Verso l’apertura di una sigla SHIP per 2015!
Walter M. Bonivento CERN/INFN Cagliari
!
CNS1 Elba 20/05/2014
CERN, Universität Zürich, EPFL Lausanne, INFN Cagliari, Università Federico II and INFN Napoli, Imperial College London
(in forte crescita)
(segue presentazione CNS1 6/2)
Walter M. Bonivento - CERN/INFN Cagliari CNS1 Elba 20/05/2104
Cosa e’ SHIPSHIP e’ una proposta di esperimento di beam dump al SPS (400GeV p) del CERN !
Obiettivi (per ora…): !
A. rivelazione particelle a lunga vita media debolmente interagenti o sterili: sensibilità’ statistica rispetto a esperimenti precedenti dello stesso tipo x10000 !
B. rivelazione 𝜈𝝉 con sensibilità’ statistica rispetto a esperimenti precedenti x200
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Walter M. Bonivento - CERN/INFN Cagliari CNS1 Elba 20/05/2104
Δ(>>0!) rispetto al talk del 6/2 (i)
• Estensione del programma di Fisica!
• Manifestazione di interesse di altri gruppi italiani!
• contributi attivi su vari fronti per il TP!
• partecipazione ad apertura sigla a Settembre!
• Manifestazione di interesse di altri gruppi stranieri!
• Workshop di Zurigo 10-12 Giugno —>estensione della collaborazione
3
Walter M. Bonivento - CERN/INFN Cagliari CNS1 Elba 20/05/2104
Δ(>>0!) rispetto al talk del 6/2 (ii)
• Proposte dettagliate di alcune tecnologie di rivelatore —>quasi definizione di alcune; discussione approfondita su altre!
• Task force fascio e infrastrutture (nominata dal DG) !
• Studi con GEANT del filtro di muoni: confronto filtro attivo/filtro passivo!
• Definizione preliminare della schedule!
• Indicazione possibile esistenza di N dark matter in spettri X
4
Layout esperimento
Walter M. Bonivento - CERN/INFN Cagliari
lead/iron
tungsten
60m
magnet
5m
50m
5 CNS1 Elba 20/05/2104
x2p
rivelatore ντ
muon
UT+VETOECAL
tracking
Perche’ e’ importante il fattore 10000?
Walter M. Bonivento - CERN/INFN Cagliari 6 CNS1 Elba 20/05/2104
Walter M. Bonivento - CERN/INFN Cagliari 7 CNS1 Elba 20/05/2104
John Ellis, QFPP, CERN, 6/5/2014
Walter M. Bonivento - CERN/INFN Cagliari CNS1 Elba 20/05/2104
Una nuova idea: il 𝜈MSM! Premessa: Massa del Higgs misurata a ≈125 GeV —> SM teoria di campo effettiva, auto-consistente, debolmente accoppiata fino a grandi scale (almeno fino a 1010GeV, vedi Strumia, Giudice, Isidori ecc.)!
Oggetto: 𝜈MSM e’ un modello che estende lo SM, in modo minimale, cioe’ senza introdurre nuovi principi fisici (SUSY or ED) o nuove scale di energia (GU)!
Modo: 3 partner di Majorana (HNL), singoletti destrorsi e sterili dei neutrini ordinari con MN<MW!
Soluzione: In un particolare spazio dei parametri (N2 e N3 quasi degeneri e con m=O(GeV) e N1 disaccoppiato con m=O(keV) ) il 𝜈MSM risolve i tre problemi osservativi del MS: massa dei neutrini (see-saw), bariogenesi (via lepto-genesi) e materia oscura (N1)!!
8
long-awaited Higgs boson of the Standard Model (SM) [3]. This discovery implies that the Landaupole in the Higgs self-interaction is well above the quantum gravity scale MPl ' 1019 GeV (see, e.g.Ref. [4]). Moreover, within the SM, the vacuum is stable, or metastable with a lifetime exceeding thatof the Universe by many orders of magnitude [5]. Without the addition of any further new particles,the SM is therefore an entirely self-consistent, weakly-coupled, e↵ective field theory all the way up tothe Planck scale (see Refs. [5, 6] for a recent discussion).
Nevertheless, it is clear that the SM is incomplete. Besides a number of fine-tuning problems (such asthe hierarchy and strong CP problems), the SM is in conflict with the observations of non-zero neutrinomasses, the excess of matter over antimatter in the Universe, and the presence of non-baryonic darkmatter.
The most economical theory that can account simultaneously for neutrino masses and oscillations,baryogenesis, and dark matter, is the neutrino minimal Standard Model (⌫MSM) [7,8]. It predicts theexistence of three Heavy Neutral Leptons (HNL) and provides a guideline for the required experimentalsensitivity [9]. The search for these HNLs is the focus of the present proposal.
In addition to HNLs, the experiment will be sensitive to many other types of physics models thatproduce weakly interacting exotic particles with a subsequent decay inside the detector volume, seee.g. Refs. [10, 11, 12, 13, 14, 15]. Longer lifetimes and smaller couplings would be accessible comparedto analogous searches performed previously by the CHARM experiment [16].
In the remainder of this document the theoretical motivation for HNL searches is presented inSection 2 and the limits from previous experimental searches are then detailed in Section 3. Theproposed experimental set-up is presented in Section 4 and in Section 5 the background sources arediscussed, before the expected sensitivity is calculated in Section 6. The conclusions are presented inSection 7.
2 Theoretical motivation
In type-I seesaw models (for a review see Ref. [17]) the extension of the SM fermion sector by threeright-handed (Majorana) leptons, NI , where I = (1, 2, 3), makes the leptonic sector similar to thequark sector (see Fig. 1). Irrespective of their masses, these neutral leptons can explain the flavouroscillations of the active neutrinos. Four di↵erent domains of HNL mass, MN , are usually considered:
Left
Left
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4.2 GeV
-⅓
νeelectronneutrino
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neutrino
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-1 μmuon
105.7 MeV
-1 τtau
1.777 GeV
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± 1
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mass→
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Three Generations
of Matter (Fermions) spin ½
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of Matter (Fermions) spin ½
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N~10 keV
1 N~GeV
2 N~GeV
3
Figure 1: Particle content of the SM and its minimal extension in the neutrino sector. In the (left) SM theright-handed partners of neutrinos are absent. In the (right) ⌫MSM all fermions have both left- and right-handedcomponents and masses below the Fermi scale.
2
T.Asaka e M.Shaposhnikov, PLB620 (2005) 17
Walter M. Bonivento - CERN/INFN Cagliari CNS1 Elba 20/05/2104
!
• nel νMSM forti limitazioni nello spazio dei parametri (U2,m)!
• molte ricerche di HNL in passato ma, per m>mK, con sensibilità’ non di interesse cosmologico (es LHCb in decadimenti del B raggiunge U2≈10-4, arXiv:1401.5361)
• questa proposta: ricerca in decadimenti dei mesoni D (prodotti ad alta statistica nella collisione di p di 400 GeV su bersaglio fisso)!
• Considerati i fasci esistenti e possibili in un futuro non troppo remoto, questo e’ il migliore esperimento che possa sondare la regione di interesse cosmologico
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Future Hadron Collider meeting, CERN, February 6, 2014 R. Jacobsson
� Production in mixing with active neutrino from leptonic/semi-leptonic weak decays of charm mesons
• Total production depend on ଶ = σ κூ ଶூୀଵ,ଶκୀ,ఓ,ఛ
• Relation between ଶ,ఓ
ଶand ఛଶ depends on exact flavour mixing
Î For the sake of determining a search strategy, assume scenario with a predominant coupling to the muon flavour
� Production mechanism “probes” ఓଶ = σ ௩మ ഋ
మ
ೃమ
ூୀଶ,ଷ
Î Br(ܦ ՜ ) ~ 10 െ 10ଵଶ
12
ఓߥܪ
௦ܦ
ଶ,ଷ
ߤ
ఓߥܪ
ܦ
ଶ,ଷ
ߤ
ߨ
(arXiv:0705.1729)
Produzione di N2,3
Future Hadron Collider meeting, CERN, February 6, 2014 R. Jacobsson
1. See-saw: Lower limit on mixing angle with active neutrinos to produce oscillations and masses 2. BAU: Upper limit on mixing angle to guarantee out-of-equilibrium oscillations (Ȟேమ,య < H)
3. BBN: Decays of ଶ and ଷ must respect current abundances of light nuclei Î Limit on lifetime ேమ,య < 0.ͳݏ ( > (ܯ 3
4. Experimental: No observation so far Î Constraints 1-3 now indicate that previous searches were largely outside interesting parameter space
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gerarchia inversa di massa dei neutrini
Walter M. Bonivento - CERN/INFN Cagliari CNS1 Elba 20/05/2104
Decadimenti del N2,3• Accoppiamento HNL-ν attivo molto debole
—>N2,3 hanno vita media molto lunga
• distanze di decadimento O(km)!: per U2
μ=10-7, τN =1.8x10-5s
• Vari modi di decadimento : i BR’s dipendono dal mescolamento tra sapori
• Probabilità’ che N2,3 decada nel volume fiduciale dell’esperimento ∝Uμ
2
—> numero di eventi ∝Uμ4
10
—>aumento di sensibilita’ x10000 permette di accedere alla regione di interesse cosmologico!
