Jua nde Zo rno za (I Jua nde Zo rno za (I F F I I C, UV-CSI - - PowerPoint PPT Presentation

Da rk ma tte r fro m Ze V to a e V: 3rd I BS-MultiDa rk-I PPP Wo rksho p Durha m, No ve mb e r 2016

Jua nde Zo rno za (I F I C, UV-CSI C) Jua nde Zo rno za (I F I C, UV-CSI C)

Da rk ma tte r fro m Ze V to a e V: 3rd I BS-MultiDa rk-I PPP Wo rksho p Durha m, No ve mb e r 2016

 I

ntro duc tio n

 X-ra ys a nd ste rile ne utrino s  Ne utrino te le sc o pe s  Re sults

• Sun
• E

a rth

• Milky Wa y
• E

xtra -g a la c tic

 F

uture

 Summa ry



T he e vide nc e fo r the e xiste nc e

• f da rk ma tte r is ve ry so lid a nd,

whic h is ve ry impo rta nt, a t ma ny diffe re nt sc a le s

Viria l the o re m Co mma Cluste r Ro ta tio n c urve s Co smic Mic ro wa ve Ba c kg ro und Gra vita tio na l L e nsing Bulle t Cluste r

+ BNN, N-b o dy simula tio ns…

 We do no t kno w wha t is da rk ma tte r, so it is ha rd to sa y

whic h is the winning stra te g y: multi-fro nt a tta c k!

χ χ

q , W+, Z… q , W-, Z… Dire c t de te c tio n I ndire c t de te c tio n Ac c e le ra to rs

XE NON CDMS Co GE NT DAMA ANAI S … PAME L A, AMS F E RMI , MAGI C ANT ARE S, I c e Cub e … L HC

I n a ny c a se :

• we wa nt mo re tha n o ne

“de te c tio n”

• re sults (c o nstra ints) o f e a c h

stra te g y a re input fo r the o the rs

+a stro physic a l pro b e s ( se lf- inte ra c tio n o f DM a ffe c ting da rk ma tte r de nsitie s in g a la xie s…)

Cre dit: Sky & T e le sc o pe / Gre g g Dinde rma n

 X-ra y a stro no my (1-100 ke V) diffe rs fro m g a mma ra y

a stro no my in the de te c tio n stra te g y

 Atmo sphe re a b so rb s X-ra ys a nd fluxe s a re hig h, so

• b se rva tio n is b a se d o n b a llo o ns a nd sa te llite s

 X-ra ys c a nno t b e fo c use d b y le nse s, so fo c using is b a se d

• n to ta l re fle c tio n (Wo lte r te le sc o pe )

 Pro je c ts: Cha ndra , XMM-Ne wto n, Suza ku

XMM-Ne wto n: L a rg e c o lle c ting a re a Simulta ne o us ima g ing a nd hig h re so lutio n spe c tro sc o py

 Mo no c hro ma tic 3.5 ke V photon line

• b se rve d in da ta o f XMM-Ne wto n

fro m 73 g a la xy c luste rs

 L

• c a te d within 50-100 e V o f se ve ra l

kno wn fa int line s

 I

nte rpre te d a s de c a y from ste rile

ne utrinos with m s=7.1 ke V, whic h

wo uld b e da rk ma tte r

 Also o b se rve d in Andro me da a nd

Pe rse us

Bo ya rsky, a rxiv:1402.4119 Bulb ul, a rxiv:1402.2301



I nte rpre ta tio n a s ste rile ne utrino (sin2 (2θ)∼7x10-11) c o nsiste nt with pre se nt c o nstra ints



Ho we ve r, sig nific a nt a stro physic a l unkno wns invo lve d (fo r insta nc e , po ta ssium XVI I I line )

Bo ya rsky, a rxiv:1402.4119 Bulb ul, a rxiv:1402.2301

• Ne w a na lysis b y Cha nd ra b a se d o n
• b se rva tio ns o f 33 g a la c tic c luste rs

ne ithe r find s a nd e xc e ss

Cha ndra

Astronomy & Astrophysics 592: A112 (2016)



Astro -H sa te llite (a ka Hito mi), e q uippe d with a X-ra y spe c tro me te r, wa s la unc he d in F e b 2016.



