1 INTRODUCTION
Ultra-luminous X-ray sources (ULXs) are X-ray sources located outside the nucleus of their host galaxy, with luminosities that exceed the Eddington luminosity (L Edd) of a stellar mass black hole (BH), where L Edd = 1.3 × 1038 (M M⊙ −1) erg s−1. In the literature, an off-nuclear source is often considered to be a ULX if L > 1.3 × 1039 erg s−1. These enigmatic sources were first discovered with the Einstein observatory between 1978 and 1981 (Fabbiano Reference Fabbiano1989) and their nature was unclear. Fabianno (Reference Fabbiano1989) did state that if these sources were indeed accreting compact objects, they would indicate massive (stellar mass) black holes. The high luminosities, in conjunction with observations that showed various ULXs in different spectral states, along with the fact that some ULXs appeared to show spectral state transitions (Kubota et al. Reference Kubota, Mizuno, Makishima, Fukazawa, Kotoku, Ohnishi and Tashiro2001), supported the idea that most ULXs are accreting black holes.
The masses of the ULX black holes are still somewhat under debate. If we assume that the maximum radiative luminosity from the spherical accretion of matter is indeed at the Eddington limit, the high luminosities observed from ULXs would imply that these sources are the previously unobserved and long sought after intermediate mass black holes (IMBH; ~102 to ~105 M⊙). Such sources are believed to exist as it is thought that mergers of IMBHs could be at the origin of supermassive black holes, e.g. Madau & Rees (Reference Madau and Rees2001), or that super-Eddington accretion onto smaller mass BHs could allow them to grow into supermassive black holes, via the IMBH state (Kawaguchi et al. Reference Kawaguchi, Aoki, Ohta and Collin2004). How IMBHs form and where they are located are two of a number of open questions concerning IMBH (Miller & Colbert Reference Miller and Colbert2004). They could be formed through the accretion of gas or smaller stars and therefore reside in the centres of old dense stellar clusters (globular clusters) or they may be formed directly in young star forming regions, e.g. Miller & Colbert (Reference Miller and Colbert2004). IMBHs are therefore the missing BH link. Further, they are interesting for a diverse range of fundamental physics and astrophysical subjects. It has been proposed that they may inject essential energy into globular clusters to slow down the eventual core collapse, e.g. Hut et al. (Reference Hut1992), that dark matter may be relatively simple to detect around IMBH, e.g. Fornasa & Bertone (Reference Fornasa and Bertone2008), that IMBHs may have played a role in the cosmological ionisation (Madau et al. Reference Madau, Rees, Volonteri, Haardt and Oh2004), or that they may be strong sources of gravitational waves if the IMBH has a compact object companion in an elliptical orbit around it (Miller & Colbert Reference Miller and Colbert2004) and that gas accretion onto IMBHs should have made a significant contribution to the UV background (Kawaguchi Reference Kawaguchi2003).
However, not all ULXs can host black holes of such a high mass. For instance, King (Reference King2004) showed that the population of ULXs in the cartwheel galaxy is difficult to explain if they are all IMBHs, as much of the star-forming mass would then end up as IMBHs. Alternatively, if the ULX emission is collimated, possibly through a geometrically thick accretion disc (King et al. Reference King, Davies, Ward, Fabbiano and Elvis2001) or via relativistic boosting (Körding, Falcke, & Markoff Reference Körding, Falcke and Markoff2002), the emission could simply appear to exceed the Eddington limit. Indeed a number of Galactic black hole binaries are seen to surpass such a limit, i.e. V4641 Sgr (Hjellming et al. Reference Hjellming2000) and GRS 1915+105 (Done, Wardziński, & Gierliński Reference Done, Wardziński and Gierliński2004). Luminosities up to ~1041 erg s−1 can be plausibly explained through beaming effects (Poutanen et al. Reference Poutanen, Lipunova, Fabrika, Butkevich and Abolmasov2007; Freeland et al. Reference Freeland, Kuncic, Soria and Bicknell2006) and/or hyper-accretion onto stellar mass BHs (Poutanen et al. Reference Poutanen, Lipunova, Fabrika, Butkevich and Abolmasov2007; Begelman Reference Begelman2002). Therefore, the majority of ULXs are thought to host BHs with masses close to those of stellar mass black holes (Roberts Reference Roberts2007). However, a rare class of ULXs – the hyper-luminous X-ray sources (HLX) – emit X-rays at luminosities >1041 erg s−1 (Gao et al. Reference Gao, Wang, Appleton and Lucas2003) and require increasingly complicated scenarios to explain them without invoking the presence of an IMBH.
