类星体-1.ppt

SolvingQuasarspartI MartinElvisHarvard SmithsonianCenterforAstrophysics inparticular UnderstandingQuasarAtmospheres ElvisM 2000 AstrophysicalJournal545 63 FermilabColloqium29October2003 Quasars unsolvedafter40years Oncewerea hottopic WerethefirsttostartthedownfallofSteadyStateCosmology via evolution changeindensitywithcosmictimeNowastronomershavemovedontoeasierproblems Largescalestructure DarkEnergyandGamma rayburstsQuasarstudiescontinuetogeneratemanypapers butlittleunderstanding Discoveredin1963QuasarsarethemostpowerfulcontinuousradiationsourcesintheUniverse Noteforthepedantic By quasars Imeanalltypesof activity ingalaxies FermilabColloqium29October2003 What stheproblem Enormousarrayofdetail WehavenoimagesofaquasaratmosphereWouldneed1000timessharperpicturesthanHubbleorChandra 100mas Mustrelyonspectra spanallwavelengths X ray optical radio Superficialunderstanding FermilabColloqium29October2003 WhyStudyQuasars WeliveonaplanetAstargivesuslifeGalaxiesdominatetheUniverse butwhydoquasarsmatter Hereare4answers FermilabColloqium29October2003 Outsidethewavelengthrangethatoureyesaresensitiveto 1 AnAstronomer sAnswer Radio Gamma ray X ray Quasarsdominatethenightsky FermilabColloqium29October2003 2 AnAstrophysicist sAnswer Gravitypowered notfusion viaBlackHoles106 109asmassiveastheSun Gasheatsupfallingtowardit likeaspacecraftonre entry FermilabColloqium29October2003 ThepoweravailablefromgravityforheatingisalltooobviousfollowingtheColumbiatragedy 3 ACosmologist sAnswer 4 APhysicist sAnswer ReynoldsC ReynoldsC FermilabColloqium29October2003 Whatdoweknow Highleveltheoryrapidlygaveaclearpicture massiveblackholeLynden Bell1969accretiondiskLynden Bell1969 Pringle Rees1972 Shakura Sunyaev1972relativisticjetRees1967 PhD Blandford Rees1974 Allestablishedjust10yearsafterdiscovery FermilabColloqium29October2003 doesnotconnecttotheatomicphysicsfeaturesobservedinquasars Thistheorydescribesanakedquasar Leavesuswithnowaytoorderobservations nothingtotest FermilabColloqium29October2003 AtomicfeaturesinQuasarAtmospheres Highionization e g CIV OVILowionization e g MgII Hb FermilabColloqium29October2003 Allstudiedseparatelywithseparatetelescopes Comptongamma rayObservatory Chandra Hubble MMT Sub millimeterarray VLA Quasarshavenotemperature Whipple10meter Blindmenandtheelephant MangaVIIIHokusai Katsushika 1760 1849 Wall Tree Rope Spear Snake FanNothavingthecompletepicturecanbemisleading FermilabColloqium29October2003 weneeda lowtheory thatdealswiththemultitudeofquasardetails Justastherearetextbookson StellarAtmospheres weneedthesubjectof QuasarAtmospheres Takesmorethan1step Firstbuildanobservationalparadigmi e whatdotheobservationsdriverequireofanytheory TheseopticallythinfeaturesareallinterconnectedS quasaratmosphere FermilabColloqium29October2003 AParadigmforQuasarAtmospheres Accretiondisk BroadAbsorptionLines Reflectionfeatures Narrowabsorptionlines X ray warm absorbers BroadEmissionLines hollowcone ElvisM 2000 AstrophysicalJournal545 63 X ray UVionizingcontinuum NB IndependentofUnificationJetsarenotincluded noabsorptionlines AGeometric Kinematicsolutionc f Reesrelativisticjetsforblazars radiosources Cannowre constructthismodelusingdatanotinElvis2000 QuasarAtmosphere FermilabColloqium29October2003 Takealessonfromlabplasmas useallthedata NSTXdiagnosticinstrumentscovereverything