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GOODS: Great Observatories Origins Deep Survey - Department of ...

Welcome to UC Riverside!


Schedule– Welcome to department (Harry)Friday9:15 - 11:00 AM Introduction11:00 - 12:30 PM Meetings with faculty–––The UCR the physics program (Ken)Astrophysics at UCR (Bahram)Particle physics at UCR (Bob)12:30 - 1:30 PM Lunch– Condensed mater physics at UCR (Roland)1:30 - 2:00 PM Lab tour– Graduate program requirements (Umar)2:00 - 3:00 PM Special Colloquium(Fundamental Constants in Physicsand their Time Dependence)3:00 - 4:00 PM Campus Tour4:00 - 5:00 PM Meetings with faculty6:00 PM Dinner with grad studentsSaturdayJoshua Tree National ParkSelf organize local stuffHiking – mountainsUCR botanic gardenHistoric downtown areaOther …


UCR Physics DepartmentAstrophysicsParticle/NuclearCondensed MatterExperimental x-ray/Gamma raySatellites/BalloonsLand Based ObservationsZych, Shen, Cordova,Canalizo,MobasherIGPPTheoryZankCosmology / particleastrophysicsHanson,Ma,Wudka,MobasherConnections to MathProton CollidersFNAL/CERN/SLACWimpenny,EllisonShen,Clare,HansonLepton CollidersLEP/SLACClare ,HansonGary,Shen,LongRelativistic Heavy IonsBNL-RHICBarish,SetoNeutrino factoryHansonTheoryMa, Wudka, DesaiCorrelated ElectronsBeyermann, MacLaughlin,MillsFundamental ForcesMohideenBiophysicsBeyermann, Mills, Tom,Mohideen, ZandiTheoryPryadko, Varma, Tsai,Shtengel, ZandiOptical, LasersMohideen, Tom,Kawakami, Jing ShiSurfacesYarmoff, TomSpintronicsJing Shi, Kawakami, LauEnvironmentalTom, YarmoffConnections toEnvironmental Sciences,Engineering, Chemistry,Biology


Condensed Matter FacultyCondensed MatterCorrelated ElectronsBeyermann, MacLaughlin,MillsFundamental ForcesMohideenBiophysicsBeyermann, Mills, Tom,Mohideen, ZandiTheoryPryadko, Varma, Tsai,Shtengel, ZandiOptical, LasersMohideen, Tom,Kawakami, Jing ShiSurfacesYarmoff, TomSpintronicsJing Shi, Kawakami, LauEnvironmentalTom, YarmoffConnections toEnvironmental Sciences,Engineering, Chemistry,BiologyWardBeyermann Roland Jeanie LauKawakamiDoug MacLaughlin Allen P. MillsUmar MohideenLeonid Kirill ShtengelPryadkoJing ShiShan-WenTsaiHarry TomChandra VarmaJory YarmoffRoya Zandi


Particle/Nuclear FacultyParticle/NuclearProton CollidersFNAL/CERN/SLACWimpenny/EllisonShen/Clare/HansonLepton CollidersLEP/SLACClare / HansonGary/Shen/ LongRelativistic Heavy IonsBNL-RHICBarish/SetoNeutrono factoryHansonTheoryMa, Wudka, DesaiKen Barish Bob Clare Bipin Desai John Ellison Bill GaryGail Hanson Owen Long Ernest Ma Rich SetoCosmology / particleasttrophysicsHanson,Ma,Wudka,MobasherBenjamin Shen Steve Wimpenny Jose Wudka


Fellowship/TA/GSR packages‣ 1 st year– Fellowship (min 3.5 GPA of 3.5)– 25% TA (10 h/week) (covers tuition & health)‣ 2 nd year– 50% TA (20 h/week) (covers tuition & health)– Summer research support through PI (or TA)‣ 3 rd year +– TA/GSR (min 3.0 GPA) (covers tuition & health)– Summer research support through PI (or TA)


WELCOME TO UCR


RELEVANT FACTS ABOUTUCR18000 Total Students1800 Graduate Students80 Undergraduates in Physics100 Graduate Students in Physics800 Total Faculty29 Faculty in PhysicsMost ethnically diverse UC Campus


