Ultraluminous X-ray Sources

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Presentation transcript:

Ultraluminous X-ray Sources Tim Roberts ULXs in the interacting galaxy pair NGC 4485/4490 (Gladstone & Roberts 2008 - also poster B.11)

A definition ULX: an X-ray source in an extra-nuclear region of a galaxy with an observed luminosity in excess of 1039 erg s-1 Heterogeneous population - includes some recent supernovae - but bulk of sources are black holes accreting from a secondary star The Antennae - Chandra ACIS Wednesday 28th May 2008 Tim Roberts - Ultraluminous X-ray Sources

A new class of black hole? But Eddington limit for spherical accretion: LEdd ~ 1.3 × 1038 (M/M) erg s-1 hence ULXs contain  10 M compact objects – larger still if accretion sub-Eddington – massive black holes. Not super-massive BHs (MBH  106 M); fall to Galactic centre in a Hubble time due to effects of dynamical friction. Too massive for stellar remnants (3M  MBH  18M). Are we observing a new, 102 – 105 M “intermediate mass” class of accreting black hole (IMBHs; e.g. Colbert & Mushotzky 1999)? Again pretty self-evident – but worth adding lots of emphasis to this slide as IMBHs are still very sexy. Wednesday 28th May 2008 Tim Roberts - Ultraluminous X-ray Sources

X-ray evidence for IMBHs X-ray spectroscopic evidence – cool accretion discs (Miller et al. 2003). NGC 1313 X-1 T  M-0.25 Animation – first shows T (temp of accretion disc) prop to Mass of BH to power of -0.25 – i.e. bigger black hole, cooler disc. Next two clicks bring up Miller’s measured temp for ULXs, then typical temp for stellar mass BH. Final click shows mass inferred from Miller’s paper, due to cooler disc. kTin ~ 0.15 keV → ~ 1000 M BHs c.f. kTin ~ 1 keV for stellar BHs Wednesday 28th May 2008 Tim Roberts - Ultraluminous X-ray Sources

Tim Roberts - Ultraluminous X-ray Sources LX – kTin relationship IMBH candidates occupy separate part of parameter space to stellar-mass BHs. Strong evidence for IMBHs as new class underlying luminous ULXs. From Miller et al. (2004) LX  T4 Be brief – self-evident! Wednesday 28th May 2008 Tim Roberts - Ultraluminous X-ray Sources

Vanishing IMBHs problem But some problems with IMBHs, most notably… X-ray luminosity function (XLF), normalised to star formation rate, unbroken over 5 decades. XLF break at ~ 0.1 LEdd for 1000-M IMBHs. No other source population switches off at 0.1 LEdd like this. From Grimm, Gilfanov & Sunyaev (2003) Break at ~ 2 × 1040 erg s-1 Emphasize that IMBHs certainly not a perfect solution – some severe problems! Big point here is that all other sources (NSs, BHs, AGNs) easily surpass a tenth Eddington accretion rate – rather strange that ULXs do not if they’re IMBHs… Wednesday 28th May 2008 Tim Roberts - Ultraluminous X-ray Sources

The link with massive stars High mass stars can feed stellar mass black holes at a sufficient rate to produce the extreme X-ray luminosity From Gao et al. (2003) Potential X-ray luminosities for accretion onto a 10 M BH from 2 – 17 M secondaries (Rappaport, Podsiadlowski & Pfahl 2005) Populations of ULXs (10+) detected in bright starbursts - ULXs must be short-lived, so cannot all be IMBHs Wednesday 28th May 2008 Tim Roberts - Ultraluminous X-ray Sources

Physical processes Still need to break the Eddington limit; suggested methods include: Relativistic beaming (e.g. Körding et al. 2002) Radiative anisotropy (e.g. King et al. 2001) Truly super-Eddington discs (e.g. Begelman 2002; Heinzeller & Duschl 2007) Can combine at least two of the above, e.g. King (2008) - within Rsph local energy release is kept ~ Eddington by driving a bi-conical outflow; so apparent line-of-sight Bolometric luminosity is This summarises a lot of stuff very briefly. Probably best not to go into detail of models. Note on Super-Edd mass transfer based on figure (from Rappaport et al. paper). Note blue stellar companions from ID’ed counterparts (usually HST data – references omitted). For beaming factor b and super-Eddington rate M/MEdd . . Wednesday 28th May 2008 Tim Roberts - Ultraluminous X-ray Sources

