Hostname: page-component-745bb68f8f-v2bm5 Total loading time: 0 Render date: 2025-02-06T22:34:50.608Z Has data issue: false hasContentIssue false
  • English
  • Français

Elliptical Galaxies: Darkly Cloaked or Scantily Clad?

Published online by Cambridge University Press:  26 May 2016

A. J. Romanowsky ,
N. G. Douglas ,
K. Kuijken ,
M. R. Merrifield ,
M. Arnaboldi ,
N. R. Napolitano ,
H. Merrett ,
M. Capaccioli ,
K. C. Freeman  and
O. Gerhard
A. J. Romanowsky
Affiliation:
School of Physics and Astronomy, University of Nottingham
N. G. Douglas
Affiliation:
Kapteyn Institute, Groningen
K. Kuijken
Affiliation:
Kapteyn Institute, Groningen Leiden Observatory
M. R. Merrifield
Affiliation:
School of Physics and Astronomy, University of Nottingham
M. Arnaboldi
Affiliation:
INAF-Osservatorio Astronomico di Pino Torinese, Turin
N. R. Napolitano
Affiliation:
Kapteyn Institute, Groningen
H. Merrett
Affiliation:
School of Physics and Astronomy, University of Nottingham
M. Capaccioli
Affiliation:
INAF-Osservatorio Astronomico di Capodimonte, Naples
K. C. Freeman
Affiliation:
RSAA, Mt. Stromlo and Siding Spring Observatories
O. Gerhard
Affiliation:
Astronomisches Institut, Universität Basel

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

Planetary nebulae (PNe) may be the most promising tracers in the halos of early-type galaxies. We have used multi-object spectrographs on the WHT and the VLT, and the new Planetary Nebula Spectrograph on the WHT, to obtain hundreds of PN velocities in a small sample of nearby galaxies. These ellipticals show weak halo rotation, which may be consistent with ab initio models of galaxy formation, but not with more detailed major merger simulations. the galaxies near L* show evidence of a universal declining velocity dispersion profile, and dynamical models indicate the presence of little dark matter within 5 Reff—implying halos either not as massive or not as centrally concentrated as CDM predicts.

Type
Part 5: Clusters and Ellipticals
Information
Symposium - International Astronomical Union , Volume 220: Dark Matter in Galaxies , 2004 , pp. 165 - 170
Copyright
Copyright © Astronomical Society of the Pacific 2004 

References

Baes, M., & Dejonghe, H. 2001, ApJ, 563, L19.Google Scholar
Bahcall, N. A., Lubin, L. M., & Dorman, V. 1995, ApJ, 447, L81.Google Scholar
Beasley, M. A., et al. 2004, in preparation.Google Scholar
Bendo, G. J., & Barnes, J. E. 2000, MNRAS, 316, 315.CrossRefGoogle Scholar
Bergond, G., et al., in preparation.Google Scholar
Bertin, G., et al. 1994, A&A, 292, 381.Google Scholar
Borriello, A., Salucci, P., & Danese, L. 2003, MNRAS, 341, 1109.Google Scholar
Ciardullo, R., et al. 1998, ApJ, 492, 62.CrossRefGoogle Scholar
Côté, P., et al. 2001, ApJ, 559, 828.Google Scholar
Côté, P., et al. 2003, ApJ, 591, 850.CrossRefGoogle Scholar
Douglas, N. G., et al. 2002, PASP, 114, 1234.CrossRefGoogle Scholar
Eke, V., Efstathiou, G., & Wright, L. 2000, MNRAS, 315, L18.CrossRefGoogle Scholar
Fall, S. M. 1983, in Internal Kinematics and Dynamics of Galaxies, ed. Athanassoula, E. (Dordrecht: Reidel), 391.CrossRefGoogle Scholar
Gerhard, O., Kronawitter, A., Saglia, R. P., & Bender, R. 2001, AJ, 121, 1936.Google Scholar
Lambas, D. G., Maddox, S. J., & Loveday, J. 1992, MNRAS, 258, 404.Google Scholar
Loewenstein, M., & White, R. E. III. 1999, ApJ, 518, 50.CrossRefGoogle Scholar
Matsushita, K., et al. 2002, A&A, 386, 77.Google Scholar
Méndez, R. H., et al. 2001, ApJ, 563, 135.Google Scholar
Natarajan, P., Kneib, J.-P., & Smail, I. 2002, ApJ, 580, L11.Google Scholar
Navarro, J. F., Frenk, C. S., & White, S. D. M. 1995, MNRAS, 275, 56.Google Scholar
O'Sullivan, E., Ponman, T. J., & Collins, R. S. 2003, MNRAS, 340, 1375.Google Scholar
Peng, E. W., Ford, H. C., & Freeman, K. C. 2002, in Extragalactic Star Clusters, ed. Geisler, D., Grebel, E. K., & Minniti, D.. (San Francisco: ASP), 312.Google Scholar
Prada, F., et al. 2003, ApJ, in press (astro-ph/0301360).Google Scholar
Romanowsky, A. J., & Kochanek, C. S. 2001, ApJ, 553, 722.Google Scholar
Romanowsky, A. J., et al. 2003, Science, 301, 1696.Google Scholar
Rusin, D., Kochanek, C. S., & Keeton, C. R. 2003, ApJ, 595, 29.CrossRefGoogle Scholar
Seljak, U. 2002, MNRAS, 334, 797.Google Scholar
Schindler, S., Binggeli, B., & Böhringer, H. 1999, A&A, 343, 420.Google Scholar
Schneider, S. E., et al., 1989, AJ, 97, 666.Google Scholar
Weil, M. L., & Hernquist, L. 1996, ApJ, 460, 101.Google Scholar
Weinberg, D. H., et al. 2004, ApJ, in press (astro-ph/0212356).Google Scholar
Wilson, G., Kaiser, N., Luppino, G. A., & Cowie, L. L. 2001, ApJ, 555, 572.CrossRefGoogle Scholar
Wright, , et al., 2004, MNRAS, submitted (astro-ph/0310513).Google Scholar