scholarly journals Spectroscopic Metallicities for Fornax Ultracompact Dwarf Galaxies, Globular Clusters, and Nucleated Dwarf Elliptical Galaxies

2006 ◽  
Vol 131 (5) ◽  
pp. 2442-2451 ◽  
Author(s):  
S. Mieske ◽  
M. Hilker ◽  
L. Infante ◽  
A. Jordán
Keyword(s):  
Globular Clusters ◽  
Dwarf Galaxies ◽  
Elliptical Galaxies ◽  
Dwarf Elliptical Galaxies

scholarly journals GMOS Spectroscopy of Globular Clusters in Dwarf Elliptical Galaxies

2007 ◽  
Vol 3 (S246) ◽  
pp. 429-430
Author(s):  
Bryan W. Miller ◽  
Jennifer Lotz ◽  
Michael Hilker ◽  
Markus Kissler-Patig ◽  
Thomas Puzia
Keyword(s):  
Globular Clusters ◽  
Milky Way ◽  
Elliptical Galaxies ◽  
Preliminary Results ◽  
Dwarf Elliptical Galaxies ◽  
Milky Way Halo

AbstractWe present a Gemini/GMOS program to measure spectroscopic metallicities and ages of globular clusters (GCs) and nuclei in dwarf elliptical galaxies in the Virgo and Fornax Clusters. Preliminary results indicate that the globular clusters are old and metal-poor, very similar to the GCs in the Milky Way halo. The nuclei tend to be more metal-rich than the globular clusters but more metal-poor and older, on average, than the stars in the bodies of the galaxies. The [α/Fe] ratio appears to be solar for the GCs, nuclei, and dEs, but the uncertainties do not exclude some globular clusters from being enhanced in alpha elements.

scholarly journals Tidal Effects on Spherical Stellar Systems

1975 ◽  
Vol 69 ◽  
pp. 53-55
Author(s):  
D. W. Keenan ◽  
K. A. Innanen
Keyword(s):  
Internal Structure ◽  
Globular Clusters ◽  
Elliptical Galaxies ◽  
Star Cluster ◽  
Stellar Systems ◽  
Tidal Effects ◽  
Dwarf Elliptical Galaxies

Many self-gravitating stellar systems are satellites of larger galaxies and must therefore be subjected to the tidal field of the parent system. Examples are the globular clusters and dwarf elliptical galaxies, which are satellites of our Galaxy. Most previous studies of tidal effects have been highly simplified, e.g. clusters in circular planar galactic orbits (Bok, 1934), or have assumed that the tidal field acts to limit the size of a star cluster without any effects on its internal structure or stability (Spitzer and Shapiro, 1972; Spitzer and Thuan, 1972).

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 Globular Clusters in Dwarf Elliptical Galaxies

2002 ◽  
Vol 207 ◽  
pp. 303-305
Author(s):  
Bryan W. Miller ◽  
Jennifer M. Lotz ◽  
Henry C. Ferguson ◽  
Massimo Stiavelli ◽  
Bradley C. Whitmore
Keyword(s):  
Globular Cluster ◽  
Globular Clusters ◽  
Luminosity Function ◽  
Elliptical Galaxies ◽  
Preliminary Results ◽  
The Galaxy ◽  
Dwarf Elliptical Galaxies

We present preliminary results on the shape of the globular cluster luminosity function and the colors and inferred metallicities of the clusters in dwarf elliptical galaxies imaged with HST. The luminosity function (LF) of the GC candidates is consistent with a Gaussian-shaped LF similar to that in giant ellipticals. Also, with a mean color of (V - I) = 0.94, most of the GCs appear to be old and metal-poor ([Fe/H] = −1.4) like GCs in the Galaxy and in nearby giant ellipticals. This suggests that the bulk of the clusters were formed more than 10 Gyr ago.

scholarly journals The Dynamical Mass of the Young Cluster W3 in NGC 7252: Heavy-Weight Globular Cluster or Ultra-Compact Dwarf Galaxy?

2005 ◽  
Vol 13 ◽  
pp. 169-170
Author(s):  
Claudia Maraston ◽  
N. Bastian ◽  
R. P. Saglia ◽  
Markus Kissler-Patig ◽  
François Schweizer ◽  
...  
Keyword(s):  
Globular Clusters ◽  
Stellar Population ◽  
Milky Way ◽  
Dwarf Galaxy ◽  
Elliptical Galaxies ◽  
Star Cluster ◽  
Dynamical Mass ◽  
Fundamental Plane ◽  
Dwarf Elliptical Galaxies ◽  
First Time

AbstractWe have measured the dynamical mass of the highly luminous star cluster W3 in the young merger remnant galaxy NGC 7252. The value is Mdyn = (8 ± 2) × 107M⊙, and represents the highest dynamically-confirmed mass for an extra-galactic star cluster so far. The dynamical mass is in excellent agreement with the luminous mass (Maraston et al. 2001). This results from the use of stellar population models that include correctly the brightest AGB stellar phase, dominant in young stellar populations. To classify W3, we employ the fundamental plane of stellar systems (Bender, Burstein & Faber 1992), for the first time in these kinds of studies. We find that W3 lies far from typical Milky Way globular clusters, but it is also far from the heavyweights ωCen in the Milky Way and G1 in M31, because it is too extended for its mass, and from dwarf elliptical galaxies because it is much more compact for its mass. Instead W3 lies close to the ultra-compact Fornax objects (Drinkwater et al. 2003) and to the compact elliptical M32, possibly shedding light on the still mysterious nature of these objects. A previously deserted region of the fundamental plane starts to be populated.

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)

Evolution of dwarf galaxies in a semi-analytic galaxy formation model

2018 ◽  
Vol 14 (S344) ◽  
pp. 491-494
Author(s):  
Masahiro Nagashima ◽  
Motohiro Enoki ◽  
Tomoaki Ishiyama ◽  
Masakazu A. R. Kobayashi ◽  
Ryu Makiya ◽  
...  
Keyword(s):  
Galaxy Formation ◽  
Cold Dark Matter ◽  
Dwarf Galaxies ◽  
Elliptical Galaxies ◽  
Dynamical Response ◽  
Cold Dark Matter Model ◽  
Gas Removal ◽  
Dwarf Elliptical Galaxies ◽  
Velocity Dispersions ◽  
Dark Matter Model

AbstractDwarf galaxies provide us many important clues to understanding of galaxy formation. By using the current version of our own semi-analytic model of galaxy formation, in which cosmic structure forms and evolves based on the cold dark matter model of cosmology, we analyze dwarf galaxies. We find that the model well reproduces many properties such as magnitudes, sizes, and velocity dispersions of, especially, dwarf elliptical galaxies. We also find that the dynamical response of the gravitational potential well of dwarf galaxies to the supernova-induced gas removal plays a very important role to obtain large sizes and small velocity dispersions as observed.

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