Abstract
Quasars are associated with and powered by the accretion of material onto massive black holes; the detection of highly luminous quasars with redshifts greater than z = 6 suggests that black holes of up to ten billion solar masses already existed 13 billion years ago1. Two possible present-day ‘dormant’ descendants of this population of ‘active’ black holes have been found2 in the galaxies NGC 3842 and NGC 4889 at the centres of the Leo and Coma galaxy clusters, which together form the central region of the Great Wall3—the largest local structure of galaxies. The most luminous quasars, however, are not confined to such high-density regions of the early Universe4,5; yet dormant black holes of this high mass have not yet been found outside of modern-day rich clusters. Here we report observations of the stellar velocity distribution in the galaxy NGC 1600—a relatively isolated elliptical galaxy near the centre of a galaxy group at a distance of 64 megaparsecs from Earth. We use orbit superposition models to determine that the black hole at the centre of NGC 1600 has a mass of 17 billion solar masses. The spatial distribution of stars near the centre of NGC 1600 is rather diffuse. We find that the region of depleted stellar density in the cores of massive elliptical galaxies extends over the same radius as the gravitational sphere of influence of the central black holes, and interpret this as the dynamical imprint of the black holes.
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References
Wu, X.-B. et al. An ultraluminous quasar with a twelve-billion-solar-mass black hole at redshift 6.30. Nature 518, 512−515 (2015)
McConnell, N. J. et al. Two ten-billion-solar-mass black holes at the centres of giant elliptical galaxies. Nature 480, 215−218 (2011)
Geller, M. J. & Huchra, J. P. Mapping the universe. Science 246, 897–903 (1989)
Trainor, R. F. & Steidel, C. C. The halo masses and galaxy environments of hyperluminous QSOs at z 2.7 in the Keck baryonic structure survey. Astrophys. J. 752, 39 (2012)
Fanidakis, N., Macciò, A. V., Baugh, C. M., Lacey, C. G. & Frenk, C. S. The most luminous quasars do not live in the most massive dark matter haloes at any redshift. Mon. Not. R. Astron. Soc. 436, 315−326 (2013)
Ma, C.-P. et al. The MASSIVE survey. I. A volume-limited integral-field spectroscopic study of the most massive early-type galaxies within 108 Mpc. Astrophys. J. 795, 158 (2014)
Peletier, R. F., Davies, R. L., Illingworth, G. D., Davis, L. E. & Cawson, M. CCD surface photometry of galaxies with dynamical data. II—UBR photometry of 39 elliptical galaxies. Astron. J. 100, 1091–1142 (1990)
Bender, R., Saglia, R. P. & Gerhard, O. E. Line-of-sight velocity distributions of elliptical galaxies. Mon. Not. R. Astron. Soc. 269, 785–813 (1994)
Thomas, J. et al. Mapping stationary axisymmetric phase-space distribution functions by orbit libraries. Mon. Not. R. Astron. Soc. 353, 391–404 (2004)
McConnell, N. J. & Ma, C.-P. Revisiting the scaling relations of black hole masses and host galaxy properties. Astrophys. J. 764, 184 (2013)
Kormendy, J. & Ho, L. C. Coevolution (or not) of supermassive black holes and host galaxies. Ann. Rev. Astron. Astrophys. 51, 511−653 (2013)
Saglia, R. P. et al. The SINFONI black hole survey: the black hole fundamental plane revisited and the paths of (co)evolution of supermassive black holes and bulges. Astrophys. J. 818, 47 (2016)
Lauer, T. R. et al. The centers of early-type galaxies with Hubble Space Telescope. VI. Bimodal central surface brightness profiles. Astrophys. J. 664, 226–256 (2007)
Begelman, M. C., Blandford, R. D. & Rees, M. J. Massive black hole binaries in active galactic nuclei. Nature 287, 307–309 (1980)
Rusli, S. P. et al. Depleted galaxy cores and dynamical black hole masses. Astron. J. 146, 160 (2013)
Faber, S. M. et al. The centers of early-type galaxies with HST. IV. Central parameter relations. Astron. J. 114, 1771−1796 (1997)
Kormendy, J. & Bender, R. Correlations between supermassive black holes, velocity dispersions, and mass deficits in elliptical galaxies with cores. Astrophys. J. 691, L142−L146 (2009)
Thomas, J., Saglia, R. P., Bender, R., Erwin, P. & Fabricius, M. The dynamical Fingerprint of core scouring in massive elliptical galaxies. Astrophys. J. 782, 39 (2014)
