scholarly journals Distribution of Dark Matter in Polar Ring Galaxies

1987 ◽  
Vol 117 ◽  
pp. 315-315
Author(s):  
Bradley C. Whitmore ◽  
Douglas B. McElroy ◽  
François Schweizer ◽  
Vera C. Rubin
Keyword(s):  
Dark Matter ◽  
Gravitational Potential ◽  
Three Dimensions ◽  
Polar Ring ◽  
Ring Galaxies ◽  
Spherical Potential

The discovery of SO galaxies with polar rings makes it possible to directly measure the gravitational potential of a galaxy in three dimensions. Schweizer, Whitmore and Rubin (1983) find a spherical potential in the case of A0136-0801. We have observed three more polar ring galaxies using the 4 meter telescope at CTIO. The following table summarizes the results for these three systems as well as A0136-0801, and figure 1 shows an example of the data.

scholarly journals To be or not to be oblate: the shape of the dark matter halo in polar ring galaxies

2014 ◽  
Vol 441 (3) ◽  
pp. 2650-2662 ◽  
Author(s):  
S. A. Khoperskov ◽  
A. V. Moiseev ◽  
A. V. Khoperskov ◽  
A. S. Saburova
Keyword(s):  
Dark Matter ◽  
Dark Matter Halo ◽  
Polar Ring ◽  
Ring Galaxies

scholarly journals Simulating the galactic system in interaction AM 2229-735 and the formation of its polar structure

2019 ◽  
Author(s):  
Luis F Quiroga ◽  
J C Muñoz-Cuartas ◽  
I Rodrigues ◽  
Noam I Libeskind
Keyword(s):  
Dark Matter ◽  
Initial Conditions ◽  
Polar Structure ◽  
Polar Ring ◽  
Galactic System ◽  
Galaxy Disk ◽  
Ring Galaxies ◽  
Tidal Stream ◽  
Minor Mergers ◽  
A Minor

Abstract We study the formation of polar ring galaxies via minor mergers. We used N-body+hydrodynamics simulations to reproduce the dynamics of the observed system AM 2229-735 that is a minor merger whose interaction signals are those of a progenitor for a polar ring galaxy. We used the observational information of the system to get initial conditions for the orbit and numerical realisations of the galaxies to run the simulations. Our simulations reproduce the global characteristics of interaction observed in the system such as arms and a material bridge connecting the galaxies. As a merger remnant, we found a quasi-stable and self gravitating planar tidal stream with dark matter, stars and gas orbiting in a plane approximately perpendicular to the main galaxy disk leading in the future to a polar ring galaxy. We studied the dynamical conditions of the polar structure and found evidence suggesting that this kind of merger remnant can settle down in a disk-like structure with isothermal support, providing inspiring evidence about the process of formation of galactic disks and providing a potentially independent scenario to study the presence of dark matter in this kind of galaxies.

scholarly journals Dark Matter in the Polar Ring Spiral NGC 660

1995 ◽  
Vol 164 ◽  
pp. 435-435
Author(s):  
Wim Van Driel
Keyword(s):  
Dark Matter ◽  
Three Dimensional ◽  
Polar Ring ◽  
Ring Galaxies ◽  
Dimensional Distribution

Polar ring galaxies, where rotation velocities can be measured in two orthogonal planes, are generally considered to be ideal objects for studies of the three-dimensional distribution of dark matter in galaxies.

9. The Outer Galactic Environment

1988 ◽  
Vol 20 (01) ◽  
pp. 396-404
Keyword(s):  
Dark Matter ◽  
Galactic Plane ◽  
Dwarf Galaxies ◽  
Single System ◽  
Narrow Strip ◽  
Polar Ring ◽  
Ring Galaxies

One of the highlights of the study of the galactic environment is the demonstration that companions and hydrogen clouds surrounding our Galaxy form a ring-like structure similar to that surrounding external polar-ring galaxies. Probably this feature is common in giant galaxies. Dwarf galaxies may possess their own dark coronas, which fact, if confirmed, puts severe constraints on the nature of dark matter. Available evidence confirms earlier suggestions that our Galaxy with its massive corona, companions, and surrounding gas forms a single system with many mutual interactions. Most companions of our Galaxy as well as the main hydrogen streams are located in a narrow strip inclined 70° to the galactic plane.

scholarly journals Structure and Kinematics of Polar Ring Galaxies: New Observations and Estimation of the Dark Halo Shape

2015 ◽  
Vol 24 (1) ◽  
Author(s):  
A. Moiseev ◽  
S. Khoperskov ◽  
A. Khoperskov ◽  
K. Smirnova ◽  
A. Smirnova ◽  
...  
Keyword(s):  
Dark Matter ◽  
Observational Data ◽  
Dark Matter Halo ◽  
Dark Halo ◽  
Dark Matter Halos ◽  
Ionized Gas ◽  
Polar Ring ◽  
Gas Kinematics ◽  
Open Questions ◽  
Ring Galaxies

