High Spatial Resolution Imaging of NGC 1068 in the Mid-Infrared

Bock, J. J.; Neugebauer, G.; Matthews, K.; Soifer, B. T.; Becklin, E. E.; Ressler, Michael E.; Marsh, K. A.; Werner, M. W.; Egami, E.; Blandford, R. D.

doi:10.1086/316871

Cited by 124 publications

(194 citation statements)

References 49 publications

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“…These structures are in excellent agreement with previously published highspatial resolution MIR observations (e.g. Bock et al 2000;Tomono et al 2001;Galliano et al 2005;Poncelet et al 2007).…”

Section: Spectro-polarimetrysupporting

confidence: 92%

“…Braatz et al 1993;Cameron et al 1993;Lumsden et al 1999;Bock et al 1998;Alloin et al 2000;Bock et al 2000;Tomono et al 2001;Jaffe et al 2004;Galliano et al 2005;Mason et al 2006;Tomono et al 2006;Raban et al 2009;López-Gonzaga et al 2014), a very low polarization with an upper-limit of 0.3 per cent at this location is detected within the 8−13 µm wavelength range ( Fig. 2 and 3).…”

Section: The Obscuring Dusty Structurementioning

confidence: 71%

“…At all wavelengths NGC 1068 appears as an unresolved core in the E-W direction, with extended emission along N-S. The N-S extended emission slightly bends to the N-W direction up to 0.5 arcsec (30 pc), and then to the N-E direction up to 1.4 arcsec (84 pc); this feature was termed as 'tongue' (see Bock et al 2000, fig. 2).…”

Section: Spectro-polarimetrymentioning

confidence: 99%

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Mid-infrared imaging- and spectro-polarimetric subarcsecond observations of NGC 1068

López-Rodríguez

Packham

Roche

et al. 2016

Mon. Not. R. Astron. Soc.

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We present sub-arcsecond 7.5−13 µm imaging-and spectro-polarimetric observations of NGC 1068 using CanariCam on the 10.4-m Gran Telescopio CANARIAS. At all wavelengths, we find: (1) A 90 × 60 pc extended polarized feature in the northern ionization cone, with a uniform ∼44 • polarization angle. Its polarization arises from dust and gas emission in the ionization cone, heated by the active nucleus and jet, and further extinguished by aligned dust grains in the host galaxy. The polarization spectrum of the jet-molecular cloud interaction at ∼24 pc from the core is highly polarized, and does not show a silicate feature, suggesting that the dust grains are different from those in the interstellar medium. (2) A southern polarized feature at ∼9.6 pc from the core. Its polarization arises from a dust emission component extinguished by a large concentration of dust in the galaxy disc. We cannot distinguish between dust emission from magnetically aligned dust grains directly heated by the jet close to the core, and aligned dust grains in the dusty obscuring material surrounding the central engine. Silicate-like grains reproduce the polarized dust emission in this feature, suggesting different dust compositions in both ionization cones. (3) An upper limit of polarization degree of 0.3 per cent in the core. Based on our polarization model, the expected polarization of the obscuring dusty material is 0.1 per cent in the 8−13 µm wavelength range. This low polarization may be arising from the passage of radiation through aligned dust grains in the shielded edges of the clumps.

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Section: Spectro-polarimetrysupporting

confidence: 92%

Section: The Obscuring Dusty Structurementioning

confidence: 71%

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Mid-infrared imaging- and spectro-polarimetric subarcsecond observations of NGC 1068

López-Rodríguez

Packham

Roche

et al. 2016

Mon. Not. R. Astron. Soc.

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“…First mid-IR images with 0.1 spatial resolution are reported by Bock et al (2000), using the 10 m Keck II telescope. They interpret the northern elongation of the central peak as reprocessed radiation from the AGN.…”

Section: Introductionmentioning

confidence: 99%

A new analysis of the nucleus of NGC 1068 with MIDI observations

Poncelet

Perrin²,

Sol³

2006

A&A

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We present a new analysis of the first mid-infrared N-band long-baseline interferometric observations of an extragalactic source: the nucleus of the Seyfert 2 galaxy NGC 1068, obtained with MIDI (Mid-InfrareD Interferometer), the mid-infrared beamcombiner at the European Southern Observatory (ESO) Very Large Telescope Interferometer (VLTI). The resolution of λ/B ∼ 10 mas allows us to study the compact central core of the galaxy between 8 and 13 µm. Both visibility measurements and MIDI spectrum are well reproduced by a simple radiative transfer model with two concentric spherical components. The derived angular sizes and temperatures are ∼35 and 83 mas, and ∼361 K and 226 K for these two components respectively. Other evidence strongly supports such low temperatures. This modeling also provides the variation of optical depth as a function of wavelength for the extended component across the N-band suggesting the presence of amorphous silicate grains. This shows that MIDI has carried out the first direct observations of the distribution of dust around the central engine.

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“…Several high-resolution infrared observations of NGC 1068 showing a compact central IR core and surrounding structure were carried out by, for instance, Thatte et al (1997), Rouan et al (1998), Wittkowski et al (1998), Weinberger et al (1999), and Bock et al (2000. Wittkowski et al (1998) presented both a K-band visibility function up to spatial frequencies corresponding to a baseline of 6 m, as well as the first 76 mas resolution K-band image of the nucleus of NGC 1068 obtained by bispectrum speckle interferometry.…”

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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High Spatial Resolution Imaging of NGC 1068 in the Mid-Infrared

Cited by 124 publications

References 49 publications

Mid-infrared imaging- and spectro-polarimetric subarcsecond observations of NGC 1068

Mid-infrared imaging- and spectro-polarimetric subarcsecond observations of NGC 1068

A new analysis of the nucleus of NGC 1068 with MIDI observations

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

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