Walter M. Bonivento - CERN/INFN Cagliari CNS1 Elba 20/05/2104
New!
Portali verso Hidden sectors!
!
!
Le particelle dello SM non sono sensibili direttamente all’interazione di gauge GD ma attraverso un mediatore: gli operatori SM di dimensione piu’ piccola sono detti “portali”!
recentemente si e’ rivitalizzata l’attenzione verso questo tipo di interazioni per spiegare alcune anomalie astrofisiche (e.g. aumento e+/e- con energia , concentrazione di linea a 511keV dal centro galattico), interpretate nel contesto di dark matter; il range di masse suggerito, da qualche MeV a qualche GeV, con 𝝉<1sec e 𝝉>100ns e’ peculiare per esperimenti fixed-target (PhysRevD.80.095024)!
In questo esperimento simile metodologia di esperimenti già effettuati come CHARM ma con molta maggiore statistica e/o con maggiore energia del fascio (es. rispetto a U70) —>stiamo studiando le sensibilita’ in SHIP
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The idea of the existence of a hidden gauge sector weakly coupled with the SM through some mixing mechanism dates back to the early 80’s. (see for instance P. Fayet Nucl. Phys. B 347 (1990) 743) It has nowadays been reproposed by several authors, as a possible explanation of recent puzzling astrophysical observations
3
Basically all of these models postulate the existence of a sort of “dark” or “hidden” world, sensitive to a specific new gauge interaction GD
SM particles are not charged under GD but, as specified above, can “feel” the new force because of mixing between it and the SM gauge interaction
Walter M. Bonivento - CERN/INFN Cagliari CNS1 Elba 20/05/2104
Portali et al.Higgs portal —>mediatore inflatone (scalare); produzione diretta o da decadimento mesone; decadimenti e+e-, μ+μ-; accoppiamenti rinormalizzabili (μ𝜒+λ𝜒2)H+H!
Neutrino portal ->mediatore HNL, di cui sopra!
Vector portal —> mediatore para-fotone; produzione in mixing con fotoni; decadimenti e+e-, μ+μ-; accoppiamenti rinormalizzabili ϵFμ𝛎F’μ𝛎!
axion portal —> mediatore PNGB o axion-like particles (in questo caso non sono Dark Matter particles); produzione diretta mixing con π0; decadimenti e+e-, μ+μ-!
Anche sotto studio low-energy SUSY:!
! !
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New!
Walter M. Bonivento - CERN/INFN Cagliari CNS1 Elba 20/05/2104
Soppressione fondiInterazioni di neutrini muonici e di muoni non soppressi dal filtro!
1. nel tunnel di decadimento—>vuoto!
2. nell’ultima lunghezza di interazione del dump ->produzione di K0L—>μπν (eπν) !
—>rigettate da tagli cinematica sul parametro di impatto e p +muon ID e electron ID per canali Hidden sector!
inoltre un altro fattore 10-40 si puo’ ottenere equipaggiando l’ultima parte del dump con un rivelatore attivo per “taggare” le interazioni di neutrino —> ANCORA DA TROVARE CHI SE NE OCCUPA!
in ogni caso e’ importante sopprimere il K0L anche sopra 500MeV perche’ non sappiamo ancora come e se riusciremo a tenere sotto controllo le code non gaussiane della risoluzione in impulso!
Combinazioni casuali di due muoni dal PV —> risoluzione temporale spinta di almeno un rivelatore e alta efficienza del VETO cruciali (sotto studio)
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Walter M. Bonivento - CERN/INFN Cagliari CNS1 Elba 20/05/2104
Sensibilita’per HNLAssumendo 0 fondo (che pare ben giustificato dai nostri studi, ma sara’ comunque l’oggetto di simulazioni molto dettagliate) e 2x1020p.o.t. !
—> finestra di opportunità’ per questo esperimento di sondare la zona di interesse cosmologico
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solo con N—>μπ(in uno scenario in cui l’accoppiamento !
al sapore muonico e’ dominante)
BBN
(gerarchia di massa dei neutrini attivi inversa)
/CHARM
Walter M. Bonivento - CERN/INFN Cagliari CNS1 Elba 20/05/2104
Sensibilita’ per Hidden Photon
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con canali e+e- e μ+μ-
VERY PRELIMINARY E UNOFFICIAL
New!
Walter M. Bonivento - CERN/INFN Cagliari CNS1 Elba 20/05/2104
Fisica dei neutrini attivi: 𝛎𝝉 e 𝛎μApprofittando del beam dump, con un rivelatore dedicato che prende dati simultaneamente a quello per HNL, e’ possibile lo studio di interazioni del neutrino 𝝉 con statistica >200x attuale:!
• l’esperimento DONUT ha osservato 9 eventi (da charm) con 1.5 stimato di fondo!
• l’esperimento OPERA ha osservato 4 eventi (da oscillazione)!
In generale la terza generazione di leptoni puo’ essere piu’ sensibile a NF per la sua maggiore massa !
Inoltre la NF nel settore del 𝝉 e’ sperimentalmente limitata con minore precisione rispetto alle altre due famiglie. !
In particolare due “anomalie” sperimentali (su 3) nella fisica del charged flavor coinvolgono il 𝝉:!
A. ! R(D), R(D*) dalle B factories —>3.4𝝈 dal MS!
B. A(CP) (𝝉—>πK0
S𝛎𝝉) —>2.8𝝈 dal MS
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Walter M. Bonivento - CERN/INFN Cagliari CNS1 Elba 20/05/2104
Fisica dei neutrini attivi: 𝛎𝝉 e 𝛎μ—> Misure di sezioni d’urto e distribuzioni angolari nelle interazioni CC: stiamo studiando con i teorici (Datta, U.Massachussets) la sensibilita’ a Higgs carico, W’ e Leptoquarks!
Altre misure importanti:!
A. osservazione di anti-ντ (unica particella del MS non ancora osservata)!
B. produzione di charm in interazioni di νμ (grande aumento di statistica, >100x, rispetto a CHORUS in particolare per anti-νμ, : infatti in beam dump anti-νμ/νμ 60%)!
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Walter M. Bonivento - CERN/INFN Cagliari CNS1 Elba 20/05/2104
Bersaglio e filtro per muoni!
!
!
!
!• Bersaglio di W (50cm-1m) : il fascio va allargato e/o diluito sul bersaglio per evitare fusione,
seguito da assorbitore adroni e un filtro per muoni con due opzioni allo studio!
• Problema non banale perche’ il flusso di muoni e’ enorme: 1011/SPS-spill(5×1013 pot); !
• per ora la baseline per l’estrazione e’ 1sec (CNGS 10μs)!
• sicuramente il problema tecnico piu’ difficile dell’esperimento!
• Problemi radiologici sotto controllo con la costruzione di un target bunker e con circuito di raffreddamento chiuso
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target Experimentmop−up shieldingabsorberhadron
muon shield (U / W)beam
(detector, fiducial volume)
~ 3m ~ 52m~ 1m ~ 1m~ 0.5m
wall / earth
Figure 7: Schematic view of the target, hadron absorber and muon shield in front of the experiment. The totallength from the target to the entrance of the fiducial volume is ⇠ 60 m.
4.2 Detector
The detector consists of a long decay volume followed by a spectrometer. For a given detector length,the detector diameter should be maximised. In the discussion below the 5 m aperture of the LHCbspectrometer [59] is taken as a realistic scale.
Figure 8 shows a scan of the length of the detector for both a single detector element and fortwo longitudinally arranged detector elements. For a given HNL lifetime and detector aperture, thenumber of HNLs decaying in the apparatus with the decay products going through the spectrometersaturates as a function of the length of the detector. The use of two magnetic spectrometers increasesthe geometric acceptance by 70% compared to a single element. Therefore, the proposed detectorwill have two almost identical detector elements as depicted in Fig. 9. A diagram of a single detectorelement is also shown in Fig. 10.
