[PPT] - Status of the Silicon Photomultiplier Telescope FAMOUS for the PowerPoint Presentation

SLIDE 1

Status of the Silicon Photomultiplier Telescope FAMOUS for the Detection of UHECR

Tim Niggemann

III. Physikalisches Institut A, RWTH Aachen University

January 24, 2013 HAP Workshop Topic 4, Advanced Technologies, Karlsruhe

SLIDE 2

Outline

1. Introduction
2. Silicon Photomultipliers
3. Baseline Design of FAMOUS
4. Night-Sky Measurements with FAMOUSONE
5. Current Status of FAMOUSSEVEN
6. Summary & Outlook

Tim Niggemann (RWTH Aachen) | Status of the SiPM Telescope FAMOUS | 2

SLIDE 3

Who is FAMOUS?

◮ Lisbon

Pedro Assis, Pedro Brogueira, Miguel Ferreira, Luís Mendes, Mário Pimenta

◮ Granada

Antonio Bueno, Sergio Navas, Angel Ruiz

◮ Aachen

Franz Adamczyk, Michael Eichler, Josef Grooten, Thomas Hebbeker, Tobias Kowalew, Markus Lauscher, Lukas Middendorf, Tim Niggemann, Christine Peters, Barthel Philipps, Johannes Schumacher, Maurice Stephan, Franz-Peter Zantis (Senior Researcher, Junior Researcher, Technician)

Tim Niggemann (RWTH Aachen) | Status of the SiPM Telescope FAMOUS | 3

SLIDE 4

What do we want to measure?

Shower Images by F . Schmidt Tim Niggemann (RWTH Aachen) | Status of the SiPM Telescope FAMOUS | 4

SLIDE 5

Fluorescence Detection of High-Energy-Cosmic Rays

·

Rp shower axis telescope

Earth's atmosphere primary particle: proton, iron, etc.

avalanche of secondary particles UV-light ground Xmax

Fluorescence Light Spectrum

300 350 400 450 wavelength λ / nm 0.00 0.05 0.10 0.15 0.20 0.25 0.30 fraction

◮ Secondary particles excite nitrogen → emittance of fluorescence light ◮ Gain information on the primary particle (origin, energy, even chemical

composition?)

Tim Niggemann (RWTH Aachen) | Status of the SiPM Telescope FAMOUS | 5

SLIDE 6

Silicon Photomultipliers

◮ Light detectors with single photon detection capability ◮ Made up of cells (100, 3600, 14400, ...) ◮ Small form factor (1 × 1 mm2, 3 × 3 mm2, 6 × 6 mm2, ...) ◮ Promise high photon detection efficiency > 40 % ◮ Dark noise rate ≈ 10 kHz/cell

N u m b e r

f

d e t e c t e d p h

t
n

s 3 c e l l s f i r e d 1 c e l l f i r e d Time 1 p.e. 2 p.e. 3 p.e. Oscilloscope Reading

Tim Niggemann (RWTH Aachen) | Status of the SiPM Telescope FAMOUS | 6

SLIDE 7

Photon Detection Efficiency of SiPMs

SiPM prototype (MEPhI 100B)

350 400 450 500 550 600 650 700 750 800 10 20 30 40 50 60 70 PDE, % Wavelength λ, nm

MEPHI XP2020 (error=17%) for U=38V (∆U=4,7V) Musienko (same type SiPMsample with U=37.5V)

E. Popova, NDIP 2011

Very high PDE in UV regime up to 60 % Not yet commercially available! Hamamatsu S10985-100C

◮ 3600 cells ◮ PDE in UV

regime ≈ 25 % − 36 %

◮ Extensively

studied in

ur

laboratories

◮ Used for

FAMOUS

◮ Typical PDE of photomultiplier tubes used in fluorescence detection telescopes

≈ 27 %, ≈ 35 % (optimized in Wuppertal)

Tim Niggemann (RWTH Aachen) | Status of the SiPM Telescope FAMOUS | 7

SLIDE 8

Baseline Design of FAMOUS

◮ Modular & simple refractive

design

◮ 64 hexagonally arranged pixels ◮ 1.5°field of view per pixel ◮ 12°total field of view ◮ Fresnel lens with

f = D = 510 mm

◮ Pixel = Light funnel + four

3 × 3 mm2 SiPMs (Hamamatsu S10985-100C)

◮ Transmission efficiency of the Fresnel lens ≈ 80 % ◮ Transmission efficiency of the system w/o SiPMs ≈ 80 % · 69 % = 55 %

Tim Niggemann (RWTH Aachen) | Status of the SiPM Telescope FAMOUS | 8

SLIDE 9

Light Funnel: Winston Cone

◮ Entrance radius r1 = 6.7 mm ◮ Exit radius r2 = 3 mm ◮ Maximum allowed incidence angle

θmax = 27 °

◮ Polished aluminum (reflectivity

studied in Aachen)

