Compton Polarimetry ICompton Polarimetry In Gamma-ray Astronon Gamma-ray Astrono

mymy

Jeng-Lwen, ChiuJeng-Lwen, Chiu

Institute of Physics, NTHUInstitute of Physics, NTHU

2006/01/122006/01/12

OutlineOutline

1.1. IntroductionIntroduction

2.2. Polarized Gamma-Ray Emission Polarized Gamma-Ray Emission MechanismsMechanisms

3.3. Potential Astronomical Potential Astronomical SitesSites of Polarized Gam of Polarized Gamma-Ray Emissionma-Ray Emission

4.4. A Review of Gamma-Ray Polarimetric A Review of Gamma-Ray Polarimetric InstrumInstrumentationentation

5.5. Computer and Laboratory Computer and Laboratory Tests ofTests of Novel Novel PolaPolarimetric Techniquesrimetric Techniques

6.6. ConclusionConclusion

IntroductionIntroduction

For the most part, the analysis of compact X-ray and gamma-ray sources has been confined to spectral characteristics and time variability.

This analysis often allows two or more very different models to successfully explain the observations.

It is possible to double the number of observational parameters through measurements of the polarization angle and degree of linear polarization of the source emission to discriminate between the various models.

Polarized Gamma-Ray EmissionPolarized Gamma-Ray Emission

Magneto-Bremsstrahlung RadiationMagneto-Bremsstrahlung Radiation

Cyclotron EmissionCyclotron Emission

Synchrotron EmissionSynchrotron Emission

Curvature RadiationCurvature RadiationBremsstrahlung RadiationBremsstrahlung RadiationCompton ScatteringCompton ScatteringMagnetic Photon SplittingMagnetic Photon Splitting

Cyclotron Emission

Synchrotron Emission

Bremsstrahlung Radiation

Compton Scattering

Magnetic photon splitting

Potential Astronomical Sites of Potential Astronomical Sites of Polarized Gamma-Ray EmissionPolarized Gamma-Ray Emission

Gamma-Ray BurstsGamma-Ray BurstsPulsarsPulsarsSolar FlaresSolar FlaresOther Possible Sites for Polarized EmissionOther Possible Sites for Polarized Emission

Crab NebulaCrab Nebula

AGNsAGNs

Galactic Black Hole CandidatesGalactic Black Hole Candidates

Gamma-ray Pulsars

• Only 7 gamma-ray pulsars are known to exist. (e.g. Crab, Vela, Geminga (radio-quiet) )

• Polarization characteristics of gamma-ray pulsars: rare information & difficult to collect.

• Optical polarization of Crab pulsar (Smith et al. 1988).

• Observations of the polarization of the pulsed optical emission: both the angle and the degree of polarization change during the period of the pulses.

• The similarities in the polarization characteristics indicate that the pulses originate from two separate sources with the same emission mechanism.

• Polarization: the key to differentiating between

polar cap models &

outer gap models ?!

γ-Ray Polarization Instrumentationγ-Ray Polarization Instrumentation

The measurement of the degree of linear polarization of The measurement of the degree of linear polarization of was was firstfirst reported in 1950 by Metzger and Deustch, whe reported in 1950 by Metzger and Deustch, when they exploited the Compton scattering process n they exploited the Compton scattering process to meato measuresure the asymmetry in the azimuthal distributionthe asymmetry in the azimuthal distribution of sof scattered gamma-rayscattered gamma-rays..

Since then polarimeters have been constructed with ever Since then polarimeters have been constructed with ever increasing sensitivitiesincreasing sensitivities. .

Several X-ray polarimeters but few dedicated gamma-raSeveral X-ray polarimeters but few dedicated gamma-ray polarimeters have been launched. y polarimeters have been launched.

• The differential Compton cross-section, dσ, is the probability that a photon of energy E will suffer a c

ollision with an electron in a medium in which the electron density is 1 cm-3.

ξ/(ξ‘) : electric vector of the incident/(scattered) photon

Φ : the angle between incident and scattered photons

r0 : classical electron radius

me : mass of an electron

θ: the angle between the incident photon direction and the scattered photon

direction.

η: the azimuthal angle of the scattered photon with respect to the electric

vector of the incident photon

azimuthal angle of the scattered photon wrt. the electric vector of the incident photon

electric vector

angle between the incidentphoton direction and the scattered photon direction

• After averaging over the electric vector of the scattered photon, the differential cross-section can be rewritten as (4.2) (Evans, 1955)

• For a fixed scattering angle, the cross-section will be at a maximum for those photons scattered at right angles to the direction of the electric vector of the incident photon.