To reduce to a negligible level the background caused by interactions of neutrinos with the remainingair inside the decay volume, a pressure of less than ⇠ 10�2 mbar will be required (see Section 5). Eachdetector element therefore consists of a ⇠50 m long cylindrical vacuum vessel of 5m diameter. The first⇠ 40 m constitute the decay volume and the subsequent 10 m are used for the magnetic spectrometer.The combined calorimeter and muon detector have a length of 2 m.
The magnetic spectrometer includes a 4 m long dipole magnet, two tracking layers upstream of themagnet, and two tracking layers downstream of the magnet (see Fig. 9). For the required level ofvacuum, the tracking chamber thickness and resolution are matched to give a similar contributionto the overall spectrometer resolution (see Fig. 11). Using straw tubes with ⇠120 µm resolution andwith 0.5% X/X
0
, like those presently being produced for the NA62 experiment [60], simulation studiesindicate that 2.5m is required between tracking chambers, giving ⇠ 10 m length for each magneticspectrometer.
An electromagnetic calorimeter is located behind each vacuum vessel for ⇡0 reconstruction andlepton identification. The calorimeter material is also part of the muon filter for the muon detector,which consists of an iron wall followed by a tracking station. An additional tracking station at thebeginning of each decay vessel will be used to veto charged particles entering the fiducial volume.These stations will also reject upstream neutrino interactions.
For a mass MN = 1 GeV, 75% of the µ�⇡+ decay products have both tracks with momentump < 20 GeV. The momentum and hence mass resolution scales with the integrated field of the magnets.
11
Walter M. Bonivento - CERN/INFN Cagliari CNS1 Elba 20/05/2104
Filtro passivo!
!
• Simulazione con PYTHIA8/GEANT4!
• Un cono di solo W troppo caro
• Miglior compromesso: nocciolo di W 250t di 40m (10M€ x costo al Kg/40€) circondato da Pb (2500t); totale 70m (100t di W per totale 60m per ottimizzazione costi)
• dopo 40m lo scattering multiplo e’ così grande che non vale la pena di continuare con un nocciolo di W
• rate di muoni stimato sullo spettrometro: 25k/spill da 5e13 (x10 con 100t)19
New!
Walter M. Bonivento - CERN/INFN Cagliari 20 CNS1 Elba 20/05/2104
New!
Walter M. Bonivento - CERN/INFN Cagliari CNS1 Elba 20/05/2104
Rivelatori et al.• Quasi nessun R&D da fare, per ora non e’ emerso nessun parametro che
necessiti di un “nuovo” rivelatore: ce la possiamo fare con rivelatori già costruiti in passato, ottimizzando i parametri—> questo significa che dall’approvazione si puo’ iniziare subito a costruire il rivelatore!
• Rivelatore di Muoni. varie opzioni allo studio:!
• RPC di nuova generazione.!
• RPC ricuperate da OPERA!
• Scintillatori con fibre WLS e lettura SiPM (FNAL/NICADD) !
• HCAL!
• trigger e acquisizione dati: pensiamo di utilizzare il modello HLT dell’upgrade di LHCb (i.e. no L0)
• computing: FairRoot framework (F.Rademacher)
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Walter M. Bonivento - CERN/INFN Cagliari CNS1 Elba 20/05/2104
Un possibile calorimetro!
!
!
• Il calorimetro Shashlik a spirale proposto dal gruppo di IHEP Protvino (non ancora ufficialmente membro di SHIP)
• Uniformita’ qualche %, risoluzione temporale σ∼1ns quale σ(E)/E=6.5%/√E⊕1%
• con possibilmente un pre-shower per distinguere γ da π0
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New!
Walter M. Bonivento - CERN/INFN Cagliari CNS1 Elba 20/05/2104
Tracking e VETOStraw tubes simili a NA62 con
risoluzione spaziale di 120 μm, 0.5% X0/X Risoluzione in impulso ottenuta nel nostro caso
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Principali differenze con NA62: A. 5m di lunghezza !B. vuoto 10-2 mbar C. 2kHz/straw di 1cm di diam D. configurazione X,X-θ,X+θ,X
con θ piccolo
possibile sinergia su vari fronti con NA62
Walter M. Bonivento - CERN/INFN Cagliari CNS1 Elba 20/05/2104
Rivelatore per 𝛎Rivelatore a emulsioni con la tecnologia di OPERA ma con massa molto minore (750 mattoni) molto compatto (2m) posto davanti al tunnel di decadimento per il HNL —>immerso in campo B e seguito da un rivelatore di muoni (per sopprimere il fondo di charm)!
Si stima di dovere cambiare il rivelatore circa 10 volte nel corso del run —>totale di 5400 m
2 di piates di emulsioni —> 5% di OPERA!
Due opzioni allo studio:!
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New!
Walter M. Bonivento - CERN/INFN Cagliari CNS1 Elba 20/05/2104
Stato della proposta Raccomandazione SPSc —>gia detto a Febbraio!
L’Extended Directorat del CERN ha istituito recentemente una task force composta da fisici degli acceleratori del CERN (Saban, Goddard, Arduini, Gatignon ecc.) per dare un “first assessment” per la fattibilita’ e costi del nostro esperimento in termini di beam line e dump!
Un draft del documento e’ gia’ pronto (ma non ancora pubblico) e sara’ discusso probabilmente al prossimo RB!
Pagina web http://ship.web.cern.ch/ship/ !
Costo stimato: 100M (CERN) per il fascio 15M+15M+12M (F.A.) per il rivelatore (inclusi i contributi in-kind)
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New!
Walter M. Bonivento - CERN/INFN Cagliari CNS1 Elba 20/05/2104
Tempistica (moolto preliminare)
• Proposal : 1 meta’ del 2015
• Approvazione SPSc: seconda meta’ 2015
• incoraggiamento continuare —> council 2016
• Due anni per fare i TDR, meta’ 2017: approvazione fine 2017; Technical Design del fascio
• Prime richieste finanziarie per produzione rivelatori: 2018
• costruzione beam line: LS2
• 4-5 anni produzione-istallazione (durante LS3)
• Data taking: dopo LS3, 2022-2027
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New!
Walter M. Bonivento - CERN/INFN Cagliari CNS1 Elba 20/05/2104
Il workshop di ZurigoPrimo meeting open di Collaborazione il 10-12 Giugno a Zurigo: sara’ un workshop a cui sono invitati molti teorici e si discuteranno le opzioni per i vari sotto-sistemi
Ci sara’ una sessione in cui si decidera’ l’estensione della collaborazione a nuovi membri della collaborazione (che ovviamente ne facciano richiesta) a cui sara’ richiesto di dichiarare il tipo di impegno potenziale su:
a ) preparazione proposal, b) preparazione TDR, c) costruzione
Sara’ dato tempo fino a Settembre per le “late entries” per a)
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Walter M. Bonivento - CERN/INFN Cagliari CNS1 Elba 20/05/2104
Coordinamento• interim membership committee: io (firmatario della
EOI e uno dei progettisti iniziali) membro per Italia
• interim executive committee: i firmatari della EOI +Addendum —>G DeLellis + me
• Muon detector: io
• Neutrino detector: G DeLellis (e Panman)
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New!
Walter M. Bonivento - CERN/INFN Cagliari CNS1 Elba 20/05/2104
Partecipazione gruppi INFN• Ci sono due anime: provenienza G1 e G2 (soprattutto OPERA)
• interesse ex-OPERA particolarmente nel rivelatore di 𝜈𝝉
• Stiamo cercando sinergie tra le due parti —>una individuata nei rivelatori di muoni
• Bari (da G1 e G2): rivelatori MUON e rivelatore 𝜈𝝉
• Bologna (da G1): elettronica ECAL e rivelatore MUON
• Cagliari (da G1): rivelatore MUON e DAQ
• Lab.Naz.GranSasso (da G2): elettronica MUON e rivelatore 𝜈𝝉
• LNF (da G1 e da G2): rivelatori MUON e tracciatore per 𝜈𝝉 (opzione GEM)
• Napoli (da G1 e G2): rivelatori MUON e rivelatore 𝜈𝝉
29
New!
Walter M. Bonivento - CERN/INFN Cagliari CNS1 Elba 20/05/2104
Scelta della Commissione
• Per ora facciamo l’ipotesi di fare le richieste in Gruppo Uno
• La Giunta si riserva di decidere una diversa collocazione entro Luglio
30
Walter M. Bonivento - CERN/INFN Cagliari CNS1 Elba 20/05/2104
Percentuali• A oggi le percentuali non sono ancora definite
• Probabilmente ci saranno alcuni gruppi con la sigla locale (>2FTE) ed altri no (su DTZ): per una fase di TP va bene cosi'
• Sicuramente si aprira’ la sigla nazionale
• Probabile 7-10 FTE per il 2015 a ovviamente salire a esperimento approvato
• Necessita’ finanziarie:
• 2014: missioni su DTZ (per me e Giovanni) per il coordinamento dello sviluppo del progetto (se si vogliono nuove idee…)
• 2015: missioni e consumo per preparare TP per tutti i gruppi
• test beams
• test in laboratorio (e.g. riutilizzo muon detector di OPERA, test scanning, test traccianti per rivelatore di neutrini, ecc.)