PhysicsAstrophysicsParticle/NuclearCondensed MatterExperimental x-ray/Gamma raySatellites/BalloonsLand Based ObservationsZych, Shen, Cordova,Canalizo,MobasherIGPPTheoryZankCosmology / particleastrophysicsHanson,Ma,Wudka,MobasherConnections to MathProton CollidersFNAL/CERN/SLACWimpenny,EllisonShen,Clare,HansonLepton CollidersLEP/SLACClare ,HansonGary,Shen,LongRelativistic Heavy IonsBNL-RHICBarish,SetoNeutrino factoryHansonTheoryMa, Wudka, DesaiCorrelated ElectronsBeyermann, MacLaughlin,MillsFundamental ForcesMohideenBiophysicsBeyermann, Mills, Tom,Mohideen, ZandiTheoryPryadko, Varma, Tsai,Shtengel, ZandiOptical, LasersMohideen, Tom,Kawakami, Jing ShiSurfacesYarmoff, TomSpintronicsJing Shi, Kawakami, LauEnvironmentalTom, YarmoffConnections toEnvironmental Sciences,Engineering, Chemistry,Biology


What are the requirements for PhD?Core Classes ( all done in first year)Classical Mechanics 1 quarterElectricity and Magnetism 2 quartersQuantum Mechanics 3 quartersStatistical Mechanics 2 quartersElective Classes (second year)3 quarters of either Condensed Matter Physicsor Elementary Particle Physics or Astrophysics**Pass all classes with B- grade or better.


Exams I1. Written Qualifying exam at the end of the firstyear. Pass at the PhD level. (Written +Oral)Subjects:Classical Mechanics (Undergrad level)Thermodynamics (Undergrad level)Quantum Mechanics (graduate level)Electricity and Magnetism (graduate level)- Two Tries : Sept of 1 st year and Jan of 2 nd year- Pass rate ~75% after 2 tries (~50% on 1 try).


Exams IIPick a research Advisor by Spring quarter offirst year.Oral exam on research potential before the endof the 3 rd year.Two attempts allowed.


GraduationWrite and Defend aThesisMean Time to graduationis about 6 yrs.General range 4-7 yrs.National Average 6.8years


Median salary and age for major employment sectors,PhDs 2004.


Requirements for MS degree36 units of classes (core + elective classes)Pass with grade better than B-Pass the Qualifying Exam at the MS levelorDo MS research thesisAutomatic for students continuing towardsPhD


50% TA DutiesNominal 20 hours per week job (7assigned hours). Duties are:1. Manage two 3 hr labs per week2. Office hours (2hrs/week)3. Grade the lab books (about 20 students perlab)


Quantum UniverseThe revolution in the 21 st century particle physics: DOE/NSF HEPAP (2004)1. Undiscovered principles of natureClare, Ellison, Gary, Hanson, Long, Shen, Wimpenny, Ma,Wudka, Mohideen2. Dark EnergyClare, Ellison, Gary, Hanson, Shen, Wimpenny, Mohideen3. Extra DimensionsClare, Ellison, Gary, Hanson, Shen, Wimpenny, Mohideen,Wudka4. Forces become oneClare, Ellison, Gary, Hanson, Shen, Wimpenny5. So many kinds of particlesClare, Ellison, Gary, Hanson, Long, Shen, Wimpenny6. Dark matterClare, Ellison, Gary, Hanson, Wimpenny, Shen, Mohideen7. What are neutrinos sayingMa, Hanson8. How did universe come to beClare, Ellison, Gary, Hanson, Shen, Wimpenny,Barish, Seto9. AntimatterGary, Long, Shen, Ma


Theory Group‣ Desai– Origins of mass. Is there a symmetry behind the mass spectrumthat we observe?‣ Ma– Origin of neutrino mass• Why is the mass so small, but not zero?– Leptogenesis• Can we use neutrinos to generate the baryon asymmetry in theuniverse?‣ Wudka– Effective theories• We see nothing (yet!) beyond SM. What does this imply about theunderlying physics?– Extra dimensions• Trying to find a model with right particle content…


Neutrino Factory - Muon Collider‣ Hanson


‣ Gary, Long, ShenBabar at SLAC


Babar - Example physics‣ Studying rare Bmeson decays‣ Investigating CPviolation with Bmesons


D0 at Fermilab‣ Clare, Ellison, Heinson, Wimpenny– Electroweak physics– Top quark– Searches for newphenomena


D0 - Example physics‣ First evidence for single top production‣ Use to measure coupling of W to tb


D0 - Example physics‣ Search for Higgs boson


CMS at CERN‣ Clare, Ellison, Gary, Hanson, Shen,Wimpenny


CMS - Example physics‣ None, yet! Data taking is scheduled to startthe end of this year.‣ But maybe soon:Signal of the Higgs!