NSTXatPPPLNationalSphericalToruseXperimentPrincetonPlasmaPhysicsLaboratory 2mminterferometerX rayPHAX raycrystalspectrometerRadiometerThomsonscatteringFarinfraredtangentialInterferometer polarimeterVisiblespectrometerVacuumUVsurveyspectrometer GrazingincidencespectrometerTangentialbolometerarraySinglechannelvisibleBremsstrahlungdetectorPolarimeterX raypinholecameraSoftX rayarraysFasttangentialX raycameraReflectometerarrayInfraredcameras PrincetonAGNPhysicswiththeSDSS 29July2003 12 277PapersonQuasarssince1963 ADSto4 18 03 refereedonly searchonabstractcontaining quasar AGN 1 day Now2perday 5 ofallastronomypapersSpam Needfilters PhysicalmeasurementsMass length density Notratios columndensitiesFavorabsorption advicefromSteveKahnc 19851 Dspatialintegral not3 D blueshift outflowUsePolarizationNon sphericalgeometryWiththesefiltersjustadozenpapersdefinethestructureofquasaratmospheres FermilabColloqium29October2003 1 PhysicalMeasurements BELVelocity radiusrelation ReverberationmappingshowsKeplerianvelocityrelationinBELs Pole on BroadEmissionLinesclosetoKeplerianvelocities 1000rs Schwartzchildradii FermilabColloqium29October2003 1 PhysicalMeasurements Angle Pole on UseVLBI X raytogetangleofjettolineofsightRokakietal 2003astroph 0301405 2 ContinuumdropsascosqEW EW0 1 3cosq 1 2cosq 1limbdarkeneddiskHadoesnot HascaleheightlargerthandisklikeopticalcontinuumButBLRisrotating rotatingcylinder Ahighlynon equilibriumshape Simplestsolution BLRisinarotatingwind Rotationaboutjetaxisc f Wills Browne1986 Brotherton1996 McLure Jarvis2003HapolarizationrotationalsoimpliesorbitinggasSmithetal2002 FermilabColloqium29October2003 2 AbsorptionFeatures NarrowUVlines HighionizationCIV OVI HighionizationOVII OVIII Outflow 1000kms 1 Seenin50 ofquasars Seeninsame50 ofquasars Simplestsolution Samegas 2phases PrincetonAGNPhysicswiththeSDSS 29July2003 Windsarecommoninquasars ChandraHETGS850ksecspectrumofNGC3783 Over100absorptionfeaturesfittedbya6parametermodel OneT 106KandoneT 104K inpressurebalanceto5 Krongold Nicastro Brickhouse Elvis Liedahl Mathur 2003ApJ inpress astro ph 0306460 2 phasegasinpressureequilibrium 2 Absorption MorePhysicsfromX rays FermilabColloqium29October2003 Krongold Nicastro Brickhouse Elvis Liedahl Mathur 2003ApJ inpress astro ph 0306460 2 phasegasinpressureequilibrium 2 Absorption PressureBalance Freeparametersinblue Ifatsamedistance NGC3783ChandraHETG MEG spectrumsolution FermilabColloqium29October2003 2 Absorption whereisthewind Velocitydependentcoveringfactors Absorberisclosetocontinuumsource absorberismovingtransverse Windisclosetocontinuum crosseslineofsight Arav Korista deKool2002 ApJ566 699Arav Korista deKool Junkkarinen Begelman1999ApJ516 27 FermilabColloqium29October2003 Aquasarwindislikeaflame Wearelookingthroughaflow Apparentlackofchangeisacommonhandicapforastronomersthe StaticIllusion e g expansionoftheUniverse clustercoolingflows quasardisks FermilabColloqium29October2003 Emissionlines athinwind NarrowLineSeyfert1galaxies NLSy1s showbroad stronglyblueshiftedhighionization CIV linesUnderstandableasdiskwindredshiftedlineshiddenbydiskLowionizationlinesfromouterdiskc f Collin Souffrin Hameury Joly 1988A A205 19 Leighly Moore2003 ApJsubmitted See Gaskell1982Wilkes1984 LowionizationMgII BELsarerotating transverse thinwinds FermilabColloqium29October2003 2 Absorption 1 