x-ray surveyor andthe spectroscopy of...

MartinElvisHarvard-Smithsonian CenterforAstrophysics

X-raySurveyorand theSpectroscopyofSupermassive BlackHoleOutflows

MartinElvis.X-rayVision,DC,6-8October2015 [email protected]

I

X-ray Surveyor


Theneedhaslongbeenobvious


Because:

hereisfree.com


Diagnostics!

HighResolutionX-raySpectroscopyhasalsolongbeenobviouslyneeded


StateoftheArtinX-rayAGNWinds

1keV

ActiveGalaxyNGC3783 >100spectralfeatures

10days(900ksec)withChandraHETGS@R~400


Kaspi etal.2001Krongold etal.2005…

1hour@R~5000withX-raySurveyor

Vikhlinin etal.2013

×100Chandragratings10

0.2 0.5

ChandraHRC-LETGS

Area4000cm-2

>250XChandraR ~5000

>10XChandra


Diagnostics

RESOLUTION• Resolves~allblends•Weakerlinesdetectableàmore (ne,T)diagnostics• 60kms-1à thermallinewidthsresolved

•incollisional X-rayplasma• Dopplershifts• Turbulentvelocities,Tthermal vs Tion• Curveofgrowthà nion• ResolvescomponentsseeninUV• Needsexcellentcalibration:

• wavelength/energytosmallfractionofresolution(5%?)


DiagnosticsneedArea

PHOTONHUNGRY• R=5000requires~10× #photonsasR=500Forabsorptionlines•ΔE=0.1eV @0.5keV• Δλ =0.0044A@22A

• 104 resolutionelements/keV• 100countseach• =106 counts/1keVwidespectrum


AreaEnablesAREAENABLES

• Depth:– 1Msec givestoNGC3783-qualityspectraatf =4× 10-14cgsà Highz

• Fe-K@z>2(6.4keVà 2.1keV)

• OVII21.6Åà 64.80Åà LowLuminosityL<<LEddà WeakLines

• Speed:à LargeSurveys:M�,L/LEdd,…à 100s/yearNGC3783-qualityspectraof10×faintersources,f =10-12cgsà Variabilityonshort-timescalesà density, radius.

• 1MsonNGC3783à 250spectra• Needsspacecraftagility:rapidslew/settle


• Howsupermassive blackholeswork• HowSMBHgrow• HowSMBHmerge• Accretionluminosityoftheuniverse• Effectsongalaxies,clustergrowth• “Pollution”oftheprimordialgas

The Big Questions

OutflowsfromSuper-MassiveBlackHoles

Ø Whatisaquasar?Ø QuasarevolutionØ RunawayblackholesØ Versusnuclear fusion(stars)Ø FeedbackØ Warm-HotIntergalacticMedium


• Howsupermassive blackholeswork• HowSMBHgrow• HowSMBHmerge• Accretionluminosityoftheuniverse• Effectsongalaxies,clusters• “Pollution”oftheprimordialgas

Why do we care?




rg

101001000104

IonizedWindWAs

1

Black Hole

BELR

Nucleus

10510 kpc

1 kpc

BiconesExtended NELR

[OIII]

Bicones

~107 M¤➱

log(Radius)

Compton WindUFOs

Martin Elvis, September 2007

100 kpc

1Mpc

Host Galaxy

BulgeDisk


BALs

6 orders of magnitude in scale for AGN physics

?


HowdoSupermassive BlackHolesWork?

Luo etal.,2013Elvis2000

Just4Mechanisms1. Comptonscattering– electrons:onlyatL=LEdd2. Linedriving– atoms:forcemultiplierL>~0.05LEdd3. Dustdriving–molecules,solids4. Magnetic“slingshot”

IsthephysicsoftheInnerStructureofQuasarsdominatedbywinds?

Isapredictivephysicstheorypossible?


Highionization CIV, OVI HighionizationOVII, OVIII

Seenin50%of AGN Same 50%of AGN

UsehighR UVspectraasaguideforX-raySurveyor

Chandra HETG: 900ksec NGC3783

NarrowUVlines NarrowX-raylines

Outflow~1000kms-1 Outflow~1000kms-1

NarrowX-raylines:WANarrowUVlines:NAL

WarmAbsorberoutflows(WAs)

CIVλ1550Å

àSame Wind:Fromaccretiondisk?From“torus”?Baseofbi-conesonkpc scale?



Lineblendingiswidespread@R=500VirtuallygoneatR=5000

PieceofcakewithX-raySurveyor

model

R=500050ksec

HETGSR~500900ksec

X-raySurveyor


Evensupersonic flowshavenarrowvelocitystructures

100ksec X-raySurveyor

adaptedfromArav,WHIMEXsimulation

Δv ~50kms-1800kms-1 spread

Multiplemassejectionepisodes?



UVstructure

X-raystructure

Gabeletal.2003NGC3783HETGS


Wherearethey?

