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DDO 161 and UGCA 319: an Isolated Pair of Nearby Dwarf Galaxies

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DDO 161 and UGCA 319: an Isolated Pair of Nearby Dwarf Galaxies MNRAS 000, 1–5 (2016) Preprint 27 July 2018 Compiled using MNRAS LATEX style file v3.0 DDO 161 and UGCA 319: an isolated pair of nearby dwarf galaxies I. D. Karachentsev,1⋆ L. N. Makarova,1 R. B. Tully,2 L. Rizzi,3 V. E. Karachentseva4 and E. J. Shaya5 1 Special Astrophysical Observatory of RAS, Nizhnij Arkhyz, KChR, 369167, Russia 2 Institute for Astronomy, University of Hawaii, 2680 Woodlawn Drive, HI 96822, USA 3 W. M. Keck Observatory, 65-1120 Mamalahoa Hwy, Kamuela, HI 96743, USA 4 Main Astronomical Observatory, Academy of Sciences of Ukraine, 27 Akademika Zabolotnoho St, UA-03143 Kyiv, Ukraine 5 Astronomy Department, University of Maryland, College Park, MD 20743, USA 27 July 2018 ABSTRACT We report HST /ACS observations of two nearby gas-rich dwarf galaxies: DDO 161 and UGCA 319. Their distances determined via the Tip of the Red Giant Branch are . +0.29 . ± . 6 03−0.21 Mpc and 5 75 0 18 Mpc, respectively. The galaxies form an isolated pair dynamically well separated from the nearest neighbors: KK176 (7.28 ± 0.29 Mpc) and NGC 5068 (5.16 ± 0.21 Mpc). All four galaxies have a bulk spatial peculiar velocity towards the Virgo cluster of ∼ 158 ± 17kms−1 in the Local Group rest frame and ∼ 330kms−1 with respect to the cluster center. Key words: galaxies: distances and redshifts – galaxies: dwarf – galaxies: stellar content – galaxies: individual: DDO 161, UGCA 319, KK 176, NGC 5068 1 INTRODUCTION rest frame, Karachentsev & Makarov (2008) and Makarov & Karachentsev (2011) clusterized this popu- Tully et al. (2002) drew attention to the existence of a spe- lation into groups of different multiplicity. Their clus- cial category of systems of galaxies containing only galax- tering algorithm took into account the large observed ies of low luminosity, like Magellanic clouds or below. Sub- diversity of galaxies in luminosities. In this sample, sequent accurate measurements of their distances with the Karachentsev & Makarov (2008) noted the unexpected Hubble Space Telescope (HST ) using the Tip of the Red Gi- abundance of binary dwarf galaxies. Makarov & Uklein ant Branch (TRGB) confirmed that dwarf galaxies in these (2012) compiled a list 57 systems in the volume of nests are associated with each other not only on the sky but −1 VLG < 3500 km s formed by two or more dwarf galaxies. also by the spatial distances (Tully et al. 2006). Their clos- A typical size of these MU-groups is ∼ 30 kpc, a typical est example is a quartet of dwarfs: NGC 3109, Sex A, Sex B −1 velocity dispersion is only ∼ 10 km s . At the mean stellar and Antlia, located just beyond the Local Group threshold 8 mass of group of dwarfs about 3 × 10 M , their typical arXiv:1704.07648v1 [astro-ph.GA] 25 Apr 2017 ⊙ at a distance of ∼ 1.4 Mpc. Later, the quartet was trans- virial-to-stellar mass ratio turns out to be ∼ 40. The formed into elongated sextet due to the detection of two authors noted a lack of gap in size and luminosity between ultra-dwarf galaxies: Antlia B and Leo P (McQuinn et al. the MU-groups and associations of dwarfs discussed by 2013; Sand et al. 2015). According to Tully et al. (2006), Tully et al. (2006). However, while a ”crossing time” for associations of dwarfs are characterized by a dimension of − associations of dwarfs is ∼ 9 Gyr, i.e. comparable with the ∼ 400 kpc, a radial velocity dispersion of ∼ 30 km s 1, a age of the universe, the mean crossing time for MU-groups total stellar mass of ∼ 109 M and a virial-to-stellar mass ⊙ is only ∼ 3 Gyr, being typical for dynamically relaxed ratio of ∼ (300 − 1000). Because of low luminosity, associa- systems. tions of dwarfs are detectable predominantly in the nearby volume. As has been noted by Makarov & Uklein (2012), pairs Considering a sample of about 10000 galax- and groups of dwarfs prefer to reside in regions of low ies in the nearby universe with radial velocities spatial density, and their components are usually gas-rich −1 dwarfs. Observing the population of nearby voids in the VLG < 3500 km s respect to the Local Group 21 cm HI line with the Giant Metrewave Radio Telescope, Chengalur & Pustilnik (2013) and Chengalur et al. (2017) ⋆ E-mail: [email protected] found several multiple gas-rich dwarfs of very low metal- c 2016 The Authors 2 I. D. Karachentsev, L. N. Makarova, R. B. Tully, L. Rizzi, V. E. Karachentseva & E. Shaya Table 1. TRGB and distance measurements for the pair compo- Table 2. Global properties of the pair components nents. Parameter DDO 161 UGCA 319 TRGB parameters DDO161 UGCA319 R.A.,Dec.