Results 1 to 10 of about 503,274 (25)
On the fundamentality of the radial acceleration relation for late-type galaxy dynamics [PDF]
MNRAS 2023 525 (4): 6130-6145, 2023 Galaxies have been observed to exhibit a level of simplicity unexpected in the complex galaxy formation scenario posited by standard cosmology. This is particularly apparent in their dynamics, where scaling relations display much regularity and little intrinsic scatter.
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Velocity Dispersion of 335 Galaxy Clusters Selected from the Sloan Digital Sky Survey: Statistical Evidence for Dynamical Interaction, and Against Ram-Pressure Stripping [PDF]
Mon.Not.Roy.Astron.Soc. 359 (2005) 1415-1420, 2005 There has been plenty of observational evidence of cluster galaxy evolution. However, it has been difficult to identify the origin of the cluster galaxy evolution. Here we show that gravitational interaction/friction between galaxies is the statistically dominant physical mechanism responsible for the cluster galaxy evolution, and that the well-favored
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Dynamics of Companion Galaxies of Early-Type Galaxies [PDF]
, 2020 We estimated the dynamical masses of 115 early-type galaxies (ETGs) by analyzing the dynamics of satellite and companion galaxies of these ETGs. We selected galaxies with absolute magnitudes between -22 and -25 in the $K_s$-band from the Extragalactic Distance Database (EDD). We also selected 216 spiral galaxies for comparison.
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266 E+A Galaxies Selected from the Sloan Digital Sky Survey Data Release 2: The Origin of E+A Galaxies [PDF]
Mon.Not.Roy.Astron.Soc. 357 (2005) 937, 2005 E+A galaxies are characterized as a galaxy with strong Balmer absorption lines but without any [OII] nor H$\alpha$ emission lines. The existence of strong Balmer absorption lines indicates that E+A galaxies have experienced starburst within recent one Gyr.
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The Elephant in the Bathtub: when the physics of star formation regulate the baryon cycle of galaxies [PDF]
, 2020 In simple models of galaxy formation and evolution, star formation is solely regulated by the amount of gas present in the galaxy. However, it has recently been shown that star formation can be suppressed by galactic dynamics in galaxies that contain a dominant spheroidal component and a low gas fraction. This 'dynamical suppression' is hypothesised to
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Measuring dark matter by modeling interacting galaxies [PDF]
AIP Conf.Proc.1240:383-386,2010, 2009 The dark matter content of galaxies is usually determined from galaxies in dynamical equilibrium, mainly from rotationally supported galactic components. Such determinations restrict measurements to special regions in galaxies, e.g. the galactic plane(s), whereas other regions are not probed at all.
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Determination of the dynamical structure of galaxies using optical spectra [PDF]
, 1998 Galaxy spectra are a rich source of kinematical information since the shapes of the absorption lines reflect the movement of stars along the line-of-sight. We present a technique to directly build a dynamical model for a galaxy by fitting model spectra, calculated from a dynamical model, to the observed galaxy spectra.
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Formation of a polar-ring galaxy in a galaxy merger [PDF]
, 1998 We numerically investigate stellar and gas dynamics in star-forming and dissipative galaxy mergers between two disk galaxies with specific orbital configurations. We find that violent relaxation combined with gaseous dissipation in galaxy merging transforms two disk galaxies into one S0 galaxy with polar-rings: Both the central S0-like host and the ...
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Galaxy Properties in Clusters: Dependence on the Environment and the Cluster Identification Techniques [PDF]
, 2009 We investigate the dependence of several galaxy properties on the environment and cluster identification techniques. We select clusters of galaxies from two catalogues based on the SDSS: the ROSAT-SDSS Galaxy Cluster Survey, and the MaxBCG Catalogue. Based on a volume limited sample of galaxies drawn from the spectroscopic DR5 SDSS, we constructed sub ...
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Proc. IAU 14 (2019) 101-108, 2019 Dynamical models will be key to exploitation of the incoming flood data for our Galaxy. Modelling techniques are reviewed with an emphasis on f(J) modelling.
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