-Cygni -Cygni the GeV to TeV Morphology the GeV to TeV - PowerPoint PPT Presentation

γ-Cygni -Cygni γ the GeV to TeV Morphology the GeV to TeV Morphology with with MAGIC and Fermi-LAT MAGIC and Fermi-LAT Marcel C. Strzys a I. Vovk a , C. Fruck a , S. Masuda b and T. Saito b for the MAGIC Collaboration a) Max Planck Institute for Physics, Germany b) Kyoto University, Japan ICRC 2017 Busan, 17 th Jul. 2017 Marcel C. Strzys

Gamma-ray supernova remnants Gamma-ray supernova remnants [VERITAS ICRC 2015] [H.E.S.S. - Aharonian+ 2007] ● π 0 Cutofg → Evidence for hadronic CRs Shell bright ● ● Interaction region ● Leptonic / bright hadronic ? ● Matured SNRs ● ≈ 1-5 10 3 yrs (≈ 10 4 yrs) [Funk ‘15] Mon. 17. July 2017 2/9 Marcel C. Strzys γ-Cygni with MAGIC | ICRC Busan

The γ γ-Cygni supernova remnant -Cygni supernova remnant The [English+T aylor/CGPS] [ 1 4 2 0 M H z D a t a f r o m C G P S ] Age: 5 – 10 kyr SNR clearly in Sedov phase: → reverse shock hit centre 1.5 kyr ago [Hui+‘14] Remnant of a core-collapse SNR (PSR at the centre) Distance: 1.5 – 2.6 kpc Extend: ≈0.56⁰ radius , (≈17 pc) Mon. 17. July 2017 3/9 Marcel C. Strzys γ-Cygni with MAGIC | ICRC Busan

γ-Cygni in -Cygni in γ γ-rays -rays γ TeV GeV VERITAS (> 320 GeV) Fermi -LAT (> 15 GeV) [ A l i u + ’ 1 3 ] [ L a n d e + ’ 1 2 ] Detected at T eV by VERITAS using 21 h obs. time → extended emission (σ=0.23⁰) towards north-west → power-law spectrum (Γ=2.37+/-0.14) → integral fmux 3% Crab Units Fermi -LAT observes emission all over shell at GeV energies < 10 GeV emission dominated by PSR J2021+4026 → only known γ-ray variable PSR Mon. 17. July 2017 4/9 Marcel C. Strzys γ-Cygni with MAGIC | ICRC Busan

MAGIC observations of γ γ-Cygni -Cygni MAGIC observations of [Aleksić+’16] Situated at the Observatorio Roque de los Muchachos @ 2200 m a.s.l. Stereo system of 2 x 17m telescopes Energy range from 50 GeV – 50 T eV Obs. time 46 h Data selection: aerosol transmission (>80%) measured with LIDAR system Mon. 17. July 2017 5/9 Marcel C. Strzys γ-Cygni with MAGIC | ICRC Busan

MAGIC view on γ γ-Cygni -Cygni MAGIC view on > 200 GeV Emission strongest in the Preliminary north-west: → bright extended source → part of emission aligned along shell → hint for emission inside shell PSR not visible Emission can be well described by multiple component model: → Disk matching radio shell → Gaussian source ◆ : PSR 2021+4026 Simultaneous 2D-Likelihood fjt: ★ : Sadr (mag. 2.2) → novel SkyPrism program ─ : 408 MHz Cont. → 5.7 σ for disk (CGPS) → 11.9 σ for Gaussian Mon. 17. July 2017 6/9 Marcel C. Strzys γ-Cygni with MAGIC | ICRC Busan

Energy dependent morphology Energy dependent morphology 200 - 450 GeV - MAGIC 50 - 200 GeV - Fermi -LAT 15 - 50 GeV - Fermi -LAT > 450 GeV - MAGIC Energy ● > 50 GeV emission concentrated towards north-west, compare [Fraija+’16] ● > 450 GeV emission outside shell Mon. 17. July 2017 7/9 Marcel C. Strzys γ-Cygni with MAGIC | ICRC Busan

ISM around the SNR ISM around the SNR CO 2->1 contours + MAGIC flux map HI [-11 to -19 km/s] (Planck) ROSAT PSPC [ 0 . 5 - 2 k e V ] [Ladouceur+’08] → ● S o f t X - r a y s s h o w s h o c k h e a t e d g a s i n n o r t h d e n s e r m e d i u m , b u t n o M a s e r f o u n d ● A G N c l o s e t o S N R , b u t n o c o u n t e r p a r t w h e r e T e V e m i s s i o n i s f o u n d ● C O e m i s s i o n n e x t t o M A G I C e m i s s i o n r e g i o n ● H i n t f o r a H I s h e l l s u r r o u n d i n g t h e S N R , c a v i t y w a l l c r e a t e d b y p r o g e n i t o r [ L a d o u c e u r + ’ 0 8 ] Mon. 17. July 2017 8/9 Marcel C. Strzys γ-Cygni with MAGIC | ICRC Busan

Summary Summary MAGIC observations revealed multiple component morphology Spectrum consistent with Fermi and VERITAS Energy dependent morphology: → LE (<450 GeV) confjned in shell → HE extending beyond Leakage of CRs interacting with cloud or cavity wall as plausible scenario Thank you for your attention and interest! Mon. 17. July 2017 9/9 Marcel C. Strzys γ-Cygni with MAGIC | ICRC Busan