2019 11CTAmeeting ppt Multiwavelength Imaging SpectroPolarimetry for Transient

2019 -11_CTAmeeting. ppt Multiwavelength Imaging. Spectro-Polarimetry for Transient Objects (多波長偏光分光撮像観測で探る突発現象) November 15, 2019@CTA meeting Tsunefumi Mizuno (Hiroshima Univ. ) K. Kawabata, Y. Fukazawa, M. Uemura (Hiroshima Univ. ), H. Nagai (NAOJ) 1/22

Polarization (1) • Electron path Magnetic field line (B) photon polarization vector ⊥ B direction 2/22

Polarization (2) • Reflected photons are polarized Sun w/o polarization filter reflection (pol. ) w polarization filter surface reflection + bottom (polarized + unpolarized) water surface bottom (unpol. ) • Unique probe to geometry of compact objects (light source and accretion disk) not accessible (in most cases) by imaging 3/22

3 C 279 (Abdo +10, Nature 463, 919) • Optical polarization aided with MW obs. revealed (possible) helical magnetic field associated with flare 4/22

Imaging-Spectro-Polarimetry for Transients • Polarization is powerful probe to magnetic field and source geometry – It improves our understanding of transient jets – Multiwavelength observation is important • Hiroshima group promotes SGMAP project aiming unbiased polarimetric-survey of Northern sky in optical – To. O observation of transients and monitoring of sources in optical polarization possible • Coordinated polarimetric obs. with radio and X-ray would provide vital information • (g-ray (Fermi, CTA) will also play key role) 5/22

SGMAP: Overview • ‘ 6/22

SGMAP: Telescope • Two options under consideration 1 st candidate 2 nd candidate or 1. 3 -m Telescope (ISAS/JAXA) Kanata 1. 5 telescope (Hiroshima) ü Just remove tertiary mirror or ü Replace 2 ndary mirror (To enlarge the vignetting-free FOV) Higashi-Hiroshima Observatory Recently ISAS decided to call for new proposal to make full use of 1. 3 -m telescope. (Relocation from Sagamihara campus is possible) ü Relocate to Higashi-Hiroshima Observatory ü Remove tertiary mirror or replace secondary mirror 7/22

SGMAP: Survey Plan • Primarily for polarimetric survey (60% of sky in 5 ys) – 1 set obs. 4. 6 min. , 100 sets per night => 46. 4 deg 2/day • ~10% time for transient monitor also possible ‘ Region 1’: Higher priority for multi -wavelength study of Galactic structures including Radio loop/Fermi bubble region. 8/22

Improvement by SGMAP • Past sparse survey (~9000 stars in Heiles 2000) => Dense survey (>106 stars) by SGMAP Red dots: Stars brighter than V=14 (will be observed dy SGMAP) No star in Heiles (2000) Black squares : Samples registered in existing catalog (Heiles 2000) 14 stars in Heiles(2000) 9/22

SGMAP: Schedule • Optimistic schedule Fiscal Year Telesocpe/Dome Instrument 2019 Final selection of candidate telescope Design completion, fabrication of optical components 2020 Refurbrishment, installation Detector unit Lens unit Assembling Mounting to telescope Experimental observation 2021 Observation/ Data reduction Survey obs. starts Region 1 2022 -23 Obs. Region 1 2024 -25 Obs. Region 2 Data reduction 2026 -28 (Obs. Region 2) Data reduction Catalogue release 10/22

ALMA • Largest millimeter/submillimeter array by Europa, North America, East Asia with Republic of Chile • 66 high precision antennas at 5000 m altitude (Atacama desert) • ACA (4 12 -m antenna + 12 7 -m antenna) and Band 8&10 receiver by Japan • Cycle 7 operation ongoing ACA 11/22

Polarimetry with ALMA • Imaging-polarimetry from Cycle 3 (2013) • First full pol. obs. (3 C 286) supports aligned B near the jet base • Many more results recently, To. O (< a few days) possible SS 433 (Brundell +18) GRB 171205 A (Urata +18) 3 C 286 (Nagai +16) GRB 190114 C (Laskar +18) 12/22

Ka. VA and Polarimetry • Ka. VA = VERA(Japan)+KVN(Korea) joint array • 3 VERA and 3 KVN antennas dual polarized – VLBI polarimetry now possible Ka. VA network M 87 by VERA vs. Ka. VA 13/22

