2018A&A...616A..22P


C.D.S. - SIMBAD4 rel 1.7 - 2020.07.08CEST02:22:53

2018A&A...616A..22P - Astronomy and Astrophysics, volume 616A, 22-22 (2018/8-1)

Evidence for the formation of the young counter-rotating stellar disk from gas acquired by IC 719.

PIZZELLA A., MORELLI L., COCCATO L., CORSINI E.M., DALLA BONTA E., FABRICIUS M. and SAGLIA R.P.

Abstract (from CDS):


Aims. The formation scenario of extended counter-rotating stellar disks in galaxies is still debated. In this paper, we study the S0 galaxy IC 719 known to host two large-scale counter-rotating stellar disks in order to investigate their formation mechanism.
Methods. We exploit the large field of view and wavelength coverage of the Multi Unit Spectroscopic Explorer (MUSE) spectrograph to derive two-dimensional (2D) maps of the various properties of the counter-rotating stellar disks, such as age, metallicity, kinematics, spatial distribution, the kinematical and chemical properties of the ionized gas, and the dust map.
Results. Due to the large wavelength range, and in particular to the presence of the Calcium Triplet λλ8498, 8542, 8662Å (CaT hereafter), the spectroscopic analysis allows us to separate the two stellar components in great detail. This permits precise measurement of both the velocity and velocity dispersion of the two components as well as their spatial distribution. We derived a 2D map of the age and metallicity of the two stellar components, as well as the star formation rate and gas-phase metallicity from the ionized gas emission maps.
Conclusions. The main stellar disk of the galaxy is kinematically hotter, older, thicker and with larger scale-length than the secondary disk. There is no doubt that the latter is strongly linked to the ionized gas component: they have the same kinematics and similar vertical and radial spatial distribution. This result is in favor of a gas accretion scenario over a binary merger scenario to explain the origin of counter-rotation in IC 719. One source of gas that may have contributed to the accretion process is the cloud that surrounds IC 719.

Abstract Copyright: © ESO 2018

Journal keyword(s): galaxies: individual: IC 719 - galaxies: kinematics and dynamics - galaxies: stellar content - galaxies: formation

Simbad objects: 13

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Number of rows : 13

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 NGC 448 GiP 01 15 16.530 -01 37 33.98   13.2       ~ 81 0
2 NGC 524 GiP 01 24 47.707 +09 32 19.65   11.5       ~ 419 1
3 NGC 1366 GiG 03 33 53.658 -31 11 38.78   12.94   11.49   ~ 86 0
4 NGC 3593 GiG 11 14 36.9733686308 +12 49 05.505076217   11.8       ~ 326 2
5 NGC 3595 GiG 11 15 25.5492403964 +47 26 49.400333146   13.0       ~ 59 0
6 IC 718 G 11 39 52.762 +08 52 28.16   14.6       ~ 39 0
7 IC 719 G 11 40 18.490 +09 00 35.50   13.6       ~ 103 0
8 NGC 4138 Sy1 12 09 29.788 +43 41 07.14 12.46 12.29 11.32 10.82   ~ 348 1
9 NGC 4191 LIN 12 13 50.380 +07 12 03.03   13.9       ~ 89 0
10 NGC 4550 GiP 12 35 30.612 +12 13 15.44 12.97 12.56 11.68     ~ 504 1
11 NGC 5102 EmG 13 21 57.6093133937 -36 37 48.385654208   9.74 9.65 8.47 10.2 ~ 318 1
12 NGC 5718 LIN 14 40 42.835 +03 27 55.52   14.6       ~ 50 1
13 NGC 5719 GiP 14 40 56.393 -00 19 05.49   13.10   12.061   ~ 148 1

    Equat.    Gal    SGal    Ecl

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2020.07.08-02:22:53

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