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1LNF Scientific Committee, October 28th
Paola Gianotti
LNF
2LNF Scientific Committee, October 28th
Outlook
Where we are since last committee…• Detector installation progress• Detector debug• Targets preparation• Online software/hardware upgrades • Online luminosity monitor • Micro-strips alignment procedure
Where we plan to arrive till next committee…• Magnet work in progress• Central detectors installation plans• Detector debug • Cosmic rays tests
Where we are since last committee…• Detector installation progress• Detector debug• Targets preparation• Online software/hardware upgrades • Online luminosity monitor • Micro-strips alignment procedure
Where we plan to arrive till next committee…• Magnet work in progress• Central detectors installation plans• Detector debug • Cosmic rays tests
3LNF Scientific Committee, October 28th
Where we were…
During last committee (May 18th) the mechanical frame that houses FINUDA detectors, “CLESSIDRA”, was brought into the DANE hall
To gain some time on the schedule the “CLESSIDRA” was also inserted inside the magnet (May 19th)
4LNF Scientific Committee, October 28th
Work done during the August shutdown (30/73/9)
“Clessidra” alignment inside the magnet Piping and cabling detectors-FEE racks (ST, outer LMDC, TOFONE)
Detector checkout & debug started (ST, outer LMDC, TOFONE)
Begin of He-bag piping Slow control & safety systems installation TRIGGER cabling & debug New DAQ installation & debug
5LNF Scientific Committee, October 28th
1. “Clessidra” has been aligned to the iron yoke to be planar (x-z plane horizontal) 2. The axis has been aligned to that of the cryostat.3. The center of the “Clessidra” has been moved along z to be centered to have the same
distance from the 2 end-caps
The precision obtained on the x-z plane is 0.01degreesThe precision obtained on the z axis alignement is 0.5 mm
“Clessidra” has been aligned using a laser tracker (Leica LTD500)
6LNF Scientific Committee, October 28th
e side
e side
7LNF Scientific Committee, October 28th
New DAQ system
CPU
Corbo
VIC8250
GTSGTS
CPU
Corbo
VIC8250
TOFTOF
CPU
Corbo
VIC8250
LMDLMD
CPU
Corbo
VIC8250
STBSTB
CPU
Corbo
VIC8250
ISIMISIM
OSIMOSIMPVICdiff BUS for data stream
Run Control + GEB+ Storage
VMEcrates
Ethernet for command transmission and event monitoring C
PU
Corbo
VIC8250
PVICoptical connectionfor data stream
COUNTING ROOM
DAFNE HALL
8LNF Scientific Committee, October 28th
Monitoring scheme
Run Control PC
Global monitorEvent Display
Single detectormonitor
Slow Control
9LNF Scientific Committee, October 28th
Performance of the new DAQ system
Active Detectors: TOF GTS Tot. buffer size: 1 kBTrigger rate DAQ rate MB/s [Hz] [Hz] 350 346 0.4 400 394 0.4 450 400 0.4
Active Detectors: TOF GTS Tot. buffer size: 1 kBTrigger rate DAQ rate MB/s [Hz] [Hz] 350 346 0.4 400 394 0.4 450 400 0.4
Active Detectors: TOF GTS Tot. buffer size: 2 kBTrigger rate DAQ rate MB/s [Hz] [Hz] 300 296 0.6 350 345 0.7 400 345 0.7
