X-Ray Polarimetry Reveals the Magnetic-field Topology on Sub-parsec Scales in Tycho’s Supernova Remnant

Riccardo Ferrazzoli; Patrick Slane; Dmitry Prokhorov; Ping Zhou; Jacco Vink; Niccolò Bucciantini; Enrico Costa; Niccolò Di Lalla; Alessandro Di Marco; Paolo Soffitta; Martin C. Weisskopf; Kazunori Asakura; Luca Baldini; Jeremy Heyl; Philip E. Kaaret; Frédéric Marin; Tsunefumi Mizuno; C. Y. Ng; Melissa Pesce-Rollins; Stefano Silvestri; Carmelo Sgrò; Douglas A. Swartz; Toru Tamagawa; Yi Jung Yang; Iván Agudo; Lucio A. Antonelli; Matteo Bachetti; Wayne H. Baumgartner; Ronaldo Bellazzini; Stefano Bianchi; Stephen D. Bongiorno; Raffaella Bonino; Alessandro Brez; Fiamma Capitanio; Simone Castellano; Elisabetta Cavazzuti; Chien Ting Chen; Stefano Ciprini; Alessandra De Rosa; Ettore Del Monte; Laura Di Gesu; Immacolata Donnarumma; Victor Doroshenko; Michal Dovčiak; Steven R. Ehlert; Teruaki Enoto; Yuri Evangelista; Sergio Fabiani; Javier A. Garcia; Shuichi Gunji; Kiyoshi Hayashida; Wataru Iwakiri; Svetlana G. Jorstad; Fabian Kislat; Vladimir Karas; Takao Kitaguchi; Jeffery J. Kolodziejczak; Henric Krawczynski; Fabio La Monaca; Luca Latronico; Ioannis Liodakis; Simone Maldera; Alberto Manfreda; Andrea Marinucci; Alan P. Marscher; Herman L. Marshall; Giorgio Matt; Ikuyuki Mitsuishi; Fabio Muleri; Michela Negro; Stephen L. O’Dell; Nicola Omodei; Chiara Oppedisano; Alessandro Papitto; George G. Pavlov; Abel L. Peirson; Matteo Perri; Pierre Olivier Petrucci; Maura Pilia; Andrea Possenti; Juri Poutanen; Simonetta Puccetti; Brian D. Ramsey; John Rankin; Ajay Ratheesh; Oliver Roberts; Roger W. Romani; Gloria Spandre; Fabrizio Tavecchio; Roberto Taverna; Yuzuru Tawara; Allyn F. Tennant; Nicholas E. Thomas; Francesco Tombesi; Alessio Trois; Sergey S. Tsygankov; Roberto Turolla; Kinwah Wu; Fei Xie; Silvia Zane

doi:10.3847/1538-4357/acb496

X-Ray Polarimetry Reveals the Magnetic-field Topology on Sub-parsec Scales in Tycho’s Supernova Remnant

Riccardo Ferrazzoli, Patrick Slane, Dmitry Prokhorov, Ping Zhou, Jacco Vink, Niccolò Bucciantini, Enrico Costa, Niccolò Di Lalla, Alessandro Di Marco, Paolo Soffitta, Martin C. Weisskopf, Kazunori Asakura, Luca Baldini, Jeremy Heyl, Philip E. Kaaret, Frédéric Marin, Tsunefumi Mizuno, C. Y. Ng, Melissa Pesce-Rollins, Stefano SilvestriCarmelo Sgrò, Douglas A. Swartz, Toru Tamagawa, Yi Jung Yang, Iván Agudo, Lucio A. Antonelli, Matteo Bachetti, Wayne H. Baumgartner, Ronaldo Bellazzini, Stefano Bianchi, Stephen D. Bongiorno, Raffaella Bonino, Alessandro Brez, Fiamma Capitanio, Simone Castellano, Elisabetta Cavazzuti, Chien Ting Chen, Stefano Ciprini, Alessandra De Rosa, Ettore Del Monte, Laura Di Gesu, Immacolata Donnarumma, Victor Doroshenko, Michal Dovčiak, Steven R. Ehlert, Teruaki Enoto, Yuri Evangelista, Sergio Fabiani, Javier A. Garcia, Shuichi Gunji, Kiyoshi Hayashida, Wataru Iwakiri, Svetlana G. Jorstad, Fabian Kislat, Vladimir Karas, Takao Kitaguchi, Jeffery J. Kolodziejczak, Henric Krawczynski, Fabio La Monaca, Luca Latronico, Ioannis Liodakis, Simone Maldera, Alberto Manfreda, Andrea Marinucci, Alan P. Marscher, Herman L. Marshall, Giorgio Matt, Ikuyuki Mitsuishi, Fabio Muleri, Michela Negro, Stephen L. O’Dell, Nicola Omodei, Chiara Oppedisano, Alessandro Papitto, George G. Pavlov, Abel L. Peirson, Matteo Perri, Pierre Olivier Petrucci, Maura Pilia, Andrea Possenti, Juri Poutanen, Simonetta Puccetti, Brian D. Ramsey, John Rankin, Ajay Ratheesh, Oliver Roberts, Roger W. Romani, Gloria Spandre, Fabrizio Tavecchio, Roberto Taverna, Yuzuru Tawara, Allyn F. Tennant, Nicholas E. Thomas, Francesco Tombesi, Alessio Trois, Sergey S. Tsygankov, Roberto Turolla, Kinwah Wu, Fei Xie, Silvia Zane

