MUon RAdiographY (MU-RAY) of volcanoes and the “challenge” at … · 2008-09-29 · MUon...
Transcript of MUon RAdiographY (MU-RAY) of volcanoes and the “challenge” at … · 2008-09-29 · MUon...
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MUon RAdiographY (MU-RAY)of volcanoes and the “challenge” at
Mt. Vesuvius
P. StrolinFerrara, 15 settembre 2008
G.B. Lusieri, ~1780
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Radiografia di vulcani con µ da raggi cosmici
• Misura assorbimento differenziato(come per raggi X)
• Idea radiografia muonica non nuova:- 1955: Georg (misura spessore strati di
neve)- 1970: Alvarez (ricerca di camere funebri
nella piramide di Chefren)
• Dal 2003: indagine della strutturainterna dell’ “edificio” di vulcanimediante µ quasi orizzontali:
→ alta risoluzione spaziale (decine di m) → bellissimi risultati (Tanaka et al., Nature)→ predizione modalità eruzioni, ….. … monitoraggio in tempo (quasi) reale
• Grande interesse per Vesuvio, .…Stromboli, … altri vulcani:→ Collaborazione internazionale
Radiografia muonica della zonasotto il fondo della caldera del
M. Asama (Giappone)
Si noti una zona ad alta densità(lava solidificata) e una cavità
sottostante
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Main features of Mt. Vesuvius
- Active (now quiescent) volcano, 1280 m high
- Grown in the caldera of an older, larger volcano (Mt. Somma)
- Muon radiography is a “challenge”, due to its morphology :Mt. Somma, secondary cones (Colle Umberto)
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“Plinyan” and sub-Plinyaneruptions
…. 79 (Pompeii), …. 1631, … 1906, …. 1944 …. ?
1631
1906
1944
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Status and recent history
But look at (relatively) recent history !
At present, the monitoring systemdoes not give signs of notable activity
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Morphological evolution1630-1944
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The highest volcanic risk in Europe:about 600,000 people live in the “red zone”
around Mt. Vesuvius or on its slopes
2 km
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Stromboli
Altezza 930 m s.l.m., attivitàvulcanica ordinaria a 750 m
Attività “stromboliana”: esplosioniintermittenti dovute ad accumulodi gas, condotto essenzialmenteaperto
Rara e modesta attività effusivaIl segnale dovuto all’attivitàesplosiva e il tremore vulcanicohanno origine a piccola profondità,a circa 200 m al di sottodell'area craterica.
2007
Grande interesse per radiografia
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Workshop MU-RAYNapoli 11-12 settembre
• Programma:– Radiografia con neutrini e muoni (con proceedings su
Earth and Planetary Sciences)– Aspetti specifici del progetto MU-RAY
• Partecipazione di ∼30 fisici e vulcanologi daItalia, Giappone, Francia, Spagna e USA
• Definite le linee guida del progetto MU-RAY• Prese le decisioni operative per iniziarne la
realizzazione
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Linee guida del progetto MU-RAY• Fattibilità dimostrata da osservazioni in Giappone• Obbiettivo di MU-RAY: radiografia ad alta
risoluzione in 3D con accesso a zone profonde:(importanti passi in avanti)
• Coll. Internazionale, Vesuvio come progetto pilota• Sviluppare telescopio adattabile ad altri vulcani
(Stromboli, … Antille … Giappone …) e con capacitàdi “zoom”
• Uso di scintillatori con tecnologie collaudate• Iniziare subito, in parallelo:
– Progetto e realizzazione dei (3) telescopi MU-RAY– Prime misure sul campo con telescopio giapponese: area
1m2, basse accettanza e risoluzione angolari
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Simulazione
Serve per:•ottimizzare il progetto e la collocazione dei telescopi inrelazione a flusso di muoni•Stimare la sensibilità a strutture interne•Mettere a punto i metodi e le esigenze dell’analisi inversaper la ricostruzione in 3D (almeno 3 telescopi)
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Estimate of muon rate and of sensitivityto internal structures:a geometrical model
θ
µ detector
structurediameter Φ
volcanoedifice
500 m
250
m25
0 m 50
0 m
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Estimate of muon rate and of sensitivity: physics input
Part. Data Gr.
