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New insights into ultraluminous X-ray sources from deep XMM-Newton observations



arXiv:astro-ph/0511077v1 2 Nov 2005

T.P. Roberts1 , A.-M. Stobbart1 , M.R. Goad1 , R.S.Warwick1 , J. Wilms2 , P. Uttley3 , and J.N. Reeves3,4

X-ray & Observational Astronomy Group, Dept. of Physics & Astronomy, University of Leicester, University Road, Leicester, LE1 7RH, UK 2 Astronomy & Astrophysics Group, Department of Physics, University of Warwick, Coventry, CV8 1GA, UK 3 Exploration of the Universe Division, NASA Goddard Space Flight Center, Greenbelt Road, Greenbelt, MD 20771, USA 3 Dept. of Physics & Astronomy, Johns Hopkins University, 3400 N Charles Street, Baltimore, MD 21218, USA

ABSTRACT The controversy over whether ultraluminous X-ray sources (ULXs) contain a new intermediate-mass class of black holes (IMBHs) remains unresolved. We present new analyses of the deepest XMM-Newton observations of ULXs that address their underlying nature. We examine both empirical and physical modelling of the X-ray spectra of a sample of thirteen of the highest quality ULX datasets, and ?nd that there are anomalies in modelling ULXs as accreting IMBHs with properties simply scaledup from Galactic black holes. Most notably, spectral curvature above 2 keV in several sources implies the presence of an optically-thick, cool corona. We also present a new analysis of a 100 ks observation of Holmberg II X-1, in which a rigorous analysis of the temporal data limits the mass of its black hole to no more than 100 M⊙ . We argue that a combination of these results points towards many (though not necessarily all) ULXs containing black holes that are at most a few 10s of M⊙ in size. Key words: black hole physics - X-rays: binaries - Xrays: galaxies.

The outstanding piece of recent evidence in support of the presence of IMBHs in ULXs derives from ?tting their Xray spectra with the same empirical model as used for Galactic black hole X-ray binaries (BHXRBs). It has been found that a number of luminous ULXs are well ?tted by the combination of a soft multi-colour disc blackbody (MCDBB, representative of an accretion disc spectrum) plus a hard power-law continuum model (representative of a hot, optically thin corona). However, there is one crucial difference: the temperature of the accretion disc in these ULXs is a factor ? 10 lower, at ? 0.1 ? 0.2 keV, than in Galactic systems. As the temperature of the innermost edge of an accretion disc scales with the mass ?0.25 of the compact object as kTin ∝ MBH , this implies very massive black holes in these ULXs, at ? 1000 M⊙ (e.g. Miller et al. 2003; Miller et al. 2004a). However, recent analyses of high spectral quality ULX data have shown that some ULXs are best described by a variant of this empirical model where the power-law continuum dominates at low energies (e.g. Stobbart et al. 2004; Foschini et al. 2004), and the disc component is similar to that observed in stellar-mass black holes. Furthermore, in the case of NGC 5204 X-1 there is a clear ambiguity, with both model variants ?tting the same data (Roberts et al. 2005). So a bona ?de “alternate” empirical description for the spectra of some ULXs does exist, albeit one with serious physical challenges. In particular the origin of the dominant soft power-law is unclear - it appears too soft to originate in a jet, and cannot be disc-Comptonisation as it dominates well below the peak emissivity of the disc spectrum.



ULXs have garnered a great detail of attention since the launch of Chandra and XMM-Newton, as these missions have provided the ?rst opportunity to study these remarkable objects in great detail (see e.g. Miller & Colbert 2004). The key question in these sources is whether their extreme X-ray luminosities originate in isotropic radiation from a compact object accreting below the Eddington rate - requiring the presence of an IMBH - or whether it can be explained by another means, with the prime suspects being anisotropic or super-Eddington radiation from a stellar-mass black hole.



