attempt to fit the Pioneer anomaly with dark matter has been suggested. Remarkably, MOG provides a closely fitsolution to the Pioneer 10/11 anomaly and is consistent with the accurate equivalence principle, all current satellite,laser ranging observations for the inner planets, and the precession of perihelion for all of the planets.A fit to the acoustical wave peaks observed in the cosmic microwave background (CMB) data using MOG has beenachieved without dark matter. Moreover, a possible explanation for the accelerated expansion of the Universe hasbeen obtained in MOG (Moffat, 2007).Presently, on both an empirical and theoretical level, MOG is the most successful alternative to dark matter. Thesuccessful application of MOG across scales ranging from clusters of galaxies (Megaparsecs) to HSB, LSB and dwarfgalaxies (kiloparsecs), to the solar system (AU’s) provides a clue to the question of missing mass. The apparentnecessity of the dark matter paradigm may be an artifact of applying the Newtonian 1/r2 gravitational force law toscales where it is not valid, where a theory such as MOG takes over. The “excess gravity” that MOG accounts formay have nothing to do with the hypothesized missing mass of dark matter. But how can we distinguish the two?In most observable systems, gravity creates a central potential, where the baryon density is naturally the highest.So in most situations, the matter which is creating the gravity potential occupies the same volume as the visiblematter. Clowe et al. (2006c) describes this as a degeneracy between whether gravity comes from dark matter, orfrom the observed baryonic mass of the hot ICM and visible galaxies where the excess gravity is due to MOG. Thisdegeneracy may be split by examining a system that is out of steady state, where there is spatial separation betweenthe hot ICM and visible galaxies. This is precisely the case in galaxy cluster mergers: the galaxies will experiencea different gravitational potential created by the hot ICM than if they were concentrated at the center of the ICM.Moffat (2006a) considered the possibility that MOG may provide the explanation of the recently reported “extragravity” without non-baryonic dark matter which has so far been interpreted as direct evidence of dark matter. Theresearch presented here addresses the full-sky data product for the Bullet Cluster 1E0657-558, recently released tothe public (Clowe et al., 2006b).NPAC SeminarSeptember 29,2011Probing Dark Matter with NeutrinosIna SarcevicUniversity of ArizonaIn collaboration withArif Erkoca, Graciela Gelminiand Mary Hall RenoFIG. 1:False colour image of Bullet Cluster 1E0657-558.The surface density Σ-map reconstructed fromX-ray imaging observations is shown in redand the convergence κ-map as reconstructedfrom strong and weak gravitational lensing observations is shown in blue.Image provided courtesy of Chandra X-ray Observatory.
EVIDENCE FOR DARK MATTERIn 1930’s Zwicky observed theComa cluster and found thatgalaxies were moving too fastto be contained by the visiblematter.In 1970’s Vera Rubin andcollaborators discovered thatstars in galaxies were rotatingtoo fast implying existance ofinvisible matterObservations indicate the existence ofnon-luminous matter with density profile at1far distances in the form ρ r2
successful application of MOG across scales ranging from clusters ofgalaxies (kiloparsecs), to the solar system (AU’s) provides a clue tnecessity of the dark matter paradigm may be an artifact of applyinscales where it is not valid, where a theory such as MOG takes ovemay have nothing to do with the hypothesized missing mass of darIn most observable systems, gravity creates a central potential, whSo in most situations, the matter which is creating the gravity pomatter. Clowe et al. (2006c) describes this as a degeneracy betweefrom the observed baryonic mass of the hot ICM and visible galaxiedegeneracy may be split by examining a system that is out of steadythe hot ICM and visible galaxies. This is precisely the case in galaa different gravitational potential created by the hot ICM than if thMoffat (2006a) considered the possibility that MOG may providegravity” without non-baryonic dark matter which has so far been intresearch presented here addresses the full-sky data product for thethe public (Clowe et al., 2006b).Non-baryonic Dark MatterMany observations indicate presence of dark matter:Galaxy rotation curves, galaxy clusters, BBN, CMB radiation,gravitational lensing, etc.Bergstrom, Rep. Prog. Phys. 63, 793 (2000)Bullet Cluster (IE0657-56)813Non-baryonic dark matterv (km/s)observed100expectedfromluminous disk50510R (kpc)M33 rotation curveFigure 4. Observed HI rotation curve of the nearby dwarf spiral galaxy M33 (adaptedfrom [74]), superimposed on an optical image (NED image from STScI Digitized Sky Survey,http://nedwww.ipac.caltech.edu. The NASA/IPAC Extragalactic Database (NED) is operated by
Dark Matter Density Profileswwww[87]In the Milkyway, the rotation curves of the stars suggest that the darkmatter density in the vicinity of our Solar System is:
Dark Matter –What do we know?Dark matter is about 23% of the totaldensity of the Universe, while baryonic matteris only 4% Large-scale structure formation in theUniverse imply that dark matter is “cold”(i.e. non-relativistic at freeze-out time)
Dark Matter as a Cold RelicDM produced as a thermal relic of theBig Bang (Zeldovich,Steigman,Turner)Comoving number density Ydn 3Hn σv (n2 n2eq )dtInitially DM is in thermalequilibriumχχ f fχχ f fn e mχ /TUniverse coolsn e mχ /TFreese out time whenn σv HneqThermal relic density:Feng, arXiv:1003.0904(time )Ωχ 0.23 σv f.o.3 10 26 cm3 /s 1The current dark matter abundance in the Universe depends onthe annihilation cross section at freeze-out.
