Orbital decomposition of CALIFA spiral galaxies

Ling Zhu; Remco van den Bosch; Glenn van de Ven; Mariya Lyubenova; Jesús Falcón-Barroso; Sharon E. Meidt; Marie Martig; Juntai Shen; Zhao-Yu Li; Akin Yildirim; C. Jakob Walcher; Sebastian F. Sanchez

doi:10.1093/mnras/stx2409

paper

Orbital decomposition of CALIFA spiral galaxies

arXiv:1709.06649 · doi:10.1093/mnras/stx2409

Abstract

Schwarzschild orbit-based dynamical models are widely used to uncover the internal dynamics of early-type galaxies and globular clusters. Here we present for the first time the Schwarzschild models of late-type galaxies: an SBb galaxy NGC 4210 and an S0 galaxy NGC 6278 from the CALIFA survey. The mass profiles within $2 R_{e}$ are constrained well with $1 σ$ statistical error of $\sim 10%$ . The luminous and dark mass can be disentangled with uncertainties of $\sim 20%$ and $\sim 50%$ respectively. From $R_{e}$ to $2 R_{e}$ , the dark matter fraction increases from $14 \pm 10%$ to $18 \pm 10%$ for NGC 4210 and from $15 \pm 10%$ to $30 \pm 20%$ for NGC 6278. The velocity anisotropy profiles of both $σ_{r} / σ_{t}$ and $σ_{z} / σ_{R}$ are well constrained. The inferred internal orbital distributions reveal clear substructures. The orbits are naturally separated into three components: a cold component with near circular orbits, a hot component with near radial orbits, and a warm component in between. The photometrically-identified exponential disks are predominantly made up of cold orbits only beyond $\sim 1 R_{e}$ , while they are constructed mainly with the warm orbits inside. Our dynamical hot components are concentrated in the inner regions, similar to the photometrically-identified bulges. The reliability of the results, especially the orbit distribution, are verified by applying the model to mock data.

arXiv commentaccepted by MNRAS

Orbital decomposition of CALIFA spiral galaxies

Abstract

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