Phenix at RHIC (Heavy Ions)‣ Barish, Seto


Phenix - Example Physics‣ Investigating the quark-gluon plasma– High energy heavy ion collisions‣ What makes up the spin of the proton?– Polarized proton collisions• Protons are not those prosaic things made of 3 quarks.


TheoryGroupLeonidPryadkoKirillShtengelShan-WenTsaiChandraVarmaRoyaZandiExperimentGroupWardBeyermannRolandKawakamiJeanieLauDougMacLaughlinAllenMillsUmarMohideenJingShiHarryTomJoryYarmoff


Theory of Quantum Computing (QC)Make use of quantum mechanical entanglement for enormous computing powerKirill ShtengelUsing “Anyons” in 2D systems for quantum computing.• In 3D, you have fermions and bosons only.• In 2D, you can have “anyons,” recentlyobserved in experiments.• Anyons are good for QC because of low decoherence ( insensitive to quantum noise).Leonid Pryadko• Use pulse shaping to reduce decoherence• Applicable to many implementations of QC


Nanoscience1D: Nanowires and NanotubesJeanie Lau1D superconducting wires oncarbon nanotube scaffoldShan-Wen Tsai (theory)Theory of high Tc superconductorsin confined geometriesWard BeyermannMagnetoresistance of electrodepositedmagnetic nanowiresDNA as a nanowireJing Shi, Roland KawakamiSpin-polarized transport in carbonnanotubes with ferromagnetic contacts0.5 μmResistance (kΩ)9.89.79.61.75 K-3 -2 -1 0 1 2 3Magnetic Field (kG)


Nanoscience2D: Surfaces, Interfaces, and Thin FilmsJory YarmoffIon-surface interactionse-e-e-e- e -Ion scattering fromnanocrystalsRadiation damage tosurfaceshν, e - +ADSORBATESSUBSTRATE+_+_+Semiconductorsurface etching_+++Reactive Gasses:CF 4 , SF 6 , Cl 2 , etc.InsulatorPlasma+_Substrate+Insulator_+++_+Harry TomInvestigation of surfaces and interfaces bynonlinear opticsJing Shi, Roland Kawakami,Jeanie Lau, Shan Wen Tsai (theory)Spin, charge, and electric fieldeffects in graphiteω2ω


Spintronics and Molecular ElectronicsNanoscienceHarry Tom, Roland KawakamiSpin dynamics and coherence insemiconductors GaAs and siliconTime Resolved Faraday RotationTi:sapphire laser(~76 MHz)probeVary pump-probedelaypumpΔtθ F100 fse -BθF∝ S x1ν LΔtJeanie LauPressure-modulation conductancemicroscopy of molecular junctionsmetalmoleculemetalJing Shi, Roland KawakamiSpin transport in organicsemiconductorsRoland KawakamiSpintronic materials bymolecular beam epitaxyJory Yarmoff, Allen MillsTransport in molecular crystalsXTEM


Atomic Physics and Precision MeasurementsAllen MillsPositrons and high densitypositronium gas.Interacting positroniumUmar MohideenPrecision measurement of Casimir forceusing atomic force microscopes1. Explore the Quantum Vacuume+ e-e+ e-U 1 U 2U 2< U 1Attractive Casimir Force0.0-0.1XP2020 Amplitude (V)10 -110 -210 -31 mm10 0 -50 0 50 100 150 200 250 300single lifetime fitFit with spin exchangeExpandedCompressedSystem responseCasimir force (10 -9 N)-0.2-0.3-0.4-0.550 100 150 200 250 300 350Plate-sphere surface separation (nm)10 -4time (ns)Gold coating = 85.6±0.6nm


BiophysicsRoya Zandi(theory)• Statistical mechanics applied to biological systems• Physical basis for icosahedral symmetry of sphericalviruses• Passage of polymers through membrane pores• Statistical mechanics of virus assemblyUmar MohideenAFM tipSingle Bio-MoleculeInteraction ForcesHarry TomOptical biosensorAllen MillsDNA Computing600400aNi coated plateForce (pN)2000ce-200bd-400-200 0 200 400 600Distance Moved By Plate (nm)


