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ThisLecture

•  Reprocessing-howcanwelearnaboutthematerialinandaroundtheblackholefromspectralandtemporalsignaturesinthespectra

•  Spinanditsinfluence

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•  X-ray�reflection�imprintswell-definedfeaturesinthespectrum

Reynolds (1996)

WhatWeWouldLiketoProbe

Reynolds2019)

DependanceofRadiusofISCOonSpin

BasicComponentsofX-raySpectra•  X-rayspectradisplaystandardcomponents

–  PrimaryX-raycontinuum(Γ~2powerlawwithcutoffat50—300keV)dN/dE~E-Γphotons/cm2/sec/keV

–  Absorption(coldandphotoionizedgasalongline-of-sight)–  X-rayreflectionfromdistantgas(torusoftheunifiedscheme)

–  X-rayreflectionfromtheinneraccretiondisk(stronglybroadened)

–  Softexcess(originunknown...maybeluke-warmComptonization,orX-rayreflectionfromionizedaccretiondisk)(willnottalkabout)

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RelativisticX-rayLinesfromtheInnerAccretionDisksAroundBlackHolesJ.M.MillerARA&A200745,441

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BasicComponentsofAGNX-raySpectra•  .

52RamosAlmeida&Ricci(2017)HickoxandAlexander2018

UV/optical

Infrared

X-rays

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r

absorbercutoffpowerlaw

reflectionfromdistant(green)andclosein(red)material

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BlackHoleX-raySpectraAGN StellarMassBlackHole

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ConnectionBetweenSourceGeometryandSpectrainanBlackholebinary

'Reflection'-referstoreprocessingoftheintrinsicx-ray'powerlaw'bymaterialThenatureofthereprocessingdependsonthecolumndensity,ionizationstate,chemicalcomposition,velocitystructureandgeometryofthe'reprocessor'MainprocessesareComptonscattering,flourescentemission,photoelectricabsorption

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'Reflection'-ReprocessingofPhotonsintheDisk

photoelectricabsorptioncrosssection

electronscatteringcrosssection

ThelargercrosssectionatlowenergiesofphotoelectricabsorptionmeansthatlowEphotonsareabsorbednotscatteredandsomearere-emittedaslinesviafluorescence.Comptonscatteringreducestheenergyofthehighenergyphotons.Thecombinationproducesacharacteristicpeakinthespectrum.

EmissionduetothetwoprocessesfromacoldslabofthicknessτThompson=1

ModelsofDiskReprocessing

58Varyingtheinputradiationfield

"Cold"Reprocessor IonizedReprocessors

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Adominantcomponentof"Reflection'isComptonscattering

Important consequence of corona: underlying disk is irradiated by intense X-ray source… results in a characteristic spectrum being �reflected� from the disk surface layers Different amounts of flux can change ionization of disk

Reflectionfrommaterialofdifferentionizationstate

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Parmar et al. (1984) Solar Maximum Mission (Bent Crystal Spectrometer)

Iron Kα fluorescence from the Sun

Withveryhighresolutionthereare2FeKflourescentfeatureKα1,Kα2

energylevelsforCu

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Relativisticeffects-C.Done

Fabian et al. 1989

Energy (keV)

flux

•  Relativisticeffects(specialandgeneral)affectallemission(Cunningham1975)

•  Hardtoeasilyspotoncontinuumcomponents

•  FeKα linefromirradiateddisc–broadandskewed!(Fabianetal1989)

•  BroadeninggivesanindependentmeasureofRin–sospinifISO(Laor1991)

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Relativisticeffectsimprintcharacteristicprofileontheemissionline…

Andy Young

Theoreticallineprofiles[LauraBrenneman]

R=1000rgR=100rgR=30rgR=10rgR=6rg

DiskInclinationdeterminedbyhighEcutoff

FeKLineShape•  Lineprofilesaffectedby

–  Dopplershift–  Gravitationalredshift–  Other“astrophysics”…Comptonbroadening,blendingoflinesetc…

•  Principalparametersinfittingdata–  Lineenergy–  Diskinclination–  Inner&Outerradii–  Runofemissivitybetweeninnerandouterradii-e.g.whereinthediskthelinecomesfrom

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Noticethefullrangeof0.6cinthevelocities-colorbarisredshift(T.Dauser)

CombingtheEffectsofSpecialandGeneralRelativity

Milosevic20181811.09583.pdf

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67

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•  Firstseenin1994withASCAobservatory

•  5dayobservationofSeyfert-1galaxyMCG-6-30-15

•  Neededlongobservationtocollectenoughphotonstoformdetailedspectrum

Observationsofrelativisticemissionlines

Power-law continuum subtracted ASCA: Tanaka et al. (1995)

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RelativisticEffects

•  Lightraysarebentbystronggravity-makingthegeometryrathercomplicated

•  Donotknow'where'x-raysourceis-trytousedatatofigureitout–e.g.heightabovedisk

70Uttley2010

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•  Possiblestrongeffectoflightbending.

