The globular clusters of the dwarf elliptical galaxies NGC 147, NGC 185, and NGC 205. I - Abundances

1988 ◽  
Vol 334 ◽  
pp. 159 ◽  
Author(s):  
G. S. Da Costa ◽  
J. R. Mould
Keyword(s):  
Globular Clusters ◽  
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 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 The Nuclei of Nucleated Dwarf Elliptical Galaxies - Are they Globular Clusters?

1988 ◽  
Vol 126 ◽  
pp. 603-604 ◽  
Author(s):  
H. Zinnecker ◽  
C. J. Keable ◽  
J. S. Dunlop ◽  
R. D. Cannon ◽  
W. K. Griffiths
Keyword(s):  
Globular Clusters ◽  
Star Clusters ◽  
Physical Nature ◽  
Elliptical Galaxies ◽  
Virgo Cluster ◽  
Central Nucleus ◽  
Ccd Observations ◽  
Total Light ◽  
Dwarf Elliptical Galaxies ◽  
Parent Galaxy

It came as a great surprise that many dwarf elliptical galaxies of very low surface brightness in the Virgo Cluster have conspicuous bright star-like nuclei (Reaves 1983, Binggeli, Sandage and Tammann 1985). These nuclei are at least a factor of 10 more luminous than the brightest globular clusters in the Local Group and comparable only to the very brightest globulars surrounding M87. They contain a considerable fraction (1 to 20%) of the total light of the parent galaxy (Binggeli, priv. commun.). Their physical nature and origin are a matter of debate (Zinnecker et al. 1985, van den Bergh 1985, Norman 1986, Zinnecker 1986) but optical spectroscopy for 3 objects indicates a stellar composition with a range similar to globular clusters (Bothun et al. 1985). It has been suggested that a central nucleus is formed when off-center bound star clusters migrate to the center as a consequence of dynamical friction (Norman 1986). Support for such a scenario comes from CCD observations of IC 3475 which reveal numerous knots near the center of this dwarf irregular galaxy (Vigroux et al. 1986). These knots have the same color as the parent galaxy and are interpreted as intermediate age star clusters.

scholarly journals Embedded disks in Fornax dwarf elliptical galaxies

2003 ◽  
Vol 400 (1) ◽  
pp. 119-125 ◽  
Author(s):  
S. De Rijcke ◽  
H. Dejonghe ◽  
W. W. Zeilinger ◽  
G. K. T. Hau
Keyword(s):  
Elliptical Galaxies ◽  
Dwarf Elliptical Galaxies ◽  
Embedded Disks

scholarly journals Physical Properties of Nearby Dwarf Elliptical Galaxies

2006 ◽  
Vol 2 (S235) ◽  
pp. 69-69
Author(s):  
M. R. Seo ◽  
H. B. Ann
Keyword(s):  
Physical Properties ◽  
Stellar Populations ◽  
Elliptical Galaxies ◽  
High Density ◽  
Emission Lines ◽  
Dwarf Elliptical Galaxies ◽  
Nuclear Regions

AbstractMost dwarf elliptical galaxies except for ‘dE, N’ galaxies which are characterized by young stellar populations in the nuclear regions are located in the high density environment. The colors and spectra of ‘dE, N’ galaxies are different from other types, in the sense that they have redder colors with little emission lines. The majority of dwarf elliptical galaxies are younger than 7 Gyr with metallicity larger than [z/H]=−0.5.

scholarly journals Surface brightness fluctuation distances for nearby dwarf elliptical galaxies

2001 ◽  
Vol 380 (1) ◽  
pp. 90-101 ◽  
Author(s):  
H. Jerjen ◽  
R. Rekola ◽  
L. Takalo ◽  
M. Coleman ◽  
M. Valtonen
Keyword(s):  
Surface Brightness ◽  
Elliptical Galaxies ◽  
Brightness Fluctuation ◽  
Dwarf Elliptical Galaxies
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