What is dark matter? The unknowns: Modification of the standard, Newtonian1/r 2 law, so that the observed effect is dueto only baryonic matter is ruled out by BulletCluster observations Particle physics candidate for dark matter:weakly interacting particle which is non-relativistic at the time of freeze-out. No viable candidate for dark matter in theStandard Model
annihilation(Indirect detection)χχqqscattering(Direct detection)production(Particle colliders)DARK MATTER DETECTION
Dark Matter DetectionDirect Detection Experiments :Look for energy deposition via nuclear recoils from darkmatter scattering by using different target nuclei anddetection strategiesDAMA, NAIAD, KIMS, CDMS, EDELWEISS, EURECA,ZEPLIN, XENON, WARP, LUXIndirect Detection Experiments :Look for annihilation products of dark matter (Gamma-rays,positrons, electrons, neutrinos )HESS, MAGIC, VERITAS, CANGAROO-III, EGRET,Fermi/LAT, INTEGRAL, PAMELA, ATIC, AMS, HEAT,ICECUBE, KM3NET
Dark Matter Searches Direct searches:look for DM interactions with targetnuclei (XENON, CDMS, CoGeNT, DAMA,CRESST-II)CoGeNT Collaboration:arXiv:1002.4703v2, PRL 106,131301 (2011)
Recent CRESST-II data (4.7 σ )CRESST-II Collaboration:arXiv:1109.0702
NOP'FG77' QORJS1QDAMA 8 σ signalNOP'FG77' QORJS1Q!"## % "&'()* '%,"-#.'/,)&0 ')%'!"## % "&'()* '%,"-#.'/,)&0 ')%'1)(*,2%'3 #"/ *4').%'Rateshould change as1)(*,2%'3 #"/ *4').%'/"&%*(-/* 3 #45. %*(-/* 3 #4'6 *,'*, 'Earth’svelocity adds/"&%*(-/* 3 #45. %*(-/* 3 #4'6 *,'*, '7-&2%'Æ )&&-)#'8".-#)* "&constructively/destructively7-&2%'Æ )&&-)#'8".-#)* "&ICCARDOCCERULLIERULLIRRRICCARDOICCARDO C ERULLI2-6keVkeV2-62-6 keVto the Sun’s - annual V)(cpd/kg/keV)ResidualsDAMA/LIBRA!!250250 kg (0.87(0.87 ton"yr)DAMA/LIBRA9(-: (;' ( % ;'7 (0 #' ?@ABCDAMA/LIBRA ! 250kgkg (0.87ton"yr)ton"yr)9(-: (;' ( % ;'7 (0 #' ?@ABC9GFGI'AV % 0&)#'6 *,'J'K'?'4 )(;'8)L'K'M-& 'D9GFGI'AV % 0&)#'6 *,'J'K'?'4 )(;'8)L'K'M-& 'DTime(day)(day)TimeTime ionwithX-rays/γwithwith twotwo lowlow backgroundbackground PMTsPMTs workingworking inin coincidence);coincidence); energyenergy calibrationcalibration withwith tdowndowntotofewfew keVkeVinin thethe samesameconditionsconditions asas sureof0.87ton viouslycollectedbyofof 0.870.87ton yrton yr [15,[15, 20].20]. ConsideringConsidering thesethese datadata togethertogether withwith thosethose previouslypreviously collectedcollected byby9GFG' DHHAC9GFG' fthesingle-hitevents,measuredbyFigureFigure 1:1: Model-independentModel-independent result:result: residualresidual raterate ofof thethe single-hitsingle-hit events,events, measuredmeasured ionfunctionofofthethetime.time. horizontalbars.bars. TheThe2π2πsuperimposedcurveisthefunctionAcosω(t t 1yr,t 152.5day(June)withT 2π00superimposedcurveisisthefunctionAAcosω(t t0t0))witht0t0 152.5day(JuneTT ωωω A/LIBRAandDAMA/NaIcumulativeexposure(1.17ton lativeexposureexposure(1.17(1.17tonton ,lineslines correspondcorrespond toto thethe maximummaximum expectedexpected forfor thethe DMDM signalsignal (June(June 222nd), whilewhile thethe tothetheminimumminimum[20].[20].9GFG'#"6'8)%%'% 0&)#'&"6'%- # 8 &* .'T4'!"U RJ9GFG'#"6'8)%%'% 0&)#'&"6'%- # 8 &* .'T4'!"U RJDM-IceDark Matter Experiment at the South Pole will crosscheck DAMA annual modulation observationDE'F)('?DE'F)('? &0''D? &0''D?
