Gas cloud black_hole

Gas cloud black_hole

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  LETTER doi:10.1038/nature10652 A gas cloud on its way towards the supermassive black hole at the Galactic Centre S. Gillessen1, R. Genzel1,2, T. K. Fritz1, E. Quataert3, C. Alig4, A. Burkert4,1, J. Cuadra5, F. Eisenhauer1, O. Pfuhl1, K. Dodds-Eden1, C. F. Gammie6 & T. Ott1 Measurements of stellar orbits1–3 provide compelling evidence4,5 requirement of complete photo-ionization sets a lower limit to fV of that the compact radio source Sagittarius A* at the Galactic 1021 6 0.5 for the extreme case that the cloud is a thin sheet. Centre is a black hole four million times the mass of the Sun. The combined astrometric and radial velocity data tightly constrain With the exception of modest X-ray and infrared flares6,7, Sgr A* the cloud’s motion. It is on a highly eccentric (e 5 0.94) Keplerian orbit is surprisingly faint, suggesting that the accretion rate and radiation bound to the black hole (Fig. 1, Table 1 and Supplementary efficiency near the event horizon are currently very low3,8. Here we Information section 2). The pericentre radius is a mere 36 light hours report the presence of a dense gas cloud approximately three times (3,100 Schwarzschild radii, RS), which the cloud will reach in summer the mass of Earth that is falling into the accretion zone of Sgr A*. 2013. Only the two stars S2 (rperi 5 17 light hours) and S14 (rperi 5 11 Our observations tightly constrain the cloud’s orbit to be highly light hours) have come closer to the black hole2,3 since our monitoring eccentric, with an innermost radius of approach of only 3,100 started in 1992. Although the cloud’s gas density may be only modestly times the event horizon that will be reached in 2013. Over the past greater than that of other ionized gas clouds in the central parsec— three years the cloud has begun to disrupt, probably mainly through ne < (0.122) 3 105 cm23; refs 12 and 14—it has a specific angular tidal shearing arising from the black hole’s gravitational force. The momentum about 50 times smaller12. cloud’s dynamic evolution and radiation in the next few years will For the nominal properties of the X-ray detected accretion flow onto probe the properties of the accretion flow and the feeding processes the black hole15,16 the cloud should stay close to Keplerian motion all of the supermassive black hole. The kilo-electronvolt X-ray emis- the way to the pericentre (Supplementary Information sections 3 sion of Sgr A* may brighten significantly when the cloud reaches and 4). Its density is currently about 300fV21/2 times greater than that pericentre. There may also be a giant radiation flare several years of the surrounding hot gas in the accretion flow15: extrapolating to the from now if the cloud breaks up and its fragments feed gas into the pericentre, its density contrast will then still be about 60fV–1/2. central accretion zone. Similarly, the cloud’s ram pressure by far exceeds that of the hot gas As part of our NACO9 and SINFONI10,11 Very Large Telescope throughout the orbit. In contrast, the thermal pressure ratio will (VLT) observation programmes studying the stellar orbits around the quickly decrease from unity at apocentre and the hot gas is expected Galactic Centre supermassive black hole, Sgr A*, we have discovered an to drive a shock slowly compressing the cloud. Whereas the external object moving at about 1,700 km s21 along a trajectory almost straight pressure compresses the cloud from all directions, the black hole’s tidal towards Sgr A* (Fig. 1). The object has a remarkably low temperature forces shear the cloud along the direction of its motion, because the (about 550 K; Supplementary Fig. 2) and a luminosity about five times Roche density for self-gravitational stabilization exceeds the cloud that of the Sun, unlike any star we have so far seen near Sgr A*. It is also density by nine orders of magnitude3. In addition, the ram pressure seen in the spectroscopic data as a redshifted emission component in compresses the cloud parallel to its motion. The interaction between the Brc and Brd hydrogen lines, and the 2.058 mm He I lines, with the the fast-moving cloud and the surrounding hot gas should also lead to same proper motion as the L9-band object. Its