Detection of the Characteristic Pion-Decay Signature in Supernova Remnants

  title={Detection of the Characteristic Pion-Decay Signature in Supernova Remnants},
  author={Markus Ackermann and Marco Ajello and Alice Allafort and Luca Baldini and Jean Ballet and Guido Barbiellini and Matthew G. Baring and Denis Bastieri and Keith C. Bechtol and Ronaldo Bellazzini and Roger D. Blandford and Elliott D. Bloom and Emanuele Bonamente and A. W. Borgland and Eugenio Bottacini and Theresa J. Brandt and Johan Bregeon and Monica Brigida and Philippe Bruel and Rolf Buehler and G. Busetto and Sara Buson and G. A. Caliandro and R. A. Cameron and Patrizia A. Caraveo and J. M. Casandjian and Claudia Cecchi and {\"O}. Çelik and Eric Charles and Sylvain Chaty and Ryan C. G. Chaves and A. Chekhtman and C. C. Cheung and J. Chiang and Graziano Chiaro and Anal{\'i}a N. Cillis and Stefano Ciprini and Richard O. Claus and J. Cohen-Tanugi and Lynn R. Cominsky and Janet M. Conrad and St{\'e}phane Corbel and S. Cutini and Filippo D’Ammando and Alessandro De Angelis and Francesco de Palma and Charles D. Dermer and Eduardo do Couto e Silva and P. S. Drell and Alex Drlica-Wagner and Luigi Falletti and Cecilia Favuzzi and Elizabeth C. Ferrara and Anna Franckowiak and Yasushi Fukazawa and Stefan Funk and Piergiorgio Fusco and Fabio Gargano and Stefano Germani and Nicola Giglietto and Paolo Giommi and Francesco Giordano and Marcello Giroletti and Tom Glanzman and Gary Lunt Godfrey and Isabelle A. Grenier and M.-H. Grondin and J. E. Grove and Sylvain Guiriec and D. Hadasch and Yoshitaka Hanabata and Alice K. Harding and Morihiro Hayashida and K. Hayashi and Elizabeth Hays and John W. Hewitt and A. B. Hill and Richard Edward Hughes and Miranda S. Jackson and T. Jogler and Guðlaugur J{\'o}hannesson and A. S. Johnson and Tuneyoshi Kamae and Jun Kataoka and J. Katsuta and J{\"u}rgen Kn{\"o}dlseder and Michael Kuss and Joshua Lande and Stefan Larsson and Luca Latronico and Marianne Lemoine-Goumard and Francesco Longo and Francesco Loparco and Michael N. Lovellette and Pasquale Lubrano and Grzegorz Madejski and Francesco Massaro and Matthias P. Mayer and Mario Nicola Mazziotta and Julie Mcenery and J. M{\'e}hault and P. F. Michelson and Roberto P. Mignani and W. Mitthumsiri and Tsunefumi Mizuno and Alexander A Moiseev and M. E. Monzani and A. Morselli and Igor V. Moskalenko and Simona Murgia and Takeshi Nakamori and Rodrigo S. Nemmen and Eric Nuss and Masanori Ohno and Takashi Ohsugi and Nicola Omodei and Monica Orienti and E. Orlando and J. F. Ormes and D. Paneque and Jeremy S. Perkins and Melissa Pesce-Rollins and F. Piron and G. Pivato and S. Rain{\'o} and R. Rando and Massimiliano Razzano and Soebur Razzaque and Anita Reimer and O. Reimer and Steven M. Ritz and Carlo Romoli and M. S{\'a}nchez-Conde and Alex Schulz and Carmelo Sgro’ and Paul Simeon and Eric J. Siskind and D. A. Smith and Gloria Spandre and Paolo Spinelli and Floyd W. Stecker and A. W. Strong and Daniel J. Suson and Hiroyasu Tajima and H. Takahashi and T. Takahashi and T. Tanaka and John Gregg Thayer and Jana Thayer and D. J. Thompson and Stephen Erik Thorsett and Luigi Tibaldo and Omar Tibolla and Marco Tinivella and Eleonora Troja and Yasunobu Uchiyama and T. L. Usher and Justin Vandenbroucke and Vlasios Vasileiou and Giacomo Vianello and Vincenzo Vitale and A. P. Waite and M. Werner and Brian Winer and Kent S. Wood and Matthew J.A. Wood and Ryo Yamazaki and Z. Yang and Stephan Zimmer},
  pages={807 - 811}
Accelerated Protons Although cosmic rays were first detected a hundred years ago, their origin is still not fully understood. Comic rays are high-energy particles, mostly protons, which bombard Earth from outer space. Most of those that originate from within our galaxy are thought to be accelerated in the shock waves from the explosion of massive stars, or supernovae. Protons accelerated in a supernova remnant will collide with interstellar material producing pions, a type of subatomic particle… 

