MAGIC and CTA LST

Koji Noda (ICRR, U. Tokyo)
for MAGIC Collaboration and CTA consortium
18-20 Feb 2019
VHEPA 2019 @ ICRROutline• MAGIC science–Galactic–Extragalactic–Fundamental physics–Transients• CTA status–Overview–Large Sized Telescopes (LSTs)–LST1 status• Summary2MAGIC• The MAGIC Collaboration: ~170 collaborators in 10 countries.
• Stereo system of two Imaging Atmospheric Cherenkov Telescopes(IACTs). MAGIC-I since 2004, and MAGIC-II since 2009.
• Upgraded to homogenise the system. Stable operation since 2013.
• 17 m diameter, Eth ~= 70 GeV (analysis), lower with sum trigger• Light weight => fast movement to catch transients (20 s / 180º)3

Performance since 2013
• Trigger threshold down
to ~50 GeV (low zenith)• Analysis threshold down
to 70 GeV.
• Energy resolution
15%-23% below 10 TeV• Angular resolution<0.07° above 300 GeV• Sensitivity 0.6% CrabNebula flux in 50 hours
More special efforts to maximise the duty cycle• Correction for atm. transmission with LIDAR (operational since2013, method available since 2015)• Systematic observations under moon (Astropart.Phys. 94 (2017) 29)
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MAGIC science highlights(roughly, from closer to further, and to unknown)
5Galactic: pulsars
Crab pulsar(MAGIC Coll. A&A 585 (2016) A133)• MAGIC discovery > 25 GeV(Science 322 (2008) 1221)– VERITAS detects > 100 GeV (2011)• Extended the spectra up to 400
GeV and measured P1/2 spectra
separately (A&A 540 (2012) 69)• MAGIC discovery of emission
up to TeV (A&A 585 (2016) A133)

Geminga pulsar• MAGIC discovery of P2 > 5 sigma
from 30 hr obs. with sum trigger• Became the 3rd known pulsar inVHE gamma
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Galactic: SNR CasA

M. Ahnen et al. (MAGIC Coll.), MNRAS, 472 (2017) 3• SNRs as PeV CR accelerators "PeVatron". CasA is one of the best
candidates: young (~300 yr) & good MWL data to limit the models• ~158 hr of MAGIC obs, 3/4 of which is taken under moon
• MAGIC spectrum shows a cut-off at a few TeV• If hadronic (and unless significant diffusion), CasA is not a PeVatron
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Galactic: binaries
PSR J2032+4107
New binary in TeV
range discovered
through joint
campaign ofMAGIC & VERITAS
ApJL, 867 (2018) L19

HESS J0632+057
Joined effort of H.E.S.S., MAGIC & VERITAS to publish last paper on thissource with current generation of Cherenkov telescopes

LS I +61 303
20 hrs of data taken in 2018 within campaign with VERITAS and opticaltelescope Liverpool on La PalmaOthers (CygX-1, V404 Cygni, SS433/W50,,,)8

Extragalactic: Nearby AGNs
NGC1275 / IC310

Ahnen et al., A&A, 603 (2017) A25• z = 0.017, 0.019• MW studies of extremely fastvariability in IC310 in 2014 =>• NGC1275 also has day-scalevariability in 2016-2017 data(A&A 617 (2018) A91)

Mrk421 / 501• Well known HBL at z ~= 0.03
• Yearly monitoring campaigns• Mrk501 2012: hard spectrum
do not change with states, behaving
as an extreme HBL• 'Bump' in Mrk501 flare in 2014?

