Discovery of a hierarchical distribution of dark matter in the Fornax cluster of galaxies

Ikebe, Y.; Ezawa, H.; Fukazawa, Yasushi; Hirayama, M.; Ishisaki, Yoshitaka; Kikuchi, K.; Kubo, H.; Makishima, Kazuo; Matsushita, Kyoko; Ohashi, T.; Takahashi, Tadayuki; Tamura, Takayuki

doi:10.1038/379427a0

Cited by 108 publications

(152 citation statements)

References 18 publications

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“…At the radial limit of our sample (500 ), the PN dispersion reaches 220 km s −1 indicating that these PNe are not in the regime dominated by the cluster potential, but still within the NGC 1399 halo. Mass models based on ASCA and Rosat X-ray data (Ikebe et al 1996;Paolillo et al 2002) indicate that the transition to the cluster potential might be at around 500 . However, these mass models may not be consistent with the globular cluster kinematics (Schuberth et al 2009); this issue requires more work.…”

Section: Fornax Cluster Galaxiesmentioning

confidence: 99%

Counter-dispersed slitless-spectroscopy technique: planetary nebula velocities in the halo of NGC 1399

McNeil

Arnaboldi

Freeman³

et al. 2010

A&A

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Aims. Using a counter-dispersed slitless spectroscopy technique, we detect and measure the line-of-sight velocities of 187 planetary nebulae (PNe) around one of the nearest cD galaxies, NGC 1399, with FORS1 on the VLT. Methods. We describe the method for identifying and classifying the emission-line sources and the procedure for computing their J2000 coordinates and velocities. The number of PN detections and the errors in the velocity measurements (37 km s −1 ) indicate that this technique is comparable to other methods. Results. We present the spatial distribution of the PNe and a basic analysis of their velocities. The PN two-dimensional velocity field shows marginal rotation consistent with other studies. We also find a low-velocity substructure in the halo and a flatter velocity-dispersion profile compared to previous observations that extends to ∼400 . The detection of a low-velocity subcomponent underscores the importance of discrete velocity tracers for the detection of un-mixed components. Conclusions. The new velocity-dispersion profile is in good agreement with revised velocity dispersions for the red globular clusters in NGC 1399. The outer parts of this profile are consistent with one of the dynamical models, which corresponds to a circular velocity of 340 km s −1 and a rescaled B-band mass-to-light ratio of 20 at 7 radius. These measurements trace the kinematics of the outer halo and disentangle the heterogenous populations in the Fornax Cluster core. The new data set the stage for a revised dynamical model of the outer halo of NGC 1399.

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Section: Fornax Cluster Galaxiesmentioning

confidence: 99%

Counter-dispersed slitless-spectroscopy technique: planetary nebula velocities in the halo of NGC 1399

McNeil

Arnaboldi

Freeman³

et al. 2010

A&A

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“…Their results were recently confirmed by the analysis of the high quality data acquired with the European Photon Imaging Camera (EPIC) and Reflection Grating Spectrometer (RGS) onboard XMM-Newton (Takahashi et al 2009). The preference for the 2P scenario was also reported in the works on the Fornax cluster (Ikebe et al 1996;Matsushita et al 2007) and the NGC 5044 group (Buote & Fabian 1998;Buote et al 2003;Tamura et al 2003) with ASCA, Chandra, XMM-Newton, and Suzaku observations. However, due to the lack of such studies on more representative relaxed clusters or groups that exhibit strong CCCs, it is not yet clear whether or not the 2P scenario do surpass the 1P scenario in general, and if yes, to what extent the 2P model can be applied to constrain the origin of the CCC.…”

Section: Introductionmentioning

confidence: 85%

Two-phase ICM in the central region of the rich cluster of galaxies Abell 1795: A joint Chandra, XMM-Newton, and Suzaku view

Makishima

2012

AIP Conference Proceedings

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Based on a detailed analysis of the high-quality Chandra, XMM-Newton, and Suzaku data of the X-ray bright cluster of galaxies Abell 1795, we report clear evidence for a two-phase intracluster medium (ICM) structure, which consists of a cool (with a temperature T c ≈ 2.0 − 2.2 keV) and a hot (T h ≈ 5.0 − 5.7 keV) component that coexist and dominate the X-ray emission at least in the central 80 kpc. A third weak emission component (T 3 ≈ 0.8 keV) is also detected within the innermost 144 kpc and is ascribed to a portion of inter-stellar medium (ISM) of the cD galaxy. Deprojected spectral analysis reveals flat radial temperature distributions for both the hot phase and cool phase components. These results are consistent with the ASCA measurements reported in Xu et al. (1998), and resemble the previous findings for the Centaurus cluster (e.g., Takahashi et al. 2009). By analyzing the emission measure ratio and gas metal abundance maps created from the Chandra data, we find that the cool phase component is more metal-enriched than the hot phase one in 50 − 100 kpc region, which agrees with that found in M87 (Simionescu et al. 2008). The coexistence of the cool phase and hot phase ICM cannot be realized by bubble uplifting from active galactic nuclei (AGN) alone. Instead, the two-phase ICM properties are better reconciled with a cD corona model (Makishima et al. 2001). In this model, the -2 -cool phase may be ascribed to the plasmas confined in magnetic loops, which are surrounded by the intruding hot phase ICM and have been polluted by metals synthesized in the cD galaxy. AGN feedback energy released in the innermost 10 kpc can serve as the heating source to prevent the loop-interior gas from cooling down to temperatures much lower than the observed value. The total gravitating mass profile exhibits a hierarchical structure, regardless of the ICM temperature modeling.

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“…Machacek et al 2001) and in poor clusters they are limited to the central regions where gas is detected (e.g. Ikebe et al 1996). For an overview of the hydrostatic and dynamical techniques, see Tremaine (1992).…”

Section: Cluster Massesmentioning

confidence: 99%

The 2001 Australian Galaxy Cluster Workshop

Drinkwater

2002

Publ. – Astron. Soc. Aust

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The first ‘Australian Cluster Workshop’ was held at the Australia Telescope National Facility in Sydney on 2001 February 6. The aim of the workshop was to bring together the many and varied groups working on clusters of galaxies in Australia, to forge new multi-disciplinary links, and to generate enthusiasm and support for new cluster work and further cluster meetings in Australia. In this paper I present a summary of the workshop as well as some additional review material intended to place current Australian research in a broader perspective, looking ahead to the major issues still to be addressed.

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Discovery of a hierarchical distribution of dark matter in the Fornax cluster of galaxies

Cited by 108 publications

References 18 publications

Counter-dispersed slitless-spectroscopy technique: planetary nebula velocities in the halo of NGC 1399

Counter-dispersed slitless-spectroscopy technique: planetary nebula velocities in the halo of NGC 1399

Two-phase ICM in the central region of the rich cluster of galaxies Abell 1795: A joint Chandra, XMM-Newton, and Suzaku view

The 2001 Australian Galaxy Cluster Workshop

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