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Reflection from the strong gravity regime in a lensed quasar at redshift z = 0.658

Nature volume 507, pages 207–209 (2014)Cite this article

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Abstract

The co-evolution of a supermassive black hole with its host galaxy1 through cosmic time is encoded in its spin2,3,4. At z > 2, supermassive black holes are thought to grow mostly by merger-driven accretion leading to high spin. It is not known, however, whether below z ≈ 1 these black holes continue to grow by coherent accretion or in a chaotic manner5, though clear differences are predicted3,4 in their spin evolution. An established method6 of measuring the spin of black holes is through the study of relativistic reflection features7 from the inner accretion disk. Owing to their greater distances from Earth, there has hitherto been no significant detection of relativistic reflection features in a moderate-redshift quasar. Here we report an analysis of archival X-ray data together with a deep observation of a gravitationally lensed quasar at z = 0.658. The emission originates within three or fewer gravitational radii from the black hole, implying a spin parameter (a measure of how fast the black hole is rotating) of a = at the 3σ confidence level and a > 0.66 at the 5σ level. The high spin found here is indicative of growth by coherent accretion for this black hole, and suggests that black-hole growth at 0.5 ≤ z ≤ 1 occurs principally by coherent rather than chaotic accretion episodes.

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Figure 1: Chandra image of RX J1131−1231.
Figure 2: Broad Fe line, soft and hard excess in RX J1131−1231.
Figure 3: Goodness of fit versus the spin parameter of the supermassive black hole in RX J1131−1231.

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Acknowledgements

R.C.R. thanks the Michigan Society of Fellows and NASA for support through the Einstein Fellowship Program, grant number PF1-120087. We thank the ESA XMM-Newton Project Scientist N. Schartel and the XMM-Newton planning team for carrying out the DDT observation. The scientific results reported in this article are based on data obtained from the Chandra Data Archive.

Author information

Authors and Affiliations

  1. Department of Astronomy, University of Michigan, Ann Arbor, 48109, Michigan, USA

    R. C. Reis, M. T. Reynolds & J. M. Miller

  2. Cahill Center for Astronomy and Astrophysics, California Institute of Technology, Pasadena, 91125, California, USA

    D. J. Walton

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  1. R. C. Reis
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Contributions

R.C.R. performed the data reduction and analysis of all the Chandra data reported here. The XMM-Newton data was reduced by both R.C.R and M.T.R. The pile-up study was carried out by R.C.R., J.M.M. and M.T.R. The text was composed, and the paper synthesised, by R.C.R., with help from D.J.W. and M.T.R. The smoothed subpixel images were made by R.C.R. and M.T.R. All authors discussed the results and commented on the manuscript.

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Correspondence to R. C. Reis.

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Extended data figures and tables

Extended Data Figure 1 Phenomenological models for all 27 Chandra observations of image B.

a, Chandra data has been fitted with a DISKBB component to mimic the soft excess as well as a RELLINE line profile to account for the residuals in the 2–4-keV range and a power law for the continuum. The normalization of the various components, as well as the power-law indices, is allowed to vary between epochs. However, the intrinsic column density, the ionization state (related to the centroid of the line), the emissivity profile and the inclination of the disk are assumed to be unchanging between the various epochs. b, Data-to-model ratio plot, made in a manner similar to that for Extended Data Fig. 2, for all 27 epochs. The solid magenta line is the baseline theoretical best-fitting model-to-power-law ratio expected from the self-consistent REFLIONX model found for epoch 23. The data have been rebinned for visual clarity.

Extended Data Figure 2 Co-added Chandra spectra of the various Chandra images during all observations.

a, The spectra for images B (black) and C (magenta) are shown fitted with a simple power law, and the residuals to this model are shown in units of 1σ deviations in the middle panel. The data in the bottom panel have been rebinned for display purposes. b, Co-added spectra of periods 1 and 3 (black) and period 2 (magenta) of image D shown as residuals to a simple power law together with Gaussians similar to those shown in ref. 16. The residuals to this model are shown in units of 1σ deviations. The bottom panel shows similar residuals for the corresponding periods 1+3 of image A. The data have been rebinned for display purposes.

Extended Data Figure 3 Co-added spectrum of all Chandra epochs fitted with the baseline-reflection model.

a, The spectrum was fitted with a physically motivated, self consistent model for both the soft excess and the broad Fe line. The residuals to the model are shown in the middle panel. The REFLIONX, power-law and narrow Gaussian components are shown in magenta, green and blue, respectively, with the total model shown in cyan. The blue vertical line is the narrow Gaussian component. The bottom panel shows the residuals without the narrow Gaussian component. b, Extrapolated model showing a reflection-dominated continuum. The data were rebinned for display purposes.