◮ Successful production in Aachen

& Lisbon

r2 r1

5 10 15 20 25 30 35 incidence angle θin / ◦ 20 40 60 80 100 transmission efficiency / % r1 =3 mm, r2 =6.7 mm, θmax =27 ◦ Round entrance Hexagonal entrance Rectangular entrance

Tim Niggemann (RWTH Aachen) | Status of the SiPM Telescope FAMOUS | 9

Simulation

SLIDE 10

Readout Electronics

◮ Readout electronics developed by ◮ Based on MAROC3 chip ◮ 64 channels with two discriminators

each

◮ ADCs for charge digitization ◮ Individiual bias voltage control for

each of the 64 SiPMs

◮ FPGA for digital signal processing

including triggers

◮ Electronics currently beeing tested

and development of firmware started

Tim Niggemann (RWTH Aachen) | Status of the SiPM Telescope FAMOUS | 10

SLIDE 11

Full Detector Simulation

◮ CONEX air shower simulation ◮ Geant4 for raytracing and response simulation ◮ G4SiPM: dedicated SiPM simulation developed by

ur Auger & CMS groups in Aachen

60 40 20 20 40 60 position x / mm 60 40 20 20 40 60 position y / mm 3.0 3.2 3.4 3.6 3.8 4.0 4.2 4.4 4.6 mean arrival time / /s

vertical E = 1018 eV shower, 4 km distance

2500 3000 3500 4000 4500 5000 time t / ns 3500 3000 2500 2000 1500 1000 500 500 voltage V / mV

Pixel 34

2500 3000 3500 4000 4500 5000 time t / ns 700 600 500 400 300 200 100 100 voltage V / mV

Pixel 0

Tim Niggemann (RWTH Aachen) | Status of the SiPM Telescope FAMOUS | 11

SLIDE 12

FAMOUSONE Setup

◮ Measure night-sky brightness ◮ Commercial Newton reflector (D = 20 cm, f/4) with one single FAMOUS pixel

Tim Niggemann (RWTH Aachen) | Status of the SiPM Telescope FAMOUS | 12

SLIDE 13

Sky Scan with FAMOUSONE

◮ Sky scan around Vega ◮ Field of view of a single measurement αfov = (0.71 ± 0.02) °

l i g h t f l u x / a . u .

RA / dec DEC / deg

40 38 36 278 280 282

1 2 3 4 ... 10 11 ... 19 ... . . . background star-light of Vega star tracking stopped preliminary

◮ Night-sky background radiance (after UV pass filter) between L 60 m−2ns−1sr−1

(moonless) and L 450 m−2ns−1sr−1 (full moon) in Aachen

Tim Niggemann (RWTH Aachen) | Status of the SiPM Telescope FAMOUS | 13

SLIDE 14

FAMOUSSEVEN

◮ Final baseline

design of FAMOUS but with 7 pixels to test construction

◮ Modular design

easily extendable to 64 pixels

◮ Made in Aachen’s

mechanical facility

◮ Mechanical design

for 7 pixels fully constructed

Tim Niggemann (RWTH Aachen) | Status of the SiPM Telescope FAMOUS | 14

SLIDE 15

FAMOUSSEVEN Readout Electronics

◮ Amplifiers are attached perpendicularly to the SiPM

breadboard

◮ Each of the four signals of the SiPM 2 × 2 array is

processed separately

◮ Data acquisition and digitization with common NIM / VME

hardware

SiPM Amplifier

NIM Bias control unit

Tim Niggemann (RWTH Aachen) | Status of the SiPM Telescope FAMOUS | 15

SLIDE 16

First Darknoise Measurements

Oscilloscope Reading

◮ 1, 2 & 3 photon equivalent pulses clearly visible ◮ Baseline noise smaller than 1 p.e. pulse ◮ Dynamic range currently limited by amplifiers to 500 p.e.

Tim Niggemann (RWTH Aachen) | Status of the SiPM Telescope FAMOUS | 16

SLIDE 17

First Darknoise Measurements

Oscilloscope Reading

◮ 1, 2 & 3 photon equivalent pulses clearly visible ◮ Baseline noise smaller than 1 p.e. pulse ◮ Dynamic range currently limited by amplifiers to 500 p.e.

Tim Niggemann (RWTH Aachen) | Status of the SiPM Telescope FAMOUS | 16

SLIDE 18

First Light Measurements

◮ Charge Spectrum of a measurement with a pulsed UV LED 400 600 800 1000 1200 1400 1600 QDC channel 200 400 600 800 1000 entries / channel QDC measurement Famous pixel ◮ QDC spectra with single photon resolution possible

Tim Niggemann (RWTH Aachen) | Status of the SiPM Telescope FAMOUS | 17

SLIDE 19

Summary

◮ FAMOUS = small fluorescence telescope prototype with silicon photomultipliers ◮ Simple refractive telescope, up to 64 pixels ◮ Full detector simulation to evaluate performance ◮ Dedicated and cross-checked SiPM simulation G4SiPM (journal paper & public

release in preparation)

◮ Telescope with seven pixels fully assembled ◮ Electronics for upgrade to 64 pixels currently being programed