Few candidate HLX have been observed, but one excellent candidate is a 2XMM X-ray catalogue source (Watson et al. Reference Watson2009) 2XMM J011028.1460421, discovered as an off-nuclear X-ray source seemingly associated with the galaxy ESO 243-49, 95 Mpc (z = 0.0224) away (Farrell et al. Reference Farrell, Webb, Barret, Godet and Rodrigues2009). The optical counterpart located by Soria et al. (Reference Soria, Hau, Graham, Kong, Kuin, Li, Liu and Wu2010) using the excellent X-ray position derived from Chandra data (Webb et al. Reference Webb, Barret, Godet, Servillat, Farrell and Oates2010) shows an Hα emission line commensurate with the galaxy distance, thus confirming the association with ESO 243-49 (Wiersema et al. Reference Wiersema, Farrell, Webb, Servillat, Maccarone, Barret and Godet2010). Taking the maximum X-ray luminosity of 1.1 × 1042 erg s−1 (0.2–10.0 keV, unabsorbed) and assuming that this value exceeds the Eddington limit by a factor of 10, implies a minimum mass of 500 M⊙ (Farrell et al. Reference Farrell, Webb, Barret, Godet and Rodrigues2009). Modelling and Eddington scaling of the X-ray data imply a mass of ~104 M⊙ (Godet et al. Reference Godet2012a; Davis et al. Reference Davis, Narayan, Zhu, Barret, Farrell, Godet, Servillat and Webb2011; Servillat et al. Reference Servillat, Farrell, Lin, Godet, Barret and Webb2011) and recent radio observations yield an upper mass limit of 9 × 104 M⊙, supposing Eddington scaling (Webb et al. Reference Webb2012). This source goes under the name of ESO 243-49 HLX-1 or HLX-1 for short.
1.1 ULXs and their different states
Many ULXs are seen to be variable, particularly in the X-ray domain, e.g. Kubota et al. (Reference Kubota, Mizuno, Makishima, Fukazawa, Kotoku, Ohnishi and Tashiro2001) and Kajava & Poutanen (Reference Kajava and Poutanen2009). In addition, the fact that most ULXs are accreting black holes means that they are frequently likened to Galactic black hole X-ray binaries (GBHB), albeit extreme versions. GBHBs show both long and short term X-ray variability. On the long term, they exhibit well-defined X-ray states: the high/soft (or thermal), low/hard (or hard) and very high (or steep power law) states, see for instance Remillard & McClintock (Reference Remillard and McClintock2006). Much work has gone into understanding if ULXs behave in a similar way to GBHBs (Gladstone & Roberts Reference Gladstone and Roberts2009; Kajava & Poutanen Reference Kajava and Poutanen2009; Roberts et al. Reference Roberts2012). Such studies indicate that the majority of ULXs show a more extreme version of the GBHB states, going beyond the high state and into super-Eddington accretion regimes, known as the ultra-luminous accretion state (Gladstone, Roberts, & Done Reference Gladstone, Roberts and Done2009), see also Section 2. Observing these states, and transitions between them, could provide important information on how the Eddington limit can be broken, which may require new physics. Super Eddington accretion has been invoked to explain how the earliest supermassive black holes were formed, e.g. Kajava et al. (Reference Kajava and Poutanen2009).
Some ULXs, however, have been shown to exhibit the canonical X-rays states observed from GBHBs, the first of these being HLX-1, see Section 2.1. This may indicate that ULXs can be divided into sub-classes, namely with sub- and super-Eddington emission. The implications of this are discussed further in Section 2.1.
