Relazione A. Garfagnini - Gruppo 2 - INFN

Transcript

Un sommario personale sulla riunione della
Commissione Scientifica Nazionale II
Ferrara 15-19 Settembre 2014
A. Garfagnini
Padova University and INFN
30 Ottobre 2014
(INFN PD)
CdS-PD
30 Ottobre 2014
1 / 53
Esperiment WNEXT
Le nuove proposte
Nel pacchetto WHAT . . .
. . . e di Commissione
• JUNO
• LSPE
• QUAX
• FISH
• COSMO_WNEXT
(INFN PD)
CdS-PD
30 Ottobre 2014
2 / 53
Esperiment WNEXT
LSPE / SWIPE
•
•
•
•
•
Large-Scale Polarization Explorer e’ uno strumento dedicato alla misura della polarizzazione
del CMB a grande scala angolare and in particolare per la ricerca dei modi B previsti dal
modello inflazionario (Rif. Presentazione P. de Bernardis CSN2 Luglio 2104)
Due strumenti: STRIP (ricevitori coerenti a 44 e 90 GHz), SWIPE( bolometri TES in cavità
integratici multimodo da 90, 140, 220 GHz)
Risoluzione angolare: 1.5-2.3° FWHM
Copertura: 20-25% del cielo
Volo di lunga durata su pallone stratosferico: si sfrutta il vortice stratosferico polare invernale
per realizzare un volo circumpolare da 1 a 3 settimane. Base: Svalbard (ASI/Sapienza);
Palloni da 800000 m3 per carichi di 2.5 t a quote medie di 37 Km.
(INFN PD)
CdS-PD
30 Ottobre 2014
3 / 53
Esperiment WNEXT
LSPE/SWIPE
•
Progetto finanziato da ASI con 3,5 M! ( Criostato, Sistema Ottico, Rivelatori-Non
Bolometrici, Navicella, Controllo d’ Assetto, Processori di Bordo) a Sapienza, IASFINAF-Bologna, IFAC-CNR-Firenze, UniMI e Bicocca ( attività in corso da 2 anni),
con la PI-ship di P. de Bernardis.
•
Il volo non e’ stato ancora finanziato da ASI (circa 1.5 M!)
•
SWIPE (responsabile P. de Bernardis)
•
Il contributo INFN: “Bolometric Detection Chain” 1.5 M!
•
Ottica di piano focale (horn e cavita’) e test con calibratori (testbed) (Roma1)
•
Bolometri TES a grande area per 350 mK (Genova)
•
Elettronica di FE a SQUID (Genova)
•
Risuonatori LC superconduttivi (Pisa)
•
Elettronica per il Frequency Division Multiplexing e DAQ (Pisa)
•
Facility di integrazione e test dello strumento (Roma2)
(INFN PD)
CdS-PD
30 Ottobre 2014
4 / 53
Esperiment WNEXT
LSPE
ROMA1 GENOVA
GENOVA
PISA
PISA
(INFN PD)
16
CdS-PD
30 Ottobre 2014
5 / 53
Esperiment WNEXT
!"#$%&'%'()*+$,-./$0,-")&"&"$./1'23$
•  !"#$%"&'(&()*+",'-$)",("$.&+(-,",/$"*.-(#"$+$0,'(#"0(1&+-#2"
•  31$",(",/$"4(5(#"(6",/$")(+*'")7),$4"-#",/$"2*+*.78",/$"*.-(#"39"
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•  ;/$"="&&'8)92"65$<&)2(16'2$12$)$8)92"6>";$()8%*"$0*#"<$"$.0-,$:"
*#:",/1)""81<($815&'#)7"$%?'<'2($
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• 
• 
• 
• 
EF9F"G'*1))8"HF"9((:78"BF"@-+0I$0J8"3FKF"9(''-)8"LM&-#"0(1&+$:"*.-(#":$,$05(#)L8"NO;CPQRS!TTU"VWXQRY"
EF9F"G'*1))8"L!.-(#)"FF",/$")$*'0/"0(#5#1$)L8"=*+$"C'$&'-#,"=;C"QRPZW"VWXQRY"
