ULX accretion state(s)ULX accretion state(s)

Roberto SoriaRoberto SoriaUniversity College London (MSSL)

Thanks also in random order toThanks also in random order to Doug Swartz, Manfred Pakull, Hua Feng, Doug Swartz, Manfred Pakull, Hua Feng,Christian Motch, Luca Zampieri, Fabien Grise’, Jess Broderick, Tim RobertsChristian Motch, Luca Zampieri, Fabien Grise’, Jess Broderick, Tim Roberts

OutlineOutline

Accretion states as mass indicators for ULXsAccretion states as mass indicators for ULXs

Classifying X-ray properties of ULXs into “states”Classifying X-ray properties of ULXs into “states”

Mechanical vs radiative states (jets or no jets)Mechanical vs radiative states (jets or no jets)

Canonical accretion states and state transitionsCanonical accretion states and state transitions

Comptonization-dominated stateComptonization-dominated stateSlim disk stateSlim disk state(High) hard state(High) hard state and where is the standard high-soft state?and where is the standard high-soft state?

1.1. Canonical BH states (short review)Canonical BH states (short review) Mostly defined from stellar-mass Galactic BHsMostly defined from stellar-mass Galactic BHs

State transitions in Cyg X-1 October 1972State transitions in Cyg X-1 October 1972

harder – non-thermal – radio loudharder – non-thermal – radio loud softer – thermal – radio quietsofter – thermal – radio quiet

““Canonical” BH accretion statesCanonical” BH accretion states(From the 1980s… eg, Cyg X-1, GX339-4)(From the 1980s… eg, Cyg X-1, GX339-4)

Low/Hard state Low/Hard state

High/Soft stateHigh/Soft state

FF(0.3-10 keV)(0.3-10 keV)

EE1 keV1 keV 5 keV5 keV

Standard disk Standard disk Radio quietRadio quiet

Jet? Corona? Jet? Corona? ADAF? CENBOL?ADAF? CENBOL?Radio loudRadio loud

Very high stateVery high stateHeavily Comptonized disk Heavily Comptonized disk Radio flaringRadio flaring

m

0.010.01

0.10.1

11

Disk + plDisk + pl

Power-lawPower-law

diskdisk

(Hao, Soria et al 2010, in preparation)(Hao, Soria et al 2010, in preparation)

GRS1758GRS1758

Radio lobesRadio lobes(ATCA 5 GHz)(ATCA 5 GHz)

Canonical state evolution of Galactic BHsCanonical state evolution of Galactic BHs

)( diskCC LLL

diskC LL

Low/hardLow/hard

High/softHigh/soft

0 10.5

Very highVery high

Thick flowThick flowNoisyNoisyJetJet

Thin flowThin flowQuietQuietNo jetNo jet

EddL

ThermalThermalOptically-thickOptically-thickemission from diskemission from disk

EddMM

Power-lawPower-law 0.010.01

0.10.1

11

0.0010.001

Power-lawPower-lawIC in inner disk IC in inner disk or base of outflowor base of outflow(+BMC from outflow?)(+BMC from outflow?)

Truncated disk + ADAFTruncated disk + ADAF Full disk + jet + coronaFull disk + jet + corona

““Canonical” BH accretion statesCanonical” BH accretion states

High/soft state = disk-blackbody spectrumHigh/soft state = disk-blackbody spectrum

4242 ~~ inBHininXdisk TMTRLL

4/1~

~

mT

mLL

in

Xdisk

High/soft state can be used to estimate BH massHigh/soft state can be used to estimate BH mass

erg/s10~ 38BHEddXdisk MLLL

2. Accretion states as indicators 2. Accretion states as indicators of BH mass in ULXsof BH mass in ULXs (where no direct BH mass measurements)(where no direct BH mass measurements)

ULX luminosity functionULX luminosity function

Cartwheel: ~ 1E41 erg/sCartwheel: ~ 1E41 erg/sM82: ~ 1E41 erg/sM82: ~ 1E41 erg/sNGC2276: ~ 1E41 erg/sNGC2276: ~ 1E41 erg/sNGC5775: ~ 8E40 erg/sNGC5775: ~ 8E40 erg/sARP240: ~ 7E40 erg/sARP240: ~ 7E40 erg/sNGC7714: ~ 7E40 erg/sNGC7714: ~ 7E40 erg/s

(ESO243-49: ~ 5—8 E41 erg/s)(ESO243-49: ~ 5—8 E41 erg/s)

0.3-10 keV isotropic L0.3-10 keV isotropic Lof the most luminous ULXsof the most luminous ULXs

Chandra survey of ~200 Chandra survey of ~200 nearby star-forming galaxiesnearby star-forming galaxies

Steepening Steepening or cut-off?or cut-off?

