2015A&A...581A..65C


C.D.S. - SIMBAD4 rel 1.7 - 2020.07.08CEST02:46:58

2015A&A...581A..65C - Astronomy and Astrophysics, volume 581A, 65-65 (2015/9-1)

Properties and formation mechanism of the stellar counter-rotating components in NGC 4191.

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

Abstract (from CDS):

We here distinguish two counter-rotating stellar components in NGC 4191 and characterize their physical properties such as kinematics, morphology, age, and metallicity. We obtained integral field spectroscopic observations with VIRUS-W and used a spectroscopic decomposition technique to separate the contribution of two stellar components to the observed galaxy spectrum. We also performed a photometric decomposition, modeling the galaxy with a Sersic bulge and two exponential disks of different scale length, with the aim of associating these structural components with the kinematic components. We then measured the equivalent width of the absorption line indices on the best-fit models that represent the kinematic components and compared our measurements to the predictions of stellar population models that also account for the variable abundance ratio of α elements. We have evidence that the line-of-sight velocity distributions (LOSVDs) are bimodal and asymmetric, consistent with the presence of two distinct kinematic components. The combined information of the intensity of the peaks of the LOSVDs and the photometric decomposition allows us to associate the Sersic bulge and the outer disk with the main kinematic component and to associate the inner disk with the secondary kinematic component. We find that the two kinematic stellar components counter-rotate with respect to each other. The main component is the most luminous and massive; the secondary component rotates along the same direction as the ionized gas. The study of the stellar populations reveals that the two kinematic components have the same solar metallicity and subsolar abundance ratio, without significant radial gradients. On the other hand, their ages show negative gradients and the possible indication that the secondary component is the younger. We interpret our results in light of recent cosmological simulations and suggest gas accretion along two filaments as the formation mechanism of the stellar counter-rotating components in NGC 4191.

Abstract Copyright:

Journal keyword(s): galaxies: abundances - galaxies: kinematics and dynamics - galaxies: formation - galaxies: stellar content - galaxies: individual: NGC 4191

VizieR on-line data: <Available at CDS (J/A+A/581/A65): list.dat mfNGC4191.fits>

Simbad objects: 10

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Number of rows : 10

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 3593 GiG 11 14 36.9733686308 +12 49 05.505076217   11.8       ~ 326 2
3 * bet Vir PM* 11 50 41.7182390 +01 45 52.991019 4.26 4.15 3.60 3.13 2.85 F9V 856 0
4 HD 106210 PM* 12 13 13.1187136931 +10 49 17.961030099   8.24   7.1   G3V 74 0
5 NGC 4191 LIN 12 13 50.380 +07 12 03.03   13.9       ~ 89 0
6 NGC 4546 GiG 12 35 29.506 -03 47 35.62 11.89 11.30 10.32     ~ 201 1
7 NGC 4550 GiP 12 35 30.612 +12 13 15.44 12.97 12.56 11.68     ~ 504 1
8 * 20 Boo PM* 14 19 45.2350539949 +16 18 24.995504868       4.1   K3III 145 0
9 NGC 5719 GiP 14 40 56.393 -00 19 05.49   13.10   12.061   ~ 148 1
10 NGC 7332 GiP 22 37 24.522 +23 47 54.06   12.0       ~ 353 0

    Equat.    Gal    SGal    Ecl

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2020.07.08-02:46:58

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