Kormendy, J. & Bender, R. The L σ8 correlation for elliptical galaxies with cores: relation with black hole mass. Astrophys. J. 769, L5 (2013)
Boylan-Kolchin, M., Ma, C.-P. & Quataert, E. Red mergers and the assembly of massive elliptical galaxies: the fundamental plane and its projections. Mon. Not. R. Astron. Soc. 369, 1081–1089 (2006)
Gebhardt, K. et al. The black hole mass in M87 from Gemini/NIFS adaptive optics observations. Astrophys. J. 729, 119 (2011)
Walsh, J. L., Barth, A. J., Ho, L. C. & Sarzi, M. The M87 black hole mass from gas-dynamical models of space telescope imaging spectrograph observations. Astrophys. J. 770, 86 (2013)
Doeleman, S. S. et al. Jet-launching structure resolved near the supermassive black hole in M87. Science 338, 355−358 (2012)
Smith, R. M., Martínez, V. J., Fernández-Soto, A., Ballesteros, F. J. & Ortiz-Gil, A. NGC 1600: cluster or field elliptical? Astrophys. J. 679, 420−427 (2008)
Crook, A. C. et al. Groups of galaxies in the two micron all sky redshift survey. Astrophys. J. 655, 790–813 (2007)
Sivakoff, G. R., Sarazin, C. L. & Carlin, J. L. Chandra observations of diffuse gas and luminous X-ray sources around the X-ray-bright elliptical galaxy NGC 1600. Astrophys. J. 617, 262–280 (2004)
Rines, K., Geller, M. J., Kurtz, M. J. & Diaferio, A. CAIRNS: the cluster and infall region nearby survey. I. Redshifts and mass profiles. Astron. J. 126, 2152–2170 (2003)
Kubo, J. M. et al. The mass of the Coma cluster from weak lensing in the Sloan Digital Sky Survey. Astrophys. J. 671, 1466−1470 (2007)
Ikebe, Y., Reiprich, T. H., Böhringer, H., Tanaka, Y. & Kitayama, T. A new measurement of the X-ray temperature function of clusters of galaxies. Astron. Astrophys. 383, 773–790 (2002)
Graham, A. W., Erwin, P., Trujillo, I. & Asensio Ramos, A. A new empirical model for the structural analysis of early-type galaxies, and a critical review of the Nuker model. Astron. J. 125, 2951–2963 (2003)
Barth, A. J., Ho, L. C. & Sargent, W. L. W. A study of the direct fitting method for measurement of galaxy velocity dispersions. Astron. J. 124, 2607–2614 (2002)
McConnell, N. J. et al. Dynamical measurements of black hole masses in four brightest cluster galaxies at 100 Mpc. Astrophys. J. 756, 179 (2012)
Cappellari, M. & Copin, Y. Adaptive spatial binning of integral-field spectroscopic data using Voronoi tessellations. Mon. Not. R. Astron. Soc. 342, 345–354 (2003)
Hill, G. J., MacQueen, P. J., Palunas, P., Barnes, S. I. & Shetrone, M. D. Present and future instrumentation for the Hobby-Eberly Telescope. Proc. SPIE 7014, 701406 (2008)
Adams, J. J. et al. The HETDEX pilot survey. I. Survey design, performance, and catalog of emission-line galaxies. Astrophys. J. (Suppl.) 192, 5 (2011)
Sánchez-Blázquez, P. et al. Medium-resolution Isaac Newton Telescope library of empirical spectra. Mon. Not. R. Astron. Soc. 371, 703–718 (2006)
Cappellari, M. & Emsellem, E. Parametric recovery of line-of-sight velocity distributions from absorption-line spectra of galaxies via penalized likelihood. Pub. Astron. Soc. Pacific 116, 138−147 (2004)
Bender, R. & Moellenhoff, C. Morphological analysis of massive early-type galaxies in the Virgo cluster. Astron. Astrophys. 177, 71–83 (1987)
Magorrian, J. Kinematical signatures of hidden stellar discs. Mon. Not. R. Astron. Soc. 302, 530–536 (1999)
Thomas, J. et al. Regularized orbit models unveiling the stellar structure and dark matter halo of the Coma elliptical NGC 4807. Mon. Not. R. Astron. Soc. 360, 1355–1372 (2005)
Schwarzschild, M. A numerical model for a triaxial stellar system in dynamical equilibrium. Astrophys. J. 232, 236–247 (1979)
Richstone, D. O. & Tremaine, S. Maximum-entropy models of galaxies. Astrophys. J. 327, 82–88 (1988)
McConnell, N. J. et al. The black hole mass in the brightest cluster galaxy NGC 6086. Astrophys. J. 728, 100 (2011)
Gebhardt, K. & Thomas, J. The black hole mass, stellar mass-to-light ratio, and dark halo in M87. Astrophys. J. 700, 1690−1701 (2009)
van der Marel, R. P. The velocity dispersion anisotropy and mass-to-light ratio of elliptical galaxies. Mon. Not. R. Astron. Soc. 253, 710–726 (1991)