The existence of this second class of ULX spectral shape, and the ambiguity between this model and the “IMBH”

2 spectrum in NGC 5204 X-1, led us to consider the following questions: ? How easy is it to differentiate the two spectral forms? ? How common is each type of spectrum? ? What are the physics underlying the alternate spectral model? We have therefore selected and uniformly reduced a sample of 13 ULXs, comprising the highest quality EPIC spectral data available from the XMM-Newton archive, to address these questions. The data were primarily selected on the basis of datasets with ? 10 ks or more EPIC exposure, and a measured ROSAT High Resolution Imager count rate > 10 ct ks?1 (taken from Roberts & Warwick 2000 or Colbert & Ptak 2002). Though this sample is small, the ULXs are representative of the full range of ULX luminosity (? 1039 ? 2 × 1040 erg s?1 ), and with a minimum of a few thousand counts per source represent the best de?ned X-ray spectra of ULXs to date. More details on this work will appear in Stobbart et al. (2006). also well-?t by the IMBH model, hence spectral ambiguity is present in 6/13 of the ULXs even in our high data quality sample. Of the remaining sources, two apiece were uniquely well-?t by either the IMBH or alternate model, and the remaining three were well-?t by neither (though two favoured an IMBH ?t, and one the alternate). There is a potential discriminator between the two models that allows us to investigate which model the ambiguous sources prefer, namely curvature in the 2–10 keV range. This should be present in the alternate model (which is dominated by the MCDBB in this regime) but not the power-law-dominated IMBH model. We therefore examined the 2–10 keV data for each ULX by ?tting both power-law and broken power-law models, and looking for a signi?cant improvement between the two ?ts. This approach was vindicated by demonstrating that those sources best ?t by the alternate model showed strong curvature (> 4σ improvements in the broken power-law ?t over the power-law ?t, according to the F-test). Of the ambiguous sources, 3/6 also showed some evidence for curvature (> 2σ signi?cance) as, rather surprisingly, did two of the IMBH model sources. Hence we ?nd at least marginal evidence for 2–10 keV curvature in > 50% of our spectra. The above results suggests that the alternate model is at least a viable description of the spectrum of more than half of our sample. Hence we are once again faced with the problem of the dominant soft power-law. However, as there is no strong physical motivation for using a powerlaw to describe the soft excess apparent in these sources, we decided to test substituting another component, with the constraint that it should have morphological similarities to an absorbed power-law. We therefore attempted ?ts using a classical black body to describe the soft excess, and retained a MCDBB as the harder component (we describe this as a “dual thermal” model). We found this to be the most successful empirical description of the data, producing good ?ts to 10/13 ULXs, with typical parameters of kTBB ? 0.25 keV and kTin ? 1 ? 2 keV. We speculate that this could describe the spectrum of the accretion disc around a stellar-mass black hole, with a related optically-thick out?ow (or “black hole wind”, c.f. King & Pounds 2003) producing the soft excess. We demonstrate one interesting implication of these ?ts in Fig. 1. We essentially re-plot the results of Miller et al. (2004b) as elliptical regions in kTin ? LX space, representing the high-luminosity, low temperature IMBH candidate discs in the top left-hand corner, and the lower luminosity, warm discs of stellar-mass black holes in our own Galaxy in the bottom-right. In the left panel we demonstrate that when we model our sample of ULXs as IMBHs, we reproduce the results of Miller et al. (2004b), that is that the IMBH candidates sit in a separate part of kTin ?LX parameter space from stellar-mass black holes. However, the right panel demonstrates that when we use the (more successful) dual-thermal model, the ULXs appear to sit in a direct, high luminosity continuation of the stellar-mass black hole relationship (broadly LX ∝ T 4 as the accretion rate increases, as expected for standard ac-

2.1. Empirical spectral models Our initial spectral ?ts were made utilising simple single component spectral models, subject only to absorption by material along the line-of-sight to the ULXs. The high de?nition and underlying complexity of the ULX spectra were highlighted by these ?ts, with none of the sources being well-?t (using a 95% probability of rejection criterion) by an absorbed MCDBB model, and only 5/13 being adequately ?t by a power-law continuum (including the three lowest quality datasets). The use of two-component models improved the ?ts considerably. In particular, the IMBH model (i.e. cool MCDBB + hard power-law) produced good ?ts to 8/13 datasets (using the same criterion as above), with an inner-disc temperature kTin ? 0.1 ? 0.25 keV and a power-law photon index Γ ? 1.6 ? 2.5. Again, the disc temperatures inferred in these sources lead to black hole mass estimates in the range ? 1000 M⊙ . However, the anomaly in power-law slope discussed by Roberts et al. (2005) remains - though one might reasonably expect the IMBH accretion disc to be in a “high/soft” or “very high” state, given that it appears to be accreting at or above roughly 10% of the Eddington rate, these states typically (though not exclusively) show power-law continua with photon index Γ > 2.4 (McClintock & Remillard 2005). The power-law continua exhibited by these IMBH candidates therefore appear to possess photon indices that are somewhat on the low side. The alternate empirical model (soft power-law, dominant at low energies, plus a warm MCDBB) also produced a total of 8/13 good ?ts. In fact, six of these sources were


