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Visual and Near-Infrared Imaging of Ultraluminous Infrared Galaxies: The IRAS 2 Jy Sample

Murphy, T. W., Jr. and Armus, L. and Matthews, K. and Soifer, B. T. and Mazzarella, J. M. and Shupe, D. L. and Strauss, M. A. and Neugebauer, G. (1996) Visual and Near-Infrared Imaging of Ultraluminous Infrared Galaxies: The IRAS 2 Jy Sample. Astronomical Journal, 111 (3). pp. 1025-1052. ISSN 0004-6256. https://resolver.caltech.edu/CaltechAUTHORS:20170213-101148833

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Abstract

New near-infrared and visual images at 2.2 μm and 6550 Å are presented for 46 galaxies having infrared luminosities of L_(IR) > 8.5 x 10^(11) L_⊙, 60 μm flux densities greater than 1.94 Jy, and declinations greater than -35°. These galaxies make up a significant fraction of a complete, northern hemisphere sample of ultraluminous infrared galaxies. Visual and/or near-infrared imaging data now exist for 56 ultraluminous infrared galaxies out to nearly 50 000 km s^(-1). Of these 56 galaxies, 53 (95%) show evidence for current or past interactions. Among these systems, there are a large variety of visual morphologies, including strongly interacting pairs with apparent tidal tails, as well as single, distorted galaxies with close double nuclei. There are three galaxies which, to the limits of the imaging data, do not appear to have suffered a recent interaction or merger. Approximately 47% (25/53) of the interacting systems have double nuclei, with projected nuclear separations ranging from 0.3 to 48 kpc. Seven systems have nuclear separations larger than 10 kpc. If the 53 interacting galaxies are viewed as stages in the evolution of pairs of interacting spiral galaxies to a single, luminous AGN or starburst, the present imaging data can be used to estimate the lifetime of the bright infrared phase. Including only those sample galaxies with morphological evidence for interactions, we calculate a lower and an upper limit to the lifetime of the ultraluminous infrared phase of the sample as a whole to be 2 x 10^8 and 2 x 10^9 yr, respectively. Comparison of these dynamical estimates to models of the mergers of gas-rich galaxies and the rates at which fuel is exhausted by starbursts or AGN suggests the lifetime of the ultraluminous phase lies much closer to the smaller of these two values. Selecting galaxies based upon luminous infrared activity clearly biases the sample towards merging galaxies with small physical separations. However, the existence of pairs with large separations indicates that the ultraluminous phase may in some cases start early during the merger process. Alternatively, these systems may contain unresolved third nuclei responsible for triggering the ultraluminous activity. We briefly compare our results to recent models of merging spiral galaxies.


Item Type:Article
Related URLs:
URLURL TypeDescription
http://dx.doi.org/10.1086/117849DOIArticle
http://adsabs.harvard.edu/full/1996AJ....111.1025MADSArticle
ORCID:
AuthorORCID
Armus, L.0000-0003-3498-2973
Mazzarella, J. M.0000-0002-8204-8619
Shupe, D. L.0000-0003-4401-0430
Strauss, M. A.0000-0002-0106-7755
Additional Information:© 1996 American Astronomical Society. Received 1995 August 7; revised 1995 December 11. We thank the night assistants at the Palomar Observatory, J. Carasco, S. Staples, and J. Moriarity, and the entire staff at the observatory for their assistance in obtaining these data. Discussions with J. C. Mihos and E. S. Phinney were most helpful. Infrared astronomy at Caltech is supported by grants from NASA and the NSF. This research has made use of the NASA/IPAC Extragalactic Database which is operated by the Jet Propulsion Laboratory, Caltech, under contract with NASA.
Group:Infrared Processing and Analysis Center (IPAC)
Funders:
Funding AgencyGrant Number
NASA/JPL/CaltechUNSPECIFIED
NSFUNSPECIFIED
Subject Keywords:Infrared: Galaxies, Galaxies: Active, Galaxies: Kinematics and Dynamics, Galaxies: Interactions
Issue or Number:3
Record Number:CaltechAUTHORS:20170213-101148833
Persistent URL:https://resolver.caltech.edu/CaltechAUTHORS:20170213-101148833
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:74233
Collection:CaltechAUTHORS
Deposited By: Melissa Ray
Deposited On:13 Feb 2017 19:53
Last Modified:03 Oct 2019 16:36

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