Документ взят из кэша поисковой машины. Адрес оригинального документа : http://www.naic.edu/~astro/chicago2/talks/Harrison-HighEnergy-Radio_Connection.pdf Дата изменения: Tue Aug 22 00:13:08 2006 Дата индексирования: Sun Dec 23 00:57:14 2007 Кодировка: Поисковые слова: m 63

New Opportunities 2010 and Beyond: The High-Energy/Radio Connection


High Energy Missions
Timeline
XMM, Suzaku... Chandra Swift Integral GLAST 2006 NEXT

... ... ...
2013 Swift

Con-X EXIST HXR Focus (SIMBOL-X, Explorer ?) 2020

2010

Energy band

Integral XMM Chandra HXR Focus NEXT EXIST Con-X

GLAST

0.1 X-ray

1

100 keV 10 Hard X-ray/soft -ray

100 MeV 1 GeV gamma-ray


New Opportunities
X-ray (0.1 - 10 keV) - Constellation-X Thermal (106 K) plasmas accretion disks, galaxy clusters large-area high-resolution spectroscopy Hard X-ray/soft gamma-ray (10 - 1000 keV) - EXIST, HXR Focuser non-thermal processes (synchrotron, IC,nuclear lines) Relativistic jets in GRBs, microquasars, binaries; SNe, obscured AGN GeV Gamma-ray - GLAST Relativistic jets in blazars, GRB


Hard X-ray Sky
Hard X-ray (~3-600 keV) all-sky imaging each orbit to measure: Highly variable sources, short-lived transients GRBs out to z ~20 and first stellar Black Holes ( ~5-20X Swift sensitivity) Stellar Black Holes in Galaxy & IMBHs in Local Group

Previous Hard X-ray Sky HEAO-1, BeppoSAX 2010 Hard X-ray Sky Swift & INTEGRAL 2017(?) Hard X-ray Sky EXIST


Wide-Field Hard X-ray Imaging: EXIST
·~20X more sensitive than Swift or INTEGRAL and cover full sky ·Detect ~104 sources, 10 positions, 3-600 keV spectra ·unique temporal survey: full sky imaging each orbit

High Energy Telescope HET (10-600keV)
(6 x 3 coded aperture telescopes; 131o x 65o FoV)

Low Energy Telescope LET (3-30 keV)
(4 arrays of 7 x 1 coded aperture telescopes; 116o x 64o FoV)


Radio Connections
Gamma-ray bursts (Kulkarni) Stellar mass black holes(&NS) in Galactic binaries `low/hard states' now believed to be jet-powered down to 10-6 LEddington (through radio observations) High states dominated by accretion disk Jet studies; physical timescales associated with jet formation set by size (mass); days to decades probes jet-accretion disk coupling Radio - indicates jet component Radio nebulae - calorimeters for jet kinetic power Time-constrained (simultaneous w/ X-ray) observations over wide flux range


Focusing in the Hard X-ray Band

optics

NuSTAR Integral
Focal point

NuSTAR

Pinhole camera
High background, large detector, low resolution

Low background, compact detector, high resolution

Focusing telescope


Sensitivity Advance

.0 0 1 Jy


Science Goals
Census of accreting supermassive black holes in the Universe Evolution of SMBH over cosmic time Current Chandra/XMM surveys do not reach F peak in XRB Nature of obscured Galactic binary population Nucleosynthesis and dynamics in supernovae Resolve origin of diffuse Galactic emission Mapping non-thermal components in galaxy clusters, radio galaxies


The 30 keV X-ray date of the extragalactic high energy best view to sky with Integral (2 sq degrees) X-ray sky

Deepest current image; 2 x 2 deg with Integral IBIS, 20 - 40 keV; dominated by the bright glow of unresolved sources


2 x 2 degrees at 30 keV with focusing HXR telescope


Radio Connection
BH Census Deep radio surveys (and mid IR) required to identify Compton thick component Deep imaging observations of selected survey fields Diffuse non-thermal emission Hard X-ray maps IC scattering off CMB, radio maps synchrotron emission - combined can map magnetic field strength in galaxy clusters, relic radio galaxies Low-frequency radio maps


Summary
One of the new frontiers in high energy astrophysics 2010-2020 will be hard X-ray (10 - 1000 keV) time domain sensitivity For fast transients, jets in BH on all scales, evolution of accreting black holes, strong connection to radio observations


Expected EXIST Survey Sensitivity
Continuum Narrow Line

LET 3-30 keV; HET 10-600 keV 0.05mCrab = 5 x 10 band E
low -13

cgs, (over any

2E

low)

5, 1yr, 20-40% duty cycle any source