2014A&A...563A..82T


C.D.S. - SIMBAD4 rel 1.7 - 2019.11.11CET22:24:26

2014A&A...563A..82T - Astronomy and Astrophysics, volume 563A, 82-82 (2014/3-1)

The dusty torus in the Circinus galaxy: a dense disk and the torus funnel.

TRISTRAM K.R.W., BURTSCHER L., JAFFE W., MEISENHEIMER K., HOENIG S.F., KISHIMOTO M., SCHARTMANN M. and WEIGELT G.

Abstract (from CDS):

With infrared interferometry it is possible to resolve the nuclear dust distributions that are commonly associated with the dusty torus in active galactic nuclei (AGN). The Circinus galaxy hosts the closest Seyfert 2 nucleus and previous interferometric observations have shown that its nuclear dust emission is particularly well resolved. The aim of the present interferometric investigation is to better constrain the dust morphology in this active nucleus. To this end, extensive new observations were carried out with the MID-infrared Interferometric instrument (MIDI) at the Very Large Telescope Interferometer, leading to a total of 152 correlated flux spectra and differential phases between 8 and 13µm. To interpret this data, we used a model consisting of black-body emitters with a Gaussian brightness distribution and with dust extinction. The direct analysis of the data and the modelling confirm that the emission is distributed in two distinct components: a disk-like emission component with a size (FWHM) of ∼0.2x1.1pc and an extended component with a size of ∼0.8x1.9pc. The disk-like component is elongated along PA∼46° and oriented perpendicular to the ionisation cone and outflow. The extended component is responsible for 80% of the mid-infrared emission. It is elongated along PA∼107°, which is roughly perpendicular to the disk component and thus in polar direction. It is interpreted as emission from the inner funnel of an extended dust distribution and shows a strong increase in the extinction towards the south-east. We find both emission components to be consistent with dust at T∼300K, that is we find no evidence of an increase in the temperature of the dust towards the centre. From this we infer that most of the near-infrared emission probably comes from parsec scales as well. We further argue that the disk component alone is not sufficient to provide the necessary obscuration and collimation of the ionising radiation and outflow. The material responsible for this must instead be located on scales of ∼1pc, surrounding the disk. We associate this material with the dusty torus. The clear separation of the dust emission into a disk-like emitter and a polar elongated source will require an adaptation of our current understanding of the dust emission in AGN. The lack of any evidence of an increase in the dust temperature towards the centre poses a challenge for the picture of a centrally heated dust distribution.

Abstract Copyright:

Journal keyword(s): galaxies: active - galaxies: nuclei - galaxies: Seyfert - galaxies: individual: Circinus - galaxies: structure - techniques: interferometric

Simbad objects: 14

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Number of rows : 14

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2020
#notes
1 NGC 424 Sy2 01 11 27.6374462713 -38 05 00.404099901   13.76 14.12 12.38 12.8 ~ 268 0
2 M 77 GiP 02 42 40.771 -00 00 47.84 9.70 9.61 8.87 10.1 9.9 ~ 3988 2
3 NGC 3783 Sy1 11 39 01.7095761008 -37 44 19.008597647   12.46 13.43 11.33 12.1 ~ 1445 0
4 NGC 4151 Sy1 12 10 32.5771747733 +39 24 21.057727323   12.18 11.48     ~ 3308 2
5 * eps Cru PM* 12 21 21.6093625 -60 24 04.129070   5.01 3.59     K3III 81 0
6 NGC 4593 Sy1 12 39 39.4435521178 -05 20 39.035028119   13.95 13.15     ~ 916 0
7 Mrk 231 Sy1 12 56 14.2340989340 +56 52 25.238555193   14.68 13.84     ~ 1737 3
8 NAME Centaurus A Sy2 13 25 27.61509104 -43 01 08.8056025   8.18 6.84 6.66   ~ 3894 3
9 HD 120404 * 13 51 47.4342248812 -69 24 04.515687153   7.459 5.727     K5/M0III 22 0
10 NAME Circinus Galaxy Sy2 14 13 09.906 -65 20 20.47   10.89 9.84 10.6 10.0 ~ 969 2
11 V* V1003 Cen LP? 14 22 52.2433393098 -55 57 44.364171171   9.66 7.88     M5II 15 0
12 * alf TrA * 16 48 39.89508 -69 01 39.7626   3.36 1.92     K2III_Ba1 227 0
13 EM* AS 220 Ae* 17 10 08.1238 -27 15 18.801 12.86 12.79 12.22 12.03 10.82 A6Ve+G5Ve 125 0
14 * alf Lyr dS* 18 36 56.33635 +38 47 01.2802 0.03 0.03 0.03 0.07 0.10 A0Va 2472 0

    Equat.    Gal    SGal    Ecl

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2019.11.11-22:24:26

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