Measuring polarization at gamma-rays with Fermi

Slides:

Advertisements

Similar presentations

NDVCS measurement with BoNuS RTPC M. Osipenko December 2, 2009, CLAS12 Central Detector Collaboration meeting.

Advertisements

RHESSI Studies of Solar Flare Hard X-Ray Polarization Mark L. McConnell 1, David M. Smith 2, A. Gordon Emslie 4, Martin Fivian 3, Gordon J. Hurford 3,

Advanced GAmma Tracking Array

Geant4 Low Energy Polarized Compton Processes Gerardo Depaola * Francesco Longo + Francesco Longo + * National University of Córdoba (Argentina) + University.

14.5m 100 m ~480 m Junction Box ~70 m String-based detector; Downward-looking (45°) PMTs; 2475 m deep; 12 detection lines 25 storeys / line 3 PMTs / storey.

X-ray polarisation: Science

Space Applications of Geant4 Polarized Processes F.Longo + G.Depaola * + University of Ferrara and INFN (Italia) * National University of Córdoba (Argentina)

X-ray Polarimeter Biswajit Paul Raman Research Institute, Bangalore

RHESSI Studies of Solar Flare Hard X-Ray Polarization Mark L. McConnell 1, David M. Smith 2, A. Gordon Emslie 4, Martin Fivian 3, Gordon J. Hurford 3,

A Search for Point Sources of High Energy Neutrinos with AMANDA-B10 Scott Young, for the AMANDA collaboration UC-Irvine PhD Thesis:

Bill Atwood, Core Meeting, 9-Oct GLAS T 1 Finding and Fitting A Recast of Traditional GLAST Finding: Combo A Recast of the Kalman Filter Setting.

A THREE-DIMENSIONAL OUTER MAGETOSPHERIC MODEL FOR GAMMA-RAY PULSARS : GEOMETRY, PAIR PRODUCTION, EMISSION MORPHOLOGIES, AND PHASE- RESOLVED SPECTRA K.S.CHENG,

1 Gamma-Ray Astronomy with GLAST May 24, 2008 Toby Burnett WALTA meeting.

Roberto Francisco Pérez Benito On behalf the HERMES Collaboration European Graduate School Lecture Week on Hadron Physics Jyväskylä, Aug 25-29, 2008 HERMES.

Marcus ZieglerAPS April Meeting Gamma-Ray Pulsars in the GLAST Era Gamma-ray Large Area Space Telescope Marcus Ziegler Santa Cruz Institute for.

Event Analysis for the Gamma-ray Large Area Space Telescope Robin Morris, RIACS Johann Cohen-Tanugi INFN, Pisa.

C&A 17April06 1 Point Source Detection and Localization using DC2 pulsars Toby Burnett University of Washington.

The ANTARES Neutrino Telescope Mieke Bouwhuis 27/03/2006.

RF background, analysis of MTA data & implications for MICE Rikard Sandström, Geneva University MICE Collaboration Meeting – Analysis session, October.

Beijing, Feb 3 rd, 2007 LEPOL 1 Low Energy Positron Polarimetry for the ILC Sabine Riemann (DESY) On behalf of the LEPOL Collaboration.

Potential Neutrino Signals from Galactic  -Ray Sources Alexander Kappes, Christian Stegmann University Erlangen-Nuremberg Felix Aharonian, Jim Hinton.

Geant4 Low Energy Polarized Processes Gerardo Depaola * Francesco Longo + Francesco Longo + * National University of Córdoba (Argentina) + University of.

Gamma-Ray Burst Polarimeter – GAP – aboard the Solar Powered Sail Mission Gamma-Ray Burst Polarimeter – GAP – aboard the Solar Powered Sail Mission Daisuke.

A study of systematic uncertainties of Compton e-detector at JLab, Hall C and its cross calibration against Moller polarimeter APS April Meeting 2014 Amrendra.

Introduction to gamma-ray astronomy GLAST-Large Area Telescope Introduction to GLAST Science New way of studying astrophysics Schedule of GLAST project.