AF"[*'<-$'-8"9F"\$':(#-(8"?F"B-('$#5#-8"MF"]-,*+$8"C/7)F"E$^F"["__U8"ZR`"VWXQXY""
!F>F"G*J/-I:$8">F"]F"G(+(J(+(a8"M(aF"C/7)F"HK;C"`_"RXQ"VWXXWY"
(INFN PD)
CdS-PD
30 Ottobre 2014
6 / 53
Esperiment WNEXT
!"#$%&'()*+%)*,-$
QUAX
•  !"#"$%&'()#)*"#+",,'-./0"12#3"4'0.02"#5+637#(04(8"#.#
-./0"19"8#:",,(-./0"12#-.)",(.&#
./#0!"#$,)1+(&(2)1$(04(8"#.#-./0"12#-"8(.#2.0#;"#)<0"8#
;=#.0#)3*),(&4$%&'()567('$8)49$.08#&("4#(0#)*"#%:45$;<6$
,&(')$5,.8('#:,"><"02=7#
=$>$$?@$AB$;<6$
(INFN PD)
CdS-PD
30 Ottobre 2014
7 / 53
Esperiment WNEXT
!"#"$%&'()$*"+"(
QUAX
•  !"#"$%&'()"*+&*,"-(.'(/(*,-*(.(
+,$/&012"(/")&'1#&/(
•  3"//,+1-'"%$(+1#"/,14()0/$"-(.'(
1'%'&5")(&+(#1"(*"2&'/#&*(
•  3"2&'/#&*(.'(/'(*&+&-"'&6)(
17,14(+1-'"%$(8"45(
•  9/:&-"',$():)#"+(#&(/4&.-(50/$6(
5&-7()1&#&'2(/'-(#&("'1/'$"(
)*&)"*%"2(&+(,/8'"%$(,/#"*./0(
•  ;&0('&,)"(5"#"$#&/($1/.'(
9:;/'#;,(0.,.#"-<=(
•  >/4.#7(#&("'*1'$"(<=>(
(INFN PD)
CdS-PD
30 Ottobre 2014
8 / 53
Esperiment WNEXT
FISH
Ultracold atoms: successful quantum simulators for
important cond-PDWSUREOHPV«
Quantum phase transitions
M. Greiner et al., Nature (2002)
Fermi-Hubbard model
R. Jördens et al., Nature (2008)
Disordered systems
G. Roati et al., Nature (2007)
Low-dim many-body physics
T. Kinoshita et al., Science (2004)
Quantum magnetism
J. Simon et al., Nature (2011)
Graphene physics
L. Tarruell et al., Nature (2012)
«DQGIRUIXQGDPHQWDOSK\VLFDOeffects
Fermionic superfluidity
M. Zwierlein et al., Nature (2005)
Higgs mechanism
M. Endres et al., Nature (2012)
SU(N) fermions
G. Pagano et al., Nat. Phys. (2014)
Kibble-Zureck mechanism
G. Lamporesi et al., Nat. Phys. (2014)
VR³ZKDWQH[W´"Ultralow-energy simulators of high-energy physics!!!
(INFN PD)
CdS-PD
30 Ottobre 2014
9 / 53
Esperiment WNEXT
Ultracold atoms: quantum engineering in a table-top setup
FISH
10 nK!
UNIFI
Many control knobs for realizing Hamiltonians in the lab!
fermions and bosons
interactions
dispersion (also relativistic)
temperature
topology / dimensionality
disorder
gauge fields
dynamics
I. Bloch et al., Rev. Mod. Phys. 80, 885 (2008)
M. Inguscio and L. Fallani, Atomic Physics (Oxford, 2013)
(INFN PD)
CdS-PD
30 Ottobre 2014
10 / 53
Esperiment WNEXT
FISH
Scientific goal of the FISh experiment:
engineer the interactions in ultracold quantum gases in order to realize
quantum simulators for some aspects of high-energy physics,
connected to the colour symmetry and to the quark confinement in QCD

strong interconnections between HEP and atomic physics

highly-innovative project

ambitious goal, with a lot of interesting physics at hand on the way
Disclaimer:
We don't (and cannot!) promise to perform a full quantum simulation of QCD
We plan to realize certain simplified models to make cold atoms behave as quark matter,
to learn something new about basic phenomenology of QCD.