Absorption
Decay
srGeVscmEE
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Atmospheric µ flux
GeVinE0
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GeVE 1000>
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Estimate of µ rate and of sensitivity: rates and required detector area x time
Φ of structure [m] 20ρ = 0
50Δρ/ρ0 = 0.1
Rate N through structure [m-2 day-1](ρ0 = 2.2 g cm-3, Eµ > 0.5 GeV)
2.5 16
ΔN/N by structure 0.09 0.02
Events for 3 σ detection of structure 1,150 20,000
Detector area x time [m2 month] 15 40
~10 m2 required for a few months data taking
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Full simulation (in progress)
Similarity withEarth radiography by neutrinosν ↔ µ Earth ↔ volcano
Methods and codes have been developed:first applied to Earth radiography (Miele and coll.),
now being applied to Mt. Vesuvius
ν
µ
Digital Elevation Map (DEM)of Mt. Vesuvius
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Step 1: generate atmospheric muons
• 3D Digital Elevation Map
• Tracks intercepting the detector generated and
projected backward
• Along their directions,muons generated accordingto the known spectrum
(from PDG)
enteringµ tracks
3D digital map
detector
structure
Input to full simulation of µ reaching thedetector through Vesuvius
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Step 2: full simulation of µ reaching thedetector through Mt.Vesuvius
• Simulation of the geometry and µ tracking done withGEANT4 (Geometry ANd Tracking tool)
• “Experimental apparatus” defined as Vesuvius + detector
• The longitudinal dimension of the apparatus is the lengthof rock intercepted by the track (from the previous step)
• The experimental apparatus can consist of zones withdifferent densities, allowing to simulate structures insideVesuvius
• The rock initial density will be taken to be 2.2 g/cm3
In progress
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Multiple Scattering: Monte Carlo(risultati preliminari)
Dati in ingresso• Energia fissa o spettro• 1-2 Km di roccia
• ρ = 2.6 g/cm3 (alta)
Diffusione Multiplaσ ∼ 15 mrad
Risultati analoghi dai giapponesi
Intenso lavoro in corso
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Observation at Mt.Asama
ScintillatorsResolution 66 mradNIM A507 (2003) 657
EmulsionsResolution < 10 mrad
EPS Lett. 263 (2007) 104
Angular resolution is important
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Progetto dei telescopi MU-RAY
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Dagli attuali telescopi a MU-RAY
• Area: x 10• Buona risoluzione spaziale e piani a distanza ravvicinata: massimaaccettanza angolare
• Risoluzione angolare ∼10 mrad e misure in tempo (quasi) reale• Operatività in ambiente vulcanico: minima manutenzione, bassapotenza, trasportabilità, …..
⇓
Strips di scintillatori con risoluzione spaziale
• Area: ~ 1 m2
→ osservazioni a bassa profondità (es. 50-100 m sotto fondo caldera del Mt. Asama) a causa di assorbimento nella roccia e riduzione flusso di µ• Tecniche di rivelazione
– Scintillatori (8-10 cm larghezza): modesta risoluzione (∼40 mrad)– Emulsioni: alta risoluzione, ma misure laboriose e non in tempo reale
Att
uali
telesc
opi
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The MINERvA Inner Detector scintillators
• The triangular shape offers advantages:– No gaps between strips– Continuous position determination by weighted average of the
signals from two strips: no pixel effects– Good spatial resolution (~3 mm) → 10 mrad angular resolution with “short” lever arm (~ 0.5 m)
• Wave Length Shifting Fibre in a hole created in extrusion• Strips with co-extruded coating: easier to assemble
3.3 cm
WLS fibre
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The MU-RAY muon telescope(MINERvA scintillators, PMTs, OPERA electronics and DAQ)
• Each plane 64 x 2 scintillators(total width ~2.1 m)
• Two x-y doublets• Total 512 scintillators• Read-out on one side: 512 channels• Multianode PMTs as in OPERA but
with clear fibres• Electronics and DAQ: evolution
from OPERA• Angular resolution ~ 3mm x √ 2 /
(0.5m distance) ≈ 10 mrad
The telescope must be housed in a barrack, hence to achieve a largerarea, use more telescopes
2.1m
2.1m
x y x y
32x2 ch↓64ch PMT
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Procurement of scintillators
• Various large experiments are using scintillator stripsin the USA: MINOS, MINERvA, ….
• FNAL-NICADD have set-up an “industrial” extrusionfacility:
see A. Bross, Advanced Extruded Scintillator R&D,www.fnal.gov/directorate/ANL-FNAL-Collaboration/files/2008-06-27-ANL_FNAL_Bross.ppt (2008)
• They accept to produce scintillators for MU-RAY
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Programma diricerca
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Vesuvio e Asama• I coni sommitali dell’Asama (2560 m) e del Vesuvio (1280 m)
sono simili, anche se la caldera del Vesuvio è più grande
• Si intende fare una prima misura con un telescopio esistente (“1 m2”), in parallelo con lo sviluppo del telescopio
MU-RAY (di grande area)
Mt. Asama
500 m
N
Mt. Vesuvius
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Il telescopio da 1m2
• Scintillatori 7.8 cm dilarghezza• Due piani (x-y) a 2 m didistanza (per ovviare a poverarisoluzione spaziale e ottenere unarisoluzione angolare di ∼ 40 mrad*)• Attualmente in misura all’isolaSatsuma Iwo-jima
Disponibile a inizi 2009 per osservazioni a bassaprofondità (50-100 m) sotto il fondo della caldera del
Grande Cono del VesuvioI collaboratori francesi stanno costruendo un telescopio simile per
prime misure ai vulcani delle Antille
* Tenendo conto di un deterioramento di un fattore ~2.5 per effetti di pixel
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Aim for the MU-RAY time-table after theWorkshop (3 telescopes, no time contingency)
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Il programma di ricerca
2008-9• Simulazioni: flusso µ in siti tel. 1m2 e MU-RAY• Definizione siti dei telescopi, sensibilità a disomogeneità• Installazione e prime osservazioni con telescopio 1m2: risultati
geofisica, messa a punto metodologia, validazione simulazione, ….• Costruzione e prove di un piano del telescopio MU-RAY
2010• Possibile continuazione presa dati con telescopio 1m2
• Costruzione e inizio presa dati con il primo telescopio MU-RAY• Costruzione degli altri telescopi MU-RAY
• 2011• Inizio presa dati con i telescopi MU-RAY per osservazioni in 3D
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Collaborazione erichieste finanziarie
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The Collaboration
F. Beauducel1, S. Buontempo2, L. D’Auria3, Y. Déclais6, G. DeLellis,2,4, G. Festa4, P. Gasparini4,5, D. Gibert1, G. Iacobucci2, N.Lesparre1, A. Marotta2, J. Marteau6, M. Martini3, G. Miele2,4, P.Migliozzi2, C.A. Moura2, O. Pisanti2,4, S. Pastor7, R. Peluso3, G.Scarpato3, G. Sekhniaidze2, P. Strolin2,4, H. Taira8, M. Tanaka9,H.K.M. Tanaka8, A. Tarantola1, T. Uchida10, M. Vassallo2,5, I.