X-ray/g-ray Polarimetry • Only a few measurements in X-ray/g-ray – – Integral (Crab, Cyg X-1) in >100 ke. V Po. GO+ (Crab, Cyg X-1) in 20 -160 ke. V ASTROSAT (Crab, Cyg X-1) in > 100 ke. V Hitomi SGD (Crab) in >60 ke. V • In soft X-ray (<10 ke. V), Crab Nebula is first and only positive detection OSO-8 satellite (1975 -) Weisskopf 18 14/22

IXPE Mission • With IXPE, we can study several 10 s sources in soft X-ray polarization • NASA and ASI collaboration, NASA SMEX mission, launch in April 2021, baseline duration 2 years • Japanese group provides key devices of the instruments • Data are made public after validation Weisskopf 18 15/22

Pol. Measurement Principle • Direction of photoelectron is parallel (on average) to incident X-ray polarization pol. direction GEM (RIKEN) Electron track image Gas pixel detector (GPD) 16/22

IXPE Instruments • Mirror Module Assembly + GPD, test with EM underway MMA Engineering Unit 3 MMAs, 210 cm 2 (2. 3 ke. V) each Thermal Shields (Nagoya) HPD < 25" Outer Housing ΔE@5. 9 ke. V (stability test) 17/22

IXPE Scientific Capability • Time to reach minimum detectable polarization (MDP) ~100 times shorter than that of OSO-8 • Various classes of sources accessible Crab Nebula 18/22

Scientific Capability (Contd. ) • X-ray imaging polarimetry for the first time • For example, Cen A: Targets under discussion (Tobs=1 -10 days) – B field configuration of jet – ULX contamination excluded – (employ Stokes-param. based analysis to fully utilize imaging capability) 19/22

Strategy of MW Polarimetry • Dedicated observation by SGMAP for selected IXPE targets during its observation (planned or To. O) – If rapid polarization change detected, will issue trigger for ALMA/Ka. VA polarimetry • Repetitive pol. survey by SGMAP for AGNs of Vmag >14 – If rapid polarization change detected, will issue trigger for ALMA/Ka. VA/IXPE polarimetry • Comments and possible collaboration welcome 20/22

+ Fermi, CTA • Fermi has large FOV (~2. 4 sr) and provides daily light curve of every source • Follow-up in Te. V also crucial, as exemplified by MAGIC obs. of Ice. Cube-170922 A and GRB 190114 C Aasten +18 9 years 1. 5 months 21/22

Summary • Polarization is powerful probe to magnatic field and source geometry • Three new polarimetric obs. available / will be available – SGMAP(opt. ): Transient monitor in polarimetry – ALMA/Ka. VA (radio): Already started, To. O (<a few days) possible – IXPE (X-ray): several 10 s sources for the first time • Coordinated polarimetric obs. (+ Fermi, CTA) would provide vital information Thank you for your Attention 22/22

Reference • • Aasten et al. 2018, Science, eaat 1378 Abdo et al. 2010, Nature 463, 919 Brundell et al. 2018, Ap. JL 867, 25 Laskar et al. 2018, Ap. JL 878, 26 Nagai et al. 2016, Ap. J 824, 132 Urata et al. 2018, Ap. JL 884, 58 Weisskopf et al. 1978, Ap. JL 220, 117 Weisskopf 2018, Galaxies 6, 33 23/22

Backup Slides 24/22

Polarimetry with ALMA • Imaging-polarimetry from Cycle 3 (2013) • First full pol. obs. (3 C 286) supports aligned B near the jet base • Many more results recently, To. O (< a few days) possible 3 C 286 (Nagai +16) 25/22

IXPE Mission • Bilateral collaboration between NASA and Italian Space Agency (ASI), NASA SMEX mission, launch in April 2021 • Japanese group: RIKEN, Nagoya Univ. , Hiroshima Univ. , Yamagata Univ. , Osaka Univ. , Chuo Univ. , Tokyo Univ. of Science) PI: Martin Weisskopf (NASA Marshall Space Flight Center) 26/22

Mission Description • Will move to backup Parameter Launch Planning (Pegasus XL baselined) Mission Duration Initial Orbit State Ground Stations Communications Value 21 day launch period Can launch on any day on or after 04/20/2021 25 months including 1 month commissioning/payload verification Low Earth orbit (LEO) Altitude = 540 km, circular Inclination = 0 degrees Malindi, Kenya (primary station) Singapore NEN station (backup) TDRSS (early mission operations, contingency) 2. 0 Mbps downlink via S-band LGA (to ground) 1 kbps downlink via S-band LGA (to TDRS) 2 kbps uplink via S-band LGA (from ground) Fault Management Autonomously places observatory in a safe configuration, Ground control used for recovery 27/22

Stokes Param. based Analysis • Will move to backup (Slide by S. Gunji for JPS meeting 2019/Mar) 28/22