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From the Big Bang to the Nobel Prize: The Cosmic Background Explorer (COBE) and Beyond

From the Big Bang to the Nobel Prize: The Cosmic Background Explorer (COBE) and Beyond. Goddard Space Flight Center Conference John Mather November 21, 2006. Astronomical search for origins. The First Galaxies. Big Bang. Life. Galaxies evolve. Planets. Star. Looking back in time.

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From the Big Bang to the Nobel Prize: The Cosmic Background Explorer (COBE) and Beyond

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  1. From the Big Bang to the Nobel Prize: The Cosmic Background Explorer (COBE) and Beyond Goddard Space Flight Center Conference John Mather November 21, 2006

  2. Astronomical search for origins The First Galaxies Big Bang Life Galaxies evolve Planets Star

  3. Looking back in time

  4. Distance measurement This technique allows the measurement of huge distances

  5. The astronomer toolbox #2:Doppler-light displacement Atoms emit light at discrete wavelengths that can be seen with a spectroscope This "line spectrum" identifies the atom and its velocity

  6. Galaxies attract each other, so expansion should slow down -- right? To say, we need to compare the speed we measure in nearby galaxies with those at a very high level of displacement. In other words, we need to extend Hubble's speed against the distance frame at much greater distances.

  7. Nobel Prize press release The Royal Swedish Academy of Sciences has decided to award the Nobel Prize in Physics for 2006 together to John C. Mather, Goddard Space Flight Center of NASA, Greenbelt, MD, USA, and George F. Smoot, University of California, Berkeley, CA, USA. "for his discovery of the black body shape and the anisotropy of cosmic microwave background radiation".

  8. The power of thought George Gamow Georges Lemaitre & Albert Einstein Robert Herman & Ralph Alpher Rashid Sunyaev Jim Peebles

  9. Power hardware-CMB Spectrum Paul Richards Mike Werner David Woody Herb Gush Rai Weiss Frank Low

  10. A Brief History of COBE • 1965, CMB announced-Penzias & Wilson; Dicke, Peebles, roll, and Wilkinson • 1974, NASA AO for Explorers: 150 proposals, including: • Proposal for anisotropy JPL (Gulkis, Janssen...) • Berkeley anisotropy proposal (Alvarez, Smoot...) • Proposal by Goddard/MIT/Princeton COBE (Hauser, Mather, Muehlner, Silverberg, Thaddeus, Weiss, Wilkinson)

  11. History of COBE (2) • 1976, Team of Science of Definition of MissionSelectedBy HQ (Nancy Boggess, ProgramScientific); The IP Chose • • 1979, Decision of BuildIn COBE house In Gsfc • 1982, Approval paraca Build paraca Flight • 1986, Explosion Challenger, Start The Redesign COBE for the Launch Delta • 1989, November 18, Launch • 1990, Results of the first Spectrum; HeliumEndsIn 10 Mo • 1992, FirstResults of Anisotropy • 1994, Operations End • 1998, TheMainResults of Background Go Cosmic

  12. Starting COBE Mike & Deanna Hauser Dave & Eunice Wilkinson John • Jane Mather Pat Thaddeus Rai And Becky Weiss Sam And Margie Gulkis, Mike & Sandie Janssen Jorge Smoot

  13. The TeamScientific COBE Chuck And Renee Bennett Ed And Tammy Cheng Nancy & Al Boggess Eli And Florence Dwek Tom & Ann Kelsall Philip & Georganne Lubin

  14. COBE's scientific team Tom & Jeanne Murdock Harvey • Sarah Moseley Steve • Sharon Meyer Ned & Pat Wright Rick And Gwen Shafer Bob & Beverly Silverberg

  15. COBE Engineering Leadership Back row: Bill Hoggard, Herb Mittelman, Joe Turtil, Bob Sanford Middle row: Don Crosby, Roger Mattson, Irene Ferber, Maureen Menton Front row: Jeff Greenwell, Ernie Doutrich, Bob Schools, Mike Roberto

  16. COBE Engineering Leadership Back row: Dennis McCarthy, Bob Maichle, Loren Linstrom, Jack Peddicord Middle row: Lee Smith, Dave Gilman, Steve leete, Tony Fragomeni Front row: Earle Young, Chuck Katz, Bernie Klein, John Wolfgang

