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


C.D.S. - SIMBAD4 rel 1.7 - 2021.03.05CET12:18:21

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 - 2021
#notes
1 * del Phe PM* 01 31 15.1047497 -49 04 21.730837   4.918 3.935     G8.5IIIb 114 0
2 M 77 GiP 02 42 40.771 -00 00 47.84 9.70 9.61 8.87 10.1 9.9 ~ 4180 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+1 136 0
4 2MASX J05580206-3820043 Sy1 05 58 02.0566732230 -38 20 04.453517461   16.05 14.98 11.6   ~ 207 1
5 * eta Col * 05 59 08.8051933 -42 48 54.482180 6.18 5.10 3.96 3.14 2.56 G8/K1II 67 0
6 HD 41047 * 06 01 16.2976972757 -33 54 42.602815732   7.102 5.524     K5III 30 0
7 HD 75929 * 08 49 39.6008874808 -63 10 55.037838057   8.21 7.13     K0III 8 0
8 * bet Car PM* 09 13 11.97746 -69 43 01.9473 1.72 1.69 1.69 1.63 1.61 A1III- 215 0
9 [VV96] J091609.5-621929 Sy1 09 16 09.3662174299 -62 19 29.559790552   12.51 12.26 11.5   ~ 110 0
10 V* GZ Vel LP* 10 19 36.7507384 -55 01 45.502292   6.146 4.543     K2.5II 53 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 225 0
12 * nu. UMa * 11 18 28.7366424 +33 05 39.510697 6.44 4.89 3.49 2.43 1.73 K3-III: 192 0
13 * eps Crt * 11 24 36.5904786153 -10 51 33.557849078   6.338 4.802     K4III 86 0
14 HD 100074 * 11 30 43.9152853312 -39 14 07.746893098   8.22 7.24     K0III 11 0
15 * ksi Hya ** 11 33 00.1150559 -31 51 27.443449 5.17 4.47 3.54 2.84 2.36 G7IIIb 237 0
16 HD 100586 * 11 34 21.3823783511 -36 12 16.414159009   8.71 7.41     K1III 7 0
17 NGC 3783 Sy1 11 39 01.7095761008 -37 44 19.008597647   12.46 13.43 11.33 12.1 ~ 1500 0
18 * 26 Crt * 11 41 43.9467327788 -32 29 57.843983672   6.675 5.200     K5III 33 0
19 NGC 4151 Sy1 12 10 32.5771747733 +39 24 21.057727323   12.18 11.48     ~ 3436 2
20 HD 107341 PM* 12 20 13.4992088486 +37 54 07.683745390   7.67 6.68     K0IIIb 36 0
21 HD 107485 * 12 21 04.0823926920 +38 01 25.772487186   8.45 7.47     G7II-III 17 0
22 HD 110392 * 12 41 26.9626801314 +40 34 45.601168481   8.53 7.60     K0III 19 0
23 HD 112213 V* 12 55 19.4331534012 -42 54 56.646116797   7.093 5.445     M0III 43 0
24 ESO 323-77 Sy2 13 06 26.1213873662 -40 24 52.594127368   13.58 13.42 12.01   ~ 199 0
25 * 41 Com PM* 13 07 10.7300255 +27 37 29.058512 8.14 6.22 4.69 3.64 2.83 K5-III 145 0
26 NAME Centaurus A Sy2 13 25 27.61509104 -43 01 08.8056025   8.18 6.84 6.66   ~ 4077 3
27 2RE J1337+244 Sy1 13 37 18.7198121987 +24 23 03.320690345     15.0     ~ 365 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 109 0
29 V* DX Boo LP* 14 28 46.0298426081 +25 51 13.969007280   8.233 6.698     MIII 26 0
30 * chi Sco * 16 13 50.9069224118 -11 50 15.905491351   6.615 5.239     K3III 63 0

    Equat.    Gal    SGal    Ecl

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2021.03.05-12:18:21

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