SNRs as PeVatron candidates for CTA

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Presentation transcript:

SNRs as PeVatron candidates for CTA 1/18/2019 SNRs as PeVatron candidates for CTA Ziwei Ou Institut de Physique Nucléaire d’Orsay Université Paris-Sud Supervisor: Tiina Suomijärvi 2018|10|08 1 1

Cherenkov Telescope Array Supernova Remnants as PeVatron candidates 1/18/2019 Cherenkov Telescope Array Supernova Remnants as PeVatron candidates Naima and model fitting Main results Summary 2 2

Cherenkov Telescope Array (CTA) Small-sized telescopes (SST): 1 TeV - 300 TeV Medium-sized telescopes (MST): 100 GeV - 10 TeV Large-sized telescopes(LST): 20 GeV- 200 GeV North site: La Palma (Spain) South site: Paranal (Chile)

CTA detect the Cherenkov light induced by gamma-ray

LST, 2017-11, La Palma, Spain

MST, 2018-09, DESY, Germany

CTA: Cosmic-rays PeVatron as a Key Science Project (KSP) from Rene Ong (2015)

Cosmic-Rays accelerated up to 1 PeV PeVatrons: astrophysical object accelerated particles above 1 PeV (10^15eV). The energy of spectrum of Cosmic-Rays (CRs) extends until few PeV where it steepens originating the ‘knee’. Theoretical prediction and measurements of CR indicate that the CR should be accelerated up to 1 PeV in our Galaxy.

Supernova Remnants (SNRs) as promising Galactic PeVatron candidates The detection of SNRs with spectrum up to 100 TeV imply that they are one kinds of PeVatron candidates, because ~100 TeV photons are produced by ~ PeV protons. (observation) SNRs are able to satisfy the cosmic-ray energy requirement by converting the kinetic energy into accelerated particle. (theory) SNRs (and Pulsar Wind Nebulae) are the majority of Galactic poululation.

Proton-proton collision induces pion decay \ For accelerated protons, hadronic interactions with ambient matter produce neutral pion, decaying into two γ-ray photons

DC-1 data, Prod3b IRF and ctools Data Challenge one (DC-1): simulated data enable the CTA Consortium Science Working Group to derive science benchmarks for the CTA KSP. DC-1 includes Galactic Plane Scan (GPS) as one of the key science projects. We use GPS data to analysis SNRs. Prod3b Instrumental Response Functions (IRFs): the performance values are derived from Monte Carlo simulation of CTA instrument based on the CORSIKA air shower code. Ctools: a soft package developed for scientific analysis of CTA data. We run ctools pipeline to judge whether SNRs from TeVCat are considered in DC-1 GPS, and to draw the spectrums.

Low Galactic latitude from TeVCat

Naima python package

Radiation mechanism for SNRs Four main non-thermal radiative mechanisms for producing γ-ray Synchrotron pion-decay

Electron and proton follow exponential cutoff power-law

1/18/2019 18 18

HESS J1731-347 Spectral Energy Distribution 1/18/2019 HESS J1731-347 Spectral Energy Distribution 19 19

1/18/2019 20 20

Summary Proton cut-off energy values as PeVatron indicators. Distinguish pion-decay or inverse Compton process dominate SNRs radiation. I do not consider the energy dispersion. Reset the XML model definition file to smooth residuals maps.