Rotationally Supported Virgo Cluster Dwarf Elliptical Galaxies: Stripped Dwarf Irregular Galaxies?

2004 ◽  
Vol 128 (1) ◽  
pp. 121-136 ◽  
Author(s):  
Liese van Zee ◽  
Evan D. Skillman ◽  
Martha P. Haynes
Keyword(s):  
Elliptical Galaxies ◽  
Virgo Cluster ◽  
Irregular Galaxies ◽  
Dwarf Elliptical Galaxies ◽  
Dwarf Irregular Galaxies

scholarly journals Morphology and Environment of Dwarf Galaxies in the Local Universe

2007 ◽  
Vol 3 (S244) ◽  
pp. 346-347
Author(s):  
H. B. Ann
Keyword(s):  
Dwarf Galaxies ◽  
Elliptical Galaxies ◽  
Significant Fraction ◽  
Local Universe ◽  
Irregular Galaxies ◽  
Dwarf Elliptical Galaxies ◽  
Dwarf Irregular Galaxies

AbstractAnalysis of dwarf galaxies in the local universe shows that dwarf irregular galaxies are its dominant populations and the majority of dwarf elliptical galaxies are likely to be located in the overdense regions, However, a significant fraction of blue dwarf ellipticals (dEblue) and peculiar dwarf ellipticals (dEpec are found to be located in the under-dense regions.

scholarly journals Dwarf Elliptical Galaxies in the Cena and Sculptor Groups

1998 ◽  
Vol 11 (1) ◽  
pp. 107-108
Author(s):  
H. Jerjen ◽  
K.C. Freeman ◽  
B. Binggeli
Keyword(s):  
Dwarf Galaxies ◽  
Dwarf Galaxy ◽  
Elliptical Galaxies ◽  
Large Program ◽  
Irregular Galaxies ◽  
First Results ◽  
Complete Survey ◽  
Group Members ◽  
Dwarf Elliptical Galaxies ◽  
Dwarf Irregular Galaxies

Côté (1995) surveyed the nearby Centaurus A (Cen A) and Sculptor (Sci) group regions in the search for gas-rich, dwarf irregular galaxies (Irr) which are associated with these galaxy aggregates. 36 Irrs have been found and confirmed as new group members via 21cm/Hα redshifts. In finding this large number of Irrs, the question rises whether systems from the other dwarf galaxy family, the gas-poor dwarf ellipticals (dE), also exist in the two groups. So far nothing is known about dE membership but taking into account the morphology-density relation for dwarfs (Binggeli et al. 1990) a number ratio Irr/dE≈ 1 - 2 would be expected. Prompted by these “missing” dEs we started a large program to identify and study dEs in Cen A and Sci. The main scientific goals are (1) to find dE candidates and to establish group membership via velocity or distance and (2) to estimate the luminosity function (LF) of dwarf galaxies to the faintest possible luminosities. For the two groups, being respectively at a mean distance of 4.0 Mpc and 2.5 Mpc, we will be able to reach dwarf galaxies 4-5 magnitudes fainter than in the previous studies in the Virgo and Fornax clusters and the five groups Leo I, Dorado, NGC1400, NGC5044, and Antlia (Sandage et al. 1985, Ferguson &: Sandage 1990). We briefly outline here first results from the CenA group. All details about the complete survey including Scl will be presented in Jerjen et al. (1997)

scholarly journals 3D view on Virgo and field dwarf elliptical galaxies: late-type origin and environmental transformations

2012 ◽  
Vol 10 (H16) ◽  
pp. 334-334
Author(s):  
Agnieszka Ryś ◽  
Jesús Falcón-Barroso ◽  
Glenn van de Ven
Keyword(s):  
Large Scale ◽  
Stellar Population ◽  
Line Strength ◽  
Elliptical Galaxies ◽  
Formation Mechanisms ◽  
Population Parameters ◽  
Irregular Galaxies ◽  
Model Predictions ◽  
Dwarf Elliptical Galaxies ◽  
Star Formation Histories

AbstractIn our contribution we show the effects of environmental evolution on cluster and field dwarf elliptical galaxies (dEs), presenting the first large-scale integral-field spectroscopic data for this galaxy class. Our sample con sists of 12 galaxies and no two of them are alike. We find that the level of rotation is not tied to flattening; we observe kinematic twists; we discover large-scale kinematically-decoupled components; we see varying gradient s in line-strength maps: from nearly flat to strongly peaked in the center. The great variety of morphological, kinematic, and stellar population parameters seen in our data supports the claim that dEs are defunct dwarf spiral/irregular galaxies and points to a formation scenario that allows for a stochastic shaping of galaxy properties. The combined influence of ram-pressure stripping and harassment fulfills these requirements, still, the exact impact of the two is not yet understood. We further investigate the properties of our sample by performing a detailed comprehensive analysis of its kinematic, dynamical, and stellar population parameters. The combined knowledge of the dynamical properties and star-formation histories, together with model predictions for different formation mechanisms, will be used to quant itatively determine the actual transformation paths for these galaxies.

scholarly journals Galaxy Populations and Evolution in Clusters. IV. Deep HiObservations of Dwarf Elliptical Galaxies in the Virgo Cluster

2003 ◽  
Vol 591 (1) ◽  
pp. 167-184 ◽  
Author(s):  
Christopher J. Conselice ◽  
Karen O’Neil ◽  
John S. Gallagher ◽  
Rosemary F. G. Wyse
Keyword(s):  
Elliptical Galaxies ◽  
Virgo Cluster ◽  
Dwarf Elliptical Galaxies ◽  
Galaxy Populations

scholarly journals HST WFPC-2 Imaging of Four Nearby LSB Galaxies

1999 ◽  
Vol 171 ◽  
pp. 210-213
Author(s):  
Karen O’Neil
Keyword(s):  
Elliptical Galaxies ◽  
Virgo Cluster ◽  
Small Scale ◽  
Giant Stars ◽  
Structural Peculiarities ◽  
The Galaxy ◽  
Dwarf Elliptical Galaxies ◽  
Giant Branch Stars ◽  
Lsb Galaxies ◽  
Spiral Arm

AbstractBetween May, 1996 and January, 1997 HST WFPC-2 images of four nearby LSB galaxies were taken through both the 8140Å and 3000Å filters. The first galaxy imaged, UGC 12695, is a nearby (z~0.021) LSB disk galaxy. UGC 12695 has an unusual morphology, consisting of a Y-shaped nucleus surrounded by a faint spiral arm. Additionally, numerous HI regions are spread throughout the galaxy. One of the surprising discoveries with the WFPC2 imaging was that a number of what were previously believed to be structural peculiarities in the galaxy are actually background galaxies. Once the effects of these galaxies are removed, the resultant U—I color of UGC 12695 is only −0.2, making it possibly the bluest galaxy in the local universe. When combined with the metallicity studies of McGaugh (1992), these colors indicate UGC 12695 to be a highly unevolved galaxy.The other three galaxies imaged - V1L4, V2L8, and V7L3 - are dwarf elliptical galaxies located in the Virgo cluster. The intent of their images was to determine the galaxies’ small scale structure and place limits on the density and type of giant branch stars within each galaxy. Placed at the distance of the Virgo cluster, luminosity fluctuations indicate the galaxies to contain only from 4 – 13 stars per pixel, coinciding with a K/M giant ratio ranging from 6 to ∞ (no M giant stars). Additionally, we found no evidence for stellar clumping in these galaxies although an extremely red, extremely small bulge was found at the core of V2L8.

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