2011A&A...536A..78K


Query : 2011A&A...536A..78K

2011A&A...536A..78K - Astronomy and Astrophysics, volume 536A, 78-78 (2011/12-1)

Mapping the radial structure of AGN tori.

KISHIMOTO M., HOENIG S.F., ANTONUCCI R., MILLOUR F., TRISTRAM K.R.W. and WEIGELT G.

Abstract (from CDS):

We present mid-IR interferometric observations of six type 1 AGNs at multiple baseline lengths ranging from 27m to 130m, reaching high angular resolutions up to λ/B∼0.02arcsec. For two of the targets, we have simultaneous near-IR interferometric measurements as well, taken within a week. We find that all the objects are partially resolved at long baselines in these IR wavelengths. The multiple-baseline data directly probe the radial distribution of the material on sub-pc scales. We show that for our sample, which is small but spans over ∼2.5 orders of magnitudes in the UV/optical luminosity L of the central engine, the radial distribution clearly and systematically changes with luminosity. The brightness distribution at a given mid-IR wavelength seems to be rather well described by a power law, which makes a simple Gaussian or ring size estimation quite inadequate. In this case, a half-light radius R1/2 can be used as a representative size. We show that the higher luminosity objects become more compact in normalized half-light radii R1/2/Rin in the mid-IR, where Rin is the dust sublimation radius empirically given by the L1/2 fit of the near-IR reverberation radii. This means that, contrary to previous studies, the physical mid-IR emission size (e.g. in pc) is not proportional to L1/2, but increases with L much more slowly. With our current datasets, we find that R1/2∝L0.21±0.05 at 8.5 µm, and R1/2 nearly constant at 13 µm. The derived size information also seems to correlate with the properties of the total flux spectrum, in particular the smaller R1/2/Rin objects having bluer mid-IR spectral shape. We use a power-law temperature/density gradient model as a reference, and infer that the radial surface density distribution of the heated dust grains at a radius r changes from a steep ∼r–1 structure in high luminosity objects to a shallower ∼r0 structure in those of lower luminosity. The inward dust temperature distribution does not seem to smoothly reach the sublimation temperature - on the innermost scale of ∼Rin, a relatively low temperature core seems to co-exist with a slightly distinct brightness concentration emitting roughly at the sublimation temperature.

Abstract Copyright:

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

Simbad objects: 30

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Number of rows : 30
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2022
#notes
1 * del Phe PM* 01 31 15.1047497 -49 04 21.730837   4.918 3.935     G8.5IIIb 119 0
2 M 77 GiP 02 42 40.7091669408 -00 00 47.859690204 9.70 9.61 8.87 10.1 9.9 ~ 4324 2
3 * bet Col PM* 05 50 57.5921991 -35 46 05.915211 5.49 4.28 3.12 2.27 1.69 K1III_CN+1 141 0
4 LEDA 75476 Sy1 05 58 02.0566707456 -38 20 04.452162288   16.05 14.98 11.6   ~ 213 1
5 * eta Col * 05 59 08.8051933 -42 48 54.482180 6.18 5.10 3.96 3.14 2.56 G8/K1II 72 0
6 HD 41047 * 06 01 16.2976481208 -33 54 42.608011716   7.102 5.524     K5III 33 0
7 HD 75929 * 08 49 39.5969966664 -63 10 54.968374596   8.21 7.13     K0III 9 0
8 * bet Car PM* 09 13 11.97746 -69 43 01.9473 1.72 1.69 1.69 1.63 1.61 A1III- 218 0
9 [VV96] J091609.5-621929 Sy1 09 16 09.3662148312 -62 19 29.562130128   12.51 12.26 11.5   ~ 122 0
10 V* GZ Vel LP* 10 19 36.7507384 -55 01 45.502292   6.146 4.543     K2.5II 55 0
11 * 46 LMi PM* 10 53 18.7048735 +34 12 53.537492 5.79 4.87 3.83 3.00 2.46 K0+III-IV 230 0
12 * nu. UMa * 11 18 28.7366424 +33 05 39.510697 6.44 4.89 3.49 2.43 1.73 K3-III: 196 0
13 * eps Crt * 11 24 36.5912121144 -10 51 33.575503752   6.338 4.802     K4III 87 0
14 HD 100074 * 11 30 43.9148057856 -39 14 07.748846916   8.22 7.24     K0III 12 0
15 * ksi Hya ** 11 33 00.1150559 -31 51 27.443449 5.17 4.47 3.54 2.84 2.36 G7IIIb 247 0
16 HD 100586 * 11 34 21.3824702400 -36 12 16.416536112   8.71 7.41     K1III 8 0
17 NGC 3783 Sy1 11 39 01.7096819040 -37 44 19.009642992   12.46 13.43 11.33 12.1 ~ 1551 0
18 * 26 Crt * 11 41 43.9473963672 -32 29 57.851230272   6.675 5.200     K5III 35 0
19 NGC 4151 Sy1 12 10 32.5759813872 +39 24 21.063527532   12.18 11.48     ~ 3520 2
20 HD 107341 PM* 12 20 13.4992383648 +37 54 07.679493144   7.67 6.68     K0IIIb 37 0
21 HD 107485 * 12 21 04.0821230400 +38 01 25.769754480   8.45 7.47     G7II-III 18 0
22 HD 110392 * 12 41 26.9626890096 +40 34 45.598296360   8.53 7.60     K0III 20 0
23 HD 112213 V* 12 55 19.4317990920 -42 54 56.639555352   7.093 5.445     M0III 44 0
24 ESO 323-77 Sy2 13 06 26.1214861728 -40 24 52.595604396   13.58 13.42 12.01   ~ 212 0
25 * 41 Com PM* 13 07 10.7299222671 +27 37 29.055438610 8.14 6.22 4.69 3.64 2.83 K5-III 150 0
26 NAME Centaurus A Sy2 13 25 27.6039817176 -43 01 09.493008456   8.18 6.84 6.66   ~ 4231 3
27 LEDA 101275 Sy1 13 37 18.7199358192 +24 23 03.319883484     15.0     ~ 373 0
28 V* AW CVn LP? 13 51 47.4753428 +34 26 39.261252 8.36 6.40 4.74 3.21 1.93 M3-IIIa 112 0
29 V* DX Boo LP* 14 28 46.0294486320 +25 51 13.981814460   8.233 6.698     MIII 27 0
30 * chi Sco * 16 13 50.9062585128 -11 50 15.892301544   6.615 5.239     K3III 64 0

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2022.05.28-23:11:27

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