Post on 30-Dec-2015
transcript
What are the essential ingredientsWhat are the essential ingredients of ultraluminous X-ray sources?of ultraluminous X-ray sources?
Roberto Soria (CfA & MSSL)Roberto Soria (CfA & MSSL)
Some ULX collaborators: M Cropper, C Copperwheat (MSSL),R Fender (Southampton), Z Kuncic, C Hung (Sydney), D Swartz (MSFC), A Goncalves (Paris-M), M Pakull, F Grise’ (Strasbourg), R. Mushotzky (GSFC)
What we’d like to know about ULXsWhat we’d like to know about ULXs
1)1) MassMass No direct (kinematic) mass determination yet. Two or three candidates perhaps feasible now.
2) How to gain a factor of ~ 50 in apparent 2) How to gain a factor of ~ 50 in apparent LLxx
with respect to stellar-mass BHs
Beamed (microblazars?)
Not beamedHigher BH mass (IMBHs?)
Super-Eddington luminosity
Searching for common features Searching for common features in the ULX populationin the ULX population
““Soft-excess” in their X-ray spectra?Soft-excess” in their X-ray spectra?
Signature of a cool disk? higher BH mass?
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)
Searching for common features Searching for common features in the ULX populationin the ULX population
““Soft-excess” in their X-ray spectra?Soft-excess” in their X-ray spectra?
Signature of a cool disk? higher BH mass?
Most bright ULXs (Lx ~ 1E40 erg/s) have it (Stobbart et al 06)
A few do not, pure power-law spectrum (Winter et al 06)
Evidence of IMBHs, M ~ 1000 Msun ?
““Soft-excess” interpretation is still unclearSoft-excess” interpretation is still unclear
See also poster by Soria, Goncalves & Kuncic
Cool disk emissionCool disk emission
Smeared absorption linesSmeared absorption linesin fast, ionized outflowin fast, ionized outflow
Holmberg II X-1 (Lx ~ 2E40 erg/s)
Power law ( ~ 2.5)
Holmberg II X-1 (Lx ~ 2E40 erg/s)
Injected spectrum (power-law)Injected spectrum (power-law)
Emerging spectra with absorption Emerging spectra with absorption from ionized, fast-moving outflow from ionized, fast-moving outflow (v ~ 0.1 c, n(v ~ 0.1 c, nHH ~ 3E22) ~ 3E22)
Models by Goncalves et al.Models by Goncalves et al.
References:Gierlinski & Done (2004)Crummy et al (2006)Goncalves & Soria (2006)
““Soft-excess” interpretation is still unclearSoft-excess” interpretation is still unclear
See also poster by Soria, Goncalves & Kuncic
Cool disk emissionCool disk emission
Smeared absorption linesSmeared absorption linesin fast, ionized outflow in fast, ionized outflow More generally: absorption + re-emission + reflectionMore generally: absorption + re-emission + reflection
Standard disk around IMBH
Non-standard disk
Essential feature of X-ray spectra:Essential feature of X-ray spectra:
Dominated by non-thermal emissionDisk radiates only ~ 10-20% of output accretion power
Most power is efficiently transferredfrom disk to upscattering medium (jet/corona)
Disk should be cooler than a standard SS disk for a given BH mass
Chilled diskChilled disk
see also Z. Kuncic’s talk
Cooler than standard disk because power is drained from disk into jet+wind+corona
Chilled diskChilled disk
see also Z. Kuncic’s talk
Cooler than standard disk because power is drained from disk into jet+wind+corona
(Soria & Kuncic, in prep.)
Searching for common features Searching for common features in the ULX populationin the ULX population
Jets, outflows?Jets, outflows?
Radio cores:Radio cores: not detectable yet (< 0.1 mJy)Resolved jets:Resolved jets: not detectable yet Radio lobes:Radio lobes: likely detection in a few sources Energy in lobes >~ 1E52 erg Size ~ 50-70 pc Typical fluxes ~ 0.1-0.2 mJy at 5 GHz
(Soria, Fender et al 2006)
Subaru B + ATCA 5 GHz
CFHT H + ATCA 5 GHz
Radio lobes of a ULXRadio lobes of a ULXin NGC 5408in NGC 5408
Searching for common features Searching for common features in the ULX populationin the ULX population
Jets, outflows?Jets, outflows?