Evidence from our own Galaxy Super-Eddington luminosities are seen! GRS 1915+105 has intermittently exceeded LEdd over its ~15 yr outburst (Done et al. 2004) SS433 is super-critically accreting (perhaps exceeding M/MEdd by >103) - if seen face-on it would be an ULX (Fabrika & Mescheryakov 2001, Poutanen et al. 2007) . . SS433: cartoon showing jet precession & inclination Wednesday 28th May 2008 Tim Roberts - Ultraluminous X-ray Sources

Tim Roberts - Ultraluminous X-ray Sources A pause for reflection Dichotomy X-ray evidence such as extreme luminosities and cool accretion discs point to IMBHs, but… Other evidence stacking up in favour of smaller black holes. Which one is the correct interpretation? This slide is simply a bridge into the second half of the talk (my recent stuff). Wednesday 28th May 2008 Tim Roberts - Ultraluminous X-ray Sources

X-ray timing – PSDs & break frequency Break frequencies in PSDs related to black hole mass and accretion rate (McHardy et al. 2006) But most ULXs show little or no variability power (Feng & Kaaret 2005) Break feature in NGC 5408 X-1 PDS @ ~3 mHz (Soria et al. 2004; Strohmayer et al. 2007) implies mass of 100 - 1000 M Frequency regime probed by XMM for bright ULXs Adapted from Vaughan et al. (2005) Scaling of break frequencies with mass, assuming accretion at mdotEdd Wednesday 28th May 2008 Tim Roberts - Ultraluminous X-ray Sources

ULX QPOs Two ULXs with known QPOs - both luminous with LX > 1040 erg s-1 Cannot be beamed Scaling arguments from Galactic black holes - masses ~100 - 1000 M if in known state (talk by Zampieri; Casella et al. 2008) Double QPO in NGC 5408 X-1 (from Strohmayer et al. 2007) QPO in M82 X-1 (from Strohmayer et al. 2003) Wednesday 28th May 2008 Tim Roberts - Ultraluminous X-ray Sources

EPIC-pn light-curve of Ho II X-1 Ho II X-1: timing Goad et al. 2006 Ho II X-1 is a good example of a ULX with little variability power - can we explain this using known accretion states? Not disc-dominated Insufficient power for high or classic very high states Energy spectrum not low/hard state Similar to “χ”-class of GRS 1915+105 in VHS? Band-limited PSD - but don’t see variability, so must be at high-f  MBH < 100 M. EPIC-pn light-curve of Ho II X-1 (0.3 – 6 keV, 100 s binning) Animation – show on second point – emphasizes effectively zero power measured in PSD of Holmberg II. Logical argument is that zero power rules out high state (note that we expect to see red noise power, as we are dominated by the coronal component) Alternatives are very high state or low state – energy spectrum looks like VHS. But VHS is mainly red noise power too – except for some states seen in GRS 1915 In these states PSD noise limited to narrow band at high frequency. If BH is much bigger would expect to see this noise shifted to lower frequency – but we don’t. So BH must be small. Wednesday 28th May 2008 Tim Roberts - Ultraluminous X-ray Sources

ULX spectra revisited Look at best archival XMM-Newton data Stobbart, Roberts & Wilms 2006 Look at best archival XMM-Newton data Demonstrate that 2-10 keV spectrum fit by a broken power-law in all of the highest quality data Invalidates IMBH model - hard component is not a simple power-law Disc Power-law Wednesday 28th May 2008 Tim Roberts - Ultraluminous X-ray Sources

ULX spectra vs Galactic black holes Physical accretion disc plus corona model: cool discs (kT ~ 0.1-0.3 keV), optically-thick coronae ( ~ 5 - 100) ULXs operate differently to common black hole states, but… “Strong” VHS in XTE J1550-564 (Done & Kubota 2006) Disc appears cool as its inner regions are obscured by an optically-thick corona. from Kubota & Done (2004) “ultraluminous branch” (from Soria 2007) Wednesday 28th May 2008 Tim Roberts - Ultraluminous X-ray Sources

A new, ultraluminous accretion state? Spectrum defined by apparently cool disc, power-law turning over at > 2 keV. Little or no variability power present. Occurs at extreme accretion rates Low hard state in GX339-4 vs a classic ULX, Ho IX X-1 Wednesday 28th May 2008 Tim Roberts - Ultraluminous X-ray Sources

