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G., González Riestra R., Rodríguez Caderot G., 1994, ApJS, 95, 3870035-871110.1111/j.1365-2966.2009.15989.xhttps://hdl.handle.net/20.500.14352/44588This article has been accepted for publication in Monthly notices of the Royal Astronomical Society. © 2009 The Authors. Journal compilation © 2009 RAS. Published by Oxford University Press on behalf of the Royal Astronomical Society. All rights reserved. It is a pleasure to thank those people who welcomed our project into the 3.5-m telescope in CAHA, where we always felt at home, especially those cozy snowy nights full of pastries and hot chocolates. We would especially like to thank Ana Guijarro, Jesús Aceituno and Santos Pedraz. We also thank Carlos Hoyos for interesting and highlighting discussions. Finally, we thank our referee, Matthew Bershady, for his helpful comments and suggestions. JPG acknowledges support from a University of Florida Alumni Fellowship and RG from NASA Grant LTSA NA65-11635. This work is partially funded by the Spanish MICINN under the Consolider-Ingenio 2010 Programme grant CSD2006-00070: First Science with the GTC (http://www.iac.es/consolider-ingenio-gtc). This work is partially funded by the Spanish Programa de Astronomía y Astrofísica under grants AYA2006-02358 and AYA2006-15698-C02-02.The kinematic properties of the ionized gas of local luminous compact blue galaxy NGC 7673 are presented using three-dimensional data taken with the PPAK integral field unit at the 3.5-m telescope in the Centro Astronomico Hispano Aleman. Our data reveal an asymmetric rotating velocity field with a peak-to-peak difference of 60 km s(-1). The kinematic centre is found to be at the position of a central velocity width maximum (sigma = 54 +/- 1 kms(-1)), which is consistent with the position of the luminosity-weighted centroid of the entire galaxy. The position angle of the minor rotation axis is 168 degrees as measured from the orientation of the velocity field contours. At least two decoupled kinematic components are found. The first one is compact and coincides with the position of the second most active star formation region (clump B). The second one is extended and does not have a clear optical counterpart. No evidence of active galactic nuclei activity or supernovae galactic winds powering any of these two components has been found. Our data, however, show evidence in support of a previously proposed minor merger scenario in which a dwarf galaxy, tentatively identified with clump B, is falling into NGC 7673 and triggers the starburst. Finally, it is shown that the dynamical mass of this galaxy may be severely underestimated when using the derived rotation curve or the integrated velocity width, under the assumption of virialization.engjournal articlehttp://dx.doi.org/10.1111/j.1365-2966.2009.15989.xhttp://mnras.oxfordjournals.org/open access52Star-forming galaxiesHubble deep fieldEmission-line galaxiesStellar mass functionsRedshift surveyStructural parametersNearby counterpartsStarburst galaxiesFormation historyDwarf galaxiesAstrofísica