The Arizona–New Mexico Spectroscopic Survey of Galaxies. II. Structures in the Perseus Supercluster

Gregory, S. A.; Tifft, W. G.; Moody, J. W.; Newberry, Michael V.; Hall, Shannon M.

doi:10.1086/301196

Cited by 3 publications

(2 citation statements)

References 15 publications

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“…The superclusters of galaxies, the largest systems in the Universe, are giant filamentary structures in the large-scale structure (e.g., such superclusters as Perseus (Gregory et al 2000) Pisces -Cetus (Porter and Raychaudhury 2005)) and are not virialized structures. The peculiar motions in the region of various superclusters were investigated by many authors (by Aaronson et al (1989) in the Hydra -Centaurus supercluster and by Han and Mould (1992), Baffa et al (1993), Hudson et al (1997), and Springob et al (2003) in the Perseus -Pisces supercluster).…”

Section: Introductionmentioning

confidence: 99%

Peculiar motions in the region of the Ursa Major supercluster of galaxies

Kopylova

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2007

Astron. Lett.

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Abstract. We have investigated the peculiar motions of clusters of galaxies in the Ursa Major (UMa) supercluster and its neighborhood. Based on SDSS (Sloan Digital Sky Survey) data, we have compiled a sample of early-type galaxies and used their fundamental plane to determine the cluster distances and peculiar velocities. The samples of early-type galaxies in the central regions (within R 200 ) of 12 UMa clusters of galaxies, in three main subsystems of the superclusterthe filamentary structures connecting the clusters, and in nine clusters from the nearest UMa neighborhood have similar parameters. The fairly high overdensity (3 by the galaxy number and 15 by the cluster number) suggests that the supercluster as a whole is gravitationally bound, while no significant peculiar motions have been found: the peculiar velocities do not exceed the measurement errors by more than a factor of 1.5-2. The mean random peculiar velocities of clusters and the systematic deviations from the overall Hubble expansion in the supercluster are consistent with theoretical estimates. For the possible approach of the three UMa subsystems to be confirmed, the measurement accuracy must be increased by a factor of 2-3.

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Section: Introductionmentioning

confidence: 99%

Peculiar motions in the region of the Ursa Major supercluster of galaxies

Kopylova

Копылов

2007

Astron. Lett.

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“…The diffuse feature locates at the bottom of the FAST map and may well reach beyond the map. In the large-scale environment, SQ is in a rather high-density region embedded within one of the main filaments of the Perseus supercluster (Gregory et al 2000). Tammann (1970) suggested that SQ is perhaps part of the Zwicky Cluster at 22 h 31 2+37°32′ (Zwicky & Kowal 1968).…”

Section: Origin Of the Diffuse H I Featurementioning

confidence: 99%

Deep H i Mapping of Stephan’s Quintet and Its Neighborhood

Cheng,

Xu,

Appleton

et al. 2023

ApJ

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We carried out deep mapping observations of the atomic hydrogen (H i) 21 cm line emission in a field centered on the famous galaxy group Stephan's Quintet (SQ), using the Five-hundred-meter Aperture Spherical Telescope (FAST) equipped with a 19-beam receiver. The final data cube reaches an H i column density sensitivity of 5σ = 2.1 × 1017 cm−2 per 20 km s−1 channel with an angular resolution of 4.′0. The discovery of a large diffuse feature of the H i emission in the outskirts of the intragroup medium of SQ was reported in a previous paper (Xu et al.). Here we present a new study of the total H i emission of SQ and the detection of several neighboring galaxies, exploiting the high sensitivity and the large sky coverage of the FAST observations. A total H i mass of M H I = 3.48 ± 0.35 × 1010 M ☉ is found for SQ, which is significantly higher than previous measurements in the literature. This indicates that, contrary to earlier claims, SQ is not H i deficient. The excessive H i gas is mainly found in the velocity ranges of 6200–6400 km s−1 and 6800–7000 km s−1, which were undetected in previous observations that are less sensitive than ours. Our results suggest that the “missing H i” in compact groups may be hidden in the low-density diffuse neutral gas instead of in the ionized gas.

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