CF2 Instrumentation Jim Buckley for the CF2 working group M. - - PowerPoint PPT Presentation

CF2 Instrumentation

Jim Buckley

for the CF2 working group

• M. Cahill-Rowley, R. Cotta, A. Drlica-Wagner, S. Funk, J. Hewett, A.

Ismail, T. Rizzo and M. Wood (SLAC and Irvine Particle Theory groups)

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Snowmass 2013 CF2: Indirect Detection James Buckley

Direct and Indirect Detection

• Scientific complementarity
• Technical complementarity

[hep-ph] arXiv:1011.4514 L. Bergstrom et al.

Proposed CTA SC camera module with 25 2” MAPMTs Xenon100 Detector

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Snowmass 2013 CF2: Indirect Detection James Buckley

CF2 Experiments

Table 1-1. Current and planned indirect detection experiments.

Status Experiment Target Location Major Support Comments Current AMS e+/e−, anti-nuclei ISS NASA Magnet Spectrome- ter, Running Fermi Photons, e+/e− Satellite NASA, DOE Pair Telescope and Calorimeter, Run- ning HESS Photons, e− Namibia German BMBF, Max Planck Society, French Ministry for Research, CNRS- IN2P3, UK PPARC, South Africa Atmospheric Cherenkov Telescope (ACT), Running IceCube/ DeepCore Neutrinos Antarctica NSF, DOE, International *Belgium, Germany, Japan, Sweden) Ice Cherenkov, Running MAGIC Photons, e+/e− La Palma German BMBF and MPG, INFN, WSwiss SNF, Spanish MICINN, CPAN, Bulgarian NSF, Academy of Finland, DFG, Polish MNiSzW ACT, Running PAMELA e+/e− Satellite VERITAS Photons, e+/e− Arizona, USA DOE, NSF, SAO ACT, Running Planned CALET e+/e− ISS Japan JAXA, Italy ASI, NASA Calorimeter CTA Photons ground- based (TBD)

International (MinCyT, CNEA, CONICET, CNRS-INSU, CNRS-IN2P3, Irfu-CEA, ANR, MPI, BMBF, DESY, Helmholtz Association, MIUR, NOVA, NWO, Poland, MICINN, CDTI, CPAN, Swedish Research Council, Royal Swedish Academy of Sciences, SNSF, Durham UK, NSF, DOE

ACT GAMMA- 400 Photons Satellite Russian Space Agency, Russian Academy of Sciences, INFN Pair Telescope GAPS Anti- deuterons Balloon (LDB) NASA, JAXA TOF, X-ray and Pion detection HAWC Photons, e+/e− Sierra Ne- gra NSF/DOE Water Cherenkov, Air Shower Surface Array PINGU Neutrinos Antarctica NSF Ice Cherenkov

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Snowmass 2013 CF2: Indirect Detection James Buckley

Indirect Detection

Fermi VERITAS Super K AMS PAMELA Super-K ICECUBE

γ ν

e−, e+, p, ¯ p

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Snowmass 2013 CF2: Indirect Detection James Buckley

Gamma-Ray Detection

• Both space-based and ground-based instruments use electromagnetic calorimeters,

but for ground-based instruments the earth’s atmosphere is basically a continuous 27 rad. length total absorption calorimeter, viewed with an array of telescopes.

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Snowmass 2013 CF2: Indirect Detection James Buckley

VERITAS Array

• First Light in April 2007

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Snowmass 2013 CF2: Indirect Detection James Buckley

VERITAS Array

• First Light in April 2007
• 10 mCrab sensitivity - 5σ detection at 1%

Crab (2x10-13 erg cm-2 s-1 @ 1 TeV) in 28 hrs.

