Valter Bonvicini, Giulio Orzan, Gianluigi Zampa, Nicola Zampabonvicin/CASIS2/Bonvicini_SIF08.pdf ·...

Valter Bonvicini - Congresso Nazionale SIF, Genova 22-26 Settembre 2008

SviluppiSviluppi

di di elettronicaelettronica

VLSI VLSI avanzataavanzataper per calorimetriacalorimetria

al al siliciosilicio

in in fisicafisica

astroparticellareastroparticellare

Valter Bonvicini, Giulio

Orzan, Gianluigi

Zampa, Nicola ZampaINFN – Trieste

INDICE:1.

Calorimetri

Si-W per esperimenti

nello

spazio2. Sfide

future: fisica

astroparticellare

(ben) oltre

il

TeV3. Gli

esperimenti

CASIS e CASIS24. Il chip CASIS: motivazioni, obiettivi

e progetto

dell’ASIC5. Risultati

(parziali)6. Conclusioni

e prospettive


1. Si-W Calorimeters for space experiments -

1Advantages of a Si-W calorimeter:

• Silicon detectors ⇒ dE/dx measurement anddetermination of Z for minimum ionizing particles;

• Excellent linearity, stability and efficiency• Low voltage operation;• Compactness;• Low power consumption;• Maturity of the design (balloon flights WiZard

TS93, CAPRICE 94 and CAPRICE 98) and space“heritage”

(Sil-Eye, NINA, NINA 2, PAMELA);

Example:

the Si-W Imaging Calorimeterof PAMELA• 22 W plates (2.6 mm / 0.74 X0)• 44 Si layers (X-Y), 380 µm thick• Total depth: 16.3 X0 / 0.6 λI• Mass: 110 kg• Power Consumption: 48 W

Designed to meet the PAMELA physics tasks:precise measurement of the positron flux from 50 MeV

to 270 GeV

and of the antiproton flux from 80 MeV

to 190 GeV


44 Si detector views (22X and 22Y)• 8x8 cm2

detectors arranged in a3x3 matrix

• 32 strips/detector, 2.4 mm pitch

• Strips of detectors in the same row(column) are bonded together(ladder) ⇒ 24 cm long strips

• Each ladder (32 channels) is readout by 2 CR1.4P front-end chips⇒ 6 front-end chips/view

• In total:• 396 silicon detectors• 264 CR1.4P chips• 4224 channels

Architecture of one channel of the CR1.4P •Front-end

⇒ CR1.4P ASIC (full custom design)Design characteristics:-

16 channels/chip-

channel structure: CSA, shaper, T/H, out. mux.-

input-selectable calibration circuit-

integrated self-trigger circuit-

shaping time = 1 µs-

sensitivity = 5 mV/MIP-

wide dynamic range: 7.1 pC

= 1400 MIP (1 MIP = 4.9 fC)-

ENC ≈

2700 e-

rms

+ 5 e-

/pF

1. Si-W Calorimeters for space experiments -

2


PAMELA

ATIC

CREAM

Ground basedIndirect measurements

2. Future challangesScientific interest:

direct

measurement of the cosmic-ray fluxes above the TeV

region

Major concern: the dynamic range of the read-out electronics

U. Bravar, S. Stochaj, M. Boezio,V. Bonvicini and A. Vacchi, “Simulationstudy of the Si-W calorimeter forACCESS”, Astrop. Phys.19 (2003) 463-

476

It is necessary to measure signals from 0.1 MIP to 107

MIP, i.e. a dynamic range of ~ 108

An example…


CASIS

(CAlorimetria

al SIlicio

per lo Spazio)

:INFN R&D project aimed at improving the present performance of Si –

W

calorimeters (both detectors and front-end electronics) in view of future astroparticle physics experiments, where very high energy (above

1015

eV) particles are to be studied.

Development of integrated front-end electronics with

very largedynamic range for silicon detectors in calorimeter applications

3. The CASIS project

Development of silicon detectors optimised for calorimetryin presence of very large charge releases

p strips+

n strips+

hole signal

electron signal

Preamplifier 1

Preamplifier 2

Double-sided silicon strip detectors withparallel strips on p and n-sides.

“The idea is to collect the same charge oncorresponding n and p strips and to readthem out by using two different front-endcircuits, with different sensitivities,in order to increase the overall dynamicrange by covering different signal regions”.

