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

  1. Da rk ma tte r fro m Ze V to a e V: 3 rd I Da rk ma tte r fro m Ze V to a e V: 3 rd I BS-MultiDa rk-I BS-MultiDa rk-I PPP Wo rksho p PPP Wo rksho p Durha m, No ve mb e r 2016 Durha m, No ve mb e r 2016 Jua nde Zo rno za (I Jua nde Zo rno za (I F F I I C, UV-CSI C, UV-CSI C) C)

  2.  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

  4. T he e vide nc e fo r the e xiste nc e  Viria l the o re m o 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 Co mma Cluste r Ro ta tio n c urve s Co smic Mic ro wa ve Ba c kg ro und Bulle t Cluste r Gra vita tio na l L e nsing + BNN, N-b o dy simula tio ns…

  5.  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! PAME L A, AMS F E RMI , MAGI C ANT ARE S, I c e Cub e … I ndire c t de te c tio n Dire c t de te c tio n χ XE NON q , W + , Z… I n a ny c a se : CDMS Co GE NT -we wa nt mo re tha n o ne DAMA +a stro physic a l “de te c tio n” ANAI S -re sults (c o nstra ints) o f e a c h pro b e s ( se lf- … stra te g y a re input fo r the o the rs inte ra c tio n o f χ DM a ffe c ting q , W - , Z… da rk ma tte r de nsitie s in g a la xie s…) Ac c e le ra to rs L HC

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

  8.  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 o 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 o 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

  9.  Mo no c hro ma tic 3.5 ke V photon line o b se rve d in da ta o f XMM-Ne wto n fro m 73 g a la xy c luste rs  L o 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 Bulb ul, a rxiv:1402.2301 ne utrinos with m s =7.1 ke V, whic h wo uld b e da rk ma tte r Bo ya rsky, a rxiv:1402.4119  Also o b se rve d in Andro me da a nd Pe rse us

  10. nte rpre ta tio n a s ste rile ne utrino (sin 2 (2 θ ) ∼ 7x10 -11 ) c o nsiste nt I  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 ) Bulb ul, a rxiv:1402.2301 Bo ya rsky, a rxiv:1402.4119

  11. Astro -H  Astro -H sa te llite (a ka Hito mi), e q uippe d with Cha ndra 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 • Ne w a na lysis b y Cha nd ra b a se d o n me a sure me nts o f the line s in Pe rse us o 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  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 Astronomy & Astrophysics 592: A112 (2016)

  13. Photon a nd pr oton me a n fre e ra ng e pa th  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 o n) a re ne de d γ ν n p

  14. 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 ta rg e t  ARGE  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 o r lo w e ne rg ie s, a po o l is via b le : SK Che re nko v lig ht lig ht de te c to rs (pho to multiplie rs)

  15. Ca sc a de s a re a n impo rta nt  Cle a r sig na ture o f o sc illa tio ns.  a lte rna tive sig na ture : ANT ARE S is to o sma ll to de te c t  de te c tio n o f e le c tro n a nd ta u do ub le b a ng sig na ture (the y a re ne utrino s. to o ra re ) Also ne utra l inte ra c tio n  Ho we ve r, c ub ic -kilo me te r  c o ntrib ute (o nly ha dro nic te le sc o pe s c o uld de te c t the m c a sc a de ) Ma ximum se nsitivity a t 1-10 Pe V  tra c k c a sc a de do ub le b a ng τ ν τ 1 km a t 300 Ge V 5-10 m lo ng 25 km a t 1 Pe V d ia me te r ~ 10 c m

  16.  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) p a tm b a c kg ro und lux µ F c o smic sig na l ν ν E ne rg y p

  17. 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: a rg e r sc a tte ring le ng th → b e tte r a ng ula r re so lutio n  L  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 40 K b a c kg ro und, no b io fo uling  E a sie r de plo yme nt  L o 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.

  18. 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 ANT ARE S GVD K M3Ne T SK I c e Cub e

  19. I c e Cub e (So uth Po le ) ANT ARE S/ K M3Ne T (43° No rth) (a ng . re s.: 0.5°) (a ng . re s.: ~0.3°/ 0.1°) Mkn 421 Mkn 501 Mkn 501 Cr ab Cr ab RX J1713.7- 39 Ve to o r HE thre sho ld Ve la SS433 SS433 GX339- 4 te c hniq ue s a llo w Galac tic SH… a t a pric e Ce ntr e

  20. Orig in o f c o smic ra ys  De te c to r size Ha dro nic vs. le pto nic sig na ture s  Ne utrino ma ss hie ra rc hy  Da rk ma tte r  L imita tio n a t Supe rno va e L imita tio n a t lo w hig h e ne rg ie s: Osc illa tio ns-Ma ss hie ra rc hy e ne rg ie s: F a st de c re a sing -Sho rt muo n ra ng e Dar k matte r -2 , E -3 fluxe s E -L o w lig ht yie ld Astro physic a l ne utrino s - 40 K (in wa te r) GZK Me V Ge V T e V Pe V E e V De te c to r de nsity Othe r physic s: mo no po le s, nuc le a rite s, L o re ntz inva ria nc e , e tc ...

  21. 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 χ Sun E ar th ν µ µ De te c tor

  22.  L imits o n ne utrino c ha nne l  F o 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

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

  24. Diffe re ntia l ne utrino flux is re la te d I f we a ssume with the a nnihila tio n ra te a s: 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:

  25.  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: T ypic a lly Ma xwe ll distrib utio n o f  Sun: 620 km/ s ve lo c itie s is a ssume d  E a rth: 11-15 km/ s Othe r v distrib utio ns: <20% c ha ng e in C Cho i e t a l. JCAP 1405 (2014) 049

  26. 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)  o 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

  27.  Ga mma ra ys, ne utrino s (a nnihila tio n): ( γ  γ , ν ) Da rk ma tte r distrib utio n Pa rtic le Physic s (J-fa c to r) (fo r de c a y: ~ ρ )  Co smic ra ys:  pro pa g a tio n mo re c o mple x

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