It ha d the c a pa b ility o f a c c ura te spe c tra l me a sure me nts o f the line s in Pe rse us



Unfo rtuna te ly, o n Ma rc h 2016 the o rie nta tio n c o ntro l sto ppe d wo rking a nd is no t o pe ra tive a nymo re .



So me first me a sure me nts we re do ne during the c a lib ra tio n pha se . No hint o f X-ra y in the re g io n o f inte re st

Astro -H

 Adva nta g e s:

• Pho to ns: inte ra c t with CMB

a nd ma tte r

• Pro to ns: inte ra c t with CMB

a nd a re de fle c te d b y ma g ne tic fie lds

 Dra wb a c k: la rg e de te c to rs

(~GT

• n) a re ne de d

Photon a nd pr

• ton me a n fre e ra ng e pa th

p

ν

n

γ

Che re nko v lig ht lig ht de te c to rs (pho to multiplie rs)

Whe re to put the de te c to r? 1) I n a tra nspa re nt me dium 2) Ne utrino s inte ra c t we a kly 

 We ne e d a L

ARGE ta rg e t 

 I

t ha s to b e c he a p  Na tura l me dium

 Oc e a ns (o r la ke s) o r Anta rc tic ic e

*F

• r lo w e ne rg ie s, a

po o l is via b le : SK



Cle a r sig na ture o f o sc illa tio ns.



ANT ARE S is to o sma ll to de te c t do ub le b a ng sig na ture (the y a re to o ra re )



Ho we ve r, c ub ic -kilo me te r te le sc o pe s c o uld de te c t the m



Ma ximum se nsitivity a t 1-10 Pe V

1 km a t 300 Ge V 25 km a t 1 Pe V 5-10 m lo ng d ia me te r ~ 10 c m

tra c k c a sc a de

ντ τ

do ub le b a ng



Ca sc a de s a re a n impo rta nt a lte rna tive sig na ture : de te c tio n o f e le c tro n a nd ta u ne utrino s.



Also ne utra l inte ra c tio n c o ntrib ute (o nly ha dro nic c a sc a de )

p

ν

p

µ ν



T he re a re two kinds o f b a c kg ro und:

• Muo ns pro duc e d b y c o smic ra ys in the

atmosphere (→ detector deep in the sea and

se le c tio n o f up-g o ing e ve nts)

• Atmo sphe ric ne utrino s (c ut in the e ne rg y)

E ne rg y F lux a tm b a c kg ro und c o smic sig na l



Ve ry la rg e vo lume s o f me dium tra nspa re nt to Che re nko v lig ht a re ne e de d:

• Oc e a n, la ke s…
• Anta rc tic ic e



Adva nta g e s o f o c e a ns:

• L

a rg e r sc a tte ring le ng th → b e tte r a ng ula r re so lutio n

• We a ke r de pth-de pe nde nc e o f o ptic a l pa ra me te rs
• Po ssib ility o f re c o ve ry
• Cha ng e a b le de te c to r g e o me try



Adva nta g e s o f ic e :

• L

a rg e r a b so rptio n le ng th

• No b io lumine sc e nc e , no 40K

b a c kg ro und, no b io fo uling

• E

a sie r de plo yme nt

• L
• we r risk o f po int-fa ilure



Anywa y, a de te c to r in the No rthe rn He misphe re in ne c e ssa ry fo r c o mple te sky c o ve ra g e (Ga la c tic Ce nte r!), a nd it is o nly fe a sib le in the o c e a n.

I c e Cub e ANT ARE S K M3Ne T



Se ve ra l pro je c ts a re wo rking / pla nne d, b o th in ic e a nd o c e a n a nd la ke s.

