The Fundamental Plane of black hole activity in the optical band

Saikia, Payaswini; Körding, Elmar; Falcke, H.

doi:10.1093/mnras/stv731

Cited by 53 publications

(92 citation statements)

References 50 publications

(56 reference statements)

Supporting

Mentioning

Contrasting

Order By: Relevance

“…This is in contrast with X-ray binaries and CVs, which generally show flaring at radio, optical, and X-ray wavelengths alongside strong Balmer emission lines. Similarly, the fundamental plane of black hole activity (e.g., Plotkin et al 2012;Saikia et al 2015) predicts L R significantly greater than~10 22 W Hz −1 when =Ĺ 1.5 10 X 44 erg s −1 .…”

Section: Disk-jet Connectionmentioning

confidence: 90%

iPTF Discovery of the Rapid “Turn-on” of a Luminous Quasar

Gezari

Hung

Cenko

et al. 2017

ApJ

137

175

View full text Add to dashboard Cite

We present a radio-quiet quasar at z=0.237 discovered "turning on" by the intermediate Palomar Transient Factory (iPTF). The transient, iPTF 16bco, was detected by iPTF in the nucleus of a galaxy with an archival Sloan Digital Sky Survey spectrum with weak narrow-line emission characteristic of a low-ionization nuclear emissionline region (LINER). Our follow-up spectra show the dramatic appearance of broad Balmer lines and a power-law continuum characteristic of a luminous ( » L 10 bol 45 erg s −1 ) type 1 quasar 12 yr later. Our photometric monitoring with PTF from 2009-2012 and serendipitous X-ray observations from the XMM-Newton Slew Survey in 2011 and 2015 constrain the change of state to have occurred less than 500 days before the iPTF detection. An enhanced broad Hα/[O III] λ5007 line ratio in the type 1 state relative to other changing-look quasars also is suggestive of the most rapid change of state yet observed in a quasar. We argue that the >10 increase in Eddington ratio inferred from the brightening in UV and X-ray continuum flux is more likely due to an intrinsic change in the accretion rate of a preexisting accretion disk than an external mechanism such as variable obscuration, microlensing, or the tidal disruption of a star. However, further monitoring will be helpful in better constraining the mechanism driving this change of state. The rapid "turn-on" of the quasar is much shorter than the viscous infall timescale of an accretion disk and requires a disk instability that can develop around a  M 10 8 black hole on timescales less than 1 yr.

show abstract

Section: Disk-jet Connectionmentioning

confidence: 90%

iPTF Discovery of the Rapid “Turn-on” of a Luminous Quasar

Gezari

Hung

Cenko

et al. 2017

ApJ

137

175

View full text Add to dashboard Cite

show abstract

“…The LLAGN sample used in the optical fundamental plane of black hole activity (Saikia et al 2015) is extracted from the Palomar Spectroscopic Survey (Ho et al 1995), comprising the nuclear region of 486 bright nearby galaxies with the B-magnitude in Tycho photometric band BT < 12.5 mag.…”

Section: Low Luminosity Agn In the Optical Fpmentioning

confidence: 99%

“…Moreover, a Kendall Tau Partial Correlation analysis was performed in Saikia et al (2015) with distance as the third variable, and the FP relation was found to be real even after taking into account the large range of inferred distance. The chi-square confidence map for the parameters of the fundamental plane was found to be an elongated ellipse, showing that the parameters are coupled (Saikia et al 2015). The uncertainties in the directly measured quantities like radio and [OIII] fluxes and the inferred quantities like distances and black hole masses are properly taken into account using the merit function while deriving the fundamental plane parameters.…”

Section: Low Luminosity Agn In the Optical Fpmentioning

confidence: 99%

“…Studying the blazars with the optical FP can give us more insight as unlike the X-ray and radio luminosities, the [OIII] emission line luminosity is assumed to be direction-independent and hence not affected by relativistic boosting. Saikia et al (2015) construct the optical FP by performing a multivariate correlation linear regression analysis on the SMBH sample. The relation was then extrapolated to lower black hole masses and the stellar mass black hole were consistent with the plane found with only the SMBHs.…”

Section: Blazars In Previous Fundamental Planesmentioning

confidence: 99%

See 1 more Smart Citation

Lorentz factor distribution of blazars from the optical Fundamental Plane of black hole activity

Saikia

Körding

Falcke

2016

Mon. Not. R. Astron. Soc.

