Boquien, M. and Duc, P. A. and Wu, Y. and Charmandaris, V. and Lisenfeld, U. and Braine, J. and Brinks, E. and Iglesias-Páramo, J. and Xu, C. K. (2009) Collisional debris as laboratories to study star formation. Astronomical Journal, 137 (6). pp. 4561-4576. ISSN 0004-6256 http://resolver.caltech.edu/CaltechAUTHORS:20090707-114648129
- Published Version
See Usage Policy.
Use this Persistent URL to link to this item: http://resolver.caltech.edu/CaltechAUTHORS:20090707-114648129
In this paper we address the question of whether star formation (SF) is driven by local processes or the large-scale environment. To do so, we investigate SF in collisional debris where the gravitational potential well and velocity gradients are shallower and compare our results with previous work on SF in noninteracting spiral and dwarf galaxies. We have performed multiwavelength spectroscopic and imaging observations (from the far-ultraviolet to the mid-infrared) of six interacting systems, identifying a total of 60 star-forming regions in their collision debris. Our analysis indicates that in these regions (1) the emission of the dust is at the expected level for their luminosity and metallicity, (2) the usual tracers of SFR display the typical trend and scatter found in classical star-forming regions, and (3) the extinction and metallicity are not the main parameters governing the scatter in the properties of intergalactic star-forming regions; age effects and variations in the number of stellar populations seem to play an important role. Our work suggests that local properties such as column density and dust content, rather than the large-scale environment seem to drive SF. This means that intergalactic star-forming regions can be used as a reliable tool to study SF.
|Additional Information:||© 2009 American Astronomical Society. Print publication: Issue 6 (2009 June) Received 2008 November 18; accepted for publication 2009 March 18; published 2009 April 15. This research has made use of the NASA/IPAC Extragalactic Database (NED) which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. GALEX is a NASA Small Explorer, launched in 2003 April. We gratefully acknowledgeNASA’s support of the construction, operation, and science analysis for the GALEX mission, developed in cooperation with the Centre national d’´etudes spatiales, France, and the Korean Ministry of Science and Technology. Based on observations obtained at the Canada-France-Hawaii Telescope (CFHT) which is operated by the National Research Council of Canada, the Institut National des Sciences de l’Univers of the Centre National de la Recherche Scientifique of France, and the University of Hawaii. M.B. acknowledges support by NASA-ADP grant NNX07AN90G and D. Calzetti for fruitful discussions. U.L. acknowledges financial support by the Spanish Science Ministry under grant AYA2007-67625-C02-02 and by the Junta de Andaluc´ıa. V.C. would like to acknowledge partial support from EU ToK grant 39965. Finally, we also thank the referee for useful comments. Facilities: CAO:2.2 m, CFHT, ESO:3.6 m, GALEX, KPNO:2.1 m, NTT, Spitzer.|
|Subject Keywords:||galaxies: dwarf; galaxies: interactions; galaxies: irregular; infrared: galaxies; stars: formation; ultraviolet: galaxies|
|Usage Policy:||No commercial reproduction, distribution, display or performance rights in this work are provided.|
|Deposited By:||Jason Perez|
|Deposited On:||10 Jul 2009 16:28|
|Last Modified:||26 Dec 2012 11:04|
Repository Staff Only: item control page