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LSS: A microwave vision

LSS: A microwave vision. Jose M. Diego (Instituto de Fisica de Cantabria). Why Microwave Observations ?. Unique negative K- corrections make observationms nearly insensitive to z beyond z=1

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LSS: A microwave vision

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  1. LSS: A microwavevision Jose M. Diego (Instituto de Fisica de Cantabria)

  2. WhyMicrowaveObservations ? • Uniquenegative K-correctionsmakeobservationmsnearlyinsensitiveto z beyond z=1 • Protoclusters can bedetected at mm wavelengthswhich are verysensitivetostarforminggalaxies. Abilitytoseegalaxies up tothereionizationperiod (longerwavelengths (radio) can seebeyondthereionization time (LOFAR, SKA)) • Plasma can beseenthroughSunyaev-Zeldovicheffect (thermal & kinetic), Ostriker-Vishniaceffect. Great complementto X-rayobservations. Densityprofiles can beconstrainedbetterwith SZ+XR. • Hot plasma traces gravitationalpotentials. Correlatewithgravitationaldistortions of the CMB (lensing, ISW). Use X-rayobservations as a tracer of thepotentialwells.

  3. Negative K-correctionmakesobservations of distantgalaxieseasier Planck 5.13 degrees Thelowerthefrequency, the more sensitivetohigherredshift (relativetohigherfreqs.) PlanckCollaboration

  4. Herschel’sview of theLockmanHole 3.5 arcmin Amblard , Cooray, Serra et al 2011 PlanckCollaboration

  5. Herschel-ATLAS 600 hours 550 sq. Degrees (16 sq. deg. shown) About 250000 galaxies 5 bands (100-500 microns) Up toabout z = 4 Checkforresultssoon!

  6. 1.5 sq. Degreebefore and afterGalacticsubtraction. Rigby et al. 2010

  7. 1.5 sq. Degreebefore and afterGalacticsubtraction. Angular correlationisstronger at longerwavelengths. Low-z normal galaxies ? High-z star-bustgalaxies ? Maddox et al. 2010 Rigby et al. 2010 Clusteringseemsstronger at longerwavelengths (starforminggalaxies vs normal galaxies)

  8. Planck: Galaxyclusters Hot gas clearlyseenthroughtheSunyaevZel-dovicheffect (Compton) • Thethermal SZ effectisduetothesamehot gas that produces X-rays in clusters • Unlikethe X-raysthe SZ effect traces directlythepressure of the gas (robustmass proxy ?) • Nearlyhalfthebaryonsscapedetection. SZ + X-rayobservationsneeded. Abell 2319 Proportionalto Y PlanckCollaboration

  9. ESZ AllSkyDistribution ESZ sample: 189 clusters. Masses (1–15 x 1014) . Redshifts (0.01, 0.55). Blue known clusters. Green dots new and confirmed with XMM-Newton Red ESZ candidate new clusters yet to be confirmed. PlanckCollaboration

  10. ESZ as a function of redshift and mass PlanckCollaboration

  11. ESZ. Selectionfunction. Hardtoseewith SPT, SCT Nearly flat selectionfunctionbeyond z=0.5 PlanckCollaboration

  12. SZ sensitivetomassivesystems PLCK G214.6-37.0, z = 0.45. A super cluster ? 15 arcminutes PlanckCollaboration

  13. Scalinglaws in clusters Key ingredients in cosmologicalstudiesto link observables withtheory (massfunction) Blue dots : coldcore X-rayderivedquantitiesagreewellwithindependent SZ measurements. “Y” couldbeused as a goodmass proxy ? Number of members in SDSS groups. PlanckCollaboration

  14. Universal gas profile ? (Arnaud et al.) X-rayselected Notseen in X-raysoriginallybutonlyon SZ X-raybiasedtowardshigherdensities. SZ notaffected as much. BUT, bothagreeonthis. Definitelynot a standard-model ! Explainssmallernumber of SZ detections in ACT, SPT ? Thedensityprofile at thevirialradiuswilltell. PlanckCollaboration Diego & Partridge 2010