Impact parameter resolution study for ILC detector Tomoaki Fujikawa (Tohoku university) ACFA Workshop in Taipei Nov

Interaction of Cosmic-Rays with the Solar System Bodies as seen by Fermi LAT Monica Brigida Bari University For the Fermi LAT Collaboration.

Hard X-ray Polarimeter for Small Satellite Design, Feasibility Study, and Ground Experiments K. Hayashida (Osaka University), T. Mihara (RIKEN), S. Gunji,

M. Dugger, February Triplet polarimeter study Michael Dugger* Arizona State University *Work at ASU is supported by the U.S. National Science Foundation.

Event Analysis for the Gamma-ray Large Area Space Telescope Robin Morris, RIACS Johann Cohen-Tanugi SLAC.

44 th Rencontres de Moriond 1 Blind Period Search gamma-ray pulsar by Fermi-LAT F. Giordano Dipartimento Interateneo di Fisica and INFN Sez. Bari for the.

Potential Neutrino Signals from Galactic  -Ray Sources Alexander Kappes, Christian Stegmann University Erlangen-Nuremberg Felix Aharonian, Jim Hinton.

PoGO_collimator_ ppt1 Study of PoGO background dependence on the collimator material/slow scintillator threshold April 21, 2004 Tsunefumi Mizuno.

The Luminosity Calorimeter Iftach Sadeh Tel Aviv University Desy ( On behalf of the FCAL collaboration ) June 11 th 2008.

Forward Tagger Simulations Implementation in GEMC Moller Shield Tracking Studies R. De Vita INFN –Genova Forward Tagger Meeting, CLAS12 Workshop, June.

PoGO_G4_ ppt1 Study of optimized fast scintillator length for the astronomical hard X- ray/soft gamma-ray polarimeter PoGO November 1, 2004 Tsunefumi.

High Energy Astrophysics with the Fermi Large Area Telescope Elizabeth Hays (NASA/GSFC) On behalf of the Fermi LAT Collaboration.

O Tsunefumi Mizuno, Tuneyoshi Kamae, Jonny Ng, Hiroyasu Tajima (SLAC), John W. Mitchell, Robert Streitmatter (NASA GSFC), Richard C. Fernholz, Edward Groth.

Dollan, Laihem, Lohse, Schälicke, Stahl 1 Monte Carlo based studies of polarized positrons source for the International Linear Collider (ILC)

04/10/2015PHY 712 Spring Lecture 301 PHY 712 Electrodynamics 9-9:50 AM MWF Olin 103 Plan for Lecture 30: Finish reading Chap. 14 – Radiation from.

Manoj B. Jadhav Supervisor Prof. Raghava Varma I.I.T. Bombay PANDA Collaboration Meeting, PARIS – September 11, 2012.

MOHAMAD KHALIL APC LABORATORY PARIS 17/06/2013 DSSD and SSD Simulation with Silvaco.

Achim Stahl RWTH Aachen Hadron Therapy, Jülich Oct, Workshop Nuclear Models for Use in Hadron Therapy October 8./ Achim Stahl – RWTH Aachen.

Characterisation and Comparison of Event Generators for Pair Conversion: A Crucial Step for Future Low Energy Gamma Telescopes Philippe Gros LLR, Ecole.

Roberto Francisco Perez Benito

Discovery of a GeV blazar shining through the galactic plane

Recent Results of Point Source Searches with the IceCube Neutrino Telescope Lake Louise Winter Institute 2009 Erik Strahler University of Wisconsin-Madison.

June 1, 2004 Tsunefumi Mizuno Expected Modulation Factor of PoGO calculated with Geant4 Simulator with PoGO-fix June 1, 2004 Tsunefumi.

Comparison of GAMMA-400 and Fermi-LAT telescopes

Observation of Pulsars and Plerions with MAGIC

Analysis of Fermi Source 3FGL

GLAST LAT tracker signal simulation and trigger timing study

GAMMA-400 performance a,bLeonov A., a,bGalper A., bKheymits M., aSuchkov S., aTopchiev N., bYurkin Y. & bZverev V. aLebedev Physical Institute of the Russian.

