x-ray surveyor andthe spectroscopy of...
TRANSCRIPT
MartinElvisHarvard-Smithsonian CenterforAstrophysics
X-raySurveyorand theSpectroscopyofSupermassive BlackHoleOutflows
MartinElvis.X-rayVision,DC,6-8October2015 [email protected]
HighResolutionX-raySpectroscopyhasalsolongbeenobviouslyneeded
MartinElvis.X-rayVision,DC,6-8October2015 [email protected]
StateoftheArtinX-rayAGNWinds
1keV
ActiveGalaxyNGC3783 >100spectralfeatures
10days(900ksec)withChandraHETGS@R~400
MartinElvis.X-rayVision,DC,6-8October2015 [email protected]
Kaspi etal.2001Krongold etal.2005…
1hour@R~5000withX-raySurveyor
Vikhlinin etal.2013
×100Chandragratings10
0.2 0.5
ChandraHRC-LETGS
Area4000cm-2
>250XChandraR ~5000
>10XChandra
MartinElvis.X-rayVision,DC,6-8October2015 [email protected]
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%?)
MartinElvis.X-rayVision,DC,6-8October2015 [email protected]
DiagnosticsneedArea
PHOTONHUNGRY• R=5000requires~10× #photonsasR=500Forabsorptionlines•ΔE=0.1eV @0.5keV• Δλ =0.0044A@22A
• 104 resolutionelements/keV• 100countseach• =106 counts/1keVwidespectrum
MartinElvis.X-rayVision,DC,6-8October2015 [email protected]
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
MartinElvis.X-rayVision,DC,6-8October2015 [email protected]
• 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
MartinElvis.X-rayVision,DC,6-8October2015 [email protected]
• Howsupermassive blackholeswork• HowSMBHgrow• HowSMBHmerge• Accretionluminosityoftheuniverse• Effectsongalaxies,clusters• “Pollution”oftheprimordialgas
Why do we care?
OutflowsfromSuper-MassiveBlackHoles
Ø Whatisaquasar?Ø QuasarevolutionØ RunawayblackholesØ Versusnuclear fusion(stars)Ø FeedbackØ Warm-HotIntergalacticMedium
MartinElvis.X-rayVision,DC,6-8October2015 [email protected]
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
OutflowsfromSuper-MassiveBlackHoles
BALs
6 orders of magnitude in scale for AGN physics
?
MartinElvis.X-rayVision,DC,6-8October2015 [email protected]
HowdoSupermassive BlackHolesWork?
Luo etal.,2013Elvis2000
Just4Mechanisms1. Comptonscattering– electrons:onlyatL=LEdd2. Linedriving– atoms:forcemultiplierL>~0.05LEdd3. Dustdriving–molecules,solids4. Magnetic“slingshot”
IsthephysicsoftheInnerStructureofQuasarsdominatedbywinds?
Isapredictivephysicstheorypossible?
MartinElvis.X-rayVision,DC,6-8October2015 [email protected]
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?
MartinElvis.X-rayVision,DC,6-8October2015 [email protected]
WarmAbsorberoutflows(WAs)
Lineblendingiswidespread@R=500VirtuallygoneatR=5000
PieceofcakewithX-raySurveyor
model
R=500050ksec
HETGSR~500900ksec
X-raySurveyor
WarmAbsorberoutflows(WAs)
Evensupersonic flowshavenarrowvelocitystructures
100ksec X-raySurveyor
adaptedfromArav,WHIMEXsimulation
Δv ~50kms-1800kms-1 spread
Multiplemassejectionepisodes?
PieceofcakewithX-raySurveyor
MartinElvis.X-rayVision,DC,6-8October2015 [email protected]
UVstructure
X-raystructure
Gabeletal.2003NGC3783HETGS
WarmAbsorberoutflows(WAs)
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?
. .
MartinElvis.X-rayVision,DC,6-8October2015 [email protected]
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?
MartinElvis.X-rayVision,DC,6-8October2015 [email protected]
Ultra-FastOutflows(UFOs)
• LowionizationcomponentsarefoundinWarmAbsorbers
• 2-3phasesinpressureequilibrium?• WhynotinUFOs?
à R=5000toseelownion linesà LowenergiesforlowΞ transitions
LowIonization,Lownion phases?
Chakravorty etal.,2009
Fe-K
OVII
MartinElvis.X-rayVision,DC,6-8October2015 [email protected]
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
MartinElvis.X-rayVision,DC,6-8October2015 [email protected]
BUTUFOsandBALs
HavewildlydifferentcoldNH>1024 vs <1022 cm-2
BroadAbsorptionLines(BALs)
…havecomplexnarrowvelocitystructureWhynotUFOstoo?
à R=5000toseenarrowcomponents
MartinElvis.X-rayVision,DC,6-8October2015 [email protected]
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?
MartinElvis.X-rayVision,DC,6-8October2015 [email protected]
CouplingMechanisms:1. Winds2. RelativisticJets3. Radiation
Whichdominateswhere?
AlltheseinteractionsshouldgenerateX-raysSpectroscopycandiagnosetheprocess
NarrowEmissionLineRegions(NELRs)
ImagingX-rayOutflows:X-rayCalorimeter
ActiveGalaxyMRK573.ACISsubpixel binning
Paggi etal.,2012
MartinElvis.X-rayVision,DC,6-8October2015 [email protected]
3”
NarrowEmissionLineRegions(NELRs)
X-raysmapinteractionofwind([OIII]),jet(radio)withHostgalaxyISMActiveGalaxyMRK573
[OIII]contoursHST
Paggi etal.,2012
MartinElvis.X-rayVision,DC,6-8October2015 [email protected]
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
MartinElvis.X-rayVision,DC,6-8October2015 [email protected]
3”
NarrowEmissionLineRegions(NELRs)
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
MartinElvis.X-rayVision,DC,6-8October2015 [email protected]
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
MartinElvis.X-rayVision,DC,6-8October2015 [email protected]
• GratingSpectroscopyatR~5000à PhysicsofAGNStructure- ultra-fastoutflows/broadabsorptionlines,warmabsorbers/narrowabsorptionlines
• CalorimeterIntegralFieldUnità AGNFeedbackPhysics- bi-conicalnarrowemissionlineregions
• Modestchangescanmakeadisproportionatedifferenceinscienceoutput
X-raySurveyorand theSpectroscopyofSupermassive BlackHoleOutflows
BUTWillthesebethesciencequestions
In2030?
MartinElvis.X-rayVision,DC,6-8October2015 [email protected]
X-raySurveyorisRobustagainstScienceChanges
X-raySurveyorOpensaLargeDiscoverySpace“100×”
• Imaginggoes~100× deeper• Surveyingis~500-800x faster• Spectrahave~200× #photons,10× resolutionelements
• ~150× informationcontent• newphysicsavailable
MartinElvis.X-rayVision,DC,6-8October2015 [email protected]
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
OutflowsfromSuper-MassiveBlackHoles
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?
PieceofcakewithX-raySurveyor
20σ in20ksec
MartinElvis.X-rayVision,DC,6-8October2015 [email protected]
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?
OutflowsfromSuper-MassiveBlackHoles
Ø Whatisaquasar?Ø QuasarevolutionØ RunawayblackholesØ Versusnuclear fusion(stars)Ø FeedbackØ Warm-HotIntergalacticMedium
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
NarrowEmissionLineRegions(NELRs)
KineticPow
er
Whathappenshere?