AGIS Project(Advanced Gamma-ray Imaging System)
Hiro Tajima on behalf of AGIS collaboration
SLAC National Accelerator Laboratory
Kavli Institute for Particle Astrophysics and Cosmology
Outline❖ Project concepts❖ Science drivers❖ Technology development❖ Summary and Prospects
January 9, 2010
CTA Japan Workshop
ICRR, Japan

Current/Past Gamma-Ray Telescopes❖ MeV region (Compton, photo absorption)✤ INTEGRAL, Swift? (not really MeV instrument)✤ COMPTEL✦ State of art “ACT” in study, however, no clear future path
✦ SGD (sub-MeV) onboard JAXA ASTRO-H to be launched in 2014

❖ GeV region (pair conversion)✤ EGRET, AGILE✤ Fermi (GLAST)✦ ~ $700M/mission, state of art instrumentation✦ Constraints on volume, mass and power❖ TeV region (air shower)✤ HESS, CANGAROO, MAGIC, VERITAS✦ ~$15M/site (2–4 telescopes)✦ Room for technology development✤ Milagro (large FOV, limited sensitivity)
AGIS Project
CTA Japan Workshop, JAN 9, 2010, ICRR. Japan

2 /26

Future TeV Gamma-Ray Telescopes❖ HAWC✤ Larger active area and better background rejection by
rearrangement of PMTs
✦ Lessons learned from Milagro✤ Further increase of effective area is not easy

❖ Future IACT (Imaging Atmospheric Cherenkov Telescope)✤ x~10 better sensitivity✤ CTA (European effort)✦ Majority of members from HESS/MAGIC + new members✦ Tends to be conservative on technology choices✦ ~150M€ (100/50M€ for southern/northern sites)✤ AGIS (US effort)✦ Open to new technologies (optics, photon detectors, ASICs)• Submit joint R&D proposals to NSF/DOE✦ Aiming $~200M level project• New technologies required to reduce cost
AGIS Project
CTA Japan Workshop, JAN 9, 2010, ICRR. Japan

3 /26

AGIS Science Drivers❖ Origin of Comic rays
✤ High-energy cut-offs in cosmic-ray accelerators in the Milky Way✤ Extragalactic sources?
✦ AGN (Active galactic nuclei) and GRB (Gamma-ray burst)✦ Extragalactic background light❖ Dark matter search❖ Dark TeV sources❖ Complementary to Fermi LAT (higher energy band)
Simulation significance H.E.S.S. (Real Exposure)

Simulation significance AGIS/CTA (Flat Exposure)

AGIS Project
CTA Japan Workshop, JAN 9, 2010, ICRR. Japan

Digel & Funk
4 /26

AGIS Project
CTA Japan Workshop, JAN 9, 2010, ICRR. Japan

5 /26

Institutions:
Adler
ANL
BarnardDelaware
IAFE
INAF (Brera)
Iowa StateLANL
McGillMSFC
Penn State
Pittsb. State
PurdueAGIS Project
CTA Japan Workshop, JAN 9, 2010, ICRR. Japan

5 /26

Institutions:
Adler
ANL
BarnardDelaware
IAFE
INAF (Brera)
Iowa StateLANL
McGillMSFC
Penn State
Pittsb. State
PurdueSAO
Stanford/SLAC
UNAM
UCLA
UCSC
U. Chicago
U. Iowa
U. Utah
Yale U.
Washington U.

AGIS Project
CTA Japan Workshop, JAN 9, 2010, ICRR. Japan

5 /26

Institutions:
Adler
ANL
BarnardDelaware
IAFE
INAF (Brera)
Iowa StateLANL
McGillMSFC
Penn State
Pittsb. State
PurdueSAO
Stanford/SLAC
UNAM
UCLA
UCSC
U. Chicago
U. Iowa
U. Utah
Yale U.
Washington U.

