Deep VLT spectroscopy of high redshift radio galaxy MRC 2104-242: Evidence for a metallicity gradient

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dc.creatorOverzier, R.
dc.creatorRottgering, H.
dc.creatorKurk, J.
dc.creatorDe Breuck, C.
dc.date2001-02-21
dc.date.accessioned2026-07-07T01:57:46Z
dc.date.available2026-07-07T01:57:46Z
dc.descriptionIn this contribution we will present deep VLT spectroscopy observations of the giant emission line halo around the z=2.49 radio galaxy MRC 2104-242. The morphology of the halo is dominated by two spatially resolved regions. Lya is extended by >12" along the radio axis, C IV and He II are extended by ~8". The overall spectrum is typical for that of high redshift radio galaxies. Interestingly, N V is present in the spectrum of the region associated with the center of the galaxy hosting the radio source, the northern region, while absent in the southern region. Using a simple photoionization model, the difference in N V can be explained due to a metallicity gradient within the halo. This is consistent with a scenario in which the halo is formed by a massive cooling flow or originates from the debris of the merging of two or more galaxies. However, also other mechanisms such as jet-cloud interactions or starburst-winds could be important.
dc.description5 pages, 8 figures, to be published in the proceedings of 'Emission Lines from Jet Flows' Nov 2001, Mexico, Eds. W. Henney, W. Steffen, L. Binette, A. Raga
dc.identifierhttps://arxiv.org/abs/astro-ph/0102364
dc.identifierhttp://arxiv.org/abs/astro-ph/0102364
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/2520
dc.subjectAstrophysics
dc.titleDeep VLT spectroscopy of high redshift radio galaxy MRC 2104-242: Evidence for a metallicity gradient
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