• piano dettagliato a Settembre
31
New!
Walter M. Bonivento - CERN/INFN Cagliari CNS1 Elba 20/05/2104
Gruppi stranieri • Da Zurigo probabilmente:
• Russia: 5 istituti
• UK: 3 istituti
• F: 3 istituti
• CH: 4 istituti
• CERN>7 fisici
• D: 1-2 istituti
• Svezia: 2 istituti
• Cile: 1-2 istituti
• Giappone: 4 istituti
32
New!
Walter M. Bonivento - CERN/INFN Cagliari CNS1 Elba 20/05/2104
N1: appena dopo la CNS1 di Febbraio!
!
!
!
!
!
• idea: mettere insieme 73 osservazioni di cluster di galassie per aumentare la statistica: analizzate le osservazioni di XMM-Newton e Chandra. Correzioni per il red-shift (0.01-0.35)
33
Submitted
to
ApJ,2014February10
Preprin
tty
pesetusin
gL ATEX
style
emulateapjv.04/17/13
DETECTIO
NOFAN
UNID
ENTIF
IED
EMISSIO
NLIN
EIN
THE
STACKED
X-R
AY
SPECTRUM
OFGALAXY
CLUSTERS
EsraBulbul
1,2
,Maxim
Markevitch
2
,Adam
Foster
1
,RandallK.Smith
1
MichaelLoewenstein
2
,and
ScottW
.Randall
1
1Harvard
-Smith
sonian
Cen
terfor
Astrop
hysics,
60Gard
enStreet,
Cam
brid
ge,MA
02138.2NASA
Goddard
Space
Fligh
tCen
ter,Green
belt,
MD,USA.
SubmittedtoApJ,2014February10
ABSTRACT
Wedetect
aweak
unidentifi
edem
issionlin
eat
E=
(3.55�
3.57)±
0.03keV
inastacked
XMM
spectru
mof
73galaxy
clusters
span
ningared
shift
range
0.01�
0.35.MOS
and
PN
observation
sindep
endently
show
thepresen
ceof
thelin
eat
consistent
energies.
When
thefullsam
ple
isdivid
edinto
three
subsam
ples
(Perseu
s,Centau
rus+
Ophiuchu
s+Com
a,an
dall
others),
thelin
eis
seenat
>3�
statisticalsign
ifican
cein
allthree
indep
endent
MOSspectra
andthePN
“alloth
ers”spectru
m.
Thelin
eisalso
detected
atthesam
eenergy
intheChan
dra
ACIS-S
andACIS-Ispectra
ofthePerseu
sclu
ster,with
afluxcon
sistentwith
XMM-N
ewton
(how
ever,it
isnot
seenin
theACIS-I
spectru
mof
Virgo).
Thelin
eis
present
evenifweallow
maxim
um
freedom
forall
thekn
owntherm
alem
issionlin
es.How
ever,itisvery
weak
(with
anequ
ivalentwidth
inthefullsam
pleof
only
⇠1eV
)an
dlocated
with
in50–110
eVof
severalkn
ownfaint
lines;
thedetection
isat
thelim
itof
thecurrent
instru
ment
capab
ilitiesan
dsubject
tosign
ificant
mod
elinguncertainties.
Ontheorigin
ofthislin
e,weargu
ethat
there
shou
ldbenoatom
ictran
sitionsin
therm
alplasm
aat
this
energy.
Anintrigu
ingpossib
ilityis
thedecay
ofsterile
neutrin
o,alon
g-sought
dark
matter
particle
candidate.
Assu
mingthat
alldark
matter
isin
sterileneutrin
oswith
ms=
2E=
7.1keV
,ou
rdetection
inthefullsam
ple
correspon
dsto
aneutrin
odecay
mixin
gan
glesin
2(2✓)⇡
7⇥10
�11,
below
thepreviou
supper
limits.
How
ever,based
ontheclu
stermasses
anddistan
ces,thelin
ein
Perseu
sismuch
brighter
than
expected
inthismod
el,sign
ificantly
deviatin
gfrom
other
subsam
ples.
This
appears
tobebecau
seof
anan
omalou
slybright
lineat
E=
3.62keV
inPerseu
s,which
could
bean
Arxviidielectron
icrecom
bination
line,
althou
ghits
emissivity
wou
ldhave
tobe30
times
theexp
ectedvalu
ean
dphysically
di�
cultto
understan
d.In
prin
ciple,
such
anan
omaly
might
explain
ourlin
edetection
inoth
ersubsam
ples
aswell,
thou
ghit
wou
ldstretch
thelin
eenergy
uncertainties.
Anoth
eraltern
ativeis
theab
ovean
omaly
intheArlin
ecom
bined
with
thenearby
3.51keV
Klin
ealso
exceedingexp
ectationby
factor10–20.
Con
firm
ationwith
Chan
dra
andSuzak
u,an
deventu
allyAstro-H
,are
required
todeterm
inethenatu
reof
this
new
line.
1.IN
TRODUCTIO
N
Galaxy
clusters
arethelargest
aggregationsof
hot
in-
tergalacticgas
and
dark
matter.
Thegas
isenrich
edwith
heavy
elements
(Mitch
ellet
al.(1976);
Serlem
itsoset
al.(1977)
andlater
works)
that
escapefrom
galaxiesan
daccu
mulate
intheintraclu
ster/intergalacticmedium
(ICM)over
billion
sof
yearsof
galactican
dstellar
evo-lution
.Thepresen
ceof
variousheavy
ionsis
seenfrom
their
emission
lines
intheclu
sterX-ray
spectra.
Data
fromlarge
e↵ective
areatelescop
eswith
spectroscop
icca-
pab
ilities,such
asASCA,Chan
dra,
XMM-N
ewton
and
Suzak
u,uncovered
thepresen
ceof
many
elements
inthe
ICM,inclu
dingO,Ne,
Mg,
Si,
S,Ar,
Ca,
Fe,
and
Ni
(forareview
see,e.g.,
Boh
ringer
&Wern
er2010).
Re-
cently,weak
emission
lines
oflow
-abundan
ceCran
dMn
were
discovered
(Wern
eret
al.2006;
Tam
ura
etal.
2009).Relative
abundan
cesof
variouselem
entscontain
valuab
leinform
ationon
therate
ofsupern
ovaeof
di↵erent
types
ingalaxies
(e.g.,Loew
enstein
2013)an
dillu
minate
theen-
richment
history
oftheIC
M(e.g.,
Bulbulet
al.2012b
).Lineratios
ofvariou
sion
scan
alsoprovid
ediagn
osticsof
thephysical
prop
ertiesof
theIC
M,uncover
thepres-
ence
ofmulti-tem
peratu
regas,
non
equilib
rium
ionization
ebulbul@
cfa.harva
rd.ed
u
statesan
dnonth
ermal
emission
processes
such
ascharge
exchan
ge(P
aerels&
Kah
n2003).
Asfor
dark
matter,
80years
fromits
discovery
by(Zwicky
1933,1937),
itsnatu
reisstill
unkn
own(th
ough
now
wedokn
owfor
sure
itexists
—from
X-ray
and
gravitational-len
singob
servationsof
theBullet
Cluster,
Clow
eet
al.(2006),
andwekn
owaccu
ratelyits
cosmo-
logicalab
undan
ce,e.g.,
Hinshaw
etal.
(2013)).Amon
gthevariou
splau
sible
dark
matter
candidates,
onethat
has
motivated
ourpresent
work
isthehyp
othetical
ster-ile
neutrin
othat
isinclu
ded
insom
eexten
sionsto
the
standard
mod
elof
particle
physics
(Dod
elson&
Widrow
(1994)an
dlater
works;
forrecent
reviewssee,
e.g.,Abaza
jianet
al.(2007);
Boyarsky
etal.
(2009)).Ster-
ileneutrin
osshou
lddecay
spontan
eously
with
therate
�� (m
s ,✓)=
1.38⇥
10�29s �
1
✓sin
22✓
10�7
◆⇣
ms
1keV
⌘5
,(1)where
theparticle
mass
msan
dthe“m
ixingan
gle”✓
areunkn
own
buttied
toeach
other
inany
particu
larneutrin
oprod
uction
mod
el(P
al&
Wolfen
stein1982).
