Hostname: page-component-848d4c4894-8kt4b Total loading time: 0 Render date: 2024-07-01T04:09:57.612Z Has data issue: false hasContentIssue false
  • English
  • Français

Supermassive black holes in BCGs

Published online by Cambridge University Press:  01 August 2006

E. Dalla Bontà ,
L. Ferrarese ,
J. Miralda-Escudé ,
L. Coccato ,
E. M. Corsini  and
A. Pizzella
E. Dalla Bontà
Affiliation:
Dipartimento di Astronomia, Università di Padova, Padova, Italy Herzberg Institute of Astrophysics, Victoria, Canada
L. Ferrarese
Affiliation:
Herzberg Institute of Astrophysics, Victoria, Canada
J. Miralda-Escudé
Affiliation:
Institut de Ciencies de l'Espai (CSIC-IEEC)/ICREA, Barcelona, Spain
L. Coccato
Affiliation:
Kapteyn Astronomical Institute, University of Groningen, Groningen, The Netherlands
E. M. Corsini
Affiliation:
Dipartimento di Astronomia, Università di Padova, Padova, Italy
A. Pizzella
Affiliation:
Dipartimento di Astronomia, Università di Padova, Padova, Italy
Rights & Permissions [Opens in a new window]

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.

We observed a sample of three Brightest Cluster Galaxies (BCGs), Abell 1836-BCG, Abell 2052-BCG, and Abell 3565-BCG, with the Advanced Camera for Surveys (ACS) and the Imaging Spectrograph (STIS) on board the Space Telescope. For each target galaxy we obtained high-resolution spectroscopy of the Hα and [N II] λ6583 emission lines at three slit positions, to measure the central ionized-gas kinematics. ACS images in three different filters (F435W, F625W, and FR656N) have been used to determine the optical depth of the dust, stellar mass distribution near the nucleus, and intensity map. We present supermassive black hole (SBH) mass estimates for two galaxies which show regular rotation curves and strong central velocity gradients, and an upper limit on the SBH mass of the third one. For the SBHs of Abell 1836-BCG and Abell 3565-BCG, we derived M• = 4.8+0.8−0.7 × 109 M⊙ and M• = 1.3+0.3−0.4 × 109 M⊙ at 1 σ confidence level, respectively. For the SBH of Abell 2052-BCG, we found M• ≤ 7.3 × 109 M⊙.

Keywords

Black hole physics – galaxies: kinematics and dynamics – galaxies: structure
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 2 , Symposium S238: Black Holes from Stars to Galaxies – Across the Range of Masses , August 2006 , pp. 355 - 356
Copyright
Copyright © International Astronomical Union 2007

References

Coccato, L. et al. 2006, MNRAS, 366, 1050CrossRefGoogle Scholar
Ferrarese, L. & Ford, H. 2005, Sp. Sci. Rev., 116, 523CrossRefGoogle Scholar
Laine, S. et al. 2003, ApJ, 125, 478CrossRefGoogle Scholar
Marconi, A. & Hunt, L. K. 2003, ApJ, 589, L21CrossRefGoogle Scholar
Sarzi, M. et al. 2002, ApJ, 567, 237CrossRefGoogle Scholar
Smith, R. J. et al. 2000, MNRAS, 313, 469CrossRefGoogle Scholar