1.2 ULX nebulae
Some ULXs show optical emission-line nebulae, due to shock-ionised driven jets, outflows or disc winds, and/or because of photo-ionisation from the X-ray and UV emission around the black hole. Some of these also show a radio counterpart. These nebulae can be used as a calorimeter to infer the total intrinsic power of the ULX (Pakull & Mirioni Reference Pakull and Mirioni2002, Reference Pakull and Mirioni2003), and also to understand how outflows and photo-ionisation can play a role in the behaviour of the ULX and on its surrounding environment (Pakull & Mirioni Reference Pakull and Mirioni2002, Reference Pakull and Mirioni2003; Roberts et al. Reference Roberts, Goad, Ward and Warwick2003; Kaaret et al. Reference Kaaret, Alonso-Herrero, Gallagher, Fabbiano, Zezas and Rieke2004b).
1.3 Spatial and temporal variability with upcoming instrumentation
With the wide range of new and forthcoming observatories and surveys over the next few years, there will be a huge amount of data available to study open questions surrounding ULXs. The new hard X-ray observatory, Nuclear Spectroscopic Telescope Array (NuSTAR), launched on 2012 June 13 operates in the band 3-79 keV (Harrison et al. Reference Harrison2013). Compared to other X-ray satellites such as XMM-Newton and Chandra, that only probe the spectrum up to ~12 keV, NuSTAR’s extended X-ray spectral band allows us, for the first time, to probe ULX spectra above 10 keV with high signal to noise. This should allow us to constrain models describing the ultra-luminous state in the near future. It will also allow us to uncover new ULXs (e.g. Walton et al. Reference Walton2013b), thanks to the large field of view (FOV; 10 arcmin at 10 keV, 50% response), that were previously veiled by strong interstellar absorption, maybe revealing a new shrouded population of ULXs, for example.
In the optical, future surveys such as the Large Synoptic Survey Telescope (LSST)Footnote 1 will observe the sky using an 8.4-m telescope. The observations will be made using 6 bands (0.3–1.1 micron), and have a 3.5° FOV. It is expected to be operating in 2022 and will regularly scan the sky, so it will be ideal for picking out new and monitoring known transient ULXs. This will help to identify ULXs undergoing state transition, in order to understand how these processes relate to those in GBHBs, see Section 2.
At longer wavelengths still, the new radio arrays that are coming on line in the near future will allow us to probe the same region of the sky repeatedly, to depths that equal the most sensitive radio telescopes currently in use. The Hunt for Dynamic and Explosive Radio Transients with Meerkat (Thunderkat) project will devote 3000 h of time between 2016 and 2020 on the 64 dishes that comprise Meerkat (0.9–1.7 GHz)Footnote 2 . This high sensitivity observatory will allow a 5-σ detection of a faint radio source (14 μJy) in just 8 h. Thunderkat will be devoted to following up transient phenomena as a compliment to the regular Meerkat program. Spectral changes along with spatial and temporal variability in the radio nebulae around ULXs will be probed and new radio ULXs will be discovered with such a program. Similarly, VAST, An ASKAP Survey for Variables and Slow Transients, (Murphy et al. Reference Murphy2013) will have a root mean square (RMS) continuum sensitivity of 47 μJy beam−1 in just 1 h, thanks to its 36 Australian Square Kilometre Array Pathfinder (ASKAP) dishes. It will have a 30° FOV and will conduct broad and deep observations to achieve similar goals, starting as early as 2012.
