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Alma Observations of Warm Molecular Gas and Cold Dust in Ngc 34∗

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Alma Observations of Warm Molecular Gas and Cold Dust in Ngc 34∗ View metadata, citation and similar papers at core.ac.uk brought to you by CORE provided by Caltech Authors The Astrophysical Journal, 787:48 (10pp), 2014 May 20 doi:10.1088/0004-637X/787/1/48 C 2014. The American Astronomical Society. All rights reserved. Printed in the U.S.A. ALMA OBSERVATIONS OF WARM MOLECULAR GAS AND COLD DUST IN NGC 34∗ C. K. Xu1,C.Cao1,2,3,N.Lu1,Y.Gao4, P. van der Werf5,A.S.Evans6,7, J. M. Mazzarella1, J. Chu8,S.Haan9, T. Diaz-Santos1, R. Meijerink5, Y.-H. Zhao1,4, P. Appleton1, L. Armus1, V. Charmandaris10,11,12,S.Lord1, E. J. Murphy1, D. B. Sanders8, B. Schulz1, and S. Stierwalt6,13 1 Infrared Processing and Analysis Center, MS 100-22, California Institute of Technology, Pasadena, CA 91125, USA 2 School of Space Science and Physics, Shandong University at Weihai, Weihai, Shandong 264209, China; [email protected] 3 Shandong Provincial Key Laboratory of Optical Astronomy and Solar-Terrestrial Environment, Weihai, Shandong 264209, China 4 Purple Mountain Observatory, Chinese Academy of Sciences, 2 West Beijing Road, Nanjing 210008, China 5 Leiden Observatory, Leiden University, P.O. Box 9513, NL-2300 RA Leiden, Netherlands 6 Department of Astronomy, University of Virginia, P.O. Box 400325, Charlottesville, VA 22904, USA 7 National Radio Astronomy Observatory, Charlottesville, VA 22904, USA 8 Institute for Astronomy, University of Hawaii, 2680 Woodlawn Drive, Honolulu, HI 96816, USA 9 CSIRO Astronomy and Space Science, ATNF, P.O. Box 76, Epping 1710, Australia 10 Department of Physics, University of Crete, GR-71003, Heraklion, Greece 11 Institute for Astronomy, Astrophysics, Space Applications & Remote Sensing, National Observatory of Athens, GR-15236, Penteli, Greece 12 Chercheur Associe,´ Observatoire de Paris, F-75014, Paris, France 13 Spitzer Science Center, California Institute of Technology, 1200 E. California Boulevard, Pasadena, CA 91125, USA Received 2013 November 25; accepted 2014 April 3; published 2014 May 2 ABSTRACT We present Atacama Large Millimeter Array (ALMA) Cycle-0 observations of the CO (6–5) line emission (rest- frame frequency = 691.473 GHz) and of the 435 μm dust continuum emission in the nuclear region of NGC 34, a local luminous infrared galaxy at a distance of 84 Mpc (1 = 407 pc) which contains a Seyfert 2 active galactic nucleus (AGN) and a nuclear starburst. The CO emission is well resolved by the ALMA beam (0.26 × 0.23), with −1 an integrated flux of fCO(6–5) = 1004 (±151) Jy km s . Both the morphology and kinematics of the CO (6–5) emission are rather regular, consistent with a compact rotating disk with a size of 200 pc. A significant emission feature is detected on the redshifted wing of the line profile at the frequency of the H13CN (8–7) line, with an integrated flux of 17.7 ± 2.1(random) ± 2.7(systematic) Jy km s−1. However, it cannot be ruled out that the feature is due to an outflow of warm dense gas with a mean velocity of 400 km s−1. The continuum is resolved into an 6.97±0.13 elongated configuration, and the observed flux corresponds to a dust mass of Mdust = 10 M. An unresolved central core (radius 50 pc) contributes 28% of the continuum flux and 19% of the CO (6–5) flux, consistent with insignificant contributions of the AGN to both emissions. Both the CO (6–5) and continuum spatial distributions 4 −2 suggest a very high gas column density (10 M pc ) in the nuclear region at radius 100 pc. Key words: galaxies: active – galaxies: evolution – galaxies: general – galaxies: interactions – galaxies: starburst – galaxies: Seyfert – submillimeter: galaxies 1. INTRODUCTION Sturm et al. 2011; Aalto et al. 2012; Veilleuxet al. 2013; Combes et al. 2013; Cicone et al. 2014). Hence, feedback from merger Luminous infrared galaxies (LIRGs; LIR[8–1000 μm] > induced extreme starbursts and AGNs is the most popular mech- 11 10 L), including ultra-luminous infrared galaxies (ULIRGs; anism for explaining the star formation quenching in massive 12 LIR > 10 L), have a space density exceeding that of optically galaxies that lead to the formation of red-sequence galaxies selected starburst and Seyfert galaxies at comparable bolomet- (Faber et al. 2007; Hopkins et al. 2008a), and (U)LIRGs are the ric luminosity (Soifer et al. 1987). They are an ensemble of best local laboratories for studying these processes. However, single galaxies, galaxy pairs, interacting systems, and advanced due to the enormous dust obscuration in (U)LIRGs (Sanders mergers (Sanders & Mirabel 1996; Wang et al. 2006). Most & Mirabel 1996), it is very difficult to study them using