•  ifweonlyknewwherethex-rayscomefrom(hs~rs)fromtimevariabilityarguments

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•  ModernXMM-Newtonobservations

•  Confirmrelativisticlinewithextremeredshifts

•  IfnolineemissionfromwithinISCO,needtoinvokespinningblackholetogetstrongenoughredshifting

•  Blackholesmustdoubletheirmasstochangetheirspin.(Bardeen70,Thorne74)

•  •Impossibleinstellarbinaries.Stellar-massblackholespinsaresetinthecreationeventwhileAGNcanchangetheirspinviaaccretionormergers.

MCG-6-30-15 Power-law continuum subtracted XMM: Fabian et al. (2002)

AsObservedwithanX-rayCCD

Reis(2012)

Relativistic lines

MCG-8-11-11(Mattetal.2006)

Relativisticlinesareoftenobserved,butnotalwaysLinesensitivetoemissivityprofile,inclination,R(in),spin

MCG-6-30-15(Fabianetal.2002)

)

~25%ofallAGNshowbroadFeKlinesstrongfunctionofsignaltonoise

stacked199highzAGN

EffectsofInclinationandKerrvsSchwarschild

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EffectofinclinationSchwarzschild6rg(i.e.theradiusofmarginalstability)to30rg.inclination10°,30°and60°.

KerrvsSchwarzschild

BLACKHOLEBINARY

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WhyMeasureSpin

•  BHhasonly3measurablepropertiesMass,spin,charge.•  Blackholespinsaffects

–  theefficiencyoftheaccretionprocesses,hencetheradiativeoutput–  howmuchenergyisextractablefromtheholeitself–  theretentionofblackholesingalaxies–  gravitationalwavesignature–  possibleoriginofjets.

•  OriginofBHSpin–  natal–  history

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Spin•  Forgalacticblackholes-notenoughaccretiontoaccountforspin

beingduetoaccretionofangularmomentum-needtoaccrete~3/4ofthemasstospinituptothemaximalspin(seegraph-spinvsaccretedmass)

•  IfaccretingattheEddingtonlimittakesaverylongtime(~108yrs)–  toolongforwindfedorRocheLobesystems–  toomuchmassforlowmasscompanions

•  Spinisnatal

•  SeeThemassesandspinsofneutronstarsandstellar-massblackholesMillerandMiller2015PhysicsReports5481

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Spin•  Forsupermassiveblackholes-IfaccretingattheEddingtonlimit

(~108M¤accretes0.25M¤/yr)sotakes4x108yrstodoubleitsmassandspinup

•  Spincanbeduetoaccretion•  Requires'organized'accretionofangularmomemtum

Alternativelyspincouldbeduetomergersofblackholes(Gravitationalwaves)

mergers only (left), mergers and prolonged accretion (center), and mergers and chaotic accretion

Volontierietal2010

Spin

BlackHoleBinaries

81

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Reminder-RadiusofISCOdependsonSpin•  Spin-is

measuredinunitsofc/GM2

X-rayBinaries

AGNBlackHoleSpinfromFeKline•  Reynoldsetal2019•  ItseemsasmostlowmassAGNBHshavehighspin

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ASSEMBLYANDMERGINGHISTORYOFSUPERMASSIVEBLACKHOLESINHIERARCHICALMODELSOFGALAXYFORMATION

Volonteri,Haardt,&Madau•  Gravitationalinstabilityduetothe

non-uniformmatterdistributioncausedmattertocondenseuntilsmallregionsbecomegravitationallybound

•  Thefirstcollapsingobjects(halos)aresmallandmergelatertoform

•  moremassivesystems:BOTTOM-UP/HIERARCHICAL

•  MakeAssumptionthatthese'small'objectshostBHsandthatasthegalaxiesmergetheBHsalsodo

•  Whentheymergetheyemitgravitationalwaves

•  PrimesciencegoalofLISA

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Volonteri2008

Massgrowthof2SMBHs

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