Almost all of the above-cited projects rely on detecting variability, on temporal or spatial scales, to identify new ULXs, and eventually respond to the open questions cited above. Identifying more ULXs is essential to understand their demographics, especially those that are thought to contain IMBH, as to how they form and evolve and whether they exist in globular clusters are still very much open questions, see Sections 1 and 3. Further, if ULXs are black holes accreting from a high-mass companion, many will evolve to form compact object binaries, e.g. Mandel et al. (Reference Mandel, Brown, Gair and Miller2008). Whilst it will be possible to detect such binaries using the electromagnetic spectrum, the new gravitational wave detectors Advanced LIGO and Advanced Virgo should allow us to detect the inspiral of these binaries for which the BH has a mass greater than 50 M⊙ and up to 10 000 M⊙ (Mandel et al. Reference Mandel, Brown, Gair and Miller2008; Gair et al. Reference Gair, Mandel, Miller and Volonteri2011). Many of the current studies aimed at identifying the numbers of such binaries use the estimated population of ULXs, e.g. Mandel et al. (Reference Mandel, Brown, Gair and Miller2008). It is therefore through determining the population of ULXs that we should get a handle on the number of compact object binaries that we will detect with the new gravitational wave detectors.
In the rest of this review we will look at some specific aspects of ULX variability and how the new facilities coming on line will enable us to respond to questions surrounding ULXs.
2 VARIABILITY DUE TO STATE CHANGES
X-ray spectral changes in conjunction with X-ray luminosity changes have been observed in a number of ULXs, e.g. Kubota et al. (Reference Kubota, Mizuno, Makishima, Fukazawa, Kotoku, Ohnishi and Tashiro2001). However, contrary to the GBHBs, the harder state is often associated with the higher luminosity and the softer state with the lower luminosity. This leads to the fourth GBHB state being proposed, the apparently standard regime (Kubota, Makishima, & Done Reference Kubota, Makishima and Done2004) or ultra-luminous state (Gladstone et al. Reference Gladstone, Roberts and Done2009), when the BH accretes at or above the Eddington limit. However, the physics of this state is not yet understood, e.g. Walton et al. (Reference Walton, Miller, Harrison, Fabian, Roberts, Middleton and Reis2013a). Variability of a factor of about 10 or more in X-rays can be seen during these state changes. Recently Soria et al. (Reference Soria, Kuntz, Winkler, Blair, Long, Plucinsky and Whitmore2012b) observed a previously undetected (L < 1036 erg s−1) object enter the ULX state (L ~ 4×1039 erg s−1), an X-ray flux change of more than 3 orders of magnitude. More recently, a new X-ray binary in M 31 was discovered (Henze et al. Reference Henze2012), which peaks at L x > 1 × 1039 erg s−1, qualifying it as a ULX. Its X-ray emission shows typical ULX states, but radio emission varying on minute timescales has been observed at the mJy level (Middleton et al. Reference Middleton2013). Another source, also showing a transition to the ULX state and with a variability of at least a factor of 100, has been found in M 94 (Lin, Webb, & Barret Reference Lin, Webb and Barret2014). How and why this transition occurs is unclear, but it may be that super-Eddington discs remain slim and accelerate a significant wind with a ‘thick disc’ geometry, unlike in the standard scenario where accretion discs become thick, e.g. Dotan & Shaviv (Reference Dotan and Shaviv2011).
It should be noted, however, that an X-ray variability of a factor of a few can be seen with no spectral state change, see e.g. Soria et al. (Reference Soria, Risaliti, Elvis, Fabbiano, Bianchi and Kuncic2009). The variability and the spectral changes are therefore poorly understood and further observations of known and new sources are essential to understand the behaviour of ULXs, especially in the ultra-luminous regime.