V. Bonvicini et al., “New developments in silicon calorimetry for space experiments”, NIM A 518 (2004) 186-187


Design approach:

•

Front-end section: a double gain (double range) CSA with automatic gain control followed by a Correlated Double Sampling (CDS) filter.

•

ADC: Cyclic ADC with 12 bits of resolution, clock up to a few MHz.•

Technology:

0.35 um C35B4 CMOS from AMS (4M/2P, 3.3V supply).

Development of integrated front-end electronics with

very largedynamic range for silicon detectors in calorimeter applications

Phase1-

2006 (CASIS1.0): front-end circuit with• Range of 50 pC

(~ 104

MIP for 380 µm thick Si detectors);• ENC < 6000 e-

rms

@ Cdet

= 300 pF;• Power consumption < 3 mW/channel.Perform a feasibility test of integration of one ADC/channel

Phase2-

2007 (CASIS1.1): improved prototype, including all lessonslearned from CASIS1.0 (especially concerning the ADC)Phase3-

2008 (CASIS1.2): “Final”

16-channel complete circuit with 1 ADC/channel.

4. The CASIS chip: design and development


CASIS1.1: CSA and Correlated Double Sampling block scheme


CASIS1.1: Cyclic ADC block scheme

+

-

ADCON

CYCLE

0.5 pF

0.5 pF

0.25 pF

CYCLE

CLK3N

ADCON

0.25 pF

CYCLE ADCON

Vcm

Vcm

Vcm

CLK3N

CLK2N

SAMPLE

Vinput

CLK4

Vom

CLK2N

CLK4Vop

+

-

CLK2

CLK2

0.5 pF

0.5 pF

CLK1 ADCON

CLK1 ADCON

CLK2

CLK2

0.5 pF

0.5 pF

CLK3

SUBPOS

SUBNEG

Vref+

Vref-

CLK3

SUBNEG

SUBPOS

Vref+

Vref-

Vcm

Vcm

+

-

Vip

Vim

Vcm

CLK3

CLK3

Q

Q

CLR

CLK2

CLK2

30 fF

30 fF

CLK3

QSUBPOS

SUBNEG

SUBPOSCLK3

Q

CLK3

QSUBNEG

CLK3

Q


Input diff. amp. BiasInput diff. amp.

Output buffer CMFB amplifier

Diff. Op. Amp. Solution 1 (baseline)


Diff. Op. Amp. Solution 2 (back-up)


Micrograph of a die (chip CASIS1.1)

3.1 mm

3.1 mm

CDS ch. 1

Buffer ch. 1

CSA ch. 1CSA bias

3 “Type O”ADC

ADC control

3 “Type N”ADC

3 “Type F”ADC

The CASIS1.1

chip was designed during 2006/2007 and produced within an Europractice

MPW run in April 2007.


5. CASIS1.1 –

Front-end results -

1

100 MIP

200 MIP

300 MIP

400 MIP

From bottom to top:8000 MIP9000 MIP10000 MIP11000 MIP


Linearity_LowGain

y = 0.1456x + 921.55

0

500

1000

1500

2000

2500

3000

0 2000 4000 6000 8000 10000 12000

Input charge, MIP

Out

put v

olta

ge, m

V

Linearity_HighGain

y = 2.9393x + 933.19

0

500

1000

1500

2000

2500

3000

0 100 200 300 400 500 600

Input charge, MIP

Out

put v

olta

ge, m

V

Non-linearity_HighGain

-0.4

-0.3

-0.2

-0.1

0

0.1

0.2

0.3

0 100 200 300 400 500 600

Input charge, MIP

%Er

ror

Non-linearity_LowGain

-0.8

-0.6

-0.4

-0.2

0

0.2

0.4

0.6

0 10 20 30 40 50 60

Input charge, fC

%Er

ror

Dynamic ranges : 560 MIP

for high gain, and 11000 MIP

for low gain (or ~ 52 pC)Maximum deviation from linear fit : < 0.3%

for high gain, and 0.6%

for low gain Power consumption: 2.8 mW/channel

5. CASIS1.1 –

Front-end results -

2


•

ENC@0 pF = 2280 e-

rms

(~12.9 SNR for 1 MIP)

•

ENC@200 pF = 3800 e-

rms


•

ENC@300 pF

= 4560 e-

rms


Measured noisey = 7.5588x + 2278.7

0

1000

2000

3000

4000

5000

6000

0 50 100 150 200 250 300 350

Cd, pF

ENC

, e- r

ms

ENCLinear (ENC)

5. CASIS1.1 –

Front-end results -

3


Linearity (FE + int. ADCs) Chip 1

0255075

100125150175200

0 5 10 15 20 25 30

Input charge [MIP]

Sign

al -

ped.

