ROSAT Observations of Five Poor Galaxy Clusters with Extended Radio Sources

Doe, Stephen M.; Ledlow, Michael J.; Burns, Jack O.; White, R. A.

doi:10.1086/117496

Cited by 31 publications

(49 citation statements)

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“…This gives an average density of the intracluster medium in the group of ≤6 × 10 −4 cm −3 , assuming standard cooling functions (McKee & Cowie 1977;McCray 1987). This is lower than the densities inferred in many rich clusters and compact groups (e.g., Jones & Forman 1984;Pildis et al 1995), but consistent with those found in some poor clusters (Doe et al 1995), some of which contain 'head-tail' radio sources.…”

Section: Comparison With Other Radio Galaxiessupporting

confidence: 83%

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Interstellar Gas in the NGC 4410 Galaxy Group

Smith¹

2000

ApJ

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We present new radio continuum, 21 cm HI, and 2.6 mm CO data for the peculiar radio galaxy NGC 4410A and its companion NGC 4410B, and compare with available optical and X-ray maps. Our radio continuum maps show an asymmetric double-lobedstructure, with a high surface brightness lobe extending 3.6 arcmin (~100 kpc) to the southeast and a 6.2 arcmin (~180 kpc) low surface brightness feature in the northwest. Molecular gas is abundant in NGC 4410A, with M(H2) ~ 4 X 10^9 M(sun) (using the standard Galactic conversion factor), but is undetected in NGC 4410B. HI is less abundant, with M(HI) ~ 10^9 M(sun) for the pair. Our HI map shows a 3 X 10^8 M(sun) HI tail extending 1.7 arcmin (50 kpc) to the southeast of the pair, coincident with a faint optical tail and partially overlapping with the southeastern radio lobe. The HI tail is anti-coincident with a 2' (56 kpc) long X-ray structure aligned with a stellar bridge that connects the pair to a third galaxy. If this X-ray emission is associated with the group, there is 3 - 8 X 10^8 M(sun) of hot gas in this feature: either intracluster gas or shocked gas associated with the bridge. Our detection of abundant interstellar gas in this pair suggests that the distortions in this lobe map have been caused by the interstellar medium in this system. The interaction of the two galaxies and the subsequent motion of the interstellar medium in the system relative to the jet may have produced sufficient ram pressure to bend the radio jet. An alternative hypothesis is that the jet was distorted by ram pressure due to an intracluster medium, although the small radial velocity of NGC 4410A relative to the group and the lack of diffuse X-ray emission in the group makes this less likely unless the group is not virialized or is in the process of merging with another group.Comment: 12 pages, Latex, 8 figures (some multiple panels); figures 4a and 4b are color; Astrophysical Journal, in pres

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Section: Comparison With Other Radio Galaxiessupporting

confidence: 83%

“…If the group is dynamically young, the argument given in Section 4.2 against ram pressure bending by the intracluster medium does not hold (e.g., Venkatesan et al 1994;Doe et al 1995). It is possible that there is a large-scale motion of the group relative to an intracluster medium, perhaps due to the merging of two groups.…”

Section: A Group-group Merger?mentioning

confidence: 99%

Interstellar Gas in the NGC 4410 Galaxy Group

Smith¹

2000

ApJ

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“…However, Doe, Ledlow & Burns (1995) point out that the jet bulk kinetic energy is likely to dominate its non‐thermal internal pressure. We refer to their discussion and their results (summarized in their fig.…”

Section: The X‐ray and Radio Relationshipmentioning

confidence: 99%

X-ray analysis of the cluster 3C 129

Leahy¹,

Yin²

2000

Monthly Notices of the Royal Astronomical Society

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The cluster 3C 129 is classified as a rich cluster. An analysis of the properties of the cluster 3C 129 from ROSAT PSPC and HRI, Einstein IPC, and EXOSAT ME observations is presented. The mean temperature from a joint fit of the ROSAT PSPC and EXOSAT ME data is 5.5(±0.2) keV. The luminosity is 0.6×1044 erg s−1 in 0.2–2.4 keV and 2.7×1044 erg s−1 in 0.2–10 keV. We find a cooling flow with a rate of ∼84 M⊙ yr−1. The central gas density is 6×10−3 cm−3, and the ICM mass is 3.6×1013 M⊙. The total cluster mass is ∼5×1014 M⊙. The X‐ray morphology shows an east–west elongation, which is evidence for a recent merger event. The radio source 3C 129.1 is located near the X‐ray centre. Another cluster member galaxy (the radio galaxy 3C 129) is a prototype of head‐tailed radio galaxies, and is located in the west part of the cluster. The tail points along the gradient of intracluster gas pressure. There are no significant point X‐ray sources associated with the AGNs of the two radio galaxies.

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“…Numerical simulations tested the validity of these models (Balsara & Norman 1992), showing that both the JO and BRB models produce the observed NAT morphology and properties (Balsara, private communication). An intriguing characteristic of NAT radio sources is that they have also been observed in poor clusters of galaxies (Doe et al 1995). Such environments often have central ICM densities an order of magnitude lower than in rich clusters.…”

Section: Introductionmentioning

confidence: 99%

Cluster-subcluster mergers and the formation of narrow-angle tailed radio sources

Bliton¹,

Rizza²,

Burns³

et al. 1998

Monthly Notices of the Royal Astronomical Society

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firstpage-lastpage 1998 document firstpage abstract We have examined the ROSAT PSPC X-ray properties of a sample of 15 Abell clusters containing 23 narrow-angle tailed (NAT) radio galaxies. We find that clusters with NATs show a significantly higher level of substructure than a similar sample of radio-quiet clusters, indicating that NAT radio sources are preferentially located in dynamically complex systems. Also, the velocity distribution of the NAT galaxies is similar to that of other cluster members; these velocities are inadequate for producing the ram pressure necessary to bend the radio jets. We therefore propose a new model for NAT formation, in which NATs are associated with dynamically complex clusters undergoing merger events. The U-shaped NAT morphology is produced in part by the merger-induced bulk motion of the ICM bending the jets.

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ROSAT Observations of Five Poor Galaxy Clusters with Extended Radio Sources

Cited by 31 publications

References 0 publications

Interstellar Gas in the NGC 4410 Galaxy Group

Interstellar Gas in the NGC 4410 Galaxy Group

X-ray analysis of the cluster 3C 129

Cluster-subcluster mergers and the formation of narrow-angle tailed radio sources

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