• This will lead to an asymmetry in the number of photons scattered in directions parallel and orthogonal to the electric vector of a beam of photons incident on some scattering medium.

• By a suitable arrangement of detector elements this asymmetry can be used to determine the direction and degree of polarization of the beam.

used to scatter photons from the source into a detector at B.

rotated about η until a maximum is found in the coincidence counts between A and B.

Q polarimetric modulation factor : the response of the polarimeter to a 100% polarized beam of photons (Suffert 1959)

The theoretical form of the Q factor at an angle Φ with respect to the X-axis,

for a given polarization vector angle with respect to the X-axis, Ψ

Computer and Laboratory Tests of Computer and Laboratory Tests of Novel Polarimetric TechniquesNovel Polarimetric Techniques

Polarization DependentPolarization Dependent M-C CodeM-C Code Polarization Data AnalysisPolarization Data Analysis The Moving Mask Technique (The Moving Mask Technique (MMTMMT)) The Radial Bin Technique (The Radial Bin Technique (RBTRBT)) Systematic Modulation EffectsSystematic Modulation Effects Effect of Effect of Non-UniformNon-Uniform Polarimetric Response Polarimetric Response Effect of Effect of Off-AxisOff-Axis Incidence Incidence Effect of Effect of Background NoiseBackground Noise Effect of Effect of PixellationPixellation Laboratory Laboratory TestsTests with Pixellated Detector Arrays with Pixellated Detector Arrays The Geometrical The Geometrical OptimizationOptimization of a Pixellated Planar of a Pixellated Planar

PolarimeterPolarimeter

Polarization Dependent Polarization Dependent M-C CodeM-C Code

a Si(Li) detector is used as the scattering element and two Ge detectors are used as the analysers.

the Swinyard et al. (1991) method: the Compton polarization algorithm is applied only to the first scattering of the incident photon

Polarization Data AnalysisPolarization Data Analysis

The simple determination of the Q factor used in The simple determination of the Q factor used in the classic Compton polarimeter data analysis the classic Compton polarimeter data analysis ccannot be used with non-rotationalannot be used with non-rotational polarimeters s polarimeters such as COMPTEL.uch as COMPTEL.

Consequently Consequently two analysis routinestwo analysis routines for determini for determining the Q factor have evolved the ng the Q factor have evolved the Moving Mask Moving Mask Technique (Technique (MMTMMT)) and the and the Radial Bin TechniqRadial Bin Technique (ue (RBTRBT)). .

The Moving Mask Technique (MMT)

each event is transformed onto a displacement plane showing the deviation in the detector X and Y-axis directions (ΔX, ΔY) between the two interactions. A mask is then applied to the data dividing the displacement plane into quadrants.

The mask is rotated, usually in 2 or 5∘steps∘ , and the resultant distribution of

Q(Φ) is fitted to the cos2Φ form given by Equation (4.10) to find the maximum Q factor and the angle of the polarization vector.

Problem of MMT

1) the most significant is the non-independence of Nn(Φ).2) the smearing effect due to the broad binning size.

• A single event will be sampled many times during the analysis.

The Q(Φ) points will also be non-independent and so the variance in Q(Φ) cannot be used to obtain the errors in the determined Q factor and the polarization angle.

• One way to avoid the non-independent data points problem is to reduce the mask size (e.g., to 15 ) and move t∘he masks in step size equals to the mask size.

• the smearing effect is also significantly reduced.

The Radial Bin Technique (RBT) The RBT tackles the problem of determining the Q factor by dividing up the displacement plane into a number of equal sized radial bins, usually 15 or 24 in size giving 24 or 15 ra∘ ∘dial bins, respectively. Each event is placed into its corresponding bin and the radial distribution is fitted to the expression

(P1: the amplitude of the curve; P2: the polarization angle; P3: the average height of the curve. )

All of the N(Φ) points are independent and thus the errors in each parameter can be simply determined from the variance of the points from the fitted curve.

Minimum degradation in the Q factor vs. sufficiently large size as to ensure the best possible statistics for the Q(Φ) points. Bin sizes of between 10 and 30 are s∘ ∘uitable.

Degree of linear polarization

1.1% 2.9% 10%

• The above comparisons with analytical calculations have shown the validity of using either the Moving Mask Technique (MMT) or the Radial Bin Technique (RBT) to analyze the polarimetric distribution for a continuous and uniform detector plane in an ideal case.