(INFN PD)
CdS-PD
30 Ottobre 2014
11 / 53
Esperiment WNEXT
Firenze
Leonardo Fallani
TIFPA
Multi-component fermions
with SU(N)-symmetric interactions
FI
Trento
Gabriele Ferrari
Topological defects in BECs
Simulation of quark confinement
(INFN PD)
CdS-PD
30 Ottobre 2014
12 / 53
Esperiment WNEXT
!"#$%
EUCLID
$&#'()%
*+(&,-%
•  =>?@)54#ABCD#=,=CEF#G'#&'#H'?54(4/4'%4/#I&J#
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•  R4&OH54#S2!#IG%Q#9"9T#4K#O4'OGM0G%J3#S'! IG%Q#9"6#O4'OGM0G%J#
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(INFN PD)
+,-,*1)2"#++3#-455&5&#6789:8;96<#
CdS-PD
;#
30 Ottobre 2014
13 / 53
Esperiment WNEXT
EUCLID
$%4U&')*>VRN'NWXVSO*;96<*1$,;#
! !"#$%&'%(%)(*+,%-&,./%$01213,2,*%4%#.&2),''%#5,62*1+*(50%789:;<98=µ3%%
!  9"==>4?;@#AB$$#C#6D9E?#@#.FGHI#C#;99G@#JH!HAHJIK#C#;<9#LMN%8/&O@#
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!";IJ% %
%A%>521%?,60(B&6(.%@'',3C.D%&B%20,%'(2,..&2,%E1./%$(D)1(/%?1/F.,%
%A%G,2,6H1B%#D'2,3%31FB2,/%1B%!";>?@%
%A%I(*3%J.,62*1B&6'%&B%20,%K(*3%'(2,..&2,%#,*L&6,%?1/F.,#
I(*3%#,*L&6,%?1/F.,%
(INFN PD)
!"#$%&'()#*#+,-,#.&/)0&#
CdS-PD
+,-,*1)2"#++3#-455&5&#6789:8;96<#
30 Ottobre 2014
6=#14 / 53
Esperiment WNEXT
EUCLID
$%4>&')*?@AB'BCD@EF*;96<*1$,;#
Individuate alcune aree per un possibile contributo INFN
nell’ambito delle responsabilità italiane in Euclid
–  integrazione SW di bordo nell’HW delle unità di qualifica e di volo per
Data Processing Unit (DPU) e per Instrument Control Unit (ICU) del
Near Infrared Spectro-Photometer (NISP)
–  integrazione e test delle unità di warm electronics di NISP con
qualifica funzionale e verifica delle performance presso laboratori
INFN
–  contributo alle attività di sviluppo del SW di bordo
–  attività di system engineering della warm electronics del NISP
–  possibile contributo al Science Ground Segment con la partecipazione
allo sviluppo degli algoritmi di riduzione e analisi dati
e contributo alla gestione dei dati.
(INFN PD)
CdS-PD
30 Ottobre 2014
15 / 53
Experimental site
Esperiment WNEXT
JUNO
11
(INFN PD)
CdS-PD
30 Ottobre 2014
16 / 53
Esperiment WNEXT
Spectral information
JUNO
How the interference happens?
Fourier transform to L/E spectrum:
L/E spectrumÅÆǻm2
spectrum(oscillation frequency)
J. Learned et. al. hep-ex/0612022
L. Zhan et. al. 0807.3203
5
(INFN PD)
CdS-PD
30 Ottobre 2014
17 / 53
Esperiment WNEXT
Observatory of astrophysical sources
JUNO
9
(INFN PD)
CdS-PD
30 Ottobre 2014
18 / 53
Esperiment WNEXT
Detector concept
JUNO
Requirements:
Large detector: 20 kt LS
Energy resolution:
3%/E Æ 1200 p.e./MeV
12
(INFN PD)
CdS-PD
30 Ottobre 2014
19 / 53
Esperiment WNEXT
Collaboration Established
19
(INFN PD)
CdS-PD
JUNO
30 Ottobre 2014
20 / 53
Esperiment WNEXT
Liquid scintillator
16
(INFN PD)
CdS-PD
JUNO
30 Ottobre 2014
21 / 53
Esperiment WNEXT
Veto system
14
(INFN PD)
JUNO
CdS-PD
30 Ottobre 2014
22 / 53
Esperiment WNEXT
Notizie recenti sugli esperimenti WNEXT
QUAX
LSPE
Il progetto è approvato dalla Giunta con un
finanziamento aggiuntivo di 213 kEuro per il 2015.
Questi fondi saranno messi a disposizione a
Novembre 2014 e sranno assegnati a QUAX in
quella data. Se la fase di R/D proposta dai
referees avrà esito positivo, la Giunta coprirà le
spese di costruzione per gli anni successivi
Il progetto è approvato dalla Giunta con un
finanziamento aggiuntivo di 447 kEuro per il 2015.
Questi fondi, già assegnati in commissione,
saranno messi a disposizione a Novembre 2014.
