Spectropolarimetry and the nature of NGC 1068

Antonucci, Robert; Miller, Joseph S.

doi:10.1086/163559

Cited by 1,477 publications

(1,304 citation statements)

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“…Many observational evidences (see Alexander et al 2005;Page et al 2004;Stevens et al 2006) and theoretical arguments (Menci et al 2008, and references therein) in favor of the evolutionary sequence do exist. These results challenge our 20-years old AGN view, in which the differences we see in different classes of sources -especially between "obscured" and "unobscured" ones -are simply due to orientations effects (Antonucci et al 1985;Antonucci 2003;Urry & Padovani 1995).…”

Section: Introductioncontrasting

confidence: 69%

Black hole growth and starburst activity atz= 0.6–4 in the Chandra Deep Field South

Brusa¹,

Fiore

Santini

et al. 2009

A&A

104

113

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Aims. The co-evolution of host galaxies and the active black holes which reside in their centre is one of the most important topics in modern observational cosmology. Here we present a study of the properties of obscured active galactic nuclei (AGN) detected in the CDFS 1 Ms observation and their host galaxies. Methods. We limited the analysis to the MUSIC area, for which deep K-band observations obtained with ISAAC@VLT are available, ensuring accurate identifications of the counterparts of the X-ray sources as well as reliable determination of photometric redshifts and galaxy parameters, such as stellar masses and star formation rates. In particular, we: 1) refined the X-ray/infrared/optical association of 179 sources in the MUSIC area detected in the Chandra observation; 2) studied the host galaxies observed and rest frame colors and properties. Results. We found that X-ray selected (L X > ∼ 10 42 erg s −1 ) AGN show Spitzer colors consistent with both AGN and starburst dominated infrared continuum; the latter would not have been selected as AGN from infrared diagnostics. The host galaxies of X-ray selected obscured AGN are all massive (M * > 10 10 M ) and, in 50% of the cases, are also actively forming stars (1/SSFR < t Hubble ) in dusty environments. The median L/L Edd value of the active nucleus is between 2% and 10% depending on the assumed M BH /M * ratio. Finally, we found that the X-ray selected AGN fraction increases with the stellar mass up to a value of ∼30% at z > 1 and M * > 3 × 10 11 M , a fraction significantly higher than in the local Universe for AGN of similar luminosities.

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Section: Introductioncontrasting

confidence: 69%

Black hole growth and starburst activity atz= 0.6–4 in the Chandra Deep Field South

Brusa¹,

Fiore

Santini

et al. 2009

A&A

104

113

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“…Since the discovery of its Seyfert 1 nucleus in linearly polarized light (Antonucci & Miller 1985), it presents the strongest case for a unified model of active galactic nuclei (AGNs).…”

Section: Introductionmentioning

confidence: 99%

What powers the starburst activity of NGC 1068? Star-driven gravitational instabilities caught in the act

Romeo

Fathi

2016

Mon. Not. R. Astron. Soc.

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We explore the role that gravitational instability plays in NGC 1068, a nearby Seyfert galaxy that exhibits unusually vigorous starburst activity. For this purpose, we use the Romeo-Falstad disc instability diagnostics and data from BIMA SONG, SDSS and SAURON. Our analysis illustrates that NGC 1068 is a gravitationally unstable 'monster'. Its starburst disc is subject to unusually powerful instabilities. Several processes, including AGN/stellar feedback, try to quench such instabilities from inside out by depressing the surface density of molecular gas across the central kpc, but they do not succeed. Gravitational instability 'wins' because it is driven by the stars via their much higher surface density. In this process, stars and molecular gas are strongly coupled, and it is such a coupling that ultimately triggers local gravitational collapse/fragmentation in the molecular gas.

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“…Active galaxies appear as types 1 and 2, where the spectra of the former exhibit broad and narrow emission lines, and those of the latter show only narrow lines. Antonucci & Miller (1985) suggested that the broad-line emission regions are located inside an optically and geometrically thick disk and that central continuum and broad-line photons are scattered into the line-of-sight by free electrons above and below the disk. Depending on the observer's viewing angle, the broad-line emission region is either obscured or not.…”

Section: Introductionmentioning

confidence: 99%

VLTI/VINCI observations of the nucleus of NGC 1068 using the adaptive optics system MACAO

Wittkowski

Kervella

Arsenault

et al. 2004

A&A

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Abstract. We present the first near-infrared K-band long-baseline interferometric measurement of the nucleus of the prototype Seyfert 2 Galaxy NGC 1068 with resolution λ/B ∼ 10 mas obtained with the Very Large Telescope Interferometer (VLTI) and the two 8.2 m diameter Unit Telescopes UT 2 and UT 3. The adaptive optics system MACAO (Multi Application Curvature Adaptive Optics) was employed to deliver wavefront-corrected beams to the K-band commissioning instrument VINCI. A squared visibility amplitude of 16.3 ± 4.3% was measured for NGC 1068 at a sky-projected baseline length of 45.8 m and azimuth angle 44.9 deg. This value corresponds to a FWHM of the K-band intensity distribution of 5.0 ± 0.5 mas (0.4 ± 0.04 pc at the distance of NGC 1068) if it consists of a single Gaussian component. Taking into account K-band speckle interferometry observations (Wittkowski et al. 1998;Weinberger et al. 1999;Weigelt et al. 2004), we favor a multi-component model for the intensity distribution where a part of the flux originates from scales clearly smaller than ∼5 mas ( < ∼ 0.4 pc), and another part of the flux from larger scales. The K-band emission from the small ( < ∼ 5 mas) scales might arise from substructure of the dusty nuclear torus, or directly from the central accretion flow viewed through only moderate extinction.

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Spectropolarimetry and the nature of NGC 1068

Cited by 1,477 publications

References 0 publications

Black hole growth and starburst activity atz= 0.6–4 in the Chandra Deep Field South

Black hole growth and starburst activity atz= 0.6–4 in the Chandra Deep Field South

What powers the starburst activity of NGC 1068? Star-driven gravitational instabilities caught in the act

VLTI/VINCI observations of the nucleus of NGC 1068 using the adaptive optics system MACAO

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