Extended Data Figure 4 Co-added spectra of all Chandra images fitted with the baseline-simple model.

a, The unfolded spectrum is shown for the best-fitting simple model with the relativistic line, soft disk component and power law shown in magenta, blue and green, respectively. The residuals to this model are shown in units of 1σ deviations in the middle panel. The bottom panel shows the residuals after rebinning the data for display purposes. b, The top panel shows the residuals to a simple power law and the bottom panel shows similar residuals after the addition of a DISKBB component.

Extended Data Figure 5 Goodness of fit versus spin parameter.

a, Range of spin values found by fitting image B alone. b, Similar value for the spin, albeit at a lesser statistical significance, is found when using image C alone. By co-adding the spectra we are probing the time-averaged behaviour of the reflection spectrum. Fits were made with the spin parameter varying from 0.495 to 0.995 in steps of 0.01. The blue contour was made using the relativistic line model RELLINE assuming a broken emissivity profile and a further narrow Gaussian line at 6.4 keV. The black contour assumes a broken emissivity without the extra narrow Gaussian line. The magenta contour is for the self-consistent REFLIONX model together with the RELCONV blurring kernel and a Gaussian line at 6.4 keV (see text for details). For image B, we have also included the green contour, found for the time-resolved analyses described in section 3.2.1 of the Supplementary Information. c, Co-added spectrum of all Chandra (magenta contour), XMM-Newton (green contour) and simultaneous data (black contour). These contours are made with the baseline-reflection model. The dotted lines show the 99.99%, 99.73% (3σ) and 90% confidence limits.

Extended Data Figure 6 XMM-Newton EPIC-PN spectrum of RX J1131−1231.

a, The unfolded spectrum is shown with a broken power law, together with a soft excess and narrow Gaussian in magenta. The second panel from the top shows the residuals upon removal of the soft component, the narrow line and the break in the power law. The next panel down shows the fit with the addition of a break in the power law and the bottom panel shows the best phenomenological fit to the XMM-Newton data. b, XMM-Newton data, now fitted with the baseline-reflection model. The reflection component is again shown in magenta, with the total, power-law and narrow lines shown in black, green and blue, respectively. The bottom panel shows the ratio to this model. The data have been rebinned for display purposes.

Extended Data Figure 7 Detected counts per frame as a function of observation epoch.

The counts have been corrected with a PSF to account for the size of the extraction region. As such, the counts presented are approximately a factor of 1.69, 1.71, 1.69 and 1.21 higher that that observed for images A, B, C and D, respectively. We show with solid and dotted horizontal lines the expected 10% pile-up fraction assuming grade migration parameters of α = 1 and 0.5, respectively. The highlighted epoch corresponds to that used in the in-depth study of possible spectral distortions caused by pile-up/cross-contamination. We use this epoch to assess the implication of high count rate on our results as it presents the greatest chance of cross-contamination due to the peak brightness of image A. The work highlighted in the Methods shows that the features observed in this epoch are consistent with those observed in all (fainter) observations.

Extended Data Figure 8 Testing for pile-up in a bright Chandra observation.

a, Chandra spectra of images B, C and D from the observation made on 28 November 2009. This observation is highlighted in Extended Data Fig. 1 and is representative of the brightest Chandra epochs used in this work. It is also the observation in which image A is at its brightest and therefore presents the largest chance of cross-contamination because sources are only about 1′′ apart. The spectra were fitted phenomenologically with a combination of power-law, DISKBB and RELLINE line profiles to describe the continuum, soft excess and Fe emission features, respectively. The ratios to the model are shown both with (centre) and without (bottom) the disk component representing the soft excess. The spectra of images B, C and D are shown in black, magenta and green, respectively. The power-law, DISKBB and RELLINE components for image B are shown in cyan, magenta and blue, respectively, with the total model shown as solid lines for the three images. b, Data-to-model ratio obtained after removing the RELLINE and DISKBB components (top) and after refitting with a single power law (bottom). The ratio for images B, C and D are shown in black, magenta and green, respectively, and have been rebinned for display purposes. Despite the different flux levels of these three images, it is clear that the residuals to a simple power law remains similar, suggesting that pile-up is not significant in the brightest observations of image B.

Extended Data Table 1 Model summary for the co-added spectra of images B and C
Full size table
Extended Data Table 2 The time-averaged Chandra spectrum of RX J1131−1231 and the XMM-Newton EPIC-PN data using the baseline-reflection model
Full size table

Supplementary information

Supplementary Information

This file contains Supplementary Text and additional references. (PDF 238 kb)

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Reis, R., Reynolds, M., Miller, J. et al. Reflection from the strong gravity regime in a lensed quasar at redshift z = 0.658. Nature 507, 207–209 (2014). https://doi.org/10.1038/nature13031

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