Early-type disk galaxies: Structure and kinematics

Засов, А. В.; Моисеев, А. В.; Хоперсков, А. В.; Sidorova, E. A.

doi:10.1134/s1063772908020017

Cited by 20 publications

(46 citation statements)

References 34 publications

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“…The data were obtained with the SCORPIO (Afanasiev & Moiseev 2005) focal reducer in the long-slit mode (with the slit size of 6 ′ × 1 ′′ ) mounted at the primary focus of the 6-m telescope of the Special Astrophysical Observatory. Observations and data reduction are described in detail in Zasov et al (2008) for NGC 1167 and NGC 4150 and in Zasov et al (2012) for NGC 338 and NGC 3245.…”

Section: Datamentioning

confidence: 99%

“…The bulge has a steep photometric profile (the Sérsic index n ≈ 3 according to Zasov et al 2008) and dominates over the disc up to 15 − 20 ′′ . The total disc luminosity is three times greater than the bulge luminosity.…”

Section: Datamentioning

confidence: 99%

“…The vertical dashed line separates the region R < r e,b where bulge dominates. Morphological type (2) was taken from Zasov et al (2008) and Zasov et al (2012). Inclination angle (3) references are (I) , (II) LEDA database (Lyon/MeudonExtragalactic Database).…”

Section: Stellar Velocity Dispersionsmentioning

confidence: 99%

“…One way is to construct a set of maximum-mass marginally stable discs (N-body models). Then the line-of-sight velocity dispersion profiles can be constructed and compared with observational data to choose the most reliable model (Bottema & Gerritsen 1997;Zasov et al 2008Zasov et al , 2012. Another way is to pick out σ R , σ ϕ and σ z directly from σ los along the major and minor axes, provided the epicycle approximation that connects σ R , σ ϕ and the rotational velocity of starsv ϕ (Gerssen et al 1997(Gerssen et al , 2000Shapiro et al 2003;Gerssen & Shapiro Griffin 2012;Verheijen et al 2004;Noordermeer et al 2008).…”

Section: Introductionmentioning

confidence: 99%

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Reconstructing the velocity dispersion profiles from the line-of-sight kinematic data in disc galaxies

Marchuk

Sotnikova

2016

Mon. Not. R. Astron. Soc.

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We present a modification of the method for reconstructing the stellar velocity ellipsoid (SVE) in disc galaxies. Our version does not need any parametrization of the velocity dispersion profiles and uses only one assumption that the ratio σ z /σ R remains constant along the profile or along several pieces of the profile. The method was tested on two galaxies from the sample of other authors and for the first time was applied to three lenticular galaxies NGC 1167, NGC 3245 and NGC 4150 as well as to one Sab galaxy NGC 338. We found that for galaxies with a high inclination (i > 55 − 60• ) it is difficult or rather impossible to extract the information about SVE while for galaxies at an intermediate inclination the procedure of extracting is successful. For NGC 1167 we managed to reconstruct SVE, provided that the value of σ z /σ R is piecewise constant. We found σ z /σ R = 0.7 for the inner parts of the disc and σ z /σ R = 0.3 for the outskirts. We also obtained a rigid constrain on the value of the radial velocity dispersion σ R for highly inclined galaxies and tested the result using the asymmetric drift equation, provided that the gas rotation curve is available.

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Section: Datamentioning

confidence: 99%

Section: Datamentioning

confidence: 99%

Section: Stellar Velocity Dispersionsmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Reconstructing the velocity dispersion profiles from the line-of-sight kinematic data in disc galaxies

Marchuk

Sotnikova

2016

Mon. Not. R. Astron. Soc.

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“…Both the analysis of the available measurements of the galactic disks velocity dispersion (Shapiro et al, 2003) and the results of numerical modeling (see e.g. Zasov et al, 2008) show that in most cases m ≈ 0.4 − 0.7.…”

Section: The Local Criterion Of Gravitational Stabilitymentioning

confidence: 99%

Gravitational stability and mass estimation of stellar disks

Saburova

Засов

2013

Astron Nachr

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Abstract. We estimate the masses of disks of galaxies using the marginal gravitational stability criterion and compare them with the photometrical disk mass evaluations. The comparison reveals that the stellar disks of most of spiral galaxies we considered cannot be substantially overheated (at least within several radial scalelengths) and are therefore unlikely to have experienced a significant merging event in their history. However, for substantial part of S0-type galaxies a stellar velocity dispersion is well in excess of the gravitational stability threshold suggesting a major merger event in the past. For four low surface brightness galaxies we found that the disk masses corresponding to the marginal stability condition are significantly higher than it may be expected from their brightness. Either their disks are dynamically overheated, or they contain a large amount of non-luminous matter.

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NGC 6340: an old S0 galaxy with a young polar disc

Chilingarian

Novikova

Cayatte

et al. 2009

A&A

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Context. Lenticular galaxies are believed to form by a combination of environmental effects and secular evolution. Aims. We study the nearby disc-dominated S0 galaxy NGC 6340 photometrically and spectroscopically to understand the mechanisms of S0 formation and evolution in groups. Methods. We use SDSS images to build colour maps and the light profile of NGC 6340, which we decompose using a three-component model including Sérsic and two exponential profiles. We also use Spitzer Space Telescope archival near-infrared images to study the morphology of regions containing warm interstellar medium and dust. Then, we re-process and re-analyse deep long-slit spectroscopic data for NGC 6340, applying a novel sky subtraction technique and recover its stellar and gas kinematics, distribution of age and metallicity with the NBursts full spectral fitting. Results. We obtain the profiles of internal kinematics, age, and metallicity out to >2 half-light radii. The three structural components of NGC 6340 are found to have distinct kinematic and stellar population properties. We see a kinematic misalignment between inner and outer regions of the galaxy. We confirm the old metal-rich centre and a wrapped inner gaseous polar disc (r ∼ 1 kpc) having weak ongoing star formation, counter-rotating in projection with respect to the stars. The central compact pseudo-bulge of NGC 6340 looks very similar to compact elliptical galaxies. Conclusions. In accordance with the results of numerical simulations, we conclude that the properties of NGC 6340 can be explained as the result of a major merger of an early-type galaxy and a spiral galaxy that occurred about 12 Gyr ago. The intermediate exponential structure might be a triaxial pseudo-bulge formed by a past bar structure. The inner compact bulge could be the result of a nuclear starburst triggered by the merger. The inner polar disc appeared recently, 1/3-1/2 Gyr ago, as a result of another minor merger or cold gas accretion.

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Early-type disk galaxies: Structure and kinematics

Cited by 20 publications

References 34 publications

Reconstructing the velocity dispersion profiles from the line-of-sight kinematic data in disc galaxies

Reconstructing the velocity dispersion profiles from the line-of-sight kinematic data in disc galaxies

Gravitational stability and mass estimation of stellar disks

NGC 6340: an old S0 galaxy with a young polar disc

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