TY - JOUR
T1 - Probing cosmic ray ion acceleration with radio-submm and gamma-ray emission from interaction-powered supernovae
AU - Murase, Kohta
AU - Thompson, Todd A.
AU - Ofek, Eran O.
N1 - NASA - Space Telescope Science Institute [51310]; NASA [NAS 5-26555]KM thanks John Beacom, Roger Chevalier, Boaz Katz, Brian Lacki, Keiichi Maeda, Jose Prieto, Masaomi Tanaka and Ryo Yamazaki for useful discussions. KM is supported by NASA through Hubble Fellowship, Grant No. 51310.01 awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., for NASA, under Contract No. NAS 5-26555. KM also thanks supports by CCAPP since this project was started in the beginning of 2011 when KM was a member of CCAPP. The preliminary results of this work was presented in 2013 March, Hubble Fellows Symposium.
PY - 2014/5
Y1 - 2014/5
N2 - The optical and near-IR emission from some classes of supernovae (SNe), including Type IIn and possibly some super-luminous SNe, is likely powered by a collision between the SN ejecta and dense circumstellar material (CSM). We argue that for a range of CSM masses and their radii, a collisionless shock can form, allowing for efficient cosmic ray (CR) acceleration. We show that pp collisions between these newly accelerated CRs and the CSM leads to not only gamma rays but also secondary electrons and positrons that radiate synchrotron photons in the high-frequency radio bands. Our estimates imply that various facilities including the Jansky Very Large Array (and the Atacama Large Millimeter/submillimetre Array (ALMA) may observe such SNe at Gpc distances by followup observations in months-to-years, although the detectability strongly depends on the CSM density as well as observed frequency. Detecting this signal would give us a unique probe of CR acceleration at early times, and even non-detections can put interesting limits on the possibility of CR ion acceleration. Following our previous work, we also show that GeV gamma rays can escape from the system without severe attenuation, encouraging point-source and stacking analyses with Fermi. We provide recipes for diagnosing interaction-powered SN scenario with multi-messenger (neutrino and gamma-ray) observations.
AB - The optical and near-IR emission from some classes of supernovae (SNe), including Type IIn and possibly some super-luminous SNe, is likely powered by a collision between the SN ejecta and dense circumstellar material (CSM). We argue that for a range of CSM masses and their radii, a collisionless shock can form, allowing for efficient cosmic ray (CR) acceleration. We show that pp collisions between these newly accelerated CRs and the CSM leads to not only gamma rays but also secondary electrons and positrons that radiate synchrotron photons in the high-frequency radio bands. Our estimates imply that various facilities including the Jansky Very Large Array (and the Atacama Large Millimeter/submillimetre Array (ALMA) may observe such SNe at Gpc distances by followup observations in months-to-years, although the detectability strongly depends on the CSM density as well as observed frequency. Detecting this signal would give us a unique probe of CR acceleration at early times, and even non-detections can put interesting limits on the possibility of CR ion acceleration. Following our previous work, we also show that GeV gamma rays can escape from the system without severe attenuation, encouraging point-source and stacking analyses with Fermi. We provide recipes for diagnosing interaction-powered SN scenario with multi-messenger (neutrino and gamma-ray) observations.
UR - https://www.scopus.com/pages/publications/84898824669
U2 - 10.1093/mnras/stu384
DO - 10.1093/mnras/stu384
M3 - Article
SN - 0035-8711
VL - 440
SP - 2528
EP - 2543
JO - MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
JF - MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
IS - 3
ER -