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Probing Particle Acceleration with Probing Particle Acceleration with X-ray/Gamma X ray/Gamma ray/Gamma-ray ray/Gamma ray ray Polarimetry ray Polarimetry Polarimetry Polarimetry Mar 22, 2012 ASTRO-H Session, ASJ meeting T. Mizuno, H.

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SLIDE 1

Probing Particle Acceleration with Probing Particle Acceleration with X-ray/Gamma ray/Gamma-ray ray Polarimetry Polarimetry

Mar 22, 2012

X ray/Gamma ray/Gamma ray ray Polarimetry Polarimetry

ASTRO-H Session, ASJ meeting

T Mi H T k h hi Y F k

  • T. Mizuno, H. Takahashi, Y. Fukazawa

(Hiroshima Univ), H. Tajima (Nagoya Univ.),

  • T. Tanaka, Y. Uchiyama (KIPAC/Stanford),

S Takeda H Odaka S Watanabe G Sato

  • S. Takeda, H. Odaka, S. Watanabe, G. Sato,
  • M. Kokubun, T. Takahashi (ISAS/JAXA),
  • K. Nakazawa (Tokyo Univ.), P. Coppi

(Yale Univ.) and T. Tamagawa (RIKEN)

1

(Yale Univ.) and T. Tamagawa (RIKEN)

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SLIDE 2

ASTRO ASTRO-

  • H SGD

H SGD

  • Si-CdTe Compton Camera + BGO shiled
  • Constrain incident angle using Compton kinematics
  • Constrain incident angle using Compton kinematics

– efficient background suppression

cosθ = 1+ mec2 − mec2

Background Level

cosθ = 1+ E1 + E2 − E2

Tajima+ 10 Suzaku HXD-GSO

Background Level

Tajima+ 10

Compton Scat.

0.1 Crab

Photo-abs.

Astro-H SGD

2

BG<=100 mCrab

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SLIDE 3

ASTRO ASTRO-

  • H SGD as a

H SGD as a Polarimeter Polarimeter

  • Si-CdTe Compton Camera + BGO shiled
  • Constrain incident angle using Compton kinematics
  • Constrain incident angle using Compton kinematics

– efficient background suppression – polarization measurement

cosθ = 1+ mec2 − mec2

p

cosθ = 1+ E1 + E2 − E2

Tajima+ 10 Takeda+ 10, NIMA prototype test

  • Proc. SPIE

Compton Scat. Photo-abs.

M 0 58 (80 300 k V)

3

M=0.58 (80-300 keV) w/ flight configuration

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SLIDE 4

X-

  • ray/Gamma

ray/Gamma-

  • ray

ray Polarimetry Polarimetry

  • Why polarization? (1) place constraints on source

geometries (2) break model degeneracy geometries (2) break model degeneracy

– Synchrotron emission (magnetic field) – Compton up-scattering radiation (see photons, disk) P l d t QED l l ti it ( t i t – Pol. due to QED or general relativity (constraints on fundamental physics and compact object)

PWN Pulsar BHB, AGN

4

Magnetic field, Accelerated electrons Pulsar emission model, QED Accretion disk, Jet X/γ-ray pol. not subject to Faraday rotation/depolarization

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SLIDE 5

X-

  • ray/Gamma

ray/Gamma-

  • ray

ray SpectroPolarimetry SpectroPolarimetry

  • Measuring energy dependent polarization is crucial to

disentangle emission mechanisms disentangle emission mechanisms

– transition from one pol. generation process to another may

  • ccur over broad energy range

disk reflection model (Matt+93) Blazar model (Poutanen94) 10% disk reflection model (Matt+93)

  • pol. vector disk

Blazar model (Poutanen94)

  • n flux

1% degree h t e photo 1%

  • pol. d

synchrotron IC total

  • l. degree

5

3 10 keV 50 0.1% IC po ** pol. may be low in EC **

slide-6
SLIDE 6

X-

  • ray/Gamma

ray/Gamma-

  • ray

ray SpectroPolarimetry SpectroPolarimetry

  • Measuring energy dependent polarization is crucial to

disentangle emission mechanisms disentangle emission mechanisms – synergy with GEMS and PoGOLite will enhance science outputs

PoGOLite (2012) 30-80 keV lll l ballloon, Plasctic scint.