Active Detectors: TOF GTS Tot. buffer size: 2 kBTrigger rate DAQ rate MB/s [Hz] [Hz] 300 296 0.6 350 345 0.7 400 345 0.7
Active Detectors: TOF GTS LMD STBTot. buffer size: 4 kBTrigger rate DAQ rate MB/s [Hz] [Hz] 100 106 0.4 200 200 0.7 300 200 0.7
Active Detectors: TOF GTS LMD STBTot. buffer size: 4 kBTrigger rate DAQ rate MB/s [Hz] [Hz] 100 106 0.4 200 200 0.7 300 200 0.7
10LNF Scientific Committee, October 28th
Online luminosity monitor I
With MC studies we have defined the Bhabha events topology:• imult: ITOF mult = 2; • back: back-to-back ITOF topology ;• emult: ETOF mult 2 4; • energy: small E inside ITOF;• tof: t betweeen ETOF and ITOF 4.5 6.5 ns;
x
y
10 cm
cut Bhabha K+ K K s K l Touscheknone 1000 1000 1000 100000imult 981 523 368 2327back 864 306 84 2emult 739 171 60 0tof 739 138 55 0energy 739 18 55 0acceptance 0.739 0.018 0.055 < 1.9 ·10 -7
11LNF Scientific Committee, October 28th
Online luminosity monitor II
Bhabha = 810 nb for 45o<<135o
MC Bhabha trigger efficiency ~ 0.74@ L= 5·1031 Bhabha trigger rate ~ 30Hz
If Bhabha reconstruction efficiency 1~ 15’ to to give L value @ 1%
Bhabha = 810 nb for 45o<<135o
MC Bhabha trigger efficiency ~ 0.74@ L= 5·1031 Bhabha trigger rate ~ 30Hz
If Bhabha reconstruction efficiency 1~ 15’ to to give L value @ 1%
As a cross check we can also obtain luminosity and energy values counting KK pairs
12LNF Scientific Committee, October 28th
Work done during October shutdown (15/1021/10)
Test of end-caps closure Installation -strips FEE Start of central detector cables spreading upon the magnet~2/3 He-bag piping going on Detector checkout & debug going on (ST, outer LMDC, TOFONE)
TOF laser installation DAQ tests
13LNF Scientific Committee, October 28th
Targets design
Vanadium target profile
Aluminum target profile
Carbon target profile
Lithium target profiles
Silicon target profile
200.00
44.10210.0044.10
26.0
1.7
0
0.0
3
4.7
0
0.0
3
244.00
244.00
27.10
3.7
0
2.6
02
.60
4.1
027.10
27.10
27.10
4.7
0
1.0
0
4.7
0
0.6
0
192.9652.62 52.62
2.6
0
4.1
0
0.0
3
1.4
0
0.0
3
182.960.033
.32
50
.03
2.6
0
210.00
200.00
44.1044.10
0.6
25
2.6
0
210.00
200.00
1.0
0
44.1044.10
3.7
0
.03
To decide which targets willbe mounted for the first datataking, we are organizing a Workshop March 20/22 2002together with the major theoretical experts (A. Gal, A.Ramos,…)http://fidabs.ing.unibs.it/WHPD/
To decide which targets willbe mounted for the first datataking, we are organizing a Workshop March 20/22 2002together with the major theoretical experts (A. Gal, A.Ramos,…)http://fidabs.ing.unibs.it/WHPD/
14LNF Scientific Committee, October 28th
SpectroscopizedSpectroscopized
Li K 6-
He n n 4
06 He
-6 Li H6
Spectroscopized in coincidence
First case ofexclusive NM
decay: a few/pb-1
Why a 6Li target?
15LNF Scientific Committee, October 28th
Spectroscopized-6 Li
p He5
d+d spectr. (1/pb-1 if B.R. 10-3)
p+ 3H spectr.(0.5/ pb-1 if B.R. 10-3) ++n+3H many events ( 102/pb-1)how distinguishable?
