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.
arxiv +1 more source
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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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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Detection of a Star Forming Galaxy in the Center of a Low-Mass Galaxy Cluster [PDF]
, 2018 Brightest Cluster Galaxies (BCGs) residing in the centers of galaxy clusters are typically quenched giant ellipticals. A recent study hinted that star-forming galaxies with large disks, so-called superluminous spirals and lenticulars, are the BCGs of a subset of galaxy clusters.
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Color Differences between Clockwise and Counterclockwise Spiral Galaxies [PDF]
arXiv, 2013 While spiral galaxies observed from Earth clearly seem to spin in different directions, little is yet known about other differences between galaxies that spin clockwise and galaxies that spin counterclockwise. Here we compared the color of 64,399 spiral galaxies that spin clockwise to 63,215 spiral galaxies that spin counterclockwise.
arxiv
The Fastest Galaxy Evolution in an Unbiased Compact Group Sample with WISE [PDF]
, 2017 We study the mid-infrared (MIR) properties of galaxies in compact groups and their environmental dependence using the \textit{Wide-field Infrared Survey Explorer (WISE)} data. We use a volume-limited sample of 670 compact groups and their 2175 member galaxies with $M_r< -19.77$ and $0.01
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Active Dwarf Galaxies as Circumnuclear Regions of LSB-galaxies [PDF]
arXiv, 2006 Some arguments are brought that often active dwarf galaxies are the circumnuclear regions of LSB-galaxies in fact,rather than an ordinary galaxies.
arxiv
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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Visualizing the Hidden Features of Galaxy Morphology with Machine Learning [PDF]
arXiv, 2018 We train three convolutional neural networks (CNNs) to classify galaxies with Galaxy Zoo 2 dataset and extract the activations from the last fully connected layer or the last average pooling layer of CNNs to study the high-dimensional abstract feature representations of galaxy images.
arxiv
Comparisons of the environmental dependence of galaxy properties between galaxies above and below M [PDF]
, 2009 From the Main galaxy sample of the Sloan Digital Sky Survey Data Release 6 (SDSS DR6), we construct two volume-limited samples above and below the value of M, to explore the difference of the environmental dependence of galaxy properties between galaxies above and below the value of M .
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