MAGICによる最近の観測結果
齋藤浩二 (ICRR)
03.09.2013

1

MAGIC望遠鏡
MAGIC(Major Atmospheric Gamma-ray Imaging Cherenkov)* 17 m鏡面を持つ大気チェレンコフ望遠鏡* エネルギー閾値: 50 GeV* 2004年〜 MAGIC-I、2009年〜2台の望遠鏡によるステレオ観測* 2011-2012年 望遠鏡アップグレード

MAGIC-IIMAGIC-I
17 m2

MAGIC望遠鏡
Bulgaria: Sofia
Croatia: Consortium (Zagreb+)
Finland: Consortium (Tuorla+)
Germany: U. Dortmund, MPI München,
U. Würzburg, DESY Zeuthen
Italy: U. Como, INFN Padova/U.
Padova, INAF Rome, INFN Pisa/U.
Siena, INFN Trieste/U. Udine
Japan: Consortium (Kyoto+)
Poland: Univ. ŁódźSpain: IFAE Barcelona, UAB Barcelona,
U. Barcelona, IEEC-CSIC Barcelona,
IAA Granada, IAC Tenerife, U.
Complutense Madrid, CIEMAT Madrid
Switzerland: ETH Zurich

MAGIC望遠鏡: スペイン・カナリア諸島ラパルマ島(28°46N, 17°53W, 2231 m a.s.l.)3

望遠鏡アップグレード
新MAGIC-Iカメラ: MAGIC-IIカメラクローン
567 PMTs → 1039 PMTs
トリガー領域 1.9 Φ → 2.5 Φ
PMT量子効率向上
etc.
新リードアウトシステム
Mux FADCs(M-I) & DRS2(M-II) → DRS4
DRS2→DRS4: 帯域幅、クロストーク、リニアリテ
ィ、S/N、デッドタイム(500μs → 26μs)向上

旧MAGIC-Iカメラ

1.9°

MAGIC-IIカメラ

2011年6月-11月
両望遠鏡リードアウトDRS4へ
Electrics roomリニューアル他2012年6月-10月
MAGIC-Iカメラ交換
MAGIC-Iリードアウト、トリガーシステムアップグレード

2.5°4望遠鏡アップグレード
22 h CrabNebula data 2012 Oct. - 2013 Jan, Zd < 30

E < 100 GeV
Sensitivity: 5.4 % C.U.
(Before Upgrade ~10 %)E > 250 GeV
Sensitivity: 0.7 % C.U.
(Before Upgrade ~0.8 %)5

W51
ROSAT 0.7-2.5 keV
Koo+ 2002

Fermi-LAT 2-10 GeV
Uchiyama+ 2011

H.E.S.S. >1 TeVFiasson+ ICRC2009

W51C: d ~ 5.5 kpc, medium age (30 kyr)supernova remnant (SNR)
Possible pulsar wind nebula associatedto W51C
W51C interacts with W51B
Discovered by Fermi (~GeV)
H.E.S.S. 4.4σ (>1 TeV)
6

W51
Data taken in 2010 & 2011
> 150 GeV

53 h eﬀective time
11.6σ detection (>150 GeV)
Extension:
0.12 0.02 sys 0.02 stat

Observation center
Determined position
Molecular gas
Possible PWN

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W51
Top: 300 GeV - 1 TeV
Bottom: > 1 TeV
Underlying structures?
Two independent
resolved sources
cannot be statisticallyestablishedNo energy dependent
Cloud: 1.2 % C.U.
(> 300 GeV)PWN: 0.7 % C.U.
(> 300 GeV)

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W51Best ﬁt results:Possible 20 %contribution from PWN,
within the statisticaland systematic errorsof MAGIC observation
No one-zone Leptonic model matching the data is found.
Agreement with Abdo+ 2009
Simple one-zone hadronic model explains the data

9HESS J1857+026
Discovered by H.E.S.S.
(Aharonian+ 2008)
Spectral slope -2.4 (>500GeV)~0.1 extension
Possible pulsar wind nebula
PSR J1856+02245 (Hessels+2008)
Distance ~9 kpc
Ė = 4.6 1036 erg/s
Fermi-LAT (Rousseau+ 2012):
Spectral slope -1.5 (< 100GeV)
Point like (>10 GeV)
10HESS J1857+026
Preliminary

Observed in 2010~30 h eﬀective time
~12σ detection
2 sources above 1 TeVMAGIC J1857.2+0263:
0.21 extension
45 % ﬂux contribution
Preliminary

Counterparts: HESS J1857+026,
PSR J1856+0245, Fermi-LAT
MAGIC J1857.6+0297:
0.14 extension
20 % ﬂux contribution
No counterpart11

HESS J1857+026
13CO(J = 1→0) line emission integrated intensity

Preliminary

Preliminary

Preliminary

Nature of the VHE emission of MAGIC J1857.6+0297 remains a mystery
MAGIC J1857.6+0297 lies in the vicinity of HII region
Compact HII region U36.40+0.02 with VLSR = 53.3 km/s (3.3 kpc) which may
be associated with the molecular cloud G036.59-00.06
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PG 1553+113
Discovered by H.E.S.S. & MAGIC in 2005
Uncertain redshift z >0.4 (Danforth+ 2010), z <0.66 (Prandini+ 2010)
Have been observed by MAGIC since 2005, showing modest ﬂux variation
Stable ﬂux seen during 4 years by Fermi-LAT
February-March 2012 high ﬂux
state was observed by MAGIC(ATel #3977)
April 2012 MAGIC detected ﬂare(ATel #4069)
Most extensive multiwavelength
campaign13PG 1553+113