• Effective area 105 m2 above 500 GeV
• Angular resolution <0.1 deg
• Energy range 150 GeV - 30 TeV, 15%

resolution (for spectral measurements)

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Snowmass 2013 CF2: Indirect Detection James Buckley

VERITAS Array

• First Light in April 2007
• 10 mCrab sensitivity - 5σ detection at 1%

Crab (2x10-13 erg cm-2 s-1 @ 1 TeV) in 28 hrs.

• Effective area 105 m2 above 500 GeV
• Angular resolution <0.1 deg
• Energy range 150 GeV - 30 TeV, 15%

resolution (for spectral measurements)

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Snowmass 2013 CF2: Indirect Detection James Buckley

VERITAS Array

• First Light in April 2007
• 10 mCrab sensitivity - 5σ detection at 1%

Crab (2x10-13 erg cm-2 s-1 @ 1 TeV) in 28 hrs.

• Effective area 105 m2 above 500 GeV
• Angular resolution <0.1 deg
• Energy range 150 GeV - 30 TeV, 15%

resolution (for spectral measurements)

γ γ γ γ γ γ

Snowmass 2013 CF2: Indirect Detection James Buckley

VERITAS Array

• First Light in April 2007
• 10 mCrab sensitivity - 5σ detection at 1%

Crab (2x10-13 erg cm-2 s-1 @ 1 TeV) in 28 hrs.

• Effective area 105 m2 above 500 GeV
• Angular resolution <0.1 deg
• Energy range 150 GeV - 30 TeV, 15%

resolution (for spectral measurements)

γ γ γ γ γ γ

Snowmass 2013 CF2: Indirect Detection James Buckley

VERITAS Array

• First Light in April 2007
• 10 mCrab sensitivity - 5σ detection at 1%

Crab (2x10-13 erg cm-2 s-1 @ 1 TeV) in 28 hrs.

• Effective area 105 m2 above 500 GeV
• Angular resolution <0.1 deg
• Energy range 150 GeV - 30 TeV, 15%

resolution (for spectral measurements)

γ γ γ γ γ γ

Snowmass 2013 CF2: Indirect Detection James Buckley

VERITAS Array

• First Light in April 2007
• 10 mCrab sensitivity - 5σ detection at 1%

Crab (2x10-13 erg cm-2 s-1 @ 1 TeV) in 28 hrs.

• Effective area 105 m2 above 500 GeV
• Angular resolution <0.1 deg
• Energy range 150 GeV - 30 TeV, 15%

resolution (for spectral measurements)

γ γ γ γ γ γ

Snowmass 2013 CF2: Indirect Detection James Buckley

VERITAS Array

• First Light in April 2007
• 10 mCrab sensitivity - 5σ detection at 1%

Crab (2x10-13 erg cm-2 s-1 @ 1 TeV) in 28 hrs.

• Effective area 105 m2 above 500 GeV
• Angular resolution <0.1 deg
• Energy range 150 GeV - 30 TeV, 15%

resolution (for spectral measurements)

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Snowmass 2013 CF2: Indirect Detection James Buckley

Technical Details

Stage et al. 2006

Telescope (x 4)

12-m diameter Davies-Cotton f 1.0, 110 m2 area

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Snowmass 2013 CF2: Indirect Detection James Buckley

Technical Details

Stage et al. 2006

Telescope (x 4)

12-m diameter Davies-Cotton f 1.0, 110 m2 area

Camera (x 4)

499 PMTs, 3.5o FOV

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Snowmass 2013 CF2: Indirect Detection James Buckley

Technical Details

Stage et al. 2006

Telescope (x 4)

12-m diameter Davies-Cotton f 1.0, 110 m2 area

Mirror Facets (x 350)

Reflectivity ~ 88% (Recoated every 2 years)

Camera (x 4)

499 PMTs, 3.5o FOV

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Snowmass 2013 CF2: Indirect Detection James Buckley

Technical Details

Stage et al. 2006

Telescope (x 4)

12-m diameter Davies-Cotton f 1.0, 110 m2 area

Mirror Facets (x 350)