Supernova remnants and the origin of cosmic rays

  • J. Vink
  • Physics
    Proceedings of the International Astronomical Union
  • 2013
Abstract Supernova remnants have long been considered to be the dominant sources of Galactic cosmic rays. For a long time the prime evidence consisted of radio synchrotron radiation from supernova

Theoretical study of ionization profiles of molecular clouds near supernova remnants. Tracing the hadronic origin of GeV gamma radiation

Context : Since a few years, signatures of supernova remnants have been detected in gamma rays, particularly those that are known to be associated with molecular clouds. Whether these gamma rays are

Gamma Rays from Cosmic Rays in Supernova Remnants

Context. Cosmic rays are thought to be accelerated at supernova remnant (SNR) shocks, but obtaining conclusive evidence for this hypothesis is difficult. Aims. New data from ground-based -ray

Gamma-ray and Neutrino Signatures of Galactic Cosmic-ray Accelerators

Supernova remnants are believed to be the major contributors to the observed Galactic cosmic-ray flux, though indisputable observational pieces of evidence of such statement are still missing. A

Search for New Cosmic-Ray Acceleration Sites within the 4FGL Catalog Galactic Plane Sources

Cosmic rays are mostly composed of protons accelerated to relativistic speeds. When those protons encounter interstellar material, they produce neutral pions, which in turn decay into gamma-rays.

The supernova remnant SN 1006 as a Galactic particle accelerator

The origin of cosmic rays is a pivotal open issue of high-energy astrophysics. Supernova remnants are strong candidates to be the Galactic factory of cosmic rays, their blast waves being powerful

Gamma-ray observations of supernova remnants

Abstract In the past few years, gamma-ray astronomy has entered a golden age. At TeV energies, only a handful of sources were known a decade ago, but the current generation of ground-based imaging

SNR G39.2−0.3, an hadronic cosmic rays accelerator

Recent results obtained with gamma-ray satellites have established supernova remnants as accelerators of GeV hadronic cosmic rays. In such processes, CRs accelerated in SNR shocks interact with

Cosmic-ray acceleration and escape from post-adiabatic supernova remnants

Context. Supernova remnants are known to accelerate cosmic rays on account of their nonthermal emission of radio waves, X-rays, and gamma rays. Although there are many models for the acceleration of



Gamma-Ray Emission from the Shell of Supernova Remnant W44 Revealed by the Fermi LAT

An image is obtained of the supernova remnant W44, which shows associated gamma-ray emissions in the order of gigaelectronvolts, conforming with models indicating local proton and nuclei acceleration, and implies that the emission is produced by particles accelerated there.

High energy gamma-ray emission from supernova remnants

Since Galactic cosmic rays are believed to be created in supernova remnants (SNRs), SNRs are expected to be a source of high energy gamma -rays through the decay of neutral pions produced by p-p

Measuring the Cosmic-Ray Acceleration Efficiency of a Supernova Remnant

The pressure induced by cosmic rays exceeds the thermal pressure behind the northeast shock of the supernova remnant RCW 86, where the x-ray emission is dominated by synchrotron radiation from ultrarelativistic electrons.

Extremely fast acceleration of cosmic rays in a supernova remnant

Broadband X-ray spectrometric measurements of RX J1713.7-3946 indicate that electron acceleration proceeds in the most effective (‘Bohm-diffusion’) regime, providing a strong argument for acceleration of protons and nuclei to energies of 1 PeV (1015 eV) and beyond in young supernova remnants.

Gamma-rays from molecular clouds illuminated by cosmic rays escaping from interacting supernova remnants

Recently, the gamma-ray telescopes AGILE and Fermi observed several middle-aged supernova remnants (SNRs) interacting with molecular clouds. It is likely that their gamma-rays arise from the decay of


The discovery of bright gamma-ray emission coincident with supernova remnant (SNR) W51C is reported using the Large Area Telescope (LAT) onboard the Fermi Gamma-ray Space Telescope. W51C is a


The supernova remnant (SNR) IC 443 is an intermediate-age remnant well known for its radio, optical, X-ray, and gamma-ray energy emissions. In this Letter, we study the gamma-ray emission above 100


We report observation of the supernova remnant (SNR) IC 443 (G189.1+3.0) with the Fermi Gamma-ray Space Telescope Large Area Telescope (LAT) in the energy band between 200 MeV and 50 GeV. IC 443 is a

Broad-band non-thermal emission from molecular clouds illuminated by cosmic rays from nearby supernova remnants

Molecular clouds are expected to emit non-thermal radiation due to cosmic ray interactions in the dense magnetized gas. Such emission is amplified if a cloud is located close to an accelerator of