La Giunta si impegna a coprire le spese di
costruzione per i prossimi anni.
FISH
COSMO_WNEXT
Il progetto recentemente discusso con la Giunta,
(non ragioni scientifiche) per la necessità di
aumentare l’impegno in termini di FTE e definire
un accordo con ASI e INAF. La discussione è in
corso e molto probabilmente il progetto sarà
finanziato dalla Giunta per il 2015. La cifra precisa
non è ancora disponibile ma si pensa che coprirà
la proposta dei referees per il 2015 e le spese di
costruzione per i prossimi anni.
(INFN PD)
Il progetto ha referee della CSNI e CSNII. Giudizio
pienamente positivo da parte dei referee; la CSNII
aveva deciso un approfondimento, per verificare la
tempistica dei risultati. INFN ritiene strategica
l’approvazione di FISH in tempi rapidi. La Giunta
INFN mette a disposizione la cifra di 364 kEuro
proposta da referee e si impegna a coprire le
spese di costruzione per i prossimi anni.
CdS-PD
30 Ottobre 2014
23 / 53
fisica dei neutrini
Fisica delle oscillazioni dei neutrini
Esperimenti in presa dati
• T2K
R&D, nuove proposte, ed exp in
costruzione
• KM3
• ICARUS@CERN
• LVD
• NESSIE
• BOREX
• BOREX-SOX
Esperimenti in chiusura
• ICARUS@LNGS
• OPERA
(INFN PD)
CdS-PD
30 Ottobre 2014
24 / 53
!"#$%&'()&'(*+$",-./",-0$
fisica dei neutrini
(INFN PD)
CdS-PD
30 Ottobre 2014
25 / 53
!"#$%&'(&)(*+,(Æ(*-.%$&(*+/,(
fisica dei neutrini
(0-1)2%3)-4)5(
• %61%()41'47)1%·!+89:(
• 0)7;$%(&)("$'<)7)-4'(&)(7'3)-4)(G·XUWR(
• 0)7;$'((&)(7'3)-4'(G·XUWR(()4(%<=;%(((
(
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• O-4&$%(D)<'E?$'(+89P(
• INQA(M);#4-(+89R(
(INFN PD)
CdS-PD
30 Ottobre 2014
26 / 53
fisica dei neutrini
!"#$%&'$"($)*+,)-(),$%+.&#",+)&)/)01)
23+)GHWHFWRUDWPGRQ·WXVHWKHVDPH
T2K
#+43("."56)&(7)#&,5+#)&8)9:)
23+);.-<)8++()&#)/=>1)$8)("#)#3+)8&1+)&8)#3&#)8++()
?6)9:@))
A()&77$#$"()#3+)*"",)0("B.+75+)";)#3+)(+-#,$(")
4,"88)8+4#$"()$()B&#+,),+*,+8+(#)"(+)";)#3+).&,5+8#)
-(4+,#&$(#$+8)";)#3+)2/:)1+&8-,+1+(#@))
)
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,$4"8#,-'$"(+)7&#$)*+,)I-+8#")7+#+4#",)J,$43$+8#+)4&.4"."K))

(INFN PD)
CdS-PD
30 Ottobre 2014
27 / 53
fisica dei neutrini
Detection principle
Search for neutrino induced
events, mainly vµ N ! µ X , deep
underwater
Down-going ! from atm. showers
S/N ~ 10-6 at 3500m w.e. depth
p, nuclei
KM3
E!-3
-  Atmospheric neutrino flux ~
-  Neutrino flux from cosmic sources ~ E!-2
!  Search for neutrinos with E!>1÷10 TeV
-  ~TeV muons propagate in water for several km
before being stopped
•  go deep to reduce down-going atmospheric ! backg.
•  long ! tracks allow good angular reconstruction
0.7°
E " [TeV ]
For E " # 1TeV $ µ" ~
! direction reconstructed from the
arrival time of Cherenkov photons on
Neutrinos from cosmic sources the Optical Modules: needed good
induce 1-100 muon evts/y
measurement of PMT hits, "(t)~1ns,
3
in a km Neutrino Telescope and good knowledge of PMT positions
(" ~10cm)
Cherenkov
Neutrino
Telescope
!
p, nuclei
Up-going ! from neutrinos
generated in atm. showers
S/N ~ 10-4
< 0.1°
charge current
interactions
43°
!