about 102/pb-1
n p He4
p(incoinc.) about 10/pb-1
n(incoinc.) a few/pb-1
p p H4 4He+ + spectr. (102/pb-1) calibration
16LNF Scientific Committee, October 28th
7Li target prototype 4mm thickness7Li target prototype 4mm thickness
Lithium is enclose in a 110 m thickness foil consisting of 3 layers: polypropylene+aluminum+polyester
Lithium is enclose in a 110 m thickness foil consisting of 3 layers: polypropylene+aluminum+polyester
17LNF Scientific Committee, October 28th
Lithium target mounted on the mechanical supportLithium target mounted on the mechanical support
18LNF Scientific Committee, October 28th
7Li target prepared as manufacturing test for the final 6Li target 7Li target prepared as manufacturing test for the final 6Li target
Drawn Li target
Target obtained with melting
19LNF Scientific Committee, October 28th
Melted Lithium inside the oven. Due to the high surfacetension Lithium is not filling all the melting pot
Melted Lithium inside the oven. Due to the high surfacetension Lithium is not filling all the melting pot
20LNF Scientific Committee, October 28th
A Lithium block obtained by melting is then drawnA Lithium block obtained by melting is then drawn
21LNF Scientific Committee, October 28th
Preliminary analysis:• 1 telescope of 4 modules• aligned with the “3D residual vectors” method• convergence of parameters by using a sequential and iterative technique. Present analysis made for a stack of 4 modules, 6x4 parameters to be minimized • check the distributions of residuals
Aims:• work out an alignment strategy for the double-sided silicon detector (VDET)• test the VDET response while working at nominal conditions
Aims:• work out an alignment strategy for the double-sided silicon detector (VDET)• test the VDET response while working at nominal conditions
VERTEX DETECTORAlignment procedure using cosmic data
Data:• collected ~106
“good” events• VDET continuously working for ~3 months• used 18 modules cooled @ (18º±2º)C• VDET in the ASTRA clean room @ 21º-25ºC
22LNF Scientific Committee, October 28th
Layout of the FINUDA central region
2
osim
isim
target
tofino
beam pipe
telescope used in the present analysis
reconstructed cosmic ray
34
1
1 cm
8
7
6 5
d
23LNF Scientific Committee, October 28thndf = # events - # paramndf = # events - # param
d = - 426 µm
= - 2.3 mrad = - 0.3 mrad
r = 126 µm
z = 45 µm
= - 0.2 mrad
1st s
tep
Position of # 1 after the 1st step
Translation parameter: DdTranslation parameter: Dd Translation parameter: DzTranslation parameter: DzTranslation parameter: DrTranslation parameter: Dr
Rotation parameter: 0rRotation parameter: 0r Rotation parameter: 0dRotation parameter: 0d Rotation parameter: 0zRotation parameter: 0z
24LNF Scientific Committee, October 28th
2nd
step
d = 2.6 µm z = - 1.4 µm
r = 105 µm
= 0.1 mrad = - 0.2 mrad
= - 0.2 mrad
ndf = # events - # paramndf = # events - # param
… final step
Translation parameter: DdTranslation parameter: Dd Translation parameter: DzTranslation parameter: DzTranslation parameter: DrTranslation parameter: Dr
Rotation parameter: 0rRotation parameter: 0r Rotation parameter: 0dRotation parameter: 0d Rotation parameter: 0zRotation parameter: 0z
25LNF Scientific Committee, October 28th
Results:
• int : pitch/12 =
• <> = 2int + mscat + 2
sag
… to be analyzed and corrected
• average efficiency (1234/123)
of a single module > 97% in the
active region
<Z> = 59.9 0.6µm
Assessed time scale:
~ 20.000 tracks required ~ 4 Hz of cosmic ray crossing TOFINOrate of 5678 tracks / all tracks ~ 0.005 ~2 weeks of cosmic rays data taking
d [um]
z ~ 30 µm
d ~ 15 µm
<d > = 36.9 0.3µmStand. dev. of residues along dStand. dev. of residues along d
Stand. dev. of residues along ZStand. dev. of residues along Z
26LNF Scientific Committee, October 28th
Work plans for January shutdown (02/0217/02?)
Reconnection of the magnet to the Cryogenic lineMagnet cooling down (~12 days after Kloe cooling)ITOF mounting & test; installation of few microstrips Inner LMDC insertionHe Bag installation going onEnd-caps closureMagnet switching on
Finuda foresees about 6 weeks of DAFNE shutdown starting from January 2nd
27LNF Scientific Committee, October 28th
January shutdown details I
28LNF Scientific Committee, October 28th
January shutdown details II
29LNF Scientific Committee, October 28th
Conclusions
Up to now FINUDA installation is going on without particular problems. Good cooperation with A.D.
Detectors installation & debug is our priority, but we are also preparing all the tools for running (targets, DAQ, Monitors, alignment procedure…)
We are working in connection with the best theoreticians of the field to select the best set of targets [http://fidabs.ing.unibs.it/WHPD/ ]
Cosmic rays tests are foreseen starting from March Detector will be ready for roll-in by summer 2002