Highly Correlated Electron SystemsExploring complex behavior where standard Fermi liquid models fail.Chandra VarmaTheory of high temperaturesuperconductorsShan-Wen TsaiRenormalization groupapproach to interactingfermions coupled to bosonsDoug MacLaughlin (experiment)NMR and μSR of heavyfermion superconductorsKirill ShtengelQuantum spin modelsLeonid PryadkoDoes superconductivityexist in the t-J model?Ward Beyermann (experiment)Transport and thermal properties ofcorrelated electron materials


Observational Astronomy andCosmology in RiversideBahram Mobasher


Fundamental QuestionsGOODS: Great ObservatoriesOrigins Deep Surveyin Cosmology• How do galaxies form and evolve ?• How galaxies develop the morphology and themass they have today ?• Is the Universe open or closed ?• What are the first generation of galaxies like ?• How the Universe started ?• How about the future of the Universe?• Does dark energy exist ?• What is the nature of Dark Energy?• How do we find the most distant galaxies?November 12, 2002Treasury Workshop


GOODS: Great ObservatoriesOrigins Deep SurveyWhat data do we need?•A large-area, deep survey–Need much more area than the Hubble Deep Fields– Need comparable depth• High-resolution and multi-wavelength data– Need to follow morphology through cosmic time• Large wavelength coverage (colors)– provide redshift constraints for very faint sources– Chandra, ACS, Spitzer, Radio + sub-mm probe theoverall energetic output, dust obscurationNovember 12, 2002Treasury Workshop


GOODS: Great ObservatoriesOrigins Deep SurveyNovember 12, 2002Treasury Workshop


GOODS: Great ObservatoriesOrigins Deep SurveyNovember 12, 2002Treasury Workshop


GOODS: Great ObservatoriesOrigins Deep SurveyNovember 12, 2002Treasury Workshop


GOODS: Great ObservatoriesOrigins Deep SurveyNovember 12, 2002Treasury Workshop


GOODS: Great ObservatoriesOrigins Deep SurveyThe multi-λ Milky Wayradio (408MHz)HIradio (2.5GHz)H 2infraredmid-infrarednear-infraredopticalx-rayGSFC/NASAgamma rayNovember 12, 2002Treasury Workshop


MultiwavelengthGOODS: Great ObservatoriesOrigins Deep SurveygalaxyFrom the ultraviolet throughto the near-infrared,different stellar populationsare visible, and dust hasmore, or less impact.The characteristics at eachwavelength for all galaxiesgive a cumulative measurement.November 12, 2002Treasury Workshop


GOODS: Great ObservatoriesOrigins Deep SurveyTo address these questions,we need multi-waveband galaxysurveysGreat Observatories Origins Deep Survey(GOODS)Cosmic Evolution Survey (COSMOS)Hubble Ultra-Deep Field (HUDF)Coma Hubble Treasury ProgramNovember 12, 2002Treasury Workshop


GOODS: Great ObservatoriesOrigins Deep SurveyGreat Observatories OriginsDeep Survey (GOODS)Medium Deep Surveys of Large Areas –designed to study formation and evolutionof galaxies and to search for high redshiftgalaxiesNovember 12, 2002Treasury Workshop


Seeing back into theGOODS: Great ObservatoriesOrigins Deep SurveysirtfcosmosgalexalmaNovember 12, 2002Treasury Workshop


The GOODSGOODS: Great ObservatoriesOrigins Deep SurveyTreasury/Legacy MissionAim: to establish deep reference fields with public data sets from X-raythrough radio wavelengths for the study of galaxy and AGN evolution of thebroadest accessible range of redshift and cosmic time.GOODS unites the deepest survey data from NASA’s Great Observatories (HST,Chandra, SIRTF), ESA’s XMM-Newton, and the great ground-basedobservatories.Primary science goals:• The star formation and mass assembly history of galaxies• The growth distribution of dark matter structures• Supernovae at high redshifts and the cosmic expansion• Census of energetic output from star formation and supermassive black holes• Measurements or limits on the discrete source component of the EBLRaw data public upon acquisition; reduced data released as soonas possibleNovember 12, 2002Treasury Workshop