Radio cores:Radio cores: not detectable yet (< 0.1 mJy)Resolved jets:Resolved jets: not detectable yet Radio lobes:Radio lobes: likely detection in a few sourcesOptical nebulae:Optical nebulae: observed in many bright ULXs sizes ~ 50-400 pc X-ray photoionized or collisionally ionized?
ULX
Jet lobes?
Hot spot? (hot ring?)
MF16 “SNR” + ULX, in NGC 6946MF16 “SNR” + ULX, in NGC 6946(Swartz et al 2006, in prep)
Optical nebulaeOptical nebulae
30 pc
HST/ACS
NGC 1313 X-2NGC 1313 X-2(Pakull, Grise & Motch 2006)
= 80 pc
Star
Searching for common features Searching for common features in the ULX populationin the ULX population
Jets, outflows?Jets, outflows?
Likely to be essential ingredient Likely to be essential ingredient but more evidence neededbut more evidence needed
Searching for common features Searching for common features in the ULX populationin the ULX population
Young host environment?Young host environment?
Not essential for fainter ULXs (Lx <~ 3E39 erg/s)
Essential for brighter ULXsEssential for brighter ULXs (Lx >~ 1E40 erg/s) Only found in spiral & irregular galaxies
“Young” = less than 50 MyrDonor = OB star transferring gas on its nuclear timescale
Searching for common features Searching for common features in the ULX populationin the ULX population
Starburst environment?Starburst environment?Some ULXs are in starburst galaxies (eg, Cartwheel, Antennae, Mice)
Some are in very quiet corners of nuclear starburst or starforming galaxies (eg, NGC 7714, M83, M99)
Some are in tidal dwarfs with little star formation (eg, Ho II, Ho IX)
NOT AN ESSENTIAL INGREDIENT NOT AN ESSENTIAL INGREDIENT but some associationbut some association
Searching for common features Searching for common features in the ULX populationin the ULX population
Super star-clusters?Super star-clusters?
Suggested as site of IMBH formation via O-star coalescence (Portegies Zwart et al; Rasio et al)
But inconsistent with ULX observations (except for M82 X-1)
Most ULXs found in OB associations or open clusters, with masses <~ a few 1000 Msun
NOT AN ESSENTIAL INGREDIENTNOT AN ESSENTIAL INGREDIENT
Searching for common features Searching for common features in the ULX populationin the ULX population
Colliding or tidally interacting systems?Colliding or tidally interacting systems?
Galaxy-galaxy collisions (eg, ULXs in Antennae, Mice, Cartwheel, NGC 4485/90, NGC 7714/15)
Satellite dwarf – galaxy collisions (eg ULX in NGC 4559) HI cloud – disk collisions (eg ULX in M99)
Tidal dwarfs and tails (eg ULXs in Ho II, Ho IX)
Searching for common features Searching for common features in the ULX populationin the ULX population
Colliding or tidally interacting systems?Colliding or tidally interacting systems?
Essential or very important ingredientEssential or very important ingredient
The Antennae
NGC 4559Examples of ULXs Examples of ULXs formed in colliding eventsformed in colliding events
M99 (Soria & Wong 2006)
XMM EPIC image (0.2-12 keV)
HI contours over R image
LX ~ 2 1040 erg/s
(see poster by Soria & Wong)
High-velocity cloud collision with M99 gas disk
Only a coincidence?
Searching for common features Searching for common features in the ULX populationin the ULX population
Low-metallicity environment?Low-metallicity environment?
Probably a very important ingredientProbably a very important ingredient
Mounting evidence but no systematic study yet (eg, ULXs in Cartwheel, Ho II, NGC 4559, NGC 5408, 1 Zw 18)
More massive BH remnants expected from metal-poor O stars (Mwind ~ Z0.5-0.8)
.
