High-resolution kinematic observations of rapidly rotating spheroidal components of galaxies

Carter, D.; Jenkins, Charles

doi:10.1093/mnras/263.4.1049

Cited by 18 publications

(14 citation statements)

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“…Tempel & Tenjes (2006) produced a model, based on Jeans equations, of the Sombrero galaxy (M 104, NGC 4594). They used the averaged major-axis kinematics from previous literature works (Kormendy & Illingworth 1982;Carter & Jenkins 1993;Hes & Peletier 1993;van der Marel et al 1994;Emsellem et al 1996;Kormendy et al 1996) and they determined the σ z and σ R radial profiles, as well as the orientation of the stellar velocity ellipsoid. In this paper, we adopt the mean value of σ z /σ R in the disc-dominated range, between 2 and 10 kpc approximately.…”

Section: Dynamical Models: Schwarzschild Three Integral and Jeans Mementioning

confidence: 99%

Revisiting the stellar velocity ellipsoid–Hubble-type relation: observations versus simulations

Pinna

Falcón-Barroso

Martig

et al. 2018

Monthly Notices of the Royal Astronomical Society

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The stellar velocity ellipsoid (SVE) in galaxies can provide important information on the processes that participate in the dynamical heating of their disc components (e.g. giant molecular clouds, mergers, spiral density waves, bars). Earlier findings suggested a strong relation between the shape of the disc SVE and Hubble type, with later-type galaxies displaying more anisotropic ellipsoids and early-types being more isotropic. In this paper, we revisit the strength of this relation using an exhaustive compilation of observational results from the literature on this issue. We find no clear correlation between the shape of the disc SVE and morphological type, and show that galaxies with the same Hubble type display a wide range of vertical-to-radial velocity dispersion ratios. The points are distributed around a mean value and scatter of σ z /σ R = 0.7 ± 0.2. With the aid of numerical simulations, we argue that different mechanisms might influence the shape of the SVE in the same manner and that the same process (e.g. mergers) does not have the same impact in all the galaxies. The complexity of the observational picture is confirmed by these simulations, which suggest that the vertical-to-radial axis ratio of the SVE is not a good indicator of the main source of disc heating. Our analysis of those simulations also indicates that the observed shape of the disc SVE may be affected by several processes simultaneously and that the signatures of some of them (e.g. mergers) fade over time.

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Section: Dynamical Models: Schwarzschild Three Integral and Jeans Mementioning

confidence: 99%

Revisiting the stellar velocity ellipsoid–Hubble-type relation: observations versus simulations

Pinna

Falcón-Barroso

Martig

et al. 2018

Monthly Notices of the Royal Astronomical Society

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“…In these cases, we used the Gauss‐‐Hermite expansion of the LOSVDs to estimate V ˜ and σ˜ using the same method as used by Emsellem et al (1996). We also made use of other published kinematics such as that in Kormendy & Richstone (1992, hereafter KR92) and Carter & Jenkins (1993), and the recent high spatial resolution FOS/HST and SIS/CFHT data (Kormendy et al 1996, hereafter K+96). We finally included the data of Illingworth & Schechter (1982, hereafter IS82) for offset axes and Capaccioli et al (1993, hereafter C+93) for the kinematics at large radii along the major axis.…”

Section: Observational Datamentioning

confidence: 99%

“…This trend has been very recently confirmed with FOS (faint object spectrograph) spectroscopy (Kormendy et al 1996), yielding σ 0 ∼445 km s −1 at HST resolution. Other studies mainly focused on the major‐axis kinematics (Carter & Jenkins 1993;van der Marel et al 1994;Bender, Saglia & Gerhard 1994;Fisher 1997). Finally, Capaccioli et al (1993) have shown that the stellar rotation and dispersion profiles were flat at large radii ( R >100 arcsec), thus indicating the presence of a massive dark halo.…”

Section: Introductionmentioning

confidence: 99%

Dynamical models of NGC 3115

Emsellem

Dejonghe

Bacon

1999

Monthly Notices of the Royal Astronomical Society

109

120

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We present new dynamical models of the S0 galaxy N3115, making use of the available published photometry and kinematics as well as of two-dimensional TIGER spectrography. We first examined the kinematics in the central 40 arcsec in the light of two integral f(E,J) models. Jeans equations were used to constrain the mass to light ratio, and the central dark mass whose existence was suggested by previous studies. The even part of the distribution function was then retrieved via the Hunter & Qian formalism. We thus confirmed that the velocity and dispersion profiles in the central region could be well fit with a two-integral model, given the presence of a central dark mass of ~10^9 Msun. However, no two integral model could fit the h_3 profile around a radius of 25 arcsec where the outer disc dominates the surface brightness distribution. Three integral analytical models were therefore built using a Quadratic Programming technique. These models showed that three integral components do indeed provide a reasonable fit to the kinematics, including the higher Gauss-Hermite moments. Again, models without a central dark mass failed to reproduce the observed kinematics in the central arcseconds. This clearly supports the presence of a nuclear black hole of at least 6.5 10^8 Msun in the centre of NGC 3115. These models were finally used to estimate the importance of the dark matter in the outer part of NGC 3115, suggested by the flat stellar rotation curve observed by Capaccioli et al. (1993).Comment: 18 pages, 22 figures, accepted for publication in MNRA

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“…To test our ability to measure rotation curves and velocity dispersions, we compared our results to stellar kinematic results of Carter and Jenkins (1993). These authors have accounted for the seeing variations, guiding, and surface brightness which must be included when modeling kinematics.…”

Section: Testing the Techniquesmentioning

confidence: 99%

Measuring stellar kinematics in galaxies with the near-infrared (2-0) (12) CO absorption bandhead

Gaffney¹,

Lester²,

Doppmann³

1995

PASP

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ABSTRACT. The shape and strength of the near-infrared (2-0) 12 CO absorption bandhead provide astronomers with a unique tool for measuring stellar kinematics in galaxies with strong dust obscuration. However, the asymmetric shape of the bandhead introduces complexities when extracting the kinematics from an observed spectrum. This paper discusses the benefits, drawbacks, and observational constraints associated with using this bandhead to measure kinematics in galaxies, focusing on applications in high spectral-resolution data. Additionally, we discuss techniques found useful for extracting the kinematics from the absorption feature, and outline our success with two different methods.

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High-resolution kinematic observations of rapidly rotating spheroidal components of galaxies

Cited by 18 publications

References 0 publications

Revisiting the stellar velocity ellipsoid–Hubble-type relation: observations versus simulations

Revisiting the stellar velocity ellipsoid–Hubble-type relation: observations versus simulations

Dynamical models of NGC 3115

Measuring stellar kinematics in galaxies with the near-infrared (2-0) (12) CO absorption bandhead

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