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Mid-Infrared Imaging of 25 Local AGN with VLT-VISIR

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Mid-Infrared Imaging of 25 Local AGN with VLT-VISIR A&A 495, 137–146 (2009) Astronomy DOI: 10.1051/0004-6361:200809878 & c ESO 2009 Astrophysics Mid-infrared imaging of 25 local AGN with VLT-VISIR H. Horst1,2,3,4,W.J.Duschl1,5, P. Gandhi6, and A. Smette4 1 Institut für Theoretische Physik und Astrophysik, Christian-Albrechts-Universität zu Kiel, Leibnizstr. 15, 24098 Kiel, Germany e-mail: [email protected] 2 Zentrum für Astronomie, ITA, Universität Heidelberg, Albert-Ueberle-Str. 2, 69120 Heidelberg, Germany 3 Max-Planck-Institut für Radioastronomie, Auf dem Hügel 69, 53121 Bonn, Germany 4 European Southern Observatory, Casilla 19001, Santiago 19, Chile 5 Steward Observatory, The University of Arizona, 933 N. Cherry Ave, Tucson, AZ 85721, USA 6 RIKEN Cosmic Radiation Lab, 2-1 Hirosawa, Wakoshi Saitama 351-0198, Japan Received 31 March 2008 / Accepted 13 December 2008 ABSTRACT Context. High angular resolution N-band imaging is used to discern the torus of active galactic nuclei (AGN) from its environment in order to allow a comparison of its mid-infrared properties to the expectations of the unified scenario for AGN. Aims. We present VLT-VISIR images of 25 low-redshift AGN of different Seyfert types, as well as N-band SEDs of 20 of them. In addition, we compare our results for 19 of them to Spitzer IRS spectra. Methods. We find that at a resolution of ∼0. 35, all the nuclei of our observed sources are point-like, except for 2 objects whose extension is likely of instrumental origin. For 3 objects, however, we observed additional extended circumnuclear emission, even though our observational strategy was not designed to detect it. Comparison of the VISIR photometry and Spitzer spectrophotometry indicates that the latter is affected by extended emission in at least 7 out of 19 objects and the level of contamination is (0.20 ∼ 0.85) · FIRS. In particular, the 10 μm silicate emission feature seen in the Spitzer spectra of 6 type I AGN, possibly 1 type II AGN and 2 LINERs, also probably originates not solely in the torus but also in extended regions. Results. Our results generally agree with the expectations from the unified scenario, while the relative weakness of the silicate feature supports clumpy torus models. Our VISIR data indicate that, for low-redshift AGN, a large fraction of Spitzer IRS spectra are contaminated by extended emission close to the AGN. Conclusions. Key words. galaxies: active – galaxies: nuclei – galaxies: Seyfert – infrared: galaxies 1. Introduction In two recent publications, Horstetal.(2006, 2008), here- after called Papers I and II, respectively, we investigated the The unification model for active galactic nuclei (AGN) inter- correlation between the mid-IR and hard X-ray luminosities in ff prets the di erent appearance of Seyfert 1 and Seyfert 2 galaxies AGN and its implications for dusty torus models. To this end, ff uniquely as the result of an orientation e ect (Antonucci 1993; we observed 25 local (z < 0.1) AGN with the VISIR (Lagage Barthel 1994; Urry & Padovani 1996). The central engine is con- et al. 2004) instrument at the VLT and found a highly signifi- sidered to be surrounded by an optically and geometrically thick cant correlation between their rest frame 12.3 μmand2−10 keV molecular torus that appears as a grey body, mainly emitting in luminosities. Moreover, we found the luminosity ratio L /L μ MIR X the infrared; the SED peaks around 20 m in terms of energy to be independent of Seyfert type and luminosity, in agreement emitted per unit wavelength. Therefore, one way to study the with the studies by Krabbe et al. (2001), Alonso-Herrero et al. physical properties of the putative torus, is to observe AGN in (2002)andLutz et al. (2004). Our sample has recently been ex- ∼ μ ∼ μ the mid infrared (MIR) regime between 8 mand 30 m. panded to 41 VISIR detections, including many Compton-thick In recent years, this field progressed rapidly thanks to the AGN, by Gandhi et al. (2008). arrival of powerful new instruments, mainly the Spitzer space In the present article, we present the mid-IR properties of telescope on one hand and high-resolution imagers and spec- this sample of objects in more detail. Typically, we achieved a trographs at 10 m-class telescopes (COMICS, LWS/LWIRC, spatial resolution of ∼0. 