Mid‐Infrared Spectral Energy Distribution of NGC 1068 with 0.̋1 Spatial Resolution

Tomono, Daigo; Doi, Yoshihiro; Usuda, Tomonori; Nishimura, Tetsuo

doi:10.1086/322262

Cited by 48 publications

(83 citation statements)

References 34 publications

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“…As discussed by the authors, this coincidence between Hα and dust emission is comparable to what happens in galactic HII regions, and could be due to dust entrained into HII regions. Nevertheless, these features are clearly not detected in Mid-IR either by Bock et al (2000) or by Tomono et al (2001). An explanation could be the lower sensitivity of the 10 µm observations.…”

Section: Southern Structuresmentioning

confidence: 84%

Four quadrant phase maskK-band coronagraphy of NGC 1068 with NAOS-CONICA at VLT

Gratadour

Rouan²,

Boccaletti³

et al. 2004

A&A

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Abstract.We observed the nucleus of NGC 1068 at Ks with NAOS-CONICA on the VLT, using the new four quadrant phase mask coronagraph that we recently developed. As the K-band emission is dominated by an intense compact central source, previous K-band adaptive optics images were severely affected by the limited exposure time and by scattered light in the immediate vicinity of the source. Thanks to the use of this new type of coronagraph coupled to adaptive optics, the complex dust structure near the central core is becoming observable at a resolution of 0.07 . North of the nucleus, an elongated, bending structure, and a series of four elongated and well aligned knots, superposable on the same pattern previously observed by us at 3.8 and 4.8 µm are well identified. This agrees with our first interpretation that, given the direction they align in, these knots may trace shocks induced in the ISM by the passage of the jet, very close to its origin. Moreover, precise relative photometry supports our interpretation of very small dust grains transiently heated by UV photons of the central source. To the South we detect a new group of filamentary structures, distributed in a cone at about 150 pc from the core. They might trace the redshifted southern narrow line region, seen through the dust. Finally, on larger scale (within a radius of three hundred pc) the source has an overall biconical shape whose angle matches well with the bicone observed in the UV-visible.

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Section: Southern Structuresmentioning

confidence: 84%

Four quadrant phase maskK-band coronagraphy of NGC 1068 with NAOS-CONICA at VLT

Gratadour

Rouan²,

Boccaletti³

et al. 2004

A&A

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“…At the highest spatial sampling, continuum core fluxes of 9-10 Jy have been reported around 12-μm (Mason et al 2006;Tomono et al 2001), and they correspond to log λL λ ≈ 43.8.…”

Section: A110 Ngc 6814mentioning

confidence: 96%

Resolving the mid-infrared cores of local Seyferts

Gandhi

Horst

Smette

et al. 2009

A&A

394

112

647

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We present new photometry of 16 local Seyferts including 6 Compton-thick sources in N-band filters around 12-μm, obtained with the VISIR instrument on the 8-m Very Large Telescope. The near-diffraction-limited imaging provides the least-contaminated core fluxes for these sources to date. Augmenting these with our previous observations and with published intrinsic X-ray fluxes, we form a total sample of 42 sources for which we find a strong mid-infrared:X-ray (12.3 μm:2-10 keV) luminosity correlation. Performing a physically-motivated subselection of sources in which the Seyfert torus is likely to be best-resolved results in the correlation L MIR ∝ L X 1.11±0.07 , with a reduction of the scatter in luminosities as compared to the full sample. Consideration of systematics suggests a range of 1.02-1.21 for the correlation slope. The mean 2-keV:12.3-μm spectral index (α IX ) is found to be −1.10 ± 0.01, largely independent of luminosity. Indirectly-computed 12-μm bolometric corrections range over ≈10-30 if a known luminosity trend of X-ray bolometric corrections is assumed. Comparison with ISO data spanning a wider luminosity range suggests that our correlation can be extended into the quasar regime. That unobscured, obscured, and Compton-thick sources all closely follow the same luminosity correlation has important implications for the structures of Seyfert cores. The typical resolution-limit of our imaging corresponds to ∼70 pc at a median z = 0.01, and we use the tightness of the correlation to place constraints on the dominance of any residual emission sources within these physical scales. An upper-limit for any contaminating star formation of ≈40% of the unresolved flux is inferred, on average. We suggest that uncontaminated mid-IR continuum imaging of AGN is an accurate proxy for their intrinsic power.

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“…The original aims of this study were two-fold: (1) perform preliminary observations of active galaxies in order to prepare future observations with VISIR at the VLT, (2) look for extended MIR emission directly related to the AGN, as was observed along the radio jet direction in NGC 1068 (Alloin et al 2000;Bock et al 2000;Tomono et al 2001). To address these aims, we chose a sample of nearby (few Mpc) to moderately nearby (few hundreds of Mpc) AGN.…”

Section: Observationsmentioning

confidence: 99%

“…MIR imaging of this source at 0.6 resolution revealed extended and collimated 10 and 20 µm emission up to 5 from the core, along the direction of the radio jet (Alloin et al 2000). At higher angular resolution (0.1 after deconvolution: Bock et al 2000;Tomono et al 2001), the complex structure of the MIR emission is found to be coincident with the narrow line region (NLR) clouds (Galliano et al 2003). Therefore, the access to high resolution imaging brings new clues regarding the morphology of the material around the central engines of AGN.…”

Section: Introductionmentioning

confidence: 99%

Mid-infrared imaging of active galaxies

Galliano¹,

Alloin

Pantin

et al. 2005

A&A

163

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Abstract. High resolution, mid-infrared (MIR) images of nine nearby active galaxies are presented. The data were obtained with the TIMMI 2 instrument mounted at the ESO 3.6 m telescope using a set of N-band narrow filters. The resulting images have an angular resolution of 0.6 −1 . The MIR emission has been resolved in four galaxies: NGC 253, NGC 1365, NGC 1808 and NGC 7469. The images show a circumnuclear population of unknown MIR sources in NGC 1365 and NGC 1808, coincident with radio sources. These MIR/radio sources are interpreted in terms of embedded young star clusters. A high-resolution MIR map of NGC 253 is also presented, and enables the identification of a previously unknown MIR counterpart to the radio nucleus. Extended MIR emission is detected in NGC 7469, and concurs with previous observations in the NIR and radio. For this source, an interesting morphological difference between the 10.4 µm and the 11.9 µm emission is observed, suggesting the presence of a dust-rich micro-bar. Our MIR images of Circinus do not show resolved emission from the nucleus down to an angular scale of 0.5 . In the case of NGC 2992, an upper limit to the extended MIR emission can be set. We provide new MIR flux measurements for the unresolved AGN in NGC 5995, IZw1 and IIZw136.

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Mid‐Infrared Spectral Energy Distribution of NGC 1068 with 0.̋1 Spatial Resolution

Cited by 48 publications

References 34 publications

Four quadrant phase maskK-band coronagraphy of NGC 1068 with NAOS-CONICA at VLT

Four quadrant phase maskK-band coronagraphy of NGC 1068 with NAOS-CONICA at VLT

Resolving the mid-infrared cores of local Seyferts

Mid-infrared imaging of active galaxies

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