HMXB extrapolation

HMXB extrapolation

Nu

mb

er

of s

ou

rce

s N

(>L)

Nu

mb

er

of s

ou

rce

s N

(>L)

Intrinsic 0.5—8 keV Luminosity (10Intrinsic 0.5—8 keV Luminosity (103939 erg/s) erg/s)

1E391E39 1E401E40

(Swartz et al 2010, in prep)(Swartz et al 2010, in prep)

Most or all of these sources consistent Most or all of these sources consistent with “heavy” stellar BHs up to ~ 70 Mwith “heavy” stellar BHs up to ~ 70 Msunsun

11

1010

100100

Different class? IMBHs?Different class? IMBHs?

D Swartz’s talk todayD Swartz’s talk today

Let’s take a ULX at Let’s take a ULX at LLXX ~ 1E40 erg/s ~ 1E40 erg/s::

What accretion state do we expect?What accretion state do we expect?

If BH mass > 1,000 MIf BH mass > 1,000 Msunsun

we expect to find it in the we expect to find it in the low/hardlow/hard state state (hot corona, jet)(hot corona, jet)

If BH mass ~ 100 – 1,000 MIf BH mass ~ 100 – 1,000 Msunsun

we expect to find it in the we expect to find it in the high/softhigh/soft state state (diskbb, no jet)(diskbb, no jet)

If BH mass ~ 30 -- 100 MIf BH mass ~ 30 -- 100 Msunsun

we expect to find it in we expect to find it in some kind of very high statesome kind of very high state (mildly super-Eddington, Comptonized disk)(mildly super-Eddington, Comptonized disk)

If BH mass ~ 10 -- 30 MIf BH mass ~ 10 -- 30 Msunsun

we expect to find it in we expect to find it in a new kind of strongly super-Edd statea new kind of strongly super-Edd state (thick outflows, beamed?)(thick outflows, beamed?)

If BH mass > 1,000 MIf BH mass > 1,000 Msunsun

If BH mass ~ 100 – 1,000 MIf BH mass ~ 100 – 1,000 Msunsun

If BH mass ~ 30 -- 100 MIf BH mass ~ 30 -- 100 Msunsun

If BH mass ~ 10 -- 30 MIf BH mass ~ 10 -- 30 Msunsun

super-stellarsuper-stellar

stellarstellar

Direct collapse of a metal-poor star (Z ~ 0.1) Direct collapse of a metal-poor star (Z ~ 0.1) with initial mass ~ 120—150 Mwith initial mass ~ 120—150 Msunsun

Core mass up to 70 MCore mass up to 70 Msunsun

+ fallback + accretion+ fallback + accretion

is there a big difference between:is there a big difference between:

-- “normal” stellar BHs (M ~ 5 – 20 solar)-- “normal” stellar BHs (M ~ 5 – 20 solar)-- “heavy” stellar BHs (M ~ 30 – 100 solar)-- “heavy” stellar BHs (M ~ 30 – 100 solar) ??

Let’s look at the Let’s look at the apparent luminosityapparent luminosity

If ULXs are stellar (M < 100 MIf ULXs are stellar (M < 100 Msunsun ) )

mMM

bL

sun

BH ln53

1103.1 38

Accretion rate > 1Accretion rate > 1Beaming ~ 0.2—0.5Beaming ~ 0.2—0.5 BH mass >~ 10BH mass >~ 10

