Observational Evidence of Jet Precession in Galactic Nuclei Caused by Accretion Disks

Lu, Jing; Zhou, Bo-Yan

doi:10.1086/499333

Cited by 41 publications

(41 citation statements)

References 41 publications

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“…A shorter period than our derived SMBHB P orb implies an even faster rising velocity, which is less likely given the speed of sound. Also, the critical radius for the precessing disk is ∼ 0.02 pc (derived according to Lu & Zhou 2005), which is a factor of ∼ 10 smaller than the inner megamaser disk size of 0.17 pc (Kondratko et al 2008). Since there appears to be good alignment between the axis of the megamaser disk and the ionization cones (Kondratko et al 2008), there is no evidence for misalignment between the extended and inner disks.…”

Section: Accretion Disk Precessionmentioning

confidence: 87%

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CHEERS Results from NGC 3393. II. Investigating the Extended Narrow-line Region Using Deep Chandra Observations and Hubble Space Telescope Narrow-line Imaging

Maksym

Fabbiano

Elvis

et al. 2017

ApJ

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The CHandra Extended Emission Line Region Survey (CHEERS) is an X-ray study of nearby active galactic nuclei (AGN) designed to take full advantage of Chandra's unique angular resolution by spatially resolving feedback signatures and effects. In the second paper of a series on CHEERS target NGC 3393, we examine deep high-resolution Chandra images and compare them with Hubble narrow line images of [O III], [S II] and Hα, as well as previously-unpublished midultraviolet (MUV) images. We find evidence for a complex multi-phase structure in the circumnuclear ISM, with no single simple correlation between X-rays and high-ionization ([O III]/Hα-dominated) and low-ionization ([S II]-dominated) features. We also find X-ray structures ∼ 50-pc in extent, Hα evidence for gas compression, and extended MUV emission associated with the Sshaped arms that envelope the radio jets. In conjunction with existing STIS kinematics, these findings support a role for shock contributions to the feedback, driven by the radio outflows associated with the radio jets.

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Section: Accretion Disk Precessionmentioning

confidence: 87%

“…Such precession would be due to the Bardeen & Petterson (1975) effect, where Lense-Thirring precession causes a misaligned disk to warp and align with the SMBH spin. From Lu & Zhou (2005), expected period ranges from P BP ∼ 7.8 × 10…”

Section: Accretion Disk Precessionmentioning

confidence: 99%

CHEERS Results from NGC 3393. II. Investigating the Extended Narrow-line Region Using Deep Chandra Observations and Hubble Space Telescope Narrow-line Imaging

Maksym

Fabbiano

Elvis

et al. 2017

ApJ

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“…Using data in the literature, Lu & Zhou (2005) find that the expected precession period for a jet with a single SMBH (Lu & Zhou 2005) is: log(τprec/yr) ∼ 0.48M abs + 0.14 log M 10 8 M + A where A = 15.18 − 18.86, depending on the values of constant parameters relating to the viscosity and angular momentum of the SMBH system. For a representative quasar with M abs = −25 with a 10 8 M SMBH, this gives a period between 10 2.2−6.9 years which is much longer than the observed periods reported here.…”

Section: A Jet With a Varying Viewing Anglementioning

confidence: 99%

A systematic search for close supermassive black hole binaries in the Catalina Real-time Transient Survey

Graham

Djorgovski

Stern

et al. 2015

Mon. Not. R. Astron. Soc.

286

291

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Hierarchical assembly models predict a population of supermassive black hole (SMBH) binaries. These are not resolvable by direct imaging but may be detectable via periodic variability (or nanohertz frequency gravitational waves). Following our detection of a 5.2 year periodic signal in the quasar PG 1302-102 (Graham et al. 2015), we present a novel analysis of the optical variability of 243,500 known spectroscopically confirmed quasars using data from the Catalina Real-time Transient Survey (CRTS) to look for close (< 0.1 pc) SMBH systems. Looking for a strong Keplerian periodic signal with at least 1.5 cycles over a baseline of nine years, we find a sample of 111 candidate objects. This is in conservative agreement with theoretical predictions from models of binary SMBH populations. Simulated data sets, assuming stochastic variability, also produce no equivalent candidates implying a low likelihood of spurious detections. The periodicity seen is likely attributable to either jet precession, warped accretion disks or periodic accretion associated with a close SMBH binary system. We also consider how other SMBH binary candidates in the literature appear in CRTS data and show that none of these are equivalent to the identified objects. Finally, the distribution of objects found is consistent with that expected from a gravitational wave-driven population. This implies that circumbinary gas is present at small orbital radii and is being perturbed by the black holes. None of the sources is expected to merge within at least the next century. This study opens a new unique window to study a population of close SMBH binaries that must exist according to our current understanding of galaxy and SMBH evolution.

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“…The expected precession period for a single SMBH is given by where α is the viscosity parameter, a is black hole spin, andṀ • is the mass accretion rate (Lu & Zhou 2005). This period is typically much longer than the observed period unless a approaches extraordinarily close to 0.…”

Section: Precessing Jet Modelmentioning

confidence: 99%

Spectroscopic Indication of a Centi-Parsec Supermassive Black Hole Binary in the Galactic Center of Ngc 5548

Wang

et al. 2016

ApJ

111

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As a natural consequence of cosmological hierarchical structure formation, sub-parsec supermassive black hole binaries (SMBHBs) should be common in galaxies but thus far have eluded spectroscopic identification. Based on four decades of optical spectroscopic monitoring, we report that the nucleus of NGC5548, a nearby Seyfert galaxy long suspected to have experienced a major merger about 1 billion yr ago, exhibits long-term variability with a period of ∼14 yr in the optical continuum and broad Hβ emission line. Remarkably, the double-peaked profile of Hβ shows systematic velocity changes with a similar period. These pieces of observations plausibly indicate that an SMBHB resides in the center of NGC5548. The complex, secular variations in the line profiles can be explained by orbital motion of a binary with equal mass and a semimajor axis of ∼22 light-days (corresponding to ∼18 milli-parsec). At a distance of 75Mpc, NGC5548 is one of the nearest sub-parsec SMBHB candidates that offers an ideal laboratory for gravitational wave detection.

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Observational Evidence of Jet Precession in Galactic Nuclei Caused by Accretion Disks

Abstract: We show that the observational data of extragalactic radio sources tend to support the theoretical relationship between the jet precession period and the optical luminosity of the sources, as predicted by the model in which an accretion disk causes the central black hole to precess.

Cited by 41 publications

References 41 publications

CHEERS Results from NGC 3393. II. Investigating the Extended Narrow-line Region Using Deep Chandra Observations and Hubble Space Telescope Narrow-line Imaging

CHEERS Results from NGC 3393. II. Investigating the Extended Narrow-line Region Using Deep Chandra Observations and Hubble Space Telescope Narrow-line Imaging

A systematic search for close supermassive black hole binaries in the Catalina Real-time Transient Survey

Spectroscopic Indication of a Centi-Parsec Supermassive Black Hole Binary in the Galactic Center of Ngc 5548

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