three-dimensional shredding and disruption, owing to the Kelvin–Helmholtz and velocity increased from 1,200 km s21 in 2004 to 2,350 km s21 in Rayleigh–Taylor instabilities17–20. Rayleigh–Taylor instabilities at the 2011. The Brc emission is elongated along its direction of motion with leading edge should in fact break up the cloud within the next few years a spatially resolved velocity gradient (Fig. 2). Together, these findings if it started as a spheroidal, thick blob (Supplementary Information show that the object is a dusty, ionized gas cloud. section 3). A thin, dense sheet would by now already have fragmented The extinction of the ionized gas is typical for the central parsec and disintegrated, suggesting that fV is of the order of unity. (Supplementary Information section 1) and its intrinsic Brc luminosity We are witnessing the cloud’s disruption happening in our spectro- is 1.66 (60.25) 3 1023 times that of the Sun. For case B recombination scopic data (Fig. 2). The intrinsic velocity width more than tripled over {1=2 the implied electron density is nc ~2:6|105 fV R{3=2 Te cm23, c 0:54 the last eight years, and we see between 2008 and 2011 a growing for an effective cloud radius of Rc < 15 milli-arcseconds (mas), volume velocity gradient along the orbital direction. Test particle calculations filling factor fV (#1) and an assumed electron temperature Te in units of implementing only the black hole’s force show that an initially spher- 104 K, a value typical for the temperatures measured in the central ical gas cloud placed on the orbit (Table 1) is stretched along the orbit 1=2 parsec12. The cloud mass is Mc ~1:7|1028 fV R3=2 Te g or about c 0:54 and compressed perpendicular to it, with increasing velocity widths 1/2 3fV Earth masses. It may plausibly be photo-ionized by the ultraviolet and velocity gradients reasonably matching our observations (Fig. 3 radiation field from nearby massive hot stars, as we infer from a com- and Supplementary Fig. 4). There is also a tail of gas with lower surface parison of the recombination rate with the number of impinging Lyman brightness on approximately the same orbit as the cloud, which cannot continuum photons3,13. This conclusion is supported by the He I/Brc be due to tidal disruption alone. It may be stripped gas, or lower- line flux ratio of approximately 0.7, which is similar to the values found density, lower-filling-factor gas on the same orbit. The latter explana- in the photo-ionized gas in the central parsec (0.35–0.7). If so, the tion is more plausible given that the integrated Brc and L9-band 1 Max-Planck-Institut fur extraterrestrische Physik (MPE), Giessenbachstrasse 1, D-85748 Garching, Germany. 2Department of Physics, Le Conte Hall, University of California, Berkeley, California 94720, ¨ USA. 3Department of Astronomy, University of California, Berkeley, California 94720, USA. 4Universitatssternwarte der Ludwig-Maximilians-Universitat, Scheinerstrasse 1, D-81679 Munchen, Germany. ¨ ¨ ¨ 5 Departamento de Astronomıa y Astrofısica, Pontificia Universidad Catolica de Chile, Vicuna Mackenna 4860, 7820436 Macul, Santiago, Chile. 6Center for Theoretical Astrophysics, Astronomy and Physics ´ ´ ´ ˜ Departments, University of Illinois at Urbana-Champaign, 1002 West Green Street, Urbana, Illinois 61801, USA. 5 J A N U A RY 2 0 1 2 | VO L 4 8 1 | N AT U R E | 5 1 ©2012 Macmillan Publishers Limited. All rights reserved
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  RESEARCH LETTER a b c N E S2 1′′ April 2011 Ks July 2011 L′ 40 mpc d 0.2 e 2,000 0.1 S2 1,000 Declination (arcsec) VLSR (km s–1) 0 0 0.1 1,000 0.2 2,000 0.3 0.2 0.1 0 2005 2010 2015 2020 Right ascension (arcsec) t (yr) Figure 1 | Infalling dust/gas cloud in the Galactic Centre. a, b, NACO9 on a 2011 Ks-band image). The cloud is also detected in deep spectroscopy with adaptive optics VLT images showing that the cloud (dashed circle) is detected the adaptive-optics-assisted integral field unit SINFONI10,11 in the H I n 5 7–4 in the L9-band (3.76 mm, deconvolved and smoothed with a 2-pixel Gaussian Brc recombination line at 2.1661 mm and in He I at 2.058 mm, with a radial kernel) but not in the Ks-band (2.16 mm, undeconvolved), indicating that it is velocity of 1,250 km s21 (in 2008) and 1,650 km s21 (in 2011). d, e, The not a