MAGIC Observations of the enigmatic γ-Cygni supernova remnant Marcel C. Strzysa S. Masu ab, ". Saitob, an I. #ovka for the MAGIC Collaboration a% Ma& 'lanc$ Institute for Physics! Germany b% Kyoto University! *apan "e# 'article Astrophysics +,-. at C/01! -2th Sep. +,-. G067.28,+.1 – the shell type S1R in the Cygnus region [English/Taylor/CGPS] [Nasa/Fermi LAT] ● Shell-type radio S10 ● Changing radio spectral inde& over shell: ,.5 9 ,.7 ;<adouceur8=,7> ● ?istance: -.6 9 +.. $pc @A I) ;<eahy8=-B> C-.6 $pc @D@?%) ;<ozins$aya8=,,> ● /&tent: C ,.2.◦ @C-6 pc% ● Age: C 5!7,, 9 -,!,,, years ;-5+, Mhz Data from CGPS] 15 - Sep. - +,-. M. Strzys 3 γ-Cygni 3 "e#'a +,-. +4-5 In ication of a cavity wall in A I [3 to 9 km/s] [-19 to -11 km/s] [adopted from Ladouceur+’08] ● Aint for a AI shell surrounding the SN0 ;<adouceur8=,7> ● Suppose to be compresse ISM by the Eind of the progenitor star ● "he region is comple& an e&istence of Eind-bloEn bubble not yet establishe ! feature might be ue to absorption ;<eahy+=-B> 15 - Sep. - +,-. M. Strzys 3 γ-Cygni 3 "e#'a +,-. B4-5 "he puzzling X-ray morphology ;ROSA" – ,.2-+ $e# – adopte - <eahy+=-B> ;0OSA" - <eahy+=-B> ;ASCA - )chiyama8=,+> ● In soft F-ray strong emission in north- and south-EestG in north even beyond shell ➔ "hermal emission from shock heated gas in non-eHuilibrium state ;<eahy8=-B> ➔ Chandra observation of centre suggest: reverse shock Iust recently shocked centre ;Aui8=-2> ● 'art of the north F-ray emission may come from stellar Eind of JB star @#-.72Cyg) ;<eahy8=-B> ● A feE hard non-thermal hard F-ray emission regions of Ehich C+ might be associated Eith S10 ;<eahy8=-B> 15 - Sep. - +,-. M. Strzys 3 γ-Cygni 3 "e#'a +,-. 54-5 "he Fermi high energy vieE – discovery of a peculiar pulsar ;count map ---, Ge#> ;Allafort8=-B> ● /mission dominated by 'S0 *+,+-85,+.! emits all its non-thermal energy in gamma-rays: L M <γ ● "he only $noEn pulsar variable in γ-rays ● N-, Ge# @'ulsar less significant% /mission all over the shell ;<ande8=-+> 15 - Sep. - +,-. M. Strzys 3 γ-Cygni 3 "e#'a +,-. 24-5 "oEar s the highest energies– the #/RI"AS observation ;Aliu8=-B> ● #/0ITAS observations found e&tended emission @P Q ,.+BR% toEar s north-Eest edge of the S10 ● Observations Eere preformed in +,,S an observation time Eas +-.. h ● Spectrum foun is single poEer-laE Eith inde& of +.B684-,.-5 and a level of B.6T Crab @NB+, Ge#% 15 - Sep. - +,-. M. Strzys 3 γ-Cygni 3 "e#'a +,-. .4-5 Aint for an energy dependent morphology in gamma-rays ;Aliu8=-B> Kermi-LA" count map B, - +,, Ge# ● #/0ITAS emission toEards north-Eest edge of the S10! structure not clearly resolve ● "oEards higher energies Kermi emission seen more toEards north-Eest shell (counts are Huite loE% 15 - Sep. - +,-. M. Strzys 3 γ-Cygni 3 "e#'a +,-. 64-5 A kind of magic – the MAGIC telescopes on Canary islan La 'alma ● Situated at the Observatorio del 0oHue de los Muchachos U ++,, m a.s.l. ● Stereo system of + & -6m dish telescopes ● /nergy range of 2, Ge# - 2, "e# [Aleksić+’16] 15 - Sep. - +,-. M. Strzys 3 γ-Cygni 3 "e#'a +,-. 