My (biased) conclusions:My (biased) conclusions:
I: NATURE OF (MOST) ULXsI: NATURE OF (MOST) ULXs
Simplest model still consistent with the data:
BH masses ~ 30 – 100 Msun (upper limit of stellar processes)
Age of the accreting systems < 50 Myr (OB donor)
II: (SPECULATIVE) FORMATION PROCESSII: (SPECULATIVE) FORMATION PROCESS
Triggered star formationTriggered star formation (eg, ram p from cloud/galaxy collisions)
Dynamical collapse of molecular clumpsDynamical collapse of molecular clumps(as opposed to turbulent fragmentation)
Fast gas accretion and protostellar mergersFast gas accretion and protostellar mergersin a dense protocluster corein a dense protocluster core (clump mass ~ a few 1000 Msun, much smaller than a super cluster)
Massive stellar progenitor, MMassive stellar progenitor, Mstarstar ~ 200 M ~ 200 Msunsun
BH with a mass ~ 50-100 MBH with a mass ~ 50-100 Msunsun
if metal abundance is lowif metal abundance is low
Total mass ~ 1700 Msun Infall rate ~ 10-3 Msun/yrInfall timescale ~ 1.7 105 yr
CMM3 has 40 MCMM3 has 40 Msunsun, still accreting & merging , still accreting & merging
Externally-triggered dynamical collapse Externally-triggered dynamical collapse of a molecular clump in the Milky Wayof a molecular clump in the Milky Way
Peretto et al. (2006)
40 M40 Msunsun15 M15 Msunsun
35 M35 Msunsun
Very massive stars from clustered star formation exist in the Milky Way & LMC:
Pistol star: initial mass ~ 200 Msun
(but too metal rich to collapse into a BH)
R145 in 30 Dor: M sin3i = (140 +/- 37) Msun
III. POWER BUDGETIII. POWER BUDGET
Accretion rate up to ~ 10 times Eddington
Luminosity near or a few times Eddington
Disk radiates only < 20% of the output power
Disks are cooler than standard SS
Kin. power available for outflows and jets
Can BHs have steady jets when accreting Can BHs have steady jets when accreting at or above Eddington?at or above Eddington?
ULXs could be test cases for QSO super-Edd ULXs could be test cases for QSO super-Edd accretion and feedback models at high redshiftaccretion and feedback models at high redshift
A finis si’. Mersi’ che i l’eve scota’.
Black hole masses in ULXsBlack hole masses in ULXs
X-ray Luminosity function cuts off at ~ 3 x 10X-ray Luminosity function cuts off at ~ 3 x 104040 erg/s erg/sEddington limitEddington limit suggests suggests MM ~ 30 - 200 ~ 30 - 200 MMsunsun
Optical counterparts too faint for direct Optical counterparts too faint for direct mass-function determinationsmass-function determinations
Higher masses (~ 10~ 1033 MMsunsun) speculated from X-ray timing and spectral studies
BH mass from X-ray spectral modelsBH mass from X-ray spectral models
Galactic X-ray binaries generally show:power-law component + thermal disk component
Flatter ( ~ 1.5) when LX <~ 0.01 LEdd
Steeper ( ~ 2.5) when LX ~ LEdd
LLmaxmax ~ L ~ LEddEdd ~ M ~ T ~ M ~ Tinin
LLXX ~ T ~ Tinin R R22 ~ T ~ Tinin M M
22 44 44
- 4- 4
Power-law ( ~ 2.3)Tbb ~ 0.12 keV
X-ray spectrum of NGC4559 X7 (XMM)
X-ray spectrum of NGC4559 X7 (XMM)
Disk kTin ~ 0.13 keV
~ 2.0
kTphot ~ 0.27 keV