15 US University groups
4 National Labs
4 International groups

AGIS Project
CTA Japan Workshop, JAN 9, 2010, ICRR. Japan

5 /26

Institutions:
Adler
ANL
BarnardDelaware
IAFE
INAF (Brera)
Iowa StateLANL
McGillMSFC
Penn State
Pittsb. State
PurdueSAO
Stanford/SLAC
UNAM
UCLA
UCSC
U. Chicago
U. Iowa
U. Utah
Yale U.
Washington U.

15 US University groups
4 National Labs
4 International groups

AGIS Project
CTA Japan Workshop, JAN 9, 2010, ICRR. Japan

Executive Committee:
J. Buckley
S. Funk
H. Krawzcynski
F. Krennrich (SP)V. Vassiliev
5 /26

IACT Technique

1968

Image analysis yields:
 Shower direction
 Primary energy
 background rejection
Whipple: Weekes et al. 1989, ApJ, 342, 379

AGIS Project
CTA Japan Workshop, JAN 9, 2010, ICRR. Japan

6 /26

IACT Technique

1968

Whipple: Weekes et al. 1989, ApJ, 342, 379

AGIS Project
CTA Japan Workshop, JAN 9, 2010, ICRR. Japan

6 /26

IACT Technique

1968

Stereo image analysis improves: background rejection
 angular resolution
 geometry over-constrained
Whipple: Weekes et al. 1989, ApJ, 342, 379

AGIS Project
CTA Japan Workshop, JAN 9, 2010, ICRR. Japan

6 /26

AGIS Instrument Concept❖ Improve sensitivity by a factor of ~10 in 0.1–10 TeV✤ 4 telescope → 36 telescope array✤ Wide FOV (3–5° → 8°), large telescope spacing❖ High resolution imaging (0.1° → 0.05°)✤ Sharper image✤ Better BG rejection✤ Better sensitivity❖ Similar improvement in # ofsources like EGRET ➡ Fermi (GLAST)❖ 220 M$ project(includes construction,
operation for 10 years)✤ Large collaboration(> 20 institutes)
supporting AGIS

AGIS

AGIS Project
CTA Japan Workshop, JAN 9, 2010, ICRR. Japan

7 /26

Large Array Concept❖ Event containment:✤ angular resolution x 3✤ background rejection x 2

Photonstatistics!

✤ collection area x 10
✤ FOV x 4

S ∝ Θ × back × area × Ω

100 m

Event containment only works for minimum
size of array, so that combination of collection
area and angular resolution are achieved!

AGIS Project
CTA Japan Workshop, JAN 9, 2010, ICRR. Japan

8 /26

Large Array Concept❖ Event containment:✤ angular resolution x 3✤ background rejection x 2

Photonstatistics!

✤ collection area x 10
✤ FOV x 4

S ∝ Θ × back × area × Ω

100 m

Event containment only works for minimum
size of array, so that combination of collection
area and angular resolution are achieved!

AGIS Project
CTA Japan Workshop, JAN 9, 2010, ICRR. Japan

8 /26

AGIS Specifications
Specification of the AGIS-36 Array

TargetTelescope Spacing

120 - 150 m

Effective Mirror Area per Tel.

100 m2

Field of View (FOV)

8 deg

Pixelation

0.05 - 0.10 deg

Effective Collection Area

1 km2

Energy Threshold

100 GeV

Angular Resolution

0.02 - 0.05 deg

AGIS Project
CTA Japan Workshop, JAN 9, 2010, ICRR. Japan

9 /26

AGIS Specifications
Specification of the AGIS-36 Array

TargetTelescope Spacing

120 - 150 m

Effective Mirror Area per Tel.