• Practical limitations of a polarimeter & ways of removing their undesired side effects

Systematic Modulation EffectsSystematic Modulation Effects

Non-uniform

As the distribution of events on the displacement plane is highly dependent upon the detector geometry, this will result in the distortion of the Q distribution, masking the polarimetric signature or even possibly creating a false result.

Polarimeter calibration: The effect of the non-uniformity can be removed using the detector response to non-polarized photons.

Off-axisIt is necessary to transform each point on the displacement plane onto a new displacement plane normal to the incident photon direction so the true polarimetric distribution.

Assuming the incident direction is at (α,β) azimuth and zenith angles; (ΔX, ΔY, ΔZ) is the displacement in the coordinates of the polarimeter (or telescope)(ΔX’, ΔY’, ΔZ’) is the displacement in a coordinates whose Z’-axis is in the direction of the incident photon and the X’-axis is in the X-Y plane of the telescope coordinates.

After the transform, one can proceed with the removal of off-axis and non-uniform response effects and perform the polarimetric analysis using either the MMT or RBT techniques.

(By RBT)

Effect of Background Noise

The minimum detectable polarization (MDP), at n-σ level. SF: the source flux in units of (photons/s*cm2), B: the background flux in units of (counts/s), Q100: the modulation factor of the polarimeter to 100% polarized photons, A: the detection area in cm2, ε: the detection efficiency T: the observation time in seconds.

If background is not removed Reduced Q value & introduce pseudo polarimetric modulation

In order to minimize the background effect, its distribution has to be measured by an on/off observation strategy or derived by detailed modeling.

Background noise, if well understood and properly removed, will not degrade the polarimetric characteristics, such as the detection efficiency and modulation factor, of a polarimeter. It will, however, reduce the sensitivity of a polarimeter statistically.

• There are three principle pixel shapes which will tessellate to form a continuous detection plane: triangular pixels, square pixels and hexagonal pixels.

• The polarimetric analysis of a pixellated detector plane requires significant alteration of the RBT and takes the form of the Decoupled Ring Technique (DRT).

Effect of Pixellation

The DRT analysis is conducted by first selecting only those events where energy is deposited in two pixels. One pixel is then transformed onto the central pixel of a pixellated displacement plane. In this technique, the resultant distribution shows the displacement as pixels rather than in terms of ΔX and ΔY.

Unfortunately, using pixellated detectors, it is impossible to determine the exact location of the interaction site. Thus, for the purposes of the DRT, the interaction is generally assumed to occur at the centre of the pixel. Radial binning cannot be applied in this technique because of the centering that has occurred due to pixellation. The N(Φ) points occurring at the wrong Φ.

Effect of Pixellation In the DRT, the number of events in a displacement plane pixel is used instead of the number of events in a radial bin:

Azimuthal distribution: N(Φ) P(Φ)

( P(Φ): the number of events in a displacement plane pixel whose centre is Φ from the X-axis. )

Complications:

1) The pixels subtend a finite angle. The first ring of pixels that surround the central pixel, 1DR (1st Decoupled Ring), subtend the greatest angle, whilst those in subsequent rings subtend increasingly smaller angles. The important effect is that in general the 1DR ring will contain the highest number of events and will thus have the best statistics for fitting. The 1DR ring also subtends the largest angle and will thus suffer the greatest degree of smearing.

2). Events detected in the 1DR have a much broad range of scattered angle, while events detected in the 2DR or higher will have more narrowly restricted around 90∘, due to the finite thickness of the detector plane. cf. Fig 4.3 lead to higher Q factor.

It is impossible to completely decouple the P(Φ) distribution for these cases.

In practice the DRT is best suited to hexagonal pixels

It is usually sufficient to only decouple the 1DR ring, as this is where the smearing is most apparent.

Effect of Pixellation

(By RBT)

Q=0.215 1DR

Q=0.393 2DR

The de-coupled ring method can be used, so as to maximise the sensitivity of the polarimeter.

Laboratory TestsLaboratory Tests

with Pixellated Detector Arrayswith Pixellated Detector Arrays

The experimental setup of the polarization measurement.

The electronic system has been set to only accept those events that occur in triple coincidence.1). A signal must be received from the photomultiplier tube, indicating that one of the two emitted photons has been detected.2). A second signal must be received from the central pixel due to the alignment of the collimator3). Final signal must be received from one of the surrounding pixels. The selected photons are ~17% polarized (Hills, 1997), a polarization angle of approximately 120∘to the module X-axis.

Experiment (Hills 1997)

37 discrete CsI(Tl)-photodiode detectors housed in a spark eroded aluminum honeycomb structure.