The importance of winds Hydrodynamical simulations of extreme accretion rates (M >> MEdd) onto stellar-mass black holes - Ohsuga (2006, 2007) Extreme wind driven - column ~ 3  1024 cm2 at the poles, much higher elsewhere Explains coronae, lack of variability power, giant nebulae…link to high-Z QSOs, Galactic-scale feedback • • Wednesday 28th May 2008 Tim Roberts - Ultraluminous X-ray Sources

Other explanations for spectral break Kerr disc models (Makishima et al. 2000) “Slim” accretion discs (e.g. Watarai et al. 2000) Accretion disc structure changes at highest accretion rates (close to the Eddington limit). Model disc profile T(r)  r -p; standard disc has p = 0.75, slim disc p = 0.5. Recent work finds p ~ 0.6 for ULXs (e.g. Tsuneda et al. 2006, Vierdayanti et al. 2006, Mizuno et al. 2007). Fully comptonised VHS with spectrum modified by ionised fast outflow (Goncalves & Soria 2006). Common thread: high accretion rate, small black holes (MBH < 100 M). Animation – use at Goncalves & Soria paper point. This is an illustration of their model. It illustrates the “bite” taken out of the spectra by absorption from ionised material in a fast-moving wind (Roberto can certainly explain this better than I can!). Make the points pretty much as listed! Wednesday 28th May 2008 Tim Roberts - Ultraluminous X-ray Sources

A multi-wavelength perspective Optical - counterparts and “beambags” (cf. Pakull & Grisé 2008) Bubbles also seen in radio (e.g. Lang et al. 2007) Spitzer observations of NGC 4490 - AGN-like emission lines from ULXs (Vazquez et al. 2007) Identified ULX counterparts are blue - OB stars (e.g. Liu et al. 2004, Kuntz et al. 2005) Nebula around Ho IX X-1 (Grise & Pakull 2006) Wednesday 28th May 2008 Tim Roberts - Ultraluminous X-ray Sources

New HST imaging of ULXs ACS WFC F606W F330W F435W F606W Roberts, Levan & Goad (2008) - arXiv:0803.4470v1 ACS WFC F606W Early F supergiant? NB. high extinction No counterpart, tho’ very high extinction Consistent with late O or early B star F330W F435W F606W mF606W = 23.9 mF606W > 26 mF606W = 24.9 Wednesday 28th May 2008 Tim Roberts - Ultraluminous X-ray Sources

New HST imaging of ULXs (2) ACS WFC F606W Young stellar cluster? (MV ~ 8 - 9) OB Star (odd colours?): U-B ~ -1.4, B-V ~ 0.1 Real ULX, or related to background galaxy? F330W F435W F606W mF606W = 22.0 mF606W = 24.9 mF606W = 25.6 Wednesday 28th May 2008 Tim Roberts - Ultraluminous X-ray Sources

Are these really secondary stars? High LX will affect optical emission; reprocessing in accretion disc becomes more important to optical light as black hole mass increases Stellar heating: stars may be later types than initial colour IDs suggest (late B, not late O/early B) (Patruno & Zampieri 2008; Copperwheat et al. 2007) - small black holes Alternatively, IMBHs may be favoured (Madhusudhan et al. 2008) Stellar-mass BHs IMBHs From Madhusudhan et al. (2008) Wednesday 28th May 2008 Tim Roberts - Ultraluminous X-ray Sources

The goal: mass functions Urgency to finding counterparts: race to get first ULX mass function Best way to resolve mass controversy! He II 4686Å line from accretion disc of NGC 1313 X-2; 300 km s-1 shift (Pakull et al. 2006). Could be used to constrain RV curve, hence constrain ULX black hole mass Radial velocity curve from extragalactic Wolf-Rayet black hole binary IC 10 X-1. Uses He II 4686Å line to constrain mass function, find a black hole mass of ~ 24 - 33 M (Silverman & Filippenko 2008) Wednesday 28th May 2008 Tim Roberts - Ultraluminous X-ray Sources

Tim Roberts - Ultraluminous X-ray Sources So, what are ULXs? Bulk of evidence - few keV X-ray spectral breaks, star formation link etc - argues most ULXs are extreme accretion rate, small (< 100 M) black holes ULX is an accretion state, not a source class Cannot rule out some larger IMBHs - NGC 5408 X-1, M82 X-1 and HLXs (with LX > 1041 erg s-1) are the best candidates? Mass functions are within reach - will resolve the controversy for at least some ULXs Wednesday 28th May 2008 Tim Roberts - Ultraluminous X-ray Sources