35 FWHM, corresponding to a resolved Michelle, T-ReCS, VISIR) as well as the interferometric instru- linear size ranging from 6 pc to 510 pc, depending on the dis- ment MIDI on the other hand. Thus, it has become feasible to tance of the objects. Since our main goal was to derive the lumi- compare observations in detail to radiative transfer modelling nosity of the central point source, our imaging is not very deep. of dusty tori (e.g. Schartmann et al. 2005; Hönig et al. 2006; In a few cases, however, we detected and resolved extra-nuclear Fritz et al. 2006) and constrain the geometry of the torus (e.g. emission. Buchanan et al. 2006; Polletta et al. 2007; Treister et al. 2008) For 20 of the presented objects, photometry in different as well as test the applicability of the unified scenario in general N-band filters is available which enables us to reproduce the (Haas et al. 2007). overall shape of the N-band SEDs of these objects. When pos- sible, we compare our photometric data to spectra obtained with Based on ESO observing programmes 075.B-0844(C) and 077.B- the IRS instrument (Houck et al. 2004) aboard Spitzer. While 0137(A). in many cases, Spitzer and VISIR data are in good agreement, in Article published by EDP Sciences 138 H. Horst et al.: Mid-infrared imaging of 25 local AGN with VLT-VISIR others they are not. We will discuss the possible consequences of Table 1. Object names, Sy types, VISIR filters, central wavelengths, such disagreements for the study of AGN tori with Spitzer data. fluxes and resolved scales for all detected sources. References for fluxes −1 −1 Throughout this paper we assume H0 = 73 km s Mpc , are Papers I and II. ΩΛ = 0.72 and Ωm = 0.24 (Spergel et al. 2006). Object Sy type Filter λc [μm] Flux [mJy] Scale [pc] Fairall 9 1.2 SIV 10.49 256.2 ± 5.4 310 2. Observations and data analysis Fairall 9 1.2 NeIIref1 12.27 329.8 ± 18.0 340 Fairall 9 1.2 NeII 12.81 305.7 ± 10.4 340 Two samples of AGN were observed, one between April and NGC 526a 1.9 SIV 10.49 198.6 ± 22.0 115 August 2005 and the other one during the same period in 2006. NGC 526a 1.9 NeIIref1 12.27 275.3 ± 55.0 135 Details on the target selection and observing conditions are given Mrk 590 1.0 SIV 10.49 75.9 ± 20.9 120 in Paper I for the first sample and Paper II for the second sample, Mrk 590 1.0 PAH2 11.25 75.0 ± 2.1 135 respectively. Mrk 590 1.0 NeII 12.81 106.3 ± 13.3 160 We used the standard imaging template of VISIR, with par- NGC 1097 L NeIIref1 12.27 28.2 ± 6.830 allel chopping and nodding and a chop throw of 8.Inorder NGC 3783 1.5 SIV 10.49 568.1 ± 46.265 to get the best possible angular resolution, the small field ob- NGC 3783 1.5 PAH2ref2 11.88 632.2 ± 21.970 jective (0. 075/pixel) was used. Bright AGN were observed in NGC 3783 1.5 NeIIref1 12.27 721.8 ± 67.370 . ± . three filters in order to allow a reconstruction of their spec- NGC 4507 1h SIV 10.49 523 2 24 975 NGC 4507 1h PAH2 11.25 589.5 ± 21.875 tral energy distribution (SED) in the MIR. Due to time con- NGC 4507 1h NeIIref1 12.27 685.0 ± 50.180 straints, faint objects could only be observed in one filter. All NGC 4579 L SIV 10.49 64.2 ± 11.632 observations were executed in service mode with required ob- . ± . NGC 4579 L PAH2ref2 11.88 68 5 13 829 serving conditions of clear sky and 0. 8 seeing or less. The av- NGC 4579 L NeIIref1 12.27 60.7 ± 20.630 erage airmass was 1.15, with no observation being executed at NGC 4593 1.0 SIV 10.49 331.4 ± 28.860 an airmass above 1.3. Science targets and photometric standards NGC 4593 1.0 PAH2ref2 11.88 335.4 ± 26.160 were all observed within 2 h of each other and with a maximum NGC 4593 1.0 NeIIref1 12.27 382.4 ± 73.365 difference in airmass of 0.25. For most observations, however, NGC 4941 2.0 NeIIref1 12.27 81.3 ± 6.030 differences in both time and airmass are much smaller than these IRAS 13197-1627 1h SIV 10.49 527.1 ± 17.1 120 IRAS 13197-1627 1h PAH2 11.25 674.3 ± 35.8 125 values. Some exposures had to be re-executed as the atmospheric . ± . conditions were not within specified constraints. In these cases, IRAS 13197-1627 1h NeIIref1 12.27 875 0 45 8 140 Cen A 2.0 SIV 10.49 642.6 ± 26.66 we only present the data obtained under the best conditions. Cen A 2.0 PAH2 11.25 946.6 ± 29.27 We reduced science and standard star frames using the Cen A 2.0 NeIIref1 12.27 1451 ± 73.17 pipeline written by Eric Pantin (private communication, also see NGC 5135 2.0 NeIIref1 12.27 122.5 ± 12.295 Pantin 2008) for the VISIR consortium.
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