PhysicalMeasurements WindDensity thickness UV X rayabsorptionrespondstocontinuumchanges photoionized Nicastroetal 1999ApJ 512 184 Absorbingwindisdense Butrespondswithadelay recombination ionizationtime density ne 108cm 3forOVIIIne 3x107cm 3forFeXVII X raycontinuum OVIIedge OVIIIedge time density columndensity 3x1022cm 2 thickness 1015cm distancetocontinuum Absorbingwindisnarrow FermilabColloqium29October2003 3 Polarization X rayabsorbers Absorptionlinequasarsarehighlypolarizedinoptical 1 Scatteringoffnon sphericaldistribution Edge onstructure2 Pole onobjectsmustbeunobscured scatterer obscurer flattened co axial Leighlyetal 1997ApJ489 L137 Absorbersareseenedge on FermilabColloqium29October2003 Flattened TransverseWind axisymmetry Atransversewindsuggestsanaxisymetricgeometry bi coneslookingedge onseeabsorbersWinddoesnothugdiskpole on noabsorbers absorbersinallquasars Mathur Elvis Wilkes1995ApJ 452 230 PrincetonAGNPhysicswiththeSDSS 29July2003 Absorbingwindisabi coneto1storder PuttingX ray UVabsorberandBELtogether Botharediskwindsrisingwellabovethediskplane Elvis2000ApJ545 63 Krongoldetal 2003 SimilarPressure P abs 1015 104Kx1011cm 3P BELR 1015 106Kx109cm 3 MatchingIonizationParameter U T U abs 106 T abs 106K U abs 1T U BELR 106 T abs 104K U BELR 0 04 SimilarRadius forNGC5548r abs 1015 1018cmrecomb time NHXr BELR 1016cmCIVreverberationmapping Keepitsimple EmissionandAbsorptionare2phasesofthesamequasarwind Theysharephysicalproperties FermilabColloqium29October2003 ComponentsofQuasarAtmospheres Highionization e g CIV OVILowionization e g MgII Hb Ina2 phasetransversewindinpressurebalance United FermilabColloqium29October2003 TheFinalElement BroadAbsorptionLines BALs Oldquestion Specialobjects orSpecialangle Ferland Hamann1999AnnualReviewsofAstronomy Astrophysics 37 487 10 ofquasarsshowBALswithdopplerwidths 2 c 10 c 10 xNALs Clearacceleration ordeceleration FermilabColloqium29October2003 BroadAbsorptionLines BALs BELFWHMcorrelateswithBALvelocity atminimumflux V BAL 2FWHM BEL Lee Turnshek1995ApJ453L61 PrincetonAGNPhysicswiththeSDSS 29July2003 BALgasknowsaboutBELgas MoreBEL BALcorrelations Reichardetal 2003 BELwidth BALwidth 2 1 BALsfromarotatingwind RedshiftedBALonsetPossibleoccasionallyinarotationdominatedwind Halletal 2002ApJS 141 267 BALsneedarotatingwind liketheBELs blue red FermilabColloqium29October2003 3 Polarization BALtroughs Ogleetal 1999ApJS 125 1 Ogle1998PhDthesis CalTech BALtroughsarehighlypolarized scatteredlightoffflattenedstructure BALsarecommon Universal ScatteringsolvesotherBALproblems ionization abundances NHThomsonthick X rayFe K Comptonhump Ogle PhDthesis 1998 ConicalwindfitsBALswell Hamann1998ApJ500 798 Telferetal 1998ApJ509 132 IstheBALwinditselfthescatterer Bi conemodelPredictsdistributionofnon BALquasarpolarization FermilabColloqium29October2003 3 Polarization VBELR Supportedbyobservations Emissionlinestwiceasbroadinpolarized non variablelight non BALquasarshaveThomsonthickgasatlarge BAL velocitiesDon tseeinabsorptionbecauseoutofourlineofsight Largescatteringregion butnottoolarge Smithetal 2003MNRAS withBALvelocities Youngetal 1999MNRAS303 227 BALvelocitygasexistsinnon BALquasars IfBALsarecones allquasarsshouldhaveBALgas FermilabColloqium29October2003 Onelast crucial complication Anglesarewrong BALvelocitiestoohigh 10 000kms 