The Fundamental Plane of Accretion Onto Black Holes With Dynamical Masses

Gültekin, Kayhan; Cackett, Edward M.; Miller, J. M.; Matteo, Tiziana Di; Markoff, Sera; Richstone, D. O.

doi:10.1088/0004-637x/706/1/404

Cited by 207 publications

(311 citation statements)

References 118 publications

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“…It is entirely possible the data set represented in Figure 5, albeit indicative of an overall trend of radio luminosity increasing non-linearly with X-ray luminosity for sub-Eddington systems, encloses several, potentially uncorrelated phenomena that may be at the origin of its large scatter. We conclude by noticing that multiple, coordinated radio/X-ray observations of two super-massive black holes in nearby Seyfert galaxies and low-luminosity AGN, performed over periods of several months (Bell et al 2011;King et al 2011King et al , 2013, show how these systems (both akin the most radio-quiet BHBs in terms of radio-to-X-ray luminosity ratios) make almost orthogonal excursions across the fundamental plane best-fitting relation from Gültekin et al (2009), further strengthening the argument against (uncertainties in the) black hole mass or spin parameter as being entirely responsible for the large inferred intrinsic scatter.…”

mentioning

confidence: 82%

The radio/X-ray domain of black hole X-ray binaries at the lowest radio luminosities

Gallo¹,

Miller-Jones²,

Russell³

et al. 2014

Monthly Notices of the Royal Astronomical Society

155

200

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We report on deep, coordinated radio and X-ray observations of the black hole X-ray binary XTE J1118+480 in quiescence. The source was observed with the Karl G. Jansky Very Large Array for a total of 17.5 hrs at 5.3 GHz, yielding a 4.8±1.4 µJy radio source at a position consistent with the binary system. At a distance of 1.7 kpc, this corresponds to an integrated radio luminosity between 4-8 ×10 25 erg s −1 , depending on the spectral index. This is the lowest radio luminosity measured for any accreting black hole to date. Simultaneous observations with the Chandra X-ray Telescope detected XTE J1118+480 at 1.2 × 10 −14 erg s −1 cm −2 (1-10 keV), corresponding to an Eddington ratio of ∼4 × 10 −9 for a 7.5 M black hole. Combining these new measurements with data from the 2005 and 2000 outbursts available in the literature, we find evidence for a relationship of the form r =α+β X (where denotes logarithmic luminosities), with β = 0.72 ± 0.09. XTE J1118+480 is thus the third system -together with GX339-4 and V404 Cyg -for which a tight, non-linear radio/X-ray correlation has been reported over more than 5 dex in X . Confirming previous results, we find no evidence for a dependence of the correlation normalisation of an individual system on orbital parameters, relativistic boosting, reported black hole spin and/or black hole mass. We then perform a clustering and linear regression analysis on what is arguably the most up-to-date collection of coordinated radio and X-ray luminosity measurements from quiescent and hard state black hole X-ray binaries, including 24 systems. At variance with previous results, a two-cluster description is statistically preferred only for random errors < ∼ 0.3 dex in both r and X , a level which we argue can be easily reached when the known spectral shape/distance uncertainties and intrinsic variability are accounted for. A linear regression analysis performed on the whole data set returns a best-fitting slope β = 0.61 ± 0.03 and intrinsic scatter σ 0 = 0.31 ± 0.03 dex.

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mentioning

confidence: 82%

The radio/X-ray domain of black hole X-ray binaries at the lowest radio luminosities

Gallo¹,

Miller-Jones²,

Russell³

et al. 2014

Monthly Notices of the Royal Astronomical Society

155

200

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“…Bagchi et al (2014) found that, when using the black hole mass to bulge mass correlation of Marconi & Hunt (2003), the black hole mass is 2.5±0.5 × 10 8 M⊙. However Bagchi et al (2014) also find that a much larger mass of 1.4×10 9 M⊙ can be found using the MBH − σ relation of Gültekin et al (2009), using the velocity dispersion averaged within the central 2.35 kpc region along the minor axis, which they find to be 351(±25) km s −1 . As the galaxy lacks a classical bulge (it has a pseudobulge), it is challenging to accurately estimate the black hole mass using scaling relations with the bulge mass, which may cause the black hole mass estimate using this method to be underestimated.…”

