PoGOLite – A high sensitivity balloon-borne soft gamma-ray polarimeter
We describe a new balloon-borne instrument (PoGOLite) capable of detecting 10% polarisation from 200 mCrab point-like sources between 25 and 80 keV in one 6-h flight. Polarisation measurements in the soft gamma-ray band are expected to provide a powerful probe into high energy emission mechanisms as...
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| Published in | Astroparticle physics Vol. 30; no. 2; pp. 72 - 84 |
|---|---|
| Main Authors | , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , |
| Format | Journal Article |
| Language | English |
| Published |
Elsevier B.V
01.09.2008
|
| Subjects | |
| Online Access | Get full text |
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| Abstract | We describe a new balloon-borne instrument (PoGOLite) capable of detecting 10% polarisation from 200
mCrab point-like sources between 25 and 80
keV in one 6-h flight. Polarisation measurements in the soft gamma-ray band are expected to provide a powerful probe into high energy emission mechanisms as well as the distribution of magnetic fields, radiation fields and interstellar matter. Synchrotron radiation, inverse Compton scattering and propagation through high magnetic fields are likely to produce high degrees of polarisation in the energy band of the instrument. We demonstrate, through tests at accelerators, with radioactive sources and through computer simulations, that PoGOLite will be able to detect degrees of polarisation as predicted by models for several classes of high energy sources. At present, only exploratory polarisation measurements have been carried out in the soft gamma-ray band. Reduction of the large background produced by cosmic-ray particles while securing a large effective area has been the greatest challenge. PoGOLite uses Compton scattering and photo-absorption in an array of 217 well-type phoswich detector cells made of plastic and BGO scintillators surrounded by a BGO anticoincidence shield and a thick polyethylene neutron shield. The narrow field of view (FWHM
=
1.25
msr, 2.0
deg
×
2.0
deg) obtained with detector cells and the use of thick background shields warrant a large effective area for polarisation measurements (∼228
cm
2 at
E
=
40
keV) without sacrificing the signal-to-noise ratio. Simulation studies for an atmospheric overburden of 3–4
g/cm
2 indicate that neutrons and gamma-rays entering the PDC assembly through the shields are dominant backgrounds. Off-line event selection based on recorded phototube waveforms and Compton kinematics reduce the background to that expected for a ∼100
mCrab source between 25 and 50
keV. A 6-h observation of the Crab pulsar will differentiate between the Polar Cap/Slot Gap, Outer Gap, and Caustic models with greater than 5
σ significance; and also cleanly identify the Compton reflection component in the Cygnus X-1 hard state. Long-duration flights will measure the dependence of the polarisation across the cyclotron absorption line in Hercules X-1. A scaled-down instrument will be flown as a pathfinder mission from the north of Sweden in 2010. The first science flight is planned to take place shortly thereafter. |
|---|---|
| AbstractList | We describe a new balloon-borne instrument (PoGOLite) capable of detecting 10% polarisation from 200 mCrab point-like sources between 25 and 80 keV in one 6-h flight. Polarisation measurements in the soft gamma-ray band are expected to provide a powerful probe into high energy emission mechanisms as well as the distribution of magnetic fields, radiation fields and interstellar matter. Synchrotron radiation, inverse Compton scattering and propagation through high magnetic fields are likely to produce high degrees of polarisation in the energy band of the instrument. We demonstrate, through tests at accelerators, with radioactive sources and through computer simulations, that PoGOLite will be able to detect degrees of polarisation as predicted by models for several classes of high energy sources. At present, only exploratory polarisation measurements have been carried out in the soft gamma-ray band. Reduction of the large background produced by cosmic-ray particles while securing a large effective area has been the greatest challenge. PoGOLite uses Compton scattering and photo-absorption in an array of 217 well-type phoswich detector cells made of plastic and BGO scintillators surrounded by a BGO anticoincidence shield and a thick polyethylene neutron shield. The narrow Held of view (FWHM = 1.25 msr, 2.0 deg x 2.0 deg) obtained with detector cells and the use of thick background shields warrant a large effective