AbstractThe polar ring galaxies (PRGs) represent an interesting type of peculiar systems in which the outer matter is rotating in the plane which is roughly perpendicular to the disk of the main galaxy. Despite the long-lasting study of the PRGs, the amount of observational data detailed enough is insufficient; there still remain many open questions. Among the most interesting issues, there are: estimating the flattening of dark matter halos in these systems and verifying the assumption that the most massive polar structures were formed by accretion of the matter from intergalactic filaments. The new catalog recently compiled by our team using SDSS images increased, by several times, the number of known PRGs. The current paper gives an overview of our latest results on the study of morphological and photometric structure of the PRGs. Using the stellar and ionized gas kinematics data based on spectroscopic observations with the Russian 6-m telescope, we estimate the shape of dark matter halo in individual galaxies.

scholarly journals AM2020–5050: an Elliptical Galaxy with an Outer Ring

1987 ◽  
Vol 127 ◽  
pp. 413-414
Author(s):  
Bradley Whitmore ◽  
François Schweizer
Keyword(s):  
Gravitational Potential ◽  
Velocity Dispersion ◽  
Elliptical Galaxy ◽  
Rotational Velocity ◽  
Gaseous Disk ◽  
Polar Ring ◽  
Photometric And Spectroscopic Observations ◽  
The Galaxy ◽  
Ring Galaxies ◽  
Optical Ring

Photometric and spectroscopic observations show that the inner component of AM2020—5050 is an elliptical galaxy, unlike other polar-ring galaxies which have an SO disk at the center. A comparison of the central velocity dispersion with the rotational velocity in the ring suggests the presence of a nearly spherical gravitational potential. The inner component has a rapidly rotating core with rotational velocities at 3″ substantially higher than at 8″. Although the optical ring is quite narrow, Hα emission is observed all the way through the center of the galaxy, indicating the presence of an extended gaseous disk.

Distribution of Dark Matter in Polar Ring Galaxies

1987 ◽  
pp. 315-315
Author(s):  
Bradley C. Whitmore ◽  
Douglas B. McElroy ◽  
François Schweizer ◽  
Vera C. Rubin
Keyword(s):  
Dark Matter ◽  
Polar Ring ◽  
Ring Galaxies

Dust and infrared imaging of polar ring galaxies

1995 ◽  
Vol 43 (10-11) ◽  
pp. 1377-1388 ◽  
Author(s):  
M. Arnaboldi ◽  
K.C. Freeman ◽  
P.D. Sackett ◽  
L.S. Sparke ◽  
M. Capaccioli
Keyword(s):  
Infrared Imaging ◽  
Polar Ring ◽  
Ring Galaxies

scholarly journals Supernovae Blast Waves in Proto-Dwarf Galaxies

1988 ◽  
Vol 101 ◽  
pp. 513-520
Author(s):  
Alberto Noriego-Crespo ◽  
Peter Bodenheimer
Keyword(s):  
Dark Matter ◽  
Mass Loss ◽  
Gravitational Potential ◽  
Cold Dark Matter ◽  
First Generation ◽  
Dwarf Galaxies ◽  
Blast Waves ◽  
The One

AbstractGas mass loss in proto-dwarf galaxies can be efficiently driven out by blast waves created by the first generation of supernovae. There is, however, a threshold set by the total gravitational potential beyond which gas mass loss does not occur. This limit is in agreement with the one predicted by some Cold Dark Matter senarios.

scholarly journals The Polar-Ring Galaxies NGC 2685 and NGC 3808B (W 300)

1990 ◽  
Vol 124 ◽  
pp. 231-244
Author(s):  
V. P. Reshetnikov ◽  
V. A. Yakovleva
Keyword(s):  
Intergalactic Medium ◽  
Close Encounter ◽  
Main Body ◽  
Polar Plane ◽  
Polar Ring ◽  
Ring Galaxies ◽  
Companion Galaxy ◽  
Peculiar Galaxies

Polar-ring galaxies (PRG) are among the most interesting examples of interaction between galaxies. A PRG is a galaxy with an elongated main body surrounded by a ring (or a disk) of stars, gas, and dust rotating in a near-polar plane (Schweizer, Whitmore, and Rubin, 1983). Accretion of matter by a massive lenticular galaxy from either intergalactic medium or a companion galaxy is usually considered as an explanation of the observed structure of PRG. In the latter case there are two possibilities: (1) capture and merging of a neighbor galaxy, and (2) accretion of mass from a companion galaxy during a close encounter. Two PRG formation scenarios just mentioned are illustrated here by the results of our observations of the peculiar galaxies NGC 2685 and NGC 3808B.

Sign in / Sign up

Export Citation Format

Share Document