scholarly journals Extended stellar kinematics of elliptical galaxies in the Fornax cluster

1998 ◽  
Vol 133 (3) ◽  
pp. 325-336 ◽  
Author(s):  
A. W. Graham ◽  
M. M. Colless ◽  
G. Busarello ◽  
S. Zaggia ◽  
G. Longo
Keyword(s):  
Elliptical Galaxies ◽  
Stellar Kinematics ◽  
Fornax Cluster

scholarly journals A Search for M32-like Galaxies in the Fornax Cluster using Flair

1995 ◽  
Vol 148 ◽  
pp. 106-110
Author(s):  
Brett Holman ◽  
Michael Drinkwater ◽  
Michael Gregg
Keyword(s):  
Luminosity Function ◽  
Large Scale ◽  
Elliptical Galaxies ◽  
Fornax Cluster

AbstractResults of a spectroscopic search for M32-like compact elliptical galaxies in the Fornax cluster are presented. None were found, which suggests that these objects represent the low luminosity end of the giant elliptical luminosity function, rather than being formed by tidal stripping. The sample is used to investigate the large-scale distribution of bright ellipticals.

scholarly journals The Radial Velocities of Planetary Nebulae in NGC 3379

1993 ◽  
Vol 155 ◽  
pp. 570-570
Author(s):  
Robin Ciardullo ◽  
George Jacoby
Keyword(s):  
Radial Velocity ◽  
Absorption Line ◽  
Planetary Nebula ◽  
Velocity Dispersion ◽  
Planetary Nebulae ◽  
Elliptical Galaxies ◽  
Emission Lines ◽  
Surface Photometry ◽  
Stellar Kinematics ◽  
Velocity Measurements

Several authors have analyzed the kinematics of elliptical galaxies using surface photometry in combination with absorption line velocity dispersion measurements. However, these analyses never explore the halos of galaxies, since the best absorption line measurements extend only ∼1 re. The only way to extend our knowledge of stellar kinematics to larger radii is to use the emission lines of planetary nebula for radial velocity measurements.

scholarly journals Dust and the observed dark matter content of galaxies

2004 ◽  
Vol 220 ◽  
pp. 343-344 ◽  
Author(s):  
Maarten Baes ◽  
Herwig Dejonghe ◽  
Jonathan I. Davies
Keyword(s):  
Dark Matter ◽  
Interstellar Dust ◽  
Optical Rotation ◽  
Elliptical Galaxies ◽  
Matter Content ◽  
Dark Matter Halo ◽  
Stellar Kinematics ◽  
The Galaxy ◽  
Dust Attenuation ◽  
Radiative Transfer Modeling

Using detailed Monte Carlo radiative transfer modeling, we examine the effects of absorption and scattering by interstellar dust on the observed kinematics of galaxies. Our modeling results have a direct impact on the derivation of the properties of dark matter haloes around both elliptical and spiral galaxies. We find that interstellar dust has a very significant effect on the observed stellar kinematics of elliptical galaxies, in the way that it mimics the presence of a dark matter halo. Taking dust into account in kinematical modeling procedures can reduce or even eliminate the need for dark matter at a few effective radii. Dust profoundly affects the optical rotation curve and stellar kinematics of edge-on disc galaxies. This effect, however, is significantly reduced when the galaxy is more than a few degrees from strictly edge-on. These results demonstrate that dust attenuation cannot be invoked as a possible mechanism to reconcile the discrepancies between the observed shallow slopes of LSB galaxy rotation curves and the dark matter cusps found in CDM cosmological simulations.

scholarly journals Stellar Kinematics of Elliptical Galaxies in Pairs

1990 ◽  
Vol 124 ◽  
pp. 33-36
Author(s):  
Rainer Madejsky ◽  
Ralf Bender
Keyword(s):  
Radial Velocity ◽  
Elliptical Galaxy ◽  
Orbital Plane ◽  
Elliptical Galaxies ◽  
Line Of Sight ◽  
Stellar Kinematics ◽  
Velocity Difference ◽  
The Moment ◽  
Inner Parts ◽  
Very High

Observations of elliptical galaxy pairs allow the study of different states of tidal interaction between galaxies. The comparison with normal elliptical galaxies directly reveals the disturbed morphological and kinematical properties. Numerical simulations have shown that with the known initial luminosity profile, the time elapsed since closest approach between two galaxies can be estimated from the radial position of the disturbances (Aguilar and White, 1986).The two galaxy pairs Arp 166 (NGC 750/1) and 3C 278 (NGC 4782/3) considered here exhibit distorted and nonconcentric isophotes (cf. Madejsky, 1989). In Arp 166 the major relative shift of the centers of the isophotes occurs in the outer parts while in 3C 278 the nonconcentric isophotes are more pronounced in the inner parts of the galaxies, suggesting that more time ha&elapsed since the moment of closest approach in Arp 166 than in 3C 278. Furthermore, in Arp 166, both galaxies have the same radial velocity, implying that their orbital plane is perpendicular to the line of sight. In turn, the galaxies NGC 4782 and NGC 4783 are moving with a very high radial velocity difference of 680kms-1. Taking into account the location of both galaxies, which are the dominant members of a small group of about 25 galaxies (De Souza and Quintana, 1990), the true velocity difference probably is not much higher than the observed radial velocity difference. Therefore it is very likely that we are viewing at high inclination onto (i.e. nearly parallel to) the orbital plane of the galaxies NGC 4782 and 4783.

scholarly journals An Automated Search for Low Surface Brightness Dwarf Elliptical Galaxies

1996 ◽  
Vol 171 ◽  
pp. 423-423
Author(s):  
Z. Morshidi ◽  
R.M. Smith ◽  
J.I. Davies
Keyword(s):  
Surface Brightness ◽  
Elliptical Galaxies ◽  
Low Surface Brightness ◽  
Dwarf Elliptical Galaxies ◽  
East And West ◽  
Automated Technique ◽  
Almost All ◽  
Fornax Cluster ◽  
Automated Search

A new automated technique applied to APM scans of UKSTU photographic plates has been used to search for LSBGs in the Fornax cluster. 92 galaxies, almost all of which were classified by Ferguson (1989) as dwarf ellipticals, were found. Fields to the East and West of the cluster were found to have 46 and 13 LSBGs, respectively, as shown in the figure below (□ are LSBGs, ▲ are brighter galaxies).

Sign in / Sign up

Export Citation Format

Share Document