Indirect DM searches:Detection of the products of DMannihilation (or decay) in the GalacticCenter, Sun, Earth, DM halo, etc.producing electrons, positrons, gammarays (PAMELA, ATIC, FERMI/LAT,HESS, Veritas ) and neutrinos (IceCube,KM3Net )
Indirect Dark Matter DetectionPAMELAAMSFERMI/LATHESSATIC
PAMELA Positron Fraction
FERMI Cosmic Ray Electron Spectrum
If the observed anomalies are due to dark matterannihilation the annihilation cross sections must be10-1000 times more than the thermal relic value of σv 3 10 26 cm3 /sThe required enhancement in the signal is quantified bythe factor called the “Boost Factor” :Low-velocity enhancement(particle physics)Sub-halo structures in theGalaxy (astrophysics)
Dark Matter Signals in Neutrino TelescopesNeutrinos are highly stable, neutral particles.Detection of neutrinos depend on their interactions, i.ecross section.IceCubeAnnihilation of dark matter particlescould produce neutrinos, directly or viadecay of Standard Model particlesNeutrinos interacting with the matter,i.enucleons, produce muons which leavecharged tracks in the neutrino detector
Neutrinoflux from DM annihilation inthe core of the Sun/Earth, produceddirectly or from particles that decayinto neutrinos (taus, Wʼs, bʼs)Erkoca, Reno and Sarcevic, PRD 80, 043514 (2009) Model-independentresults for neutrinosignal from DM annihilation in theGalactic CenterErkoca, Gelimini, Reno and Sarcevic, PRD 81, 096007 (2010) Signalsfor dark matter when DM isgravitino, Kaluza-Klein particle orleptophilic DM.Erkoca, Reno and Sarcevic, PRD 82, 113006 (2010)
Neutrinos from DM annihilations inthe core of the Sun/EarthNeutrino flux depends on annihilationrate, distance to source (Earthʼs core orSun-Earth distance) and energydistribution of neutrinos, ated:
Dark Matter Capture Rate :ρDMC mχ vDM M2σχN vesc mpρDM 0.3 GeV cmvesc 1156 km/s 3vDM 270 km s 1vesc 13.2 km/sfor the Sunfor the EarthM is the mass of the Sun/EarthCapture rate in the Sun is about 109 timeslarger than capture rate in the EarthFor the Sun, annihilation rate C/2
Neutrinos from DM annihilation interact with matterattenuation of the neutrino Flux inthe Sun is important effect Neutrinos also interact as theypropagate through the Earthproducing muons below the detector νµ N µ Xνe N e Xνµ,e,τ N νµ,e,τ X
Neutrino DetectionNeutrinos interact as they propagatethrough the Earth producing muonsbelow the detector (upward muons) orin the detector (contained muons) orproducing showers/cascades in thedetector:νµ N µ Xνe N e Xνµ,e,τ N νµ,e,τ X
Muon FluxThe probability of the conversion of a neutrinointo a muon over a distance dr via CC interactions:where the neutrino scattering cross section is: Muons can be created in the detector (containedevents) or in the rock below the detector (upwardevents).
