We report the discovery of a complex extended density enhancement in the Globular Clusters (GCs) in the central similar to 0.5(degrees)(2) (similar to 0.06 Mpc(2)) of the Fornax cluster, corresponding to similar to 50% of the area within 1 core radius. This overdensity connects the GC system of NGC 1399 to most of those of neighboring galaxies within similar to 0 degrees.6 (similar to 210 kpc) along the W-E direction. The asymmetric density structure suggests that the galaxies in the core of the Fornax cluster experienced a lively history of interactions that have left a clear imprint on the spatial distribution of GCs. The extended central dominant structure is more prominent in the distribution of blue GCs, while red GCs show density enhancements that are more centrally concentrated on the host galaxies. We propose that the relatively small-scale density structures in the red GCs are caused by galaxy-galaxy interactions, while the extensive spatial distribution of blue GCs is due to stripping of GCs from the halos of core massive galaxies by the Fornax gravitational potential. Our investigations are based on density maps of candidate GCs extracted from the multi-band VLT Survey Telescope (VST) survey of Fornax (FDS), identified in a three-dimensional color space and further selected based on their g-band magnitude and morphology.We report the discovery of a complex extended density enhancement in the Globular Clusters (GCs) in the central similar to 0.5(degrees)(2) (similar to 0.06 Mpc(2)) of the Fornax cluster, corresponding to similar to 50% of the area within 1 core radius. This overdensity connects the GC system of NGC 1399 to most of those of neighboring galaxies within similar to 0 degrees.6 (similar to 210 kpc) along the W-E direction. The asymmetric density structure suggests that the galaxies in the core of the Fornax cluster experienced a lively history of interactions that have left a clear imprint on the spatial distribution of GCs. The extended central dominant structure is more prominent in the distribution of blue GCs, while red GCs show density enhancements that are more centrally concentrated on the host galaxies. We propose that the relatively small-scale density structures in the red GCs are caused by galaxy-galaxy interactions, while the extensive spatial distribution of blue GCs is due to stripping of GCs from the halos of core massive galaxies by the Fornax gravitational potential. Our investigations are based on density maps of candidate GCs extracted from the multi-band VLT Survey Telescope (VST) survey of Fornax (FDS), identified in a three-dimensional color space and further selected based on their g-band magnitude and morphology.We report the discovery of a complex extended density enhancement in the Globular Clusters (GCs) in the central similar to 0.5(degrees)(2) (similar to 0.06 Mpc(2)) of the Fornax cluster, corresponding to similar to 50% of the area within 1 core radius. This overdensity connects the GC system of NGC 1399 to most of those of neighboring galaxies within similar to 0 degrees.6 (similar to 210 kpc) along the W-E direction. The asymmetric density structure suggests that the galaxies in the core of the Fornax cluster experienced a lively history of interactions that have left a clear imprint on the spatial distribution of GCs. The extended central dominant structure is more prominent in the distribution of blue GCs, while red GCs show density enhancements that are more centrally concentrated on the host galaxies. We propose that the relatively small-scale density structures in the red GCs are caused by galaxy-galaxy interactions, while the extensive spatial distribution of blue GCs is due to stripping of GCs from the halos of core massive galaxies by the Fornax gravitational potential. Our investigations are based on density maps of candidate GCs extracted from the multi-band VLT Survey Telescope (VST) survey of Fornax (FDS), identified in a three-dimensional color space and further selected based on their g-band magnitude and morphology.

The extended spatial distribution of globular clusters in the core of the fornax cluster

D'ABRUSCO, RAFFAELE;PAOLILLO, MAURIZIO;CAPACCIOLI, MASSIMO;LONGO, GIUSEPPE;
2016

Abstract

We report the discovery of a complex extended density enhancement in the Globular Clusters (GCs) in the central similar to 0.5(degrees)(2) (similar to 0.06 Mpc(2)) of the Fornax cluster, corresponding to similar to 50% of the area within 1 core radius. This overdensity connects the GC system of NGC 1399 to most of those of neighboring galaxies within similar to 0 degrees.6 (similar to 210 kpc) along the W-E direction. The asymmetric density structure suggests that the galaxies in the core of the Fornax cluster experienced a lively history of interactions that have left a clear imprint on the spatial distribution of GCs. The extended central dominant structure is more prominent in the distribution of blue GCs, while red GCs show density enhancements that are more centrally concentrated on the host galaxies. We propose that the relatively small-scale density structures in the red GCs are caused by galaxy-galaxy interactions, while the extensive spatial distribution of blue GCs is due to stripping of GCs from the halos of core massive galaxies by the Fornax gravitational potential. Our investigations are based on density maps of candidate GCs extracted from the multi-band VLT Survey Telescope (VST) survey of Fornax (FDS), identified in a three-dimensional color space and further selected based on their g-band magnitude and morphology.We report the discovery of a complex extended density enhancement in the Globular Clusters (GCs) in the central similar to 0.5(degrees)(2) (similar to 0.06 Mpc(2)) of the Fornax cluster, corresponding to similar to 50% of the area within 1 core radius. This overdensity connects the GC system of NGC 1399 to most of those of neighboring galaxies within similar to 0 degrees.6 (similar to 210 kpc) along the W-E direction. The asymmetric density structure suggests that the galaxies in the core of the Fornax cluster experienced a lively history of interactions that have left a clear imprint on the spatial distribution of GCs. The extended central dominant structure is more prominent in the distribution of blue GCs, while red GCs show density enhancements that are more centrally concentrated on the host galaxies. We propose that the relatively small-scale density structures in the red GCs are caused by galaxy-galaxy interactions, while the extensive spatial distribution of blue GCs is due to stripping of GCs from the halos of core massive galaxies by the Fornax gravitational potential. Our investigations are based on density maps of candidate GCs extracted from the multi-band VLT Survey Telescope (VST) survey of Fornax (FDS), identified in a three-dimensional color space and further selected based on their g-band magnitude and morphology.We report the discovery of a complex extended density enhancement in the Globular Clusters (GCs) in the central similar to 0.5(degrees)(2) (similar to 0.06 Mpc(2)) of the Fornax cluster, corresponding to similar to 50% of the area within 1 core radius. This overdensity connects the GC system of NGC 1399 to most of those of neighboring galaxies within similar to 0 degrees.6 (similar to 210 kpc) along the W-E direction. The asymmetric density structure suggests that the galaxies in the core of the Fornax cluster experienced a lively history of interactions that have left a clear imprint on the spatial distribution of GCs. The extended central dominant structure is more prominent in the distribution of blue GCs, while red GCs show density enhancements that are more centrally concentrated on the host galaxies. We propose that the relatively small-scale density structures in the red GCs are caused by galaxy-galaxy interactions, while the extensive spatial distribution of blue GCs is due to stripping of GCs from the halos of core massive galaxies by the Fornax gravitational potential. Our investigations are based on density maps of candidate GCs extracted from the multi-band VLT Survey Telescope (VST) survey of Fornax (FDS), identified in a three-dimensional color space and further selected based on their g-band magnitude and morphology.
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Utilizza questo identificativo per citare o creare un link a questo documento: https://hdl.handle.net/11588/636644
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