# 2009A&A...502...67T

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 Query : 2009A&A...502...67T

2009A&A...502...67T - Astronomy and Astrophysics, volume 502, 67-84 (2009/7-4)

Parsec-scale dust distributions in Seyfert galaxies. Results of the MIDI AGN snapshot survey.

TRISTRAM K.R.W., RABAN D., MEISENHEIMER K., JAFFE W., ROTTGERING H., BURTSCHER L., COTTON W.D., GRASER U., HENNING T., LEINERT C., LOPEZ B., MOREL S., PERRIN G. and WITTKOWSKI M.

Abstract (from CDS):

The emission of warm dust dominates the mid-infrared spectra of active galactic nuclei (AGN). Only interferometric observations provide the necessary angular resolution to resolve the nuclear dust and to study its distribution and properties. The investigation of dust in AGN cores is hence one of the main science goals for the MID-infrared Interferometric instrument MIDI at the VLTI. As the first step, the feasibility of AGN observations was verified and the most promising sources for detailed studies were identified. This was carried out in a snapshot survey'' with MIDI using Guaranteed Time Observations. In the survey, observations were attempted for 13 of the brightest AGN in the mid-infrared which are visible from Paranal. The results of the three brightest, best studied sources have been published in separate papers. Here we present the interferometric observations for the remaining 10, fainter AGN. For 8 of these, interferometric measurements could be carried out. Size estimates or limits on the spatial extent of the AGN-heated dust were derived from the interferometric data of 7 AGN. These indicate that the dust distributions are compact, with sizes on the order of a few parsec. The derived sizes roughly scale with the square root of the luminosity in the mid-infrared, s∝sqrt(LMIR), with no clear distinction between type 1 and type 2 objects. This is in agreement with a model of nearly optically thick dust structures heated to T∼300K. For three sources, the 10 µm feature due to silicates is tentatively detected either in emission or in absorption. The faint AGN of the snapshot survey are at the sensitivity limit of observations with MIDI. Thus, the data set presented here provides a good insight into the observational difficulties and their implications for the observing strategy and data analysis. Based on the results for all AGN studied with MIDI so far, we conclude that in the mid-infrared the differences between individual galactic nuclei are greater than the generic differences between type 1 and type 2 objects.

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

Full paper

 Number of rows : 32
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2023
#notes
1 NGC 253 SyG 00 47 33.134 -25 17 19.68   8.03   6.94 8.1 ~ 3192 2
2 NGC 424 Sy2 01 11 27.6385025496 -38 05 00.421096524   13.76 14.12 12.38 12.8 ~ 304 0
3 * iot Eri PM* 02 40 40.0350054 -39 51 19.354141   5.114 4.116     K0IIIb 85 0
4 M 77 GiP 02 42 40.7091669408 -00 00 47.859690204 9.70 9.61 8.87 10.1 9.9 ~ 4424 2
5 NGC 1365 Sy1 03 33 36.458 -36 08 26.37 10.48 10.08 9.63 8.79 9.7 ~ 1686 2
6 ACO S 373 ClG 03 38 30 -35 27.3           ~ 1725 0
7 * alf Hor PM* 04 14 00.1142226166 -42 17 39.726755131 5.97 4.96 3.86 3.00 2.41 K2III 139 0
8 LEDA 17155 Sy2 05 21 01.3994605776 -25 21 45.321827832   15.47 14.75     ~ 475 0
9 * eps Col * 05 31 12.7474803792 -35 28 13.823766588 6.09 5.01 3.87 3.05 2.45 K1II/III 47 0
10 * 28 Hya * 09 25 24.0350848224 -05 07 02.622641052   7.082 5.579     K4/5III 48 0
11 * iot Hya PM* 09 39 51.3614457 -01 08 34.113491 6.68 5.23 3.91 2.92 2.25 K2.5III 171 0
12 ESO 434-40 Sy2 09 47 40.1332188528 -30 56 55.960779696   14.10 13.69 12.44   ~ 524 0
13 Mrk 1239 Sy1 09 52 19.168 -01 36 44.10   14.99 14.39 11.2   ~ 311 0
14 * alf Ant PM* 10 27 09.1006393440 -31 04 04.004901300 7.33 5.70 4.25 3.15 2.36 K3III 75 0
15 NGC 3256 IG 10 27 51.284 -43 54 13.55   11.83 11.33 10.62 11.9 ~ 811 2
16 NGC 3281 Sy2 10 31 52.086 -34 51 13.40   12.62 14.02 11.17   ~ 342 0
17 * del Crt PM* 11 19 20.4475617 -14 46 42.741307 5.66 4.67 3.56 2.73 2.13 G9IIICH0.5 162 0
18 NGC 3783 Sy1 11 39 01.7096819040 -37 44 19.009642992   12.46 13.43 11.33 12.1 ~ 1586 0
19 NGC 4151 Sy1 12 10 32.5759813872 +39 24 21.063527532   12.18 11.48     ~ 3573 2
20 * c Vir RG* 12 20 20.9813922197 +03 18 45.255217001 7.27 6.12 4.96 4.07 3.46 K0.5IIIbFe-0.5 353 0
21 3C 273 BLL 12 29 06.6998257176 +02 03 08.597629980   13.05 14.830 14.11   ~ 5637 1
22 NAME Centaurus A Sy2 13 25 27.61521044 -43 01 08.8050291   8.18 6.84 6.66   ~ 4319 3
23 IC 4329 BiC 13 49 05.314 -30 17 45.20   11.96 11.54 10.31   ~ 184 2
24 ESO 445-50 Sy1 13 49 19.2601801224 -30 18 34.213815504   13.81 13.66 12.18   ~ 770 0
25 Mrk 463E Sy2 13 56 02.886 +18 22 18.84   15.01 14.22     ~ 148 1
26 * pi. Hya PM* 14 06 22.2974865 -26 40 56.502378 5.45 4.41 3.28 2.40 1.85 K2-IIIFe-0.5 136 0
27 * kap Vir PM* 14 12 53.7453840 -10 16 25.333997 7.00 5.53 4.21 3.14 2.39 K2.5IIIFe-0.5 137 0
28 NAME Circinus Galaxy Sy2 14 13 09.906 -65 20 20.47   10.89 9.84 10.6 10.0 ~ 1127 2
29 NGC 5506 AGN 14 13 14.8761010056 -03 12 27.556909272   15.25 14.38     ~ 1061 0
30 NGC 7469 Sy1 23 03 15.674 +08 52 25.28 12.60 13.00 12.34     ~ 2027 3
31 NGC 7582 GiP 23 18 23.621 -42 22 14.06 11.62 10.92 10.62     ~ 872 2
32 * 7 Psc PM* 23 20 20.5830465120 +05 22 52.708387620   6.262 5.069     K1IV 115 0

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2023.01.27-23:04:51