Reflectivity ~ 88% (Recoated every 2 years)

Electronics

500 Msp FADC, CFD trigger, 3-fold adjacent pixels and 2/4 telescope coincidence

Camera (x 4)

499 PMTs, 3.5o FOV

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Snowmass 2013 CF2: Indirect Detection James Buckley

Technical Details

Stage et al. 2006

Telescope (x 4)

12-m diameter Davies-Cotton f 1.0, 110 m2 area

Mirror Facets (x 350)

Reflectivity ~ 88% (Recoated every 2 years)

Electronics

500 Msp FADC, CFD trigger, 3-fold adjacent pixels and 2/4 telescope coincidence

Camera (x 4)

499 PMTs, 3.5o FOV

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Snowmass 2013 CF2: Indirect Detection James Buckley

Gamma-Ray Instruments

(JB)

Fermi

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Snowmass 2013 CF2: Indirect Detection James Buckley

Neutrino Detection

(simulated neutrino event in ICECUBE)

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Snowmass 2013 CF2: Indirect Detection James Buckley

CTA-US

SC-MST (Dual Mirror) DC-MST (Single Mirror) Hybrid-1 (50 hr) Prod-1 Array I (50 hr) ~2-3x improvement in core energy range from US contribution Fermi (3yr)

Hybrid-1 SC-MST Hybrid-1 DC-MST 0.1° 0.03° 100 GeV 1 TeV

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Snowmass 2013 CF2: Indirect Detection James Buckley

CTA Camera

!

kley SCT Camera Status UCLA, J

• Electronics based on TARGET were

developed by SLAC and U. Hawaii

• Write Pointer

Read Pointer Outputs from

• ther Channels

L2 Triggers from

• ther

Telescopes stop ADCs Camera Subfield Pattern Trigger (L2) Timing and Read/Write Control Switched Capacitor Array Discriminator Discriminator Preamp Photodetector Signal Array Trigger (L3)

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Snowmass 2013 CF2: Indirect Detection James Buckley

Contained Events

!"#$%&'""()*%+""+,-%*#%./0

!"#$%&'(()&*+,"-.& /&0112031&4 &%5'"6+)&%7)7.6('7&.'+6"8# 9:77%&.'(%&;(* <7.%&%*"##7*"8#& +8,&*76(8.%*-6%"(8= >(.%&.$(:7*&6(*7.&4"..&"%? !+*#7&,7%76%"(8&+*7+ >(*7&"4+#7.&'7*&.$(:7* !(:7*&%*"##7*&%$*7.$(),

!

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Snowmass 2013 CF2: Indirect Detection James Buckley

Contained Events

250 m 350 m Deep Core

extra veto cap

AMANDA

IceCube

• equivalent
• vide an active veto shield

above; 3 rings of strings on all sides eater ed

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Snowmass 2013 CF2: Indirect Detection James Buckley

Positron/Antiproton Detection

• Typical instruments include:
• MS for measurement of momentum

(rigidity)

• EC for measurement of energy and

for discrimination of hadronic showers

• Redundant measurement of Lorentz

factor (e.g., RICH or TRD) for particle discrimination against large background of protons. Schematic of HEAT

e− e+

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Snowmass 2013 CF2: Indirect Detection James Buckley

Positron/Antiproton Detection

• Typical instruments include:
• MS for measurement of momentum

(rigidity)

• EC for measurement of energy and

for discrimination of hadronic showers

• Redundant measurement of Lorentz

factor (e.g., RICH or TRD) for particle discrimination against large background of protons. Schematic of HEAT

e− e+

Electron Proton (BETS-Tori, et. al.)

