X-ray Polarimetry - INAF-IASF-Roma

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Implementation of X-ray polarimetry with GPD in proposed missions: - POLARIX (ASI small mission, fasa A completed) 3 Jet-X optics (3,5 m FL, 20 ‘’ HED 500 cm 2 @ 2 keV, HEW=(20’’)) 3 GPD (1-cm, 1-Atm, He-DME 20-80) MDP 12 % in 10 5 s for 1 mCrab source (2-10 keV) 3.8 % in 10 5 s for 10 mCrab source (2-10 keV) - NHXM (Proposed ESA M3 Mission not selected) 1 of 4 Multi-layer optics (Pt-C) (10 m FL) 2 GPD : 1-cm, 1-Atm, He-DME (LEP) (2-10 keV); 3-cm 3-Atm Ar-DME (MEP) (6-35 keV) MDP: LEP 9.7 % in 10 5 s for 1 mCrab source (2-10 keV) 3.1 % in 10 5 s for 10 mCrab source (2-10 keV) Costa, et al., Exp Ast 2010 MEP 13 % in 10 5 s for 1 mCrab source (6-35 keV) 4.1 % in 10 5 for 10 mCrab source (6-35 keV) In study (HEP, Compton scattering) MDP 7.2 % for 10 mCrab in 10 5 s (20-80 keV) Tagliaferri et al.i, Exp Ast 2010; - IXO Soffitta et al. SPIE 2010 (ESA/NASA/JAXA Large Mission Evolved in Athena with no polarimeter on-board) Area= 2.5 m 2 FL = 20 m HEW= 5’’ XPOL: MDP 1 % 1 mCrab 10 5 s. Paolo Soffitta The Extreme and Variable High Energy Sky Chia Laguna 19-21/09/2011
A detector more tuned on hard X-rays for NHXM The simulations suggested a mixture of Ar (80%) DME (20%) with 3 cm absorption gap and 3 atm pressure. We name it Medium Energy Polarimeter First Prototype working (2 cm 2 Atm) The MEP prototype in the IASF-Rome facility. MEP detector is working apparently well. It is a good Proportional Counter. Unfortunately it broke soon after this testing. Anyway we ar foresaw further changes. A larger detector for better control of the electric field and to exclude background produced on the walls is in construction. Paolo Soffitta The Extreme and Variable High Energy Sky Chia Laguna 19-21/09/2011
Page 1 and 2: X-Ray Polarimetry Paolo Soffitta IA
Page 3 and 4: Bragg diffraction Bragg diffraction
Page 5 and 6: OSO-8 satellite with a dedicated Br
Page 7 and 8: Thomson Polarimeters They were the
Page 9 and 10: Modern polarimeters dedicated to X-
Page 11 and 12: X-ray polarimetry with a Gas Pixel
Page 13 and 14: The real implementation of a workin
Page 15 and 16: Each photon produces a track. From
Page 17 and 18: X-ray polarimetry with a micropatte
Page 19 and 20: GRAVITY and EXTREME MAGNETISMS SMAL
Page 21 and 22: The sensitivity to polarization of
Page 23: POLARIX The missions where the GPD
Page 27 and 28: Spectro-imaging polarimetry of PWNe
Page 29 and 30: Was the GC an AGN a few hundreds ye
Page 31 and 32: IXO: Polarimetry of extended Jets i
Page 33 and 34: For a non focal plane experiment to

X-ray Polarimetry - INAF-IASF-Roma

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