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An Unbiased HI Study of the Gas-Rich Interacting Galaxy Group NGC 3166/9

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An Unbiased HI Study of the Gas-Rich Interacting Galaxy Group NGC 3166/9 Mon. Not. R. Astron. Soc. 427, 2314–2327 (2012) doi:10.1111/j.1365-2966.2012.22115.x Pre-existing dwarfs, tidal knots and a tidal dwarf galaxy: an unbiased H I study of the gas-rich interacting galaxy group NGC 3166/9 K. Lee-Waddell,1 K. Spekkens,1 M. P. Haynes,2 S. Stierwalt,3 J. Chengalur,4 P. Chandra1 and R. Giovanelli2 1Department of Physics, Royal Military College of Canada, PO Box 17000, Station Forces, Kingston, ON K7K 7B4, Canada 2Center for Radiophysics and Space Research, Space Sciences Building, Cornell University, Ithaca, NY 14853, USA 3Spitzer Science Center, California Institute of Technology, 1200 East California Boulevard, Pasadena, CA 91125, USA 4National Centre for Radio Astrophysics, Tata Institute of Fundamental Research, Pune 411 007, India Accepted 2012 September 11. Received 2012 September 10; in original form 2012 April 7 ABSTRACT We present Arecibo Legacy Fast ALFA (ALFALFA) and follow-up Giant Metrewave Radio Telescope (GMRT) H I observations of the gas-rich interacting group NGC 3166/9. The sensi- tive ALFALFA data provide a complete census of H I-bearing systems in the group while the high-resolution GMRT data elucidate their origin, enabling one of the first unbiased physical studies of gas-rich dwarf companions and the subsequent identification of second-generation, tidal dwarf galaxies in a nearby group. The ALFALFA maps reveal an extended H I envelope around the NGC 3166/9 group core, which we mosaic at higher resolution using six GMRT pointings spanning ∼1deg2. A thorough search of the GMRT data cube reveals eight low-mass objects with gas masses ranging from 4 × 107 to 3 × 108 M and total dynamical masses 9 up to 1.4 × 10 M. A comparison of the H I fluxes measured from the GMRT data to those measured in the ALFALFA data suggests that a significant fraction (∼60 per cent) of the H I is smoothly distributed on scales greater than 1 arcmin (∼7 kpc at the NGC 3166/9 distance). We compute stellar masses and star formation rates for the eight low-mass GMRT detections, using ancillary Sloan Digital Sky Survey (SDSS) and Galaxy Evolution Explorer (GALEX) data, and use these values to constrain their origin. Most of the detections are likely to be either pre-existing dwarf irregular galaxies or short-lived, tidally formed knots; however, one candi- date, AGC 208457, is clearly associated with a tidal tail extending below NGC 3166, exhibits a dynamical to gas mass ratio close to unity and has a stellar content and star formation rate that are broadly consistent with both simulated as well as candidate tidal dwarf galaxies from the literature. Our observations therefore strongly suggest that AGC 208457 is a tidal dwarf galaxy. Key words: galaxies: dwarf – galaxies: groups: individual: NGC 3166/9 – galaxies: interac- tions. tain populations of recently formed stars that were produced during 1 INTRODUCTION the interaction event, but they also have older pre-enriched stel- Many present-day galaxies can be found in group environments lar populations (Duc et al. 2000). Overall, the formation of any where tidal interactions within these systems play important roles tidal feature or galaxy greatly constrains the type of interaction and in galactic dynamics (e.g. Tago et al. 2008). Certain interactions in the properties of the original objects involved in the process (Duc gas-rich groups can form tidal bridges and tails as well as second- 2011). In groups, the prevalence of tidal galaxies relative to their generation ‘tidal’ dwarf galaxies (TDGs), which differ from first- pre-existing counterparts probes the mechanisms that drive galaxy generation ‘pre-existing’ dwarfs by their lack of dark matter and evolution in these environments (Bournaud & Duc 2006). higher metallicity content (Hunter, Hunsberger & Roye 2000). Since Although TDGs are frequently produced in galaxy interaction TDGs form from the material from the outer discs of larger galaxies, simulations and over the last two decades several probable candi- they should have total to baryonic mass ratios close to unity (Barnes dates have been identified in ∼20 interacting systems, very few of & Hernquist 1992; Bournaud et al. 2004). Not only do TDGs con- these objects have been widely accepted as authentic (see Weil- bacher et al. 2003; Sheen et al. 2009). Tidally formed knots that assemble along tidal filaments tend to have total masses between 6 8 E-mail: [email protected] 10 and 10 M; however, in order to survive into long-lived dwarf C 2012 The Authors Monthly Notices of the Royal Astronomical Society C 2012 RAS An unbiased H I study of NGC 3166/9 2315 galaxies – with lifetimes >2 Gyr – these objects typically require