Disk kTin ~ 1.9 keV
Tin
LX
10.20.1
1039
1040
1042
1041
1038
(keV)
(erg/s)
Lx = LEdd
2
5 Msun
15 Msun
1000 Msun
IMBH modelIMBH modelGBHsGBHs
Hot-disk modelHot-disk model
IMBH modelIMBH model
Hot-disk modelHot-disk model
kTkTinin ~ 0.12 – 0.15 keV ~ 0.12 – 0.15 keV
M >~ 1000 MM >~ 1000 Msunsun
LLXX ~ 0.05 – 0.2 L ~ 0.05 – 0.2 LEddEdd
kTkTinin ~ 1.5 – 2.5 keV ~ 1.5 – 2.5 keV
M <~ 10 MM <~ 10 Msunsun
LLXX ~ 10 L ~ 10 LEddEdd
Miller, Fabian & Miller (2004)Feng & Kaaret (2005)
Stobbart, Roberts & Wilms (2006)
IMBH modelIMBH model
Hot-disk modelHot-disk model
kTkTinin ~ 0.12 – 0.15 keV ~ 0.12 – 0.15 keV
M >~ 1000 MM >~ 1000 Msunsun
LLXX ~ 0.05 – 0.2 L ~ 0.05 – 0.2 LEddEdd
kTkTinin ~ 1.5 – 2.5 keV ~ 1.5 – 2.5 keV
M <~ 10 MM <~ 10 Msunsun
LLXX ~ 10 L ~ 10 LEddEdd
similar to NLSy1similar to NLSy1
requires exotic requires exotic formation processesformation processes
why do they why do they never reach Lnever reach LEddEdd??
PROBLEMS:PROBLEMS:
IMBH modelIMBH model
Hot-disk modelHot-disk model
kTkTinin ~ 0.12 – 0.15 keV ~ 0.12 – 0.15 keV
M >~ 1000 MM >~ 1000 Msunsun
LLXX ~ 0.05 – 0.2 L ~ 0.05 – 0.2 LEddEdd
kTkTinin ~ 1.5 – 2.5 keV ~ 1.5 – 2.5 keV
M <~ 10 MM <~ 10 Msunsun
LLXX ~ 10 L ~ 10 LEddEdd
similar to NLSy1similar to NLSy1
requires exotic requires exotic formation processesformation processes
why do they why do they never reach Lnever reach LEddEdd??
PROBLEMS:PROBLEMS:
ad hoc (esp. ~ 10 keV)ad hoc (esp. ~ 10 keV)
standard SS disk shouldstandard SS disk shouldnot survive at 10 Lnot survive at 10 LEddEdd ! !
~ 2.8
Alternative model: broad absorption
Summary ISummary I
Unwise to estimate BH masses from X-ray spectraUnwise to estimate BH masses from X-ray spectra
““Soft excess” may be due to absorptionSoft excess” may be due to absorption
New spectral state? (for ULXs and NLSy1?) New spectral state? (for ULXs and NLSy1?)
Low/hard (flat pl)
High/soft (disk)
Very high (steep pl)
Steep pl + absorption in fast, dense outflow
M.
ULX radio counterparts: proof of IMBHs?ULX radio counterparts: proof of IMBHs?
(Merloni, Heinz & DiMatteo 2004; Fender et al 2004)
““fundamental plane” of BH activityfundamental plane” of BH activity
Few ULXs have a radio counterpartFew ULXs have a radio counterpart
M82 (Kording et al 2005)
Holmberg II (Miller, Mushotzky & Neff 2005)
NGC 5408 (Kaaret et al 2003; Soria, Fender et al 2006)
NGC 7424 (Soria, Kuncic et al 2006)
NGC 6946 (Swartz et al 2006, in prep)
NGC 5408 (zoomed in)
X-ray (~1E40 erg/s)
Radio (~ 0.3 mJy at 5 GHz)
H (~1E36 erg/s)
Coincidence between:Coincidence between:
Comparison with X-ray and radio luminosities of Galactic BHs
Steep radio spectrum (thin synchrotron)
Same value in 2000 and 2004
Marginally resolved (radius ~ 30 pc)
More likely radio emission from lobes, not coreMore likely radio emission from lobes, not core
CoreCore = X-rays, flat radio spectrum (if present) Traces the instantaneous accretion stateLobesLobes = steep radio spectrum Trace the integrated jet power over ~ 0.1 Myr
However:However:
Radio lobes or supernova remnant?Radio lobes or supernova remnant?