Non-pol Polarized

About the TestSimulation: GEANT M-C simulations were used to determine the module’s response to 100% polarized photons. For 1.173 and 1.332 MeV photons it yields Q100 = 0.263. For a 17% polarized beam as was used in the measurement, the expected Q factor is 0.0444.

Results: The experimentally determined Q factor of 0.0356±0.0040 is in good agreement with this prediction and corresponds to Π=(13.6±1.7)% which is again in good agreement with the 17% polarization expected. The polarization angle should be approximately 120 and the determined value of ∘ (129.0±3.3)∘is only 2.7σ away.A good agreement!!

Conclusion: 1). it has demonstrated the ability of the simulations to successfully match both experimental data and analytical predications based on nuclear theory. This validates the calibration/correction approach developed for the analysis of data from more intricate detectors and telescopes, such as COMPTEL and INTEGRAL. 2). it has conclusively shown that a pixellated detector plane, such as those adopted for the INTEGRAL telescope is an effective polarimeter

The Geometrical OptimizationThe Geometrical Optimization

of a Pixellated Planar Polarimeterof a Pixellated Planar Polarimeter

The product of the modulation factor Q and detection efficiency ε is normally called the figure of Merit (FOM) In general optimizing the design of a polarimeter is simply the process of achieving the best combination of the Q factor and the efficiency. Unfortunately an increase in one generally leads to a reduction in the other.

Choice of scintillator: A single material for all elements shifts the effective energy band towards the higher energy. Such a behavior is due to the impossibility for the same material to be both a high efficiency scatter (for which low Z is recommended) and a highly efficient absorber (for which high Z is required). To lower this limit, it is necessary to use different materials as scattering and absorbing elements. (e.g. CsI, CsF2, and Plastic )

Low-energy threshold: The low-energy threshold of the individual pixels is another crucial factor which determines the operational energy range of a polarimeter and it performance. 1). Hills (1997) studied the FOM as a function of the low-energy threshold for various incident energies in the case of a CsI-based polarimeter. It was found that the peak value of the FOM in CsI occurs at higher incident photon energies as the low-energy threshold increases, but remains at roughly a constant value. 2). Costa et al. (1995) found that the FOM dropped by a factor of 5 for a CaF2 polarimeter to Crab spectrum type incident photons by increasing the low-energy threshold from 5 keV to 30 keV. the low energy threshold of individual pixels should be kept as low as possible so as to ensure that the polarimeter operates at low energies where astronomical sources are strongest and mostly polarized.

Pixel size: Both the length (depth) and cross-section size of the pixel of the detector plane will greatly affect the performance of a polarimeter. The FOM tends towards a maximum for depths In terms of the pixel design, the scintillator depth should be kept as shallow as possible A smaller pixel size leads to better FOM

Pixel size --- Depth5~7 cm

Pixel size --- AF-distanceHexagonal: its size is represented by the Across-Flats (AF) distance (from one edge of the hexagon to the opposite edge).

Optimum pixel configuration

maximizing the polarimetric sensitivity of aplanar polarimeter using CsI pixels

Conclusion (1)Conclusion (1)

The measurements of the polarization angle and degree of linear polarization of the source emission will help us identify the mechanism.

Optical polarization of Crab helps identify the mechanism.

Gamma-ray polarization will be the key to differentiating between polar cap models and outer gap models

The Compton scattering process can be exploited to measure the asymmetry in the azimuthal distribution of scattered gamma rays.

Polarimetric modulation factor Q

Conclusion (2)Conclusion (2) The recent developments in polarimetric techniques, in both data analysis and instrumentation, have been discussed. It is important to incorporate the Compton polarimetric algorithm into a M-C c

ode in full, otherwise significant discrepancies from experimental results will occur at low energies.

For a continuous detection plane, analytical calculations have shown the validity of using either the MMT or the RBT to analyse polarimetric distributions.

For pixellated detector plane, it is necessary to use the DRT and this type of analysis is best suited to hexagonal tessellation (square also).

Systematic Modulation Effects (e.g. Non-Uniform Polarimetric Response, Off-Axis Incidence, Background Noise, Pixellation) could be removed or reduced by calibration.

The results of the tests made by Hills (1997) & Kroeger et al. (1997) showed the good agreement among simulations, experimental data, and analytical prediction.

The Optimum pixel configuration has been tested by FOM. (a long bar)

ReferenceReference

Lei, F., Dean, A. J., and Hills, G. L.: 1997, Lei, F., Dean, A. J., and Hills, G. L.: 1997, Space Science Reviews Space Science Reviews 8282, 309., 309.

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