area for polarisation measurements (similar to 228 cm(2) at E = 40 keV) without sacrificing the signal-to-noise ratio. Simulation studies for an atmospheric overburden of 3-4 g/cm(2) indicate that neutrons and gamma-rays entering the PDC assembly through the shields are dominant backgrounds. Off-line event selection based on recorded phototube waveforms and Compton kinematics reduce the background to that expected for a similar to 100 mCrab source between 25 and 50 keV. A 6-h observation of the Crab pulsar will differentiate between the Polar Cap/Slot Gap, Outer Gap, and Caustic models with greater than 5 sigma significance; and also cleanly identify the Compton reflection component in the Cygnus X-1 hard state. Long-duration flights will measure the dependence of the polarisation across the cyclotron absorption line in Hercules X-1. A scaled-down instrument will be flown as a pathfinder mission from the north of Sweden in 2010. The first science flight is planned to take place shortly thereafter. We describe a new balloon-borne instrument (PoGOLite) capable of detecting 10% polarisation from 200 mCrab point-like sources between 25 and 80 keV in one 6-h flight. Polarisation measurements in the soft gamma-ray band are expected to provide a powerful probe into high energy emission mechanisms as well as the distribution of magnetic fields, radiation fields and interstellar matter. Synchrotron radiation, inverse Compton scattering and propagation through high magnetic fields are likely to produce high degrees of polarisation in the energy band of the instrument. We demonstrate, through tests at accelerators, with radioactive sources and through computer simulations, that PoGOLite will be able to detect degrees of polarisation as predicted by models for several classes of high energy sources. At present, only exploratory polarisation measurements have been carried out in the soft gamma-ray band. Reduction of the large background produced by cosmic-ray particles while securing a large effective area has been the greatest challenge. PoGOLite uses Compton scattering and photo-absorption in an array of 217 well-type phoswich detector cells made of plastic and BGO scintillators surrounded by a BGO anticoincidence shield and a thick polyethylene neutron shield. The narrow Held of view (FWHM = 1.25 msr, 2.0 deg x 2.0 deg) obtained with detector cells and the use of thick background shields warrant a large effective area for polarisation measurements (similar to 228 cm(2) at E = 40 keV) without sacrificing the signal-to-noise ratio. Simulation studies for an atmospheric overburden of 3-4 g/cm(2) indicate that neutrons and gamma-rays entering the PDC assembly through the shields are dominant backgrounds. Off-line event selection based on recorded phototube waveforms and Compton kinematics reduce the background to that expected for a similar to 100 mCrab source between 25 and 50 keV. A 6-h observation of the Crab pulsar will differentiate between the Polar Cap/Slot Gap, Outer Gap, and Caustic models with greater than 5 sigma significance; and also cleanly identify the Compton reflection component in the Cygnus X-1 hard state. Long-duration flights will measure the dependence of the polarisation across the cyclotron absorption line in Hercules X-1. A scaled-down instrument will be flown as a pathfinder mission from the north of Sweden in 2010. The first science flight is planned to take place shortly thereafter. (C) 2008 Elsevier B.V. All rights reserved. We describe a new balloon-borne instrument (PoGOLite) capable of detecting 10% polarisation from 200 mCrab point-like sources between 25 and 80 keV in one 6-h flight. Polarisation measurements in the soft gamma-ray band are expected to provide a powerful probe into high energy emission mechanisms as well as the distribution of magnetic fields, radiation fields and interstellar matter. Synchrotron radiation, inverse Compton scattering and propagation through high magnetic fields are likely to produce high degrees of polarisation in the energy band of the instrument. We demonstrate, through tests at accelerators, with radioactive sources and through computer simulations, that PoGOLite will be able to detect degrees of polarisation as predicted by models for several classes of high energy sources. At present, only exploratory polarisation measurements have been carried out in the soft gamma-ray band. Reduction of the large background produced by cosmic-ray particles while securing a large effective area has been the greatest challenge. PoGOLite uses Compton scattering and photo-absorption in an array of 217 well-type phoswich detector cells made of