water/ice
rock
Antonio Capone
(INFN PD)
Km3 - presentazioneCdS-PD
richieste 2015 alla CSN2 - Ferrara, 16/09/2014
30 Ottobre 2014
6
28 / 53
fisica dei neutrini
March 2013-August 2014 - NEMO-Phase2 Tower
Since May 8th 2014:
Prototype KM3NeT detection
unit with 3 DOMs
Antonio Capone
Km3 - presentazione richieste 2015 alla CSN2 - Ferrara, 16/09/2014
(INFN PD)
CdS-PD
30 Ottobre 2014
15
29 / 53
fisica dei neutrini
N.#,7"O(P,9,6#(AQ((
!"#"$%&'(&)(#*"(++(),'-./"'#.0(1,2(34"(&56"78"(
#*"("'9:'"(&)(#*"(;,'(.#(4&7<=>(+&66:50"(#*.'<6(#&(
#*"(8"7?(6#.50"(.'-($0".'(-.#.(.$$,/,0.#"-(:'(#*"(
@76#(A(?".76(&)(#*"(B&7"2:'&(C*.6"DEE(-.#.(#.<:'9(
E77"-,$:50"(5.$<97&,'-(#&($&+"(4:#*(F(GHI(.'-(:#6((
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'7%$*8/6'()'9)&0$)($+&*"('%)9*'.)&0$):$1)9+%"'()
*$/26'();0"20)-';$*%)&0$)<+((
(INFN PD)
CdS-PD
30 Ottobre 2014
30 / 53
fisica dei neutrini
!"#$%&#'(#)$*+',%"+'$)-%.)*/0#'
'(.1$*#(''2'13-)"#'
4#5%6-#$7'",.'(.1$*#(',#$#'*.6(%-#$#-'
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5.6"+(7'
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.1$'3)3#$'QRST'UV'JWU;XK'UXV'K')'
*.6*$#"#'3&)6'
(INFN PD)
CdS-PD
30 Ottobre 2014
31 / 53
fisica dei neutrini
!"#$%%&'
BOREX
()'*+)'%"#$,-,-.'*'.$%/*$'0%+)1,-%'2+%.+*3'*4)+'#5)')-6'%7'25*8)'99'7%+'*66,:%-*$'
#5+));7%"+'<)*+8'
=,$$*+8'%7'#5)'2$*-'/),-.'8&)#>5)6?''@!A;B'CD5+%3,"3'E''*-6'@!A;0'CD)+,"3E'
2+%F)>#8G'*-6'*'#5%+%".5'2"+,H>*:%-'>*32*,.-'#*+.)#)6'#%'8"22+)88'#5)'IJK0,'#%'
#5)'-).$,.,/$)'$)L)$'CL)+<'>$%8)'#%'KE'!'!"#$%&'()*&!+)&,)!)-.!+)/01)
".!('-.".234)!25)2&3))&2+6)!2)'77.-)+$"$3)8)39$():&'+5)#.)39.)'+%"!3.)(&+!-)
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M5+%".5%"#'#5)')-:+)'2)+,%6'%7',#8'+)3*,-,-.'$,7):3)G'0%+)1,-%'N,$$'>%-:-")'#%'
/)'*'2%N)+7"$'8"2)+-%L*'%/8)+L*#%+<O'
M,3,-.'8>)-*+,%?'@!A;0'7+%3'P%L)3/)+'IKJQ'CJOQ'<)*+8'%7'6*#*'#*&,-.E';'
2"+,H>*:%-'>*32*,.-'7"$$<'>%32*:/$)'N,#5'@!A;0'R'$*#)+'@!A;B'
S%T'/)#N))-'9PUP'*-6'DVB'@*>$*<'7%+'@!A;0'CD)+,"3E'C'-%N'>*$$)6'@!A;D)E'
*$3%8#'>%32$)#)6''
(INFN PD)
CdS-PD
30 Ottobre 2014
32 / 53
fisica dei neutrini
NESSiE
Summary
-  CERN and USA, following the outcomes by ESP (European Strategy)
and P5 (strategy in USA), agreed to make R&D for neutrino at CERN
and experiments at FNAL
-  NESSiE Collaboration has submitted a Technical Report to CERN-SPSC
and a Physics Proposal to FNAL (PAC, Physics Advisory Committee,
number P-1057)
-  FNAL is undergoing a strategic plan for the Short-Baseline projects
-  Our FNAL proposal will be scrutinized in autumn
-  The CERN Neutrino Platform has been approved and funded
at the last CERN Council (5% of CERN budget for research)
-  The approved experiments WA104-Icarus, WA104-NESSiE and WA105
are expecting to have their own MoU released soon
CSN2-NESSiE, September 15th 2014
Luca Stanco for the NESSiE Collaboration
(INFN PD)
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fisica dei neutrini
Prospects for the measurement of!