UVgiveskiloparsecdistances!e.g.Dunnetal.2010–butseeMcGrawetal.2015

Energy+massflowscalewithr2~108× biggerEout :Mout >Maccretion

ISMinteractionwith“dark”outflow

High~1%c velocitiessuggestradiusWA ~few×1000rg =diskwindModestenergy+massflowrates-Moresubtlefeedbackphysics?e.g.Hopkins&Elvis(2010)

Metastable linescangivedensitiesdensitiesgivedistanceswithionizationparameters

adaptedfromArav,WHIMEXsimulation

Linera

tiodensity

distance

WherewillX-rayWAs lie?Sub-pcorkpc?

Minororpowerful?

. .


DeterminesMass/Energyoutflowrates

Reevesetal.,2009

PDS456.Suzaku XIS,190ksec

Ultra-FastOutflows(UFOs)

• Somewhatcontroversial– E.g.Laha etal.(2014)

• v >0.1cà originat<100rg?• Present location =?• CouldtheybetheBAL“dark”outflows?• X-raySurveyorhasnothingtoadd?

– Highlyionizedà Noneedforlowerenergyspectra?

– Featuresarebroadà NouseforR=5000?

High~0.1cvelocities

FeXVI atVout ~0.25c?


Ultra-FastOutflows(UFOs)

• LowionizationcomponentsarefoundinWarmAbsorbers

• 2-3phasesinpressureequilibrium?• WhynotinUFOs?

à R=5000toseelownion linesà LowenergiesforlowΞ transitions

LowIonization,Lownion phases?

Chakravorty etal.,2009

Fe-K

OVII


BroadAbsorptionLines(BALs)

2.Highionization

1.High~0.1cvelocityoutflows

Hamann etal.1998

Have3thingsincommonwithUFOs

Ogleetal.1999

à 3.ComptonThickabsorbers

Highlypolarizedelectronscatteredflux

AretheweakX-rayspolarized/scatteredtoo?

%polarization

flux

CIV

UVWavelength(A)

à SameWind?

BAL


BUTUFOsandBALs

HavewildlydifferentcoldNH>1024 vs <1022 cm-2

BroadAbsorptionLines(BALs)

…havecomplexnarrowvelocitystructureWhynotUFOstoo?

à R=5000toseenarrowcomponents


BAL BAL BAL

BAL

BALBAL BAL

Turnshek 1988

…&havelowionizationcomponentsWhynotUFOstoo?

CIV FeII

à E<~2keVtoseelowionization lines

McGrawetal.2015

King,A.etal.2015

PCygni profile inV404CygAlsoinAGNPG1211+143?

Crenshawetal.,2015

HSTSTISlongslitspectra

Supermassive BlackHoles’EffectsonGalaxies=“Feedback”

Windloses⅔KEin~20pc~0.3”E.g.ActiveGalaxyNGC4151[OIII]

1storderQuestions:• Howmuchenergy,momentumdeposited?• HowaretheycoupledtoISM?•Wherearetheycoupled?

NarrowEmissionLineRegions(NELRs)

KineticPow

erWhathappenshere?


CouplingMechanisms:1. Winds2. RelativisticJets3. Radiation

Whichdominateswhere?

AlltheseinteractionsshouldgenerateX-raysSpectroscopycandiagnosetheprocess


ImagingX-rayOutflows:X-rayCalorimeter

ActiveGalaxyMRK573.ACISsubpixel binning

Paggi etal.,2012


3”


X-raysmapinteractionofwind([OIII]),jet(radio)withHostgalaxyISMActiveGalaxyMRK573

[OIII]contoursHST

Paggi etal.,2012


Thermalregions:TemperatureEmissionmeasureDensityPressure(cf radio)TotalenergyCooling timeShockspeedCrossingtimeE-lossrateCoupling efficiency(~30%ofjetpower0.05%ofnucleus)

3”

NarrowEmissionLineRegions(NELRs)X-rayEmissionLineratiospickoutdifferentmechanisms

Photoionization (AGN).Thermal(Shocks?)

ActiveGalaxyMRK573

Paggi etal.,2012

[OIII]contoursHST

StandsoutinNeIX/OVIII


3”


ActiveGalaxyMRK573

Paggi etal.,2012

Calorimeter: Manymoreemissionlines;Kinematics1arcsec pixelsarekinda large.Smallerpixelarrayatcenter?Goodforbrightsourcestoo.VelocitiesΔE=5eViskinda large. [email protected]ΔE?“LongSlit”gratingspectra?

gridfrom

art-is-fun.com

1arcsecond pixels

Fischeretal.,2013Bi-conicaloutflowmodel

Velocity(kms-

1 )

+300

-300

±300kms-1


Centroid to5%ifgoodcalibration.

3”

Modestchangescanmakeadisproportionatedifferenceinscienceoutput• Calibration:wavelength/energytosmallfractionofresolution (5%?)