100 m2

Field of View (FOV)

8 deg

Pixelation

0.05 - 0.10 deg

Effective Collection Area

1 km2

Energy Threshold

100 GeV

Angular Resolution

0.02 - 0.05 deg

Key attributes of AGIS
AGIS Project
CTA Japan Workshop, JAN 9, 2010, ICRR. Japan

9 /26

AGIS Telescope Concept❖ AGIS Element:✤ Schwarzschild-Couder optics✦ Secondary optics✦ Short F/D✦ Compact✦ High resolution✦ Wide FOV

Pixelation

0.28o

0.20o

0.07o

FOV

3.5 deg.

8 deg.

ActualSize

DC optics

SC optics

AGIS Project
CTA Japan Workshop, JAN 9, 2010, ICRR. Japan

10 /26

AGIS Telescope Concept❖ AGIS Element:✤ Schwarzschild-Couder optics✦ Secondary optics✦ Short F/D✦ Compact✦ High resolution✦ Wide FOV

Pixelation

0.28o

0.20o

0.07o

FOV

3.5 deg.

8 deg.

ActualSize

DC optics

SC optics

AGIS Project
CTA Japan Workshop, JAN 9, 2010, ICRR. Japan

10 /26

Science Drivers
Black hole/Jet
connection

Hadrons

Jets - fromCollapse

TeV Sky as of 2009

Fermi + TeV sky

Jets - Binary

Dark Matter
TeV bright

Starburst Hadrons

…?

…?
EBL

AGIS Project
CTA Japan Workshop, JAN 9, 2010, ICRR. Japan

11 /26

Galactic Cosmic Accelerators❖ AGIS will provide precision measurements:✤ detect 200 - 300 SNRs (population studies)✤ image with arcmin resolution: radio - X-ray - TeV (hadrons?)✤ spectroscopy: 30 GeV - 100 TeV (hadrons vs. leptons)✤ role of SNRs, X-ray binaries, PWNe & dark accelerators✤ resolve point sources from diffuse emission✤ discovery potential for dark matter self-annihilation

Sky survey: Angular Resolution, FoV, Sensitivity (5 mCrab in 1 year)

AGIS Project
CTA Japan Workshop, JAN 9, 2010, ICRR. Japan

12 /26

Physics: Supernova Shocks
HESS

AGIS:
Wide Field ofView Imaging

8°
HESS

AGIS
VERITAS

RXJ1713.7-3946

Vela Junior

IC443
AGIS Project
CTA Japan Workshop, JAN 9, 2010, ICRR. Japan

13 /26

Physics: Supernova Shocks
HESS

AGIS:
Wide Field ofView Imaging

8°
HESS

AGIS
VERITAS

RXJ1713.7-3946

Vela Junior

IC443
AGIS Project
CTA Japan Workshop, JAN 9, 2010, ICRR. Japan

13 /26

Physics: Supernova Shocks
HESS

AGIS:
Wide Field ofView Imaging

8°
HESS

AGIS
VERITAS

RXJ1713.7-3946

Vela Junior

IC443
AGIS Project
CTA Japan Workshop, JAN 9, 2010, ICRR. Japan

13 /26

Physics: Supernova Shocks

0.004o

0.1o

0.02o

XMM 10 keVWith current
generation IACT

With AGIS@ few TeVAGIS Project
CTA Japan Workshop, JAN 9, 2010, ICRR. Japan

14 /26

Pr

ec

is

io
n

m

ea
su
re

m
en
t

s

Physics: Supernova Shocks

0.004o

0.1o

0.02o

XMM 10 keVWith current
generation IACT

With AGIS@ few TeVAGIS Project
CTA Japan Workshop, JAN 9, 2010, ICRR. Japan

14 /26

Physics: Galaxies/AGNs❖ AGIS will:✤ detect 100ʼs of AGN✤ probe space time
& intergal. medium✤ probe SMBH - Jet connection✤ e, p, n in relativistic jet✤ always > 1 γ-ray AGN in FOV✤ flux variability on ~ 1 sec.