!µ disappearance at the FNAL-Booster!
NESSIE
(INFN PD)
CdS-PD
FNAL-P-1057 and arXiv:1404.2521
!""#$%&'!%()'
!"#$%&'()*+),-./01.23)
The NESSiE Collaboration!
30 Ottobre 2014
5
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fisica dei neutrini
SBL at the FNAL ~ 0.8 GeV Q Booster Beam
7(89:;;4<(=>?@9(
=>@>3@4#8A(
)*"+,-(./00(
123#4544&6(
!"#$%&'(
ȹ"(B42C@()*"+,-D!"#$%&'D123#4544&6(>EE4#@(28(@:F2CG(?;:3>(@4(=>H>;4?I((
¾ "(349>#>C@(2C@>#C:@24C:;(?#4G#:J(E>:@K#2CG(7(=>@>3@4#8(:@(=2EE>#>C@(L:8>;2C>8(
LM(N0$OI((C>:#I(!"#$%&'P(J2=I(123#4544&6P(E:#I()*"+,-Q((
¾ "(34JJ4C(*4C3>?@K:;('>82GC(+>?4#@(=283K882CG(348J23(#:M(2C=K3>=(L:3FG#4KC=P(
L>:JD=>@>3@4#(8M8@>J:@238(:C=(;4G28@238R(
ICARUS presentation at CSN2, 09/2014
(INFN PD)
Slide# : 16
CdS-PD
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Dark Matter and DBD
Double Beta Decay and Dark Matter searches
R&D e nuove proposte
• CUORE
• DARKSIDE
• GERDA
• LUCIFER
• DAMA
• MARE-RD
• XENON
• SABRE
• MOSCA-B
(INFN PD)
CdS-PD
30 Ottobre 2014
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Dark Matter and DBD
CUORE-0
1 CUORE tower
• 52 TeO2 5x5x5 cm3 bolometers
• 13 floors of 4 crystals each
• total mass: 39 kg (11 kg of 130Te)
• All detector components manufactured, cleaned and stored
with same protocols defined for CUORE
• Assembled with the same procedures of CUORE:
- dedicated class 1000 clean room (underground building)
- all steps of the assembly (crystal gluing, mounting,
•
•
cabling, bonding) performed under nitrogen inside
special glove boxes.
Operated inside the 25-year-old Cuoricino cryostat at
LNGS.
Low temperature roman lead shield
Goals:
• Proof of concept of CUORE detector in all stages
• Test and debug of the CUORE tower assembly line
• Test of the CUORE DAQ and analysis framework
• Operating as independent experiment while CUORE
is under construction
• Demonstrate potential for DM detection
!"#$%&'(%)*+,+-*.(*'(%+/*+0*12(3*'+#456+,+7%$$2$2+89:;<:6;8=+
(INFN PD)
CdS-PD
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Dark Matter and DBD
CUORE-0 data taking
• August 2012: base T reached
18
5
16
4
14
12
Phase I
Run Time Efficiency: 69%
Live Time Efficiency: 43%
10
3
8
May
Accidental Warmup
June
July
2013
August
September
Cryostat Maintenance
October
November
Trap Cleaning
+ Noise Optimization
December
January
February
2014
March
Accidental
Warmup
Trap
Cleaning
April
May
- Background measurements
- Calibration runs
2
Phase II
Run Time Efficiency: 80%
Live Time Efficiency: 61%
6
Calibration Problems
April
Isotope Exposure [130Te kg!yr]
Exposure [kg!yr]
•
•
•
•
March
... problems with old Cuoricino cryostat
March 2013: start data taking (Phase I)
September 2013: first results are released (! arXiv:1402.0922)
October 2013: long maintenance stop
November 2013: background data taking restarted (Phase II)
! improved conditions
• Longer system lifetime (no warm-up required so far)
• Better noise conditions
• Improved energy resolution
• Lower Threshold
• Data analysis tools optimization
valuesExposure
Cuore-0
• Stable background
4
1
2
0
Mar-13
May-13
Jul-13
Aug-13
Oct-13
Dec-13
Mar-14
0
May-14
Time
June 2, 2014
!"#$%&'(%)*+,+-*.(*'(%+/*+0*12(3*'+#456+,+7%$$2$2+89:;<:6;8=+
(INFN PD)
CdS-PD
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Dark Matter and DBD
CUORE-0 background
Event Rate [counts/keV/kg/y]
!/" region
