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arXiv · 1011.5504

Anatomy of a post-starburst minor merger: a multi-wavelength WFC3 study of NGC 4150

R. Mark Crockett·Sugata Kaviraj·Joseph I. Silk·Bradley C. Whitmore·Robert W. O'Connell·Max Mutchler·Bruce Balick·Howard E. Bond·Daniela Calzetti·C. Marcella Carollo·Michael J. Disney·Michael A. Dopita·Jay A. Frogel·Donald N. B. Hall·Jon A. Holtzman·Randy A. Kimble·Patrick J. McCarthy·Francesco Paresce·Abhijit Saha·John T. Trauger·Alistair R. Walker·Rogier A. Windhorst·Erick T. Young·Hyunjin Jeong·Sukyoung K. Yi
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Abstract

(Abridged) We present a spatially-resolved near-UV/optical study of NGC 4150, using the Wide Field Camera 3 (WFC3) on board the Hubble Space Telescope. Previous studies of this early-type galaxy (ETG) indicate that it has a large reservoir of molecular gas, exhibits a kinematically decoupled core (likely indication of recent merging) and strong, central H_B absorption (indicative of young stars). The core of NGC 4150 shows ubiquitous near-UV emission and remarkable dusty substructure. Our analysis shows this galaxy to lie in the near-UV green valley, and its pixel-by-pixel photometry exhibits a narrow range of near-UV/optical colours that are similar to those of nearby E+A (post-starburst) galaxies. We parametrise the properties of the recent star formation (age, mass fraction, metallicity and internal dust content) in the NGC 4150 pixels by comparing the observed near-UV/optical photometry to stellar models. The typical age of the recent star formation (RSF) is around 0.9 Gyrs, consistent with the similarity of the near-UV colours to post-starburst systems, while the morphological structure of the young component supports the proposed merger scenario. The RSF metallicity, representative of the metallicity of the gas fuelling star formation, is around 0.3 - 0.5 Zsun. Assuming that this galaxy is a merger and that the gas is sourced mainly from the infalling companion, these metallicities plausibly indicate the gas-phase metallicity (GPM) of the accreted satellite. Comparison to the local mass-GPM relation suggests (crudely) that the mass of the accreted system is around 3x10^8 Msun, making NGC 4150 a 1:20 minor merger. A summation of the pixel RSF mass fractions indicates that the RSF contributes about 2-3 percent of the stellar mass. This work reaffirms our hypothesis that minor mergers play a significant role in the evolution of ETGs at late epochs.

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R. Mark Crockett, Sugata Kaviraj, Joseph I. Silk, Bradley C. Whitmore, Robert W. O'Connell, Max Mutchler, Bruce Balick, Howard E. Bond, Daniela Calzetti, C. Marcella Carollo, Michael J. Disney, Michael A. Dopita, Jay A. Frogel, Donald N. B. Hall, Jon A. Holtzman, Randy A. Kimble, Patrick J. McCarthy, Francesco Paresce, Abhijit Saha, John T. Trauger, Alistair R. Walker, Rogier A. Windhorst, Erick T. Young, Hyunjin Jeong, Sukyoung K. Yi. 2010-11-24. Anatomy of a post-starburst minor merger: a multi-wavelength WFC3 study of NGC 4150. https://doi.org/10.1088/0004-637x%2F727%2F2%2F115

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