Density and Radial Velocity Strucutre of the Hydra I Cluster of Galaxies

Baier, F. W.; Oleak, H.

doi:10.1002/asna.2113040602

Cited by 6 publications

(4 citation statements)

References 14 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…We note that the peripheral region accidentally includes the local peak of galaxy distribution as shown in Figure 5 (Fitchett & Merritt 1988). Baier & Oleak (1983) showed the secondary maximum in the galaxy number density distribution at the radius $50 0 from the Hydra I Cluster core in the southwestern area. They interpreted this as a substructure within the cluster.…”

Section: Total Lfs In the Hydra I Clustermentioning

confidence: 96%

“…Baier & Oleak (1983) and Richter (1989) studied the galaxy distribution and redshifts of Hydra I. They found that Hydra I is apparently isolated in redshift space, and member galaxies of Hydra I are not heavily contaminated by background /foreground galaxies.…”

Section: Introductionmentioning

confidence: 97%

“…A goal of this study is to reveal the LFs down to M ∼ −10 in the Hydra I cluster (Abell 1060) at z = 0.0126 (Struble & Rood 1999), for which such a very faint galaxy population, at M ∼ −10, has not been previously surveyed. Baier & Oleak (1983) and Richter (1989) studied the galaxy distribution and redshifts of Hydra I. They found that Hydra I is apparently isolated in redshift space and member galaxies of Hydra I are not heavily contaminated by background/foreground galaxies.…”

Section: Introductionmentioning

confidence: 99%

See 2 more Smart Citations

The Galaxy Luminosity Functions down toM~ -10 in the Hydra I Cluster

et al. 2007

View full text Add to dashboard Cite

We study the galaxy population of the Hydra I cluster in the central region and a region about 0.6 Mpc away from its center in the B and R C bands down to M $ À10 using Subaru Suprime-Cam photometry. We find that the luminosity function of the entire population has a slightly steeper slope ( $ À1:6) in the range of À20 < M < À10 than those reported for other clusters in slightly brighter ranges. The slope appears to be steeper in poorer clusters. The number of faint galaxies (M > À14) increases in the cluster center, as well as in bright galaxies. The Hydra I cluster is dominated by red dwarfs, and the luminosity function shows a significant upturn at M $ À16, as is seen in several other nearby clusters but not in the field. This upturn and the variation in the faint-end slope of the luminosity function may be caused by the cluster environment or the evolution history of individual clusters.

show abstract

Section: Total Lfs In the Hydra I Clustermentioning

confidence: 96%

Section: Introductionmentioning

confidence: 97%

Section: Introductionmentioning

confidence: 99%

See 1 more Smart Citation

The Galaxy Luminosity Functions down toM~ -10 in the Hydra I Cluster

et al. 2007

View full text Add to dashboard Cite

show abstract

“…The degree of substructure within the Hydra I Cluster is uncertain and difficult to quantify. For example, Baier & Oleak (1983) suggested an enhancement in the galaxy number density to the south of the cluster center, but it lacks the signatures of substructure that are often identified with statistical tests within 45 of the cluster core (Stein 1997;Lima-Dias et al 2021). Lima-Dias et al (2021) only identify substructure in this particular manner near the virial radius of the cluster.…”

Section: Substructure In Clustersmentioning

confidence: 99%

NGC 3314a/b and NGC 3312: Ram pressure stripping in Hydra I cluster substructure

Hess

Kotulla

Chen

et al. 2022

A&A

View full text Add to dashboard Cite

Cluster substructure and ram pressure stripping in individual galaxies are among the primary evidence for the ongoing growth of galaxy clusters as they accrete galaxies and groups from their surroundings. We present a multi-wavelength study of the center of the Hydra I galaxy cluster, including exquisite new MeerKAT H i and DECam Hα imaging which reveal conclusive evidence for ram pressure stripping in NGC 3312, NGC 3314a and NGC 3314b through compressed H i contours, well-defined H i tails, and ongoing star formation in the stripped gas. In particular, we quantify the stripped material in NGC 3312 and NGC 3314a, which makes up between 8% and 35% of the gas still in the disk, is forming stars at ∼ 0.5 M yr −1 , and extends ∼30-60 kpc from the main disk. The estimated stellar mass in the tails is an order of magnitude less than the H i mass. A fourth "ring" galaxy at the same velocity does not show signs of ram pressure in H i. In addition, we use the H i and stellar morphologies, combined with a Beta model of the hot intracluster medium, to constrain the real distances of the galaxies to the cluster center, and we use the chance alignment of NGC 3314b behind NGC 3314a to break the degeneracy between whether the galaxies are in front or in back of the cluster. The drag seen in the H i tails supports our preferred scenario that NGC 3312 and NGC 3314a are moving towards us as part of a foreground substructure which has already passed its pericenter and is on "out fall" from the cluster. The high surviving H i content of the galaxies may suggest that the substructure/intragroup medium can protect them from the harshest effects of ram pressure, or that in fact the galaxies are on more tangential orbits.

show abstract

On the Structure of the Coma Cluster of Galaxies

Baier¹

1984

Astron Nachr

Self Cite

View full text Add to dashboard Cite

The investigation of the distributions of number densities and radial velocities in the Coma cluster led us to the conclusion that this cluster possesses substructures. This result is in agreement with corresponding results for the Hydra I cluster and the Perseus cluster and with former conclusions by different authors that substructures are a typical phenomenon for a high percentage of all clusters of galaxies.Die Untersuchung der Anzahl-Dichte-Verteilung sowie der Verteilung der Radialgeschwindigkeiten im Coma-Haufen fuhrt uns zu dem Ergcbnis, daD dieser Haufen Unterstrukturen besitzt. Dieses Ergebnis steht in Einklang mit entsprechenden Ergebnissen f u r den Hydra I-Haufen und den Perseus-Haufen sowie mit den frliheren Ergebnissen verschiedener Autoren, daD Untcrstrukturen eine typische Erscheinung in einem groI3en Prozentsatz aller Galaxienhaufen sind.

show abstract

Density and Radial Velocity Strucutre of the Hydra I Cluster of Galaxies

Abstract: With 5 figures (l Show more

Cited by 6 publications

References 14 publications

The Galaxy Luminosity Functions down toM~ -10 in the Hydra I Cluster

The Galaxy Luminosity Functions down toM~ -10 in the Hydra I Cluster

NGC 3314a/b and NGC 3312: Ram pressure stripping in Hydra I cluster substructure

On the Structure of the Coma Cluster of Galaxies

Contact Info

Product

Resources

About