Ahnen et al., A&A, 620 (2018) A181

M87, NGC1068,,, stay tuned
9Extragalactic: distant AGN• Lowest possible energy
threshold in VHE range
less EBL, distant sources• The farthest record so far:
B0218+35 flare detected
11.5 days after Fermi-LAT,which is well interpreted asa gravitational lensing(Ahnen et al., A&A 595 (2016) A98)

• Recent news: TON0599 as
the 3rd farthest VHE source(ATel #11061, Dec 2017)

Expanding the VHE horizon
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Fundamental physics• Dark Matter search
for annihilation signal– Galactic Dwarf
Segue I
Ursa Major IIetc.
– Galactic CenterAleksic et al. JCAP 03 (2018) 009

Ahnen et al. JCAP 02 (2014) 008• Tau neutrinos
Limits on flux (1 PeV - 3 EeV)
(Astropart.Phys. 102 (2018) 77)– Observation for 31.5 hrdirecting to the sea11

Transients• Transients: new physics working group• Strong relation with multi-messenger astronomy,
as mostly triggered by other instruments• multi-wavelength: Radio, optical, keV, MeV,,,
– GRB
– FRB
(ULs on the repeating FRB 121102 (MAGIC Coll.,MNRAS 481 (2018) 2479) )– Novae, etc.

• multi-messenger:
Real time events were / will be automatically followed up– IceCube/ANTARES HE neutrinos– LIGO/Virgo gravitational waves(First IACT followup of GW151226. More to follow in the coming O3)
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Transients / multi-messenger:
blazar TXS0506+056 (z=0.3365)• flare coincident with IceCube event IC-170922A: highlight in 2018

Science361(2018)
eaat1378

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TXS0506: MWL modeling(MAGIC Coll., ApJ 863 (2018) L10)

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GRBs
• 107 GRBs observed since2005 (not all analysed)– 25 with delay <100 s– out of which 16 stereo– out of which 5 known z <1.5

• Fastest: 24 s of 160821B,
whose z known to be 0.16
(closest in MAGIC GRBs)– the second fastest is 26 s,
but z = 1.3 (131030A)– the second closest z = 0.37 is160623A, but delay ~7e4 s• 3 more <100 s && z<1.5– z = 1.16 (130701A)– z = 1.32 (141220A)– z = 0.42 (190114C!)

Delay vs. Zenith angle (as of Jan 2018)
known zdistribution(as of Jan 2018)

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GRB 160821B• Triggered by Swift-BAT
T90 ~0.5 s Short GRB• Swift-XRT:t < 300 s extended emission +steep decay, t < 30 ks plateau?

• MAGIC covered this period
24 s - 4 hr (14.4 ks)– Bright moon, adverse weather– >4 (pre-trial), 3.1 sigma (post-trial)
hint of detection in >600-800 GeV– No candidate source around– No detection ~1 yr later (not steady)• No detection by Fermi-LAT.
Kilonova hint by HST (Tanvir+, in prep)
Optical: NOT, WHT (z=0.16), GTC,MASTER, UVOT. Radio: VLA, AMI
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Lightcurve and SED• MAGIC and LAT points are compatible with a relatively flat LC,
coinciding with a possible X-ray shallow decay• EBL de-absorbed intrinsic spectrum is still acceptable but hard.
• Modelling ongoing by Inoue et al.
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GRB 190114C: First IACT GRB• Long GRB with T90 = 361 s
triggered by Swift-BAT"very bright" "half 130427A"• The 3rd closest (z=0.42) inMAGIC GRBs
• Not the fastest (~50 s) but
within the prompt phase• Zenith angle from 55 deg(mostly >60 deg)
• Under moon (again!)• First clear detection of a
GRB in VHE regime– ">20 sigma in the first 20 min
ATel #12390 (and also GCN #23701)
for >300 GeV"...
– I was the on-call burst advocate, and I am analysing the data

• Big efforts ongoing. Stay tuned!

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CTA LST

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Cherenkov Telescope Array• 1451 members from 203 institutes in 31 countries• Two observatory sites (in the northern and southern hemispheres)• >100 IACTs in total, 3 sizes of telescopes• x~10 higher sensitivity, x~10 wider energy range
x~2 angular resolution

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CTA sites• North site
Observatorio delRoque de losMuchachos
La Palma Island,Canaries, Spain
2200 m a.s.l.
Same as MAGIC• South site
<10 km from theESO Paranal
Observatory inAtacama, Chile(host agreement signed)• Headquarter in Bologna, Italy (partially in Heidelberg, Germany)• Science Data Management Centre in DESY Zeuthen, Germany