2.1 Canonical black hole states in ULXs
The first ULX to show all three GBHB X-ray states was HLX-1. The source has shown five fast rise and exponential decay (FRED) type X-ray outbursts, characterised by an increase in the count rate by a factor of 40 (Godet et al. Reference Godet2009a, Reference Godet2012a; Lasota et al. Reference Lasota, Alexander, Dubus, Barret, Farrell, Gehrels, Godet and Webb2011) and see Figure 1. From simple spectral fitting, the unabsorbed luminosities range from 1.9 × 1040 to 1.3 × 1042 erg s−1. At high luminosities, the X-ray spectrum shows a thermal state dominated by a disc component with temperatures ≤0.26 keV. At low luminosities the spectrum is dominated by a hard power law with 1.4 ≤ Γ ≤ 2.1, consistent with a hard state. The source has also been observed with a power law spectrum with Γ = 3.3 ± 0.2, consistent with the steep power law state (Farrell et al. Reference Farrell, Webb, Barret, Godet and Rodrigues2009). When HLX-1 is in the high/soft state, the luminosity of the disc component appears to scale with the inner disc temperature to the power of four, which supports the presence of an optically thick, geometrically thin accretion disc. The observed spectral changes and long-term variability are not consistent with variations in the beaming of the emission, nor are they consistent with the source being in a super-Eddington accretion state (Servillat et al. Reference Servillat, Farrell, Lin, Godet, Barret and Webb2011). Indeed, through modelling the X-ray spectra with the Kawaguchi (Reference Kawaguchi2003) disc model and assuming a non-spinning black hole and an inclination of 0°, the accretion flow was determined to be in the sub-Eddington regime for all observations (Godet et al. Reference Godet2012a), radiating close to the Eddington limit at the peak of the outburst. The disc radiation efficiency was shown to be η = 0.11 ± 0.03 (Godet et al. Reference Godet2012a).
Figure 1. The Swift X-ray lightcurve of ESO 243-49 HLX-1 from 2008 until the end of 2013.
In addition, radio flares have been detected from HLX-1 during the low/hard to high/soft state transitions in 2010 and 2011 (Webb et al. Reference Webb2012), in a similar way to GBHBs, which are known to regularly emit radio flares around this transition, e.g. Fender, Homan, & Belloni (Reference Fender, Homan and Belloni2009); Corbel et al. (Reference Corbel, Fender, Tomsick, Tzioumis and Tingay2004). These jets are associated with ejection events, where, for example, the jet is expelled, which can lead to radio flaring when the higher velocity ejecta may collide with the lower-velocity material produced by the steady jet or the local environment. This reinforces the similarity between HLX-1 and the GBHBs. Also, Webb et al. (Reference Webb, Godet, Wiersema, Lasota, Barret, Farrell, Maccarone and Servillat2014) showed that the V-band optical emission increases from before the X-ray outburst and through the X-ray outburst by two magnitudes. This concurrent increase is similar to that observed in GBHBs and opens up the possibility that optical surveys will detect spectral state changes in ULXs.
Other objects have been identified with X-ray luminosities >1040 erg s−1 that show hard power law spectra, e.g. (I. Zolotukhin, N. A. Webb, O. Godet, M. Bacchetti, and D. Barret, in preparation), and some with significant RMS variability (Sutton et al. Reference Sutton, Roberts, Walton, Gladstone and Scott2012), typical of the low/hard state. These objects are not formally HLXs. However, if they are in the low/hard state, which is thought to occur at ~1–2% Eddington luminosity (Maccarone Reference Maccarone2003), and then they switch to the high state (i.e. close to the Eddington luminosity) they will have luminosities of the order of ~1042 erg s−1 and so become HLXs. Such high luminosities indicate that they may contain IMBHs, see Section 1. However, so far, no such state change has been observed in these objects and further observations will be required to confirm the IMBH nature. If confirmed, this would provide an observational constraint for identifying ULXs containing IMBH.
2.2 The ultra-luminous state
Recent work with NuSTAR has focused on understanding the underlying mechanism of the ultra-luminous state. NuSTAR observations of the two ULXs NGC 1313 X-1 and X-2 show a clear cutoff of the X-1’s spectrum above 10 keV, which was only marginally detectable with previous X-ray observations. This cutoff rules out the interpretation of X-1 as a BH in a standard low/hard state, or in a reflection-dominated state. The cutoff is also found to differ from that which is predicted by a single-temperature Comptonisation model (Bachetti et al. Reference Bachetti2013). This is also the case for the new ULX, Circinus ULX5, discovered with NuSTAR (Walton et al. Reference Walton2013b). A spectral transition in NGC 1313 X-2, from a state with high luminosity and strong fractional variability that increases with energy to a lower-luminosity state with no detectable variability, was explained by a transition from a super-Eddington to the sub-Eddington regime (Bachetti et al. Reference Bachetti2013). This type of transition has been observed in other objects, e.g. Burke et al. (Reference Burke2013). Sutton, Roberts, & Middleton (Reference Sutton, Roberts and Middleton2013) showed that high levels of fractional variability are seen in ULXs with soft ultra-luminous spectra as well, likewise for a couple of the broadened disc sources. Furthermore, they observe variability that is strongest at high energies. They propose that such properties are consistent with models of super-Eddington emission, where a massive, radiatively driven wind forms a funnel-like geometry around the central regions of the accretion flow. Future observations with NuSTAR should help to confirm or refute such a hypothesis.
