SVadawale CZTI Polarimetry 17feb17 - Hiroshima...
Transcript of SVadawale CZTI Polarimetry 17feb17 - Hiroshima...
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Hard X-ray Polarimetrywith
Astrosat-CZTISantosh Vadawale
Physical Research Laboratory, Ahmedabad
2nd CORE-U International Conference: Cosmic Polarimetry from Micro to Macro Scales
17-18 February 2017, Hiroshima
On behalf of the CZTI team
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CZTI Team
Ø TIFR: A. R. Rao, M. K. Hinger, A. P. K. Kutty, J. P. Malkar, Milind Patil, Rakesh Khanna, Yash Bhargava, Vikas Chand, Debdutta Paul
Ø IUCAA: Dipankar Bhattacharya, Varun Bhalerao, G. C. Dewangan, Ranjeev Misra, Ajay Vibhute, Vedant, Shrikant
Ø PRL: Santosh Vadawale, Mithun N. P. S., Tanmoy Chattopadhyay (currently at PSU)
Ø VSSC: S. Sreekumar, P. Vinod, Essy Samuel, Priya
Ø SAC: Arvind Singh, Tanul
Astrosat Project Team
Astrosat Mission Team
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OutlineØ Astrosat
§ Introduction
§ CZT-Imager
§ CZTI as GRB detector
Ø X-ray Polarimetry with CZTI
§ Experimental confirmation
§ Analysis details
§ Crab results
§ GRB results
Ø Summary
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Astrosat
for Multi-wavelength Astronomy
Collaborative project of
§ Many premier Indian research institutes
§ + two international parterres
India’s first dedicated satellite
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AstrosatØ 650 km, low inclination (6 deg) orbitØ Launched by Indian PSLV on 28th September 2015Ø Observatory class, Proposal driven mission from 2nd year
§ Simultaneous multi-wavelength monitoring of broad range of cosmic sources.
§ Sky surveys in the hard X-ray and UV bands.
§ Broadband spectroscopic studies of X-ray binaries, AGN, SNRs, clusters of galaxies and stellar coronae.
§ Studies of periodic and non-periodic variability of X-ray sources.
§ Monitoring the X-ray sky for new transients.
Main scientific focus
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AstrosatØ LAXPC: Large Area X-ray Proportional Counters
§ Aeff ≈ 6000 cm2; FOV =1° X 1°; 3-80 keV; Res: 9% @ 22 keV
Ø CZTI: Cadmium-Zinc-Telluride Imager with Coded Aperture Mask§ Aeff ≈ 500 cm2; FOV = 6° X 6°;10 – 100 keV; Res: 6% @ 60 keV
Ø SXT : Soft X-ray Telescope using conical-foil mirrors§ Aeff ≈ 200 cm2 ; FOV = 0.5°; (~3‘ res); 0.3-8 keV; Res: 2% @ 6 keV
Ø SSM : Scanning Sky Monitor with 3 PSPCs and CAM§ Aeff ≈ 30 cm2 (each); 2-20 keV. Res: 20 % @ 6 keV
Ø UVIT : Ultraviolet Imaging Telescope § Two telescopes each with 38 cm aperture; N-UV, F-UV and visible bands.
Five Instruments
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Astrosat CZTIHard X-ray Spectroscopy and Imaging
Core Science AreaØ Galactic X-ray binaries:
§ Long term Spectro-temporal monitoring
§ Understanding disk-jet connetion with simultaneous multi-wavelength obsservations GMRT
Ø Pulsars:§ Searching hard X-ray
counterparts for Fermi-LAT pulsars.
Ø Gamma-ray Bursts:§ Hard X-ray spectro-
polarimetric properties of very bright GRBs
Coded Mask imaging with pixilated CZT detectors
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CAM assem bly
Colima tor hs g. a s s embly
Calibration hsg. assem bly
Mother board assembly
Details of a Quadrant
Detector Box Assembly
Size - 484 x 484 x 600 mm3
Weight - 50 kg Power- 50 Watts
Two FOVs: 4.67°× 4.67°; ~80°×80°
Shield Material – Tantalum + Aluminum(Passive shielding up to 100 keV)
Four Independent QuadrantsCZT-Imager
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CZT-Detector planeSpecifications
§ Total area 976 cm2
§ Total pixels 16384
§ Pixel size 2.46 x 2.46 mm2
§ Field of view 4.67° x 4.67°
§ Angular resolution 8'
§ Energy resolution 8 % (@60 keV)
§ 4 x 4 cm2 (16 x 16 pixel)
§ 5 mm thick
§ ASIC based readout (2 x 128 ch. ASIC)
§ Total 64 modules (16 in 4 quadrants)
Orbotech CZT modules
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Crab ResultsFirst Image Later image (less artifacts)
Pulse profilePI = 2.09
Spectrum
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11
Mayukh Pahari / J S Yadav / Mithun
Powerlaw Index: 2.1
Powerlaw Norm free; (yet to be finalized).
Good χ2
Ø Relative normalizations are yet to be optimized§ Some issues in cross-calibration of all X-ray instruments
è Expected to be resolved soon
Crab: simultaneous fitting with LAXPC
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Ø CZTI mask, collimators support structure designed up to 150 keV
Ø CZTI has good sensitivity to GRBs in 150 to 400 keV energy range
Ø First GRB on first day / first observation
Ø Extremely useful for optimizing noise reduction and data cleaning
GRBs with CZTI
Earth
Crab Crab
GRB151006A
CZTI Effective Area
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GRB 160131AGRB 160119A
GRB 160623A
GRB in CZTI FOV!!
