Volume 499, Number 2, May IV 2009
|Page(s)||427 - 437|
|Published online||19 March 2009|
On the survival of metallicity gradients to major dry-mergers
Observatoire de Paris, section de Meudon, GEPI, 5 place Jules Janssen, 92195 Meudon, France e-mail: firstname.lastname@example.org
2 Department of Physics & Astronomy, University of Southern California, Los Angeles 90089-0484, USA
3 Observatoire de Paris, LERMA, 61 avenue de l'Observatoire, 75014 Paris, France
Accepted: 8 March 2009
Using a large suite of galaxies with a variety of concentrations and metallicity gradients, we study the evolution of non-dissipative (“dry”) equal mass mergers. Our purpose in generating these simulations is to explore how the metallicity gradient in dry mergers depends on the structure and metallicity gradients of the galaxies involved in the merger. Specifically, we would like to answer: Could dry mergers lead to metallicity gradients as observed in elliptical galaxies in the local Universe? Do dry mergers always lead to a flattening of the initial (i.e., pre-merger) gradient? From this modeling, we conclude that: The ratio of the remnant and the initial galaxy slopes span a wide range of values, up to values greater than 1 (with values greater than one resulting only when companions have gradients twice the progenitor). For a merger between two ellipticals having identical initial metallicity slopes (i.e., equal companion and galaxy slopes), the metallicity profile of the remnant flattens, with a final gradient about 0.6 times the initial one. Ellipticals can maintain their original pre-merger metallicity gradient if the companion slope is sufficiently steep. The amount of flattening neither depends on the characteristics of the orbit of the progenitors or on their initial concentration. Given the diversity in outcomes of the mergers, we conclude that dry mergers do not violate any observational constraints on the systematic characteristics of metallicity gradients in local ellipticals. In fact, dry mergers may be important within the context of the results of our simulations and may explain the large scatter in gradients for massive ellipticals and the relative paucity of massive ellipticals with no or shallow metallicity gradients.
Key words: methods: N-body simulations / methods: numerical / galaxies: evolution / galaxies: interaction / galaxies: elliptical and lenticular, cD
© ESO, 2009
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