 2013-mid 2014: Definition Study of 2 selected M3 missions • End-2014: selection of 1 M3 mission for implementation – M1/2 mission candidate which was not selected competes for M3 • 2015-2021: M3 mission development (Phase B2/C/D) • 2022: Launch of M3 mission 04-10-2010 18 The Large “L” Missions IXO LISA Laplace/EJSM 04-10-2010 19 IXO, the International X-Ray Observatory • General Purpose observatory, follow-up to XMM- Newton & Chandra, e.g. • Imaging X-rays requires long focal length: – 20 to 25 m deployable bench – Light-weight X-ray mirrors at one end – 3-5 X-ray instruments at other extremity – Effective area: 3 m2 @ 1.25 keV – Angular resolution: 5 `` HPD (0.3-10 keV) – 5 years mission at L2 – Collaboration with NASA & JAXA • Assessment studies just completed: – Feasible but expensive: cost > 650 M€ • Mission feasibility depends on light weight mirror availability; 2 technologies are being developed: – Slump glass @ NASA – Silicon Pore Optics @ ESA – Need several years of development 04-10-2010 20 LISA, the gravitational wave observatory 5 8 • Observe BH formation & SMBH (M ~10 ... 10 Mo) mergers out to z > 10 with high (>300) SNR • To observe capture of stellar-mass compact objects (BH,NS,WD) into SMBH (“EMRI”) • Map space-time geometry near BH & test GR in strong field regime, including “no hair” theorem • To observe thousands of compact binaries & map their distribution across the galaxy • Measure Luminosity distances to 0.5 % accuracy → accurate cosmology (e.g. DE eq. state) 04-10-2010 21 LISA (2) 3 FrequencyWillIncluding follow BH dozenrange merger 10“verification”-4-0.1 for >1000Hz (inaccessiblebinaries orbits at→ S/Ncalibration from > 10 ground) LIGO MB H c Seismic barrier oales C cenc o e m p a c t b in a r ie s EMRI 04-10-2010 22 LISA Mission Concept • Cluster of 3 spacecraft in a heliocentric orbit – Spacecraft shield the test masses from external non-gravitational forces (solar wind, radiation pressure) → TM follow pure geodesic – Allows measurement of amplitude and polarisation of GW 04-10-2010 23 LISA Mission Concept • Cluster of 3 spacecraft in a heliocentric orbit • Trailing the Earth by 20° (50 million kilometres) • Equilateral triangle with 5 million kilometres arm length – Measure arm-lengths variations by laser interferometry – Precision of relative variation measurements <0.1
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