Volume 478, Number 2, February I 2008
|Page(s)||L23 - L26|
|Published online||04 December 2007|
Letter to the Editor
Departamento de Física, Casilla 160-C, Universidad de Concepción, Concepción, Chile e-mail: email@example.com
2 Argelander Institut für Astronomie, Auf dem Hügel 71, 53121 Bonn, Germany
3 European Southern Observatory, Karl-Schwarschildstr.2, Garching, Germany
4 Facultad de Ciencias Astronómicas y Geofísicas, Universidad Nacional de La Plata, Paseo del Bosque S/N, 1900-La Plata, Argentina; IALP-CONICET
5 UCO/Lick Observatory, University of Santa Cruz, California, 95064, USA
Accepted: 14 November 2007
Context.Central galaxies in galaxy clusters may be key discriminants in the competition between the cold dark matter (CDM) paradigm and modified Newtonian dynamics (MOND).
Aims.We investigate the dark halo of NGC 1399, the central galaxy of the Fornax cluster, out to a galactocentric distance of 80 kpc.
Methods.The data base consists of 656 radial velocities of globular clusters obtained with MXU/VLT and GMOS/Gemini, which is the largest sample so far for any galaxy. We performed a Jeans analysis for a non-rotating isotropic model.
Results.An NFW halo with the parameters and provides a good description of our data, fitting well to the X-ray mass. More massive halos are also permitted that agree with the mass of the Fornax cluster as derived from galaxy velocities. We compare this halo with the expected MOND models under isotropy and find that additional dark matter on the order of the stellar mass is needed to get agreement. A fully radial infinite globular cluster system would be needed to change this conclusion.
Conclusions.Regarding CDM, we cannot draw firm conclusions. To really constrain a cluster wide halo, more data covering a larger radius are necessary. The MOND result appears as a small-scale variant of the finding that MOND in galaxy clusters still needs dark matter.
Key words: galaxies: elliptical and lenticular, cD / galaxies: kinematics and dynamics / galaxies: individual: NGC 1399
Based on observations made with ESO Telescopes at the Paranal Observatories under program ID 70.B-0174.
Based on observations obtained at the Gemini Observatory, which is operated by the Association of Universities for Research in Astronomy, Inc., under a cooperative agreement with the NSF on behalf of the Gemini partnership: the National Science Foundation (United States), the Particle Physics and Astronomy Research Council (UK), the National Research Council (Canada), CONICYT (Chile), the 5Australian Research Council (Australia), CNPq (Brazil) and CONICET (Argentina).
© ESO, 2008
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