Self Cite

View full text Add to dashboard Cite

Blazar radiation is dominated by a relativistic jet which can be modeled at first approximation using just two intrinsic parameters -the Lorentz factor Γ and the viewing angle θ. Blazar jet observations are often beamed due to relativistic effects, complicating the understanding of these intrinsic properties. The most common way to estimate blazar Lorentz factors needs the estimation of apparent jet speeds and Doppler beaming factors. We present a new and independent method of constructing the blazar Lorentz factor distribution, using the optical fundamental plane of black hole activity. The optical fundamental plane is a plane stretched out by both the supermassive black holes and the X-ray binaries, in the 3D space provided by their [OIII] line luminosity, radio luminosity and black hole mass. We use the intrinsic radio luminosity obtained from the optical fundamental plane to constrain the boosting parameters of the VLBA Imaging and Polarimetry Survey (VIPS) blazar sample. We find a blazar bulk Lorentz factor distribution in the form of a power law as N (Γ) ∝ Γ −2.1±0.4 for the Γ range of 1 to 40. We also discuss the viewing angle distribution of the blazars and the dependence of our results on the input parameters.

show abstract

“…Such a hypothesis has been predicted by theoretical models (Heinz & Sunyaev 2003). Merloni et al (2003) as well as similar attempts to establish a relation connecting BH-powered jets of different M BH (Nagar et al 2002;Falcke et al 2004;Körding et al 2006;Plotkin et al 2012;Saikia et al 2015) have either explicitly avoided blazars focusing on low-luminosity active galactic nuclei (LLAGNs) or have included a handful of blazars. In the latter case, they have either ignored the relativistic effects or specifically chosen their sample to include only low-beamed sources.…”

Section: Introductionmentioning

confidence: 89%

Scale Invariant Jets: From Blazars to Microquasars

Liodakis

Pavlidou

Papadakis

et al. 2017

ApJ

View full text Add to dashboard Cite

Black holes, anywhere in the stellar-mass to supermassive range, are often associated with relativistic jets. Models suggest that jet production may be a universal process common in all black hole systems regardless of their mass. Although in many cases observations support such hypotheses for microquasars and Seyfert galaxies, little is known regarding whether boosted blazar jets also comply with such universal scaling laws. We use uniquely rich multi-wavelength radio light curves from the F-GAMMA program and the most accurate Doppler factors available to date to probe blazar jets in their emission rest frame with unprecedented accuracy. We identify for the first time a strong correlation between the blazar intrinsic broadband radio luminosity and black hole mass, which extends over ∼9 orders of magnitude down to microquasar scales. Our results reveal the presence of a universal scaling law that bridges the observing and emission rest frames in beamed sources and allows us to effectively constrain jet models. They consequently provide an independent method for estimating the Doppler factor and for predicting expected radio luminosities of boosted jets operating in systems of intermediate or tens of solar mass black holes, which are immediately applicable to cases such as those recently observed by LIGO.

show abstract

The Fundamental Plane of black hole activity in the optical band

Cited by 53 publications

References 50 publications

iPTF Discovery of the Rapid “Turn-on” of a Luminous Quasar

iPTF Discovery of the Rapid “Turn-on” of a Luminous Quasar

Lorentz factor distribution of blazars from the optical Fundamental Plane of black hole activity

Scale Invariant Jets: From Blazars to Microquasars

Contact Info

Product

Resources

About