star but a dusty cloud with a temperature of around 550 K (Supplementary combination of the astrometric data in L9 and Brc and the radial velocity (VLSR) Fig. 2). The cloud is also detected in the M-band (4.7 mm) but not seen in the data in Brc tightly constrains the orbit of the cloud (error bars are 1s H-band (1.65 mm). North is up, East is left. The white cross marks the position measurement errors). The cloud is on a highly eccentric, bound orbit (e 5 0.94), of Sgr A*. c, The proper motion derived from the L-band data is about with a pericentre radius and epoch of 36 light hours (3,100RS) and 2013.5 42 mas yr21, or 1,670 km s21 (in 2011), from the southeast towards the position (Table 1). The blue ellipse shows the orbit of the star S2 for comparison1–3. For of Sgr A* (red for epoch 2004.5, green for 2008.3 and blue for 2011.3, overlaid further details see the Supplementary Information. a b Figure 2 | The velocity shear in the gas cloud. The left column shows data from 2008.3, the right from 2011.3. Panels a and b show integrated Brc maps of the cloud, in comparison to the point spread function from stellar images shown above. The inferred intrinsic East–West half-width at half-maximum Star source radii are Rc 5 21 6 5 mas in 2008 and 19 6 8 mas in 2011 (approximately along the direction of orbital motion), after removal of the instrumental broadening estimated from the stellar images above. A similar 0.1′′ spatial extent is found from the spatial separation between the red- and blue- shifted emission of the cloud (Rc 5 23 6 5 mas). The minor-axis radius of the cloud is only marginally resolved or unresolved (radius less than 12 mas). We Brγ adopt Rc 5 15 mas as the ‘effective’ circular radius, by combining the results in cloud the two directions. Panels c and d are position-velocity maps, obtained with SINFONI on the VLT, of the cloud’s Brc emission. The slit is oriented 2008 2011 approximately along the long axis of the cloud and the projected orbital direction and has a width of 62 mas for the bright ‘head’ of the emission. For the c d lower-surface-brightness ‘tail’ of emission (in the enclosed white dotted 500 500 regions) we smoothed the data with 50 mas and 138 km s21 and used a slit width of 0.1199. The gas in the tail is spread over around 200 mas downstream of the cloud. The trailing emission appears to be connected by a smooth velocity 1,000 1,000 gradient (of about 2 km s21 mas21), and the velocity field in the tail VLSR (km s–1) approximately follows the best-fit orbit of the head (cyan curves; see also Table 1). An increasing velocity gradient has formed in the head between 2008 1,500 1,500 (2.1 km s21 mas21) and 2011 (4.6 km s21 mas21). As a result of this velocity gradient, the intrinsic integrated full-width at half-maximum (FWHM) velocity width of the cloud increased from 89 (630) km s21 in 2003 and 117 (625) km s21 in 2004, to 210 (624) km s21 in 2008, and 350 (640) km s21 2,000 2,000 in 2011. 2008 2011 0.4 0.2 0 0.4 0.2 0 Offset from Sgr A* (arcsec) 5 2 | N AT U R E | VO L 4 8 1 | 5 J A N U A RY 2 0 1 2 ©2012 Macmillan Publishers Limited. All rights reserved
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  LETTER RESEARCH Table 1| Orbit parameters of the infalling cloud the emission into the un-observable soft X-ray and ultraviolet bands. Parameters of Keplerian orbit around Best-fitting value Together the evolution of the 2–8-keV and Brc luminosities, as well as the 4.31 3 106M[ black hole at R0 5 8.33 kpc the Brc velocity distribution, will strongly constrain the thermal states Semi-major axis, a 521 6 28 mas and interaction of the cloud and the ambient hot gas in the at present Eccentricity, e 0.9384 6 0.0066 unprobed regime of 103RS2104RS, when compared with test particle Inclination of ascending node, i 106.55 6 0.88 deg Position angle of ascending node, V 101.5 6 1.1 deg calculations and more detailed numerical simulations (Fig. 3 and Longitude of pericentre, v 109.59 6 0.78 deg Supplementary Fig. 4). Time of pericentre, tperi 2013.51 6 0.035 The radiated energy estimated above is less than 1% of the total Pericentre distance from black hole, rperi 4.0 6 0.3 3 1015cm 5 3,140RS kinetic energy of the cloud, about 1045.4 erg. As the tidally disrupted Orbital period, to 137 6 11 years filamentary cloud