GOODS: Great ObservatoriesOrigins Deep SurveyThe Great Observatories origins DeepSurvey(GOODS)Aim: Unite extremely deep, multiwavelength observations tocreate a public, legacy data set for exploring the distantUniverse.Deepest X-ray observationsHST/ACS Treasury programSpitzer Legacy programESO/NOAO/… follow-up programs(imaging, spectroscopy)November 12, 2002Treasury Workshop


GOODS: Great ObservatoriesOrigins Deep SurveyBy looking at distant regions in theUniverse, we look back in time. Bylooking for the most distant galaxies,we look at the beginning of theUniverseNovember 12, 2002Treasury Workshop


GOODS: Great ObservatoriesOrigins Deep SurveyNovember 12, 2002Treasury Workshop


Finding High-Redshift GalaxiesGOODS: Great ObservatoriesOrigins Deep SurveyB 435V 606i 775z 850•Theory predicts that darkmatter structures form atz~20-30•It does not clearly predictgalaxies, because we do notfully understand starformationUnattenuated SpectrumSpectrum AttenuatedZ~4by IGM•We need to push empiricalstudies of galaxy evolution tothe highest redshifts•We collected the deepest andlargest quality samples ofNovember 12, 2002galaxies at z~4 through ~6Treasury WorkshopB 435 V 606 z 850


An imaging LBGGOODS: Great ObservatoriesOrigins Deep SurveydemonstrationLBGs are star forminggalaxies at z > 2,identified by the colorsignature of the Lymanlimit and Ly-α breaks.First studied in largenumbers by Steidel et al.(1995-2001).Now ~ 1000 withmeasured redshifts.November 12, 2002Treasury Workshop


GOODS: Great ObservatoriesOrigins Deep SurveyGalaxies at z~6B 435V 606i 775z 850November 12, 2002Treasury Workshop


GOODS: Great ObservatoriesOrigins Deep SurveyNovember 12, 2002Treasury Workshop


GOODS: Great ObservatoriesOrigins Deep SurveyNovember 12, 20023-Epoch stackTreasury Workshop


GOODS: Great ObservatoriesOrigins Deep SurveyNovember 12, 20025-Epoch stackTreasury Workshop


GOODS: Great ObservatoriesOrigins Deep SurveyNovember 12, 2002Treasury Workshop5-Epoch stack – bright stretch


GOODS: Great ObservatoriesOrigins Deep SurveyHubble Ultra-Deep FieldThe Deepest view to the Universeever taken by the mankindNovember 12, 2002Treasury Workshop


Hubble Ultra-Deep FieldGOODS: Great ObservatoriesOrigins Deep SurveyWhy Ultra-deep?Or when counting is not enough• In any survey of high redshift galaxies oneobtains more objects by widening the arearather than increasing the depth• However, extra depth is necessary todiscover a new class of objects or determinethe properties of a class of objects at the limitof our detectionNovember 12, 2002Treasury Workshop


GOODS: Great ObservatoriesOrigins Deep SurveyNovember 12, 2002Treasury Workshop


GOODS: Great ObservatoriesOrigins Deep SurveyNovember 12, 2002Treasury Workshop


Seeing back into theGOODS: Great ObservatoriesOrigins Deep SurveysirtfcosmosgalexalmaNovember 12, 2002Treasury Workshop


HUDF–JD2 B > 30.61 i > 30.88V > 31.02 z > 30.26GOODS: Great ObservatoriesOrigins Deep SurveyHST/ACSVLT/ISAACSST/IRACNovember 12, 2002Treasury Workshop


GOODS: Great ObservatoriesOrigins Deep SurveyNovember 12, 2002Treasury Workshop


After the Big Bang the Universe coolsdown and after about 1 million years allhydrogen in the Universe becomesneutral and opaque to ultravioletradiation as if the Universe was filledwith fog. No discrete sources of light hadyet been formed.GOODS: Great ObservatoriesOrigins Deep SurveyNovember 12, 2002Treasury Workshoptime


GOODS: Great ObservatoriesOrigins Deep SurveyAfter few 100 Myrs the First Stars form.Their light is not sufficient to “dispersethe fog”November 12, 2002Treasury Workshoptime


Some time after the First starshave formed the first galaxies willappear. These galaxies or theirsuccessors will “disperse the fog”and make it easier for us toobserve the emergence of structurein the Universe.GOODS: Great ObservatoriesOrigins Deep SurveyNovember 12, 2002Treasury Workshoptime