8o
VERITAS: Acciari et al.
2009, ApJL, 684, L73❖
AGIS:
Effective
Area

HESS: Aharonian et al., arXiv:0706.0797v2 (2007))AGN (z=0.004 - 0.536)

AGIS Project
CTA Japan Workshop, JAN 9, 2010, ICRR. Japan

15 /26

Physics: Galaxies/AGNs❖ AGIS will:✤ detect 100ʼs of AGN✤ probe space time
& intergal. medium✤ probe SMBH - Jet connection✤ e, p, n in relativistic jet✤ always > 1 γ-ray AGN in FOV✤ flux variability on ~ 1 sec.

8o
VERITAS: Acciari et al.
2009, ApJL, 684, L73❖
AGIS:
Effective
Area

HESS: Aharonian et al., arXiv:0706.0797v2 (2007))AGN (z=0.004 - 0.536)

AGIS Project
CTA Japan Workshop, JAN 9, 2010, ICRR. Japan

15 /26

Physics: Galaxies/AGNs❖ AGIS will:✤ detect 100ʼs of AGN✤ probe space time
& intergal. medium✤ probe SMBH - Jet connection✤ e, p, n in relativistic jet✤ always > 1 γ-ray AGN in FOV✤ flux variability on ~ 1 sec.

8o
VERITAS: Acciari et al.
2009, ApJL, 684, L73❖
AGIS:
Effective
Area

HESS: Aharonian et al., arXiv:0706.0797v2 (2007))AGN (z=0.004 - 0.536)

AGIS Project
CTA Japan Workshop, JAN 9, 2010, ICRR. Japan

15 /26

Physics: Galaxies/AGNs❖ AGIS will:✤ detect 100ʼs of AGN✤ probe space time
& intergal. medium✤ probe SMBH - Jet connection✤ e, p, n in relativistic jet✤ always > 1 γ-ray AGN in FOV✤ flux variability on ~ 1 sec.

8o
VERITAS: Acciari et al.
2009, ApJL, 684, L73❖
AGIS:
Effective
Area

HESS: Aharonian et al., arXiv:0706.0797v2 (2007))AGN (z=0.004 - 0.536)

AGIS Project
CTA Japan Workshop, JAN 9, 2010, ICRR. Japan

15 /26

Physics: Galaxies/AGNs❖ AGIS will:✤ detect 100ʼs of AGN✤ probe space time
& intergal. medium

AGIS:
Wide Field ofView Imaging✤ probe SMBH - Jet connection✤ e, p, n in relativistic jet✤ always > 1 γ-ray AGN in FOV✤ flux variability on ~ 1 sec.

8o
VERITAS: Acciari et al.
2009, ApJL, 684, L73❖
AGIS:
Effective
Area

HESS: Aharonian et al., arXiv:0706.0797v2 (2007))AGN (z=0.004 - 0.536)

AGIS Project
CTA Japan Workshop, JAN 9, 2010, ICRR. Japan

15 /26

Physics: EBL/Cosmology❖ AGIS will:✤ probe diffuse Cosmic IR-Background with 100s of sources✤ EBL poorly understood: near - mid IR✤ TeV beam: γ + γ → e+ + e– interaction✤ measure CIRB: absorption(z)nuclearaccretion
First stars

Star/galaxy
Formation
z<5

AGNs
z<5

Pop IIIz ~ 7 - 30

Relics?

Truly diffuse
Component?

AGIS Project
CTA Japan Workshop, JAN 9, 2010, ICRR. Japan

16 /26

Physics: EBL/Cosmology❖ AGIS will:✤ probe diffuse Cosmic IR-Background with 100s of sources✤ EBL poorly understood: near - mid IR✤ TeV beam: γ + γ → e+ + e– interaction✤ measure CIRB: absorption(z)nuclearaccretion
First stars

Star/galaxy
Formation
z<5

AGNs
z<5

Pop IIIz ~ 7 - 30

Relics?

Truly diffuse
Component?

