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ASTROSAT LAXPC. Biswajit Paul Raman Research Institute, Bangalore On behalf of the LAXPC Team. ASTROSAT. EXOSAT-ME : 1983-1986 1.5-15 keV, 1800 sq cm With LE Imaging Telescopes (CMA) GINGA-LAC: 1987-1991 2-37 keV, 4000 sq cm With All Sky Monitor RXTE-PCA: 1996-200? - PowerPoint PPT Presentation
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ASTROSAT LAXPC
Biswajit PaulRaman Research Institute, Bangalore
On behalf of the LAXPC Team
ASTROSAT
EXOSAT-ME : 1983-19861.5-15 keV, 1800 sq cmWith LE Imaging Telescopes (CMA)
GINGA-LAC: 1987-19912-37 keV, 4000 sq cmWith All Sky Monitor
RXTE-PCA: 1996-200?2-30 keV, 6000 sq cmAll Sky Monitor and Hard X-ray Instrument
ASTROSAT-LAXPC:2-80 keV, 6000 sq cmWith All Sky Monitor, Soft/Hard X-ray Instruments, UVIT
Large Area X-ray Astronomical Observatories
USA Exp,2000 sq cmIXAE, 1200 sq cm
IXAE
LAXPC Characteristics Area : 6,000 - 7,500 cm2
Mass: 390 kg
Time Resolution: 10 µs, dead time 30-35 µs
Front-end and Processing Electronics: separate electronics for each detector
Data Storage: Onboard Memory 570 MB per Orbit
Detection Efficiency: 90-100 % upto 20 keV, ~40% upto 80 keV
Energy Resolution: 12-13% at 20-60 keV
Life Time: 3-10 Years, no Consumable
LAXPC: Effective Area
LAXPC: Energy Resolution
LAXPC: Complex Energy Response
• Energy response generation:Monte Carlo simulation / Ground calibration
Spectral Leakage in PCA and LAXPC
PCA LAXPC
Spectral Leakage in PCA
LAXPC Schematic
LAXPC: Complex Energy Response
PCA: Energy resolution of single events and escape events
ASTROSAT Ground Trace
LAXPC Advantages
Large effective area in hard X-ray band
Stable background
Low Spectral leakage
Wide energy band2-80 keV with LAXPC0.3-8 keV with SXT10-150 keV with CZT
Simultaneous, sensitive, multi-band UV/Optical observations
Only timing instrument it this time frame
Studies with LAXPCOnly Timing Instrument it this Time Frame
Hard X-ray Response
X-ray Pulsars (Pulsations, QPOs, Transient Nature, Orbital Evolutions)LMXBs (KHz and Low Frequency QPOs, Hard X-rays)Millisecond Accreting PulsarsRotation Powered Pulsars (Simultaneous Radio observations)BHCs (QPOs and variations in a wide range of time scale)
Pulsar Cyclotron Line Cluster Hard X-rays ?
Sky SurveySky Monitoring
Timing Studies
BH High Frequency QPOs (MAXI!)
CRSF with ASTROSAT LAXPC
Survey with Slew Data and Deep Survey
Radio X-ray Simultaneous Observations of
Millisecond Pulsars: Absolute Timing
ASTROSAT Launch
WindowOctober-December 2011
A Thomson X-ray polarimeter has been designed, developed and successfully tested.
Detectors, Front end electronics, Processing
Electronics, Collimators with flat top response
Test and calibration setup, Rotational stage
An Engineering Model is under fabrication
•Minimum Detectable Polarisation of 3% at 5σ (50 mCrab)
•No of sources: 50
Thomson X-ray Polarimeter for a small satellite mission
Unpolarised sourcePolarised source
Results
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