  17. COBE in orbit, 1989-1994 COBE Satellite, 1989-1994

  18. The far-infrared absolute spectrophotometer John Mather Rick Shafer Bob Maichle Mike Roberto

  19. Calibrator (Eccosorb) on the arm, before isolation, attached to the parabolic hub

  20. Based on 9 minutes of data Presented at AAS, January 1990

  21. Current estimate: T x 2,725 +/-0.001 KCould the new technology reduce waste by 2 orders of magnitude?

  22. Confirming the Big Bang theory • The Theory Hot Big Bang IsCorrect • I do not know ReleasesEnergyAdditionalAfter of the first Year • There's none EventsExoticAsMovementTurbulent

  23. Microwave differential radiometers George Smoot Chuck Bennett Bernie Klein Steve leete

  24. 31.4 GHz

  25. Map of the SkyFrom DMR, 2.7 K +/-0.003 K Effect Doppler Movement of the EarthRemoved (v/c s 0.001) Variations of Temperature/DensityCosmic 389,000 Years, +/-0.00003 K

  26. Map COBE Fluctuations FROM CMB2,725 k +/-o 30 K'K RMS, 7OrRay

  27. DIRBE (diffuse infrared background experiment) • Map of the entire sky in 10 bands from 1.2 to 240 m • Measure, understand and subtract for the zodiac and galactic close-ups • Determine the small residue of the early universe, the early galaxies, etc. • Requires absolute calibration

  28. Mike Hauser Tom Kelsall Don Crosby Loren Linstrom

  29. DIRBE test drive hardware

  30. DIRBE far IR (100, 140, 240 m) Sky Modeling

  31. COBE cosmology • CMB has black body spectrum, . . . . .F/FMaximum <50 ppm. Strong limits, about 0.01%, in energy conversion (turbulence, unstable particles, etc.) after t x 1 year. There's no good explanation besides Hot Big Bang. • CMB has spatial structure, 0.001% in scales > 7Or, consistent with invariant predictions of scale and inflation, dark matter and dark energy or " and the formation of galaxies and clusters by gravity. • CIBR has 2 parts, near (few microns) and far (few hundred microns), each with brightness comparable to the known luminosity of visible and nearby IR galaxies: L of the universe is double expected value.

  32. Wmap Wilkinson Microwave Anisotropy Probe Chuck Bennett, PI The Goddard and Princeton team Launched in 2001

  33. -200 + 200 Temperature (K) relative to the average of 2,725 K The universe at the age of 389,000 Galactic plane

  34. Cosmic parameters at a percentage of accuracy WL WB WC WTot=WB+WC+WL=100% WM=WB+WC=274

  35. The Spectrum of Power CMB angle

  36. Planck Mission-ESA-led with NASA contributions, for the 2008 launch Higher spatial resolution and sensitivity than WMAP, with shorter wavelengths

  37. James Webb Space Telescope (JWST)

  38. JWST Summary • TelescopeInfraredDropdown With MirrorPrimaryAdjustableSegmented 6.5 metres Diameter • Telescope of TemperatureCryogenic and 4 Instruments for the PerformanceInfrared, Covering 0.6 to 29 Μm • LaunchJune 2013 In A Rocket Ariane 5 ProvidedBy ESA to Sun-Earth L2:1,5 Million km from DistanceIn The SpaceDeep (Necessary for the Cooling) • MissionScientific 5 out of 5 Years (Goal 10 Years)

  39. The James Webb Space Telescope • Mission Leader: Goddard Space Flight Center • International collaboration with ESA and CSA • First contractor: Northrop Grumman Space Technology • Instruments: • Near Infrared Camera (NIRCam) – Univ. Arizona • Near the Infrared Spectrograph (NIRSpec) – ESA • Medium Infrared Instrument (MIRI) - JPL/ESA • Fine Orientation Sensor (FGS) - CSA • Operations: Space telescope Science Institute

  40. Four scientific themes • The FirstObjectsFormedAfter by Big Bang • ¿SuperStar? • Super-supernovae? • ¿HolesBlack? • Mounting galaxies (from SmallParts?) • The Training of Star And SystemsPlanetary • HiddenIn The Clouds of Dust • The SystemsPlanetary and the Conditions for the Life

  41. The Star & Planet Formation Scientific objectives of JWST versus cosmic history Atoms and radiation Particle physics Big Bang Now 3 minutes 389,000 years 200 million years 1 billion years 13.7 billion years

  42. End of the dark age: first light?

  43. The Eagle Nebulaas it looks with Hubble The Eagle Nebula seen by HST

  44. The Eagle Nebulaas seen in the infrared

  45. The birth of stars and protoplanetary systems Stars on dust discs in Orion

  46. Planetary systems and the origins of life

  47. Hst Characterized To ThePlanetsInTransit; Also what Will JWST HST: The planet transits star

  48. Chemistry of transiting planets

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