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A Cosmological Perspective

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A Cosmological Perspective Dark Matter: A Cosmological Perspective Katie Mack North Carolina State University www.astrokatie.com : @AstroKatie entire Standard Model of Particle Physics What We Don’t Know Origin / particle type Particle mass Thermal history Non-trivial evolution? Particle Zoo One component or many? Non-gravitational interactions (self or SM)? Small-scale behavior (mass of smallest halos) Candidates (incomplete list) ✦ Weakly Interacting Massive Particles (WIMPs) ‣ Something not included in the Standard Model of Particle Physics, generally with weak interactions ‣ May be thermally produced (or not) Annihilating (e.g., SUSY neutralino WIMP) Decaying (e.g., sterile neutrino) Warm (WDM) (e.g., axino) Self-interacting (SIDM) (particle + dark sector force) Axion (e.g., QCD axion / string axion) Fuzzy DM (tiny mass, large deBroglie wavelength) MACHO (e.g., primordial black holes) WIMP Miracle Standard thermal WIMP dark matter • freezes out when no longer in thermal equilibrium with baryons • for weak-scale mass and cross-section, predict correct abundance of DM • discovery opportunities: annihilation, scattering, production Kolb & Turner 1990 WIMP Direct Detection 10 −38 ] 2 CRESST-II 10 −40 (2015) CDMSLite (2017) S DAMA −42 u 10 p e r C D M 10 −44 S PICO-2L E (2015) D E L CoGeNT pp 7 (2 W 0 Be 1 − 6 E 46 ) IS (2014) 10 S PICO-60 (2015) 8 DarkSide-50 10 −48 B (2015) PandaX (2016) LUX (2016) hep Solar XENON1T (2017) − SI10 WIMP-nucleon50 cross section [cm -ν LZ 10 −1 DARWIN 200 ton-year 10 0 SN-ν 10 1 Atm WIMP mass [GeV/c -ν 10 2 10 3 2] 10 4 plot via Ciaran O’Hare XENON1T Excess • may be background, or… • solar axions / ALPs? (but stellar constraints) • hidden photon DM? XENON1T Collaboration 2020 • fast (subdominant) DM component? • …? TBD. Directional Detection8 Fluorine recoils [8–50 keVr] September 6 +90◦ ‣ unique opportunity 5.5 d b +60◦ R/ to probe below 4.5 d 9 GeV/c +30◦ Ω r Solar neutrinos “neutrino floor” Galactic 3.5 [ton 0◦ plane − Ecliptic 2.5 1 2 30◦ sr WIMP − − 1 1.5 ] Galactic latitude, ‣ CYGNUS feasibility 60◦ − 0.5 90◦ paper: Vahsen+2020 − 180◦ 120◦ 60◦ 0◦ 300◦ 240◦ 180◦ 5 Galactic longitude, l arxiv:2008.12587 FIG. 5. Total angular distribution across the sky of WIMP-induced (blue contours) and neutrino-induced (red contours) fluorine 37 Cygnus 6 yrs recoils on September10− 6. We show the distributions in galactic coordinates (l, b) where the line for b =0corresponds to the CRESST ⇥ galactic plane.] 38 Both distributions have been integrated over recoil energy between 8 and 50 keVr.WechooseaWIMPmassof 2 2 10 45 2 8 9GeV c− and− a SI cross section of 5 10− cm so that its signal is of a similar size to that of the B neutrinos. For reference 39 CDMSlite ⇥ DAMA we also show10− the ecliptic in red: the path along which the Sun, shown by a star, moves over the year. Towards the center of the WIMP recoil distribution we also show the stars of the Cygnus constellation. The blue line which encircles the star Deneb 40 shows the variation10− in the peak direction of the DM wind over the year. PICO2L CYGNUS-KM DarkSide CYGNUS-10 Kamioka, Japan 41 Boulby, UK 10− COSINE-100 CYGNUS 42 3 angular resolution10− of the detector). The separation is unknown) DMPICO60 cross section ,itsprecisevalueisoflow large enough that43 it is possible to discriminateEDELWEISS the two importance before a detection is made. 10− signals even if the recoil vectors cannot be oriented in On the otherPandaX hand the great deal of uncertainty sur- galactic coordinates44 as shown here. This would be the rounding the velocity distribution of the DM is generally 10− He Xenon1T case for experiments45 in which recoil vectors were only more important to understand. The benchmark model 10− F 3 measured after beingXe projected on to a plane [36], or if assumed since the very first direct detection experimentsYGNUS CYGNO 46 10k m C -HD10 timing information10− was unavailable [37]. were conducted is the Standard Halo ModelLead, (SHM), South Dakota in Gran Sasso, Italy 47 which the Milky Way’s3 DM forms an isothermal sphere. 10− The motivation is that it is the simplest model that gives CYGNUS-OZ 48 100k m 10− rise to flat rotation curves. The SHM has a Gaussian dis- Stawell, Aus. tribution for f(v) (or Maxwellian distribution for f(v)), 49 Single electron threshold: 0.25 keVr [755:5 Torr He:SF6] SI WIMP-proton10 cross section− [cm CYGNUS-Andes Worst-case threshold: 8 keVr [755:5 Torr He:SF6] 2 50 3. WIMP astrophysics 1 v Chile/Argentina 10− Search mode: 8 keVr [760 Torr SF6] f(v)= 2 3/2 exp | |2 ⇥(vesc v ) . (9) 51 (2⇡v) Nesc − 2σv − | | 10− 1 0 1 2 3 4 ✓ ◆ 10− 10 10 10 10 10 Predicting WIMP signals requires astrophysical input Under2 the isothermal SHM, the dispersion is related to in the form of the DM velocity distribution,WIMPf( massv),aswell [GeV/cthe] local rotation speed of circular orbits: σv = v0/p2. as the local density of DM ⇢0.Whiletheformerisnot The benchmark used for this speed is the now similarly 1 known concretely, the latter can be determined with as- out-of-date value of v0 220 km s− .Amorerecent ⇠ 1 tronomicalFIG. data. 3. Constraints Decades of attempts on the to spin-independent constrain this analysis WIMP-nucleon indicates a value (left) of v0 = and 235 km spin-dependent s− [82]. As is WIMP-proton (right) cross sections. 