Lines of Galaxies from Radio Sources

Arp, Halton

doi:10.1086/128602

Cited by 39 publications

(15 citation statements)

References 11 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…The existence of a preferred axis for Virgo's bright elliptical galaxies had previously been noted by Arp (1968) and Binggeli et al ( 1987). In this section we follow the analysis of West & Blakeslee ( 2000) using an expanded sample of more precise SBF distances, with the aim of determining the threedimensional distribution of early-type Virgo galaxies, as traced by the ACSVCS sample.…”

Section: The Principal Axis Of the Virgo Clustermentioning

confidence: 85%

The ACS Virgo Cluster Survey. XIII. SBF Distance Catalog and the Three‐dimensional Structure of the Virgo Cluster

Mei

Blakeslee

Côté

et al. 2007

ApJ

682

833

View full text Add to dashboard Cite

The ACS Virgo Cluster Survey consists of HST ACS imaging for 100 early-type galaxies in the Virgo Cluster, observed in the F475W (%SDSS g) and F850LP (%SDSS z) filters. We derive distances for 84 of these galaxies using the method of surface brightness fluctuations (SBFs), present the SBF distance catalog, and use this database to examine the three-dimensional distribution of early-type galaxies in the Virgo Cluster. The SBF distance moduli have a mean (random) measurement error of 0.07 mag (0.5 Mpc), or roughly 3 times better than previous SBF measurements for Virgo Cluster galaxies. Five galaxies lie at a distance of d % 23 Mpc and are members of the W 0 cloud. The remaining 79 galaxies have a narrow distribution around our adopted distance of hdi ¼ 16:5 AE 0:1 (random mean error) AE1.1 Mpc (systematic). The rms distance scatter of this sample is (d ) ¼ 0:6 AE 0:1 Mpc, with little or no dependence on morphological type or luminosity class (i.e., 0:7 AE 0:1 and 0:5 AE 0:1 Mpc for the giants and dwarfs, respectively). The back-to-front depth of the cluster measured from our sample of early-type galaxies is 2:4 AE 0:4 Mpc (i.e., AE 2 of the intrinsic distance distribution). The M87 (cluster A) and M49 (cluster B) subclusters are found to lie at distances of 16:7 AE 0:2 and 16:4 AE 0:2 Mpc, respectively. There may be a third subcluster associated with M86. A weak correlation between velocity and line-of-sight distance may be a faint echo of the cluster velocity distribution not having yet completely virialized. In three dimensions, Virgo's early-type galaxies appear to define a slightly triaxial distribution, with axis ratios of (1: 0.7 : 0.5). The principal axis of the best-fit ellipsoid is inclined $20 Y 40 from the line of sight, while the galaxies belonging to the W 0 cloud lie on an axis inclined by $10 Y15 .

show abstract

Section: The Principal Axis Of the Virgo Clustermentioning

confidence: 85%

The ACS Virgo Cluster Survey. XIII. SBF Distance Catalog and the Three‐dimensional Structure of the Virgo Cluster

Mei

Blakeslee

Côté

et al. 2007

ApJ

682

833

View full text Add to dashboard Cite

show abstract

“…Another explanation for the formation of bridges took jets into account (Ambartsumian, 1961;Arp, 1967Arp, , 1968Arp, , 1972. When a massive galaxy ejects a fraction of its matter (gaseous, stellar or both) from its nucleus, a symmetrical pair of jets is formed but rapidly slowed down by the high densities encountered along its path 1 .…”

Section: A Controversial Scenariomentioning

confidence: 99%

Tides in Colliding Galaxies

Duc

Renaud

2013

Lecture Notes in Physics

View full text Add to dashboard Cite

Long tails and streams of stars are the most noticeable upshots of galaxy collisions. Their origin as gravitational, tidal, disturbances has however been recognized only less than fifty years ago and more than ten years after their first observations. This Review describes how the idea of galactic tides emerged, in particular thanks to the advances in numerical simulations, from the first ones that included tens of particles to the most sophisticated ones with tens of millions of them and state-of-the-art hydrodynamical prescriptions. Theoretical aspects pertaining to the formation of tidal tails are then presented. The third part of the review turns to observations and underlines the need for collecting deep multi-wavelength data to tackle the variety of physical processes exhibited by collisional debris. Tidal tails are not just stellar structures, but turn out to contain all the components usually found in galactic disks, in particular atomic / molecular gas and dust. They host star-forming complexes and are able to form star-clusters or even second-generation dwarf galaxies. The final part of the review discusses what tidal tails can tell us (or not) about the structure and content of present-day galaxies, including their dark components, and explains how tidal tails may be used to probe the past evolution of galaxies and their mass assembly history. On-going deep wide-field surveys disclose many new lowsurface brightness structures in the nearby Universe, offering great opportunities for attempting galactic archeology with tidal tails.

show abstract

“…5. Connected with the approach is Arp's (1967Arp's ( , 1968b suggestions that radio sources form pairs around peculiar galaxies and that radio galaxies are origins for lines of galaxies.…”

Section: M158mentioning

confidence: 99%