[AD

C c

h.] Ch2-ADC1

Ch2-ADC2Ch2-ADC3Ch2-ADC4Ch2-ADC5Ch2-ADC6Ch2-ADC7Ch2-ADC8Ch2-ADC9

Linearity (FE + int. ADCs), Chip1

0

500

1000

15002000

2500

3000

3500

4000

0 1000 2000 3000 4000 5000 6000 7000

Input charge, MIP

ADC

chan

nels

ADC2ADC3ADC4ADC5ADC6ADC7ADC8ADC9ADC1

5. CASIS1.1 –

ADC results -

1

Avg. power consumption:N-type ~ 5.3 mWF-type ~ 8.6 mWO-type ~ 2.9 mW

• All ADC channels work!(171 ADC channels tested);

• Random device mismatchproblems which affetcted

theprevious version solved!


Chip 8 ADCN_nd Full Range

y = 2.381x - 1780.8

0500

10001500200025003000350040004500

700 1200 1700 2200

Input voltage (from DAC), mV

ADC

out

put

ADCNndLinear (ADCNnd)

Chip8_ADCN_nd_central

2020

2030

2040

2050

2060

2070

2080

2090

1598 1603 1608 1613 1618

Input voltage (from DAC), mV

ADC

out

put

ADCNnd

Full range (1.7 V) ADC response(input voltage steps ~ 400 µV)From fit: 1 bit = 420

µV (theor. 415 µV)

Chip 8 ADC_Nnd (2nd Half-Range)

-0.15

-0.1

-0.05

0

0.05

0.1

0.15

1600 1800 2000 2200 2400

Input voltage, mV

% E

rror

Linearity in each half-range within±

0.1% at 1 MHz.

5. CASIS1.1 –

ADC results -

2


6. Outlook•

The 2nd

prototype of a VLSI front-end chip (CASIS1.1) intended for the read-out of silicon

calorimeters in future astroparticle physics experiments above the TeV

region of Cosmic Rays has been designed, produced and tested in the framework of the

INFN R&D experiment CASIS2.

•

The chip features 2 channels including a

double-range CSA

(with gains ~ 3 mV/MIP and ~ 150 µV/MIP) with a

real-time network for feedback control, a

CDS filter

and an output buffer, and

9 channels with fully differential cyclic ADCs

(2 alternative designs for the Diff. Op. Amps).

•

The front-end part (CSA + CDS) fulfils all design specs. In particular,

a dynamic range of 52.2 pC

(in Low-Gain mode), an ENC = 2280 e-

+ 7.6 e-/pF, a very good linearity and a power consumption of 2.8 mW/ch

have been achieved.

•

Tests on the ADC part have shown that:

a)

100% of the channels convert correctly (171 ADC channels fast-tested at 250 kHz and 1 MHz) and display the expected power consumption ⇒

we solved the random device mismatch problems that affected the first version;

b)

Full range (1.7 V differential) operation show that the ADC resolution is close to the design one, linearity is affected by the known drawbacks of conventional restoring cyclic ADC: nevertheless, linearity is still within ±

0.1% over each half range.

•

On the basis of these results, we are currently finalising the design of two “final”

chip versions, which we plan to submit to foundry by the end of this year:

•

CASIS1.2A: “analog”

version (without ADC), 16 channels with output analog

multiplexer;•

CASIS1.2C: 16 complete channels with 1 ADC/channel (ADC modified

to include capacitor averaging and digital correction.

This work has been completely supported by INFN (CSN5)


~ Spare slides ~


PAMELA scientific objectives

• Study antiparticles in cosmic rays

• Search for antimatter

• Search for dark matter

• Study cosmic-ray propagation

• Study solar physics and solar modulation

• Study the electron spectrum (local sources?)