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Abstract

Supernova remnants are commonly considered to produce most of the Galactic cosmic rays via diffusive shock acceleration. However, many questions regarding the physical conditions at shock fronts, such as the magnetic-field morphology close to the particle acceleration sites, remain open. Here we report the detection of a localized polarization signal from some synchrotron X-ray emitting regions of Tycho’s supernova remnant made by the Imaging X-ray Polarimetry Explorer. The derived degree of polarization of the X-ray synchrotron emission is 9% ± 2% averaged over the whole remnant, and 12% ± 2% at the rim, higher than the value of polarization of 7%-8% observed in the radio band. In the west region, the degree of polarization is 23% ± 4%. The degree of X-ray polarization in Tycho is higher than for Cassiopeia A, suggesting a more ordered magnetic field or a larger maximum turbulence scale. The measured tangential direction of polarization corresponds to the radial magnetic field, and is consistent with that observed in the radio band. These results are compatible with the expectation of turbulence produced by an anisotropic cascade of a radial magnetic field near the shock, where we derive a magnetic-field amplification factor of 3.4 ± 0.3. The fact that this value is significantly smaller than those expected from acceleration models is indicative of highly anisotropic magnetic-field turbulence, or that the emitting electrons either favor regions of lower turbulence, or accumulate close to where the orientation of the magnetic field is preferentially radially oriented due to hydrodynamical instabilities.

Original language	English (US)
Article number	52
Journal	Astrophysical Journal
Volume	945
Issue number	1
DOIs	https://doi.org/10.3847/1538-4357/acb496
State	Published - Mar 1 2023

All Science Journal Classification (ASJC) codes

Astronomy and Astrophysics
Space and Planetary Science

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10.3847/1538-4357/acb496

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Ferrazzoli, R., Slane, P., Prokhorov, D., Zhou, P., Vink, J., Bucciantini, N., Costa, E., Di Lalla, N., Di Marco, A., Soffitta, P., Weisskopf, M. C., Asakura, K., Baldini, L., Heyl, J., Kaaret, P. E., Marin, F., Mizuno, T., Ng, C. Y., Pesce-Rollins, M., ... Zane, S. (2023). X-Ray Polarimetry Reveals the Magnetic-field Topology on Sub-parsec Scales in Tycho’s Supernova Remnant. Astrophysical Journal, 945(1), Article 52. https://doi.org/10.3847/1538-4357/acb496

@article{22c7c13dbda4472a8052e0d6f745de72,

title = "X-Ray Polarimetry Reveals the Magnetic-field Topology on Sub-parsec Scales in Tycho{\textquoteright}s Supernova Remnant",

abstract = "Supernova remnants are commonly considered to produce most of the Galactic cosmic rays via diffusive shock acceleration. However, many questions regarding the physical conditions at shock fronts, such as the magnetic-field morphology close to the particle acceleration sites, remain open. Here we report the detection of a localized polarization signal from some synchrotron X-ray emitting regions of Tycho{\textquoteright}s supernova remnant made by the Imaging X-ray Polarimetry Explorer. The derived degree of polarization of the X-ray synchrotron emission is 9% ± 2% averaged over the whole remnant, and 12% ± 2% at the rim, higher than the value of polarization of 7%-8% observed in the radio band. In the west region, the degree of polarization is 23% ± 4%. The degree of X-ray polarization in Tycho is higher than for Cassiopeia A, suggesting a more ordered magnetic field or a larger maximum turbulence scale. The measured tangential direction of polarization corresponds to the radial magnetic field, and is consistent with that observed in the radio band. These results are compatible with the expectation of turbulence produced by an anisotropic cascade of a radial magnetic field near the shock, where we derive a magnetic-field amplification factor of 3.4 ± 0.3. The fact that this value is significantly smaller than those expected from acceleration models is indicative of highly anisotropic magnetic-field turbulence, or that the emitting electrons either favor regions of lower turbulence, or accumulate close to where the orientation of the magnetic field is preferentially radially oriented due to hydrodynamical instabilities.",