Section: The Energetics Of the Agnmentioning

confidence: 99%

A deep Chandra observation of the hot gaseous halo around a rare, extremely massive and relativistic jet launching spiral galaxy

Walker

Fabian

2015

Monthly Notices of the Royal Astronomical Society

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We present a deep Chandra observation of the extremely massive spiral galaxy 2MASX J23453268-0449256, the first X-ray observation of this very rare system which features the largest known relativistic jets from a spiral galaxy. We detect extended X-ray emission from the hot halo surrounding the galaxy, reaching out to 80 kpc in radius. The hot halo is elongated along the plane of the spiral galaxy, and one possibility is that the powerful relativistic jets have disrupted the hot halo gas located perpendicular to the disk. Our calculations indicate that it is energetically feasible that the AGN feedback in this system could have uplifted or completely expelled a significant fraction of the gas in the 20-80 kpc radial range. We also detect extended emission which appears to be associated with the inner and outer southern radio lobes, and is possibly the result of inverse Compton emission. Using the observed X-ray and radio luminosity of the central AGN, the fundamental plane of Gultekin et al. predicts a black hole mass of 5×10 8 M ⊙ , with a range of 1 × 10 8 -3 × 10 9 M ⊙ when the scatter in the fundamental plane relation is taken into account. This is consistent with the possibility that an exceptionally massive (> 10 9 M ⊙ ) black hole lies at the centre of this galaxy, as suggested by the M BH − σ scaling relation, but a tighter constraint cannot be made.

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“…During such active phases, a strong physical coupling (generally termed 'feedback') could have established a long-lasting link between hosts and SMBHs, leading to the well-known local scaling relations (e.g., Ferrarese & Merritt 2000;Gebhardt et al 2000;Gültekin et al 2009). …”

Section: Introductionmentioning

confidence: 99%

X-shooter reveals powerful outflows in z ∼ 1.5 X-ray selected obscured quasi-stellar objects

Brusa

Bongiorno

Cresci

et al. 2014

Monthly Notices of the Royal Astronomical Society

160

218

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We present X-shooter@VLT observations of a sample of 10 luminous, X-ray obscured QSOs at z∼ 1.5 from the XMM-COSMOS survey, expected to be caught in the transitioning phase from starburst to AGN dominated systems. The main selection criterion is X-ray detection at bright fluxes (L X > ∼ 10 44 erg s −1 ) coupled to red optical-to-NIR-to-MIR colors. Thanks to its large wavelength coverage, X-shooter allowed us to determine accurate redshifts from the presence of multiple emission lines for five out of six targets for which we had only a photometric redshift estimate, with a 80% success rate, significantly larger than what is observed in similar programs of spectroscopic follow-up of red QSOs. We report the detection of broad and shifted components in the [OIII]λλ5007,4959 complexes for 6 out of 8 sources with these lines observable in regions free from strong atmospheric absorptions. The FWHM associated with the broad components are in the range FWHM∼ 900 − 1600 km s −1 , larger than the average value observed in SDSS Type 2 AGN samples at similar observed [OIII] luminosity, but comparable to those observed for QSO/ULIRGs systems for which the presence of kpc scale outflows have been revealed through IFU spectroscopy. Although the total outflow energetics (inferred under reasonable assumptions) may be consistent with winds accelerated by stellar processes, we favour an AGN origin for the outflows given the high outflow velocities oberved (v> 1000 km s −1 ) and the presence of strong winds also in objects undetected in the far infrared.

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The Fundamental Plane of Accretion Onto Black Holes With Dynamical Masses

Cited by 207 publications

References 118 publications

The radio/X-ray domain of black hole X-ray binaries at the lowest radio luminosities

The radio/X-ray domain of black hole X-ray binaries at the lowest radio luminosities

A deep Chandra observation of the hot gaseous halo around a rare, extremely massive and relativistic jet launching spiral galaxy

X-shooter reveals powerful outflows in z ∼ 1.5 X-ray selected obscured quasi-stellar objects

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