BHEdd aMBH

LL

BHBH eMeMmMM

~~~1

For a fixed super-Eddington luminosity, For a fixed super-Eddington luminosity, the required accretion rate decreases with BH massthe required accretion rate decreases with BH mass

BHaM

BH

donordonor eMM

MM

~~

For super-Edd ULXs, the expected bright lifetime For super-Edd ULXs, the expected bright lifetime increases almost exponentially with BH massincreases almost exponentially with BH mass

m MBH mass (Msun) (Msun / yr)

cR(km)

10 10,000 2E-3 1E6

20 100 5E-5 20,000

30 10 7E-6 2,500

100 1 2E-6 900

Assuming beaming ~ 2 (quasi-isotropic), Assuming beaming ~ 2 (quasi-isotropic), a ULX with a ULX with LLxx ~ 1 E 40 erg/s ~ 1 E 40 erg/s may have: may have:

3.3. Observational classification Observational classification of ULX statesof ULX states

Main problem: spectral coverage only in 0.3-10 keVMain problem: spectral coverage only in 0.3-10 keV

Typical spectral “states” of ULXsTypical spectral “states” of ULXs

0.3 1 5 10E (keV)

Lx

“Soft excess” and break

Power-law ~ 1.5 - 2“Convex spectrum”

0.3 1 5 10E (keV)

Lx

……but very few (if any) diskbb ULXsbut very few (if any) diskbb ULXs

Typical spectral “states” of ULXsTypical spectral “states” of ULXs

Power law ( ~ 2)

“soft excess”

kT ~ 0.15 keV

Holmberg II X-1 (Lx ~ 2E40 erg/s)

Holmberg II X-1 (Lx ~ 2E40 erg/s)

Power-law spectrum Power-law spectrum Photon indexPhoton index= 1.6= 1.6

LLxx ~ 2 E 40 erg/s ~ 2 E 40 erg/s

M99 X1M99 X1

(Soria & Wong 2006)(Soria & Wong 2006)

Broken power-law: Broken power-law: = 0.75= 0.75 below 3 keV, below 3 keV, = 1.4= 1.4 above 3 keV above 3 keVLLxx ~ 2.5E40 erg/s ~ 2.5E40 erg/s

NGC 5474 X1NGC 5474 X1 (Swartz & Soria 2010, in prep)(Swartz & Soria 2010, in prep)

NGC 5575 X1NGC 5575 X1 Hard power-law: Hard power-law: = 1.5= 1.5LLxx ~ 7E40 erg/s ~ 7E40 erg/s

Power-law + soft excessPower-law + soft excess ~ 1.8~ 1.8LLxx ~ 2E39 erg/s ~ 2E39 erg/s

TTinin ~ 0.2 keV ~ 0.2 keV

RRinin ~ 1500 km ~ 1500 km

Simple power-lawSimple power-law ~ 2.1~ 2.1LLxx ~ 5E39 erg/s ~ 5E39 erg/s

NGC 4631 X4NGC 4631 X4

NGC 4631 X5NGC 4631 X5

(Soria & Ghosh 2009)(Soria & Ghosh 2009)

M82 X1 M82 X1 2-10 E 402-10 E 40 (curved) (curved) diskbb?diskbb? 2 E 40 2 E 40 1.2 +/- 0.11.2 +/- 0.1 M82 X2 M82 X2 2-3 E 40 2-3 E 40 1.3-1.5 1.3-1.5 Y YNGC925 NGC925 2.7 E 40 2.7 E 40 2.0 +/- 0.32.0 +/- 0.3IC342 X1 IC342 X1 2 E 40 2 E 40 comp / sd comp / sd 4-6 E 39 4-6 E 39 1.6-1.81.6-1.8IC342 X2 IC342 X2 1.7 E 40 1.7 E 40 comp / sd comp / sdHo IX Ho IX 3 E 40 3 E 40 1.91.9 Y Y 2 E 40 2 E 40 comp / sd comp / sd 1 E 40 1 E 40 1.6-1.81.6-1.8 Y YHo II Ho II 2 E 40 2 E 40 2.5 +/- 0.22.5 +/- 0.2 Y YNGC1313 X1 NGC1313 X1 3 E 40 3 E 40 2.4 +/- 0.12.4 +/- 0.1 Y YNGC1313 X2 NGC1313 X2 1-3 E 40 1-3 E 40 1.7-1.9 1.7-1.9 Y sd? Y sd? 4-6 E 39 4-6 E 39 2.0-2.5 2.0-2.5 Y Y NGC5055 NGC5055 2 E 40 2 E 40 2.5 +/- 0.12.5 +/- 0.1 Y Y 7 E 39 7 E 39 2.3 +/- 0.12.3 +/- 0.1 Y YNGC4559 X1 NGC4559 X1 1.5 E 40 1.5 E 40 1.8-2.1 1.8-2.1 Y YNGC4559 X2 NGC4559 X2 1 E 40 1 E 40 1.8-2.1 1.8-2.1 Y YNGC1068 NGC1068 1.5 E 40 1.5 E 40 0.9 +/- 0.10.9 +/- 0.1NGC5474 NGC5474 1.3 E 40 1.3 E 40 (~1)(~1) broken po broken poNGC3628 NGC3628 1 E 40 1 E 40 1.8 +/- 0.11.8 +/- 0.1 Y (comp) Y (comp)NGC5408NGC5408 0.7-1 E 400.7-1 E 40 2.6-2.72.6-2.7 Y (comp) Y (comp)

LL0.3-100.3-10 + soft x?+ soft x? curvedcurved HS stateHS stateULXULX

NGC5775 X1 NGC5775 X1 7 E 407 E 40 1.7 +/- 0.21.7 +/- 0.2 1 E 40 1 E 40 1.9 +/- 0.21.9 +/- 0.2 NGC5775 X2 NGC5775 X2 1 E 40 1 E 40 1.5 +/- 0.11.5 +/- 0.1 NGC1365 X1 NGC1365 X1 3 E 40 3 E 40 1.8 +/- 0.11.8 +/- 0.1

1 E 40 1 E 40 1.8 +/- 0.11.8 +/- 0.1 Y (curved) Y (curved) 5 E 39 5 E 39 1.8 +/- 0.21.8 +/- 0.2 Y YNGC1365 X2 NGC1365 X2 4 E 40 4 E 40 1.2 +/- 0.11.2 +/- 0.1 1.5 E 39 1.5 E 39 1.2 +/- 0.21.2 +/- 0.2 M99 M99 2 E 40 2 E 40 1.6 +/- 0.11.6 +/- 0.1 NGC4579 NGC4579 1.5 E 40 1.5 E 40 1.9 +/- 0.11.9 +/- 0.1 Antennae X11 Antennae X11 0.7-2 E 40 0.7-2 E 40 1.3-1.8 1.3-1.8 Antennae X16 Antennae X16 0.7-2 E 40 0.7-2 E 40 1.1-1.41.1-1.4 Antennae X42 Antennae X42 1 E 40 1 E 40 1.7 +/- 0.11.7 +/- 0.1 Antennae X35Antennae X35 3 E 403 E 40 2.5 +/- 0.52.5 +/- 0.5 Antennae X44 Antennae X44 1-1.5 E 40 1-1.5 E 40 1.6-2.01.6-2.0 Antennae X? Antennae X? 1 E 40 1 E 40 1.2 +/- 0.11.2 +/- 0.1 NGC5204 NGC5204 0.7-0.9 E 40 0.7-0.9 E 40 2.1-2.4 2.1-2.4 Y Y comp compNGC7714 NGC7714 7 E 40 7 E 40 2.1 +/- 0.22.1 +/- 0.2 4 E 40 4 E 40 (2.6 +/- 0.5)(2.6 +/- 0.5) Y comp Y compCartwheel N10 Cartwheel N10 4-12 E 404-12 E 40 1.9 +/- 0.21.9 +/- 0.2 curved curvedArp240 Arp240 7 E 407 E 40 1.5 +/- 0.51.5 +/- 0.5

