Future Measurements in Cosmology

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Future Measurements in Cosmology Aim High, Aim Long: Seeing the Infinite Universe - Technological Advancements Transforming Cosmology • John Mather • JWST Senior Project Scientist • NASA’s Goddard Space Flight Center • on behalf of 7.7 billion current humans, ~10,000 future observers, ~ 3000 engineers and technicians, ~ 100 scientists worldwide, 3 space agencies How did we get here? • Quantum mechanics determines properties of all matter from subatomic to DNA, iPhones, & concrete • Expanding universe starts smooth and hot • Instability everywhere: energy release from reorganization into complex systems (negative specific heat of gravity!!) • Infinite (?) and ancient universe explores every possibility, time enough for possibility → reality • Stored information (DNA & decoders, language, etc.) enables life, evolution (survival of the lucky), individuality, civilization • Nested feedback loops stabilize systems (create recognizable identity), destabilize too (balance of nature is temporary) (as of 1985) 3 Mather 2013 From one of a kind to AO (Announcement of Opportunity) competition, 1974 IUE (International COBE (Cosmic Background Ultraviolet Explorer) in Explorer) in space, launch space, launch 1979 1989 COBE → cryo missions The early universe very hot, very compressed no center, no edge (infinite) infinite universe expanding into itself no first moment no instant of creation not a “big firecracker” probably no end… WMAP (Wilkinson Microwave Anisotropy Probe) all- sky map of CMB fluctuations, leading to existence of galaxies, stars, etc. WMAP team won Breakthrough Prize, 2017 Contents of the Universe per WMAP 8 Delabrouille et al., Voyage 2050 9 Waves in Matter • Gas: sound pressure waves (1 scalar mode) • Solid: transverse sound waves too (3 modes) • E&M: transverse electric & magnetic fields, 2 polarizations 90°apart • Magnetized plasma: transverse electrohydrodynamic waves (2 polarizations X plasma complexity) • Gravitation: tensor mode transverse waves, 2 polarizations 45° apart 10 CMB Polarization by Thomson Scattering at recombination (or later) Quadrupole Anisotropy e' Thomson Scattering e– e' e Linear Polarization 11 CLASS (Cosmology Large Angular Scale Surveyor) CMB telescope in Chile 12 At$the$south$pole$ BICEP2$ SPT$ Oct. 11, 2010 Mather Future 13 64$ Hubble servicing →JWST M101 before and Every galaxy has a Hubble is 29 after Hubble repair black hole in the middle Galaxies attract each other, so the expansion should be slowing down -- Right?? To tell, we need to compare the velocity we measure on nearby galaxies to ones at very high redshift. In other words, we need to extend Hubble’s velocity vs distance plot to much greater distances. Nobel Prize, 2011 Dark Energy MacArthur Fellow 2008 - Adam Riess S. Perlmutter, A. Riess, B. Schmidt Shaw Prize, Hong Kong, 2006 More and more! SMM used Multimission Over 2000 CubeSats launched Modular Spacecraft, first https://cubesats.gsfc.nasa.gov designed for servicing Spitzer Kepler 8/25/2003 3/7/2009 Formulation + MIDEX/MO (2023), 10/30/2018 EOM SMEX/MO (2025), etc. Implementation ] Primary Ops Extended Ops Webb WFIRST Euclid (ESA) 2021 Mid 2020s 2022 XMM-Newton (ESA) Chandra 12/10/1999 TESS 7/23/1999 4/18/2018 NuSTAR 6/13/2012 Fermi IXPE Swift 6/11/2008 2021 11/20/2004 XRISM (XARM) (JAXA) SPHEREx 2022 2023 Hubble 4/24/1990 ISS-NICER GUSTO 2021 6/3/2017 ISS-CREAM 8/14/2017 2/15/2019 EOM SOFIA Revised + Athena (late 2020s), Full Ops 5/2014 1 February 21, 2019 LISA (mid 2030s) Advanced LIGO (Laser Interferometer Gravitational wave Observatory) – daily announcements? Transiting Exoplanet Survey Telescope (TESS) “TESS has just accelerated our chances of finding life on another planet within the next decade." Sara Seager, a professor of planetary science and physics at MIT and TESS project member closest 1,000 M stars and source list for JWST ALMA (Atacama Large Millimeter Array) sees proto-planetary disk, early galaxies too James Webb Space Telescope (JWST) Organization ▪ Mission Lead: Goddard Space Flight Center ▪ International collaboration with ESA & CSA ▪ Prime Contractor: Northrop Grumman Aerospace Systems ▪ Instruments: ― Near Infrared Camera (NIRCam) – Univ. of Arizona ― Near Infrared Spectrograph (NIRSpec) – ESA ― Mid-Infrared Instrument (MIRI) – JPL/ESA ― Fine Guidance Sensor (FGS) and Near IR Imaging Slitless Spectrograph (NIRISS) – CSA ▪ Operations: Space Telescope Science Institute Description ▪ Deployable infrared telescope with 6.5 meter diameter segmented adjustable JWST Science Themes primary mirror ▪ Cryogenic temperature telescope and instruments for infrared performance ▪ Launch on an ESA-supplied Ariane 5 rocket to Sun-Earth L2 ▪ 5-year science mission (10-year goal) End of the dark Birth of stars and Planetary www.JWST.nasa.gov ages: First light