a total mass ≥108 M (Bournaud & Duc 2006). Models predict that the most probable TDGs are found in the high-density tips of tidal tails where large tidal knots are typically formed (Bournaud et al. 2004). Genuine TDGs should also be self-gravitating (Duc et al. 2007). Nevertheless, even high-resolution studies of the neu- tral hydrogen (H I) dynamics of well-known TDG candidates in the southern tail of NGC 4038/9 failed to prove that the objects are rotating – a clear indicator of self-gravitation – and that they are therefore kinematically distinct from the tidal tail, which has given rise to much debate and speculation about their nature (Hibbard et al. 2001). As can be seen, deciding whether a given object is a tidal dwarf or not is a non-trivial issue and generally requires a host of corroborating observations. Given the properties of (young) TDGs as well as the environ- ments within which they form, H I observations are a reasonable preliminary search tool. H I traces the location of tidally formed features, can indicate regions of potential star formation and has been routinely used to map the gas distribution in and around gas- rich systems (see Freeland, Stilp & Wilcots 2009; Kent et al. 2009; Stierwalt et al. 2009; Borthakur, Yun & Verdes-Montenegro 2010 for recent examples). H I measurements can be used to estimate gas masses and total masses (discussed further in Section 4). With sufficient resolution, the internal structure and dynamics of TDG Figure 1. ALFALFA total H I intensity contours superimposed on an SDSS candidates can also be constrained (Duc et al. 2007). Interferomet- r-band grey-scale image of the region surrounding the NGC 3166/9 group. ric data from instruments such as the Very Large Array (VLA; e.g. The 4 arcmin ALFALFA beam is in the bottom left-hand corner and the crosses indicate the locations of the ALFALFA H I detections that have been Freeland et al. 2009) and the Australia Telescope Compact Array identified using an automated source extractor. The intensity contours are (ATCA; e.g. Pisano et al. 2011) become essential for resolving the N = . , . , . , , , , × 19 −2 at H I (1 125 2 25 4 5 9 15 30 60) 10 atoms cm . Due to the structure of more compact features. The Faint Irregular Galaxies varying noise in the cube, the intensities associated with AGC 5503 and GMRT Survey (FIGGS; Begum et al. 2008) shows that the Giant AGC 204302 (see Table 1) fall below the lowest contour in the moment Metrewave Radio Telescope (GMRT) is also particularly useful in map. surveying gas-rich dwarfs as its fixed antenna configuration allows for maps at different angular resolutions to be produced by tapering as well as a tail-like feature extending below NGC 3166 in the ultra- the data during imaging. violet (UV; discussed in Section 5), indicates previous and ongoing Considerable effort has been devoted to interferometric H I map- interactions within the group. The average distance to NGC 3169, ping of nearby interacting systems in order to search for TDGs (e.g. derived from the Type Ia supernova SN2003cg, is 22.6 Mpc (Wood- Duc et al. 2000; Hibbard et al. 2001; Bournaud et al. 2007). Never- Vasey et al. 2008; Mandel et al. 2009), which is assumed for all theless, none are blind in their approach: only the regions most likely group members throughout this paper. to harbour second-generation objects were studied in detail, thus Recently, the extended H I emission of this group, first observed probing an incomplete view of the dwarf galaxy population in the by Haynes (1981), was mapped at 4 arcmin (30 kpc at the distance groups. By contrast, single-dish surveys such as the H I Parkes All- of NGC 3169) resolution by ALFALFA (Giovanelli et al. 2005; Sky Survey (HIPASS; Koribalski et al. 2004), the Arecibo Legacy Fig. 1). We present the ALFALFA data for the NGC 3166/9 region Fast ALFA survey (ALFALFA; Giovanelli et al. 2005) and those us- in Section 2. Most of the detected H I is located around NGC 3169 ing the Green Bank Telescope (GBT; e.g. Borthakur et al. 2010) can with various features extending outwards; however, the spatial reso- efficiently cover the large sky areas needed to characterize group lution of the ALFALFA data is too low to characterize the structure environments but lack the angular resolution to probe the struc- of individual group members. The high H I content and clear signs ture of individual objects. An unbiased census of TDGs in nearby of interactions in the NGC 3166/9 group make it an ideal candi- groups is therefore enabled by a two-pronged approach: sensitive date for high-resolution follow-up to distinguish first- and second- single-dish observations to locate H I-bearing systems on degree generation objects, which should result in a better understanding of scales and high-resolution interferometric follow-up to elucidate galaxy evolution in groups.
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