PAMELA design performance

energy

range

particles

in 3 years

•

Antiprotons 80 MeV

-

190 GeV

O(104)•

Positrons 50 MeV

-

270 GeV

O(105)

•

Electrons up to 400 GeV

O(106)•

Protons up to 700 GeV

O(108)•

Electrons+positrons

up to 2 TeV

(from calorimeter)

•

Light Nuclei up to 200 GeV/n

He/Be/C: O(107/4/5)

•

AntiNuclei

search sensitivity of 3x10-8

in He/He

(A Payload for Antimatter Matter Exploration and Light-nuclei Astrophysics)


Si Tracker + magnet• Measures rigidity• 5 Nd-B-Fe modules (0.43T)•

6 planes of double-sided Si microstrip

detectors•

~3 µm resolution (bending view) demonstrated, ie: MDR ≈

800GV/c

Time-of-flight•

Trigger / Albedo

rejection / Particle identification (up to 1 GeV/c) / dE/dx • 3 double-layer scintillator

paddles• Timing resolution:

• σ(paddle) ≈

110 ps• σ(ToF) ≈

330 ps

(MIPs)

Si-W Imaging Calorimeter

Anticoincidence system• Rejection of events with particles

interacting with the apparatus• Plastic scintillator

paddles• MIP efficiency > 99.9%

Neutron detector• 36 3He counters• e/h

discrimination at high energies

Shower-tail catcher (S4)• Plastic scintillator

paddle, 1 cm thick• Main task: ND trigger

The PAMELA instrumentThe PAMELA instrument

Mass: 470 kgPower: ~ 360 WSize: 130x70x70 cm3

21.5 cm2sr


The ResursThe Resurs--DK1 satelliteDK1 satellite

•

Main task:

multi-spectral remote sensing of earth’s surface

•

Built by TsSKB Progress in Samara, Russia

•

Lifetime >3 years (assisted) •

Data transmitted to ground via high-speed radio downlink

•

PAMELA mounted inside a

pressurized

container

Mass: 6.7 tonnesHeight: 7.4 mSolar array area: 36 m2


2. The PAMELA Imaging Calorimeter -

1•

Main tasks:•

lepton/hadron

discrimination•

e+/-

energy measurement

•

Characteristics:•

22 W plates (2.6 mm / 0.74 X0

)•

44 Si layers (X-Y), 380 µm thick•

Total depth: 16.3 X0

/ 0.6 λΙ•

4224 channels•

Self-triggering mode option(> 300 GeV; GF~600 cm2

sr)•

Mass: 110 kg•

Power Consumption: 48 W

•

Design performance:•

p,e+

selection efficiency ~ 90%•

p rejection factor ~ 10 5•

e rejection factor > 10 4•

Energy resolution ~ 5% @ 200 GeV


• Front-end

⇒ CR1.4P ASIC (full custom design)Design characteristics:-

16 channels/chip-

channel structure: CSA, shaper, T/H, out. mux.-

input-selectable calibration circuit-

integrated self-trigger circuit-

shaping time = 1 µs-

sensitivity = 5 mV/MIP-

wide dynamic range: 7.1 pC

= 1400 MIP (1 MIP = 4.9 fC)

-

ENC ≈

2700 e-

rms

+ 5 e-

/pF

• ADC:-

1 16-bit ADC/view ⇒ 44 ADCs (AD977A)-

total calorimeter proc. time ~ 700 µs

• Readout:-

Calorimeter divided into 4 sections:Odd_X, Odd_Y, Even_X, Even_Y

-

1 DSP/section (ADSP2187) ⇒ 4 DSPs• on-line calibration• data compression

-

1 FPGA/section (A54SX72) ⇒ 4 FPGAs

Architecture of one channel of the CR1.4P

1-MIP signal distribution(S/N ~ 9)

1. The PAMELA Imaging Calorimeter -

2


Scientific interest:


region

e.g. two new proposals:

ACCESS:Main objective:


region, particularly in the “knee”

region (≈

1015

eV)ACCESS is meant to measure the energy spectra of individualelements from H to Fe in cosmic radiation up to energies ofapproximately 1015

eV.The data will permit a measurement of the elemental compositionof cosmic radiation close to the theoretically derived limits forefficient

supernova acceleration (~ Z x 1014

eV).

The experiment requires a calorimeter able to guarantee:•separation of e.m. and hadronic

showers• good energy resolution (σE

< 40% at the “knee”

for the hadroniccomponent);

• good charge resolution (σZ

< 0.25);• measurement of the elemental energy spectra up to Nickel;(Z = 28) and up to ≈

1015

eV.

ELO (Electron Observatory):Main objective:

extend the current data on the energy spectrumof cosmic-ray electrons above 10 TeV

with the potential ofdetecting predicted structures imprinted on the electron flux bythe acceleration process.The ELO detector concept is a

space based Si-W ImagingCalorimeter, optimized to identify electrons and measure theirenergy and arrival direction in the energy range from

100 GeV

to10 TeV.

