Studies of nearby poor clusters: A3574 and S753

C. N.A. Willmer; P. Focardi; R. Chan; P. S. Pellegrini; L. Nicolaci Da Costa

doi:10.1086/115665

Studies of nearby poor clusters: A3574 and S753

C. N.A. Willmer, P. Focardi, R. Chan, P. S. Pellegrini, L. Nicolaci Da Costa

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Abstract

We present a study on two clusters belonging to the Centaurus concentration of galaxies, which are about 12 Mpc (H₀ = 100 km s^-1 Mpc^-1) away from the Centaurus cluster. Photographic photometry and radial velocities have been obtained for galaxies in two square fields centered on the brightest members of each cluster. We have derived dynamical parameters for both clusters, and found that they have masses of the order of 1.5×10¹⁴ Script M sign_⊙, ranking them among the most massive components of the concentration after the Centaurus cluster. No evidence of substructure has been detected in either cluster. These clusters are very near to each other, being separated by about 3.3 Mpc projected on the sky. However, the solution of a two-body linear orbit indicates they do not form a bound system, but the result is marginal.

Original language	English (US)
Pages (from-to)	57-65
Number of pages	9
Journal	Astronomical Journal
Volume	101
Issue number	1
DOIs	https://doi.org/10.1086/115665
State	Published - Jan 1991
Externally published	Yes

ASJC Scopus subject areas

Astronomy and Astrophysics
Space and Planetary Science

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title = "Studies of nearby poor clusters: A3574 and S753",

abstract = "We present a study on two clusters belonging to the Centaurus concentration of galaxies, which are about 12 Mpc (H0 = 100 km s-1 Mpc-1) away from the Centaurus cluster. Photographic photometry and radial velocities have been obtained for galaxies in two square fields centered on the brightest members of each cluster. We have derived dynamical parameters for both clusters, and found that they have masses of the order of 1.5×1014 Script M sign⊙, ranking them among the most massive components of the concentration after the Centaurus cluster. No evidence of substructure has been detected in either cluster. These clusters are very near to each other, being separated by about 3.3 Mpc projected on the sky. However, the solution of a two-body linear orbit indicates they do not form a bound system, but the result is marginal.",

author = "Willmer, {C. N.A.} and P. Focardi and R. Chan and Pellegrini, {P. S.} and {Da Costa}, {L. Nicolaci}",

year = "1991",

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doi = "10.1086/115665",

language = "English (US)",

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TY - JOUR

T1 - Studies of nearby poor clusters

T2 - A3574 and S753

AU - Willmer, C. N.A.

AU - Focardi, P.

AU - Chan, R.

AU - Pellegrini, P. S.

AU - Da Costa, L. Nicolaci

PY - 1991/1

Y1 - 1991/1

N2 - We present a study on two clusters belonging to the Centaurus concentration of galaxies, which are about 12 Mpc (H0 = 100 km s-1 Mpc-1) away from the Centaurus cluster. Photographic photometry and radial velocities have been obtained for galaxies in two square fields centered on the brightest members of each cluster. We have derived dynamical parameters for both clusters, and found that they have masses of the order of 1.5×1014 Script M sign⊙, ranking them among the most massive components of the concentration after the Centaurus cluster. No evidence of substructure has been detected in either cluster. These clusters are very near to each other, being separated by about 3.3 Mpc projected on the sky. However, the solution of a two-body linear orbit indicates they do not form a bound system, but the result is marginal.

AB - We present a study on two clusters belonging to the Centaurus concentration of galaxies, which are about 12 Mpc (H0 = 100 km s-1 Mpc-1) away from the Centaurus cluster. Photographic photometry and radial velocities have been obtained for galaxies in two square fields centered on the brightest members of each cluster. We have derived dynamical parameters for both clusters, and found that they have masses of the order of 1.5×1014 Script M sign⊙, ranking them among the most massive components of the concentration after the Centaurus cluster. No evidence of substructure has been detected in either cluster. These clusters are very near to each other, being separated by about 3.3 Mpc projected on the sky. However, the solution of a two-body linear orbit indicates they do not form a bound system, but the result is marginal.

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Studies of nearby poor clusters: A3574 and S753

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