Contained and Upward Muon Flux The contained muon flux, for a detectorwith size l The upward muon flux is given by
where the neutrino flux isMuon survival probabilty iswhereRE 6400 km (Earth) or(Sun-Earth distance)RSE 150 Mkm
Neutrinos from DM annihilationsNeutrinos from DM annihilationsNeutrinos produced directly or throughdecaysof leptons,quarksand gaugebosons:Neutrinosproduceddirectlyor throughdecays of leptons, quarks and gauge bosons:
Neutrino Energy Distributionchannel :channels :
B 431mχ 38.9"!1.182 1026 secτ 2.29 mχ Bτ 1026 sec10.1(2)for mχ in TeV. The annihilation channel into tau pairsis less favored by the data [16].Some Kaluza-Klein models can provide a0.01DM candidate which gives the correct relic density [30]. To account for the HESS results [6], the lightest Kaluza-Kleinparticle (LKP) would have a mass of the order of a TeV[14]. The LKP is also assumed to be neutral0.001and non0 fixedbaryonic. In this model, the particle couplings aresuch that LKP pairs annihilate into quark pairs (35%),charged lepton pairs (59%), neutrinos (4%), gauge bosons(1.5%) and higgs bosons (0.5%) [14, 30].The first DM candidate proposed in the context of supersymmetry is the gravitino (ψ3/2 ) which would be thelightest supersymmetric particle (LSP). The gravitino isthe superpartner of the graviton. With the existence ofsmall R-parity breaking to allow the LSP to decay, thegravitino decays into standard model particles. The decay rate of the gravitino in this scenario is so small thatit can have a sufficiently long lifetime forDMν the correctν,maxrelic density today.FIG. 1:E /Emψ3/2 (GeV) BF (ψ3/2 γν) BF (ψ3/2 W l) BF (ψ3/2 2000.030.690.28!! - 100 GeV400ZZ, m! 0.030.680.29 #TABLE!! - "I: "Branching fractions for the two-body gravitinodecay into different R-parity violating channels for different! - Z , m 400 GeVmasses [15]. ! -131012101110-1! - l l 1010Particle/modemass Bτ or B ψ3/2 l l ν400 GeV Bτ 2.3400 GeV Bτ 2.3ψ3/2 (W l, Zν, γν)2 TeV Bτ 2.9χ µ µ B (1) B (1) (q q̄, l l , W W , ZZ, ν ν̄) 800 GeV B 2001 TeV B 400χχ µ µ 910810710µ(1/Bf) dN / dxwith a boost factor B. There are theoretical evaluationsof the boost factor [35], however, we treat the boost factor as a phenomenological parameter in this paper. Toexplain the lepton excesses, some models have constraintson the boost factor as a function of DM mass [16].In leptophilic DM models [7, 16] explaining thePAMELA positron excess, the DM annihilation or decaymust proceed dominantly to leptons in order to avoidthe overproduction of antiprotons. Moreover,1000accordingto the FERMI data, the direct production of electronsmust be suppressed with respect to the production ofelectrons (and positrons) as secondaries. It was shown[16] that the leptophilic DM with mass (mχ ) in the range100between 150 GeV and a few TeV, which annihilates ordecays into τ ’s or µ’s can fit the PAMELA [4] and Fermi[5] data as well as the HESS high energy photon data [6].The best fit parameters for the boost factor (B) and thedecay time (τ ) which determine the overall 10normalizations, for the specific case involving muons from annihilation (χχ µ µ ) or decay (χ µ µ ), respectively,are given by [16]-2(1)-1!σv" B !σv"0 ,GeV and few TeV [17]. To explain the data, the threebody gravitino decay mode (ψ3/2 l l ν) was considered [17]. We use the parameters of this model to exploreneutrino signals from gravitino decay. For illustration, inaddition to three-body decay, we also consider the twobody gravitino decay modes (ψ3/2 (W l , Zν, γν))assuming the same lifetime and mass as for the threebody decay, and with the branching fractions given inTable I.d% / dE (GeV km yr )than the value required for a thermal relic abundance[34]: !