LL0.3-100.3-10 + soft x?+ soft x? curvedcurved HS stateHS stateULXULX

Most ULXs classified asMost ULXs classified asPower-law + soft excess + downturn at E ~ 5 keVPower-law + soft excess + downturn at E ~ 5 keV

Some have pure power-law spectraSome have pure power-law spectra(usually hard, photon index < 2)(usually hard, photon index < 2)

Some have curved spectra:Some have curved spectra:thermal but not standard diskthermal but not standard disk

Fitted by slim-disk model (p-free disks)Fitted by slim-disk model (p-free disks)photon trapping & advection, outflowsphoton trapping & advection, outflows (S Mineshige’s talk)(S Mineshige’s talk)

Power-law + soft excess + downturn at E ~ 5 keVPower-law + soft excess + downturn at E ~ 5 keV

Likely physical interpretation:Likely physical interpretation:

Inner disk heavily Comptonized – covered or replaced Inner disk heavily Comptonized – covered or replaced by scattering-dominated region with Te ~ a few keVby scattering-dominated region with Te ~ a few keV

Standard disk at large radiiStandard disk at large radii++

Expected from theory when mdot ~ 10 Expected from theory when mdot ~ 10 L ~ 2-4 LL ~ 2-4 LEddEdd

inner disk becomes effectively thin, hotter (a few keV), inner disk becomes effectively thin, hotter (a few keV),

scattering dominated, scattering dominated, (scattering) ~ a few(scattering) ~ a few

sunBH MM 10030~

Inner disk heavily Comptonized – covered or replaced Inner disk heavily Comptonized – covered or replaced by scattering-dominated region with Te ~ a few keVby scattering-dominated region with Te ~ a few keV

Standard disk at large radiiStandard disk at large radii++

Because it is the most common ULX state, sometimes called Because it is the most common ULX state, sometimes called

““Ultraluminous state”Ultraluminous state” (T Roberts, J Gladstone)(T Roberts, J Gladstone)

Standard diskStandard disk

Thermal spectrumThermal spectrum

Large RLarge Rcc

Low TLow Tinin

Low fLow fqpoqpo

““reprocessing” regionreprocessing” region

Power-law spectrumPower-law spectrum

Xdisk LL %30 Xpo LL %10070

Disk and “power-law” componentsDisk and “power-law” components

Tin

LdiskConfusing definitions of ULX temperatures Confusing definitions of ULX temperatures (claims that “ULXs have hot disks” or “ULXs have cool disks”)(claims that “ULXs have hot disks” or “ULXs have cool disks”)

0.10.1 0.50.5 11

(Soria 2007)(Soria 2007)

ULXs are here?ULXs are here?

Or here?Or here?

Standard diskStandard disk

Tin

Ldisk

Standard diskStandard disk

Outer standard diskOuter standard disk(soft excess)(soft excess)

4indisk TL

indisk TL

Confusing definitions of ULX temperatures Confusing definitions of ULX temperatures (claims that “ULXs have hot disks” or “ULXs have cool disks”)(claims that “ULXs have hot disks” or “ULXs have cool disks”)

0.10.1 0.50.5 11

Slim diskSlim disk2indisk TL

(Soria 2007)(Soria 2007)

Inner hot regionInner hot region

Slim-disk models suggest L ~ 1 -- a few LSlim-disk models suggest L ~ 1 -- a few LEddEdd

““Warm” scattering model suggests L ~ 1 -- a few LWarm” scattering model suggests L ~ 1 -- a few LEddEdd

Either way, most ULXs should have M ~ 30—100 MEither way, most ULXs should have M ~ 30—100 Msunsun

Hard power-law ULXs still not well understoodHard power-law ULXs still not well understoodNo clue on BH mass yetNo clue on BH mass yet

ULXs never lose scattering coronaULXs never lose scattering corona

)( diskCC LLL

diskC LL

Low/hardLow/hard

High/softHigh/soft

0 10.5

ULXs?ULXs?

Thick flowThick flowNoisyNoisyJetJet

Thin flowThin flowQuietQuietNo jetNo jet

EddL

X1: Lx = 3E40 (in 2006)X1: Lx = 3E40 (in 2006) 5E39 (in 2007)5E39 (in 2007) ~ 1.8~ 1.8

NGC1365 X1, X2NGC1365 X1, X2

(Soria et al 2007,2009)(Soria et al 2007,2009)

X2: Lx = 4E40 (in 2006)X2: Lx = 4E40 (in 2006) 1.5E39 (in 2007)1.5E39 (in 2007) ~ 1.2~ 1.2

X1 2006X1 2006

X1 2007X1 2007

