XIPE e IXPE. Paolo Soffitta IAPS/INAF Roma.
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1 XIPE e IXPE Paolo Soffitta IAPS/INAF Roma
2 Polarimetria X ad immagine XIPE e IXPE Polarization from celestial sources may derive from: Emission processes themselves: cyclotron, synchrotron, non-thermal bremsstrahlung (Westfold, 1959; Gnedin & Sunyaev, 1974; Rees, 1975) Scattering on aspherical accreting plasmas: disks, blobs, columns. 2002). (1975; Sunyaev & Titarchuk, 1985; MÅszÇros, P. et al. 1988) Vacuum polarization and birefringence through extreme magnetic fields (Gnedin et al., 1978; Ventura, 1979; MÅszÇros & Ventura, 1979) 2
3 XIPE e IXPE Contesto internazionale 3 missions of X-ray polarimetry now in competition between ESA and NASA Lead Scientist: Paolo Soffitta (IAPS/INAF) ESA M4. Competitors: THOR: a mission to study turbolence on Solar Wind (A. Vaivads IRF/Sweden) Ariel: a mission for the spectroscopy of Exoplanets G. Tinetti UCL/UK. Decision in May/June GPDs al fuoco di 3 ottiche per raggi X PI Martin MSFC/NASA NASA SMEX. Competitors PRAXYS: a Mission of X-ray Polarimetry based on TPC. PI K. NASA/GSFC SPHEREx: a Mission of All Sky Survey of NearIR spectroscopy. PI James CalTech 3
4 Why this is now possible The Gas Pixel Detector Polarimetria Immagine Spettroscopia 4
5 The XIPE energy band Scientific goal Sources < 1keV 1-10 > 10 kev Acceleration phenomena PWN yes (but absorption) yes yes Emission in strong magnetic fields Scattering in aspherical geometries SNR no yes yes Jet (Microquasars) yes (but absorption) yes yes Jet (Blazars) yes yes yes WD yes (but absorption) yes difficult AMS no yes yes X-ray pulsator difficult yes (no cyclotron?) yes Magnetar yes (better) yes no Corona in XRB & AGNs difficult yes yes (difficult) X-ray reflection nebulae no yes (long exposure) yes Fundamental Physics QED (magnetar) yes (better) yes no GR (BH) no yes no QG (Blazars) difficult yes yes Axions (Blazars,Clusters) yes? yes difficult 5
6 XIPE scientific goals Astrophysics: Acceleration: PWN & SNR What is the role of the magnetic field (turbulent or not?) 20 ks with XIPE
7 Many sources in each class available for XIPE quoted in the proposal: 500 days of net exposure time in 3 years; average observing time of 3 days; re-visiting for some of those. What number for each class? Target Class T tot (days) T obs /source (Ms) MDP (%) Number in 3 years Number available AGN < XRBs (low+high mass) < SNRe < 15 % (10 regions) 8 8 PWN <10 % (more than 5 regions) 6 6 Magnetars < 10 % (in more than 5 bins) Molecular clouds < 10 % 2 complexes or 5 clouds 2 complexes or 5 clouds Total From catalogues: Liu et al. 2006, 2007 for X-ray binaries; and XMM slew survey 1.6 for AGNs. 7
8 Working groups set: about 300 scientists signed for participation. WG1. Acceleration mechanisms: Giampiero Taglaferri(1), Jacco Vink(2) (1) Osservatorio Astronomico di Brera INAF, Italy, (2) Astronomical Institute Anton Pannekoek, The Netherlands WG1.1 Pulsar Wind Nebulae: Emma de Ona Wilhelmi, ICE, Spain WG1.2 Supernova Remnants: Andrei Bykov, Ioffe Physical-Technical Institute, Russia WG1.3 Blazars: Ivan Agudo, Instituto de AstrofÅsica de AndalucÅa, Spain WG1.4 Micro-QSOs: Elena Gallo, University of California, Santa Barbara, USA WG1.5 Gamma Ray Bursts: Carol Mundell, University of Bath, UK WG1.6 Tidal Disruption Events: