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Prevalence of Tidal Interactions Among Local Seyfert Galaxies

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Prevalence of Tidal Interactions Among Local Seyfert Galaxies To be submitted to the Astrophysical Journal Preprint typeset using LATEX style emulateapj v. 04/21/05 PREVALENCE OF TIDAL INTERACTIONS AMONG LOCAL SEYFERT GALAXIES Cheng-Yu Kuo1,3 Institute of Astronomy & Astrophysics, Academia Sinica, PO Box 23-141, Taipei 10617, Taiwan Department of Astronomy, University of Virginia, Charlottesville, VA 22904 Jeremy Lim Institute of Astronomy & Astrophysics, Academia Sinica, PO Box 23-141, Taipei 10617, Taiwan Ya-Wen Tang1,2 Institute of Astronomy & Astrophysics, Academia Sinica, PO Box 23-141, Taipei 10617, Taiwan Department of Physics, National Taiwan University, No. 1, Sec. 4, Roosevelt Rd., Taipei 106, Taiwan and Paul T. P. Ho1,4 Institute of Astronomy & Astrophysics, Academia Sinica, PO Box 23-141, Taipei 10617, Taiwan Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138 To be submitted to the Astrophysical Journal ABSTRACT No mechanisms have hitherto been conclusively demonstrated to be responsible for initiating optically-luminous nuclear (Seyfert) activity in local disk galaxies. Only a small minority of such galax- ies are visibly disturbed in optical starlight, with the observed disturbances being at best marginally stronger than those found in matched samples of inactive galaxies. Here, we report the first system- atic study of an optically-selected sample of twenty-three active galaxies in atomic hydrogen (HI) gas, which is the most sensitive and enduring tracer known of tidal interactions. Eighteen of these galaxies are (generally) classified as Seyferts, with over half (and perhaps all) having [OIII] luminosities within two orders of magnitude of Quasi-Stellar Objects. Only ∼28% of these Seyfert galaxies are visibly dis- turbed in optical DSS2 images. By contrast, ∼94% of the same galaxies are disturbed in HI, in nearly all cases not just spatially but also kinematically on galactic (& 20 kpc) scales. In at least ∼67% and perhaps up to ∼94% of cases, the observed HI disturbances can be traced to tidal interactions with neighboring galaxies detected also in HI. The majority of these neighboring galaxies have projected −1 separations of . 100 kpc and differ in radial velocities by . 100 km s from their respective Seyfert galaxies, and many have optical luminosities ranging from the Small to Large Magellanic Clouds. In a companion paper, we show that only ∼15% of a matched control sample of inactive galaxies display comparable HI disturbances. Our results suggest that: i) most Seyfert galaxies (with high nuclear luminosities) have experienced tidal interactions in the recent past; ii) in most cases, these tidal interactions are responsible for initiating events that lead to their nuclear activity. Subject headings: galaxies: active | galaxies: Seyfert | galaxies: interactions | galaxies: structure | galaxies: ISM 1. INTRODUCTION lifetimes of ∼108 yrs, the total amount of matter required 5 7 to feed their activity is therefore ∼10 {10 M . The ori- arXiv:0802.4205v2 [astro-ph] 4 Mar 2008 Active Galactic Nuclei (AGNs) are believed to be the luminous visible evidence for the vigorous accretion of gin or source of this material, and how this material is gas onto a central SuperMassive Black Hole (SMBH). brought into the sphere of influence of the central SMBH, In the case of Quasi-Stellar Objects (QSOs), adopting is one of the longstanding unresolved problems in AGN the convenient (but arbitrary) convention that QSOs research. have absolute B-band (nonstellar) nuclear magnitudes Many mechanisms for providing fuel to the central SMBHs of active galaxies have been proposed (e.g., for MB < −23 (V´eron-Cetty & V´eron,1998), the required mass-accretion rate, assuming a 10% efficiency for the a recent brief review, see Martini, 2004). This is par- conversion of infalling matter into radiation (e.g., Nor- ticularly true at relatively low accretion rates, where −1 stellar disruptions due to close encounters with the cen- man & Silk, 1983), is at least ∼0:1 M yr . Lower- luminosity AGNs have correspondingly smaller mass- tral SMBH, dynamical friction on molecular clouds, stel- accretion rates, with those described in this paper having lar winds from massive stars or mass loss from evolved mass-accretion rates ranging down to about two orders stars (e.g., Norman & Scoville, 1988), or turbulence in of magnitude lower (x2). If the AGNs studied here have the interstellar medium (e.g., review by Wada, 2004), are among the proposed hypotheses. At higher accretion Electronic address: [email protected] rates, non-axisymmetric gravitational potentials such as Electronic address: [email protected] galactic bars (e.g., review by Combes, 2004) or gravi- Electronic address: [email