σv"0 3 10 26 cm3 s 1 . Following the currentconvention, we writeTABLE II: Model parameters characterizing fits to explainFERMI and PAMELA anomalies used as examples in thispaper.6105104Selected DM model parameters are shown in Table II.For each of the DM models considered, the decay distribution of the produced particles to neutrinos in caseof DM annihilation, or the gravitino decay distributionto neutrinos, enters into the calculation of the neutrino0.2that arrive at Earth.0.4 For annihilation0.6 directly to 0.8fluxesxneutrinos, the energy distribution of each neutrino is adelta function in energy, with the energy equal to the DMmass. This case has been well studied in the literature[21, 31, 32, 36]. Here, we look at the secondary neutrinos. Fig. 1 shows neutrino spectra, plotted in termsof x Eν /Eν,max where Eν,max mχ for annihilatingDM and Eν,max mχ /2 for decaying DM models. Thecurves in the figure are normalized to count the numberof neutrinos, and in the caseµ of the Zν final state, thefraction of Z decays to neutrinos. The muon neutrinospectra in the figure should be multiplied by the branching fraction for a specific decay channel in a given model.10310211010x Eν /Eν,maxMuon neutrino (ν ) spectra in terms of x from the three-body dec
In collaboration with Arif Erkoca, Graciela Gelmini and Mary Hall Reno Ina Sarcevic University of Arizona Probing Dark Matter with Neutrinos NPAC Seminar September 29,2011 3 galax
Relic Neutrinos as Dark Matter Number density of relic neutrinos : If neutrino mass is m υ k T 0 10-3.6 eV then non-relativistic (Cold) Dark Matter today. Neutrino mass needed to account for Dark Matter : Ω ν h 2 m i 93.5 eV m i 11.9 eV Ω ν 0.26 h 0.7 2 n(ν ν) 3 4 T ν T γ
Erkoca, Gelmini, Reno and Sarcevic, Phys. Rev D81 (2010). Erkoca, Reno and Sarcevic, Phys. Rev. D 82 (2010). Ina Sarcevic Probing Dark Matter with Neutrinos Miami 2010 Direct searches: look for DM interactions with target .
There are many dynamic probe devices in the world, such as Dynamic Cone Penetrometer (DCP), Mackin-tosh probe, Dynamic Probing Light (DPL), Dynamic Probing Medium (DPM), Dynamic Probing High (DPH), Dynamic Probing Super High (DPSH), Perth Sand Penetrometer (PSP), etc. Table 1 shows some of the dynamic probing devices and their specifications.
Ina Sarcevic University of Arizona Models of Neutrino Mass with a Low Scale Symmetry Breaking New Interactions of Supernova Relic Neutrinos Probing Neutrino Properties with Supernova Neutrinos Experimental Detection of the New Interactions via Light Scalar (HyperK, GADZOOKS, UNO, MEMPHYS) BBN and SN1987A Constraints on the Parameter Space of the
The nonlinear oscillations manifest themselves in various ways, depending on the initial conditions, and have a rich phenomenology. The study of neutrinos from these astrophysical sources therefore demands careful consideration of these nonlinear e ects. In this thesis, we put forward a framework to study nonlinear avor oscillations of neutrinos.
Reactor neutrinos can be employed to measure oscillation due to both m2 12 (so-called 'solar mixing') and m2 23 ('atmospheric mixing'). Using the mean energy of reactor neutrinos, we can calculate the baseline for the oscillation maxima corresponding to the solar and atmospheric m2 values: 2m 12 8 10 5 eV2! L 70 km; (5) 2m 23 2:5 .
INSTA PT 2021 EXCLUSIVE PART-2 (SCIENCE AND TECHNOLOGY) NOTES What are neutrinos? Detected for the first time in 1959, neutrinos are the second most abundant particles in the world, after photons, or the light particle. Neutrinos are mysterious particles, produced copiously in nuclear reactions in the Sun, stars, and elsewhere.
latino lgbt people in the criminal justice system, but limited DATA PAINT A PICTURE OF BIAS AND OVERREPRESENTATION. Sources: U.S. Census Bureau, "Annual Estimates of the Resident Population by Sex, Age, Race, and Hispanic Origin for the United States and States: April 1, 2010 to July 1, 2014," June 2015; Gary J. Gates and Frank Newport, “Special Report: 3.4% of U.S. Adults Identify