2017A&A...606A..95C


C.D.S. - SIMBAD4 rel 1.7 - 2020.07.08CEST03:46:30

2017A&A...606A..95C - Astronomy and Astrophysics, volume 606A, 95-95 (2017/10-1)

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

CORTIJO-FERRERO C., GONZALEZ DELGADO R.M., PEREZ E., SANCHEZ S.F., CID FERNANDES R., DE AMORIM A.L., DI MATTEO P., GARCIA-BENITO R., LACERDA E.A.D., LOPEZ FERNANDEZ R., TADHUNTER C., VILLAR-MARTIN M. and ROTH M.M.

Abstract (from CDS):

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 Hα and [NII]λ6584 imaging. The spectra were processed with theSTARLIGHT full spectral fitting code, and the results are compared with those for two early-stage merger LIRGs (IC 1623 W and 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 (140Myr-1.4Gyr), and a second one, traced by young stellar populations YSP (<140Myr), which is concentrated in the central regions (<1.4kpc). Our results are in agreement with the epochs of the first peri-center passage (∼200Myr ago) and coalescence (<100Myr 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 <2.8kpc, where LINER-like ionization and high-velocity dispersion (∼220km/s) 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 (∼0.5M/yr/kpc2), 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.

Abstract Copyright: © ESO, 2017

Journal keyword(s): galaxies: interactions - galaxies: evolution - galaxies: stellar content - galaxies: ISM - galaxies: star formation - techniques: spectroscopic - techniques: spectroscopic

Simbad objects: 12

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Number of rows : 12

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2020
#notes
1 IC 1623 IG 01 07 47.2 -17 30 25   15       ~ 261 1
2 IC 1623B rG 01 07 47.569 -17 30 25.04   15.04   14.07   ~ 59 1
3 NGC 1316 GiP 03 22 41.789 -37 12 29.52 9.81 9.15 8.53 7.66   ~ 1202 1
4 NGC 2623 LIN 08 38 24.016 +25 45 16.29 14.10 13.99 13.36     ~ 434 1
5 Feige 34 HS* 10 39 36.7377085527 +43 06 09.209752646 9.613 10.91 11.14 11.319 11.464 sdOp 604 0
6 NAME Antennae IG 12 01 53.170 -18 52 37.92           ~ 1555 0
7 NGC 4676 IG 12 46 10.18 +30 43 53.7   14.1       ~ 297 0
8 IC 4553 SyG 15 34 57.22396 +23 30 11.6084   14.76 13.88     ~ 2681 4
9 NGC 6090 PaG 16 11 40.3 +52 27 21   14.0       ~ 396 2
10 NGC 6090W G 16 11 40.3 +52 27 25           ~ 11 0
11 NAME IRAS F16104+5235 NE G 16 11 40.816 +52 27 26.99           ~ 19 0
12 NGC 7252 IG 22 20 44.7751096408 -24 40 41.905677809 12.26 12.46 12.06 11.57   ~ 662 1

    Equat.    Gal    SGal    Ecl

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2020.07.08-03:46:30

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