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The Next Generation Virgo Cluster Survey (NGVS). I. Introduction to the Survey

  • Authors: Laura Ferrarese, Patrick Côté, Jean-Charles Cuillandre, S. D. J. Gwyn, Eric W. Peng, Lauren A. MacArthur, Pierre-Alain Duc, A. Boselli, Simona Mei, Thomas Erben, Alan W. McConnachie, Patrick R. Durrell, J. Christopher Mihos, Andrés Jordán, Ariane Lançon, Thomas H. Puzia, Eric Emsellem, Michael L. Balogh, John P. Blakeslee, Ludovic van Waerbeke, Raphaël Gavazzi, Bernd Vollmer, J. J. Kavelaars, David Woods, Nicholas M. Ball, S. Boissier, Stéphane Courteau, E. Ferriere, G. Gavazzi, Hendrik Hildebrandt, P. Hudelot, M. Huertas-Company, Chengze Liu, Dean McLaughlin, Y. Mellier, Martha Milkeraitis, David Schade, Chantal Balkowski, Frédéric Bournaud, R. G. Carlberg, S. C. Chapman, Henk Hoekstra, Chien Peng, Marcin Sawicki, Luc Simard, James E. Taylor, R. Brent Tully, Wim van Driel, Christine D. Wilson, Todd Burdullis, Billy Mahoney, and Nadine Manset

Ferrarese et al. 2012 The Astrophysical Journal Supplement Series 200 4.

  • Provider: AAS Journals

Caption: Figure 16.

Middle and lower panels: scaling relations for early-type galaxies and globular clusters (GCs) in the Virgo cluster, Fornax cluster, and Local Group (see the text for details). For galaxies in Fornax and the Local Group, apparent B-band magnitudes and effective radii in arcseconds have been calculated as they would appear at the distance of the Virgo cluster. The dotted and dashed lines indicate the approximate selection limits for the Virgo survey of Binggeli et al. (1985) and the NGVS, respectively. The regions of parameter space where galaxies or star clusters in Virgo would be resolved are labeled, assuming an NGVS resolution limit of R e = 10 pc for compact sources (Section 5.1.4). The completeness function for the galaxy sample shown here is given in the top panel. The yellow star identifies the location of the galaxy shown in Figure 17.

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