  15. Cosmologicalconstrainsfrom SZ measurements Particular selectionfunctionhelpsincreasetherate of high-z clusters Number of detectionshighlysensitiveto8. Powerspectrumeven more sensitiveto 8 (can bemeasureddirectly) Ability to see most massive clusters at high-z SPT-CL J2106-5844 (Foley et al. 2011). Interesting for non-standard models of structure formation (test Gaussian initial conditions etc). Need X-ray follow-up. Dark energy surveys, most sensitive to cluster population at at z = 1-2 Key ingredientisthemass proxy (M_gas, Y) Planck, SPT and ACT are conductingextensivesurveys and more to come in thefuturethatwillcomplementcurrent X-raycatalogs. Diego et al. 2003 10 m class tel. Mohr 2005

  16. Cosmologicalconstrainsfromclustermeasurements Battye & Weller 2003 A bit optimistic. Gastrophysicscomplicatesthispicture. Buthowmuch ? … Multiwavelength X-ray+SZ +lensing? constrainsdensity and T distribution. More workneeded, new methods, better data.

  17. Apartfromthestandardmassfunctioncosmologicalconstraints, othertestslike angular diameterdistance, orf_gas can beusedtoconstrainthecosmologicalmodelundertheassumptionthatf_gasdoesnotevolvewith z Allen et al. 2004 Allen et al. 2004 Complete with SZ ordeeper X-rayOnlytherightcosmologypredicts a flat f_gas SZ measurementstogetherwith X-rayobservations can constrainf_gaswithunprecedentedaccuracymakingthistechnique a powerfulindependentcosmological test

  18. Gravitationaleffects, distortionsonthe CMB by LSS

  19. IntegratedSachs-Wolfe Effect. A darkenergyprobewith LSS Cteif no DE in a flat univ. In Linear Theory: Linear growthrate

  20. N-bodysimulations. Neededfortestingcorrelationtechniques ISW has samespectrum as CMB. Imposible toseparatefrom CMB 1Gpc^3. 0 < z < 1. 10^9 particles Diego et al. In prep.

  21. Clusterregion 50x50x50 (h^-1 Mpc)^3 Cai et el. 2010 ISW Full ISW Linear Rees-Sciama

  22. Voidregion 300x300x1000 (h^-1 Mpc)^3 Cai et el. 2010 ISW Full ISW Linear Nottoobad ! Rees-Sciama

  23. Cross-correlation of CMB mapswith X-raymaps (used as tracer of LSS) Revealssignificantcorrelationsignal. WMAPxHEAO-I Granett et al. 2008 Boughn & Crittenden 2004

  24. Simulated full sky lensing potential and (magnified) deflection angle fields  =  k2 Lewis & Challinor , 2006 • Lensingpotential of the CMB can berecoveredwithquadraticestimatos (lensing introduces correlationsamongsphericalharmonics) • Correlations of lensingmapswithtracers of LSS can alsoreconstructthelensingpotential. • Lensing and ISW are bothproportionaltothepotential in Fourier space.

  25. TheNearFuture Half of the 12-m antennas are at somestageconstruction (total of 50+) 84 to 950 GHz Array configurations with maximum baselines from approximately 15 meters to 15 km Ability to image sources many arcminutes across at arcsecond resolution Top spatial resolution of 5 milli-arcseconds (better than the VLA and HST) Not very sensitive to LSS but great capabilities for resolving structure. ALMA can detect SZ and evenOstriker-Vishniac (v). Reionizationstudies. Imagecourtesy ALMA (ESO/NAOJ/NRAO) Do gastrophysics in clusters

  26. C O N C L U S I O N S • IXO will open thedoortoamazingsciencebutthebest and mostrobustresultswillbeobtainedwhencomplementaryobservations are combined. • X-raysurveyswillbenefitfrominformation at mm wavelengths. In some cases, X-rays trace thesamesource as in mm observations (gas in SZE). • Galaxyclusters can provideindependentcosmologicalconstraints. • ThedistantUniversebecomes “closer” at mm wavelengthsopeningthedoorforstudyingunexploredterritory. • ALMA willboost a “goldenage” of mm science in thenearfuturealthoughisnotoptimallydesignedforstudyingthe LSS structure (surveymodeveryexpensivebutpossibleifwellmotivated).

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