Figure 1. The relationship between accretion disc luminosity and temperature, calculated and displayed as per Miller et al. (2004b). The ellipses represent the regions in which the IMBH candidates (top left) and stellar-mass black holes (bottom right) lay in Figs. 1 & 2 of that paper. Left panel: We overlay data points from our IMBH ?ts (note that we only show 6 of 8 points; of the missing pair, one had a lower temperature [? 80 eV] whilst the other had a temperature that was unconstrained). Right panel: The data points from our dual thermal model overlayed (in this case one disc was too hot to appear within the plotted range). cretion discs). This evidence shows that, at the very least, the mass of the underlying black hole inferred from empirical spectral ?tting of ULXs appears very dependent on the choice of model. Galactic BHXRBs in a classic high/soft state, and we may perhaps need new insight to explain their spectra.

3. 2.2. Physical spectral models We next investigated the origin of the possible 2–10 keV curvature using more physically-motivated models. The “slim disc” model of an accretion disc (e.g. Watarai et al. 2001; XSPEC parameterisation courtesy K. Ebisawa) was only successful in ?tting our spectra in 3/13 cases. Instead, we found a physically self-consistent accretion disc plus Comptonised corona model, using a diskpn + eqpair model in XSPEC (Gierli? ski et al. 2001, Coppi n 2000), gave good ?ts to 11/13 sources (plus a further source that was only marginally rejected at the 95% criterion). All the ?ts display a cool disc component, with temperatures ? 0.1 ? 0.3 keV, as would be expected from IMBHs. However, the majority of these ?ts also show a second remarkable characteristic; the spectral curvature present in many sources originates in a coronal component that is optically thick, with typical optical depths of τ ? 10 ? 40. This is very puzzling, because if ULXs are to be understood as direct higher-mass analogies of high-state BHXRBs, then their coronae should presumably be similarly optically thin (τ < 1). This only occurs in two of our sources, leaving this pair as the best accreting IMBH candidate ULXs within our sample. For the remaining ULXs, that possess apparent optically-thick coronae, it is evident that they are not simple scaled-up


This source is regarded as the archetypal luminous (LX > 1040 erg s?1 ) nearby ULX, and has been widely studied both in X-rays (e.g. Dewangan et al. 2004) and over complementary wavebands (e.g. Kaaret, Ward & Zezas 2004; Miller, Mushotzky & Neff 2005). We were awarded a 100-ks observation of this source in XMM-Newton AO3, the results of which we summarise here (see also Goad et al. 2005).

3.1. Spectra Though more than 60% of this observation was lost to space weather, we were still able to extract the ?rst reasonable signal-to-noise RGS spectrum of an ULX. This showed a smooth continuum shape, modelled simply as an absorbed power-law continuum (NH ? 2 × 1021 cm?2 , Γ ? 2.6) with the exception of an excess of counts slightly above 0.5 keV (see Fig. 1 of Goad et al. 2005). This could be ?t by an O VII triplet, but a much better solution was found by allowing the abundance of the absorbing material to drop to ? 0.6 of the solar value. Interestingly, this result strongly affects the EPIC data modelling. In particular, using a 0.6-solar abundance