protected] Electronic address: [email protected] tational interactions with neighboring galaxies (e.g., re- 2 Kuo et al. view by Schmitt, 2004) may be needed to drive suffi- Searches for an excess of Seyfert galaxies among (ap- cient quantities of gas inwards to fuel the AGN. At even parently) interacting galaxies compared with matched higher accretion rates, corresponding perhaps to that in samples of normal or apparently isolated spiral galax- QSOs, cannibalisms of gas-rich galaxies (minor mergers) ies have yielded similarly ambiguous if not contradictory or mergers between two gas-rich galaxies (major mergers) results. Dahari (1985) find only a marginal excess of may be necessary to carry sufficient fuel to the AGN. Seyfert galaxies among interacting spiral galaxies, but a Because of their more accessible spatial scales, most clear excess when the sample is restricted to just strongly observational studies to date have focussed on whether interacting spiral galaxies. Keel et al. (1985) also find galactic bars or galaxy-galaxy interactions are responsi- Seyfert galaxies more frequently in interacting compared ble for triggering AGNs (in disk galaxies). Nearly all with isolated spiral galaxies, but by contrast with Dahari such studies have involved optically-selected samples of (1985) find a smaller excess in the most disrupted sys- Seyfert galaxies, which make up only a very small frac- tems. On the other hand, Bushouse (1986) find a smaller tion (roughly 1%) of relatively bright field galaxies (e.g., fraction of Seyfert galaxies among violently interacting Huchra & Burg, 1992; Stepanian, 1994). Seyfert galaxies than isolated spiral galaxies. are preferentially found among early-tpe spiral galaxies, Despite the conflicting results, examinations of opti- and exhibit very broad emission lines (from their nuclei) cal images do reveal that the fraction of Seyfert galaxies compared with their inactive counterparts. They are fur- that are visibly (or apparently) interacting in the opti- ther divided into different classes depending on the rel- cal is relatively small. Indeed, even in observations with ative intensity of their broader (∼1000{15000 km s−1) the Hubble Space Telescope, the vast majority of local component, which is dominated by permitted lines, to Seyfert galaxies (Malkan, Gorjian, & Tam, 1998), as well their narrower component (∼200{2000 km s−1), which as QSO host galaxies at redshifts as high as z ≈ 0:3 (e.g., is dominated by forbidden lines. At the two extremes lie Bahcall et al., 1997; Boyce et al., 1998), do not appear Seyfert 1 galaxies, which have a relatively strong broad to be visibly disturbed in the optical. Apart from their component, and Seyfert 2 galaxies, which have a de- nuclear activity, local Seyfert galaxies appear to other- tectable narrow component only (in unpolarized light). wise resemble the general population of inactive, prefer- Searches for an excess of bars in Seyfert compared entially early-type spiral, galaxies. de Robertis, Hayhoe with inactive galaxies have yielded either null or at best & Yee (1998) find at best a marginal difference in light weakly suggestive results. For example, neither Ho, asymmetries between Seyfert and inactive galaxies; us- Filippenko, & Sargent (1997) nor Mulchaey & Regan ing the same sample but a more sophisticated analysis, (1997) found an excess of large-scale (& 1 kpc) bars be- Virani, de Robertis, & VanDalfsen (2000) find no differ- tween Seyfert and inactive galaxies, but Knapen, Shlos- ences. On the other hand, Hunt & Malkan (2004) find man, & Peletier (2000) found a marginal excess of such that 30% ± 9% of Seyfert 1 (and a comparable fraction bars amounting to 79% ± 8% in Seyfert compared with of LINERs and HII) and 63% ± 7% of Seyfert 2 galaxies 59% ± 9% in inactive galaxies. Both Regan & Mulchaey exhibit isophotal twists compared with just 6% ± 4% of (1999) and Martini & Pogge (1999) found that only a a matched sample of inactive galaxies. small fraction of Seyfert galaxies in their sample exhibit With little direct evidence for (more frequent) galaxy- small-scale (. 1 kpc) bars, and suggested that such bars galaxy interactions, studies have turned to whether cannot therefore be the primary mechanism for fueling Seyfert galaxies more frequently exhibit projected neigh- Seyfert activity. On the other hand, Laine et al. (2002) boring galaxies by comparison with matched samples of found that Seyfert galaxies have an excess or at least inactive galaxies (e.g., summary in Schmitt, 2004). Such equal fraction of bars at practically all length scales (from an excess has been found in some studies (e.g., Stauf- tens of parsecs to tens of kiloparsecs) compared with fer, 1982; Dahari, 1984; Rafanelli et al., 1995; Dultzin- inactive galaxies; taken together, 73% ± 6% of Seyfert Hacyan et al., 1999; Koulouridis et al., 2006), but
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