Immacolata Donnarumma, IAPS/INAF, Italy WG1.7 Active Stars: Nicholas Grosso, Astronomical Observatory in Strasbourg, France WG1.8 Clusters of Galaxy: Sergey Sazonov, Space Research Institute, Russian Academy of Sciences, Russia WG2. Magnetic Fields in compact objects: Andrea Santangelo (1), Silvia Zane (2) (1) Institut fçr Astronomie und Astrophysik Tuebingen, (2) University College London/MSSL, UK WG2.1 Magnetic Cataclismic Variables: Domitilla De Martino, Osservatorio di Capodimonte, taly WG2.2 Accreting Millisecond Pulsars: Juri Poutanen, Finland Tuorla Observatory, U. of Turku,Finland WG2.3 Accreting X-ray Pulsars: Victor Doroshenko, IAAT, Germany WG2.4 Magnetars: Roberto Turolla, University of Padua, Italy WG3. Scattering in aspherical geometries and accretion Physics: Eugene. Churazov (1), Rene Goosmann(2) (1)Max-Planck-Institut fçr Astrophysik, Germany (2) Astronomical Observatory in Strasbourg, France WG3.1 X-ray binaries and QPOs: Julien Malzac, CESR/CNRS, France WG3.2 AGNs: Pierre Olivier Petrucci, Institut de PlanÑtologie et d Astrophysique de Grenoble, France WG3.3 Molecular Clouds & SgrA*: FrÄdÄric Marin, Astronomical Institute of the Academy of Sciences, Czech Republic WG3.4 Ultra Luminous X-ray sources: Hua Feng, Tsinghua University, Beijing, China WG4. Fundamental Physics: Enrico Costa (1), Giorgio Matt (2) (1) INAF/IAPS, Italy (2) Universita' Roma Tre, Italy WG4.1 QED and X-ray polarimetry: Rosalba Perna, Stony Brook University, USA WG4.2 Strong Gravity: JiřÇ Svoboda, Astronomical Institute of the Academy of Sciences, Czech Republic WG4.3 Quantum Gravity: Philip E. Kaaret, Iowa University, USA WG4.4 Axion-like particles: Marco Roncadelli, University of Pavia, Italy 8
9 XIPE ESA/M4 Contesto Internazionale All Europe and more The distribution of activities 9
10 XIPE ESA/M4 Contesto Nazionale: Istituti e Universita coinvolte e contributo hardware XIPE M4/ESA IAPS/INAF INFN-Pi OAB/INAF Universita Roma Tre (Univ. Di Padova, Oss. Di Capodimonte, Oss. Astrofisico di Acetri) Gas Pixel Detectors (INFN-PI) Back End Electronics (INFN-Pi) Calibrazione completa del Detector (IAPS/INAF) Malindi G/S (ASI) Partecipazione alle calibrazioni End-to-END (OAB/INAF; IAPS/INAF) Partecipazione al design e alla qualifica delle ottiche (Telescope Advisory Group) OAB/INAF P/O presso il PI di missione (IAPS/INAF) Partecipazione e guida dei WG scientifici ( Roma Tre, IAPS/INAFOAB/INAF Uni Padova, OAA/INAF) 10
11 IXPE / SMEX Contesto internazionale IAPS/INAF (HW, Cal) INFN (HW, Cal) Universita ROMA TRE (Science) MSFC/NASA (PI, Optics, SOC) UC-LASP (MOC) McGILL University (Science) Stanford University (Science) 11
12 IXPE NASA/SMEX Contributo Italiano Instrument Gas Pixel Detector (EM 3, FU, 1 FS) Filter Wheel + Cal Sources (EM, 3 FU, 1 FS) Back End Electronics (EM, 3 FU, 1 FS) P/L Computer (EM, 1 PFM) P/L Simulator Test Equipments Attivita : Integrazione e test DU (INFN Pi) Calibrazione Stand Alone (IAPS/INAF) Partecipazione alla Calibrazione End-to-End (IAPS/INAF & INFN) Partecipazione alla definizione degli obiettivi scientifici e all analisi dei dati
13 XIPE & IXPE Timelines ESA/M4: CaC 450 Meuros NASA /SMEX CaC 175 M$ Phase A report due on 19th July 2016 Site Visit on 21st November 2016 NASA decision January 2017 Launch end 2020
14
15 END
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