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PG 1553+113
Power-law ﬁt to observed
energy spectrum in ﬂare gives
low probability χ2/d.o.f. =36.2/8Observed spectrum

Preliminary

compatible with logparabola

f0 = 5.1 0.3x10-10 cm-2s-1TeV-1
a = 3.7 0.1
b = 1.4 0.3
EBL-corrected spectra (withDominguez+ 2011): reproducedby power-law assuming z = 0.415

PG 1553+113
SED modeling assuming z = 0.4
One-zone SSC model, e- broken power-law distribution
Size of emission region is one order of magnitude higher than in theprevious observations in order to keep the Doppler factor not too highPreliminary

16IC 310
Serendipitously detected by Fermi-LAT (Neronov+2010) above 30 GeV and by MAGIC (Aleksić+ 2010)
above 260 GeV- Hard spectrum in VHE: Γ = 2.0- Daily-scale VHE ﬂux variability

IC 310 has been classiﬁed as a head-tail galaxy (e.g.
Ryle & Windram 1968) which is found only in clustersof galaxies- Jet direction is determined by the galaxyʼs motion
through the intra-cluster medium (ICM)- “head”: bow shock due to the impact of the jet onthe ICM- “tail”: redirected extended jetHowever, VLBA images show a blazar-like parsec
scale structure (Kadler+ 2012)- There is no indication of an interaction with ICM- The source belongs to a transitional population
between BL Lac and FR I radio galaxy (Rector+ 1999,Kadler+2012)17

IC 310
VHE ﬂare in Nov 2012
28.5σ in 3.5 h (>250 GeV) at beginning of MWL campaign (Cortina et al.
Atel #4583)
56 % C.U. (>250 GeV): 2.5 % C.U. for the mean ﬂux in 2009/2010, 12.5% C.U. for the high state in 2009/2010 (Aleksić+ 2013)
Spectrum shape stayed the same in spite of the large ﬂux variability18

IC 310Multiwavelength Light Curve
Fermi-LAT: only upper limit(>1 GeV)
Swift-XRT: no strong
variability but ﬂux is higher
than in previous observations
Optical: dominated by hostgalaxy
Radio: at 15 GHz nosigniﬁcant variability
Detailed analysis on theMWL data is ongoing

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FSRQsFlat Spectrum Radio Quasars: Only 3 sources seen by IACTs
3C 279 (z = 0.536)

PKS 1222+216 (z = 0.432)

Great impact discovery by MAGIC inDiscovered by MAGIC in 2010 during GeV

2006

ﬂare observed by Fermi-LAT

Detected again during historical

Fastest time scale variability (~10 min)optical ﬂare in 2007

among FSRQs

No signal in 20 h monitoring in 2011

Challenges canonical emission models

ToO in June 2011 results in nodetection

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FSRQsPKS 1510-089 (z = 0.361)
Discovered by H.E.S.S. in 2009 (Abramowski+ 2013)
MAGIC observations triggered by HE gamma-ray ﬂare (AGILE and Fermi) in 2012
MAGIC observed for 28 nights between February and April
6σ detection with 21 hour good quality dataMAGIC & LAT spectra connect smoothly

Preliminary

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FSRQsPKS 1510-089 2012 MWL
VHE ﬂux shows no signiﬁcantvariation: apparent discrepancy withthe other FSRQs
HE gamma-ray ﬂares seem to beaccompanied by the simultaneous
ﬂares in 37 GHz radio
Gamma-ray ﬂare also coincident withthe ejection of new radio component
Suggested that the gamma-ray andmillimeter ﬂaring activities are cospatial
VLBA core: 10 pc away from thecentral engine (e.g. Jorstad+ 2012)22

Newest Discoveries
MS 1221.8+2452
HBL at z = 0.218
Weak Fermi source but very hard spectrum above 10 GeV (Γ = 1.26)
Discovered in April 30th and May 1st 2013 (ATel #5038)
6σ in 3.7 hour
4 % C.U. (>200 GeV)For EBL and IGMF studies

Preliminary23

Newest Discoveries
H 1722+119
TeV candidate BL Lac in Costamante & Ghisellini (2002)
Uncertain redshift, lower limit of 0.17
Past MAGIC observations in 2004-2009: U.L. 4 % C.U. above 140 GeV
In May 2013 the Tuorla blazar monitoring program reported the highest opticalﬂux ever observed since 2005
>5σ detection in 10 hour (ATel #5080)

Preliminaryhttp://users.utu.fi/kani/1m24

Summary & Outlook
2011年-2012年望遠鏡アップグレード
低エネルギー領域でさらにパフォーマンス向上
Galactic/Extragalactic共にいくつもの興味深いサイエンス結果を提供し続けている

今後5-7年 安定したオペレーション
ステレオSumトリガーのインストール in 今年25