74-5 "he MAGIC image of γ-Cygni – the "eV emission resolve > 200 GeV ● /Vective observation time of 57.B h after Huality selection @light transmission N7,T 9 measured Eith <IDA0 system) ● /mission detected coincides Eith the radio shell! but Iust in north-Eest region ● Substructures visible ● 'ulsar not visible @at least not above the steady emission) ● Star aVects analysis at loE 0ed star 9 'S0J +,+-85,+. energies in the south-east White star 9 Sadr mag. +.+ Orange 9 5,7 MHz contours from CG'S White Cont. - MAGIC Significance contours @B.!2.!6.P% 15 - Sep. - +,-. M. Strzys 3 γ-Cygni 3 "e#'a +,-. S4-5 "he MAGIC image of γ-Cygni – Comparison with #ERI"AS4Kermi ;Jgr. 15+, MAz from CG'SG blac$ #/0I"AS; Ehite MAGIC> ;Jgr. Fermi-<A" B,-+,, Ge#G white MAGIC> ● MAGIC contours e&tend beyond #/0ITAS count map contours! maIor4brightest part overlaps ● Kermi detects emission inside radio shell! MAGIC emission e&tends to outside the radio shell 15 - Sep. - +,-. M. Strzys 3 γ-Cygni 3 "e#'a +,-. -,4-5 "he energy depen ent morphology at very high energies +,, 9 2,, Ge# 2,, 9 -+2, Ge# +,, – 2,, Ge# N-+2, Ge# E ● In the Kermi-<A" energy range emission is situated inside shell ● "oEards higher energies! emission seems to be stretched to outside the shell 15 - Sep. - +,-. M. Strzys 3 γ-Cygni 3 "e#'a +,-. --4-5 Spectra – to be han le with care ;#/RITAS - Aliu8=-BG Kermi - KraiIa8=-.> ● Spectrum of #/RITAS @re integration region) an the main source in MAGIC @Ehite integration region) agree Eithin error barsG MAGIC spectral in e&: -+.55 ● /&traction of spectra from e&ten e region reHuires li$elihoo analysis → currently ongoing ● Comparison betEeen the iVerent energy ban s is complicate as the emission regions iVer ➔ More sophisticate analysis an S1R mo elling nee e 15 - Sep. - +,-. M. Strzys 3 γ-Cygni 3 "e#'a +,-. -+4-5 Some possible scenarios MAGIC observations identify the region around the north-Eest shoc$ as the region of "eV emission ➔ ha ronic particles interacting Eith the ambient me ium @cavity Eall! no OA maser foun %X ➔ or inverse Compton emissionX 'uzzling energy dependent morphology ➔ C0 escaping ahea of shoc$ frontX ➔ diVerent componentsX ➔ particular magnetic Oel structureX ➔ What is the role of the peculiar pulsarX 15 - Sep. - +,-. M. Strzys 3 γ-Cygni 3 "e#'a +,-. -B4-5 Summary ● MAGIC observations identify the region around the shock as the region of "e# emission ● 'uzzling energy dependent morphology ● Currently e&planation not clear! but Eor$ in progress → Stay tuned for further e&citements from the Gamma-Cygni S10 Thank you very much for your attention! 15 - Sep. - +,-. M. Strzys 3 γ-Cygni 3 "e#'a +,-. -54-5 BackUp – CO Map ● CO emission not coinciding Eith "e# emission ➔ target not visible in CO ➔ or "e# emission from electrons [Torres+’03] 15 - Sep. - +,-. M. Strzys 3 γ-Cygni 3 "e#'a +,-..