AGIS Project
CTA Japan Workshop, JAN 9, 2010, ICRR. Japan

16 /26

Physics: EBL/Cosmology❖ AGIS will:✤ probe diffuse Cosmic IR-Background with 100s of sources✤ EBL poorly understood: near - mid IR✤ TeV beam: γ + γ → e+ + e– interaction✤ measure CIRB: absorption(z)nuclearaccretion
First stars

Star/galaxy
Formation
z<5

AGNs
z<5

Pop IIIz ~ 7 - 30

Relics?

Truly diffuse
Component?

AGIS Project
CTA Japan Workshop, JAN 9, 2010, ICRR. Japan

16 /26

Physics: EBL/Cosmology❖ AGIS will:✤ probe diffuse Cosmic IR-Background with 100s of sources✤ EBL poorly understood: near - mid IR✤ TeV beam: γ + γ → e+ + e– interaction✤ measure CIRB: absorption(z)nuclearaccretion
First stars

Star/galaxy
Formation
z<5

AGNs
z<5

Pop IIIz ~ 7 - 30

Relics?

Truly diffuse
Component?

AGIS Project
CTA Japan Workshop, JAN 9, 2010, ICRR. Japan

16 /26

Physics: EBL/Cosmology❖ AGIS will:✤ probe diffuse Cosmic IR-Background with 100s of sources✤ EBL poorly understood: near - mid IR✤ TeV beam: γ + γ → e+ + e– interaction✤ measure CIRB: absorption(z)nuclearaccretion
First stars

Star/galaxy
Formation
z<5

AGNs
z<5

Pop IIIz ~ 7 - 30

Relics?

Truly diffuse
Component?

AGIS Project
CTA Japan Workshop, JAN 9, 2010, ICRR. Japan

16 /26

Physics: EBL/Cosmology❖ AGIS will:

eV

0G

10

✤ probe diffuse Cosmic IR-Background with 100s of sources✤ EBL poorly understood: near - mid IR✤ TeV beam: γ + γ → e+ + e– interaction✤ measure CIRB: absorption(z)
eV
0T

-3

nuclearaccretion
First stars

Star/galaxy
Formation
z<5

AGNs
z<5

Pop IIIz ~ 7 - 30

Relics?

Truly diffuse
Component?

AGIS Project
CTA Japan Workshop, JAN 9, 2010, ICRR. Japan

16 /26

Physics: EBL/Cosmology❖ AGIS will:

eV

0G

10

✤ probe diffuse Cosmic IR-Background with 100s of sources✤ EBL poorly understood: near - mid IR✤ TeV beam: γ + γ → e+ + e– interaction✤ measure CIRB: absorption(z)
eV
0T

-3

nuclearaccretion
First stars

Star/galaxy
Formation
z<5

AGNs
z<5

Pop IIIz ~ 7 - 30

Relics?

Truly diffuse
Component?

AGIS Project
CTA Japan Workshop, JAN 9, 2010, ICRR. Japan

16 /26

Physics: EBL/Cosmology❖ AGIS will:

eV

0G

10

✤ probe diffuse Cosmic IR-Background with 100s of sources✤ EBL poorly understood: near - mid IR✤ TeV beam: γ + γ → e+ + e– interaction✤ measure CIRB: absorption(z)nuclear

eV
0T

-3

Fermi

accretion
First stars

Star/galaxy
Formation
z<5

AGNs
z<5

Pop IIIz ~ 7 - 30

Relics?

Truly diffuse
Component?