GRB 160325A
Alerts on dedicated web page: http://astrosat.iucaa.in/czti/?q=grb
Many more GRBs
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X-ray polarimetry with CZTIØ Pixilated detectors in principle can measure polarization
§ Many attempts to measure polarization from instruments not optimized for polarimetry (RHESSI, Integral-IBIS, Integral-SPI)
Ø Can Astrosat CZTI measure X-ray polarization?§ May be above 100 keV (due to scattering probability / threshold)
(Capability in modules? Preserved in data? Meaningful sensitivity? )
For scattering polarimetry with Pixilated detectors è azimuthal bins are unequal
minmax
minmax
CCCC
+-
=µ100µµPP =
( )TRR
RMDP bkgsrc
src
+=
100
29.4µ
Compton polarimetry
Electric field vector of the incident photon
Low Z scatterer
Surrounding detector
Probability
jqjqnn
nn
nns ddrd e ÷
øö
çèæ -
¢+¢
÷øö
çèæ ¢
= 2222
cossin22
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Proof-of-ConceptØ Verify multi-pixel capability of CZTI
modules
§ ~70 % Polarized beam produced by 90° Compton scattering of 122 keV X-rays from Co57
§ Energy of polarized X-rays ~100 keV
§ Time tagging à 20 µs
Time between two events Adjacent double pixel events, E2/E1>2
Co57
SourceScatterer
CZT
Polarized X-rays
CZTI Modules can detect simultaneous multi-pixel eventsE
Chattopadhyay et al. (2015)
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Modulation Curve
Ø Modulation curve has only 8 bins, which have non uniform angular coverage
Ø Can be normalized with modulation curve for unpolarized beam
obsiunpoli
unpolnori N
MMN ,
,, =
100 % polarized
Unpolarized
(Lei et al., 1997)
8 bin azimuthal histogram with low energy pixel as scattering pixel
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X-ray polarimetry with CZT-ImagerØ Significant Compton scattering
probability in 100 – 300 keV
Ø CZTI does have significant polarization capability
Ø Critical steps è event selection, background subtraction, geometry correction
Ø Experimentally verified simulations:~10% MDP for 1 Crab source in 500 ks
Vadawale et al. (2015)
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CZTI Polarimetric observations
Simulations for CZTI show that for 1 Crab source 20 % to 60 % polarization should be detected in ~100 to 20 ks
Ø Many GRBs detected so far by CZTI
Ø Total 14 observations of Crab in first year § Exposure ranging from 10 ks to ~140 ks
Ø Almost bi-weekly monitoring of Cygnus X-1 in hard state§ Exposures ranging from 15 ks to ~120 ks
à Accurate background subtraction is critical§ Background modulation due to Earth albedo is
declination dependentà Need blank sky observations with similar DEC as source,
results in relatively small exposure ~60 ks to 80 ks
X-ray Polarimetry StatusØ Only confirmed measurements: Crab, Cygnus X-1(?), few GRBsØ Any additional contribution is highly valuable
A
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CZTI Polarization AnalysisEvent selection:Adjacent double pixel events satisfying Compton criteria
Ø Validation of event selection
§ GRB Compton events light curve
§ Crab pulse profile
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Background analysisØ Background pattern changes with DECØ Need to select blank sky observations with
same DEC as CrabØ Both Crab and Cygnus X-1 should be more
then 80° away Ø Small region of sky suitable for Crab
backgroundØ Background rate varies with ground trackØ Selecting only similar tracks result in
significant reduction in exposureØ Manually optimize back ground regions and
correct for exposure
Ø Rate difference does not affect modulation or polarization angle
Ø It may only affect the polarization fraction à systematic uncertainty ~10%
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Crab PolarizationAll data added à Total exposure ~550 ks
Polarization Fraction è33.8±5.8
Polarization angle è143.0±2.8
Polarization Fraction è50.4±12.0
Polarization Angle è139.5±3.2
Off-pulseTotal Crab Polarization AngleIn general direction of the rotation axis
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Crab PolarizationAll data added à Total exposure ~550 ks
Ø Consistent measurements over time
Ø Monthly averaging to get typical exposure à 100 ks
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GRB Polarization Ø CZTI had detected more then 50 GRBs
during first year§ 11 are suitable for polarization analysis § Selected based on number of Compton events
(> 350)
Ø Modulation detection in GRB is relatively easy§ Accurate background available pre / post GRB§ High signal-to-noise§ Optimize signal by ignoring shadowed regions.
Ø Estimation of accurate polarization fraction is difficult as GRBs are highly off-axis§ Requires modulation curves for both 100% and
completely unpolarised X-rays from the location of GRB
§ Obtained by extensive Geant4 simulations with the mass model of full spacecraft
§ Require extensive computing effort
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PF
9054703895-
19-
725781
GRB Polarization Selected GRBs with initial values for polarization fraction
Ø Extensive stastical analysis is under progressØ Will be reported in near future
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Cygnus X-1 Polarization Ø Cygnus X-1 is in hard state through out 2016
Ø Many monitoring observations, typically of duration 15 – 20 ks
Ø Few longer exposure ~120 ks (accidental)
Ø Initial polarization analysis of few observations
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Ø Astrosat-CZTI is proven to have good polarimetric capabilities in extended energy range of 100 – 300 keV
Ø Most accurate measurement of Crab hard X-ray polarization§ First time possibility of phase resolved polarimetry of Crab§ Show rich variations§ New challenges for the pulsar emission models
Ø CZTI is also a prolific GRB detector and polarimeter§ Detected more then 50 GRBs in first year§ 11 of them suitable for polarization analysis§ Show variety of polarization signatures§ Potential to constrain GRB models with bigger sample
Ø Many observations of Cygnus X-1§ Few of them suitable for polarization analysis§ Work under progress… but initial analysis show promising
results
Summary
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Thanks…