Ba ika l GVD SK

Mkn 501 Mkn 421 Cr ab SS433 Mkn 501 RX J1713.7- 39 GX339- 4 SS433 Cr ab Ve la Galac tic Ce ntr e

I c e Cub e (So uth Po le ) (a ng . re s.: 0.5°) ANT ARE S/ K M3Ne T (43° No rth) (a ng . re s.: ~0.3°/ 0.1°)

Ve to o r HE thre sho ld te c hniq ue s a llo w SH… a t a pric e

Me V Ge V T e V Pe V E e V Astro physic a l ne utrino s

Dar k matte r

Osc illa tio ns-Ma ss hie ra rc hy Supe rno va e GZK

L imita tio n a t hig h e ne rg ie s: F a st de c re a sing fluxe s E

• 2, E
• 3

L imita tio n a t lo w e ne rg ie s:

• Sho rt muo n ra ng e
• L
• w lig ht yie ld
• 40K

(in wa te r)

Othe r physic s: mo no po le s, nuc le a rite s, L

• re ntz

inva ria nc e , e tc ...

De te c to r de nsity De te c to r size



Orig in o f c o smic ra ys



Ha dro nic vs. le pto nic sig na ture s



Ne utrino ma ss hie ra rc hy



Da rk ma tte r

E ar th

De te c tor

νµ

µ

χ

Sun



WI MPs (ne utra lino s, K K pa rtic le s) a re a mo ng the mo st po pula r e xpla na tio ns fo r da rk ma tte r



T he y wo uld a c c umula te in ma ssive o b je c ts like the Sun, the E a rth o r the Ga la c tic Ce nte r



T he pro duc ts o f suc h a nnhilia tio ns wo uld yie ld “hig h e ne rg y” ne utrino s, whic h c a n b e de te c te d b y ne utrino te le sc o pe s

 L

imits o n ne utrino c ha nne l

 F

• r the Sun a na lysis:
• No de pe nde nc e o n stre a m, struc ture s,

sub ha lo e s, e tc . o r the pro pe rtie s o f the Ga la c tic ma g ne tic o r ra dia tio n fie lds

• A sig na l wo uld b e ve ry c le a n (the a stro physic s

a re we ll kno wn), c o mpa re d with o the r indire c t se a rc he s (whic h c a n b e a lso inte rpre te d a s pulsa rs, e tc .)

• Give n a da rk ma tte r c a ndida te , the sig na l c a n

b e we ll pre dic te d. I f no t o b se rve d the mo de l is rule d o ut

Sun Ga la c tic Ce ntre E a rth Dwa rf g a la xie s Ga la xy c luste rs Ga la c tic Ha lo

Diffe re ntia l ne utrino flux is re la te d with the a nnihila tio n ra te a s: I f we a ssume e q uilib rium b e twe e n c a pture a nd a nnihila tio n in the Sun: whe re the c a pture ra te c a n b e e xpre sse d a s:

 Ne utrino te le sc o pe s

(fo r se a rc he s in the Sun) c o mple me nta ry to dire c t se a rc he s

• lo w ve lo c ity: e a sie r to

c a pture in the Sun

• hig h ve lo c ity: la rg e

re c o ils e a sie r a t hig h ve lo c itie s

 E

sc a pe ve lo c ity:

• Sun: 620 km/ s
• E

a rth: 11-15 km/ s

T ypic a lly Ma xwe ll distrib utio n o f ve lo c itie s is a ssume d

Othe r v distrib utio ns: <20% c ha ng e in C Cho i e t a l. JCAP 1405 (2014) 049



E ffe c t o f unc e rta intie s in ve lo c ity distrib utio ns fo r Sun re sults (Cho i e t a l., a rxiv:1312.0273)

• rb ita l spe e d o f the Sun
• e sc a pe ve lo c ity o f da rk ma tte r fro m the ha lo
• da rk ma tte r ve lo c ity distrib utio n func tio ns
• e xiste nc e o f a da rk disc



Only the e xiste nc e o f da rk disk wo uld ha ve a re le va nt (a nd ve ry po sitive ) e ffe c t)