3 value have begun to settle towards ⇢ 0.5 GeV cm− convention, the velocity distribution has been truncated We show the existing constraints⇡ and detections from various experiments as labeled (see text for the associated references). In (see,purplee.g. Refs. solid [74–78 and]andRef.[ dashed79]forareviewonmeth- lines we show our projectedat the escape 90% speed CLvesc exclusion, with the limits constant forNesc theusedCygnus to experiment operating for six years ods). However the3 standard value used3 by experimental renormalize the distribution after this truncation.3 Ex- 3 collaborationswith 10 is m0.3upGeV to cm 100,000− .Upcominganalyseswith m of He:SF6 gasperimental at 755:5 Torr analyses (where typically 6 years have assumed1000 mvesc corresponds= 544 to a 1ton-yearexposure).For 1 ⇥ ⇠ the extremelyeach volume high and we precise show statistics limits offor the two astromet- possibleor thresholds,533 km s− ,thelatterbeingthemorerecentRAVE ranging from the worst-case electron discrimination threshold of 8 keVr ric survey Gaia [80]areexpectedtoleadtoevenmore to a very best-case minimum threshold corresponding to a single electron, 0.25 keVr.Weemphasizehoweverthatweanticipate tightly constrained values in the next few years. Since 3 the localelectron dark matterdiscrimination density only well amounts below to 8 a keV mul-r.Forthe100km limits we add a third dotted line which corresponds to a mode with 3 tiplicativepurely factor SF6 whichgas can at 760 be absorbed Torr. This into the experiment (also Although, would see have Ref. [81 a] significantlyfor a specific case where higher this is total not true. mass but would come at the cost of any directional sensitivity. This ‘search mode’ could be used to extend the high mass sensitivity to just within reach of the neutrino floor. For the SI panel, we shade in gray the neutrino floor for helium, fluorine, and xenon targets (top to bottom), and for SD we show only fluorine and xenon. We define the neutrino floor as the cross section limit at which the rate of improvement with increasing exposure is the slowest in standard direct detection–the effect that Cygnus aims to circumvent. This definition corresponds to (100) neutrino events. O WIMP velocity, v, with the outgoing recoil direction ˆr, be such a powerful means to discover DM. The pri- mary signal is a dipole anisotropy towards the direction m E ˆr = vˆ ,leadingtoan (10) forward-backward asym- ˆ = A r v , − lab O v r 2 min (5) metry in the number of recoil events. The strength of · s 2µχA ⌘ this dipole means that in ideal circumstances (i.e. perfect which can be enforced in the differential cross section recoil direction reconstruction) an isotropic null hypoth- with a delta function, esis for the recoil direction distribution can be rejected at 90% confidence with only (10) events [43, 50]. With 2 O d σ dσ 1 (30) recoil directions it becomes possible to point back = v δ (v ˆr vmin) , (6) O dEr d⌦ dEr 2⇡ · − towards Cygnus and confirm the galactic origin of the sig- nal [44]. Secondary signals such as a ring feature at low where d⌦ is the solid angle element around ˆr. The event energies [51], and the aberration of recoil directions over rate then has the structure, time [52], may also aid in the confirmation of a DM sig- 2 nal, as well as for characterizing astrophysical properties d R ⇢0 SI 2 SD 2 (Er, ˆr,t)= 2 (σ0 FSI(E)+σ0 FSD(E)) of the DM halo. dErd ⌦ 4⇡µχpmχ fˆ(vmin, ˆr,t) , (7) ⇥ Existing limits and projections for Cygnus where the velocity distribution now enters in the form of its Radon transform [48, 49], Figure 3 shows a selection of constraints from di- rect detection experiments along with our headline re- ˆ 3 f(vmin, ˆr,t)= δ (v ˆr vmin) f(v,t) d v . (8) sult: the WIMP reach of Cygnus. Constraints ex- · − 2 Z ist for WIMPs with masses larger than 1 GeV c− 46⇠ 2 The characteristic angular structure of the DM flux and SI cross sections larger than 10− cm .Under- ⇠ on Earth is the reason why directional detection could neath these limits lies the neutrino floor, below which Candidates (incomplete list) ✦ Weakly Interacting Massive Particles (WIMPs) ‣ Something not included in the Standard Model of Particle Physics, generally with weak interactions ‣ May be thermally produced (or not) Annihilating (e.g., SUSY neutralino WIMP) Decaying (e.g., sterile neutrino) Warm (WDM) (e.g., axino) Self-interacting (SIDM) (particle + dark sector force) Axion (e.g., QCD axion / string axion) (Mack 2011; Mack & Steinhardt 2011) Fuzzy DM (tiny mass, large deBroglie wavelength) MACHO (e.g., primordial black holes) (Mack, Ostriker & Ricotti 2007; R,O,M 2008) Candidates (incomplete list) 6 M.R.
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