X2 2007X2 2007

X2 2006X2 2006

ULXs do not settle into high/soft stateULXs do not settle into high/soft state(never collapse accretion flow into a thin disk)(never collapse accretion flow into a thin disk)

Saturated Comptonization with TSaturated Comptonization with Tee ~ 5 keV? ~ 5 keV?

Decrease of scattering electron TempDecrease of scattering electron Temp T ~ 100 keV T ~ 10 keVT ~ 100 keV T ~ 10 keV

Increase of scattering optical depthIncrease of scattering optical depth ~ 0.1 ~ 0.1 ~ a few ~ a few

(Galactic BHs)(Galactic BHs)

(Galactic BHs)(Galactic BHs) (ULXs)(ULXs)

(ULXs)(ULXs)

Direct transitions low/hard to ultraluminous state?Direct transitions low/hard to ultraluminous state?

ULXs may not follow canonical state transitionsULXs may not follow canonical state transitions

State transition cycle is driven by 2 parameters:State transition cycle is driven by 2 parameters:Accretion rateAccretion rate

““something else” something else” (ang mom? magnetic energy of the inflow?)(ang mom? magnetic energy of the inflow?)

(Belloni 2009)(Belloni 2009)(Zhang et al 1997)(Zhang et al 1997)

Cygnus X-1 never properly switches Cygnus X-1 never properly switches to a disk-dominated stateto a disk-dominated state

GX339-4GX339-4

Cyg X-1Cyg X-1

Seyfert 1 galaxy Ark 564 behaves like a ULXSeyfert 1 galaxy Ark 564 behaves like a ULX

(Belloni 2009)(Belloni 2009)

GX339-4GX339-4

Ark 564Ark 564

Perhaps most AGN are always dominated Perhaps most AGN are always dominated by scattering corona, not pure diskby scattering corona, not pure disk

4. Radiative and mechanical output4. Radiative and mechanical output ULXs have strong winds (shock-ionized bubble nebulae)ULXs have strong winds (shock-ionized bubble nebulae) Do they also have jets?Do they also have jets?

Do ULXs also have jets? Do ULXs also have jets?

)( diskCC LLL

diskC LL

Low/hardLow/hard

High/softHigh/soft

0 10.5

ULXs?ULXs?

Thick flowThick flowNoisyNoisyJetJet

Thin flowThin flowQuietQuietNo jetNo jet

EddL

ULX bubblesULX bubblesShock-ionized nebulae Shock-ionized nebulae with E >~ 1E52 erg and d >~ 100 pcwith E >~ 1E52 erg and d >~ 100 pc

See talks by M Pakull, D RussellSee talks by M Pakull, D Russell

NGC1313 X2NGC1313 X2

Pakull & Mirioni 02, 03Pakull & Mirioni 02, 03Feng & Kaaret 08Feng & Kaaret 08

Pakull & Mirioni 02, 03Pakull & Mirioni 02, 03Grise’ et al 08Grise’ et al 08

Grise’ et al 08Grise’ et al 08

IC342 X1IC342 X1

Holmberg IX X1Holmberg IX X1

Non-nuclear radio jet with long-term-avg power ~ 5 E 40 erg/sNon-nuclear radio jet with long-term-avg power ~ 5 E 40 erg/sin a microquasar of NGC7793 in a microquasar of NGC7793

Accretion state with Accretion state with jet power ~ maximum ULX luminositiesjet power ~ maximum ULX luminositiesM W Pakull’s talkM W Pakull’s talk Pakull, Soria & Motch 2010, Nature, acceptedPakull, Soria & Motch 2010, Nature, accepted

SummarySummaryAccretion states are a BH mass indicatorAccretion states are a BH mass indicator

If high/soft stateIf high/soft state L < LL < LEddEdd, 100 < M < a few 1000 M, 100 < M < a few 1000 Msunsun

If VH or slim disk stateIf VH or slim disk state L < LL < LEddEdd, M < 100 M, M < 100 Msunsun

Most ULXs dominated by p-l or Compt. componentMost ULXs dominated by p-l or Compt. component

(see Hua Feng’s talk)(see Hua Feng’s talk)

Many have soft excess + p-l + high-energy break (“ULX state”)Many have soft excess + p-l + high-energy break (“ULX state”)inner disk modified by scattering-thick region at T ~ a few keVinner disk modified by scattering-thick region at T ~ a few keV

L ~ 1 – a few LL ~ 1 – a few LEddEdd , M ~ 30 – 100 M , M ~ 30 – 100 Msunsun

Some ULXs have hard power law spectrumSome ULXs have hard power law spectrumDirect evolution between low/hard and “high/hard” state?Direct evolution between low/hard and “high/hard” state?

Very few ULXs are found in the high/soft state Very few ULXs are found in the high/soft state (never thin disk)(never thin disk)

We expect ULX to have jets. We expect ULX to have jets. Observational challenge to find them. States with jet power ~ rad powerObservational challenge to find them. States with jet power ~ rad power

Director’s cut for this talkDirector’s cut for this talk