Magorrian, J. et al. The demography of massive dark objects in galaxy centers. Astron. J. 115, 2285–2305 (1998)
Matthias, M. & Gerhard, O. Dynamics of the boxy elliptical galaxy NGC 1600. Mon. Not. R. Astron. Soc. 310, 879–891 (1999)
Pu, S. B. et al. Radially extended kinematics and stellar populations of the massive ellipticals NGC 1600, NGC 4125, and NGC 7619. Constraints on the outer dark halo density profile. Astron. Astrophys. 516, A4 (2010)
Dullo, B. T. & Graham, A. W. Depleted cores, multicomponent fits, and structural parameter relations for luminous early-type galaxies. Mon. Not. R. Astron. Soc. 444, 2700−2722 (2014)
Merritt, D. Mass deficits, stalling radii, and the merger histories of elliptical galaxies. Astrophys. J. 648, 976–986 (2006)
Treu, T. et al. The initial mass function of early-type galaxies. Astrophys. J. 709, 1195−1202 (2010)
Conroy, C. & van Dokkum, P. G. The stellar initial mass function in early-type galaxies from absorption line spectroscopy. II. Results. Astrophys. J. 760, 71 (2012)
Cappellari, M. et al. The ATLAS3D project—XX. Mass-size and mass-σ distributions of early-type galaxies: bulge fraction drives kinematics, mass-to-light ratio, molecular gas fraction and stellar initial mass function. Mon. Not. R. Astron. Soc. 432, 1862−1893 (2013)
Thomas, J. et al. Dynamical masses of early-type galaxies: a comparison to lensing results and implications for the stellar initial mass function and the distribution of dark matter. Mon. Not. R. Astron. Soc. 415, 545−562 (2011)
La Barbera, F. et al. SPIDER VIII—constraints on the stellar initial mass function of early-type galaxies from a variety of spectral features. Mon. Not. R. Astron. Soc. 433, 3017−3047 (2013)
Smith, R. J., Lucey, J. R. & Conroy, C. The SINFONI nearby elliptical lens locator survey: discovery of two new low-redshift strong lenses and implications for the initial mass function in giant early-type galaxies. Mon. Not. R. Astron. Soc. 449, 3441−3457 (2015)
Martn-Navarro, I., Barbera, F. L., Vazdekis, A., Falcón-Barroso, J. & Ferreras, I. Radial variations in the stellar initial mass function of early-type galaxies. Mon. Not. R. Astron. Soc. 447, 1033−1048 (2015)
Milosavljević, M. & Merritt, D. Formation of galactic nuclei. Astrophys. J. 563, 34–62 (2001)
Trujillo, I., Erwin, P., Asensio Ramos, A. & Graham, A. W. Evidence for a new elliptical-galaxy paradigm: Sérsic and core galaxies. Astron. J. 127, 1917–1942 (2004)
Lauer, T. R. et al. The centers of early-type galaxies with HST. I. An observational survey. Astron. J. 110, 2622–2654 (1995)
Carollo, C. M., Franx, M., Illingworth, G. D. & Forbes, D. A. Ellipticals with kinematically distinct cores: (V–I) color images with WPFC2. Astrophys. J. 481, 710–734 (1997)
Gerhard, O. E. Line-of-sight velocity profiles in spherical galaxies: breaking the degeneracy between anisotropy and mass. Mon. Not. R. Astron. Soc. 265, 213–230 (1993)
van der Marel, R. P. & Franx, M. A new method for the identification of non-Gaussian line profiles in elliptical galaxies. Astrophys. J. 407, 525–539 (1993)
Quinlan, G. D. & Hernquist, L. The dynamical evolution of massive black hole binaries–II. Self-consistent N-body integrations. New Astron. 2, 533–554 (1997)
Acknowledgements
C.-P.M., J.E.G. and R.J. are supported by the National Science Foundation (NSF). J.E.G. is supported by the Miller Institute for Basic Research in Science, University of California, Berkeley. N.J.M. is supported by the Beatrice Watson Parrent Fellowship and Plaskett Fellowship. The spectroscopic data presented here were obtained from the Gemini Observatory and the McDonald Observatory. Gemini is operated by the Association of Universities for Research in Astronomy, Inc., under a cooperative agreement with the NSF on behalf of the Gemini partnership. The McDonald Observatory is operated by the University of Texas at Austin. The photometric data presented here are based partly on observations made with the NASA/ESA Hubble Space Telescope, and obtained from the Hubble Legacy Archive, which is a collaboration between the Space Telescope Science Institute (STScI/NASA), the Space Telescope European Coordinating Facility (ST-ECF/ESA) and the Canadian Astronomy Data Centre (CADC/NRC/CSA).