passes near pericentre some fraction of the gas may luminosities did not drop by more than 30% between 2004 and 2011, well collide with itself, dissipate and circularize22. This is probable and the integrated Brc flux of the tail is comparable to that of the cloud. because of the large velocity dispersion of the cloud, its size comparable The disruption and energy deposition processes in the next years to the impact parameter and because the Rayleigh–Taylor and Kelvin– until and after the pericentre passage are powerful probes of the phys- Helmholtz timescales are similar to the orbital timescale. Because the ical conditions in the accretion zone (Supplementary section 3). We mass of the cloud is larger than the mass of hot gas within the central expect that the interaction between hot gas and cloud will drive a strong 3,100RS or so (approximately 1027.3 g; ref. 15), it is plausible that then shock into the cloud. Given the densities of cloud and hot gas, the cloud the accretion near the event horizon will be temporarily dominated by as a whole should remain at low temperature until just before it reaches accretion of the cloud. This could in principle release up to around the pericentre. Near the pericentre the post-shock temperature of the 1048 erg over the next decade, although the radiative efficiency of the cloud may increase rapidly to Tpostshock, c < 6210 3 106 K, resulting in inflow at these accretion rates is of the order of 1–10% (refs 23 and 24). X-ray emission. We estimate the observable 228-keV luminosity to be Observations of the emission across the electromagnetic spectrum less than 1034 erg s21 there, somewhat larger than the current during this post-circularization phase will provide stringent con- ‘quiescent’ X-ray luminosity6,15,21 of Sgr A* (1033 erg s21). Rayleigh– straints on the physics of black-hole accretion with unusually good Taylor instabilities may by then have broken up the cloud into several knowledge of the mass available. fragments, in which case the emission may be variable throughout this What was the origin of the low-angular-momentum cloud? Its orbital period. Our predictions depend sensitively on the density and disrup- angular momentum vector is within 15u of the so-called ‘clockwise’ disk tion state of the cloud, as well as on the radial dependencies of the hot of young, massive O and Wolf–Rayet stars at radii of about 199 to 1099 gas properties, none of which we can fully quantify. The steeper the from Sgr A* (refs 3 and 25). Several of these stars have powerful winds. radial profiles are and the higher the value of fV, the more X-ray One star, IRS16SW, about 1.499 southeast of Sgr A*, is a massive Wolf– emission will occur. Shallower profiles and a low value of fV could shift Rayet contact binary26. Colliding winds in the stellar disk, and especially a e i m Vrad = 859 km s–1 Vrad = 1,704 km s–1 1,200 0.1 ± 0.1 mas km–1 s–1 2,000 150 150 FWHM = 118 km s–1 FWHM = 305 km s–1 t = 2000.0 t = 2000.0 t = 2012.5 1,000 0 100 100 50 50 800 2,000 600 4,000 t = 2012.5 b 0 f 0 j 1,400 n 2,000 150 Vrad = 1,037 km s–1 150 t = 2013.5 0.9 ± 0.1 mas km–1 s–1 t = 2004.5 FWHM = 124 km s–1 1,200 0 t = 2004.5 Radial velocity, Vrad km s–1) 100 100 Number of entries 50 50 1,000 2,000 800 4,000 t = 2013.5 c 0 g 0 k 1,600 o 2,000 150 Vrad = 1,295 km s–1 150 Vrad = –2,642 km s–1 2.4 ± 0.1 mas km–1 s–1 FWHM = 154 km s–1 FWHM = 960 km s–1 t = 2008.5 t = 2008.5 t = 2014.5 1,400 0 100 100 50 50 1,200 2,000 1,000 4,000 t = 2014.5 d 0 h 0 l 2,000 4.8 ± 0.1 mas km–1 s–1 p 2,000 Vrad = 1,640 km s–1 Vrad = –1,910 km s–1 5.0 ± 0.2 mas km–1 s–1 150 150 FWHM = 505 km s–1 t = 2011.5 t = 2016.5 FWHM = 289 km s–1 t = 2011.5 t = 2016.5 1,800 0 100 100 50 50 1,600 2,000 0 0 1,400 4,000 500 1,000 1,500 2,000 2,500 4,000 2,000 0 2,000 50 0 50 100 50 0 50 100 Vrad (km s–1) Position (shifted) (mas) Figure 3 | Test particle simulation of the orbital tidal disruption. An along the orbital direction, purely on the basis of the tidal disruption of the initially Gaussian cloud of initial FWHM diameter 25 mas and FWHM velocity cloud by the gravitational force of the supermassive black hole. This toy model width 120 km s21 is placed on the orbit in Table 1. a–h, As described in is a good description of the velocity (and spatial) data between 2004 and 