1. LNF Scientific Committee, October 28th 1 Paola Gianotti LNF

2. LNF Scientific Committee, October 28th 2 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

3. LNF Scientific Committee, October 28th 3 Where we were… During last committee (May 18 th ) the mechanical frame that houses FINUDA detectors, “CLESSIDRA”, was brought into the DA  NE hall To gain some time on the schedule the “CLESSIDRA” was also inserted inside the magnet (May 19 th )

4. LNF Scientific Committee, October 28th 4 Work done during the August shutdown ( 30/7  3/9 ) “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

5. LNF Scientific Committee, October 28th 5 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 0.01degrees The precision obtained on the z axis alignement is 0.5 mm “Clessidra” has been aligned using a laser tracker (Leica LTD500)

6. LNF Scientific Committee, October 28th 6 e  side e  side

7. LNF Scientific Committee, October 28th 7 New DAQ system CPUCPU CorboCorbo VIC8250VIC8250 GTS CPUCPU CorboCorbo VIC8250VIC8250 TOF CPUCPU CorboCorbo VIC8250VIC8250 LMD CPUCPU CorboCorbo VIC8250VIC8250 STB CPUCPU CorboCorbo VIC8250VIC8250 ISIM OSIM PVICdiff BUS for data stream Run Control + GEB+ Storage VME crates Ethernet for command transmission and event monitoring CPUCPU CorboCorbo VIC8250VIC8250 PVICoptical connection for data stream COUNTING ROOM DAFNE HALL

8. LNF Scientific Committee, October 28th 8 Monitoring scheme Run Control PC Global monitor Event Display Single detector monitor Slow Control

9. LNF Scientific Committee, October 28th 9 Performance of the new DAQ system Active Detectors: TOF GTS Tot. buffer size: 1 kB Trigger rateDAQ 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 kB Trigger rateDAQ 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 kB Trigger rateDAQ 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 kB Trigger rateDAQ rate MB/s [Hz] [Hz] 300 296 0.6 350 345 0.7 400 345 0.7 Active Detectors: TOF GTS LMD STB Tot. buffer size: 4 kB Trigger rateDAQ rateMB/s [Hz] [Hz] 100 106 0.4 200 200 0.7 300 200 0.7 Active Detectors: TOF GTS LMD STB Tot. buffer size: 4 kB Trigger rateDAQ rateMB/s [Hz] [Hz] 100 106 0.4 200 200 0.7 300 200 0.7

10. LNF Scientific Committee, October 28th 10 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 cutBhabhaK + KK s K l Touschek none1000 100000 imult9815233682327 back864306842 emult739171600 tof739138550 energy73918550 acceptance0.7390.0180.055<1.9·10 -7 

11. LNF Scientific Committee, October 28th 11 Online luminosity monitor II 5  Bhabha = 810 nb for 45 o <  <135 o MC Bhabha trigger efficiency ~ 0.74 @ L = 5·10 31 Bhabha trigger rate ~ 30Hz If Bhabha reconstruction efficiency 1 ~ 15’ to to give L value @ 1%  Bhabha = 810 nb for 45 o <  <135 o MC Bhabha trigger efficiency ~ 0.74 @ L = 5·10 31 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 K  K  pairs

12. LNF Scientific Committee, October 28th 12 Work done during October shutdown ( 15/10  21/10 ) 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

13. LNF Scientific Committee, October 28th 13 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 1.70  0.034.70  0.03 244.00 27.10 3.70 2.60 4.10 27.10 4.70 1.00 4.70 0.60 192.9652.62 2.60 4.10  0.03 1.40  0.03 182.96  0.03 3.325  0.03 2.60 210.00 200.00 44.10 0.625 2.60 210.00 200.00 1.00 44.10 3.7  0.03 To decide which targets will be mounted for the first data taking, we are organizing a Workshop March 20/22 2002 together with the major theoretical experts (A. Gal, A.Ramos,…) http://fidabs.ing.unibs.it/WHPD/ To decide which targets will be mounted for the first data taking, we are organizing a Workshop March 20/22 2002 together with the major theoretical experts (A. Gal, A.Ramos,…) http://fidabs.ing.unibs.it/WHPD/

14. LNF Scientific Committee, October 28th 14 Spectroscopized in coincidence First case of exclusive NM decay: a few/pb -1 Why a 6 Li target?