author = "Riccardo Ferrazzoli and Patrick Slane and Dmitry Prokhorov and Ping Zhou and Jacco Vink and Niccol{\`o} Bucciantini and Enrico Costa and {Di Lalla}, Niccol{\`o} and {Di Marco}, Alessandro and Paolo Soffitta and Weisskopf, {Martin C.} and Kazunori Asakura and Luca Baldini and Jeremy Heyl and Kaaret, {Philip E.} and Fr{\'e}d{\'e}ric Marin and Tsunefumi Mizuno and Ng, {C. Y.} and Melissa Pesce-Rollins and Stefano Silvestri and Carmelo Sgr{\`o} and Swartz, {Douglas A.} and Toru Tamagawa and Yang, {Yi Jung} and Iv{\'a}n Agudo and Antonelli, {Lucio A.} and Matteo Bachetti and Baumgartner, {Wayne H.} and Ronaldo Bellazzini and Stefano Bianchi and Bongiorno, {Stephen D.} and Raffaella Bonino and Alessandro Brez and Fiamma Capitanio and Simone Castellano and Elisabetta Cavazzuti and Chen, {Chien Ting} and Stefano Ciprini and {De Rosa}, Alessandra and {Del Monte}, Ettore and {Di Gesu}, Laura and Immacolata Donnarumma and Victor Doroshenko and Michal Dov{\v c}iak and Ehlert, {Steven R.} and Teruaki Enoto and Yuri Evangelista and Sergio Fabiani and Garcia, {Javier A.} and Shuichi Gunji and Kiyoshi Hayashida and Wataru Iwakiri and Jorstad, {Svetlana G.} and Fabian Kislat and Vladimir Karas and Takao Kitaguchi and Kolodziejczak, {Jeffery J.} and Henric Krawczynski and {La Monaca}, Fabio and Luca Latronico and Ioannis Liodakis and Simone Maldera and Alberto Manfreda and Andrea Marinucci and Marscher, {Alan P.} and Marshall, {Herman L.} and Giorgio Matt and Ikuyuki Mitsuishi and Fabio Muleri and Michela Negro and O{\textquoteright}Dell, {Stephen L.} and Nicola Omodei and Chiara Oppedisano and Alessandro Papitto and Pavlov, {George G.} and Peirson, {Abel L.} and Matteo Perri and Petrucci, {Pierre Olivier} and Maura Pilia and Andrea Possenti and Juri Poutanen and Simonetta Puccetti and Ramsey, {Brian D.} and John Rankin and Ajay Ratheesh and Oliver Roberts and Romani, {Roger W.} and Gloria Spandre and Fabrizio Tavecchio and Roberto Taverna and Yuzuru Tawara and Tennant, {Allyn F.} and Thomas, {Nicholas E.} and Francesco Tombesi and Alessio Trois and Tsygankov, {Sergey S.} and Roberto Turolla and Kinwah Wu and Fei Xie and Silvia Zane",

note = "Publisher Copyright: {\textcopyright} 2023. The Author(s). Published by the American Astronomical Society.",