Two or 3 ULXs are in a weird Two or 3 ULXs are in a weird “supersoft state”, T <~ 0.1 keV“supersoft state”, T <~ 0.1 keV

Like Galactic SS sources (= nuclear burning WDs)Like Galactic SS sources (= nuclear burning WDs)But can a WD reach L ~ 1E39 erg/sBut can a WD reach L ~ 1E39 erg/sPhotosphere of massive outflows around a BH?Photosphere of massive outflows around a BH?

HLX1 in ESO243-49HLX1 in ESO243-49 showed a (brief) state transition showed a (brief) state transition from power-law dominated to pure thermal from power-law dominated to pure thermal True high/soft state? True IMBH?True high/soft state? True IMBH?

S Farrell’s talkS Farrell’s talk

Why do some BHs lack a thermal dominant state?Why do some BHs lack a thermal dominant state?

Different BH mass range? Different BH mass range? (ULXs 5 times bigger? 100 times?)(ULXs 5 times bigger? 100 times?)

That should not matterThat should not matter

Different BH spin? Different BH spin? (why?)(why?)

That seems very contrivedThat seems very contrived

Different magnetic field?Different magnetic field?

Different mode of mass transfer?Different mode of mass transfer?No. ULXs are Roche Lobe fed, like LMXBsNo. ULXs are Roche Lobe fed, like LMXBs

Most Galactic BH transients have low-mass donor starsMost Galactic BH transients have low-mass donor stars strongly magnetized accretion flow?strongly magnetized accretion flow?

Most ULXs have OB-type donor starsMost ULXs have OB-type donor stars weakly magnetized accretion flow?weakly magnetized accretion flow?

Why do some BHs lack a thermal dominant state?Why do some BHs lack a thermal dominant state?

Possible effect of the magnetic fieldPossible effect of the magnetic field

Corona may be produced via irradiated disk evaporationCorona may be produced via irradiated disk evaporation(balance between disk evaporation and condensation…Liu & Taam 2007,2009)(balance between disk evaporation and condensation…Liu & Taam 2007,2009)

Mass evaporation rate scales with thermal conductivityMass evaporation rate scales with thermal conductivity(Meyer-Hofmeister & Meyer 2006)(Meyer-Hofmeister & Meyer 2006)

Heat conduction strongly reduced in magnetized plasmasHeat conduction strongly reduced in magnetized plasmas(Chandran & Cowley 1998)(Chandran & Cowley 1998)

Most Galactic BHs have low-mass (magnetic) donor starsMost Galactic BHs have low-mass (magnetic) donor stars (strongly magnetized accretion flow….less evaporation into corona?)(strongly magnetized accretion flow….less evaporation into corona?)

Most ULXs and AGN have non-magnetic accretion flowsMost ULXs and AGN have non-magnetic accretion flows (weakly magnetized accretion flow….more evaporation into corona…(weakly magnetized accretion flow….more evaporation into corona………denser, thicker corona… more difficult to collapse it into pure disk state?)denser, thicker corona… more difficult to collapse it into pure disk state?)

New discovery: New discovery: ULX & bubble inULX & bubble inNGC 5585NGC 5585 (d ~ 7 Mpc)(d ~ 7 Mpc)

SDSS imageSDSS image

Check with Matonick & Fesen’s HCheck with Matonick & Fesen’s H survey survey

Chandra image

300 pc300 pc

ULX with Lx = 5 E 39 erg/sULX with Lx = 5 E 39 erg/s

New discovery:New discovery:

NGC 7793 S26NGC 7793 S26(d ~ 3.9 Mpc)(d ~ 3.9 Mpc)

GalexGalex

Magellan image (BVR)Magellan image (BVR)Liu & Soria (August 09)Liu & Soria (August 09)

S26 nebula discovered by Blair & Long 1997S26 nebula discovered by Blair & Long 1997Radio nebula by Pannuti et al 2002Radio nebula by Pannuti et al 2002X-ray counterpart identified by Pakull et al 2008X-ray counterpart identified by Pakull et al 2008

X-ray “triple source” in S26X-ray “triple source” in S26

X-ray core + hot spotsX-ray core + hot spots

Proof of collimated jetProof of collimated jet

Core (active BH): power-law spectrum Core (active BH): power-law spectrum

erg/s1064.1 3683.0 L

keV9.03.0 kTerg/s102 37

83.0 L

Hot spots: thermal spectrumHot spots: thermal spectrum

Chandra spectra of core and hot spots in S26Chandra spectra of core and hot spots in S26(Pakull, Soria & Motch 2010; Soria et al 2010)(Pakull, Soria & Motch 2010; Soria et al 2010)

5.5 GHz (ATCA)5.5 GHz (ATCA)

9.0 GHz (ATCA)9.0 GHz (ATCA)