Thedecay
ofsterile
neutrin
oshou
ldprod
uce
aphoton
ofE
=m
s /2an
dan
activeneutrin
o.Themass
ofthester-
ileneutrin
omay
liein
thekeV
range,
which
wou
ldplace
arXiv:1402.2301v1 [astro-ph.CO] 10 Feb 2014
Submitted to ApJ, 2014 February 10
Preprint typeset using LATEX style emulateapj v. 04/17/13
DETECTION OF AN UNIDENTIFIED EMISSION LINE IN THE STACKED X-RAY SPECTRUM OF GALAXYCLUSTERS
Esra Bulbul
1,2
, Maxim Markevitch
2
, Adam Foster
1
, Randall K. Smith
1
Michael Loewenstein
2
, and
Scott W. Randall
1
1 Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138.2 NASA Goddard Space Flight Center, Greenbelt, MD, USA.
Submitted to ApJ, 2014 February 10
ABSTRACT
We detect a weak unidentified emission line at E = (3.55 � 3.57) ± 0.03 keV in a stacked XMMspectrum of 73 galaxy clusters spanning a redshift range 0.01 � 0.35. MOS and PN observationsindependently show the presence of the line at consistent energies. When the full sample is dividedinto three subsamples (Perseus, Centaurus+Ophiuchus+Coma, and all others), the line is seen at> 3� statistical significance in all three independent MOS spectra and the PN “all others” spectrum.The line is also detected at the same energy in the Chandra ACIS-S and ACIS-I spectra of the Perseuscluster, with a flux consistent with XMM-Newton (however, it is not seen in the ACIS-I spectrum ofVirgo). The line is present even if we allow maximum freedom for all the known thermal emissionlines. However, it is very weak (with an equivalent width in the full sample of only ⇠ 1 eV) and locatedwithin 50–110 eV of several known faint lines; the detection is at the limit of the current instrumentcapabilities and subject to significant modeling uncertainties. On the origin of this line, we argue thatthere should be no atomic transitions in thermal plasma at this energy. An intriguing possibility isthe decay of sterile neutrino, a long-sought dark matter particle candidate. Assuming that all darkmatter is in sterile neutrinos with ms = 2E = 7.1 keV, our detection in the full sample corresponds toa neutrino decay mixing angle sin2(2✓) ⇡ 7⇥ 10�11, below the previous upper limits. However, basedon the cluster masses and distances, the line in Perseus is much brighter than expected in this model,significantly deviating from other subsamples. This appears to be because of an anomalously brightline at E = 3.62 keV in Perseus, which could be an Arxvii dielectronic recombination line, althoughits emissivity would have to be 30 times the expected value and physically di�cult to understand. Inprinciple, such an anomaly might explain our line detection in other subsamples as well, though itwould stretch the line energy uncertainties. Another alternative is the above anomaly in the Ar linecombined with the nearby 3.51 keV K line also exceeding expectation by factor 10–20. Confirmationwith Chandra and Suzaku, and eventually Astro-H, are required to determine the nature of this newline.
1. INTRODUCTION
Galaxy clusters are the largest aggregations of hot in-tergalactic gas and dark matter. The gas is enrichedwith heavy elements (Mitchell et al. (1976); Serlemitsoset al. (1977) and later works) that escape from galaxiesand accumulate in the intracluster/intergalactic medium(ICM) over billions of years of galactic and stellar evo-lution. The presence of various heavy ions is seen fromtheir emission lines in the cluster X-ray spectra. Datafrom large e↵ective area telescopes with spectroscopic ca-pabilities, such as ASCA, Chandra, XMM-Newton andSuzaku, uncovered the presence of many elements in theICM, including O, Ne, Mg, Si, S, Ar, Ca, Fe, and Ni(for a review see, e.g., Bohringer & Werner 2010). Re-cently, weak emission lines of low-abundance Cr and Mnwere discovered (Werner et al. 2006; Tamura et al. 2009).Relative abundances of various elements contain valuableinformation on the rate of supernovae of di↵erent types ingalaxies (e.g., Loewenstein 2013) and illuminate the en-richment history of the ICM (e.g., Bulbul et al. 2012b).Line ratios of various ions can also provide diagnosticsof the physical properties of the ICM, uncover the pres-ence of multi-temperature gas, nonequilibrium ionization
states and nonthermal emission processes such as chargeexchange (Paerels & Kahn 2003).As for dark matter, 80 years from its discovery by
(Zwicky 1933, 1937), its nature is still unknown (thoughnow we do know for sure it exists — from X-ray andgravitational-lensing observations of the Bullet Cluster,Clowe et al. (2006), and we know accurately its cosmo-logical abundance, e.g., Hinshaw et al. (2013)). Amongthe various plausible dark matter candidates, one thathas motivated our present work is the hypothetical ster-ile neutrino that is included in some extensions to thestandard model of particle physics (Dodelson & Widrow(1994) and later works; for recent reviews see, e.g.,Abazajian et al. (2007); Boyarsky et al. (2009)). Ster-ile neutrinos should decay spontaneously with the rate
��(ms, ✓) = 1.38⇥ 10�29 s�1
✓sin2 2✓
10�7
◆⇣ ms
1 keV
⌘5
,
(1)where the particle mass ms and the “mixing angle” ✓are unknown but tied to each other in any particularneutrino production model (Pal & Wolfenstein 1982).The decay of sterile neutrino should produce a photon ofE = ms/2 and an active neutrino. The mass of the ster-ile neutrino may lie in the keV range, which would place
arX
iv:1
402.
2301
v1 [
astro
-ph.
CO]
10 F
eb 2
014
Walter M. Bonivento - CERN/INFN Cagliari CNS1 Elba 20/05/2104
Un altra breaking news!
• Osservazione consistente di una linea at 3.5KeV with 3-4 σ significance!
• Analisi diversa dalla precedente e su dati diversi, con controlli anche sulla dipendenza radiale e sul contenuto relativo di DM!
• Molte analisi in corso che potranno chiarire la situazione!
• Missione Astro-H sara’ lanciata nel 2015 e aiutera’ a chiarire la situazione
34
arX
iv:1
402.
4119
v1 [
astro
-ph.
CO]
17 F
eb 2
014
An unidentified line in X-ray spectra of the Andromeda galaxy and Perseus galaxy cluster
A. Boyarsky1, O. Ruchayskiy2, D. Iakubovskyi3,4 and J. Franse1,51Instituut-Lorentz for Theoretical Physics, Universiteit Leiden, Niels Bohrweg 2, Leiden, The Netherlands
2Ecole Polytechnique Federale de Lausanne, FSB/ITP/LPPC, BSP, CH-1015, Lausanne, Switzerland3Bogolyubov Institute of Theoretical Physics, Metrologichna Str. 14-b, 03680, Kyiv, Ukraine
4National University “Kyiv-Mohyla Academy”, Skovorody Str. 2, 04070, Kyiv, Ukraine5Leiden Observatory, Leiden University, Niels Bohrweg 2, Leiden, The Netherlands
We identify a weak line at E ∼ 3.5 keV in X-ray spectra of the Andromeda galaxy and the Perseus galaxycluster – two dark matter-dominated objects, for which there exist deep exposures with the XMM-Newton X-rayobservatory. Such a line was not previously known to be present in the spectra of galaxies or galaxy clusters.Although the line is weak, it has a clear tendency to become stronger towards the centers of the objects; it isstronger for the Perseus cluster than for the Andromeda galaxy and is absent in the spectrum of a very deep“blank sky” dataset. Although for individual objects it is hard to exclude the possibility that the feature is dueto an instrumental effect or an atomic line of anomalous brightness, it is consistent with the behavior of a lineoriginating from the decay of dark matter particles. Future detections or non-detections of this line in multipleastrophysical targets may help to reveal its nature.
The nature of dark matter (DM) is a question of crucial im-portance for both cosmology and for fundamental physics. Asneutrinos – the only known particles that could be dark mat-ter candidates – are known to be too light to be consistent withvarious observations (see e.g. [1] for a review), it is widely an-ticipated that a new particle should exist to extend the hot BigBang cosmology paradigm to dark matter. Although manycandidates have been put forward by particle physicists (seee.g. [2]), little is known experimentally about the propertiesof DM particles: their masses, lifetimes, and interaction typesremain largely unconstrained. A priori, a given DM candidatecan possess a decay channel if its lifetime exceeds the ageof the Universe. Therefore, the search for a DM decay signalprovides an important test to constrain the properties of DM ina model-independent way. For fermionic particles, one shouldsearch above the Tremaine-Gunn limit [3] (! 300 eV). If themass is below 2mec2, such a fermion can decay to neutrinosand photons, and we can expect two-body radiative decay withphoton energy Eγ = 1
2mDM. Such particles can be searched
for in X-rays (see [4] for review of previous searches). Foreach particular DM model, the particle’s mass, lifetime andother parameters are related by the requirement to provide thecorrect DM abundance. For example, for one very interestingDM candidate – the right-handed neutrino – this requirementrestricts the mass range to 0.5 − 100 keV [4, 5]. A large partof the available parameter space for sterile neutrinos is fullyconsistent with all astrophysical and cosmological bounds [6],and it is important to probe it still further.