AGIS Project
CTA Japan Workshop, JAN 9, 2010, ICRR. Japan

16 /26

Dark Matter Search❖ Detection of dark matter signal from Space iscomplementary✤ Accelerator production✦ Precise measurements of DM properties: mass, cross section✦ UED (KK) vs SUSY

✤ Direct detection✦ Good sensitivity to dark matter✦ Measurement of local dark matter density✤ Indirect detection✦ Distribution of WIMP in the Universe          dΦγ( E γ , φ, θ)
dE γ

=
×

1 < σann v >4π 2m 2W I M P∆Ω ( φ, θ)

dΩ

dN γf
Bf
dE γ

f

l os

ρ2 ( r ( l, φ )) dl( r, φ )       
AGIS Project
CTA Japan Workshop, JAN 9, 2010, ICRR. Japan

17 /26

Dark Matter Search❖ AGIS:✤ probe the annihilation cross-section✤ measure the WIMP mass
AGIS:
✤ usher the era
Effectiveof “dark matter astronomy”
Area✤ Complimentary to Fermi✦ Deeper observation of Fermi sources✦ Wider mass coverage (in VHE)

AGIS:
sensitivity

AGIS Project
CTA Japan Workshop, JAN 9, 2010, ICRR. Japan18 /26

Discovery Potential❖ Discovery of TeV γ-rays
from starburst galaxy M82✤ Probing cosmic-rays
from outside our galaxy✤ Dark Matter component
possible in SB-galaxies✤ flux ~ 9 mCrab, at thelimit of VERITAS, HESS
(139 hour exposure)❖ VERITAS/Fermi arepathfinders for AGIS:✤ sensitivity < 1 mCrab✤ probe angular extent
VERITAS: Acciari et al. 2009, submitted to Nature
AGIS Project
CTA Japan Workshop, JAN 9, 2010, ICRR. Japan19 /26

Technology Development Directions❖ Two mirror optics✤ Wide FOV ~8°✦ Better survey capability and larger collection area

✤ Reduced plate scale: ~30 cm/deg → ~3 cm/deg✤ Shorter focus arms: fast slew (or less cost)❖ Large number (~50) of telescopes and camera✤ Reliability of components✤ Modular design: easy to replace and maintain✤ Low power✤ Cost reduction✦ Currently $~1M each for telescope and camera✦ Optimization of mirror size, FOV, # of telescopes• Depends on component cost

✤ More efficient trigger to reduce dead time

AGIS Project
CTA Japan Workshop, JAN 9, 2010, ICRR. Japan

20 /26

Optics Design❖ Two-mirror system required for wide FOV and/or small plate
scale

2RMS < 3ʼ over full 15 deg FoV can be achieved(V. Vassiliev, S. Fegan, astro-ph/0612718)
AGIS Project
CTA Japan Workshop, JAN 9, 2010, ICRR. Japan

21 /26

Telescope Design❖ Low cost design for telescope structure(V. Guarino, ANL)

(J. Buckley, WashU)
AGIS Project

CTA Japan Workshop, JAN 9, 2010, ICRR. Japan

22 /26

Camera Design Concept❖ Modular camera design✤ Divided into subfields✦ Logical unit for trigger generation, easy maintenance

AGIS Project
CTA Japan Workshop, JAN 9, 2010, ICRR. Japan23 /26

Front-End Electronics R&D❖ Requirements✤ Cost reduction✦ large # of pixels: 2–4k → 500k
• More telescope, wider FOV, smaller pixels✦ Current cost: $1,500 per channel with PMT✦ Target cost: $15 per channel with multi-anode PMT✤ Reliability❖ Development of custom waveform sampling ASIC, TARGET✤ 4098 samples / channel (4 µs look-back time)✤ 9 bit dynamic range✤ 16 µs readout time (dead time less option)✤ Estimated cost: ~$10 per channel✦ 16 channel per ASIC
✦ Partial ADC implemented in ASIC

✤ 2nd generation in planning✦ 16 µs look-back, shorter dead time (~5 µs)
AGIS Project
CTA Japan Workshop, JAN 9, 2010, ICRR. Japan24 /26

Cherenkov Camera Development❖ Cherenkov camera with large # of pixel✤ Wide FOV (field-of-view)✤ Better angular resolution✤ 0.5~1k ch/camera ➱ ~10k (x ~100 telescopes)✦ Target cost: $15/channel (VERITAS: $1500/channel)✤ Other requirements:✦ Fast timing: ~ ns
✦ Readout time: less than 50 µs (trigger rate < 3-5 kHz)❖ Low cost, high Q.E. photon detector❖ Low cost, low power multi-ch readout ASIC
fiber output
MAPMT
or SiPMFPGAASIC