HARPO: Gamma ray telescope and polarimeter in MeV-GeV range Philippe GROS LLR, École Polytechnique for the HARPO collaboration 04/12/2015 Atelier accéleration.

HARPO, a Micromegas+GEM TPC for gamma polarimetry above 1 MeV

A statistical model to explain the gamma-ray flare and variability of Crab nebula Qiang Yuan Institute of High Energy Physics, Chinese Academy of Sciences.

Fermi Collaboration Meeting

On behalf of the GECAM group

Outline Analysis of some real data taken with the GLAST minitower (cosmic rays only). Offline analysis software used. Full Monte Carlo simulation using.

Gamma Ray Satellites Simulations with Geant4

Special Considerations for SIDIS

Cosmic-Ray Source Generator

G0 Beam Polarization T. Horn, D. Gaskell Jefferson Lab

Target and detectors 9Li 11Li n n Coulomb breakup Target nucleus

Imaging crystals with TKR

Exploring the Gamma-Ray/Optical Connection in Blazars

Radiation from charged particles

CLAS Collaboration Meeting

Fermi LAT Observations of Galactic X-ray binaries

Presentation transcript:

Measuring polarization at gamma-rays with Fermi Rolf Buehler, Bill Atwood, Michael Kuss, Francesco Longo, Leon Rochester, Mattia Sormani, Tracy Usher for the Fermi LAT collaboration SCINEGHE 2010 Trieste

Why? One of the science goals of LAT since the beginning, as Polarization contains information about magnetic field and gamma- ray production. Brightest Fermi sources have potentially polarized emission: Pulsar : curvature radiation, phase and location dependent (Vela) Pulsar Wind Nebula : synchrotron radiation (Crab) Active Galactic Nuclei : proton synchrotron radiation or Inverse Compton radiations (3C 454, 3C 279) → Models not very specific yet (to my knowledge), this is the time!

How? Pair is preferably (~20%) produced in polarization plane → Detect azimuthal modulation e+ e- γ Z=74 Typical pair opening angle: (≈1 deg at 100 MeV)

Pair production cross section G. Depaola 1999, 2000

Azimuthal modulation Cross-section complex. Past Studies typically made Φ = π Approximation (no recoil) Simple diagnostic variable, asymmetry ratio: Ne+e- (parallel in Δψ) R ≡ Ne+e- (orthogonal in Δψ)

Can it be resolved? Multiple scattering Tracker resolution SUPPORT TRAY SILICON STRIP DETECTORS TUNGSTEN RADIATOR Tungsten Conversion Silicon Conversions TOP Conversions BOTTOM Conversions Xtungsten = 0.028 Xsilicon = 0.004 ≈ 30 mm Tracker resolution Minimum angle which can be resolved between two trackers (pitch=0.228 mm ): θMin ≈ 0.4 deg

Can it be resolved? Requirement: e+ e- direction better measured than opening angle No for typical tungsten conversion Yes between ≈50-200 MeV for silicon conversions (Idea from Bill Atwood)

→ 20% polarization detectable after 20 month at 3 sigma Sensitivity estimate Efficiency in detecting silicon conversion ≈0.3 with standard reco Purity in detecting silicon conversion ≈0.7 with standard reco Events with resolvable opening angle ≈0.7 Degree of polarization Cross section modulation ≈0.2 From Vela we get ≈200000 events/year between 50-200 MeV → 20% polarization detectable after 20 month at 3 sigma ( analysis far from optimal, but no background and trial factors considered )

Current status & Outlook Polarization measurement possible with the LAT down to ~10% polarization level for bright sources. Status: Francesco Longo modified Geant 4 in Fermi simulations, validation Improved detection of silicon conversion Unpolarized simulations show azimuthal asymmetries in the detector on 5% level. Major challenge. No look into data yet (keep analysis blind) → Measurement possible, expect results in near future.