Publication: Mapping the star formation history of Mrk 86 II. Stellar populations and global interpretation
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2000-09
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Abstract
In this paper, continuation of Gil de Pat et al. (Paper I), we derive the main properties of the stellar populations in the Blue Compact Dwarf galaxy Mrk 86. Ages, stellar masses, metallicites and burst strengths have been obtained using the combination of Monte Carlo simulations, a maximum likelihood estimator and Cluster and Principal Component Analysis. The three stellar populations detected show well defined properties. We have studied the underlying stellar population, which shows an age between 5-13 Gyr and no significant color gradients. The intermediate aged (30 Myr old) central starburst show a very low dust extinction with high burst strength and high stellar mass content (∼9x10^6 M_⨀). Finally, the properties of 46 low-metallicity (∼1/10Z_⨀) star-forming regions were also studied. The properties derived suggest that the most recent star-forming activity in Mrk 86 was triggered by the evolution of a superbubble originated at the central starburst by the energy deposition of stellar winds and supernova explosions. This superbubble produced the blowout of a fraction of the interstellar medium at distances of about 1 kpc with high gas surface densities, leading to the activation of the star formation. Finally, different mechanisms for the star formation triggering in this massive central starburst are studied, including the merging with a low mass companion and the interaction with UGC 4278. We have assumed a distance to Mrk 86 of 6.9 Mpc.
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Based on observations with the JKT, INT and WHT operated on the island of La Palma by the Royal Greenwich Observatory in the Spanish Observatorio del Roque de los Muchachos of the Instituto Astrofísico de Canarias. Based also on observations collected at the German-Spanish Astronomical Center, Calar Alto, Spain, operated by the Max-Planck-Institut für Astronomie (MPIA), Heidelberg, jointly with the spanish Comisión Nacional de Astronomía. 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. We are grateful to Carme Jordi and D. Galadí for obtaining the V -band image. We would like to thank C. Sánchez Contreras and L.F. Miranda for obtaining the high resolution spectra. We also thank A. Alonso Herrero for her help in the acquisition and reduction of the nearinfrared images. We also acknowledge the referee Dr. Tosi for several helpful comments. We thank to C.E. García Dabó, J. Cenarro, M.E. Sharina, S.A. Silich and J. Gorgas for stimulating conversations. Finally, we are very grateful to R. Giovanelli for his kind help on analyzing the properties of UGC 4278. This research has been supported in part by the grants PB93-456 and PB96-0610 from the Spanish Programa Sectorial de Promoción del Conocimiento. A. Gil de Paz acknowledges the receipt of a Formación del Profesorado Universitario fellowship from the spanish Ministerio de Educación y Cultura.
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Astrofísica, Astronomía (Física)
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