Modeling Noncircular Motions in Disk Galaxies: Application to NGC 2976

Spekkens, Kristine; Sellwood, J. A.

doi:10.1086/518471

Cited by 167 publications

(276 citation statements)

References 37 publications

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“…Large synthesized beams in radio interferometry indeed dilute the kinematics and lower the impact of asymmetries in the kinematical and dynamical modeling. Similar amplitudes to those of M 99 were found in other galaxies for k = 2 components from Hα observations (e.g., Chemin et al 2006;Spekkens & Sellwood 2007), which confirms that high-resolution data are more appropriate to estimate accurate amplitudes of kinematical asymmetries.…”

Section: Appendix A: Harmonics Of the Gravitational Potentials Of Lumsupporting

confidence: 82%

“…Jog (2002) predicted the signatures of galaxy lopsidedness on rotation curves. Spekkens & Sellwood (2007) also illustrated the effects of nonuniformity for a galaxy perturbed by an inner bar-like/oval distortion, but on l.o.s. motions and from a different harmonic model than in Schoenmakers et al (1997) and Wong et al (2004).…”

Section: Comparison With Previous Work and Numerical Simulationsmentioning

confidence: 99%

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Asymmetric mass models of disk galaxies

Chemin

Huré

Soubiran

et al. 2016

A&A

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Mass models of galactic disks traditionally rely on axisymmetric density and rotation curves, paradoxically acting as if their most remarkable asymmetric features, such as lopsidedness or spiral arms, were not important. In this article, we relax the axisymmetry approximation and introduce a methodology that derives 3D gravitational potentials of disk-like objects and robustly estimates the impacts of asymmetries on circular velocities in the disk midplane. Mass distribution models can then be directly fitted to asymmetric line-of-sight velocity fields. Applied to the grand-design spiral M 99, the new strategy shows that circular velocities are highly nonuniform, particularly in the inner disk of the galaxy, as a natural response to the perturbed gravitational potential of luminous matter. A cuspy inner density profile of dark matter is found in M 99, in the usual case where luminous and dark matter share the same center. The impact of the velocity nonuniformity is to make the inner profile less steep, although the density remains cuspy. On another hand, a model where the halo is core dominated and shifted by 2.2−2.5 kpc from the luminous mass center is more appropriate to explain most of the kinematical lopsidedness evidenced in the velocity field of M 99. However, the gravitational potential of luminous baryons is not asymmetric enough to explain the kinematical lopsidedness of the innermost regions, irrespective of the density shape of dark matter. This discrepancy points out the necessity of an additional dynamical process in these regions: possibly a lopsided distribution of dark matter.

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Section: Appendix A: Harmonics Of the Gravitational Potentials Of Lumsupporting

confidence: 82%

Section: Comparison With Previous Work and Numerical Simulationsmentioning

confidence: 99%

Asymmetric mass models of disk galaxies

Chemin

Huré

Soubiran

et al. 2016

A&A

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“…The DiskFit code (Spekkens & Sellwood 2007) allows us to correct the Hi velocity fields of Saglia et al (2010) and Chemin et al (2009) for non-circular motions in M31's central parts. The success of this mass model will be determined by the stability of a dynamical N-body realization.…”

Section: Discussionmentioning

confidence: 99%

The Stellar Mass of M31 as inferred by the Andromeda Optical & Infrared Disk Survey

Sick

Courteau

Cuillandre³

et al. 2014

Proc. IAU

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Abstract. Our proximity and external vantage point make M31 an ideal testbed for understanding the structure of spiral galaxies. The Andromeda Optical and Infrared Disk Survey (ANDROIDS) has mapped M31's bulge and disk out to R=40 kpc in ugriJKs bands with CFHT using a careful sky calibration. We use Bayesian modelling of the optical-infrared spectral energy distribution (SED) to estimate profiles of M31's stellar populations and mass along the major axis. This analysis provides evidence for inside-out disk formation and a declining metallicity gradient. M31's i-band mass-to-light ratio (M/L * i ) decreases from 0.5 dex in the bulge to ∼ 0.2 dex at 40 kpc. The best-constrained stellar population models use the full ugriJKs SED but are also consistent with optical-only fits. Therefore, while NIR data can be successfully modelled with modern stellar population synthesis, NIR data do not provide additional constraints in this application. Fits to the gi-SED alone yield M/L * i that are systematically lower than the full SED fit by 0.1 dex. This is still smaller than the 0.3 dex scatter amongst different relations for M/Li via g − i colour found in the literature. We advocate a stellar mass of M * (30 kpc) = 10.3 +2.3 −1.7 × 10 10 M for the M31 bulge and disk.

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“…For late-type galaxies, these models often consider a symmetric velocity distribution, either by assuming a thin disc geometry (e.g., Barnes & Sellwood 2003;Epinat et al 2008) or symmetrical radial distortions with respect to some axis (Spekkens & Sellwood 2007). An alternative approach is a generalisation of the isophote fitting (i.e.…”

Section: Kinematic Position Angles From Velocity Mapsmentioning

confidence: 99%

Kinematic alignment of non-interacting CALIFA galaxies

Barrera-Ballesteros

Falcón-Barroso

García-Lorenzo

et al. 2014

A&A

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We present 80 stellar and ionised gas velocity maps from the Calar Alto Legacy Integral Field Area (CALIFA) survey in order to characterise the kinematic orientation of non-interacting galaxies. The study of galaxies in isolation is a key step towards understanding how fast-external processes, such as major mergers, affect kinematic properties in galaxies. We derived the global and individual (projected approaching and receding sides) kinematic position angles (PAs) for both the stellar and ionised gas line-of-sight velocity distributions. When compared to the photometric PA, we find that morpho-kinematic differences are smaller than 22 degrees in 90% of the sample for both stellar and nebular components and that internal kinematic misalignments are generally smaller than 16 degrees. We find a tight relation between the global stellar and ionised gas kinematic PA consistent with circular-flow pattern motions in both components (∼90% of the sample has differences smaller than 16 degrees). This relation also holds, generally in barred galaxies across the bar and galaxy disc scales. Our findings suggest that even in the presence of strong bars, both the stellar and the gaseous components tend to follow the gravitational potential of the disc. As a result, kinematic orientation can be used to assess the degree of external distortions in interacting galaxies.

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Modeling Noncircular Motions in Disk Galaxies: Application to NGC 2976

Cited by 167 publications

References 37 publications

Asymmetric mass models of disk galaxies

Asymmetric mass models of disk galaxies

The Stellar Mass of M31 as inferred by the Andromeda Optical & Infrared Disk Survey

Kinematic alignment of non-interacting CALIFA galaxies

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