110timesnarrowabsorptionlinesRequiresextremeconeopeningangle Simplesolution bendwind Predicts 1 detachedBALs Lowestvelocitywherewindbendsintoourlineofsight verticalvelocityfromdisk2 10 coveringfactordratrgives6odivergenceangleradiationforcesgastodivergeBothpreviouslyunexplained Couldthisbeanionizationeffect DvaIP FermilabColloqium29October2003 QuasarAtmospheres QuasarWinds 60deg broadabsorptionlines 20deg noabsorptionlines Onegeometryunitesallthefeatures 85deg narrowabsorptionlines HighionizationBroademissionlinesLowionization FermilabColloqium29October2003 ComponentsofQuasarAtmospheres Highionization e g CIV OVILowionization e g MgII Hb Allatomicfeaturesnowincluded ThompsonthickBALscatterermustalsomakeComptonhump Fe K FermilabColloqium29October2003 Puttingitalltogetherinformationfiltersworkedefficiently hollowcone ElvisM 2000 ApJ 545 63 BALs Polarization noabsorptionlines NALs BELs WAs FermilabColloqium29October2003 Blindmenandtheelephant MangaVIIIHokusai Katsushika 1760 1849 HokusaineversawaliveElephant Notbad not100 right butgetstheidea Thispictureofquasaratmospheresisprobablyinmuchthesamestate needsphysicsbones FermilabColloqium29October2003 AQuasarObservationalParadigm DiskWinds tietogetherallthepiecesofthequasaratmosphereExplainsfeaturesnot builtin BALcoveringfactor detachmentvelocity HiionizationBELblueshifts SurvivedtestsX rayabsorberoutflowv 2 phaseUV X rayabsorber pressurebalanceMakespredictionsHighionizationBEL X UVabsorberradii thicknessareequalCreatesaresearchprogramc f Lakatos1980Allowstractablephysicsexploration WorkBACKtoorigininaccretiondiskphysicsWorkOUTtoimpactonsurroundings Canbegintobuilda low theoryofquasaratmospheres FermilabColloqium29October2003 lowtheory 2 phaseequilibrium Krolik McKee Tarter1981 ApJ 249 422 PhotoionizedgastendstohavephasesNotreallynew Doesnotworkforastaticmediumsoabandoned amistake Worksfineinawind dynamicEquilibriumdeterminedsolelyby SED ionizationthresholdsShouldbesimilarfromobjecttoobjectNoneedtoassume clouds Krongold Nicastro Brickhouse Elvis Liedahl Mathur 2003 FermilabColloqium29October2003 lowtheory accretiondiskphysics II Krongoldetal inpreparation new 106KphasedependscriticallyonSEDNicastro1999 Reynolds Fabian1995Useabsorber T x todetermineunseeableEUVSED Testmodelsofaccretiondiskinneredgeill defined boundarycondition plungingregion Kroliketal Krongold Nicastro Brickhouse Elvis Liedahl Mathur 2003 Reynolds Fabian1995MNRAS273116 FermilabColloqium29October2003 lowtheory Whyisthewindthin Intermediatelevel2DtheoryWinddrivenbyUVabsorptionlinesc f O starwinds CAKignoregaspressure3Zones Inner Middle Outer1 Inner over ionizedOnlyComptonscattering insufficientshieldsgasfurtheroutfromX rays Murray Chiang hitchhikinggas 2 Middle UVabsorptiondrivesgas windescapes3 Outer shieldedfromUV weakinitialpushfromlocaldiskradiation windfallsback Risaliti Elvis2003 ApJsubmitted new density FermilabColloqium29October2003 LookingOut quasarsasdustfactories Elvis Marengo Karovska 2002ApJ 567 L107 OutflowingBELgasexpandsandcoolsadiabaticallyBELadiabatstrackthroughdustformationzoneofAGBstars AppliestoCarbon richandOxygen richgrains PrincetonAGNPhysicswiththeSDSS 29July2003 Outflowsrates 10Msol yratL 1047erg s 0 1Msol yrofdustassumingdust gasratioofLongPeriodVariables 107Msolover108yroutburstlifetimeMetallicitysuper solareveninz 6BELsHighZ Zsolshouldenhancedustprodu