The assembly of proto-planetary systems and and reionization galaxies systems the origin of life 2 2 JWST Deployment JWST Instrumentation Instrument Science Requirement Capability Wide field, deep imaging 2.2’ x 4.4’ SW at same time as NIRCam ‣0.6 μm - 2.3 μm (SW) 2.2’ x 4.4’ LW with dichroic Univ. Az/LMATC ‣2.4 μm - 5.0 μm (LW) Coronagraph Multi-object spectroscopy 9.7 Sq arcmin Ω + IFU + slits NIRSpec ‣0.6 μm - 5.0 μm 100 selectable targets: MSA ESA/Astrium R=100, 1000, 3000 Mid-infrared imaging 1.9’ x1.4’ with coronagraph MIRI ‣ 5 μm - 27 μm ESA/Consortium 3.7”x 3.7” – 7.1”x 7.7” IFU /UKATC/JPL Mid-infrared spectroscopy ‣ 4.9 μm - 28.8 μm R=3000 - 2250 Fine Guidance Sensor Two 2.3’ x 2.3’ FGS/NIRISS 0.8 μm - 5.0 μm CSA Near IR Imaging Slitless 2.2’ x 2.2’ Spectrometer R= 700 with coronagraph JWST Cosmology with JWST • Supernova tests of dark energy, Hubble constant in the IR (tension with CMB data!!) • Maps of dark matter gravitational lensing in galaxy clusters • Magnification of early galaxies by lensing • Formation of first stars, galaxies, and black holes – all sensitive to dark matter via gravity, dark energy via time scales • Growth (by mergers) of early galaxies: brightness, contents, structure & number vs. time Europa Europa has an ocean, ice sheets, and warm water spritzers What’s a good landing spot? May 20, 2009 Mather Ottawa Museum 2009 2 6 WFIRST surveys NIR sky, measures Dark Energy, finds rare extreme objects, high z supernovae, examines AGN hosts with coronagraph No mask Planet With mask WFIRST Coronagraphy WFIRST will achieve a >100,000,000 contrast ratio to enable direct With mask and imaging of exoplanets deformable mirrors 24 meters and up! Giant Magellan 24 m European Extremely Large Telescope (GMT) 39 m Telescope (E-ELT) Thirty Meter δθ = 3 milliarcsec Telescope (TMT) Flattening the mountain top for E-ELT Adaptive Optics was for weapons, now astronomy & football Needs bright guide star(s); how about a satellite beacon? Large Synoptic Survey Telescope LSST.org This telescope will produce the deepest, widest, image of the Universe: • 27-ft (8.4-m) mirror, the width of a singles tennis court • 3200 megapixel camera • Each image the size of 40 full moons • 37 billion stars and galaxies • 10 year survey of the sky • 10 million alerts, 1000 pairs of exposures, 15 Terabytes of data .. every night! The Laser Interferometer Space Antenna (LISA) • New branch of astronomy! • Space-based gravitational wave detector • 3 spacecraft in 2,500,000 km equilateral triangle • Laser interferometer senses changes of 1/100 size of an atom NANOGrav – pulsar timing search for gravitational waves • Jocelyn Bell’s pulsars are almost perfect clocks • Sensitive to nanoHertz waves from supermassive black holes, etc. 32 Dragonfly discovers Galaxy of 99.99% DM (Dark Matter), will find many more Image credit: Pieter van Dokkum, Roberto Abraham, Gemini Observatory/AURA. Axion Dark Matter Search at U WA • Invented by Pierre Sikivie, 1983 • Magnetic field + axion → microwave photon • When cavity resonance = mass of axion, enhanced microwave signal • SQUID amplifiers, TN = 0.1 K • Nothing yet LUX (Large Underground Xenon) search for WIMP (Weakly Interacting Massive Particle) DM: UV photons + electrons • 368 kg xenon • Water shield • So far nothing The Crystal Ball The Crystal Ball has been waiting for your visit! Do you have a question that you have been waiting to ask? Click on the Crystal Ball and your personal fortune-teller browser window will appear and ask for your question. Follow the instructions carefully and you will soon receive the answers to all your questions. (http://predictions.astrology.com/cb/) but 404 - File or directory not found The Astro2020 Decadal Survey of National Academy of Sciences • Google “Astro2020” • 4 giant space telescopes (OST far IR, Lynx X-rays, HabEx and LUVOIR, large UV-near IR telescopes), 10 smaller space probes, hundreds of science papers and project papers • Extraordinary creative community effort, since 1964 • Result: book of scientific priorities and recommendations for large projects • See also: ESA Voyage 2050 Formation Flying Fresnel Telescope X-ray/Gamma-ray Imaging • Diffractive Fresnel optics • Milli-arcsecond resolution → 1 - 100 km spacecraft separation • Micro-arcsecond angular resolution → 104 - 106 km spacecraft separation • x-ray/gamma-ray band (5 - 1000 keV) • Formation flying of lens-craft and detector-craft 38 30 m telescope ideas – Oegerle study With a 100 m starshade, could see and get spectra for hundreds of solar systems Solar System at 5 pc in 1 minute 24-39 m ELT with visible AO on Earth * 170,000 km altitude matches observatory v ~ 400 m/sec * Laser beacon enables AO Image by Shaklan Possible Discoveries in 2020’s • Galaxy observations match simulations?? • New population of faint high-z
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