Not easy to distinguish or disentangle the two(eg, SS433 has SNR + jet lobes)
Leptonic jet model in NGC 5408:Leptonic jet model in NGC 5408: E ~ 3 10E ~ 3 105151 erg erg PPJJ ~ 7 10 ~ 7 103838 erg/s over 1.5 10 erg/s over 1.5 1055 yr yr
Expansion velocity ~ 80 km/sExpansion velocity ~ 80 km/s
A SN model (= 99% relativistic protons) A SN model (= 99% relativistic protons) would requirewould require E ~ 3 10E ~ 3 105252 erg erg (A hypernova, perhaps?)
NGC 7424 (d ~ 12 Mpc)
(Soria, Kuncic, Broderick & Ryder 2006)
ULX-2
State transitionlow/hard high/soft5 1038 7 1039 erg/s
(with thermal plasma)
Point-like (< 60 pc) radio sourceIndex ~ - 0.6 (thin synchrotron)LR ~ 3 x Cas A
Radio lobe or young SNR?Radio lobe or young SNR?(Soria et al 2006b)
Age = 8 +/- 2 Myr
We are starting to find ULX radio counterparts
Radio lobes (FR2 microquasars?) or SNR?
Many ULX radio lobes may have been misclassified as SNRs if the central X-ray source is off
Ratio of ULX radio lobes / “fossil” radio lobes may give us clues on the X-ray duty cycle
Radio/ULX associations useful to determine power budget = radiative vs mechanical output(also important for estimating feedback from early quasars)
Summary IISummary II
Part III: Part III: speculations on ULX formationspeculations on ULX formation
IMBH formation in a young super-star-cluster?IMBH formation in a young super-star-cluster?
Dynamical friction
Mass segregationRunaway core-collapse
Stellar collisions/mergers in the core
Short-lived, very massive star (~1000 Msun)
Hypernova or direct collapse into IMBH
Numerical simulations by Portegies Zwart et aland by Gurkan, Rasio et al.
101066 M Msunsun cluster cluster
1000 M1000 Msunsun BH BH
Problem: Problem: most ULXs are most ULXs are notnot in super-star-clusters in super-star-clusters
Near OB stars but not inside a bound cluster
Have their parent clusters dispersed?Have their parent clusters dispersed?Tidal disruption: always too slow (>~ 50 Myr)SN disruption: perhaps….but there are no signs no signs of the dispersed super clustersof the dispersed super clusters
Were they ejected?Were they ejected?Inconsistent with IMBH, would require low BH mass(eg, Zezas et al 2002; Belczynski et al 2005)
101066 M Msunsun super star clusters super star clusters
with 1000 Mwith 1000 Msunsun BHs BHs
Rarely foundRarely found
Probably not neededProbably not needed
We only need MM ~ 30 -- 200 ~ 30 -- 200 MMsunsun
SuggestionSuggestion::IMBHs formed in smaller proto-clusters, IMBHs formed in smaller proto-clusters, not super clusters not super clusters (Soria 2005)(Soria 2005)
(eg, Kroupa & Boily, 2002-2004; Geyer & Burkert 2001)
protocluster
cluster
OB assoc
Neutral gasprotostars
Ionized gas
~ 0.5 Myr~ 0.5 Myr
Ideal conditions for
forming progenitor “star” with M ~ 100 -- 300 Msun
dispersing the protocluster (binding energy <~ 1052 erg)
M ~ 103.5 -- 105 Msunh < 10 km/s
Combination of accretion (large-scale gas inflow) Combination of accretion (large-scale gas inflow) + coalescence in the protocluster core?+ coalescence in the protocluster core?