GOODS: Great ObservatoriesOrigins Deep SurveyCosmic Evolution Survey(COSMOS)LARGEST amount of Hubble Space Telescopetime ever awarded to a single project (20% of theHubble time in one cycle)Medium deep survey of a VERY LARGE area(2 sq. deg) to study properties of galaxies as afunction of environment, SFR, morphology,redshift, luminosityNovember 12, 2002Treasury Workshop


GOODS: Great ObservatoriesOrigins Deep SurveyCosmic Evolution Survey(COSMOS)• large area -- 1.4 x 1.4 deg=> cover largest large scale structures• high sensitivity ( I > 28.6 mag AB , 5σ)=> morphology of L * galaxies at z < 2• sensitivity + area=> 2x10 6 galaxies , unusual objects at higher z• equatorial => multi-λ observations from all tel.November 12, 2002Treasury Workshop


GOODS: Great ObservatoriesOrigins Deep Survey17 orbits10/31/031.4 degNovember 12, 2002Treasury Workshop


GOODS: Great ObservatoriesOrigins Deep Survey130 orbits3/31/041.4 degNovember 12, 2002Treasury Workshop


GOODS: Great ObservatoriesOrigins Deep SurveyACS I-bandACSCycle 12270 orbits5/14/041.4 deg270 orbitsas of 6/15November 12, 2002Treasury Workshop


GOODS: Great ObservatoriesOrigins Deep SurveyACS I-bandACS477 orbits1/14/051.4 degNovember 12, 2002Treasury WorkshopNICMOS-31.6 μm -- 24mag~7% of area


GOODS: Great ObservatoriesOrigins Deep SurveyACSCycle 12 & 13590 orbits1.4degNovember 12, 2002NICMOS-31.6 μm NICMOS-3 -- 24mag~7% of 1.6 area μm -- 24mag~7% of areaTreasury Workshop


GOODS and COSMOSGOODS: Great ObservatoriesOrigins Deep SurveyNovember 12, 2002Treasury Workshopoffer:• Extensive multi-waveband surveys from radio toX-ray• A number of independent SF diagnostics: X-ray,UV, Hα, IRAC (3.6-8.0 mm), MIPS (24 mm),radio (1.4 GHz)• Large area coverage ( 2 sq. deg.) – COSMOS• Deep ACS data and rest-frame morph- GOODS• HST/ACS morphologies (B/D, Sersic,concentration, asymmetry, clumpiness)• Accurate photometric/spectroscopic redshifts andspectral types (from early-type to starburst)• Galaxy stellar masses


GOODS: Great ObservatoriesOrigins Optical Deep Telescope Survey ElementJWST Main ElementsIntegrated Science InstrumentModule (ISIM) ElementSpacecraft Bus SunshieldNovember 12, 2002Treasury WorkshopSpacecraft Element


GOODS: Great ObservatoriesOrigins Deep SurveyThe JWST TelescopeNovember 12, 2002Treasury Workshop


GOODS: Great ObservatoriesOrigins Deep SurveyNovember 12, 2002Treasury Workshop


Science is all about testingGOODS: Great ObservatoriesOrigins Deep Surveyour understanding• Cosmic Geometry– WMAP + H 0 + Ly-alpha forest provide goodconstraints but do not tightly constrain Ω Λ– High-redshift supernovae when combined withWMAP provide tight constraints, but are we beingfooled by dust or evolution?• We need more independent tests of the basiccosmological parameters: a robust sample ofhigh-redshift November 12, 2002 (z>1) Treasury supernovae.Workshop


GOODS: Great ObservatoriesOrigins Deep SurveyWhat we seeNovember 12, 2002Treasury Workshop


GOODS: Great ObservatoriesOrigins Deep SurveyMeasuring the Expansion History:Changes in scale/Changes in timeNovember 12, 2002Treasury Workshop


Search for cosmicGOODS: Great ObservatoriesOrigins Deep SurveydecelerationSNe Ia at z > 1provide anessential test ofthe transitionbetween currentcosmicacceleration andpast decelerationNovember 12, 2002 Our current goal: 6-8 Treasury SNeWorkshopIa at 1.2


