Experiment Proposal - opera - Infn

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The third step of the installation consists of mounting the robot for brick handling described in Section 4.3. The loading speed of the robots is expected to be about 60 bricks/hour. 10.3 General installation schedule and commissioning The planning of the design, construction, installation and commissioning of the detector assumes that the data taking will start in May 2005, according to the CNGS beam schedule given in Fig. 178. 3 3 3 ! 3 " 3 3 3 ! 3 " 3 3 3 ! 3 " ! 3 3 3 ! 3 " " 3 3 3 ! 3 " F A I EJA B H+ EL E9 H I @ EC 6 A F H= HO ) ? ? A I I 2 EJ = I I A > A 6 K A * HE C = ? D E A A N ? = L = JA ) ? ? A I I 6 K A A N ? = L = JA 6 = HC A J+ D = > A H A N ? = L = JA , A ? = O 6 K A A N ? = L = JA 0 = @ H 5 J F + = L A A N ? = L = JA F * A = 6 K A A = HC A 0 = @ H 5 J F + = L A @ EC + A ? JE J 4 - & & @ EC @ K 2 EJ) HA = I D J? HA JA , A ? = O 6 K A A = HC A 6 = HC A J+ D = > A H ? ? HE E C 6 = HC A J+ D = > A H ? ? HE E C F * A = 6 K A @ EC + A ? JE J - + ) " I D J? HA JA ) ? ? A I I 6 K A = I I A > A 0 = @ H 5 J F 5 D EA @ E C M A H, A ? = O 6 K A 5 A A L A I M A @ 5 A A L A I F K H? ? = H K @ I A JK F / A A H= 5 A HL E? A I E I J= - G K EF J6 = HC A J+ D = > A H E I J= - G K EF JF * A = 6 K A E I J= - G K EF J K 2 EJ) HA = / 5 . = ? EEJO ? EI I E E C I J A K JHE * A = J / H= 5 = I I # # # # 3 3 3 ! 3 " Figure 178: Planning for the realisation of the CNGS beam. A summary of the planning for the construction of the detector is shown in Fig. 179. This tight schedule assumes a large parallelism in the mounting of the three supermodules. Once the experimental hall is assigned, the schedule will have to be revised depending on the space available for the detector and for its assembly. A 6 months long period is necessary for the commissioning of the experiment after installation. This means that the detector must be ready for cosmic data taking by September 2004. As a consequence the assembly and installation in the Gran Sasso hall has to start in 2002. By this date, all the work for the preparation of the underground hall will have to be completed, including the installation of the infrastructure required by OPERA. 248
Task Name Start Finish Study of main options 1 Mar '99 8 Jun '01 Testing and prototyping 1 Jul '99 9 Aug '01 Test beam activities 5 Jul '99 28 Jun '04 Design & technical drawings 31 Mar '00 12 Oct '01 Spectrometers (magnets+trackers) 31 Mar '00 9 Feb '01 Target (walls+trackers+robots) 31 Mar '00 12 Oct '01 Tendering and Ordering 8 Jan '01 18 Mar '02 Spectrometers (magnets+trackers) 9 Feb '01 5 Oct '01 Target (walls+trackers+robots) 8 Jan '01 18 Mar '02 Infrastructure preparation in GS 2 Jul '01 28 Dec '01 infrastructure of the OPERA detector 7 Jan '02 8 Jul '02 Construction 6 Aug '01 29 Dec '03 Spectrometers (magnets+trackers) 12 Oct '01 13 Dec '02 Target (walls+trackers+robots) 6 Aug '01 29 Dec '03 Assembly & installation 2 Sep '02 29 Oct '04 Spectrometer 1 2 Sep '02 2 Jun '03 Spectrometer 2 6 Jan '03 29 Sep '03 Spectrometer 3 5 May '03 29 Dec '03 Target Section 1 2 Jun '03 29 Dec '03 Target Section 2 29 Sep '03 5 Apr '04 Target Section 3 29 Dec '03 5 Jul '04 Drift tubes 1 29 Dec '03 23 Feb '04 Drift tubes 2 5 Apr '04 31 May '04 Drift tubes 3 5 Jul '04 30 Aug '04 Cabling SM1 23 Feb '04 19 Apr '04 Cabling SM2 31 May '04 26 Jul '04 Cabling SM3 + Robot rail 30 Aug '04 25 Oct '04 Robot left 19 Apr '04 29 Oct '04 Robot right 19 Apr '04 29 Oct '04 Commissioning of the trackers 19 Apr '04 20 Dec '04 Cosmic data taking without bricks 12 Jul '04 11 Feb '05 ECC brick production 9 Mar '04 1 Apr '05 ECC brick filling into the target section 5 Jul '04 23 Jun '05 filling SM1 5 Jul '04 3 Jan '05 filling SM2 30 Aug '04 25 Feb '05 filling SM3 28 Feb '05 23 Jun '05 Detector complete 23 Jun '05 23 Jun '05 Target-trackers alignment 3 Jan '05 22 Jul '05 Cosmic data taking with bricks 30 Aug '04 21 Jul '05 CNGS beam commissioning 15 Feb '05 15 May '05 Neutrino data taking starts 15 May '05 15 May '05 00 2001 2002 2003 2004 2005 3 4 1 2 3 4 1 2 3 4 1 2 3 4 1 2 3 4 1 2 3 23/6 15/5 Figure 179: General planning for the construction of the OPERA detector. 249
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CERN/SPSC 2000-028 SPSC/P318 LNGS P
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N. Bruski, S. Buontempo, F. Carbona
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Contents 1 Introduction 5 1.1 Physi
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6.7.1 Multiple scattering analysis
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1 Introduction In this document we
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eactor experiments (KAMLAND [22], B
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difference being the nature of the
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The total energy of electrons and
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through the decay topology and its
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Figure 6: Simulated ν τ event wit
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particles above 10 MeV . One can se
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vertex position as predicted by the
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• stability and maintenance: no p
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Figure 11: Illustration of the vari
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Table 3: Expected numbers of τ and
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3 The CNGS neutrino beam 3.1 The be
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per year of operation because the S
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ν µ at GS (p.o.t. GeV m 2 ) -1 10
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Figure 19: Generated (continuous li
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Emulsion Film + 56 (Lead + Emulsion
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The mechanical properties of the fi
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Figure 24: Film thickness distribut
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contact at different temperature an
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Figure 27: Photograph of a minimum
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entry : 85 RMS: 0.060 15 10 5 0 0 d
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[micron] 2 1 0 -1 -2 [micron] 2 1 0
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een searching for old emulsion plat
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Figure 33: Thickness distribution f
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Figure 35: RMS distribution of 472
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Figure 37: Wall support structure.