Yokoyama11 and A. Zollo4
1 Institut de Physique du Globe, Paris2 Sezione di Napoli, INFN3 Osservatorio Vesuviano, INGV4 Università di Napoli “Federico II”5 Consorzio Analisi e Monitoraggio Rischi Ambientali (AMRA), Napoli6 Institut de Physique Nucléaire de Lyon (IPNL)7 Instituto de Física Corpuscular (CSIC-Universitat de València)8 Earthquake Research Institute (ERI), University of Tokyo9 Institute of Particle and Nuclear Studies, KEK, Japan10 Department of Physics, University of Tokyo11 Usu Volcano Laboratory, Hokkaido University
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- INFN (Napoli): simulazioni Monte Carlo; messa in opera e operazionedel telescopio 1m2; progetto, costruzione, messa in opera e operazionedei telescopi MU-RAY; analisi dati.
- Osservatorio Vesuviano: logistica, in collaborazione con Ente Parco;trasmissione e analisi dati; analisi dati e connessione con risultatiottenuti con tecniche geofisiche.
- Vulcanologi dell'Università Federico II e del Consorzio AMRA: analisidati e connessione con risultati ottenuti con tecniche geofisiche.
- Gruppi giapponesi: messa a disposizione e contributo a installazione emessa in opera del telescopio 1m2; collaborazione alla progettazione erealizzazione dei telescopi MU-RAY; analisi dati.
- Gruppi francesi: progettazione e realizzazione elettronica e DAQ deitelescopi MU-RAY; analisi dati.
- IFIC Valencia: contributo a simulazioni Monte Carlo.
Suddivisione dei compiti prevista
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Richieste finanziarie e di supporto tecnico
2009
M.I. Inst. telescopio 1m2; contatti per prototipi tel. “grande area” 10M.E. Contatti con coll. Giappone e Europa e per prod. scintillatori 5Consumo Inst. telescopio 1m2; prototipi tel. grande area 17 (3+14)Trasporti Telescopio 1m2 da Giappone; trasporti a Vesuvio 8Apparati Meccanica prototipi tel. grande area 5Totale 45
Officina Meccanica 4 m.u.Progettazione 2 m.u.Elettronica 3 m.u.
Profilo temporale
M.I. M.E. Cons. Trasp. App. Totale2009 10 5 17 8 5 452010 10 5 10 45 702011 8 5 10 5 28Totale 143
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Conclusioni
• Attività multidisciplinare di largo interesse anche al difuori degli ambienti scientifici• Grande aspettativa e forte coinvolgimento dei vulcanologi
• Collaborazione internazionale con forte motivazione espinta a fare
• Dopo il Giappone, prime misure in programma al Vesuvio ealle Antille con telescopi di basse prestazioni
• L’ambiente internazionale spinge a realizzare in tempistretti i telescopi MU-RAY
• L’INFN può avere un ruolo di grande rilievo
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INFN-Napoli (2009)
S. Buontempo Dir. Ric. Gr. II 20%C. De Moura Post Doc INFN Gr. IV 10%G. Iacobucci Primo Ric. Gr. I 20%G. Miele Prof. Ass. Gr. IV 10%O. Pisanti Ric. Gr. IV 10%P. Strolin (resp. naz. e locale) Prof. Ordinario Gr. II 50%M. Vassallo Ass. Ric. AMRA Gr. V 30%…… Ass. Ric. Univ. Gr. V 100%
Totale 2.5 FTE
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Cost estimate of one muon telescope
• Triangular scintillators (~80 kg/plane) 3• Fibre system (as in OPERA) 3• Multianode PMTs (8 ) 16• Assembly 20?• Electronics and DAQ (~7 euro/ch) 4• Mechanics 10?• Barrack 10?• Infrastructure (el. supply, data transm. …) 22
TOTAL 88 keuro
For 3D imaging at least 3 telescopes