arXiv subjects

Keoikantse Moses Mogotsi

Publications and source records attributed to Keoikantse Moses Mogotsi.

3 recordsLinked to original sources

arXiv2019

The stellar velocity dispersion in nearby spirals: radial profiles and correlations

The stellar velocity dispersion, $σ$, is a quantity of crucial importance for spiral galaxies, where it enters fundamental dynamical processes such as gravitational instability and disc heating. Here we analyse a sample of 34 nearby spirals from the Calar Alto Legacy Integral Field Area (CALIFA) spectroscopic survey, deproject the line-of-sight $σ$ to $σ_{R}$ and present reliable radial profiles of $σ_{R}$ as well as accurate measurements of $\langleσ_{R}\rangle$, the radial average of $σ_{R}$ over one effective (half-light) radius. We show that there is a trend for $σ_{R}$ to increase with decreasing $R$, that $\langleσ_{R}\rangle$ correlates with stellar mass ($M_{\star}$) and tested correlations with other galaxy properties. The most significant and strongest correlation is the one with $M_{\star}$: $\langleσ_{R}\rangle \propto M_{\star}^{0.5}$. This tight scaling relation is applicable to spiral galaxies of type Sa $\mbox{--}$ Sd and stellar mass $M_{\star}\approx10^{9.5}\mbox{--}10^{11.5}\ \mbox{M}_{\odot}$. Simple models that relate $σ_{R}$ to the stellar surface density and disc scale length roughly reproduce that scaling, but overestimate $\langleσ_{R}\rangle$ significantly.

astro-ph.GA↗

arXiv2018

Angular momentum and local gravitational instability in galaxy discs: does $Q$ correlate with $j$ or $M\,$?

We introduce a new diagnostic for exploring the link between angular momentum and local gravitational instability in galaxy discs. Our diagnostic incorporates the latest developments in disc instability research, is fully consistent with approximations that are widely used for measuring the stellar specific angular momentum, $j_{\star}=J_{\star}/M_{\star}$, and is also very simple. We show that such a disc instability diagnostic hardly correlates with $j_{\star}$ or $M_{\star}$, and is remarkably constant across spiral galaxies of any given type (Sa$\!-\!$Sd), stellar mass ($M_{\star}=10^{9.5}\!-\!10^{11.5}\,\mathrm{M}_{\odot}$) and velocity dispersion anisotropy ($σ_{z\star}/σ_{R\star}=0\!-\!1$). The fact that $M_{\star}$ is tightly correlated with star formation rate ($\mathrm{SFR}$), molecular gas mass ($M_{\mathrm{mol}}$), metallicity ($12+\log\mathrm{O/H}$) and other fundamental galaxy properties thus implies that nearby star-forming spirals self-regulate to a quasi-universal disc stability level. This proves the existence of the self-regulation process postulated by several star formation models, but also raises important caveats.

astro-ph.GA↗

arXiv2017

What drives gravitational instability in nearby star-forming spirals? The impact of CO and HI velocity dispersions

The velocity dispersion of cold interstellar gas, sigma, is one of the quantities that most radically affect the onset of gravitational instabilities in galaxy discs, and the quantity that is most drastically approximated in stability analyses. Here we analyse the stability of a large sample of nearby star-forming spirals treating molecular gas, atomic gas and stars as three distinct components, and using radial profiles of sigma_CO and sigma_HI derived from HERACLES and THINGS observations. We show that the radial variations of sigma_CO and sigma_HI have a weak effect on the local stability level of galaxy discs, which remains remarkably flat and well above unity, but is low enough to ensure (marginal) instability against non-axisymmetric perturbations and gas dissipation. More importantly, the radial variation of sigma_CO has a strong impact on the size of the regions over which gravitational instabilities develop, and results in a characteristic instability scale that is one order of magnitude larger than the Toomre length of molecular gas. Disc instabilities are driven, in fact, by the self-gravity of stars at kpc scales. This is true across the entire optical disc of every galaxy in the sample, with few exceptions. In the linear phase of the disc instability process, stars and molecular gas are strongly coupled, and it is such a coupling that ultimately triggers local gravitational collapse/fragmentation in the molecular gas.

astro-ph.GA↗