AGIS Project
CTA Japan Workshop, JAN 9, 2010, ICRR. Japan

25 /26

Summary and Prospects❖ AGIS aims to achieve x10 better sensitivities than current
instruments by✤ Larger collection area (wide FOV, large telescope spacing)✤ Better angular resolution❖ Technology development✤ SC optics✤ More reliable, less expensive camera electronics✤ Array trigger❖ Prospects✤ AIGS received favorable review by PASAG (DOE/NSF)✦ Recommendation for funding for most funding options✦ Under assumption of merger with CTA✤ Under review by Decadal Survey✦ Results in September

AGIS Project
CTA Japan Workshop, JAN 9, 2010, ICRR. Japan

26 /26

backup slides

AGIS Project
CTA Japan Workshop, JAN 9, 2010, ICRR. Japan27 /26

Why SLAC?
❖ Strong gamma-ray community from Fermi-LAT❖ Could play role of a lead national lab in AGIS
✤ VERITAS (current US IACT) consists of mostly universities✤ Can benefit from strong involvement of national laboratory to
carry out much larger project (if DOE funds AGIS)✤ Collaborative efforts with ANL❖ Scope of SLAC involvement✤ Development of AGIS camera electronics✤ Development of DAQ✦ Could be challenging if no level-3 trigger✤ Optimization of array configuration via simulation studies❖ Status of project✤ Currently under review by PASAG and Astro2010✤ At that time it could be endorsed by NSF + DOE✤ Aiming to start operation before Fermi LAT cease to operate
AGIS Project
CTA Japan Workshop, JAN 9, 2010, ICRR. Japan28 /26

Gamma-ray Detectors
Satellite based
pair conversion

Air showerarray

Air Cherenkov
telescope

Experiments

EGRET, GLAST

Milagro, HAWC

HESS, VERITASCANGAROO, MAGIC

Energy range

0.02 – 200 GeV

1 – 100 TeV

0.1 – 100 TeV

Angular res.

0.04 – 10 deg~0.5 deg~0.1 deg

Collection area

1 m2

103 – 104 m2

105 m2

Field of view

2.4 sr2 sr

10-2 sr

Duty cycle

~95%

>90%

<10%

γ

e+

e–

AGIS Project
CTA Japan Workshop, JAN 9, 2010, ICRR. Japan

29 /26

Camera Electronics Overview❖ Camera electronics consists of✤ Camera modules: ~200/camera (~13k pixels)✦ Waveform sampling and digitization, 16 triggers✤ Subfield boards: ~10/camera (~36 modules/field)✦ Cross-link trigger information✦ Subfield trigger✤ Main board
16-ch TARGET ASIC
64-ch
MAPMT

16-ch TARGET ASIC
FPGA
16-ch TARGET ASIC
16-ch TARGET ASIC••••••••✦ Camera
trigger✦ Gb ethernet
link tooutside (orany other
commercial
solution

Subfield board

16-ch TARGET ASIC
64-ch
MAPMT

16-ch TARGET ASIC

Main board

FPGA
16-ch TARGET ASIC
16-ch TARGET ASIC

Camera module

Subfield board
Subfield board
Subfield board
Subfield board
Subfield board

Storage

AGIS Project
CTA Japan Workshop, JAN 9, 2010, ICRR. Japan

30 /26

Camera Front-end Electronics❖ Board configuration✤ Adapter board✤ ASIC board✤ FPGA board: FPGA, data link connector✤ Power supply board: DC/DC converter, HV supply                                      

  
  


 


AGIS Project
CTA Japan Workshop, JAN 9, 2010, ICRR. Japan

31 /26