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HI and CO observations of Arp 104: a spiral-elliptical interacting pair

Cullen, H. and Alexander, P. and Green, D. A. and Sheth, K. (2007) HI and CO observations of Arp 104: a spiral-elliptical interacting pair. Monthly Notices of the Royal Astronomical Society, 376 (1). pp. 98-112. ISSN 0035-8711. doi:10.1111/j.1365-2966.2007.11506.x.

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We present data probing the spatial and kinematical distribution of both the atomic (H i) and molecular (CO) gas in NGC 5218, the late-type barred spiral galaxy in the spiral–elliptical interacting pair, Arp 104. We consider these data in conjunction with far-infrared and radio-continuum data, and N-body simulations, to study the galaxies interactions, and the star formation properties of NGC 5218. We use these data to assess the importance of the bar and tidal interaction on the evolution of NGC 5218, and the extent to which the tidal interaction may have been important in triggering the bar. The molecular gas distribution of NGC 5218 appears to have been strongly affected by the bar; the distribution is centrally condensed with a very large surface density in the central region. The N-body simulations indicate a time-scale since perigalacticon of ∼3 × 10^8 yr, which is consistent with the interaction having triggered or enhanced the bar potential in NGC 5218, leading to inflow and the large central molecular gas density observed. Whilst NGC 5218 appears to be undergoing active star formation, its star formation efficiency is comparable to a ‘normal’ SBb galaxy. We propose that this system may be on the brink of a more active phase of star formation.

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Sheth, K.0000-0002-5496-4118
Additional Information:© 2007 The Authors. Journal compilation © 2007 RAS. Accepted 2006 December 21. Received 2006 December 20; in original form 2006 September 11. The James Clerk Maxwell Telescope is operated by The Joint Astronomy Centre on behalf of the Particle Physics and Astronomy Research Council of the United Kingdom, the Netherlands Organization for Scientific Research, and the National Research Council of Canada. We thank the staff of the GMRT that made these observations possible. The GMRT is run by the National Centre for Radio Astrophysics of the Tata Institute of Fundamental Research. The NRAO is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. We thank the staff of the OVRO interferometer. This research has made use of the NED which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. Funding for the SDSS and SDSS-II has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, the US Department of Energy, the National Aeronautics and Space Administration, the Japanese Monbukagakusho, the Max Planck Society, and the Higher Education Funding Council for England. The SDSS web site is The SDSS is managed by the Astrophysical Research Consortium for the Participating Institutions. The Participating Institutions are the American Museum of Natural History, Astrophysical Institute Potsdam, University of Basel, Cambridge University, Case Western Reserve University, University of Chicago, Drexel University, Fermilab, the Institute for Advanced Study, the Japan Participation Group, Johns Hopkins University, the Joint Institute for Nuclear Astrophysics, the Kavli Institute for Particle Astrophysics and Cosmology, the Korean Scientist Group, the Chinese Academy of Sciences (LAMOST), Los Alamos National Laboratory, the Max-Planck-Institute for Astronomy (MPIA), the Max-Planck-Institute for Astrophysics (MPA), New Mexico State University, Ohio State University, University of Pittsburgh, University of Portsmouth, Princeton University, the United States Naval Observatory, and the University of Washington. The Digitized Sky Surveys were produced at the Space Telescope Science Institute under US Government grant NAG W-2166. The images of these surveys are based on photographic data obtained using the Oschin Schmidt Telescope on Palomar Mountain and the UK Schmidt Telescope. The plates were processed into the present compressed digital form with the permission of these institutions. The Second Palomar Observatory Sky Survey (POSS-II) was made by the California Institute of Technology with funds from the National Science Foundation, the National Geographic Society, the Sloan Foundation, the Samuel Oschin Foundation, and the Eastman Kodak Corporation. This publication makes use of data products from the 2MASS, which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology, funded by the National Aeronautics and Space Administration and the National Science Foundation. HC acknowledges receipt of a PPARC studentship.
Group:Infrared Processing and Analysis Center (IPAC)
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Particle Physics and Astronomy Research Council (PPARC)UNSPECIFIED
Nederlandse Organisatie voor Wetenschappelijk Onderzoek (NWO)UNSPECIFIED
National Research Council of CanadaUNSPECIFIED
Alfred P. Sloan FoundationUNSPECIFIED
Department of Energy (DOE)UNSPECIFIED
National Geographic SocietyUNSPECIFIED
Samuel Oschin FoundationUNSPECIFIED
Eastman Kodak CorporationUNSPECIFIED
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Record Number:CaltechAUTHORS:20170408-144339571
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Official Citation:H. Cullen, P. Alexander, D. A. Green, K. Sheth; H i and CO observations of Arp 104: a spiral–elliptical interacting pair. Mon Not R Astron Soc 2007; 376 (1): 98-112. doi: 10.1111/j.1365-2966.2007.11506.x
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:75997
Deposited By: 1Science Import
Deposited On:02 May 2017 20:36
Last Modified:15 Nov 2021 16:56

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