Stellar captures and mergers are favoured by proto-stellar disks / envelopes
Collision cross section enhanced at low velocity dispersion (gravitational focussing)
Collision rates & maximum BH mass enhanced at high density
Dense proto-clusters ideal for coalescenceDense proto-clusters ideal for coalescence
Merging BHs: most difficultmost difficultMerging O stars: somewhat easiersomewhat easierMerging protostars, molecular cores: easiesteasiest
Two regimes for coalescence + IMBH formation?Two regimes for coalescence + IMBH formation?
M <~ 105 Msun
h < 10 km/s
IMBH formation in unbound proto-cluster
tcc <~ 0.5 Myr
M >~105.5 Msun
h >~ 10 km/s
tcc <~ 3 Myr
IMBH formation in bound cluster
ULX in a sparse OB assoc (size >~ 100 pc)with expanding gas nebula
ULX in a cluster (size <~ 3 pc)
Additional advantage of the proto-cluster scenario
Same physical process that creates massive Same physical process that creates massive [O + O] binaries, progenitors of BH HMXBs[O + O] binaries, progenitors of BH HMXBs
ULXs = high-luminosity end of HMXBsULXs = high-luminosity end of HMXBs
up to ~ 100-200 Msun
Protoclusters near the Cone nebula
(Peretto, Andre’ & Belloche 2006)
Near-IR contours + 1.2mm continuum
Peretto, Andre’ & Belloche (2006)
Supersonic global inflows in protoclusters Supersonic global inflows in protoclusters (as opposed to random turbulent motion)(as opposed to random turbulent motion)
Two necessary ingredients for a massive BH:Two necessary ingredients for a massive BH:
An An external triggerexternal trigger may cause may cause compression and dynamical collapsecompression and dynamical collapse
1
2 Small mass loss from progenitor star Small mass loss from progenitor star before SN core-collapsebefore SN core-collapse
Low metal abundance (~ 0.1 solar) reduces mass loss in stellar winds
Importance of low metal abundanceImportance of low metal abundance
Heger et al (2003)
Galaxy collisions, cloud-disk collisionsGalaxy collisions, cloud-disk collisions
Triggered star formation
Denser protoclusters, dynamical collapse,high-mass stars
ULXs, upper end of HMXB distribution
(often) starbursts, large number of HMXBs
Observational evidence for ULXs in SSCs?
ULX in a young super-star-cluster in M82Lx varying from ~ 1039 to 1041 erg/s Mbh ~ 1000 Msun Mcl ~ 4 105 Msun
Portegies Zwart et al, Nature, 2004
Near clusters but not in one
ULX in the starburst dwarf NGC 5408with Lx ~ 1040 erg/s
Near B stars but not in a cluster Kaaret et al 2003Soria et al 2004
Near OB stars but not in a super-star-cluster
ULX in the dwarf galaxy NGC 5204 Liu et al 2004
Not in super-star-clusters
ULX in the starburst dwarf NGC5408with Lx ~ 1040 erg/s
Two ULXs in NGC4559 with Lx ~ 1 – 4 1040 erg/s
NGC4559 X-10: near OB stars, no super cluster
A few B stars but no big clusters
Soria et al 2005Cropper et al 2005
Antennae: lots of ULXs, displaced from clusters
ULXs are displaced from SSCs by ~ 100 – 300 pcZezas, Fabbiano et al 2002
Massive proto-stellar mergersMassive proto-stellar mergers
proto-cluster disruptionproto-cluster disruption
Merger of 100 + 100 Merger of 100 + 100 MMsunsun stars starsreleases ~ 10releases ~ 105151 erg erg (Bally & Zinnecker 2005)
Binding energy of the gas in a 10Binding energy of the gas in a 1055 MMsunsun cluster cluster
~ a few 10~ a few 105050 -- 10 -- 105151 erg erg
Single SN releases ~ 10Single SN releases ~ 105151 erg erg
Explosive expulsion of gas
Not in clusters
4 ULXs in the colliding galaxies NGC 7714 / 7715with Lx ~ 2 – 8 1040 erg/s
Smith et al 2005, AJ, 129, 1350
2 are in clusters, 2 are not
NGC4559 X-7: near OB stars, no super cluster
A few B stars but no SSCs
Soria et al 2005