The DM decay line is much narrower than the spectral res-olution of the present day X-ray telescopes and, as previoussearches have shown, should be rather weak. The X-ray spec-tra of astrophysical objects are crowded with weak atomic andinstrumental lines, not all of which may be known. Therefore,even if the exposure of available observations continues to in-crease, it is hard to exclude an astrophysical or instrumentalorigin of any weak line found in the spectrum of individual
object. However, if the same feature is present in the spectraof a number of different objects, and its surface brightness andrelative normalization between objects is consistent with theexpected behavior of the DM signal, this can provide muchmore convincing evidence about its nature.
The present paper takes a step in this direction. We presentthe results of the combined analysis of many XMM-Newtonobservations of two objects at different redshifts – the Perseuscluster and the Andromeda galaxy (M31) – together with along exposure “blank sky” dataset. We study the 2.8–8 keVenergy band and show that the only significant un-modeledexcess that is present in the spectra of both M31 and Perseusis located at ∼ 3.5 keV energy and the line in Perseus is cor-rectly redshifted as compared to Andromeda (at 95% CL). Therelative fluxes for the two objects are in agreement with whatis known about their DM distributions. We also study sur-face brightness profiles of this line and find them consistentwith expectations for a DM decay line. We do not detect sucha line in the very deep “blank sky” dataset, which disfavorssome of the scenarios for its instrumental origin (e.g. featuresin the effective area). The upper bound from this dataset isconsistent with expectations for a DM signal that would comein this case primarily from the Milky Way halo. However, asthe line is weak (∼ 4σ in the combined dataset) and the uncer-tainties in DM distribution are significant, positive detectionsor strong constraints from more objects are clearly needed inorder to determine the nature of this signal.1
Below we summarize the details of our data analysis and then
1 During our work we became aware that a similar analysis has been carriedout by different group for a collection of galaxy clusters. When this paperwas in preparation, the arXiv preprint [7] by this group appeared, claim-ing a detection of a spectral feature at the same energy from a number ofclusters.
arXiv:1402.4119v1 [astro-ph.CO] 17 Feb 2014
Anunidentified
lineinX-ray
spectraofthe
Androm
edagalaxy
andPerseusgalaxy
cluster
A.Boyarsky
1,O.Ruchayskiy
2,D.Iakubovskyi 3
,4and
J.Franse1,5
1Instituut-LorentzforTheoreticalPhysics,U
niversiteitLeiden,Niels
Bohrweg
2,Leiden,TheN
etherlands2Ecole
PolytechniqueFederale
deLausanne,FSB/ITP/LPPC,BSP,CH
-1015,Lausanne,Switzerland
3BogolyubovInstitute
ofTheoreticalPhysics,Metrologichna
Str.14-b,03680,K
yiv,Ukraine
4NationalU
niversity“K
yiv-Mohyla
Academ
y”,SkovorodyStr.
2,04070,Kyiv,U
kraine5Leiden
Observatory,Leiden
University,N
ielsBohrw
eg2,Leiden,The
Netherlands
We
identifya
weak
lineat
E∼
3.5keV
inX
-rayspectra
oftheA
ndromeda
galaxyand
thePerseus
galaxycluster–
two
darkm
atter-dominated
objects,forwhich
thereexistdeepexposuresw
iththeX
MM
-New
tonX
-rayobservatory.
Sucha
linew
asnotpreviously
known
tobe
presentinthe
spectraofgalaxies
orgalaxyclusters.
Although
theline
isw
eak,ithasa
cleartendencyto
become
strongertowards
thecenters
oftheobjects;itis
strongerforthePerseus
clusterthanforthe
Androm
edagalaxy
andis
absentinthe
spectrumofa
verydeep
“blanksky”
dataset.Although
forindividualobjectsitishard
toexclude
thepossibility
thatthefeature
isdue
toan
instrumentaleffectoran
atomic
lineofanom
alousbrightness,itisconsistentw
iththe
behaviorofaline
originatingfrom
thedecay
ofdarkm
atterparticles.Futuredetectionsornon-detections
ofthislinein
multiple
astrophysicaltargetsmay
helpto
revealitsnature.
Thenature
ofdarkm
atter(DM
)isa
questionofcrucialim
-portanceforboth
cosmology
andforfundam
entalphysics.As
neutrinos–the
onlyknow
nparticlesthatcould
bedark
mat-
tercandidates–areknow
nto
betoolightto
beconsistentwith
variousobservations(seee.g.[1]forareview),itisw
idelyan-
ticipatedthatanew
particleshouldexistto
extendthehotBig
Bangcosm
ologyparadigm
todark
matter.
Although
many
candidateshave
beenputforw
ardby
particlephysicists
(seee.g.[2]),little
isknow
nexperim
entallyaboutthe
propertiesofD
Mparticles:theirm
asses,lifetimes,and
interactiontypes
remain
largelyunconstrained.A
priori,agiven
DM
candidatecan
possessa
decaychannelif
itslifetim
eexceeds
theage
oftheU
niverse.Therefore,thesearch
foraD
Mdecay
signalprovidesan
importanttestto
constrainthepropertiesofD
Min
amodel-independentw
ay.Forfermionicparticles,oneshould
searchabove
theTrem
aine-Gunn
limit[3](!
300eV
).Ifthem
assisbelow
2me c
2,sucha
fermion
candecay
toneutrinos
andphotons,and
wecan
expecttwo-bodyradiativedecay
with
photonenergy
Eγ=
12 mD
M .Such
particlescanbe
searchedforin
X-rays
(see[4]
forreviewofprevious
searches).For
eachparticularD
Mm
odel,theparticle’s
mass,lifetim
eand
otherparametersarerelated
bytherequirem
enttoprovidethe
correctDM
abundance.Forexample,forone
veryinteresting
DM
candidate–
theright-handed
neutrino–
thisrequirement
restrictsthem
assrangeto
0.5−
100keV
[4,5].Alarge
partofthe
availableparam
eterspaceforsterile
neutrinosis
fullyconsistentw
ithallastrophysicaland
cosmologicalbounds[6],
anditisim
portanttoprobeitstillfurther.
TheD
Mdecay
lineis
much
narrowerthan
thespectralres-
olutionofthe
presentdayX
-raytelescopes
and,asprevious
searcheshaveshown,should
beratherweak.TheX
-rayspec-
traofastrophysicalobjectsarecrowded
with
weak
atomicand
instrumentallines,notallofw
hichm
aybeknow
n.Therefore,even
iftheexposureofavailableobservationscontinuesto
in-crease,itis
hardto
excludean
astrophysicalorinstrumental
originofany
weak
linefound
inthe
spectrumofindividual
object.How
ever,ifthesam
efeature
ispresentinthe
spectraofanum
berofdifferentobjects,anditssurfacebrightnessand
relativenorm
alizationbetw
eenobjects
isconsistentw
iththe
expectedbehaviorofthe
DM
signal,thiscan
providem
uchm
oreconvincingevidenceaboutitsnature.
Thepresentpapertakes
astep
inthis
direction.W
epresent
theresults
ofthe
combined
analysisof
many
XMM-Newton
observationsoftwo
objectsatdifferentredshifts–thePerseus
clusterand
theA
ndromeda
galaxy(M
31)–
togetherw
itha
longexposure
“blanksky”
dataset.W
estudy
the2.8–8
keVenergy
bandand
showthatthe
onlysignificantun-m
odeledexcessthatispresentin
thespectra
ofbothM
31and
Perseusislocated
at∼
3.5keV
energyand
theline
inPerseusiscor-
rectlyredshiftedascom
paredtoA
ndromeda(at95%
CL).Therelative
fluxesforthetw
oobjectsare
inagreem
entwith
what
isknow
nabouttheir
DM
distributions.W
ealso
studysur-
facebrightness
profilesofthis
lineand
findthem
consistentw
ithexpectationsfora
DM
decayline.W
edo
notdetectsucha
linein
thevery
deep“blank
sky”dataset,w
hichdisfavors
some
ofthescenariosforitsinstrum
entalorigin(e.g.features
inthe
effectivearea).
