high energy astrophysics
DESCRIPTION
High Energy Astrophysics. - Detectors & Missions. Dr. Gerald J. (Jerry) Fishman NASA – Marshall Space Flight Center Huntsville, AL USAJuly 4, 2002. High Energy Astrophysics. Usual Methods of Study: X-ray Astronomy Gamma-Ray Astronomy Cosmic Ray Astrophysics But Also: - PowerPoint PPT PresentationTRANSCRIPT
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High Energy Astrophysics
Dr. Gerald J. (Jerry) Fishman
NASA – Marshall Space Flight Center
Huntsville, AL USA July 4, 2002
- Detectors & Missions
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High Energy AstrophysicsUsual Methods of Study:
• X-ray Astronomy
• Gamma-Ray Astronomy
• Cosmic Ray Astrophysics
But Also:
Radio, Optical, IR, …
(And Two New Astronomies:
• Neutrino Astronomy
• Gravitational Astronomy )
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Electromagnetic Spectrum / Temperature Scale
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Discovery of Cosmic Rays - 1912• In a balloon, at an altitude of 5,000
meters Victor Hess, the father of cosmic ray research, discovered "penetrating radiation" coming from space.
‹date/time› ‹footer› ‹#›
V.F. Hess (1883-1964) – Nobel Prize 1936
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CollimatorCoded Aperture
Grazing Incidence Mirror
Nothing (Un-collimated)..
Aperture:
CCD Proportional Counter Scintillation Detector...
Detector:
X-ray & Gamma-Ray “Telescopes”
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High-Energy
Gamma-Ray “Telescopes” :
- Compton Telescope
- Pair-tracking Telescope
- Atmospheric Cherenkov Telescope
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High-Energy Photon Interactions
- the Basis for all Detectors
• Photoelectric Effect
•Compton Scattering
•Pair Production
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Photoelectric Interaction
Photon knocks out a bound electron, losing all of its energy to the electron
CCDs, Proportional Counters, Scintillation Detectors, . .
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Compton ScatteringPhoton scatters off of an electron, losing part of its
energy to the electron and continues in another direction
Scintillation Detectors, Compton Telescope
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Pair ProductionA very high energy electron interacts with matter and
produces an electron-positron pair (E=mc2)
Used in: Pair-tracking Telescope
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UHURU (SAS-1) First X-ray Astronomy Satellite
1970-1974
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HEAO Program: 1978 - 1982High Energy Astronomy Observatory
- Had Observational Support from AAVSO
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The Great Observatories (4) :
Hubble Space Telescope 1990 - ~2010
Compton Gamma-Ray Observatory 1991 - 2000
Chandra X-Ray Observatory 1999 - ~2010
SIRTF (Space InfraRed Telescope Facility) 2003 - ~2006
High Energy Missions
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X-Ray Astronomy Collimated Detectors (Non-Focusing)
( - Primarily for sky surveys and timing studies)
Timeframe
Uhuru (SAS-1), ANS, Ariel-5,SAS-3, HEAO-A1, … 1970s
EXOSAT, WATCH/GRANAT, … 1980s
BeppoSAX, Rossi-XTE 1990s
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Focusing X-Ray Optics
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Einstein (HEAO-2)
Currently in Orbit & Operational:
CHANDRA XMM-Newton
Future:
X-ray Astronomy (Focusing)
XEUSConstellation-X
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Constellation – X (Con-X)
•Four identical satellites
•~100x present sensitivity
•Launched singly or in pairs
•Extended truss in orbit
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Constellation – X (Con-X)
Two Spacecraft in Atlas V Shroud
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Constellation-X Sensitivity
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XEUS
The Xeus Mirror Spacecraft:
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XEUSTwo-Component S/C - flying in formation with Space Station
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Gamma-Ray Astronomy
– Future Developments
Hard X-rays & GRBs Nuclear H.E. Gammas (>20 MeV)
BATSE OSSE COMPTEL EGRET
HETE-2
SWIFT INTEGRAL
Future:GLAST
EXIST - Distant Future ACT - Distant Future
CGRO
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SWIFT•~1000 GRBs studied over a three year period •0.3-2.5 arcsec positions for each GRB •Multiwavelength observatory (gamma, X-ray, UV and
optical) •20-70s reaction time •Five times more sensitive than BATSE•Spectroscopy from 0.2-150 keV •Six colors covering 170-650nm •Capability to directly measure redshift •GRB Positions publicly distributed within seconds
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SWIFT
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The INTEGRAL Mission• Scheduled for Launch: Oct. 2002
• Two Major Instruments: IBIS & SPIE
• Energy Range: 15 keV to 20 MeV
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The SPIE Instrument on the INTEGRAL Spacecraft
Coded Aperture >>Coded Aperture >>
Ge Detector Array >>
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GLAST
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GLASTLarge Area Telescope
(LAT)
Pair-Tracker Section >>
Scintillation Detector >>
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GLASTGLAST Burst Monitor
(GBM)
•Principal Investigator: Charles Meegan, MSFC
•No. Detectors: 14
•NaI (12) 5keV - 1 MeV
•BGO (2) 150 keV - 30 MeV
Un-collimated Scint. Detector Array
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Energetic X-ray Imaging Survey Telescope (EXIST)
•Obscured AGNs•GRBs out to z ~20-30 (~20X BATSE; ~5X Swift sensitivity)
• All-sky imaging (5’ resolution; ~5-50”position) every 95min
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EXIST
Side ViewDetector-collimator & Telescope
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EUSO – Extreme Energy Cosmic RaysObserved via optical emissions from above:
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Neutrino Astronomy
-Large Amount of Material Needed
to Interact with and Detect Neutrinos
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Gravitational Wave Astronomy
Space Ground
LISA LIGO
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LIGO
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LISA : Scientific Objectives
LISA - Baseline, 3 S/C
LISA : Scientific Objectives
LISA Mission
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X-ray Astronomy in Japan
Hakucho 1979-1985 Tenma 1983-1989
Ginga 1987-1991 ASCA 1993-2001
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ASTRO-E2
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The End
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Back-up slides
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Centaurus A
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High Energy Astrophysics- The study of objects and regions of space where the energy density is much greater than that of normal stars and galaxies
Some Objects of HEA:
• Compact Objects* & Binary Systems
• Cosmic Rays
• Solar Flares
• AGNs
• GRBs, …
* - BHs, Neutron stars, Strange stars
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Gamma-Ray Astronomy - Evolution
Balloon Flights – Continuous Development of Instrumentation, Techniques & Initial Observations
Early, Small Spacecraft: Explorer-11, SAS-3, COS-B
Later, Major Spacecraft: HEAO-1, HEAO-3, GRANAT/SIGMA
Compton GROHard X-rays & GRBs Nuclear H.E. Gammas (>20 MeV)
BATSE OSSE COMPTEL EGRET
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The IBIS Instrument on the INTEGRAL Spacecraft
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Future Japanese X-ray Mission – ASTRO-E2
• Astro-E lost at launch, Feb. 2000
• Astro-E2 Planned for Feb. 2005
• ~170 Layers of Nested X-ray Mirrors
• 4.5-meter Focal Length
• Three Major Instruments:
•X-ray Spectrometer
•X-ray Imaging Spectrometer
•Hard X-ray Imaging Detectors