Figure 2. Left panel: EPIC X-ray spectra of Ho II X-1. The pn data points are displayed in black, and the MOS in grey. We show the modelled contributions of the accretion disc (dotted lines) and corona (solid lines) separately in the top part of the panel, and show the model ?t residuals in the lower part. Right panel: the residual power density after ?tting the PSD of Ho II with a constant. This demonstrates the lack of variability power in the source. TBABS model in XSPEC (and interstellar abundances set to the values of Wilms, Allen & McCray 2000) greatly reduces the size of the apparent soft excess, and so the mass of the BH estimated from the IMBH model is reduced to ? 33% of its value assuming a solar abundance absorber. However, the best ?t to the data was again found to be the physically self-consistent accretion disc + corona model, with kTin ? 0.2 keV and τ ? 4 ? 9 (i.e. a cool disc and optically thick corona). The EPIC spectral data, with this best-?t model, are shown in Fig. 2. Note there is no detection of an Fe Kα line in this dataset; formally, we place a 90% upper limit of 25 eV on the equivalent width of a narrow 6.4 keV Fe Kα feature. certain very high states. Encouragingly, GRS 1915+105 shows very similar variability characteristics in its “χclass” of behaviour, which is thought to occur whilst it is in the very high state.



3.2. Timing The EPIC timing data showed Ho II X-1 to be remarkably invariant during the observation. A power spectral density (PSD) analysis was performed, ?nding that no power was evident (above the Poisson noise level) in the ? 10?4 ? 6 Hz range (see Fig. 2). This likely rules out Ho II X-1 being in a high/soft state, as a comparison to Galactic black holes and AGN shows they generally have a red noise spectrum with measureable RMS variability in this state1 . It does not rule out a state with a bandlimited PSD, such as occurs in the low/hard or some very high states. However, the strong limits placed by the nondetection of power in the observed frequency interval implies any power must be present at higher frequencies. Assuming that BH timing properties scale linearly with mass (e.g. Uttley et al. 2002), we can place an upper limit on the mass of Ho II X-1 of 100 M⊙ if it is in the low or
1 We note that dilution by photons from the accretion disc should not be a problem for Ho II X-1 if it contains an IMBH, as the 0.3– 6 keV band we derive the PSD from is dominated by the putative coronal component. However, it has been brought to our attention that there may be a dimunition of intrinsic variability in the coronae of high/soft state sources at the highest luminosities (J. Homan, priv. comm.), which merits further quanti?cation.

Whilst it is evident from this work that optically-thick coronae may be common in ULXs, what is their origin? One possible explanation is offered by the model of Zhang et al. (2000), that explains accretion discs as a two-layer system, with a cool (0.2 ? 0.5 keV) interior seeding a warm, optically thick (1 ? 1.5 keV, τ ? 10) Comptonising upper disc layer. This model therefore offers an explanation for both spectral components seen in our modelling. Crucially, it has also successfully been used to describe the X-ray spectrum of GRS 1915+105. We therefore speculate that our spectral modelling, considered along with the mass limit from Ho II X-1, argues that Ho II X-1 and many other ULXs may be analogues of GRS 1915+105. Whilst ULXs may still possess larger BH masses than GRS1915+105 (i.e. 20 - 100 M⊙ , so still technically IMBHs), we suggest they are operating in similar accretion states, with a key link being that the accretion is persistently at around the Eddington limit. Obviously, we cannot rule out cool discs being the signature of a larger, ? 1000 M⊙ IMBH. Indeed, a weakness of the above model is how we manage to see photons from the inner disc layer through an optically thick exterior. However, we note there are also weaknesses with a literal interpretation of cool disc parameters, most notably in the case of PG quasars. Similar soft spectral components - also modelled as cool discs - are seen in PG quasars, where their temperature has been shown to be completely independent of the mass of the BH (Gierli? ski & Done 2004). This implies a radically difn ferent origin for the soft excesses in PG quasars - and, by extension, ULXs - such as in an out?ow (as suggested in