Co mple me nta ry wa y to de a l with dire c t se a rc he s unc e rta intie s

 Ga mma ra ys, ne utrino s (a nnihila tio n):

 Co smic ra ys:

• pro pa g a tio n mo re c o mple x

Da rk ma tte r distrib utio n (J-fa c to r) Pa rtic le Physic s

(γ  γ,ν)

(fo r de c a y: ~ρ)

 Ma ny pro file s a va ila b le

• n the ma rke t

Cire lli e t a l., 1012.4515v4



NF W, E ina sto : c uspy, re sult fro m simula tio ns



I so the rma l, Burke rt: mo tiva te d b y

• b se rva tio ns o f g a la c tic ro ta tio n c urve s



E ffe c t o f b a ryo ns unkno wn



Ma yb e no t sphe ric a l (tria xia l)



Da rk disk: ve ry g o o d fo r NT s



Our g a la xy ve ry diffic ult to study!

a ne w o ne : Mc Milla n (MNRAS 414 (2016) 2446.)

 I

nte g ra te d J-fa c to r (in ne w ANT ARE S a na lysis):

*J-fa c to rs c a n b e c a lc ula te d with pa c ka g e s like CL UMPY (A. Cha rdo nnie r, C. Co m

• D. Ma urin, Co mp. Phys. Co mm. 183, 656 (2012))

 Simula tio ns fa vo r tha t the DM c o lla pse g ive

“c uspy” pro file s, i.e . mo re pe a ke d (g o o d fo r e nha nc ing the sig na l)

 Ob se rva tio ns o f ro ta tio n c urve s o f g a la xie s fa vo r

“c o re d” pro file s, i.e . c o nsta nt de nsity c o re s

 Sub struc ture no t we ll re so lve d b e lo w ~105M,

whic h ma y ha ve a n impo rta nt e ffe c t due to the

ρ2 de pe nde nc y o f sig na l

 E

ffe c t o f b a ryo ns is still unc le a r:

• ste e pe ning thro ug h a dia b a tic c o ntra c tio n
• fla tte ning thro ug h sta r b ursts

 2nd g e ne ra tio n o f

wa te r Che re nko v ta nk de te c to rs (1996-2016)

 50 kto n de te c to r

(22.5 kto n fiduc ia l ma ss)

 F

• r da rk ma tte r,

c o mpe titive a t lo w ma sse s (~10 Ge V)

NT

• 200



Histo ry o f the pro je c t



sinc e 1980: site studie s



1984 first sta tio na ry string



1993 NT

• 36 sta rte d



1994 first a tmo sphe ric ne utrino ide ntifie d



1998 NT

• 200 c o mmissio ne d



2005: NT 200+ c o mmissio ne d

GVD c luste r with 8 string s

Sta tus a nd pla ns

• Pro to type line de plo ye d in 2011
• One c luste r (“DUBNA”)

de plo ye d (2015). Upg ra de d in 2016

• T

wo mo re to b e insta lle d b y 2017

• E

ig ht c luste rs b y 2020 (2304 OMs)

Ic e T

• p

80 pa irs o f ic e Che re nko v ta nks T hre sho ld ~ 300 Ge V

Ic e Cube Ar r a y

80 string s with 60 OMs 17 m b e twe e n OMs 125 m b e twe e n string s 1 km 3. A 1-Gto n de te c to r

I c e Cub e + De e p Co re = 5160 OMs

De e p Cor e

6 string s with 60 HQE OMs I nne r pa rt o f the de te c to r

Horizontal layout

• 12 lines (885 PMTs)
• 25 storeys / line
• 3 PMT / storey

14.5 m ~60-75 m Buoy 350 m 100 m Junction box Readout cables Electro-

• ptical

cable Storey



Sun

• ANT

ARE S Co ll. Physic s L e tte rs B, Vo lume 759, 10

• ANT

ARE S Co ll. JCAP 1605 (2016) no .05, 016

• Ic e Cube Co ll. PRL

110, 131302 (2013)

• Ic e Cube Co ll., JCAP 04 (2016) 022
• Ba ika l Co ll., Astro pa rtic le Physic s (2015), pp. 12-20
• Supe rK