high 11.5 (U)LIRGs of LIR 10 L are advanced mergers (including angular resolution optical/NIR instruments. Observations using merger remnants) harboring extreme starbursts (star formation space FIR/submillimeter observatories, such as Spitzer (Werner −1 rate (SFR) 50 M yr ) and powerful active galactic nu- et al. 2004) and Herschel (Pilbratt et al. 2010), can pene- clei (AGNs; Kim et al. 2002). Toomre (1977) was the first to trate the dust obscuration. However, their angular resolutions suggest that merging can transform spirals into ellipticals, a the- ( a few arcsecs) are not sufficient to resolve the nuclei in ory that has been borne out observationally (Schweizer 1982; most (U)LIRGs. The Atacama Large Millimeter Array (ALMA; Genzel et al. 2001). Strong outflows of neutral and ionized gas Wootten & Thompson 2009) is changing the situation rapidly. were widely detected among (U)LIRGs (Armus et al. 1990; Once completed, submillimeter/millimeter observations using Heckman et al. 1990; Rupke et al. 2005). Recently, massive the ALMA full array (66 antennas) will detect both the line molecular gas outflows have been found in (U)LIRGs with emission of gas and the continuum emission of dust (heated ei- powerful AGNs (Fischer et al. 2010; Feruglio et al. 2013, 2010; ther by starburst or AGN, or both) with an angular resolution of ∗ 0.1 , revealing interplays between gas, starbursts, and AGNs The National Radio Astronomy Observatory is a facility of the National in (U)LIRG nuclei down to linear scales of ∼10 pc in the nearest Science Foundation operated under cooperative agreement by Associated Universities, Inc. systems. 1 The Astrophysical Journal, 787:48 (10pp), 2014 May 20 Xu et al. Table 1 ALMA Observations SB Date Time Config Nant lmax tint Tsys (yyyy/mm/dd) (UTC) (m) (min) (K) (1) (2) (3) (4) (5) (6) (7) (8) X40e374_Xba3 2012/5/20 09:17:15–10:35:34 E 16 375 24.7 850 X40e374_Xd36 2012/5/20 10:48:14–12:06:33 E 16 375 24.7 653 X40e374_Xec9 2012/5/20 12:22:31–13:07:05 E 16 375 9.9 654 X41065b_X334 2012/5/21 09:47:04–11:06:00 E 16 375 24.7 634 X41065b_X4c7 2012/5/21 11:20:00–10:41:09 E 16 375 24.7 528 X4afc39_X43b 2012/8/25 03:30:38–05:01:41 E and C 27 402 24.7 1058 Notes. Column 1: schedule-block number; 2 and 3: observation date and time; 4: configuration; 5: number of antennas; 6: maximum baseline length; 7: on-target integration time; 8: median Tsys. In this paper, we report ALMA Cycle-0 observations (uti- reported here, with an angular resolution of ∼0.25, resolved lizing up to 27 antennas) of the CO (6–5) line (rest-frame the warm and dense gas in the nuclear region of an LIRG with a frequency = 691.473 GHz) emission and of 435 μm dust linear resolution of ∼100 pc for the first time. We aim to answer continuum emission in the nuclear region of NGC 34, a local the following questions with these observations: (1) how is the 11.49 LIRG (LIR = 10 L; Armus et al. 2009) containing an Sy2 warm dense molecular gas distributed in the inner most region AGN and a nuclear starburst (see Schweizer & Seitzer 2007 for of NGC 34? (2) How is the gas related to the starburst and the an overview). With an excitation temperature of Tex = 116.2K AGN, respectively? (3) Is the dust emission dominated by an 5 −3 and a critical density of ncrit = 2.9 × 10 cm (Carilli & extended component, or by an unresolved compact component? Walter 2013), the CO (6–5) line probes the warm and dense gas (4) Is there evidence for a molecular outflow? Comparing with that is much more closely related to the star formation activities the extensive literature on NGC 34 (a late stage major-merger; than the cold and lower density gas probed by low J CO lines Mazzarella & Boroson 1993; Schweizer & Seitzer 2007) and (e.g., CO (1–0) and CO (2–1)) commonly studied in the litera- with high-resolution simulations (Hopkins et al. 2013), our ture. Among the complete sample of 202 LIRGs of the Great Ob- results shed new light on how various activities and their servatories All-sky LIRG Survey (GOALS; Armus et al. 2009), feedback set the stage for a major-merger remnant to become a which were selected from the IRAS Revised Bright Galaxy Sam- red-and-dead elliptical galaxy (Zubovas & King 2012). ple (Sanders et al. 2003), NGC 34 (also known as NGC 17, Mrk 938, and IRAS F00085-1223) was chosen for early ALMA ob- 2. OBSERVATIONS servations because of the following features. (1) Among LIRGs −1 that have the CO (6–5) line flux fCO(6–5) 1000 Jy km s Observations of the CO (6–5) line emission and 435 μm observed in the Herschel SPIRE Fourier Transform Spectrom- dust continuum emission in the nuclear region of NGC 34 eter (FTS) survey of GOALS galaxies (angular resolution: were carried out using the Band 9 receivers of ALMA in ∼30; P.
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