plastic and BGO scintillators surrounded by a BGO anticoincidence shield and a thick polyethylene neutron shield. The narrow Held of view (FWHM = 1.25 msr, 2.0 deg x 2.0 deg) obtained with detector cells and the use of thick background shields warrant a large effective area for polarisation measurements (similar to 228 cm(2) at E = 40 keV) without sacrificing the signal-to-noise ratio. Simulation studies for an atmospheric overburden of 3-4 g/cm(2) indicate that neutrons and gamma-rays entering the PDC assembly through the shields are dominant backgrounds. Off-line event selection based on recorded phototube waveforms and Compton kinematics reduce the background to that expected for a similar to 100 mCrab source between 25 and 50 keV. A 6-h observation of the Crab pulsar will differentiate between the Polar Cap/Slot Gap, Outer Gap, and Caustic models with greater than 5 sigma significance; and also cleanly identify the Compton reflection component in the Cygnus X-1 hard state. Long-duration flights will measure the dependence of the polarisation across the cyclotron absorption line in Hercules X-1. A scaled-down instrument will be flown as a pathfinder mission from the north of Sweden in 2010. The first science flight is planned to take place shortly thereafter. We describe a new balloon-borne instrument (PoGOLite) capable of detecting 10% polarisation from 200 mCrab point-like sources between 25 and 80 keV in one 6-h flight. Polarisation measurements in the soft gamma-ray band are expected to provide a powerful probe into high energy emission mechanisms as well as the distribution of magnetic fields, radiation fields and interstellar matter. Synchrotron radiation, inverse Compton scattering and propagation through high magnetic fields are likely to produce high degrees of polarisation in the energy band of the instrument. We demonstrate, through tests at accelerators, with radioactive sources and through computer simulations, that PoGOLite will be able to detect degrees of polarisation as predicted by models for several classes of high energy sources. At present, only exploratory polarisation measurements have been carried out in the soft gamma-ray band. Reduction of the large background produced by cosmic-ray particles while securing a large effective area has been the greatest challenge. PoGOLite uses Compton scattering and photo-absorption in an array of 217 well-type phoswich detector cells made of plastic and BGO scintillators surrounded by a BGO anticoincidence shield and a thick polyethylene neutron shield. The narrow field of view (FWHM = 1.25 msr, 2.0 deg × 2.0 deg) obtained with detector cells and the use of thick background shields warrant a large effective area for polarisation measurements (∼228 cm 2 at E = 40 keV) without sacrificing the signal-to-noise ratio. Simulation studies for an atmospheric overburden of 3–4 g/cm 2 indicate that neutrons and gamma-rays entering the PDC assembly through the shields are dominant backgrounds. Off-line event selection based on recorded phototube waveforms and Compton kinematics reduce the background to that expected for a ∼100 mCrab source between 25 and 50 keV. A 6-h observation of the Crab pulsar will differentiate between the Polar Cap/Slot Gap, Outer Gap, and Caustic models with greater than 5 σ significance; and also cleanly identify the Compton reflection component in the Cygnus X-1 hard state. Long-duration flights will measure the dependence of the polarisation across the cyclotron absorption line in Hercules X-1. A scaled-down instrument will be flown as a pathfinder mission from the north of Sweden in 2010. The first science flight is planned to take place shortly thereafter. |
| Author | Larsson, Stefan Ryde, Felix Ekeberg, Tomas Engdegård, Olle Fukazawa, Yasushi Kazejev, Jaroslav Takahashi, Hiromitsu Yamashita, Yuichiro Carlson, Per Kanai, Yoshikazu Hjalmarsdotter, Linnea Craig, William Thurston, Timothy Kawai, Nobuyuki Yoshida, Hiroaki Kamae, Tuneyoshi Mizuno, Tsunefumi Varner, Gary Iwan, Bianca Takahashi, Tadayuki Ylinen, Tomi Kiss, Mózsi Madejski, Grzegorz Andersson, Viktor Kataoka, Jun Tanaka, Takuya Yamamoto, Kazuhide Björnsson, Claes-Ingvar Axelsson, Magnus Ng, Johnny Ueno, Masaru Bogaert, Gilles Tajima, Hiroyasu Pearce, Mark Suhonen, Markus Marini Bettolo, Cecilia Gunji, Shuichi Klamra, Wlodzimierz Arimoto, Makoto |