Theupperbound
fromthis
datasetisconsistentw
ithexpectationsforaD
Msignalthatw
ouldcom
ein
thiscaseprim
arilyfrom
theM
ilkyW
ayhalo.H
owever,as
thelineisweak
(∼4σ
inthecom
bineddataset)and
theuncer-taintiesin
DM
distributionare
significant,positivedetections
orstrongconstraintsfrom
more
objectsareclearly
neededin
ordertodeterm
inethenatureofthissignal. 1
Beloww
esum
marizethedetailsofourdataanalysisand
then
1D
uringourw
orkw
ebecam
eaw
arethata
similaranalysishasbeen
carriedoutby
differentgroupfora
collectionofgalaxy
clusters.When
thispaper
was
inpreparation,the
arXiv
preprint[7]bythis
groupappeared,claim
-ing
adetection
ofaspectralfeature
atthesam
eenergy
froma
numberof
clusters.
Walter M. Bonivento - CERN/INFN Cagliari CNS1 Elba 20/05/2104
Un esempio di plot!
!
!
• incompatibile, dicono gli autori, con linee atomiche note e con possibili effetti strumentali (non sono un esperto per giudicare se hanno ragione)
• la significanza dichiarata e’ 3-4σ in vari sub-campioni —>pertanto e’ il caso di aspettare ed essere cauti.
35
Blank skyM31
Walter M. Bonivento - CERN/INFN Cagliari CNS1 Elba 20/05/2104
For fun: nel grafico bi-dimensionale
36
22
Figure 12. Recent constraints on sterile neutrino productionmodels, assuming sterile neutrinos constitute dark matter (Abaza-jian et al. 2007). Straight lines in black show theoretical predictionsassuming sterile neutrinos constitute the dark matter with leptonnumber L = 0, L = 0.003, L = 0.01, L = 0.1. Constraints from thecosmic X-ray background are shown in the solid (blue and hatchedregions). The region is solid green is excluded based upon obser-vations of the di↵use X-ray background (Abazajian et al. 2007).Individual galaxy cluster constraints from XMM-Newton observa-tions of the Coma and Virgo clusters are shown in light blue (Bo-yarsky et al. 2006). The horizontal pink band shows the mass scaleconsistent with producing a 100�300 pc core in the Fornax dwarfgalaxy (Strigari et al. 2006), and limits from the Milky Way byBoyarsky et al. (2006) is indicated with BMW. The orange regionat m
s
< 0.4 keV is ruled out by an application of the Tremaine-Gunn bound (Bode et al. 2001). Our measurement obtained fromthe full sample which is marked with the star in red, is consistentwith previous upper limits.
are unable to collisionally excite any Ar XVII lines, butdielectronic recombination is still possible. Examiningthe satellite line data in the AtomDB, taken from Vain-shtein & Safronova (1980), shows that even in this casethe maximum ratio is only 7%, as there are DR satellitelines at the energies of the Ar XVII triplet as well andthese lines would also be excited in such a case. Whilenot physically impossible if there was a significant andunexpected error in the atomic physics calculations, wehave no reason to believe this has occurred.We also note that our assumptions regarding rela-
tive line strengths have assumed the ICM is in thermalequilibrium or close to it. Charge exchange (CX) be-tween highly-ionized ions and neutral hydrogen or he-lium could also create X-ray emission lines with di↵erentratios (Smith et al. 2012). This could a↵ect our assump-tion of equilibrium line ratios, although we have includeda substantial range around the equilibrium values. It isimportant to note that these CX lines are not ‘new, butrather the same lines occurring in di↵erent ratios. Dueto its large cross section relative to electron excitationrates, astrophysical CX can occur only in a thin sheetwhere ions and neutrals interact directly, limiting its to-tal emission relative to the large ICM volume. In certain
cases, such as the core of the Perseus cluster where manyneutral filaments are known, it is possible that CX couldbe large enough to create a small fraction of the totalX-ray emission, although it would not create or enhancea line at 3.57 keV or the DR line at 3.62 keV. CX couldnot dominate the overall emission, however, as it wouldalso create Fe XVII and other lines that are not detected.
5.2. Sterile neutrino decay line?
An interesting interpretation of the line is the decaysignature of the sterile neutrino, a long-sought dark mat-ter particle candidate (Boyarsky et al. (e.g., 2009), seeour §1). The mass of the sterile neutrino would be dou-ble the decay photon energy, ms =7.1 keV. The line fluxdetected in our full sample corresponds to a mixing anglefor the decay sin2(2✓) ⇠ 7 ⇥ 10�11. This value is belowthe upper limits placed by the previous searches, shownin Fig. 12. Our detection from the stacked XMM-NewtonMOS observations galaxy clusters are shown with a starin red in that figure. Figure 13 shows the detections andupper limits we obtained from our various subsamples weused in this work (based on the included cluster massesand distances), as well as a comparison with previous up-per limit placed using the Bullet cluster by Boyarsky etal. (2008) at 3.57 keV, which is the most relevant earlierconstraint for us. Since the mixing angle is a universalquantity, all the subsample measurements must agree.The line in the subsample of fainter 69 clusters (full
sample sans Perseus, Coma, Ophiuchus and Centaurus)corresponds to a mixing angle that is consistent withthe full sample; the same is seen (though with a mild1.5� tension) for the subsample of bright nearby clustersComa+Centaurus+Ophiuchus. However, the brightnessof the new line in the XMM-Newton spectrum of Perseuscorresponds to a significantly higher mixing angle thanthat for the full sample (by factor 8 for the MOS spec-trum), which poses a problem in need of further investi-gation.We tried to excise the central 10 region of the Perseus
cluster, to see if the flux originates in the cool core of thecluster. Indeed, this decreased the flux in the line in halfand removed most of the tension with the other measure-ments. However, this suggests that either some of the lineflux is astrophysical in origin (at least in Perseus), or thecool gas in the core of the cluster a↵ects our ability tomeasure the continuum and the fluxes of the nearby Kxviii and Ar xvii lines, in the end resulting in an over-estimate of the flux of our detected line. It appears thatin Preseus, there is an anomalously strong line at the po-sition of the Ar xvii dielectronic recombination line at3.62 keV.With this knowledge, we have tried to add this anoma-
lous 3.62 keV line in the model for the full sample, wherewe have the most statistically significant line detection.The additional line is still required, albeit at a lower sig-nificance and a slightly lower energy of 3.55± 0.03 keV.Note that the sample of bright clusters is dominated bythe emission from the cool cores of Ophiuchus and Cen-taurus cluster, if this Ar 3.62 keV line anomaly is typicalof cool cores, they may also be a↵ected. However, free-ing the flux of the 3.62 keV line in the MOS full-samplefit did not require additional contribution from clustersother than Perseus, though the constraints are obviouslyweak.
Harvard, NASA ecc.
5
Interaction strength Sin2(2θ)
Dark matter mass MDM [keV]
10-13
10-12
10-11
10-10
10-9
10-8
10-7
2 5 50 1 10
DM overproduction
Not enough DM
Tremaine-Gunn / Lyman-α Excluded by X-ray observations
Interaction strength Sin2(2θ)
Dark matter mass MDM [keV]
10-13
10-12
10-11
10-10
10-9
10-8
10-7
2 5 50 1 10
DM overproduction
Not enough DM
Tremaine-Gunn / Lyman-α Excluded by X-ray observations
Interaction strength Sin2(2θ)
Dark matter mass MDM [keV]
10-13
10-12
10-11
10-10
10-9
10-8
10-7
2 5 50 1 10
DM overproduction
Not enough DM
Tremaine-Gunn / Lyman-α Excluded by X-ray observations
Interaction strength Sin2(2θ)
Dark matter mass MDM [keV]
10-13
10-12
10-11
10-10
10-9
10-8
10-7
2 5 50 1 10
DM overproduction
Not enough DM
Tremaine-Gunn / Lyman-α Excluded by X-ray observations
Interaction strength Sin2(2θ)
Dark matter mass MDM [keV]
10-13
10-12
10-11
10-10
10-9
10-8
10-7
2 5 50 1 10
DM overproduction
Not enough DM
Tremaine-Gunn / Lyman-α Excluded by X-ray observations
FIG. 4: Constraints on sterile neutrino DM within νMSM [4]. Theblue point would corresponds to the best-fit value from M31 if theline comes from DM decay. Thick errorbars are ±1σ limits on theflux. Thin errorbars correspond to the uncertainty in the DM distri-bution in the center of M31.
to detect the candidate line in the “strong line” regime [35]. Inparticular, Astro-H should be able to resolve the Milky Wayhalo’s DM decay signal and therefore all its observations canbe used. Failure to detect such a line will rule out the DMorigin of the Andromeda/Perseus signal presented here.