Outlook

◮ Star tracking with FAMOUSSEVEN ◮ DAQ interface for FAMOUS (Bachelor thesis starting in April) ◮ Flat-fielding and focus check of FAMOUSSEVEN (Master thesis in progress) ◮ Study designs and applications beyond FAMOUS (Master thesis in progress) ◮ Upgrade to 64 pixels

Tim Niggemann (RWTH Aachen) | Status of the SiPM Telescope FAMOUS | 18

SLIDE 20

Backup

SLIDE 21

Exit Angles of the Winston Cone

/ deg

ut

q emergent angle

10 20 30 40 50 60 70 80 90

fraction entries / total count

0.02 0.04 0.06 0.08 0.1 0.12 0.14 0.16 0.18 0.2 0.22

° = 0

in

q incident angle ° = 26

in

q incident angle = 6.7 mm

1

r = 3.0 mm

2

r

Tim Niggemann (RWTH Aachen) | Status of the SiPM Telescope FAMOUS | 20

SLIDE 22

Transmission Efficiency of PMMA

/ nm l wavelength

200 300 400 500 600 700 800 900 1000

transmission T / %

10 20 30 40 50 60 70 80 90 100

reflexite.com = 3 mm

thick

d

Tim Niggemann (RWTH Aachen) | Status of the SiPM Telescope FAMOUS | 21

SLIDE 23

Aberration Radius R90 of the Fresnel Lens

lens - focal plane distance z / mm

500 505 510 515 520 525 530 535 540 545 550

/ mm

90

aberration radius R

1 2 3 4 5 6 7 8

° = 0

in

q ° = 2

in

q ° = 3

in

q ° = 4

in

q ° = 5

in

q ° = 6

in

q ° = 1

in

q 2 grooves / mm

Tim Niggemann (RWTH Aachen) | Status of the SiPM Telescope FAMOUS | 22

SLIDE 24

Trigger Efficiency of FAMOUS

15 16 17 18 19 shower energy log10(E/eV) 2 4 6 8 10 12 shower-telescope distance Rp / km 10 20 30 40 50 60 70 80 90 100 trigger probability / %

Tim Niggemann (RWTH Aachen) | Status of the SiPM Telescope FAMOUS | 23

SLIDE 25

PDE of a pixel of FAMOUS (Winston cone + Hamamatsu S10985-100C SiPM)

5 10 15 20 25 incident angle θin / ◦ 10-2 10-1 100 101 102 103 light flux φ / ns−1 0.025 0.050 0.075 0.100 0.125 0.150 0.175 0.200 0.225 detection efficiency

Tim Niggemann (RWTH Aachen) | Status of the SiPM Telescope FAMOUS | 24

SLIDE 26

Geiger-mode Avalanche Photodiode

n substrate n- epitaxial layer n+ p+ p++ 0.5 μm 2-4 μm 300 μm electrons holes anode cathode

Tim Niggemann (RWTH Aachen) | Status of the SiPM Telescope FAMOUS | 25

SLIDE 27

Photon Detection Efficiency of the Hamamatsu S10362-11-100C

350 400 450 500 550 600 wavelength λ / nm 20 25 30 35 40 photon detection efficiency / % Hamamatsu S10362-11-100C VOV =1.3 V

A. Tadday, 2009
M. Lauscher, 2012

Tim Niggemann (RWTH Aachen) | Status of the SiPM Telescope FAMOUS | 26

SLIDE 28

Overvoltage Dependency of the Hamamatsu S10362-11-100C

0.8 1.0 1.2 1.4 1.6 1.8 10 20 30 40 50 60 PDE / % λ =400 nm 0.8 1.0 1.2 1.4 1.6 1.8 0.4 0.5 0.6 0.7 0.8 0.9 1.0 1.1 1.2 thermal noise rate / MHz 0.8 1.0 1.2 1.4 1.6 1.8

ver-voltage VOV / V

10 20 30 40 50 60 after-pulse prob. / % 0.8 1.0 1.2 1.4 1.6 1.8

ver-voltage VOV / V

10 20 30 40 50 60 cross-talk prob. / %

Tim Niggemann (RWTH Aachen) | Status of the SiPM Telescope FAMOUS | 27

SLIDE 29

UG-11 Transmission

Wavelength [nm] 200 300 400 500 600 700 800 900 1000 1100 Transmittance 0.1 0.2 0.3 0.4 0.5 0.6 0.7 0.8 0.9

M-UG 6 UG 11

Wavelength [nm] 200 300 400 500 600 700 800 900 1000 1100 Transmittance 0.1 0.2 0.3 0.4 0.5 0.6 0.7 0.8 0.9

M-UG 6 UG 11

Wavelength [nm] 200 300 400 500 600 700 800 900 1000 1100 Transmittance 0.1 0.2 0.3 0.4 0.5 0.6 0.7 0.8 0.9

M-UG 6 UG 11

Tim Niggemann (RWTH Aachen) | Status of the SiPM Telescope FAMOUS | 28