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SE-106 91 Stockholm, Sweden – sequence: 6 givenname: Claes-Ingvar surname: Björnsson fullname: Björnsson, Claes-Ingvar organization: Stockholm University, Astronomy Department, SE–106 91 Stockholm, Sweden – sequence: 7 givenname: Gilles surname: Bogaert fullname: Bogaert, Gilles organization: Ecole Polytechnique, Laboratoire Leprince-Rinquet, 91128 Palaiseau Cedex, France – sequence: 8 givenname: Per surname: Carlson fullname: Carlson, Per organization: Royal Institute of Technology, Physics Department, SE-106 91 Stockholm, Sweden – sequence: 9 givenname: William surname: Craig fullname: Craig, William organization: Stanford Linear Accelerator Center (SLAC) and Kavli Institute for Particle Astrophysics and Cosmology (KIPAC), Menlo Park, CA 94025, USA – sequence: 10 givenname: Tomas surname: Ekeberg fullname: Ekeberg, Tomas organization: Stanford Linear Accelerator Center (SLAC) and Kavli Institute for Particle Astrophysics and Cosmology (KIPAC), Menlo Park, CA 94025, USA – sequence: 11 givenname: Olle surname: Engdegård fullname: Engdegård, Olle organization: Royal Institute of Technology, Physics Department, SE-106 91 Stockholm, Sweden – sequence: 12 givenname: Yasushi surname: Fukazawa fullname: Fukazawa, Yasushi organization: Hiroshima University, Physics Department, Higashi-Hiroshima 739-8526, Japan – sequence: 13 givenname: Shuichi surname: Gunji fullname: Gunji, Shuichi organization: Yamagata University, Physics Department, Yamagata 990-8560, Japan – sequence: 14 givenname: Linnea surname: Hjalmarsdotter fullname: Hjalmarsdotter, Linnea organization: Stockholm University, Astronomy Department, SE–106 91 Stockholm, Sweden – sequence: 15 givenname: Bianca surname: Iwan fullname: Iwan, Bianca organization: Stanford Linear Accelerator Center (SLAC) and Kavli Institute for Particle Astrophysics and Cosmology (KIPAC), Menlo Park, CA 94025, USA – sequence: 16 givenname: Yoshikazu surname: Kanai fullname: Kanai, Yoshikazu organization: Tokyo Institute of Technology, 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surname: Larsson fullname: Larsson, Stefan organization: Royal Institute of Technology, Physics Department, SE-106 91 Stockholm, Sweden – sequence: 23 givenname: Grzegorz surname: Madejski fullname: Madejski, Grzegorz organization: Stanford Linear Accelerator Center (SLAC) and Kavli Institute for Particle Astrophysics and Cosmology (KIPAC), Menlo Park, CA 94025, USA – sequence: 24 givenname: Tsunefumi surname: Mizuno fullname: Mizuno, Tsunefumi organization: Hiroshima University, Physics Department, Higashi-Hiroshima 739-8526, Japan – sequence: 25 givenname: Johnny surname: Ng fullname: Ng, Johnny organization: Stanford Linear Accelerator Center (SLAC) and Kavli Institute for Particle Astrophysics and Cosmology (KIPAC), Menlo Park, CA 94025, USA – sequence: 26 givenname: Mark surname: Pearce fullname: Pearce, Mark organization: Royal Institute of Technology, Physics Department, SE-106 91 Stockholm, Sweden – sequence: 27 givenname: Felix surname: Ryde fullname: Ryde, Felix organization: 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Physics Department, Higashi-Hiroshima 739-8526, Japan – sequence: 33 givenname: Timothy surname: Thurston fullname: Thurston, Timothy organization: The Thurston Co., 11336 30th Avenue, NE, Seattle, WA 98125, USA – sequence: 34 givenname: Masaru surname: Ueno fullname: Ueno, Masaru organization: Tokyo Institute of Technology, Physics Department, Meguro-ku, Tokyo 152-8550, Japan – sequence: 35 givenname: Gary surname: Varner fullname: Varner, Gary organization: University of Hawaii, Department of Physics and Astronomy, Honolulu, Hawaii 96822, USA – sequence: 36 givenname: Kazuhide surname: Yamamoto fullname: Yamamoto, Kazuhide organization: Hiroshima University, Physics Department, Higashi-Hiroshima 739-8526, Japan – sequence: 37 givenname: Yuichiro surname: Yamashita fullname: Yamashita, Yuichiro organization: Yamagata University, Physics Department, Yamagata 990-8560, Japan – sequence: 38 givenname: Tomi surname: Ylinen fullname: Ylinen, Tomi organization: Stanford Linear Accelerator 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| Snippet | We describe a new balloon-borne instrument (PoGOLite) capable of detecting 10% polarisation from 200
mCrab point-like sources between 25 and 80
keV in one 6-h... We describe a new balloon-borne instrument (PoGOLite) capable of detecting 10% polarisation from 200 mCrab point-like sources between 25 and 80 keV in one 6-h... |
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| SubjectTerms | active binaries binaries Stars detectors detectors Techniques Galaxies general X-ray Instrumentation NATURAL SCIENCES NATURVETENSKAP neutron neutron Galaxies polarimetric polarimetric Pulsars Pulsars Stars Techniques X-ray |
| Title | PoGOLite – A high sensitivity balloon-borne soft gamma-ray polarimeter |
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