21Telescopes• Large Sized Telescopes: 4 (N), 4 (S)23 m in diameter, FoV 4.3 deg,
20 GeV - >150 GeV• Medium Sized Telescopes: 15 (N), 25 (S)11.5 m in diameter, FoV 7.5-7.7 deg,
<150 GeV - >5 TeV• Small Sized Telescopes: 0 (N), 70 (S)covered by Akira
4.0-4.2 m, FoV 8.3 - 10.5 deg,
<5 TeV - 300 TeV
North site in near future

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LST
23 m Φ, FoV 4.3 deg, mirror effective area 370 m2, Focal length 28 m, 0.11
deg / pixel, 1855 pixels, moving weight ~110 t, fast slewing 180 deg / 20 sec
Mechanics

OpticsFoundationIT infra.

Power infra.
CameraCalibrations

Drive23

LST Collaboration >200 people, 10 countries

24Mechanics, optics(a movie later)2018

201825

Camera assembly

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Software (Slow control, analysis,,,)Slow Control• Subsystems OPCUA tocommunicate with higher• Telescope Control Unit
to control the subsystems
and to talk to Observation
Execution System (OES),in ALMA Common Software(ACS), based on CORBAOES

DAQ, on-/off-line analyses• LST has the high data rate => 3 GB / s in total from the north site
• Significant data reduction (~1/10) required, for the fast calibration
and reconstruction, and the data transfer to outside the island

Compliant with the whole CTA array concept
We need a high computing power on site28

IT & power infra (by Japan)
Onsite datacenter forNorth site(not onlyfor LST)

Power supply
system for
the LST fastrotation
Each LST has
a special UPS

Instead of batteries, thesystem has two flywheels
to store the energy29

LST-1 construction movie

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LST1 Inauguration• 10 Oct 2018
• Press release from ICRR,U. Tokyo• Followed by news articles

Director ICRR, U. Tokyo
Prof. Takaaki Kajita
CTAO director
Prof. Federico Ferrini
Vice president U.Tokyo
Prof. Masashi Haneda
Minister of Science in Spain
Pedro DuqueLST PI
Prof. Masahiro Teshima(c) oxon

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Status after it• First shower images
in media before Xmas
– Mirrors not yet
adjusted!

• Another set of shower
images taken in Feb• Commissioning
phase until April-May• Stable operation
expected after thecomm. phase32

Expected soon from LST1
• Performance check with Crab and Mrks
– Crab Nebula, then pulsar– Mrk flares• GRBs and transients

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CTA expected physics• “Science with the Cherenkov Telescope Array” (arXiv:1709.07997)• Open Observatory – proposal driven• 9 Key Science Projects (KSPs) + DM
– Dark Matter: N 100 h / yr (dSph), S 200 h / yr (GC, etc.)– Transients: N 400 h / yr, S 400 h / yr
– Active Galactic Nuclei: N 320 h / yr (LST), S 200 h / yr
– Extragalactic survey: N 600 h, S 400 h in total– Clusters of Galaxies: N 300 h in total– Galactic Plane Survey: N 600 h, S 1000 h in total– Star Forming Systems: N 500 h, S 340 h in total– Galactic Center: S 500 h in total– Large Magellanic Cloud Survey: S 300 h in total– Cosmic Ray PeVatrons: S 300 h in total– others (CR nuclei, CR electron, optical interferometry,,,)34

Timeline• From CTA project• From LST PI– Preparations for
LST2-4 ongoing35

Summary36

Summary• MAGIC: experiencing more fruitful years than ever before– Galactic: pulsar, SNR, binaries,,,– Extragalactic: variable nearby AGN, distant AGN,,,– Fundamental physics: DM, tau neutrinos,,,– Transients: neutrino blazar, GRB,,,• CTA LST: soon to come with a better performance– CTA in a good shape as a project– LST1: commissioning going on– LST2-4: construction will start in 1-2 years– north site: MSTs will follow– south site: host agreement signed. Plans to start infrastructuredevelopment are ongoing37

Backups

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Galactic: SNR HESS J1912

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