GOODS: Great ObservatoriesOrigins Deep SurveyFinding High-z Sne• We found 6 of the 7 highest redshift (z>1) supernovaecurrently knownSearch completed:• 43 SNe identified•~25 Type Ia candidates at z>1–10 follow-ups by ToO program–12 spectroscopic confirmations so far–3 highest-z spectral confirmations (z>1.3)Four Additional Epochs of HDFN in 2004:–Riess et al. and Perlmutter et al.~1 FTE with HST “as is“ will yield ~100 Sneat z>1–Probe the nature of the dark energy–HST+ground=SNAP-lite NOW!High-z SN “Artemis” fromCDF-S ACS observationsNovember 12, 2002Treasury Workshop


Is Cosmic Acceleration Real?GOODS: Great ObservatoriesOrigins Deep Survey?November 12, 2002Treasury Workshop


GOODS: Great ObservatoriesOrigins Deep SurveyExpansion Kinematics(How Long Has This Been Going On?)past decelerationpresent accelerationz~0.3-0.6,~5 GYR agoNovember 12, 2002Treasury Workshop


High Redshift SN and Expansion HistoryTaylor Expansion of the left handside of the Friedman Eq: a(t)=f(t,H,q,j,…)GOODS: Great ObservatoriesOrigins Deep SurveyFainter1.0H(z)=f(z,H 0 ,q 0 ,dq/dz)=f(z,H 0 ,q 0 ,j 0 ) q 0 =-, dq/dz=0 (j 0 =0)Constant accelerationBrighterRelative Brightness (Δm)0.50.0-0.5-1.0Freely expandingq(z)=0q 0 =-, dq/dz=+ (j 0 =+)Acceleration/DecelerationConstant decelerationq 0 =+, dq/dz=0 (j 0 =0)November 12, 20020.0 0.5 1.0 1.5 2.0presentTreasury WorkshopRedshift zpast


GOODS: Great ObservatoriesOrigins Deep SurveyDark MatterpullsDark EnergypushesNovember 12, 2002Treasury Workshop


The content of theGOODS: Great ObservatoriesOrigins Deep Surveyuniverseremember,this is it!!November 12, 2002Treasury Workshop


GOODS: Great ObservatoriesOrigins Deep SurveyDark Energy: Static or Dynamic?dwdz≡ w' =?Big Rip?Big Chill?Big Crunch?November 12, 2002Treasury Workshop


GOODS: Great ObservatoriesOrigins Deep SurveyDLProbing Dark EnergyTwo fundamental properties/clues of dark energy:its strength, w0, AND is it dynamic or static, i.e. is w’=0?zc ⎧= (1 + z ) ⎨H∫0 ⎩ 0d z ′33 (1 + w 0 − w ') 3 w ' z[(1+ z ) Ω + (1 − Ω )(1 + z ) e ]M•We have doubled our knowledge of w0 and w’ in 1 year with HST•Einstein’s model now looks better than ever, a way to go…M−1 / 2⎫⎬⎭W’Einstein’sNovember 12, 2002w0Treasury Workshopw0


GOODS: Great ObservatoriesOrigins Deep SurveyNovember 12, 2002Treasury Workshop


GOODS: Great ObservatoriesOrigins Deep SurveyACSNovember 12, 2002Treasury Workshop


GOODS: Great ObservatoriesOrigins Deep SurveyACS+NICMOS+ISAACNovember 12, 2002Treasury Workshop


GOODS: Great ObservatoriesOrigins Deep SurveyACS+NICMOS+ISAAC+IRACNovember 12, 2002Treasury Workshop


GOODS: Great ObservatoriesOrigins Deep SurveyJD2 (J-dropout) in HUDF(Mobasher et al. 2005)z = 6.5no current star formationage ~ 0.65 – 1.0 GyrE B-V = 0.0M * = 5 10 11 M oZ ~ 0.2 – 1.0 Z oNovember 12, 2002Treasury Workshop


GOODS: Great ObservatoriesOrigins Deep SurveyNovember 12, 2002Treasury Workshop


GOODS: Great ObservatoriesOrigins Deep SurveyNovember 12, 2002Treasury Workshop


GOODS: Great ObservatoriesOrigins Deep SurveyNovember 12, 2002Treasury Workshop


GOODS: Great ObservatoriesOrigins Deep SurveyNovember 12, 2002Treasury Workshop


GOODS: Great ObservatoriesOrigins Deep SurveyNovember 12, 2002Treasury Workshop

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