Are the Perseus--Pisces chain and the Pavo--Indus wall connected?

Nella, H. Di; Couch, Warrick J.; Paturel, G.; Parker, Quentin A.

doi:10.1093/mnras/283.2.367

Cited by 21 publications

(13 citation statements)

References 18 publications

Supporting

Mentioning

Contrasting

Unclassified

Order By: Relevance

“…These features are seen in other reconstructions of the local neighborhood (di Nella et al 1996;Branchini et al 1999;). (2007) emphasize the important dynamic role of voids.…”

Section: The Volume Within 40 Mpcmentioning

confidence: 56%

Three-Dimensional Velocity and Density Reconstructions of the Local Universe With Cosmicflows-1

Courtois

Hoffman

Tully

et al. 2011

ApJ

View full text Add to dashboard Cite

This paper presents an analysis of the local peculiar velocity field based on the Wiener Filter reconstruction method. We used our currently available catalog of distance measurements containing 1,797 galaxies within 3000 km/s: Cosmicflows-1. The Wiener Filter method is used to recover the full 3D peculiar velocity field from the observed map of radial velocities and to recover the underlying linear density field. The velocity field within a data zone of 3000 km/s is decomposed into a local component that is generated within the data zone and a tidal one that is generated by the mass distribution outside that zone. The tidal component is characterized by a coherent flow toward the Norma-Hydra-Centaurus (Great Attractor) region while the local component is dominated by a flow toward the Virgo Cluster and away from the Local Void. A detailed analysis shows that the local flow is predominantly governed by the Local Void and the Virgo Cluster plays a lesser role. The analysis procedure was tested against a mock catalog. It is demonstrated that the Wiener Filter accurately recovers the input velocity field of the mock catalog on the scale of the extraction of distances and reasonably recovers the velocity field on significantly larger scales. The Bayesian Wiener Filter reconstruction is carried out within the ΛCDM WMAP5 framework.The Wiener Filter reconstruction draws particular attention to the importance of voids in proximity to our neighborhood. The prominent structure of the Local Supercluster is wrapped in a horseshoe collar of under density with the Local Void as a major component.

show abstract

“…These features are seen in other reconstructions of the local neighborhood (di Nella et al 1996;Branchini et al 1999;). (2007) emphasize the important dynamic role of voids.…”

Section: The Volume Within 40 Mpcmentioning

confidence: 56%

Three-Dimensional Velocity and Density Reconstructions of the Local Universe With Cosmicflows-1

Courtois

Hoffman

Tully

et al. 2011

ApJ

View full text Add to dashboard Cite

show abstract

“…It is easily the longest of the structures directly connected to Centaurus. It was entertained that this feature might directly connect with the important Perseus-Pisces chain (di Nella et al 1996) through the Southern Wall. The Pavo-Indus filament, the Southern Supercluster filament (soon to be discussed), and the Southern Wall are sectional boundaries of the immense Sculptor Void (Fairall 1998).…”

Section: Centaurus Cluster: a Local Nodementioning

confidence: 99%

Cosmography of the Local Universe

et al. 2013

View full text Add to dashboard Cite

The large scale structure of the universe is a complex web of clusters, filaments, and voids. Its properties are informed by galaxy redshift surveys and measurements of peculiar velocities. Wiener Filter reconstructions recover three-dimensional velocity and total density fields. The richness of the elements of our neighborhood are revealed with sophisticated visualization tools. A key component of this paper is an accompanying movie. The ability to translate and zoom helps the viewer follow structures in three dimensions and grasp the relationships between features on different scales while retaining a sense of orientation. The ability to dissolve between scenes provides a technique for comparing different information, for example, the observed distribution of galaxies, smoothed representations of the distribution accounting for selection effects, observed peculiar velocities, smoothed and modeled representations of those velocities, and inferred underlying density fields. The agreement between the large scale structure seen in redshift surveys and that inferred from reconstructions based on the radial peculiar velocities of galaxies strongly supports the standard model of cosmology where structure forms from gravitational instabilities and galaxies form at the bottom of potential wells.

show abstract

“…Larger TDR values indicate a best confidence for radial velocity determination. Nella et al (1996) data. CS* indicates that this galaxy has a radial velocity determined in both runs; MF, Mathewson & Ford (1996); and SWb, Sekiguchi & Wolstencroft (1993).…”

Section: Radial Velocitiesmentioning

confidence: 99%

Optical spectroscopy for a sample of southern binary galaxies

Silva

Souza²

2006

A&A

View full text Add to dashboard Cite

Aims. This work is part of a joint observational program aiming to get photometric and spectroscopic information on southern pairs of galaxies. We present optical long-slit spectroscopic data on 80 probable components of pairs, 61 of them collected with a spectral resolution of 3.4 Å, and 19 with 12 Å. Nevertheless, our analysis takes into account 53 components of pairs with better spectral resolution, as 8 of these target galaxies actually belong to optical pairs. For the sample with better resolution, the covered wavelength range is 5724 ≤ λ ≤ 7036 Å. The spectroscopic and photometric information is gathered for an analysis relating galaxy morphologies to their spectra. Methods. We use H α + [N II ] and H α equivalent widths as star formation tracers for the central region of our sample galaxies, and we classify the spectra according to the emission lines' relative strength by looking at their behavior. Results. Some of our sample galaxies exhibit high central star formation, most of them belonging to close pairs. However, not all galaxies' components of close pairs show this behavior. This may be a clue that besides interaction, other agents can stimulate central emission in binary galaxies. We suggest an enhancement in the number of galaxies with peculiar spectra (probably Seyferts) in our binary sample, when compared to isolated galaxies. Our data indicates that the morphological types of interacting galaxies are related to their spectral characteristics, as almost all early-type galaxies of our sample do not exhibit central optical emission. We note that the star formation activity is most likely to take place in both pairs' components, with a slightly higher mean strength for the less bright component of the pair. It is interesting to point out that most spirals exhibiting a strong HII emission line spectra present either a bar or a peculiarity, but on a general basis we do not find an enhancement of star formation in our interaction sample.

show abstract

Are the Perseus--Pisces chain and the Pavo--Indus wall connected?

Cited by 21 publications

References 18 publications

Three-Dimensional Velocity and Density Reconstructions of the Local Universe With Cosmicflows-1

Three-Dimensional Velocity and Density Reconstructions of the Local Universe With Cosmicflows-1

Cosmography of the Local Universe

Optical spectroscopy for a sample of southern binary galaxies

Contact Info

Product

Resources

About