– Doppler shifts

• Agility:rapidslew/settle– enableslargesurveysoftypesofobject– C.f.Swift.LargesampleslittledonesinceROSAT

• Calorimeter:– Angularresolution:factor2gives8× moreNELRs accessible– Pixelsize:centralfinerpixels(~1/2PSF)usesfullpowerofmirror– LowerparticlebackgroundisALWAYSgood– lowsurfacebrightness

• Anotherinstrument?E.g.polarimeter –alsophoton hungryà lowE.

X-raySurveyorDesiderata for theSpectroscopyofSupermassive BlackHoleOutflows


• GratingSpectroscopyatR~5000à PhysicsofAGNStructure- ultra-fastoutflows/broadabsorptionlines,warmabsorbers/narrowabsorptionlines

• CalorimeterIntegralFieldUnità AGNFeedbackPhysics- bi-conicalnarrowemissionlineregions

• Modestchangescanmakeadisproportionatedifferenceinscienceoutput

X-raySurveyorand theSpectroscopyofSupermassive BlackHoleOutflows

BUTWillthesebethesciencequestions

In2030?


X-raySurveyorisRobustagainstScienceChanges

X-raySurveyorOpensaLargeDiscoverySpace“100×”

• Imaginggoes~100× deeper• Surveyingis~500-800x faster• Spectrahave~200× #photons,10× resolutionelements

• ~150× informationcontent• newphysicsavailable


I

X-ray Surveyor


rg

101001000104

IonizedWindWAs

1

Dusty molecular torus

Dusty wind

Black Hole2000K

20K BELR

UV continuum‘Big Blue Bump’

NucleusHost Galaxy

100pc

106 105

Warped mol. disk

10 kpc

1 kpc

10 pc

1rg

107M¤:~1013 cm~3 µpc

NELRHα

[OIII] Coronal

lines

BiconesExtended NELR

[OIII]

Bicones

Rela

tivist

ic Je

t

~107 M¤➱1 pc

BulgeDisk

log(Radius)

X-ray source

symmetry

Compton WindUFOs

Martin Elvis, September 2007

100 kpc

1Mpc

HostEnvirons

CGMIGM

span 9 orders of magnitude in scale


BALs

Accretion disk

continuum

Gupta, Mathur &Krongold, 2015

HETG100ksec

BroadAbsorptionLines(BALs)e.g.MRK590:complexnarrowvelocitystructureinaUFO?

severallowS/Nlines:tantalizing

>3σ=FeXVII v=0.04c?=OVIIIv=0.176c?

2.8σ=NeVIII v=0.175c?


20σ in20ksec


Γ

1

3

101NH (1022cm-2)

‘Not-so-Ultra-FastOutflows’5000– 10000kms-1X-rayvelocities

Tombesi &Cappi 2014,MNRAS,443,L104

Vout ~6500kms-1

CluesfromIntermediateCases?

mini-BALs:HighUVvout,lowFWHM

NH ~1022 cm-2

Hamann etal.,2013

220ACIScountsin15ksecwithX-raySurveyor

DiagnosticsRESOLUTION

• Resolvesblends• 40%offeaturesinNGC3783areblends• UTAnolongerunresolved

•Weakerlinesdetectableàmore (ne,T)diagnostics• 60kms-1 à thermallinewidthsresolvedincollisional X-rayplasma.

• Turbulence,Tthermal vs Tion• Curveofgrowthà n(ion)•ResolvescomponentsseeninUV

bth =√2kT/mp

Nion(cm-2)=1.3× 1020 (EW/f λ2)

Mathur etal.1995

DiagnosticsneedAreaPHOTONHUNGRY

• R=5000requires~10× #photonsasR=500• X-raySurveyorhas

• Gratings:~8× efficiency•Mirror:~30× area

•à SameS/Ninsources25× fainter• or4%oftheexposuretime.Forabsorptionlines•ΔE=0.1eV @0.5keV

• Δλ =0.0044A@22A• 104 resolutionelements/keV• 100countseach• =106 counts/1keVwidespectrum

• #photons=fate/hν• fate=flux× area× time× efficiency

• Howsupermassive blackholeswork• HowSMBHgrow• HowSMBHmerge• Accretionluminosityoftheuniverse• Effectsongalaxies,clusters• “Pollution”oftheprimordialgas

Why do we care?



Supermassive BlackHoles’EffectsonGalaxies=“Feedback”

Windloses⅔KEin~20pc~0.3”

E.g.ActiveGalaxyNGC4151[OIII]

MechanismsforinteractionwiththeISM:1. Winds2. Relativistic Jets3. Radiation

Whichdominateswhere?

AlltheseinteractionsshouldgenerateX-raysSpectroscopycandiagnosetheprocess

HSTSTISlongslitspectra (Crenshawetal.,2015)Bi-conicalwindmodel


KineticPow

er

Whathappenshere?

x-ray surveyor andthe spectroscopy of...

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