Acknowledgments. We thank D. Malyshev for collaboration;A. Neronov for useful critical comments; M. Shaposhnikovand M. Lovell for reading the manuscript and providing com-ment. The work of D. I. was supported by part by the theProgram of Cosmic Research of the National Academy of Sci-ences of Ukraine and the State Programme of Implementationof Grid Technology in Ukraine.
[1] A. Boyarsky, O. Ruchayskiy, and D. Iakubovskyi, JCAP 0903,005 (2009).
[2] J. L. Feng, ARA&A 48, 495 (2010).[3] S. Tremaine and J. E. Gunn, Phys. Rev. Lett. 42, 407 (1979).[4] A. Boyarsky, D. Iakubovskyi, and O. Ruchayskiy, Phys. Dark
Univ. 1, 136 (2012).[5] A. Boyarsky, O. Ruchayskiy, and M. Shaposhnikov, Ann. Rev.
Nucl. Part. Sci. 59, 191 (2009).[6] A. Boyarsky, J. Lesgourgues, O. Ruchayskiy, and M. Viel,
Phys. Rev. Lett. 102, 201304 (2009).[7] E. Bulbul, M. Markevitch, A. Foster, R. K. Smith, M. Loewen-
stein, et al., 1402.2301 (2014).[8] M. J. L. Turner, A. Abbey, M. Arnaud, M. Balasini, M. Barbera,
E. Belsole, P. J. Bennie, J. P. Bernard, G. F. Bignami, M. Boer,et al., A&A 365, L27 (2001).
[9] L. Struder, U. Briel, K. Dennerl, R. Hartmann, E. Kendziorra,N. Meidinger, E. Pfeffermann, C. Reppin, B. Aschenbach,W. Bornemann, et al., A&A 365, L18 (2001).
[10] Xmm-newton science analysis system,http://xmm.esa.int/sas/.
[11] A. M. Read and T. J. Ponman, A&A 409, 395 (2003).[12] K. D. Kuntz and S. L. Snowden, A&A 478, 575 (2008).[13] A. Boyarsky, O. Ruchayskiy, D. Iakubovskyi, M. G. Walker,
S. Riemer-Sørensen, and S. H. Hansen, MNRAS 407, 1188(2010).
[14] A. De Luca and S. Molendi, Astron. Astrophys. 419, 837(2004).
[15] Fin over fout public script, v. 1.1,http://xmm.vilspa.esa.es/external/xmm_sw_cal/background/Fin_over_Fout.
[16] D. Iakubovskyi, Ph.D. thesis, Leiden University (2013).[17] T. Abbey, J. Carpenter, A. Read, A. Wells, Xmm Science Cen-
tre, and Swift Mission Operations Center, in The X-ray Uni-verse 2005, edited by A.Wilson (2006), vol. 604 of ESA SpecialPublication, p. 943.
[18] Xmm-newton epic mos1 ccd6 update,http://xmm.esac.esa.int/external/xmm_news/items/MOS1-CCD6/.
[19] Irby, B., The ftools webpage, HeaSoft,http://heasarc.gsfc.nasa.gov/docs/software/ftools/ftools menu.html (2008).
[20] J. A. Carter and A. M. Read, A&A 464, 1155 (2007).[21] D. B. Henley and R. L. Shelton, Astrophys.J.Suppl. 202, 14
(2012).[22] E. Corbelli, S. Lorenzoni, R. A. M. Walterbos, R. Braun, and
D. A. Thilker, A&A 511, A89 (2010).[23] A. Simionescu, S. W. Allen, A. Mantz, N. Werner, Y. Takei,
R. G. Morris, A. C. Fabian, J. S. Sanders, P. E. J. Nulsen, M. R.George, et al., Science 331, 1576 (2011).
[24] L. Chemin, C. Carignan, and T. Foster, Astrophys. J. 705, 1395(2009).
[25] M. A. Sanchez-Conde, M. Cannoni, F. Zandanel, M. E. Gomez,and F. Prada, JCAP 1112, 011 (2011).
[26] O. Urban, A. Simionescu, N. Werner, S. Allen, S. Ehlert, et al.,MNRAS 437, 3939 (2014).
[27] A. Boyarsky, A. Neronov, O. Ruchayskiy, and I. Tkachev, Phys.Rev. Lett. 104, 191301 (2010).
[28] L. J. King and J. M. G. Mead, MNRAS 416, 2539 (2011).[29] R. Mandelbaum, U. Seljak, and C. M. Hirata, JCAP 0808, 006
(2008).[30] S. Dodelson and L. M. Widrow, Phys. Rev. Lett. 72, 17 (1994).[31] X.-d. Shi and G. M. Fuller, Phys. Rev. Lett. 82, 2832 (1999).[32] M. Shaposhnikov, JHEP 08, 008 (2008).[33] M. Laine and M. Shaposhnikov, JCAP 6, 31 (2008).[34] T. Takahashi, K. Mitsuda, R. Kelley, H. Aharonian, F. Aarts,
et al., 1210.4378 (2012).[35] A. Boyarsky, J. W. den Herder, A. Neronov, and O. Ruchayskiy,
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Boyarski et al.
Walter M. Bonivento - CERN/INFN Cagliari CNS1 Elba 20/05/2104
Conclusioni• Test di una spiegazione alternativa rispetto ai soliti
modelli (SUSY, ED) di importanti fenomeni osservati non compatibili con il Modello Standard !
• L’osservazione di decadimenti nell’esperimento e’ manifestazione diretta di Nuova Fisica!
• Tecniche complementari rispetto a esperimenti esistenti —>lunghe vite medie, alta intensità’!
• Anche fisica dei neutrini attivi, per gli appassionati
37
Backup
Walter M. Bonivento - CERN/INFN Cagliari 38 CNS1 Elba 20/05/2104
Walter M. Bonivento - CERN/INFN Cagliari CNS1 Elba 20/05/2104
Il fascio• Fascio SPS estratto
400GeV; intensità’ come CNGS 4.5x1019 pot/anno.
• Se upgrade PS si puo’ arrivare a 7x1019
• caratteristiche dei fasci discusse in grande dettaglio con esperti del CERN —>design realistico —>5 anni di run SENZA UPGRADE: 2x1020pot
39
Walter M. Bonivento - CERN/INFN Cagliari CNS1 Elba 20/05/2104
Possibile zona sperimentale
40
Estrazione in SPS-LSS2, beam switch lungo la transfer line (TT20) alla posizione dei magneti di splitting MSSB2117. Studio di fattibilita’ in corso al CERN. gli studi effettuati per il proposal della facility del neutrino molto utili per noi
Rivelatore posto IN SUPERFICIE
Walter M. Bonivento - CERN/INFN Cagliari CNS1 Elba 20/05/2104
Stato della proposta (i)• SPC EOI-2013-010 + addendum sottomessa Ottobre 2013 e discussa alla
riunione. EOI trasmessa e discussa al Research Board ma non ancora valutata da quest’ultimo.!
• interazione con referee di SPSc e discussione alla riunione di Gennaio 2014. !
• Raccomandazione SPSc: The Committee received with interest the response of the proponents to the questions raised in its review of EOI010. The SPSC recognises the interesting physics potential of searching for heavy neutral leptons and investigating the properties of neutrinos. Considering the large cost and complexity of the required beam infrastructure as well as the significant associated beam intensity, such a project should be designed as a general purpose beam dump facility with the broadest possible physics programme, including maximum reach in the investigation of the hidden sector. To further review the project the Committee would need an extended proposal with further developed physics goals, a more detailed technical design and a stronger collaboration.
41
Walter M. Bonivento - CERN/INFN Cagliari CNS1 Elba 20/05/2104
• L’esperimento richiede un magnete dipolare simile a quello di LHCb, ma con 40% meno ferro e tre volte meno potenza dissipata.
!• LHCb: 4Tm e Apertura di ~ 16 m2 !
• Questo design: ! - Apertura 20 m2 - Due bobine di Al-99.7 - Campo di picco ~ 0.2 T - Integrale di campo ~ 0.5 Tm su 5 m !!!
Il magnete (x2)
42
Walter M. Bonivento - CERN/INFN Cagliari CNS1 Elba 20/05/2104
Altri canaliUn calorimetro e.m. permette la ricostruzione di modi addizionali di decadimento:!
N—>e+π- che permette di accedere al limite su Ue (essendo la struttura di flavor non nota questi canali potrebbero anche essere favoriti!)!
N—>μ+ρ- con ρ- —>π-π0 che permette di migliorare il limite su Uμ (tipicamente lo stesso BR di μ+π-, per m>700Mev)
43
Assumendo celle calorimetriche di 10cm