15. LNF Scientific Committee, October 28th 15 Spectroscopized d+d spectr. (  1/pb -1 if B.R.  10 -3 ) p+ 3 H spectr.(0.5/ pb -1 if B.R.  10 -3 )  + +n+ 3 H many events (  10 2 /pb -1 ) how distinguishable?    about 10 2 /pb -1   p  (in  coinc.) about 10/pb -1  n  (in  coinc.) a few/pb -1 4 He+  + spectr. (10 2 /pb -1 ) calibration

16. LNF Scientific Committee, October 28th 16 7 Li 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

17. LNF Scientific Committee, October 28th 17 Lithium target mounted on the mechanical support

18. LNF Scientific Committee, October 28th 18 7 Li target prepared as manufacturing test for the final 6 Li target Drawn Li target Target obtained with melting

19. LNF Scientific Committee, October 28th 19 Melted Lithium inside the oven. Due to the high surface tension Lithium is not filling all the melting pot Melted Lithium inside the oven. Due to the high surface tension Lithium is not filling all the melting pot

20. LNF Scientific Committee, October 28th 20 A Lithium block obtained by melting is then drawn

21. LNF Scientific Committee, October 28th 21 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 DETECTOR Alignment procedure using cosmic data Data: collected ~10 6 “good” events VDET continuously working for ~3 months used 18 modules cooled @ (18º±2º)C VDET in the ASTRA clean room @ 21º-25ºC

22. LNF Scientific Committee, October 28th 22 Layout of the FINUDA central region 2 osim isim target tofino beam pipe telescope used in the present analysis reconstructed cosmic ray 3 4 1 1 cm 8 7 6 5 d

23. LNF Scientific Committee, October 28th 23 ndf = # events - # param  d = - 426 µm  = - 2.3 mrad  = - 0.3 mrad  r = 126 µm  z = 45 µm  = - 0.2 mrad 1st step Position of # 1 after the 1 st step Translation parameter: Dd Translation parameter: Dz Translation parameter: Dr Rotation parameter: 0r Rotation parameter: 0d Rotation parameter: 0z

24. LNF Scientific Committee, October 28th 24 2nd step  d = 2.6 µm  z = - 1.4 µm  r = 105 µm  = 0.1 mrad  = - 0.2 mrad  = - 0.2 mrad ndf = # events - # param … final step Translation parameter: Dd Translation parameter: Dz Translation parameter: Dr Rotation parameter: 0r Rotation parameter: 0d Rotation parameter: 0z

25. LNF Scientific Committee, October 28th 25 Results:  int : pitch/  12 = =  2  int +   mscat +  2 sag … to be analyzed and corrected average efficiency (1234/123) of a single module > 97% in the active region = 59.9  0.6µm Assessed time scale: ~ 20.000 tracks required ~ 4 Hz of cosmic ray crossing TOFINO rate of 5678 tracks / all tracks ~ 0.005  ~2 weeks of cosmic rays data taking d [um] z ~ 30 µm d ~ 15 µm = 36.9  0.3µm Stand. dev. of residues along d Stand. dev. of residues along Z

26. LNF Scientific Committee, October 28th 26 Work plans for January shutdown ( 02/02  17/02? ) Reconnection of the magnet to the Cryogenic line Magnet cooling down (~12 days after Kloe cooling) ITOF mounting & test; installation of few microstrips Inner LMDC insertion He Bag installation going on End-caps closure Magnet switching on Finuda foresees about 6 weeks of DAFNE shutdown starting from January 2 nd

27. LNF Scientific Committee, October 28th 27 January shutdown details I

28. LNF Scientific Committee, October 28th 28 January shutdown details II

29. LNF Scientific Committee, October 28th 29 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