2011, Supplementary Information section 4 (see also Supplementary Fig. 4) these thus allowing plausible forward projections until pericentre passage. Beyond panels show the evolution of the cloud integrated velocity width for eight that, the test particle approach will probably fail owing to the hydrodynamic epochs. The mean velocity and FWHM are given for those epochs at which the effects, which will then most probably dominate further evolution. The cloud distribution is unimodal (that is, not f). i–p, These panels show the evolution of cannot be described by a simple velocity gradient between 2012 and 2015, and the velocity change as a function of position (measured in milli-arcseconds) hence we omit the corresponding value in panels m, n and o. 5 J A N U A RY 2 0 1 2 | VO L 4 8 1 | N AT U R E | 5 3 ©2012 Macmillan Publishers Limited. All rights reserved
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  RESEARCH LETTER in binaries,may create low-angular-momentum gas that then falls 18. Chandrasekhar, S. Hydrodynamic and Hydromagnetic Stability 428–514 (Dover Publications, 1961). deep into the potential of the supermassive black hole27,28. 19. Murray, S. D., &. Lin, D. N. C. Energy dissipation in multiphase infalling clouds in galaxy halos. Astrophys. J. 615, 586–594 (2004). Received 25 August; accepted 17 October 2011. 20. Cooper, J. L., Bicknell, G. V., Sutherland, R. S. & Bland-Hawthorn, J. Starburst-driven Published online 14 December 2011. galactic winds: filament formation and emission processes. Astrophys. J. 703, 330–347 (2009). 1. Ghez, A. M. et al. Measuring distance and properties of the Milky Way’s central 21. Baganoff, F. K. et al. Chandra X-ray spectroscopic imaging of Sgr A* and the central supermassive black hole with stellar orbits. Astrophys. J. 689, 1044–1062 (2008). parsec of the Galaxy. Astrophys. J. 591, 891–915 (2003). 2. Gillessen, S. et al. 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Dynamics of ionized gas at the discussions on the cloud destruction process. J.C. acknowledges support from Galactic Center: Very Large Array observations of the three-dimensional velocity FONDAP, FONDECYT, Basal and VRI-PUC. A.B. acknowledges the support of the field and location of the ionized streams in Sagittarius A West. Astrophys. J. 699, excellence cluster ’Origin and Structure of the Universe’. 186–214 (2009). 13. Martins, F. et al. Stellar and wind properties of massive stars in the central parsec of Author Contributions S.G. collected and analysed the data and discovered the orbit of the Galaxy. Astron. Astrophys. 468, 233–254 (2007). the gas cloud. R.G. and S.G. wrote the paper. T.K.F. detected the high proper motion and 14. Scoville, N. Z., Stolovy, S. R., Rieke, M., Christopher, M. & Yusef-Zadeh, F. Hubble extracted the astrometric positions and the photometry. R.G., A.B. and E.Q. derived the Space Telescope Paa and 1.9 micron imaging of Sagittarius A West. Astrophys. J. cloud’s properties, its evolution and the estimate of the X-ray luminosity. R.G., E.Q., A.B. 594, 294–311 (2003). and C.F.G. contributed to the analytical estimates. C.A. and J.C. set up numerical 15. Xu, Y.-D., Narayan, R., Quataert, E., Yuan, F. & Baganoff, F. K. Thermal X-ray iron line simulations to check the analysis. F.E., O.P. and K.D.-E. helped in the data analysis and emission from the Galactic Center black hole Sagittarius A*. Astrophys. J. 640, interpretation. T.O. provided valuable software tools. 319–326 (2006). 16. Yuan, F., Quataert, E. & Narajan, R. Nonthermal electrons in radiatively inefficient Author Information Reprints and permissions information is available at accretion flow models of Sagittarius A*. Astrophys. J. 598, 301–312 (2003). www.nature.com/reprints. The authors declare no competing financial interests. 17. Klein, R. I., McKee, C. F. & Colella, P. On the hydrodynamic interaction of shock Readers are welcome to comment on the online version of this article at waves with interstellar clouds. 1: Nonradiative shocks in small clouds. Astrophys. J. www.nature.com/nature. Correspondence and requests for materials should be 420, 213–236 (1994). addressed to S.G. (ste@mpe.mpg.de) or R.G. (genzel@mpe.mpg.de). 5 4 | N AT U R E | VO L 4 8 1 | 5 J A N U A RY 2 0 1 2 ©2012 Macmillan Publishers Limited. All rights reserved