# region
CUORE-0 Preliminary
10
Cuoricino
CUORE-0
210Po
Exposure: 18.1 kg ⋅ yr
190Pt
1
10
10
-1
Q!! = 2528 keV
-2
1000
2000
3000
4000
5000
6000
7000
Energy [keV]
• Cuoricino background model confirmed:
- environmental gamma’s from material bulk
contaminations
0!"" region
cnts/(keV kg y)
2700-3900 keV
#(%)
Cuoricino
0.153 ± 0.006
0.110 ± 0.001
83
CUORE-0
0.063 ± 0.006
0.020 ± 0.001
78
- surface radioactive contaminations of close
materials
• Evident reduction with respect to Cuoricino
- factor of 6 for surface contaminations
- factor ~2.5 in the ROI
!"#$%&'(%)*+,+-*.(*'(%+/*+0*12(3*'+#456+,+7%$$2$2+89:;<:6;8=+
(INFN PD)
CdS-PD
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/ 53
Dark Matter and DBD
Status of CUORE: cryogenics
Phased commissioning program
! add complexity gradually
•
•
Phase 1: 4 K subsystem ! completed
- OVC and IVC vacuum tightness
- Cooldown to 4K
Phase 2: full system test ! ongoing
-
cryogenic system fully assembled ! new vacuum check
Run I: first cool-downs with no additional load:
! initial problems (reached 14 mK in cooldown 1&2)
! recent successful cooldown: T below 10 mK !
next steps:
- Run II:
- wiring system (and test detector)
- Run III:
- Cold Pb shield + FCS
- DCS + Suspensions
- Towers support plate
top cold lead
• T Cold Plate
• 30 cm thick
lateral roman lead
• T=4K
• 6 cm thick
Expected completion:
! spring 2015
!"#$%&'(%)*+,+-*.(*'(%+/*+0*12(3*'+#456+,+7%$$2$2+89:;<:6;8=+
(INFN PD)
CdS-PD
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/ 53
Dark Matter and DBD
XENON program!
XENON10!
2005-2007!
15 cm drift TPC – 25 kg!
!
Achieved (2007)!
"SI = 8.8 x 10-44 cm2!
XENON100!
XENON1T / XENONnT!
2008-2015!
30 cm drift TPC – 161 kg!
!
Achieved (2011)!
"SI = 7.0 x 10-45 cm2!
Achieved (2012)!
"SI = 2.0 x 10-45 cm2!
2012-2017 / 2017-2022!
100 cm drift TPC - 3300 kg / 7000 kg!
!
Projected (2017) / Projected (2022)!
-47
2
"SI = 2 x 10 cm / "SI = 3 x 10-48 cm2!
Commissione 2, Ferrara, 15 settembre 2014
(INFN PD)
CdS-PD
5
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Dark Matter and DBD
Background prediction from MC:!!"
Full Monte Carlo simulation in
GEANT4 of the Water Tank, Support
structure, Cryostat, TPC, PMTs.!
Gamma background:!
Single scatter, 1 ton fiducial volume, [2-12]
keVee, 99.75% S2/S1 discrimination.!
0.05 ev/y!
Mainly from the Cryostat (50%), PMTs
(30%) and TPC components (< 10%)!
Commissione 2, Ferrara, 15 settembre 2014
(INFN PD)
CdS-PD
33
30 Ottobre 2014
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Dark Matter and DBD
SABRE
Il Working Group
!  Interesse di gruppi di ricercatori teso alla
conferma della misura di DAMA/LIBRA
(DL).
!  Working group per attivita’ preliminare:
!  nasce da ricercatori di DarkSide:
!  Milano, Napoli, LNGS.
!  si aggiungono ricercatori ROMA1.
(INFN PD)
CdS-PD
30 Ottobre 2014
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Dark Matter and DBD
SABRE
Sodium iodide with Active Background REjection
Nasce in DarkSide. Goals:
!  Cristalli di NaI(Tl) con radiopurezza ! DL.
!  High-QE PMTs or SiPM -> soglia inferiore a DL.
!  Veto attivo di scint. liquido -> full tagging del 40K.
A Princeton R&D sulle polveri di NaI (ottimi risultati) e
processo di crescita del cristallo (risultati da valutare) con
aziende americane. Test dei primi cristalli nel veto di
DarkSide, esperimento finale indipendente.