year = "2023",

month = mar,

day = "1",

doi = "10.3847/1538-4357/acb496",

language = "English (US)",

volume = "945",

journal = "Astrophysical Journal",

issn = "0004-637X",

publisher = "American Astronomical Society",

number = "1",

}

Ferrazzoli, R, Slane, P, Prokhorov, D, Zhou, P, Vink, J, Bucciantini, N, Costa, E, Di Lalla, N, Di Marco, A, Soffitta, P, Weisskopf, MC, Asakura, K, Baldini, L, Heyl, J, Kaaret, PE, Marin, F, Mizuno, T, Ng, CY, Pesce-Rollins, M, Silvestri, S, Sgrò, C, Swartz, DA, Tamagawa, T, Yang, YJ, Agudo, I, Antonelli, LA, Bachetti, M, Baumgartner, WH, Bellazzini, R, Bianchi, S, Bongiorno, SD, Bonino, R, Brez, A, Capitanio, F, Castellano, S, Cavazzuti, E, Chen, CT, Ciprini, S, De Rosa, A, Del Monte, E, Di Gesu, L, Donnarumma, I, Doroshenko, V, Dovčiak, M, Ehlert, SR, Enoto, T, Evangelista, Y, Fabiani, S, Garcia, JA, Gunji, S, Hayashida, K, Iwakiri, W, Jorstad, SG, Kislat, F, Karas, V, Kitaguchi, T, Kolodziejczak, JJ, Krawczynski, H, La Monaca, F, Latronico, L, Liodakis, I, Maldera, S, Manfreda, A, Marinucci, A, Marscher, AP, Marshall, HL, Matt, G, Mitsuishi, I, Muleri, F, Negro, M, O’Dell, SL, Omodei, N, Oppedisano, C, Papitto, A, Pavlov, GG, Peirson, AL, Perri, M, Petrucci, PO, Pilia, M, Possenti, A, Poutanen, J, Puccetti, S, Ramsey, BD, Rankin, J, Ratheesh, A, Roberts, O, Romani, RW, Spandre, G, Tavecchio, F, Taverna, R, Tawara, Y, Tennant, AF, Thomas, NE, Tombesi, F, Trois, A, Tsygankov, SS, Turolla, R, Wu, K, Xie, F & Zane, S 2023, 'X-Ray Polarimetry Reveals the Magnetic-field Topology on Sub-parsec Scales in Tycho’s Supernova Remnant', Astrophysical Journal, vol. 945, no. 1, 52. https://doi.org/10.3847/1538-4357/acb496

TY - JOUR

T1 - X-Ray Polarimetry Reveals the Magnetic-field Topology on Sub-parsec Scales in Tycho’s Supernova Remnant

AU - Ferrazzoli, Riccardo

AU - Slane, Patrick

AU - Prokhorov, Dmitry

AU - Zhou, Ping

AU - Vink, Jacco

AU - Bucciantini, Niccolò

AU - Costa, Enrico

AU - Di Lalla, Niccolò

AU - Di Marco, Alessandro

AU - Soffitta, Paolo

AU - Weisskopf, Martin C.

AU - Asakura, Kazunori

AU - Baldini, Luca

AU - Heyl, Jeremy

AU - Kaaret, Philip E.

AU - Marin, Frédéric

AU - Mizuno, Tsunefumi

AU - Ng, C. Y.

AU - Pesce-Rollins, Melissa

AU - Silvestri, Stefano

AU - Sgrò, Carmelo

AU - Swartz, Douglas A.

AU - Tamagawa, Toru

AU - Yang, Yi Jung

AU - Agudo, Iván

AU - Antonelli, Lucio A.

AU - Bachetti, Matteo

AU - Baumgartner, Wayne H.

AU - Bellazzini, Ronaldo

AU - Bianchi, Stefano

AU - Bongiorno, Stephen D.

AU - Bonino, Raffaella

AU - Brez, Alessandro

AU - Capitanio, Fiamma

AU - Castellano, Simone

AU - Cavazzuti, Elisabetta

AU - Chen, Chien Ting

AU - Ciprini, Stefano

AU - De Rosa, Alessandra

AU - Del Monte, Ettore

AU - Di Gesu, Laura

AU - Donnarumma, Immacolata

AU - Doroshenko, Victor

AU - Dovčiak, Michal

AU - Ehlert, Steven R.

AU - Enoto, Teruaki

AU - Evangelista, Yuri

AU - Fabiani, Sergio

AU - Garcia, Javier A.

AU - Gunji, Shuichi

AU - Hayashida, Kiyoshi

AU - Iwakiri, Wataru

AU - Jorstad, Svetlana G.

AU - Kislat, Fabian

AU - Karas, Vladimir

AU - Kitaguchi, Takao

AU - Kolodziejczak, Jeffery J.

AU - Krawczynski, Henric

AU - La Monaca, Fabio

AU - Latronico, Luca

AU - Liodakis, Ioannis

AU - Maldera, Simone

AU - Manfreda, Alberto

AU - Marinucci, Andrea

AU - Marscher, Alan P.

AU - Marshall, Herman L.

AU - Matt, Giorgio

AU - Mitsuishi, Ikuyuki

AU - Muleri, Fabio

AU - Negro, Michela

AU - O’Dell, Stephen L.