Radio spectral indexRadio spectral index

HH map map5.5 GHz contours5.5 GHz contoursX-ray core/hot spotsX-ray core/hot spots

erg/s103 38HL

FWHM = 250 km/sFWHM = 250 km/s(~ expansion velocity)(~ expansion velocity)

Size: 290 x 130 pcSize: 290 x 130 pc

Core not detectedCore not detected(2001 CTIO image)(2001 CTIO image)

HeII 4686HeII 4686

Nebula emissionNebula emission

Core emission:Core emission:EW ~ 30 AEW ~ 30 A

VLT image 2002VLT image 2002

(consistent with (consistent with Wolf-Rayet star)Wolf-Rayet star)

He II 4686 mapHe II 4686 mapwith Hwith H contours contours

Shock ionization modelsShock ionization modelssuggest v(shock) ~ 275 km/ssuggest v(shock) ~ 275 km/s

Density (ISM) ~ 1 cmDensity (ISM) ~ 1 cm-3-3

Zoomed-in viewZoomed-in viewof the S lobeof the S lobe(Magellan image 2009)(Magellan image 2009)

Core (BH)Core (BH)Optical counterpart:Optical counterpart:B ~ 23 magB ~ 23 mag

X-ray hot spotX-ray hot spot

Radio hot spotRadio hot spot

Energy in the bubbleEnergy in the bubble

Standard bubble expansion model Standard bubble expansion model (self-similar solution, Weaver et al 1977)(self-similar solution, Weaver et al 1977)

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r j

)/)(5/3( trv

Mechanical power Mechanical power PPjj ~ 3 x 10 ~ 3 x 104040 erg/s erg/s

Characteristic age ~ 2 x 10Characteristic age ~ 2 x 1055 yrs yrs

Total energy Total energy EE ~ 10 ~ 105353 erg erg

Most of it is thermal energy of protons and ionsMost of it is thermal energy of protons and ions+ work to inflate the bubble against ISM pressure+ work to inflate the bubble against ISM pressure(expanding at v ~ 250 km/s)(expanding at v ~ 250 km/s)

Main properties of S26Main properties of S26

S26 has the same power as a ULX but in the jetS26 has the same power as a ULX but in the jet

current X-ray luminosity << long-term average jet powercurrent X-ray luminosity << long-term average jet power

S26 nebula is 2 x larger and a few times more powerful than SS433/W50S26 nebula is 2 x larger and a few times more powerful than SS433/W50

Collimated jetCollimated jet

First evidence of steady collimated jet at accretion rates > Eddington?First evidence of steady collimated jet at accretion rates > Eddington?

Ultraluminous X-ray sourcesUltraluminous X-ray sources

Ultrapowerful jet sourcesUltrapowerful jet sourcesPP >~ 10 >~ 104040 erg/s erg/s

Radio hot spots & lobes = synchrotron emissionRadio hot spots & lobes = synchrotron emission

X-ray hot spots = thermal plasma emissionX-ray hot spots = thermal plasma emission

Bright optical core with HeII 4686 emission (Wolf-Rayet? Accretion disk?)Bright optical core with HeII 4686 emission (Wolf-Rayet? Accretion disk?)

Comparison between S26 and quasarsComparison between S26 and quasars

BH jets/winds ionize a gas bubble of radiusBH jets/winds ionize a gas bubble of radius

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PPjj ~ 3 x 10 ~ 3 x 104040 erg/s erg/s

Active for ~ 2 x 10Active for ~ 2 x 1055 yrs yrs

PPjj ~ a few x 10 ~ a few x 104646 erg/s erg/s

Active for ~ 5 x 10Active for ~ 5 x 1088 yrs yrs

ISM densities ~ 1 cmISM densities ~ 1 cm-3-3 IGM/ISM densities ~ 0.01-1 cmIGM/ISM densities ~ 0.01-1 cm-3-3

Can shock-heat a bubble Can shock-heat a bubble of size R ~ 100 pcof size R ~ 100 pc

Can shock-heat a bubble Can shock-heat a bubble of R ~ a few hundred kpcof R ~ a few hundred kpc

S26S26 Typical quasarTypical quasar

ConclusionsConclusions

BHs with super-Eddington accretion can be detected as ULXsBHs with super-Eddington accretion can be detected as ULXs(X-ray selected = radiation-dominated by definition!)(X-ray selected = radiation-dominated by definition!)

Most ULXs are likely to be due to super-Edd accretionMost ULXs are likely to be due to super-Edd accretionrather than intermediate-mass BHs. rather than intermediate-mass BHs. (M82 X1 is perhaps unique exception so far)(M82 X1 is perhaps unique exception so far)

Many ULXs also have powerful windsMany ULXs also have powerful winds(Mechanical power in addition to the X-ray emission)(Mechanical power in addition to the X-ray emission)

Some super-Eddington BHs may be jet dominated Some super-Eddington BHs may be jet dominated but radiatively faintbut radiatively faint (S26 in NGC7793) (S26 in NGC7793)

