The spatially resolved stellar population and ionized gas properties in the merger LIRG NGC 2623

C. Cortijo-Ferrero, R. M. González Delgado, E. Pérez, S. F. Sánchez, R. Cid Fernandes, A. L. de Amorim, P. Di Matteo, R. García-Benito, E. A. D. Lacerda, R. López Fernández, C.Tadhunter, M. Villar-Martín, M. M. Roth. 2017. The spatially resolved stellar population and ionized gas properties in the merger LIRG NGC 2623. Astronomy and Astrophysics 606, DOI: 10.1051/0004-6361/201730669

We report on a detailed study of the stellar populations and ionized gas properties in the merger LIRG NGC 2623, analyzing optical integral field spectroscopy from the CALIFA survey and PMAS LArr, multiwavelength HST imaging, and OSIRIS narrow band II alpha and [NII]lambda 6584 imaging. The spectra were processed with the starlight full spectral fitting code, and the results are compared with those for two early-stage merger LIRGs (IC 1623Wand NGC 6090), together with CALIFA Sbc/Sc galaxies. We find that NGC 2623 went through two periods of increased star formation (SF), a first and widespread episode, traced by intermediate-age stellar populations ISP (140 Myr-1.4 Gyr), and a second one, traced by young stellar populations YSP (< 140 Myr), which is concentrated in the central regions (< 1.4 kpc). Our results are in agreement with the epochs of the first peri-center passage (similar to 200 Myr ago) and coalescence (< 100 Myr ago) predicted by dynamical models, and with high-resolution merger simulations in the literature, consistent with NGC 2623 representing an evolved version of the early-stage mergers. Most ionized gas is concentrated within < 2.8 kpc, where LINER-like ionization and high-velocity dispersion (similar to 220 km s(-1)) are found, consistent with the previously reported outflow. As revealed by the highest-resolution OSIRIS and HST data, a collection of HII regions is also present in the plane of the galaxy, which explains the mixture of ionization mechanisms in this system. It is unlikely that the outflow in NGC 2623 will escape from the galaxy, given the low SFR intensity (similar to 0.5 M fi yr 1 kpc(-2)), the fact that the outflow rate is three times lower than the current SFR, and the escape velocity in the central areas is higher than the outflow velocity.

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