AU - Omodei, Nicola

AU - Oppedisano, Chiara

AU - Papitto, Alessandro

AU - Pavlov, George G.

AU - Peirson, Abel L.

AU - Perri, Matteo

AU - Petrucci, Pierre Olivier

AU - Pilia, Maura

AU - Possenti, Andrea

AU - Poutanen, Juri

AU - Puccetti, Simonetta

AU - Ramsey, Brian D.

AU - Rankin, John

AU - Ratheesh, Ajay

AU - Roberts, Oliver

AU - Romani, Roger W.

AU - Spandre, Gloria

AU - Tavecchio, Fabrizio

AU - Taverna, Roberto

AU - Tawara, Yuzuru

AU - Tennant, Allyn F.

AU - Thomas, Nicholas E.

AU - Tombesi, Francesco

AU - Trois, Alessio

AU - Tsygankov, Sergey S.

AU - Turolla, Roberto

AU - Wu, Kinwah

AU - Xie, Fei

AU - Zane, Silvia

PY - 2023/3/1

Y1 - 2023/3/1

N2 - Supernova remnants are commonly considered to produce most of the Galactic cosmic rays via diffusive shock acceleration. However, many questions regarding the physical conditions at shock fronts, such as the magnetic-field morphology close to the particle acceleration sites, remain open. Here we report the detection of a localized polarization signal from some synchrotron X-ray emitting regions of Tycho’s supernova remnant made by the Imaging X-ray Polarimetry Explorer. The derived degree of polarization of the X-ray synchrotron emission is 9% ± 2% averaged over the whole remnant, and 12% ± 2% at the rim, higher than the value of polarization of 7%-8% observed in the radio band. In the west region, the degree of polarization is 23% ± 4%. The degree of X-ray polarization in Tycho is higher than for Cassiopeia A, suggesting a more ordered magnetic field or a larger maximum turbulence scale. The measured tangential direction of polarization corresponds to the radial magnetic field, and is consistent with that observed in the radio band. These results are compatible with the expectation of turbulence produced by an anisotropic cascade of a radial magnetic field near the shock, where we derive a magnetic-field amplification factor of 3.4 ± 0.3. The fact that this value is significantly smaller than those expected from acceleration models is indicative of highly anisotropic magnetic-field turbulence, or that the emitting electrons either favor regions of lower turbulence, or accumulate close to where the orientation of the magnetic field is preferentially radially oriented due to hydrodynamical instabilities.

AB - Supernova remnants are commonly considered to produce most of the Galactic cosmic rays via diffusive shock acceleration. However, many questions regarding the physical conditions at shock fronts, such as the magnetic-field morphology close to the particle acceleration sites, remain open. Here we report the detection of a localized polarization signal from some synchrotron X-ray emitting regions of Tycho’s supernova remnant made by the Imaging X-ray Polarimetry Explorer. The derived degree of polarization of the X-ray synchrotron emission is 9% ± 2% averaged over the whole remnant, and 12% ± 2% at the rim, higher than the value of polarization of 7%-8% observed in the radio band. In the west region, the degree of polarization is 23% ± 4%. The degree of X-ray polarization in Tycho is higher than for Cassiopeia A, suggesting a more ordered magnetic field or a larger maximum turbulence scale. The measured tangential direction of polarization corresponds to the radial magnetic field, and is consistent with that observed in the radio band. These results are compatible with the expectation of turbulence produced by an anisotropic cascade of a radial magnetic field near the shock, where we derive a magnetic-field amplification factor of 3.4 ± 0.3. The fact that this value is significantly smaller than those expected from acceleration models is indicative of highly anisotropic magnetic-field turbulence, or that the emitting electrons either favor regions of lower turbulence, or accumulate close to where the orientation of the magnetic field is preferentially radially oriented due to hydrodynamical instabilities.

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UR - http://www.scopus.com/inward/citedby.url?scp=85149839422&partnerID=8YFLogxK

U2 - 10.3847/1538-4357/acb496

DO - 10.3847/1538-4357/acb496

M3 - Article

AN - SCOPUS:85149839422

SN - 0004-637X

VL - 945

JO - Astrophysical Journal

JF - Astrophysical Journal

IS - 1

M1 - 52

ER -

X-Ray Polarimetry Reveals the Magnetic-field Topology on Sub-parsec Scales in Tycho’s Supernova Remnant

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