(INFN PD)
CdS-PD
30 Ottobre 2014
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Astronomia gamma
Astronomia gamma
• AUGER
• JEM-EUSO-RD
• AGILE
• FERMI
• GAMMA-400-RD
• WIZARD
• AMS-2
• CTA-RD
• MAGIC
(INFN PD)
CdS-PD
30 Ottobre 2014
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Astronomia gamma
#$%"&#'"()*(%+,"-."+)//012%"3%/04*5"
6'7$$7:&;'32$"#<&29"#'
!'7==-&4:'>2?%$7@%'
()7%".77.8"
)**'+%,-)*'.%,'
㾃㻌㼪>!";"?"@!A",%2%/()+%/"
2)6"%*%748"/%(9)*"
!"#$%&#'(')*'+%,'
㾃㻌㼪㻌!:";"<"=",%2%/()+%/"
$04$"%*%748"/%(9)*"/0.%,1'
㾃㻌㻩㻌㻠㻙㻢㻌㼙㻌㻙㻌@AB"㻌,%2C"
23')*'456'7$%7'/829"#1'
'2%//.*37)"D%"'*4%20/"
(INFN PD)
CdS-PD
!"
30 Ottobre 2014
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Astronomia gamma
!"#$%&'()&$*+,,-).$*.)+%.+)($
(INFN PD)
CdS-PD
30 Ottobre 2014
47 / 53
Astronomia gamma
!"#$%&'()*+%#,-%.#"/#0/#)12%
•  !"#$%$&'()!*(+%,-./(
/%0%,,"#1(23(4"5-4-6%(27%(
.%34%2#-0(%80-%/01(
•  )#3+&0%+(9:()!*,(23(73'+("(
4"2#-5(3$(&;(23(<=(>?5?@(
A-)B(C44(5(C44(
•  D()!*(,%/2(23()E($3#(FGH(
,%/,3#(I3/+-/.(
•  3'%4*%56*)%7'+%
–  JAK(0'&,2%#(,2&+1(>,&4(0-#0&-2(3$(9<(
3#(<=@(
–  AAK(0"4%#"(+%43/,2#"23#(
*G0G%HI%J<K6%L%M%N%EO%P%M%N%Q%P%EI%6"90(*%
–  !7"#"02%#-6"L3/(,2&+-%,(
•  ,89%4*%"9:*+78;*)%:'%
–  !<$%;"+;5":%7'+%=!3%
–  #+*8>?("@*+%:*6:%
–  A*8)'5:%4'8+)%
•  ="0B:%%;'9;*9:+8:'+6%
C'+%!!3%.75((D2%.A$E/%3F2%
(INFN PD)
CdS-PD
30 Ottobre 2014
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Onde Gravitazionali e Meccanica Quantistica
Onde gravitazionali
• AURIGA
• NAUTILUS
• ADV-VIRGO
• LISA-PF
• VIRGO
• RARENOISE
• GGG
• MOONLIGHT-2
• G-GRANSASSO
• PVLAS
• LARASE
• MAGIA
• MICRA
• HUMOR
• MIR
(INFN PD)
CdS-PD
30 Ottobre 2014
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Last news
Renewal of the MoU between LIGO and Virgo
(1 April 2014 ± 31 March 2017)
±
±
data exchange
Source localization
Election of the new spokesperson (F. Ricci)
(on duty since May 2014)
Election of the new DA coordinator and of the Physics
group coordinators
Kick-off of the AdV squeezing group
(Chairs: J.-P. Zendri, P.F. Cohadon)
(INFN PD)
CdS-PD
30 Ottobre 2014
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Bench SIB1 (with dihedron) suspended
IMC ready for light
September 15, 2014
(INFN PD)
CSN2 Ferrara
CdS-PD
30 Ottobre 2014
10
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MIRRORS
First large optics polished (BS, PRs, CPs, POP, IM, EM)
PR
BS
September (INFN
15, 2014
PD)
CSN2
Ferrara
CdS-PD
30 Ottobre 2014
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VIRGO
Commissioning start and future steps
July 2014: commissioning of IMC ***started
October 2104: SIB2 installed, finish commissioning of
INJ
Early 2015: mirrors in the central building installed
lock of the CIFT
Summer 2015: first end mirror installed
1-arm test
Fall 2015: full interferometer
lock in the power
recycling configuration
2016: commissioning of the full interferometer
noise
hunting and science run
September
(INFN PD)15, 2014
CSN2 Ferrara
CdS-PD
30 Ottobre 201424
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