3 WHERE DO ULXs RESIDE?
ULXs are found preferentially in star forming regions, e.g. Grimm, Gilfanov, & Sunyaev (Reference Grimm, Gilfanov and Sunyaev2003), but there is also evidence to show that ULXs form in low metallicity regions, e.g. Pakull & Mirioni (Reference Pakull and Mirioni2002); Mapelli, Colpi, & Zampieri (Reference Mapelli, Colpi and Zampieri2009); and Prestwich et al. (Reference Prestwich, Tsantaki, Zezas, Jackson, Roberts, Foltz, Linden and Kalogera2013). Indeed two of the recently discovered ULXs, see Section 2, appear to have old stellar counterparts (Soria et al. Reference Soria, Kuntz, Winkler, Blair, Long, Plucinsky and Whitmore2012b; Middleton et al. Reference Middleton2013), associating them with old, low metallicity stellar populations.
If ULXs are simply BHs accreting from intermediate or high mass donor stars with the X-ray emission beamed towards us, see Section 1, Irwin, Bregman, & Athey (Reference Irwin, Bregman and Athey2004) argued that ULXs should not be found in old stellar populations. Irwin et al. (Reference Irwin, Bregman and Athey2004) showed that there are indeed very few ULXs associated with early-type galaxies. However, Maccarone et al. (Reference Maccarone, Kundu, Zepf and Rhode2007) discovered a ULX in a globular cluster (typically an old population) in the giant elliptical galaxy NGC 4472, thanks to its strong X-ray variability. Since then, at least five more ULXs have been proposed in extra-galactic globular clusters (Maccarone et al. Reference Maccarone, Kundu, Zepf and Rhode2011; Irwin et al. Reference Irwin, Brink, Bregman and Roberts2010; Shih et al. Reference Shih, Kundu, Maccarone, Zepf and Joseph2010; Brassington et al. Reference Brassington2012; Roberts et al. Reference Roberts2012). Whilst this may seem to support the idea that ULXs are found in metal poor regions, Maccarone et al. (Reference Maccarone, Kundu, Zepf and Rhode2011) found that the five globular cluster ULXs known at the time, were found in metal-rich clusters.
No ULXs have so far been detected in Galactic globular clusters, but Strader et al. (Reference Strader2012) did discover the first stellar mass black holes using radio observations. These black holes may well be slightly more massive than other Galactic stellar mass black holes, but further observations will be required to confirm this possibility (Strader et al. Reference Strader2012). Why no ULXs exist in Galactic globular clusters is so far unexplained, but it may be related to the metallicity (Mapelli & Bressan Reference Mapelli and Bressan2013) or simply because the Galactic globular cluster system is small and thus no such objects may be expected.
With regards to the HLX population, Farrell et al. (Reference Farrell2012) showed through modelling the X-ray and near UV to near IR light that HLX-1 may reside in an old stellar population, akin to a globular cluster, although the preferred solution is a young stellar population (Farrell et al. Reference Farrell2014). None of the other proposed HLXs have been reliably associated with a host stellar population.