5 our dual-thermal model), or perhaps even as atomic features on the accretion disc spectrum. REFERENCES Colbert E.J.M., Ptak A.F., 2002, ApJS, 143, 25 Coppi, P.S., 2000, HEAD, 5.2311 5. CONCLUDING COMMENTS Dewangan, G., Miyaji, T., Grif?ths, R.E., Lehmann, I., 2004, ApJ, 608, L57 Foschini, L., Rodriguez, J., Fuchs, Y., Ho, L.C., Dadina, M., Di Cocco, G., Courvoisier, T.J.-L., Malaguti, G., 2004, A&A, 416, 529 Gierli? ski, M., Done, C., 2004, MNRAS, 349, L7. n Gierli? ski, M., Maciolek-Niedzwiecki, A., Ebisawa, K., n 2001, MNRAS, 325, 1253 Goad M.R., Roberts T.P., Reeves J., Uttley P., 2005, MNRAS, in press (astro-ph/0510185) Kaaret P., Ward M.J., Zezas A., 2004, MNRAS, 351, L83 King A., 2004, MNRAS, 347, L18 King A., Pounds K.A., 2003, MNRAS, 345, 657 McClintock J.E., Remillard R.A., 2005, to appear in Compact Stellar X-ray Sources, eds. W.H.G. Lewin and M. van der Klis. (astro-ph/0306213) Miller, J.M., Fabbiano, G., Miller, M.C., Fabian, A.C., 2003, ApJ, 585, L37 Miller, J.M., Fabian, A.C., Miller, M.C., 2004a, ApJ, 607, 931 Miller, J.M., Fabian, A.C., Miller, M.C., 2004b, ApJ, 614, L117 Miller M.C., Colbert E.J.M., 2004, Int. J. Mod. Phys. D, 13, 1 Miller N.A., Mushotzky R.F., Neff S.G., ApJ, 623, L109 However, we certainly cannot exclude ULXs from containing ? 1000 M⊙ IMBHs at the current point in time, and indeed two of the sources in our sample do appear consistent with this interpretation. Ultimately it may prove that the only measurement that can resolve the debate on the underlying nature of ULXs will be a dynamical mass limit for the black hole from its orbital motion, as is the case for Galactic BHXRBs. Until then, more and deeper X-ray observations are required to advance our knowledge of these extraordinary X-ray sources. Rappaport S.A., Podsiadlowski Ph., Pfahl E., 2005, MNRAS, 356, 401 Roberts T.P., Warwick R.S., 2000, MNRAS, 315, 98 Roberts, T.P., Warwick, R.S., Ward, M.J., Goad, M.R., Jenkins, L.P., 2005, MNRAS, 357, 1363 Stobbart, A., Roberts, T.P., Warwick, R.S., 2004, MNRAS, 351, 1063 Stobbart, A., Roberts, T.P., Wilms, J., 2006, in preparation ACKNOWLEDGMENTS Uttley, P., McHardy, I.M., Papadakis, I.E., 2002, MNRAS, 332, 231 Watarai, K., Mizuno, T., Mineshige, S., 2001, ApJ, 549, L77 TPR, AMS and MRG gratefully acknowledge funding from PPARC. This work is based on observations obtained with XMM-Newton, an ESA science mission with instruments and contributions directly funded by ESA member states and NASA. Wilms J., Allen A., McCray R., 2000, ApJ, 542, 914 Zhang, S.N., Cui, W., Chen, W., Yao, Y., Zhang, X., Sun, X., Wu, X.-B., Xu, H., 2000, Science, 287, 1239

If ULXs do contain ? 1000 M⊙ IMBHs, as suggested by empirical modelling of their spectra, then one might reasonably assume from their luminosities that they are accreting at ? 10% of the Eddington rate, and so should behave like scaled-up versions of BHXRBs in the highstate. The detection of spectral curvature in the 2–10 keV range in the majority of our sample of ULXs, that can be physically modelled as a cool, optically-thick corona, argues that something different is happening in many ULXs. One explanation could be that these ULXs are operating in a fashion similar to GRS 1915+105, as suggested by the timing results for Ho II X-1, in which case the ULXs might harbour black holes not much more massive than in Galactic BHXRBs. This would bring X-ray spectral results more into line with other arguments on ULXs that suggest that the majority of sources do not contain IMBHs. For example, King (2004) argues that the sheer numbers of ULXs in the most extreme star-forming environments makes it very unlikely that they can all contain IMBHs, and the modelling of Rappaport, Podsiadlowski & Pfahl (2005) demonstrates many ordinary high-mass BHXRBs (that one would expect to ?nd in these environments) have a mass transfer rate that is substantially super-Eddington, providing an adequate reservoir of fuel for ULXs. Not least, it would agree with observations of accreting sources in our own Galaxy that show many - most notably GRS 1915+105 do experience episodes of radiating at a super-Eddington level (cf.. McClintock & Remillard 2005).

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