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Large-scale star formation triggering in the low-mass ARP 82 system: A nearby example of galaxy downsizing based on UV/optical/mid-IR imaging

Hancock, Mark and Smith, Beverly J. and Struck, Curtis and Giroux, Mark L. and Appleton, Philip N. and Charmandaris, Vassilis and Reach, William T. (2007) Large-scale star formation triggering in the low-mass ARP 82 system: A nearby example of galaxy downsizing based on UV/optical/mid-IR imaging. Astronomical Journal, 133 (2). pp. 676-693. ISSN 0004-6256. doi:10.1086/510241. https://resolver.caltech.edu/CaltechAUTHORS:HANaj07

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Abstract

As part of our Spitzer Spirals, Bridges, and Tails project to help understand the effects of galaxy interactions on star formation, we analyze Galaxy Evolution Explorer UV, Southeastern Association for Research in Astronomy optical, and Spitzer IR images of the interacting galaxy pair Arp 82 (NGC 2535/6) and compare to a numerical simulation of the interaction. We investigate the multiwavelength properties of several individual star-forming complexes (clumps). Using optical and UV colors, EW(Hα), and population synthesis models we constrain the ages of the clumps and find that the median clump age is ~9 Myr. The clumps have masses ranging from a few; x 10^6 to 10^9 M☉. In general, the clumps in the tidal features have ages similar to those in the spiral region, but are less massive. The clumps provide 33%, 36%, and 70% of the far-UV, 8.0 µm, and 24 µm emission, respectively. The 8 and 24 µm luminosities are used to estimate the far-IR luminosities and the star formation rates of the clumps. The total clump star formation rate is ~2.0 ± 0.8M☉yr^-1, while the entire Arp 82 system is forming stars at a rate of ~4.9 ± 2.0 M☉ yr^-1. We find, for the first time, stars in the H I arc to the southeast of the NGC 2535 disk. Population synthesis models indicate that all of the observed populations have young to intermediate ages. We conclude that, although the gas disks and some old stars may have formed early on, the progenitors may have been of late-type or low surface brightness, and the evolution of these galaxies seems to have halted until the recent encounter.


Item Type:Article
Related URLs:
URLURL TypeDescription
http://dx.doi.org/10.1086/510241DOIArticle
ORCID:
AuthorORCID
Struck, Curtis0000-0002-6490-2156
Appleton, Philip N.0000-0002-7607-8766
Charmandaris, Vassilis0000-0002-2688-1956
Reach, William T.0000-0001-8362-4094
Additional Information:© 2007 The American Astronomical Society. Received 2006 August 3; accepted 2006 October 12. The authors thank the anonymous referee for comments and suggestions. This work is based in part on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with NASA. GALEX is a NASA Small Explorer mission, developed in cooperation with the Centre National d’Etudes Spatiales of France and the Korean Ministry of Science and Technology. This research was supported by NASA Spitzer grant 1263924, NSF grant AST 00-97616, NASA LTSA grant NAG5- 13079, and GALEX grant GALEXGI04-0000-0026. This work has made use of the NASA/ IPAC Extragalactic Database, which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with NASA.
Group:Infrared Processing and Analysis Center (IPAC)
Funders:
Funding AgencyGrant Number
NASA1263924
NSFAST 00-97616
NASANAG5-13079
NASAGALEXGI04-0000-0026
Subject Keywords:galaxies: individual (Arp 82); galaxies: interactions; galaxies: starburst; methods: numerical
Issue or Number:2
DOI:10.1086/510241
Record Number:CaltechAUTHORS:HANaj07
Persistent URL:https://resolver.caltech.edu/CaltechAUTHORS:HANaj07
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:13427
Collection:CaltechAUTHORS
Deposited By: Tony Diaz
Deposited On:01 Jun 2009 17:18
Last Modified:08 Nov 2021 22:37

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