Black hole mass scaling relations, e.g. Lützgendorf et al. (Reference Lützgendorf2013) and stellar velocity dispersion measurements in globular clusters, e.g. Anderson & van der Marel (Reference Anderson and van der Marel2010), suggest the existence of IMBHs near or exactly at the potential centre of globular clusters. If these objects are accreting material, they should appear as ULXs/HLXs (depending on the accretion rate). Searches for such objects in Galactic globular clusters using X-ray observations have not revealed such a source, e.g. Pooley & Rappaport (Reference Pooley and Rappaport2006) and Pooley et al. (Reference Pooley2003). If, however, the BH was accreting from gas in the globular cluster, the emission of photons might be inefficient in the X-ray regime. BHs would then appear as compact radio sources co-moving with the globular cluster. Searches for sufficient quantities of gas in Galactic globular clusters have been fruitful. Despite the low gas density, Freire et al. (Reference Freire, Kramer, Lyne, Camilo, Manchester and D'Amico2001) detected a non-negligible amount of ionised gas in 47 Tuc through pulsar timing observations. M 15 also shows evidence for dust (Boyer et al. Reference Boyer, Woodward, van Loon, Gordon, Evans, Gehrz, Helton and Polomski2006) and only a small fraction (~10%, Maccarone (Reference Maccarone2004)) is required to be accreted by a putative IMBH for it to become visible in the X-ray/radio domain.
Radio flares that can accompany state changes should also be detectable in long-term radio observations. To date, neither a continuous nor a flaring radio source has been detected down to the sensitivity limits of current instruments, e.g. Maccarone & Servillat (Reference Maccarone and Servillat2008); Kirsten & Vlemmings (Reference Kirsten and Vlemmings2012); and Strader et al. (Reference Strader, Chomiuk, Maccarone, Miller-Jones, Seth and Heinke2012). This might imply IMBHs simply do not exist in globular clusters or that gas produced by AGB stars in globular clusters does not survive long enough to be accreted by the central source, hence prohibiting the formation of an accretion disc and relativistic jets (Boyer et al. Reference Boyer, Woodward, van Loon, Gordon, Evans, Gehrz, Helton and Polomski2006).
4 ULXs IN FUTURE SURVEYS
The X-ray variability allows new ULXs to be identified using X-ray catalogues such as the 2XMM catalogue of serendipitously detected XMM-Newton sources (Watson et al. Reference Watson2009), e.g. Lin, Webb, & Barret (Reference Lin, Webb and Barret2012). The recently released 3XMM catalogue includes 372 728 unique X-ray sources distributed across 650 deg2 (~1.5%) of sky, almost 50% more sources than in the previous version. Over 123 800 of these sources are provided with both spectra and lightcurves. 3XMM also has the added value that it includes complete uniform reprocessing of all of the data, that exploits the most recent processing and calibration improvements. This is then a fantastic resource for searching for new ULXs.
However, it is likely that within the next 10 yr the existing sensitive X-ray satellites (e.g. Swift, XMM-Newton, Chandra) will no longer be in operation. In the 2020s, it is possible that there will be no new big X-ray telescope to take their place before the launch of Athena+ at the end of the 2020s (Nandra et al. Reference Nandra2013). X-ray telescopes have historically been used to detect and identify new ULXs, often through the variability due to state changes, see Section 2. Without X-ray telescopes surveying the sky, the optical telescopes will take over this role, searching for the optical variability associated with state change and the intrinsic optical variability, both described in Section 2.