, PRL 114, 141301 (2015) 

E a rth

• Ic e Cube Co ll., a rXiv:1609.01492 (ANT

ARE S pa pe r in pre pa ra tio n) 

Ga la tic Ce ntre

• ANT

ARE S Co ll. JCAP 1510 (2015) no .10, 068 (ne w pa pe r fo r 07-15 in pre pa ra tio n)

• Ic e Cube Co ll. E

ur.Phys.J. C75 (2015) no .10, 492

• Ic e Cube Co ll. a rXiv: 1210.3557
• Ba ika l Astro Phys 81 (2016)



Ha lo

• Ic e Cube Co ll. Phys.Re v. D84 (2011) 022004
• Ic e Cube Co ll. E

ur.Phys.J. C75 (2015) no .99, 20

• Ic e Cube Co ll. E
• ur. Phys. J. C 76, 531 (2016)



Dwa rf g a la xie s a nd g a la xy c luste rs

• Ic e Cube Co ll. Phys.Re v. D88 (2013) 122001



I c e Cub e , two a na lysis:

• HE

(MWIMP>100 Ge V), I c e Cub e -do mina te d

• L

E (MWIMP=30-100 Ge V), De e pCo re -do mina te d



ANT ARE S is sma lle r b ut ha s a b e tte r a ng ula r re so lutio n a nd the Sun is le ss time c lo se to the ho rizo n, whe re the re is mo re b a c kg ro und



SK ha s re c e ntly a lso inc lude d c a sc a de e ve nts in the ir a na lysis

• M. Da nning e r, Ne utrino 2016

ANT ARE S

 F

• r spin-inde pe nde nt NT

s a re no t c o mpe titive with dire c t se a rc he s

• I

n this mo de l the Da rk Ma tte r, is se c lude d fro m ‘ no rma l’ ma tte r b y a

mediator, Φ, which could be some new gauge boson from the dark

se c to r, o r so me o the r c a ndida te .

• I

n the simple st pic ture the da rk ma tte r a nnihila te s into the me dia to r. I f the ma ss o f the da rk ma tte r wa s g re a te r tha n the me dia to r the n the da rk ma tte r wo uld b e le pto philic a nd mig ht b e the e xpla na tio n o f so me

• b se rva tio ns sug g e sting ‘ ne w physic s’
• the r po ssib ilitie s:
• me dia to r  ne utrino s
• me dia to r  di-muo n  ne utrino s

φµµν φµµ φνν

Ro tt, AI P Co nf. Pro c 1743, 020010 (2016)

Ne w ide a : mo no e ne rg e tic ne utrino s pro duc e d in pio n a nd ka o n de c a ys (Me V e ne rg ie s)

• π+  νµ µ+ (29.8 Me V)
• K

+  νµ µ+ (235.6 Me V)

• µ+  a nti-νµ νe (c o nt. ~ fe w-50 Me V)

• L

imits o n spin inde pe nde nt c ro ss se c tio n

• Mo re e ffic ie nt fo r ma sse s c lo se to tho se o f F

e a nd Ni

• Ba c kg ro und ha rde r to e stima te c o mpa re d to

Sun o r GC

• No e q uilib rium b e twe e n c a pture a nd

a nnihila tio n c a n b e a ssume d in g e ne ra l

• Gre a t e nha nc e me nt if the re is a da rk disk

• τE

a rth~1011 y vs to~4.5x109 y 

•  no e q uilib rium b e twe e n c a pture

a nd a nnihila tio n  ΓA ∝ C 2

• we de rive limits o n σSI a s a func tio n
• f < σ v >

ANT ARE S I c e Cub e

 Astro physic a l

b a c kg ro und c o uld b e impo rta nt

 Hig h e ne rg y c o mpo ne nt

no t a b so rb e d (c o ntra ry to the c a se o f the Sun)

 ANT

ARE S: GC mo st o f the time b e lo w the ho rizo n

 I

c e Cub e : GC a lwa ys a b o ve the ho rizo n, ve to te c hniq ue s ne e de d

E (Ge V)