Detector outline:• 24 active silicon strip detectors layers• 20 W absorbers, each 7 mm (2 X0

) thick; • Total ELO thickness 40 X0

, or about 1.5 λI

;• Full longitudinal containment of e.m. showers;• ∂E/E ≈

3.4% at 1 TeV;• Total estimated mass and power: 520 kg, 100 W.

Fig. 2 All-particleflux of Cosmic Rays

Therefore: Si-W calorimeters are an ideal choice, but dynamic range has to be drastically enhanced!

Fig. 3 Current measurements of high energy electrons along with capabilities of the ELO instrument (large open circles)

3. Future challanges


4. Silicon detectors optimised for increased rangeIn order to exploit both hole and electron signals, thus achieving optimumsignal-to-noise performance, we have designed a double-sided silicon stripdetectors with

parallel strips on p and n-sides.

The idea is to collect the same charge on corresponding n and p strips andto read it out by using two different front-end circuits, with differentsensitivities, in order to increase the overall dynamic range by

coveringdifferent signal regions, see Fig.4.

In 2002 we have designed and produced a first batch of parallel-strip detectors,which we have tested in October 2002 at The Svedberg Laboratory of Uppsala(Sweden) with N, O and Ne beams (see details and results in Section 5).

Characteristics of the detectors:• dimensions 8 x 8 cm2

• 380 µm thickness• 32 parallel strips on each side• 2.4 mm pitch

p strips+

n strips+

hole signal

electron signal

Preamplifier 1

Preamplifier 2


The front-end part (CSA + CDS) in CASIS1.0 fulfilled all design specs (dynamic range,noise, linearity and power consumption), therefore:

Only minor improvements and modifications were implemented in CASIS1.1 (mainly inthe CSA feedback and feedback control networks).

The ADC part in CASIS1.0 have shown some (expected) problems, mainly due tothe effect of random device mismatch on the Diff. Op. Amps:

-

Percentage of working channels ~ 50%;-

Anomalous power consumption in the non-working channels (~ 10 times)Therefore:

We revised the design of the Diff. Op. Amps of the ADC, implementing 9 ADC channelsdesigned around 2 alternative solutions.

4. The CASIS chip: design and development -

2


Chip 2 - ADC N1

050

100150200250300350

1690

1692

1694

1696

1698

1700

1702

1704

1706

1708

1710

ADC channels

Num

ber o

f ent

ries

DAC output (=ADC input) = 1.570 V1000 measurementsMean: 1699.845 ch.RMS: 1.19 ch

5. CASIS1.1 –

ADC results -

2


Launch and orbit

• Launch from BaikonurJune 15th

2006, 0800 UTCwith a Soyuz-U rocket

• “First light”: June 21st

2006• PAMELA in continuous data

taking mode since commissioningphase ended on July 11th

2006• As of ~ now:

• > 600 days of data taking(~ 73% live time)

• > 10 TByte

of raw data downlinked• > 109

triggers recordedSAA

Orbit characteristics:• Quasi-polar (70.4º)• Elliptical (350 –

610 km)• PAMELA traverses the South

Atlantic Anomaly• At the South Pole PAMELA

crosses the outer (electron)Van Allen belt


Calorimeter inCalorimeter in--flight performance flight performance --

11

July 2006 January 2008


Calorimeter inCalorimeter in--flight performance flight performance --

22

July 2006 January 2008


84 GeV/cinteracting antiproton

(flight data)


92 GeV/c

positron(flight data)


Preliminary

p (non-int)

ee--

ee++

p (non-int)

Fraction of charge released along the calorimeter track (left, hit, right)

p (int)

p (int)

Rigidity: 20-30 GV

Positron selection with the calorimeter Positron selection with the calorimeter --

11

Eve

nts (

x 10

3 )E

vent

s


ee--


pp

ee++

+ Energy-momentum match

Rigidity: 20-30 GV

Preliminary


22

Eve

nts

Eve

nts


ee--


pp

ee++

+ • Energy-momentum match• Starting point of shower • Longitudinal profile

Rigidity: 20-30 GV

Preliminary


33

Eve

nts

Eve

nts

Valter Bonvicini, Giulio Orzan, Gianluigi Zampa, Nicola Zampabonvicin/CASIS2/Bonvicini_SIF08.pdf ·...

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