Identifying new ULXs through optical observations should eventually lead to the discovery of optical counterparts that are sufficiently bright that short spectroscopic exposures will achieve optical spectra with high enough signal to noise to spectrally identify the companion and to carry out a radial velocity studies, to measure the mass function. This will allow an accurate mass determination of the black hole to finally settle the debate on the mass of the back holes in these objects. Previous attempts to detect a spectrum from the companion have revealed blue, almost featureless spectra (Zampieri et al. Reference Zampieri, Mucciarelli, Falomo, Kaaret, Di Stefano, Turolla, Chieregato and Treves2004; Kaaret & Corbel Reference Kaaret and Corbel2009; Cseh et al. Reference Cseh, Grisé, Corbel and Kaaret2011; Grisé et al. Reference Grisé, Kaaret, Pakull and Motch2011; Roberts et al. Reference Roberts, Gladstone, Goulding, Swinbank, Ward, Goad and Levan2011; Grisé et al. Reference Grisé, Kaaret, Corbel, Feng, Cseh and Tao2012) which are probably dominated by the accretion disc and in some cases show evidence of the surrounding nebula. Some attempts to use disc lines (Motch et al. Reference Motch, Pakull, Grisé and Soria2011; Cseh et al. Reference Cseh, Grisé, Kaaret, Corbel, Scaringi, Groot, Falcke and Körding2013) revealed no mass constraints. This may be because of inadequate time sampling of the radial velocity curve, too low spectral resolution resulting in blurred narrow and broad components, contrasting viewing geometries of the system, or that the He ii line is not emitted from the disc (Cseh et al. Reference Cseh, Grisé, Kaaret, Corbel, Scaringi, Groot, Falcke and Körding2013). M101 ULX-1 has however been shown to have a number of broad emission lines (FWHM > 20 Å), including He ii 4686 Å, He i 5876 Å, and He i 6679 Å, and He i 4471 Å, He i 4922 Å, and He ii 5411 Å lines, and N iii 4640 Å lines. The He i 5876/He ii 5411 Å equivalent width ratio suggests a Wolf-Rayet star. These lines have allowed Liu et al. (Reference Liu, Bregman, Bai, Justham and Crowther2013) to determine the mass of the Wolf-Rayet star (17.5 M⊙) and the radial velocity, which reveals a black hole mass constraint of >5 M⊙, but more likely in the range 20–30 M⊙.
The radio emission variability detected from HLX-1 (see Section 2.1) and the M 31 X-ray binary/ULX (see Section 2) opens up the possibility of discovering new, nearby, low-luminosity ULXs with the upcoming radio surveys. The new radio surveys have very low detection limits (see Section 1). Given that all the firm radio ULX counterparts have a total flux density below ~1 mJy and sizes below 2–15 arcsec at Mpc distances (Cseh et al. Reference Cseh2012; Webb et al. Reference Webb2012), the forthcoming facilities should break the silence in systematic radio surveys looking for ULXs.
Some current surveys, e.g. Legacy e-MERLIN Multi-band Imaging of Nearby Galaxies Survey (LeMMINGs), also search for extended radio emission from ULXs. However, lower resolution facilities may be able to measure flux variations of some of the already known or newly discovered radio bubbles around ULXs. Such variability is expected on the grounds of recent discoveries (Mezcua et al. Reference Mezcua, Roberts, Sutton and Lobanov2013; Cseh et al. Reference Cseh2014), where a working jet is embedded in the radio bubble, heavily perturbing it.
However, detecting distant (e.g. >100 Mpc) ULXs could still be challenging even with the new surveys. This is mainly due to the faint expected flux density of these sources and due to the natural confusion limits; see e.g. the Square Kilometre Array (SKA) (Jackson Reference Jackson2004). So, variability from future detections will have to trigger follow-up, high-resolution radio observations with very-long-baseline interferometry (VLBI).
With regards to spatial variability, measuring proper motions of ULXs (Kirsten & Vlemmings Reference Kirsten and Vlemmings2012) may be a future possibility to independently infer the masses of these objects. Several ULXs are seen to be displaced from nearby star clusters (Kaaret et al. Reference Kaaret, Alonso-Herrero, Gallagher, Fabbiano, Zezas and Rieke2004a) and they may have received natal velocity kicks that might be up to hundreds of km s−1 for a 10-M⊙ black hole (Repetto, Davies, & Sigurdsson Reference Repetto, Davies and Sigurdsson2012; Mapelli & Bressan Reference Mapelli and Bressan2013). To detect such displacements would not just require better than milli-arcsecond resolution, but also perhaps, the detection of self-absorbed compact jets that are typically associated with hard, inefficient accretion states. This might be challenging in the light of the NuStar results, where it was shown that some ULXs are not in a canonical low/hard state, even though the X-ray spectrum is hard (see Section 2.2). Nonetheless, recent VLBI observations of the ULX N5457-X9 in the low/hard state have revealed radio emission which is thought to be coming from compact jets (Mezcua et al. Reference Mezcua, Farrell, Gladstone and Lobanov2013b), indicating that this should be possible, at least for some sources.