Relative power in the jet and radiation Relative power in the jet and radiation during super-Edd accretion is a fundamental issue during super-Edd accretion is a fundamental issue to understand quasar feedbackto understand quasar feedback

Low-mass and High-mass X-ray binariesLow-mass and High-mass X-ray binaries

Sources in EllipticalsSources in Ellipticals(LMXBs)(LMXBs)

(Swartz et al 2003)

Sources in Spirals/IrrSources in Spirals/Irr(HMXBs)(HMXBs)

ULXsULXserg/s 103~ 39XL

HMXBs found in starburst or actively starforming galaxiesHMXBs found in starburst or actively starforming galaxies

Luminosity function Luminosity function

is steeper for LMXBsis steeper for LMXBs

Number of HMXBs proportional to star formation rateNumber of HMXBs proportional to star formation rate

LMXBs found in elliptical galaxies and old bulgesLMXBs found in elliptical galaxies and old bulgesNumber of LMXBs proportional to stellar mass of a galaxyNumber of LMXBs proportional to stellar mass of a galaxy

We have discovered the optical counterpart of HLX1We have discovered the optical counterpart of HLX1by subtracting the diffuse stellar component of ESO243-49by subtracting the diffuse stellar component of ESO243-49

(Soria et al 2010)(Soria et al 2010)

Properties of the optical counterpart:Properties of the optical counterpart:

R ~ 23.8 +/- 0.3 magR ~ 23.8 +/- 0.3 magV ~ 24.5 +/- 0.3 magV ~ 24.5 +/- 0.3 mag

Two possibilities:Two possibilities:

Old, massive globular cluster in ESO243 (at 100 Mpc)Old, massive globular cluster in ESO243 (at 100 Mpc)(like Omega Cen, mass ~ 1E6 solar masses)(like Omega Cen, mass ~ 1E6 solar masses)

Foreground M-star in the Galactic Halo (at 1—2 kpc)Foreground M-star in the Galactic Halo (at 1—2 kpc)

IMBH in the core of a globular cluster?IMBH in the core of a globular cluster?

Neutron star LMXB in the Galactic Halo?Neutron star LMXB in the Galactic Halo?

HLX1HLX1

Young star formation in ESO243-49 (UV emission at 2000 Ang, R contours)Young star formation in ESO243-49 (UV emission at 2000 Ang, R contours)

But is it related to the HLX1 or just a chance association?But is it related to the HLX1 or just a chance association?

Swift/UVOT (Soria et al 2010)Swift/UVOT (Soria et al 2010)

XMM spectraXMM spectra

Swift spectrumSwift spectrum

X-ray spectra are power-law + soft thermal componentX-ray spectra are power-law + soft thermal componentThermal component has Thermal component has kT ~ 0.15 keVkT ~ 0.15 keV

It could beIt could beAccretion disk around an IMBH (at d ~ 100 Mpc)Accretion disk around an IMBH (at d ~ 100 Mpc)

Surface emission from a faint neutron star LMXB Surface emission from a faint neutron star LMXB in the Galactic Halo (d ~ 1—2 kpc)in the Galactic Halo (d ~ 1—2 kpc)

Aug 2008Aug 2008 Apr 2010Apr 2010

X-ray lightcurve shows rapid state transitionsX-ray lightcurve shows rapid state transitions

State transitions of an IMBH accretion diskState transitions of an IMBH accretion diskor intermittent accretion onto a neutron star surface?or intermittent accretion onto a neutron star surface?

ConclusionsConclusions

HLX1 was called a “proven” IMBHHLX1 was called a “proven” IMBH

We found an optical counterpart to HLX1We found an optical counterpart to HLX1

From optical and X-ray properties, From optical and X-ray properties, we argue that there are still 2 possibilities:we argue that there are still 2 possibilities:

IMBH in the core of a globular cluster in that distant galaxyIMBH in the core of a globular cluster in that distant galaxyin that case, L(0.3—10 keV) ~ 1E41 – 1E42 erg/sin that case, L(0.3—10 keV) ~ 1E41 – 1E42 erg/s

Foreground neutron star LMXB in the Galactic HaloForeground neutron star LMXB in the Galactic Haloin that case, L(0.3—10 keV) ~ 1E32 – 1E33 erg/sin that case, L(0.3—10 keV) ~ 1E32 – 1E33 erg/s

(Personally, I would bet my money on the neutron star scenario)(Personally, I would bet my money on the neutron star scenario)

Slim diskSlim disk Standard diskStandard disk ADAFADAF(ULX?)(ULX?) (high/soft)(high/soft) (low/hard)(low/hard)

Radiative MHD simulations by Ohsuga et al 2009Radiative MHD simulations by Ohsuga et al 2009