(J2000.0) 130316.8–172523 130214.4–171415 +0.08 F 814W 24.94−0.04 24.84 ± 0.03 Morphological type Sm Ir hF 606W − F 814W i 1.07 ± 0.01 1.01 ± 0.01 BT , mag 13.5 15.1 E(B − V ) 0.070 0.072 Holmberg diameter, arcmin 7.94 1.26 +0.10 −1 (m − M)0 28.90−0.07 28.80 ± 0.07 VLG, kms 543 555 (529) +0.29 −1 D,Mpc 6.03−0.21 5.75 ± 0.18 W50, kms 113 94 (30) −1 log(FHI ), Jy km s 1.88 0.88 (-0.20) m(F UV ) 14.6 17.2 licity. Presumably, a thorough HI-survey of nearby dwarfs Distance, Mpc 6.03 5.75 with the spatial resolution offered by interferometers could MB, mag –16.04 –14.17 significantly extend the existing collection of multiple dwarf log(M∗/M⊙) 8.75 8.01 log(MHI /M⊙) 8.83 7.76 (6.68) galaxies. −1 log(sSFR)F UV , yr –9.80 –10.30 In this Note, we report on measurements of accurate distances to dwarf galaxies DDO 161 = UGCA 320 and Projected separation, arcmin 18.6 − − UGCA 319 with radial velocities 543 km s 1 and 555 km s 1 Projected separation, kpc 32.7 9 Orbital mass,10 M⊙ 5.6 (7.6) respectively, which form a tight pair well separated from ∗ ∗ other neighboring galaxies. Morb/(M1 + M2 ) 8.3 (11.3) Tcross, Gyr 2.7 (2.3) 2 HST OBSERVATIONS AND DATA marked in Fig. 2 by the solid line. The absolute magni- REDUCTION tude of the TRGB in the HST flight system for F606W and F814W using ACS was estimated using the calibration The galaxies DDO 161 and UGCA 319 were observed with from Rizzi et al. (2007): the Hubble Space Telescope (HST ) using Advanced Camera for Surveys (ACS) on February 11 and 14, 2017 (cycle 24 M(F 814W )= −4.06 + 0.20[(F 606W − F 814W ) − 1.23]. proposal GO-14636, PI Karachentsev). Four exposures were The formula defines a zero-point calibration of the TRGB made in a single orbit per galaxy: F606W (broad- band V ), as a function of the stellar population colour, accounting F814W (broad-band I) filters at the same position as well as for variation due to metallicity and age. As a result, we F606W and F814W at a dithered position, about 3 arcsec +0.29 derived the distances: 6.03−0.21 Mpc and 5.75 ± 0.18 Mpc away. The total exposure time per galaxy for each filter was for DDO 161 and UGCA 319 respectively. These measure- 1030 seconds. The F606W images of the galaxies are shown ments assume foreground Galactic extinction, E(B − V ), in Fig. 1. The dimension of the fields is about 3.3 arcmin. according to Schlafly & Finkbeiner (2011). Based on the The photometry of resolved stars in the galaxies were accurate TRGB distance determinations, we conclude that performed with the ACS module of the DOLPHOT package DDO 161 and UGCA 319 are spatially associated each other (http://purcell.as.arizona.edu/dolphot/) for crowded field forming a physical system. The measured distances differ by photometry (Dolphin 2002) using the recommended recipe 280 ± 310 kpc. and parameters. Only stars with photometry of good qual- ity were included in the final compilation, following recom- mendations given in the DOLPHOT User’s Guide. Artificial 3 DISCUSSION stars were inserted and recovered using the same reduction procedures to accurately estimate photometric errors, in- NASA Extragalactic Database (=NED, cluding crowding and blending effects. A large library of arti- http://ned.ipac.caltech.edu) contains 10 distance estimates ficial stars was generated spanning the full range of observed for DDO 161 made by the Tully-Fisher (Tully & Fisher stellar magnitudes and colours to assure that the distribu- 1977) method in its different modifications. The average tion of the recovered photometry is adequately sampled. value among them, 6.1 Mpc, is perfectly consistent with Colour-magnitude diagrams (CMDs) for the detected the TRGB distance 6.03 Mpc measured by us. In contrast stars in DDO 161 and UGCA 319 are shown in Figure 2. In to DDO 161, NED presents for UGCA 319 only a single the case of DDO 161 we present the CMD for the complete distance estimate, 19.7 Mpc, via the infra-red Tully-Fisher galaxy body (left panel) and after excluding some central relation (Sorce et al. 2014) that is in sharp contradiction regions crowded by star formation complexes (middle panel). to our present TRGB measurement. The nature of this The method of deriving the distance from the Tip of the Red discrepancy is caused apparently by confusion of the HI-line Giant Branch (TRGB) magnitude rests on a well understood width of UGCA 319 with the strong HI-flux from the close physical basis (Madore et al.
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