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1、TheBaryonicEffectsonthePropertiesofDarkMatterHaloesWeipengLin(ShanghaiAstronomicalObservatory,CAS)Collaborators:ShudeMao(Univ.ofManchester)YipengJing(ShanghaiAstro.Obs.)LiangGao(NAOC)The9thSino-GermanWorkshoponGalaxyFormationandCosmology,26-29April,2011@HangZhouBasicFactsofBaryon
2、Universalbaryonfractionofmass:~16%(WMAP’sresult)DMdominatesonlargescale,whileonsmallscale,therearespaces(e.g.halocenter)wherebaryonaredominated,andimportant.Baryonphysics,1storder:gasshock-heating,cooling,starformation,SN/AGNfeedback,metalenrichment;2ndorder:heatingbyUVbackground
3、&cosmicray,evaporation,rampressurestripping,gravitationalheating,magneticfield,tidalstripping,heatconduction,turbulence,convection,etc.Dynamics:ACeffect,dynamicalfrictionofsinkingsatellites,interactionbetweenrotationdisk/barsandhalomatter,etc.Whathalopropertiescouldbeinfluencedby
4、baryonphysics?Matterdistribution(DM,stellarcomponents,cold/hotgas)ofhalo,especiallyatcentralpartofhaloBaryon/stellarfraction,temperature/entropyprofilesShapeofhalo:densityorpotentialwell,x-rayhaloPropertiesofhalosub-structuresAngularmomentumdistributionandalignment(ofgas,starsand
5、DM)Extended:GravitationalshearfieldAlignmentofmatterdistributioninDMhalo，……Theeffectsareimportantforprecisecosmology!Whatwehavedonesofar?WehavedoneasetofN-body/SPHsimulationsandstudiedfollowingbaryoniceffects:Clusteringandweaklensing:Jing,etal.2006,ApJGalaxyHOD:Zhu,etal.2006Galax
6、ymergingtime-scale:Jiangetal.2008ApJ;A&A2010Massdistributionandentropyprofile:Linetal.2006,ApJSunyave-Zel’dovichEffect(thermalandkinetic):Shao,etal.2011a,bMassdistribution,haloshapeandalignment:Linetal.,tobesubmittedBriefofsimulationsLCDM(WMAPparameters),Box：100Mpc/hGadget-v2(Spr
7、ingel2005)AsetofsimulationsusingthesameICandallstartedfromz=120,softening4.5kpc(ifnotindicated)PureDMsimulation5123(PDM,asreference)Non-radiative(A4orGas512)5123DM+5123GasSF1:5123DM+5123Gaswithcooling,SF,SNFB(9kpc/h)SF2:5123DM+5123Gaswithcooling,SF,SNFB(4.5kpc/h)SF3:5123DM+5123Ga
8、swithcooling,SF,SNFB(4.5kpc/h),baryonfra