6

GEMS (2014-) 2-10 keV X-ray mirror+MPGD ASTRO-H SGD (2014-) 40-600 keV Si/CdTe Compton Camera

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SLIDE 7

Case Study 1: Case Study 1: Cyg Cyg X X-1

  • A toy model of polarized emission

– Polarized jet seen by INTEGRAL/IBIS (67% pol., φ=140eg, Polarized jet seen by INTEGRAL/IBIS (67% pol., φ 140eg, contributing in E>100keV) – Disk reflection (3% pol. in 2-10keV and 10% pol. in 30-60 keV, φ=162deg (Long+80)) φ 162deg (Long 80))

  • See how SGD (+others) can measure polarization

HE Jet Disk reflection ( l i d)

C t i ti

HE Jet (polarized) (polarized)

Comptonization (non-pol)

A-H SGD

  • pol. deg.=67+/-30%

(E>=400 keV)

7

Long+80 2.6/5.2 keV hint of weak pol. Laurent+11 (E> 400 keV)

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SLIDE 8

SGD SGD Polarimetry Polarimetry of

  • f Cyg

Cyg X X-1

  • Energy dependent polarization measurement w/ ASTRO-H SGD

– disclose jet component hidden in Comptonization down to j p p 100 keV

INTEGRAL IBIS SGD Simulation, 300 ks 10% polarization @100-180keV INTEGRAL IBIS Modulation Curve@250-400 keV (consistent with no pol.) 17% polarization @180-330keV 17% polarization @180 330keV

8

Tanaka (Stanford)

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SLIDE 9

Wide Wide-

  • band

band Polarimetry Polarimetry of

  • f Cyg

Cyg X X-1

  • Coordination with soft/hard X-ray polarimetry

– disentangle disk reflection and jet emission disentangle disk reflection and jet emission – Compare directions of magnetic field (soft γ), disk (X-ray) and jet (radio)

HE Jet disk reflection disk reflection assumption:

100 ks obs. M=0.32 (GEMS, PoGO) SGD scaled from 300ks sim

Disk reflecti n

e ee

SGD scaled from 300ks sim.

Disk reflection (perpendicular to disk) HE jet (synchrotron)

  • l. angle
  • l. degre

9

(synchrotron)

po po

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SLIDE 10

Case Study 2: Crab Nebula Case Study 2: Crab Nebula

  • A toy model based on the OSO-8/INTEGRAL data

PD 20% PA 156d (2 6/5 2k V) OSO 8 h l N b l

  • PD=20%, PA=156deg (2.6/5.2keV): OSO-8, whole Nebula
  • PD=50%, PA=124deg (>100keV): INTEGRAL, aligned with pulsar rot. axis
  • Let’s assume PD=30% and PA=138deg (30-80keV)

N

PA @2.6/5.2 keV PD=20%

E

PA@ 100 k V PA@ >100 keV PD=50%

10

2’

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SLIDE 11

Case Study 2: Crab Nebula Case Study 2: Crab Nebula

  • A toy model based on the OSO-8/INTEGRAL data

SGD ill fi ( d ) th li t

ASTRO-H/SGD (100 ks)

  • SGD will confirm (or deny) the alignment

with pulsar rot. axis

  • Constraints on PWN model w/ soft-X and

hard-X data

gle

N

PA @2.6/5.2 keV PD=20%

INTEGRAL/SPI (1.2 Ms)

har X ata

  • pol. an

E

PA@ 100 k V

(1.2 Ms)

ee

PA@ >100 keV PD=50%

  • l. degre

11

2’

po

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SLIDE 12

Summary and Prospect Summary and Prospect

  • Pol. measurement by A-H SGD can place constraints
  • n source geometry and break model degeneracy
  • n source geometry and break model degeneracy

(qualitatively new type of information)

  • Synergy with X-ray polarimeters will enhance science

t t

  • utputs
  • Two case studies are presented (Cyg X-1 and Crab;

robust targets for SGD polarimetry) robust targets for SGD polarimetry)

  • Pol. measurement of pulsars and AGN flares will also

be possible (to understand BG anisotropy is important)

Thank you for your Attention

12

Thank you for your Attention

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SLIDE 13

Backup Slides Backup Slides Backup Slides Backup Slides

13

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SLIDE 14

X-

  • ray/Gamma

ray/Gamma-

  • ray

ray SpectroPolarimetry SpectroPolarimetry

  • Measuring energy dependent polarization is crucial to

disentangle emission mechanisms disentangle emission mechanisms

disk reflection model (Matt+93) pol vector disk Strong polarization (67%) from Cyg X-1 jet in HE (Laurent+11) 10%

  • pol. vector disk

Cyg X-1 jet in HE (Laurent+11) e 1%

  • l. degree

67% pol.

0 1% po

  • pol. <20%

14

3 10 keV 50 0.1%

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SLIDE 15

Polarization Polarization

  • 光源が非一様だと偏光が生じる

そろ た磁場 シ ク – そろった磁場下でのシンクロトロン – 特定の面でのコンプトン散乱

Unpolarized

15

Polarized

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SLIDE 16

Crab Nebula Polarization (X Crab Nebula Polarization (X-

  • ray)

ray)

  • Measured by OSO-8 (Bragg reflection)

P i i l Position Angle 2.6 keV 5.2 keV Modulation @2.6 keV

16

Weisskopf+78

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SLIDE 17

Cyg Cyg X X-

  • 1 Radio Jet

1 Radio Jet

  • 8 GHz images at three orbital phases (1998 August)

17

Stirling+01