Re sults fo r 2007-2015 re c e ntly unb linde d



Be st re sults a t la rg e ma sse s (b e tte r visib ility o f Ga la c tic Ce ntre )



ANT ARE S: b e tte r tha n I C (a ll ma sse s) a nd b e st limits fo r MWI MP>30 T e V)



No te : Uppe r b o und o n DM ma ss c a n b e se t b y unita rity (Grie st, PRL , 64, 6) a t ~120 T e V (with upda te d va lue fo r h2Ω) b ut fo r so me mo de ls (no n-the rma l pro duc tio n) this is a vo ide d

Altho ug h numb e r de nsity de c re a se s with MWI M, Ve ff a nd a ng ula r re so lutio n impro ve s F

• r I

C, ve to kills sig na l a t la rg e MWIMP



Uppe r b o und o n DM ma ss c a n b e se t b y unita rity (Grie st, PRL , 64, 6) a t ~120 T e V (with upda te d va lue fo r h2Ω)



Ho we ve r, this c a n b e a vo ide d (typic a lly, b y no n-the rma l

me c ha nisms, b ut no t o nly)

• No n-the rma l: Pro fumo , Phys. Re v. D 72, 103521 (2005)
• T

he rma l: Ha rig a ya e t a l., a rxiv:1606.00159v1 (DM a s b o und sta te )



I n a ny c a se , re minde r: ANT ARE S b e a ts the re st o f the g a ng a lre a dy a t 30 T e V

 ANT

ARE S: o the r c ha nne ls, o the r pro file s

• M. Da nning e r, Ne utrino 2016

I n JCAP 05 (2016) 050: g a mma te le sc o pe s mo re se nsitive to ne utrino line s tha n NT s?  NO! (with ne w re sults fro m ANT ARE S)

ANT ARE S 07-13

 T

hre e a na lyse s b y I c e Cub e :

• Cut a nd c o unt (I

C22, 275d)

• Multipo le s (I

C79, 316d)

• All-fla vo r se a rc h (inc lusio n o f

c a sc a de s)

arXiv:1606.00209v1

 Dwa rf g a la xie s a re

sa te llite s o f MW

 L

a rg e Ma ss/ L umino sity

 Sta c king po ssib le (a nd

numb e r inc re a sing )

 K

no wn dista nc e s

Po S I CRC2015 (2016) 1215

 L

a rg e st g ra vita tio na lly b o unde d

• b je c ts in the Unive rse

 Sub struc ture is q uite unc e rta in  Bo o st fa c to rs c o uld b e la rg e

Virg o Ga la xy Cluste r c re d it: E SA

Po S I CRC2015 (2016) 1215

 54 hig h-e ne rg y e ve nts

in the 4 ye a r sa mple (e xpe c te d b a c kg ro und: 21)

 I

nte rpre ta tio n:

• Diffuse flux?
• Ga la c tic c o mpo ne nt?
• De c a ying da rk ma tte r?

 De c a ying DM fro m ha lo

c o uld e xpla in spa tia l distrib utio n o f HE e ve nts

 I

t c o uld b e a lso c o mpa tib le with e ne rg y spe c trum: pe a k a t Pe V a nd c o ntinuum fro m lo w e ne rg y c o ntrib utio n

 Also fa vo ure d b y the

fa c t tha t no e vide nc e fo r SUSY is fo und in a c c e le ra to rs

E xa mple : C. Ro tt e t a l., Phys. Re v. L e tt. D92(2) 023529 (2015)

 T

hird g e ne ra tio n o f la rg e wa te r Che re nko v de te c to r

 0.52 Mto n (380 kto n

fiduc ia l). x10/ x20 Supe r-K

 Pla n: sta rt >2026 (first

ta nk)

 Se nsitivity to WI

MPs fro m Sun, E a rth, Ga la c tic Ha lo

 E

xpe c te d se nsitivity a t 10-39 c m 2 @ 10 Ge V



Mo re re c e nt e stima tio ns:



F ro m Hype r-K L

• I(a rxiv: 1109.3262v1)



Ro o m fro m impro ve me nt:

• fla vo r info rma tio n
• F

ully c o nta ine d sa mple



K M3Ne T is a c o mmo n pro je c t to c o nstruc t ne utrino te le sc o pe in the Me dite rra ne a n with a n instrume nte d vo lume o f se ve ra l c ub ic kilo me te rs



It will a lso b e a pla tfo rm fo r e xpe rime nts o n se a sc ie nc e ,

• c e a no g ra phy, g e o physic s,

e tc .



240 g ro ups o f Astro pa rtic le Physic s a nd Se a Sc ie nc e fro m 12 c o untrie s a re invo lve d



Ne w g ro ups ve ry we lc o me ! (UGR just jo ine d)



Pro to type line s ha ve a lre a dy b e e n insta lle d



T he first K M3Ne T line ha s b e e n insta lle d in De c e mb e r 2015 (a nd two mo re in Ma y 2016)



ARCA (Astro pa rtic le Re se a rc h

with Co smic Ra ys)

• T

e st I c e Cub e sig na l

• I

ta ly

• 2x115 line s
• Spa rse c o nfig ura tio n



ORCA (Osc illa tio n Re se a rc h

with Co smic Ra ys)

• Ma ss o rde ring (a nd DM)
• F

ra nc e

• 115 line s
• De nse c o nfig ura tio n

PHASE 3: F INAL CONF IGURAT ION PHASE 1: PHASE 2.0:



Alre a d y fund e d



31 line s (24 in Ita ly, 7 in F ra nc e )to b e d e plo ye d in 2015-2017



Pro o f o f fe a sib ility a nd first sc ie nc e re sults



6x115 line s (in to ta l)



Ne utrino a stro no my inc luding Ga la c tic so urc e s

 Sa me te c hno lo g y

I ta ly F ra nc e

200 m 1 km 1 km

ORCA ARCA

 26 string s  192 DOMs pe r string  24 m ho rizo nta l spa c ing  1.5 m flo o r spa c ing  L

e ss ho le s to drill simila r pe rfo rma nc e tha n pro po sa l in a rxiv:1401.2046

 F

ive ye a rs fro m c o nstruc tio n sta rt to de te c to r c o mple tio n

a rxiv: 1607.02672

 I

nte rline spa c e : 240 m

 Size : 7 km3  E

nd c o nstruc tio n b y 2031

Sun GC



(Multi-PMT ) Optic a l Mo dule

• 31 x 3” PMT

s

• dia me te r: 17’ ’
• lo w po we r re q uire me nts
• “full” mo dule : no a dditio na l

e le c tro nic s ve sse l ne e de d

• unifo rm a ng ula r c o ve ra g e
• info rma tio n o f the a rriva l

dire c tio n o f pho to ns

• b e tte r re je c tio n o f b a c kg ro und



De te c to r Units (string s)

• 18 DOMs, se pa ra te d ve rtic a lly b y: 6 m

(ORCA) o r 36 m (ARCA)

• a nc ho re d a t se a flo o r b y a de a d

we ig ht

• ke pt ve rtic a l b y b uo ys
• 115 DUs = 1 b uilding b lo c k

• P. Co yle , Ne utrino 16

 Da rk ma tte r is o ne o f the ma jo r q ue stio ns in Physic s

no wa da ys

 T

• find una mb ig uo us e vide nc e o f its de te c tio n re q uire s

multi-fro nt a tta c k

 Ne utrino te le sc o pe s ha ve spe c ific a dva nta g e s

• Sun: fre e o f a stro physic a l b a c kg ro und a nd pro b e o f lo w

ve lo c itie s  ANT

ARE S/ K M3Ne T spe c ific a dva nta g e s:

• Be tte r a ng ula r re so lutio n
• Be tte r visib ility o f the GC

 A pro mising future is b e ing b uilt (ORCA) o r pla nne d

(PI NGU, Hype r-K )