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ensures a well defined brick positi
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Figure 41: Detail of the brick mani
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The strips are 6.7 m long, 2.6 cm w
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the effective maximal length (for p
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Table 7: Characteristics of the 64-
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photomultiplier to be tested diaphr
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modate from 512 up to 5180 fibres.
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The fast shaper has a high gain in
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The Ethernet capable device provide
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R&D already performed by the MINOS
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Figure 54: Isometric view of the di
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Figure 56: Magnetic field distribut
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RPC layout 8.00 m 8.75 m Figure 58:
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formance, it is presently foreseen
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Figure 61: Drift plane arrangement
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Figure 63: Schematic view of a XPC
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Figure 64: Acceleration spectrum fo
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Figure 65: The OPERA detector shown
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Table 9: Number of electronic chann
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Adjustable gain Channel 0 Sample &
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Trigger OUT IN Discri. Time Ref. PP
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Super Module 1 Super Module 2 Super
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5 Analysis of the electronic detect
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Track segments on both the emulsion
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5.5 Brick finding efficiency The se
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Wall finding efficiency 1 0.95 0.9
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The worst case leading to the lowes
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electromagnetic showering events an
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Studies on the strategies have star
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which may enter in such a compariso
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Figure 84: The total brick finding
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Figure 86: Charge determination of
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Figure 89: Muon momentum resolution
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Figure 91: Muon momentum resolution
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Reconstructed Pion Energy N Analog
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Figure 98: The difference between r
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By using the above running modes of
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µm EXP.: DONUT 3039/01910 MOD.:ECC
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emulsion film plastic foils and edg
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200micron base 50micron emulsion la
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Figure 106: Tracking efficiency of
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a base track on film 2 a penetratin
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Long decays, defined as a decay top
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more than 60 views/s recognising al
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Table 12: Basic numbers used to des
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an area that one S-UTS can process
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unit cell L=1300micron Pb plate ( 1
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We recall that the intrinsic positi
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Figure 116: The top histograms show
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The error on θ S due to both the s
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Figure 120: Fraction of pions which
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#1 #2 #3 #4 #5 γ γ ∆θ 4= |θ 5
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Figure 124: Energy resolution for e
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Figure 126: Efficiency for γ’s t
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7 Physics performance 7.1 Electron
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7.2 Muon identification efficiency
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Table 13: Muon identification effic
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Table 14: Brick finding efficiency
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The second result is obtained from
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Figure 134: Brick-to-brick connecti
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Figure 136: Distribution of τ deca
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For long decays the overall efficie
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The φ angle is expected to peak at
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Table 19: Summary of the kinematica
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known. Because of these uncertainti
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Table 21: Expected charm background
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π− e+ γ e- e+ e- γ π− Figur
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Table 24: Estimates of the rate of
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Table 27: Expected numbers of τ an
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Table 28: Sensitivity at the 90% CL
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Page 209 and 210: Table 31: Radioactivity measurement
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Page 213 and 214: Figure 152: A typical PMT response
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Page 217 and 218: Electrons 1GeV/c 20mm Pb Number of
Page 219 and 220: tube. An Image Intensifier (II) by
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Page 223 and 224: HPD’s pixels (Fig. 162). The cook
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Page 229 and 230: The upstream tracker T 1-3 between
Page 231 and 232: Figure 168: Distributions of the ap
Page 233 and 234: Figure 169: Example of a large-angl
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Page 237 and 238: 9.1.3 Wall support structures An al
Page 239 and 240: Nevertheless, the possibility to us
Page 241 and 242: Figure 174: (a) 3D view of the spec
Page 243 and 244: 9 p.e. and 6.9 p.e. at a distance f
Page 245 and 246: Figure 176: Neutrino induced charm
Page 247 and 248: A test programme for emulsion brick
Page 249 and 250: The space requirements in the exper
Page 251: advance. The sets of scintillator s
Page 255 and 256: 11 Experimental infrastructure 11.1
Page 257 and 258: After the exposure to cosmic rays,
Page 259 and 260: on the size of these stations. A co
Page 261 and 262: Table 38: Expected contributions to
Page 263 and 264: the developed emulsions and to stan
Page 265 and 266: As the sensitivity is not limited b
Page 267 and 268: [26] M. Apollonio et al., Phys. Let
Page 269: [89] http : //tosca.web.cern.ch/T O
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