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Snowmass 2013 CF2: Indirect Detection James Buckley

GAPS

!"#$%&'$(&)*+',")-$$$$$$$$$$$$$$$$$$$$$$$$$!"#$%%%%%%%%%%%%%%%%%%%%%%%%%./0,"$12$3$454#

&'()*%+,,-'+./%0'-%+1234)52)-'1%34)12303.+23'1

4

0)6+77+'8$)3

! "#

&5.*)+- "113/3*+23'1

4 "+

9:8)0$)3

+2'63.%2-+17323'17

';'<=1> '&?7& ';5 ';@ ';A ';> ';1 ';B

"# ! !

C9!D$E)*),*&0

/'*+E):*)0&'$F7&GF$E&G'$/'E$F*&4F$+'$

• /*)0+/7

7/08)$,"/',)$6&0$,0)/*+&'$&6$/'$)H,+*)E$ )H&*+,$/*&-$IJK+'=JLM

E))H,+*/*+&'N ! 6/F*$+&'+F/*+&'$&6$O&:'E$)7),*0&'F$I9:8)0M "#,&-47)*)$E)47)*+&'$&6$O&:'E$)7),*0&'F ! PQE0&8)'37+K)$)H&*+,$/*&-$ I':,7):FR/'*+E):*)0&'M$ E))H,+*)F$%+/$./+-+.2)-3723.%89-+:%2-+17323'17

':,7):F3/'*+E):*)0&'$/''+"+7/*+&'N$ ,3'17%+14%,-'2'17

)H&*+,$/*&-+,$4"QF+,F$:'E)0F*&&E$ I*)F*)E$+'$<J<$BSSTUV$*)F*O)/-M

J2DDD$K+?I+A 9)*),*&07

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Snowmass 2013 CF2: Indirect Detection James Buckley

Antideuteron Measurements

• GAPs looks for anti-deuterons (hard to produce as CR secondaries), uses

TOF, X-rays from short-lived exotic atom, pion star from annihilation

J2DDD$K+?I+A 9)*),*&07 L+*"$!.M$0)/ B.?3MN>$O$=)/07 F(G>$2P2O$5/=7 QF(G>$2P1OM$5/=7

(talk by P. von Doetinchem)

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SLAC CF 2013 CF2: Indirect Detection James Buckley

Technical Developments

• Analog pipeline ASICs (K. Nishimura)

Large-Area HPMT (Masahi Yokoyama) LAPPD psec timing, 8” square photodetector, (K. Byrum) SiPMs, (N. Otte)

• <$

01$

• &-$

0@$

• $
• J"$
• /012034#"%5%,41673%89:,1%

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SLAC SSI13 Instrumentation at the CF James Buckley

CTA Photosensors

• ~8ns

10x

MAPMTs SiPMs ~1ns MAPMT Pulse SiPM Pulses (after preamp)

S11828-3344 MPPC (H8500-10x MOD8) Currently, crosstalk (~10% and pixel pitch are key concerns)

• J. Buckley SCT Camera Overview CTA, Chicago 2013

TARGET ASIC

• Target-5 ASIC Designed by U. Hawaii (Garry Varner) for SLAC

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SLAC SSI13 Instrumentation at the CF James Buckley

Quiz

• Question: (a) Which is the camera module for the gamma-ray instrument

and which is the module for the optical telescope? (b) Which is the

• ptical system for the gamma-ray telescope and for the optical telescope?
• !1

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SLAC SSI13 Instrumentation at the CF James Buckley

GaN MBE Lab

• At Washington U. we are fabricating AlGaN/InGaN photocathodes with both epitaxial and

amorphous heterostructures using a Molecular Beam Epitaxy/ Transfer system. Beginning work on solid state detectors with intrinsic gain, hybrid Silicon/GaN devices.

• Potential for High QE detection at 175nm in a very low radiation background PMT housing

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SLAC SSI13 Instrumentation at the CF James Buckley

Photocathode Devices

• Semiconductor photocathodes hold promise for improvement in QE.

Features include a reflection barrier, p-type doping profiles to bend the band, and a thin dipolar Cs-O layer to achieve negative electron affinity, and a barrier to tunneling.