C.D.S. - SIMBAD4 rel 1.7 - 2020.07.05CEST06:34:58

2007A&A...466..905F - Astronomy and Astrophysics, volume 466, 905-916 (2007/5-2)

Evolution of structure in late-type spiral galaxies. I. Ionized gas kinematics in NGC 628.


Abstract (from CDS):

We study two dimensional Fabry-Perot interferometric observations of the nearby face-on late-type spiral galaxy, NGC 628, in order to analyse the ionized gas component of the interstellar medium. Covering the galaxy out to a radius larger than 12kpc, and with a spatial sampling of 1.6", we aim to investigate the large-scale dynamics as well as feedback from individual HII regions into their surrounding medium. The observed Hα emission distribution and kinematics are compared with auxiliary data from molecular and atomic gas observations, which display many similarities. We decompose the observed line-of-sight velocities into rotational and higher-order harmonic components, and study the role of gravitational perturbations along with that of external triggers which can disturb the kinematics and morphology of NGC 628. We calculate radial profiles of the emission-line velocity dispersion which we use to study the role of feedback from individual HII regions. We verify the presence of an inner rapidly rotating disc-like component in NGC 628, which we interpret as caused by slow secular evolution of the large-scale spiral arms and oval structure. In combination with auxiliary data, we find indication for that gas is falling in from the outer parts towards the central regions, where a nuclear ring has formed at the location of the inner Lindblad resonance radius of an an m=2 perturbation. Complementary continuum subtracted narrow band images in Hα have been used to identify 376 HII regions with calibrated luminosities. The mean velocity dispersion for the ionized gas (even when excluding pixels belonging to HII regions) is almost constant out to 12kpc, although it varies from 14 to 20km/s, with a steady decline in the outer parts. We have found kinematic signatures of radial motions caused by an m=2 perturbation. Such a perturbation may well be responsible for the inflow of material forming the nuclear ring and the inner rapidly rotating disc-like structure. The latter, in turn, could help build a pseudo-bulge in NGC 628. The current paper demonstrates a number of tools that we have developed for building a solid frame work for studying the evolution of structure in spiral galaxies using two dimensional kinematic observations.

Abstract Copyright:

Journal keyword(s): galaxies: spiral - galaxies: structure - galaxies: evolution - galaxies: kinematics and dynamics - galaxies: ISM - galaxies: individual: NGC 628

VizieR on-line data: <Available at CDS (J/A+A/466/905): table.dat>

Nomenclature: Table: [FBZ2007] NNN (Nos 1-376).

Status at CDS:   All or part of tables of objects could be ingested in SIMBAD with priority 2.

Simbad objects: 6

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Number of rows : 6

N Identifier Otype ICRS (J2000)
ICRS (J2000)
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2020
1 M 74 G 01 36 41.772 +15 47 00.46 10.52 10.00 9.46 9.16   ~ 1400 1
2 M 77 GiP 02 42 40.771 -00 00 47.84 9.70 9.61 8.87 10.1 9.9 ~ 4089 2
3 NGC 1365 Sy1 03 33 36.458 -36 08 26.37 10.48 10.08 9.63 8.79 9.7 ~ 1523 2
4 NGC 4593 Sy1 12 39 39.4435521178 -05 20 39.035028119   13.95 13.15     ~ 948 0
5 ESO 507-16 EmG 12 49 40.2920071852 -25 09 40.628543572   14.88   13.71   ~ 22 0
6 NGC 7690 G 23 33 02.5948392010 -51 41 54.007662728   12.93 12.01 12.19 12.6 ~ 59 0

    Equat.    Gal    SGal    Ecl

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