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J.T. developed and carried out the stellar orbit modelling. J.T. and C.-P.M. wrote the manuscript. C.-P.M. led the Gemini observation proposal. J.E.G. performed the stellar population analysis. N.J.M. and R.J. reduced the spectroscopic data. J.P.B. provided photometric analysis. All authors contributed to the MASSIVE Survey, the kinematic extractions, the interpretive analysis of the observations and the writing of the paper.
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Extended data figures and tables
Extended Data Figure 1 The MBH/σ correlation.
The black-hole masses, MBH, and host-galaxy velocity dispersions, σe, of the 21 core galaxies (red dots, with 1σ error bars) shown in Figs 3 and 4. The dashed, dotted and solid lines show recent fits (from refs 10, 11 and 12, respectively) to the MBH–σ correlation for all early-type galaxies (including both cored and coreless galaxies) and classical bulges with dynamically measured MBH. The black hole in NGC 1600 is ten times more massive than would be expected given the galaxy’s velocity dispersion (σe = 293 km s−1).
Extended Data Figure 2 Surface brightness profile of NGC 1600.
a, The circularized surface brightness distribution of NGC 1600 (filled circles) and the best-fit core-Sérsic model (red line; the best-fit parameters of the core-Sérsic function are quoted). The blue dotted line indicates the inward extrapolation of the outer Sérsic component. From the integrated difference between the blue and the red curves, we derive a ‘light deficit’ of Ldef = 9.47 × 109L⊙. b, The difference between the data points in panel a and the core-Sérsic fit. Surface brightnesses are given in mag arcsec−2 in the R-band.
Extended Data Figure 3 Best-fit MBH values for NGC 1600 and confidence intervals.
The relative likelihood of different MBH values, marginalized over M⋆/L, rDM and vDM (shaded area; the likelihood is arbitrarily scaled). The best-fit values and confidence intervals are derived from the cumulative likelihood distribution43 and indicated by the vertical lines. The red line shows , where χ2(MBH) is the minimum of all models with the same MBH, but different M⋆/L, rDM and vDM; is the minimum of χ2(MBH) over MBH.
Extended Data Figure 4 Stellar velocity data and best-fit dynamical model.
These data are shown for NGC 1600 (filled grey and orange circles, with 1σ error bars), together with the best-fit model (smoothed over 0.05 dex in log radius; solid red curves). Observed LOSVDs of galaxies are approximately Gaussian and are commonly parameterized by a Gauss–Hermite series expansion62,63. The mean stellar velocity v (in a) and velocity dispersion σ (in b) correspond to the centre and the width, respectively, of the best Gaussian approximation. Higher-order Hermite coefficients hn (in c–f) quantify deviations from a pure Gaussian LOSVD. Most data points at r < 4 arcsec came from our GMOS IFS observations (orange dots). Data at larger radii came from our Mitchell IFS observations (grey dots).
Extended Data Figure 5 The enclosed mass of NGC 1600.
a, The enclosed stellar mass (M⋆, blue), dark-halo mass (MDM, red), black-hole mass (MBH, grey) and combined total mass (black) obtained in our model from the smallest resolved radius (point-spread-function, PSF, size) out to 20 kpc (Mitchell IFU size). b, An illustration of the excessive M⋆/L gradient (dotted pale blue curve) that would be required for a hypothetical population of unresolved central dwarf stars to explain 10% of NGC 1600’s measured MBH. The stellar mass-to-light ratio would have to increase by about a factor of ten (dotted pale blue curve) over our best-fit constant value (dashed blue curve). Observations of other galaxies suggest that extreme populations of dwarf stars can increase M⋆/L by a factor of up to three.
Extended Data Figure 6 The anisotropy of stellar orbits in core galaxies.
In NGC 1600 (red line) and similar galaxies with cores12,18 (grey lines), the stellar velocity distribution is anisotropic. The anisotropy parameter, , is positive when most of the stars move along radially stretched orbits, and negative when the stellar orbits are predominantly tangential. Inside the diffuse, low-surface-brightness core region (r ≤ rb), tangential motions dominate. The shaded area indicates the range of anisotropies found in numerical N-body simulations of the core scouring mechanism58,64.
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Thomas, J., Ma, CP., McConnell, N. et al. A 17-billion-solar-mass black hole in a group galaxy with a diffuse core. Nature 532, 340–342 (2016). https://doi.org/10.1038/nature17197
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DOI: https://doi.org/10.1038/nature17197
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