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Figure 1:
Map of the VIMOS observations in the Centaurus cluster. Dots are all photometrically selected compact object candidates from the VIMOS pre-images. Open circles mark the 386 compact objects with measured radial velocities (out of 405 for which slits had been allocated). Filled (green) circles indicate the 27 compact objects with radial velocities in the range of the Centaurus cluster (
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Figure 2: Example excerpts of two reduced spectra of Centaurus compact objects. The dashed ticks at the top mark the correspondingly red-shifted regions of the Mgb and Fe5270 Lick indices. Left: object CCOS J1248.54-4119.64, with a S/N around 45. Right: object CCOS J1248.74-4118.95, with a S/N around 18. |
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Figure 3:
Radial velocity histogram of all observed sources. The green dashed lines mark the limits applied for Centaurus cluster membership selection (40 Centaurus cluster members, including 13 dEs). The two vertical ticks mark the radial velocities of NGC 4696 (![]() ![]() |
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Figure 4: Colour-magnitude diagram in VR of the sources from Fig. 1, excluding the dwarf elliptical galaxies. |
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Figure 5:
Cumulative magnitude distribution of Centaurus compact objects. Dashed lines indicate the cumulative magnitude distribution of assumed Gaussian Globular Cluster Luminosity Functions with three different widths ![]() ![]() ![]() ![]() |
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Figure 6: Comparison of cumulative radial distributions of various object samples. Left panel: Centaurus compact objects are indicated by the (blue) solid histogram. The sample of 13 dwarf ellipticals is indicated by the (black) dotted histogram. For this plot, the radial distance was calculated with respect to NGC 4696 for the Cen30 members and with respect to NGC 4709 for the Cen45 members. The samples of compact objects and dEs have identical parent distributions at the 0.2% confidence level according to a KS-test. Right panel: the short dashed red line is the distribution of GC candidates around NGC 4696 from Mieske et al. (2005), see Fig. 1. The long dashed blue histogram is the distribution of compact objects restricted to the same field as the GC candidate sample. According to a KS test, both samples stem at 98% probability from the same parent distribution. |
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Figure 7:
Comparison between measured and literature Lick index values for the four Lick standard stars included in our observations. Index
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Figure 8:
Lick index
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Figure 9: Left panel: logarithm of the MgFe line index plotted vs. V for the Centaurus compact objects. The upper x-axis indicates an estimate of the corresponding [Fe/H], accurate to 0.2-0.3 dex, see text. Symbols surrounded by (red) circles indicate Cen45 members. The solid squares indicate spectra with S/N larger than 30. The green asterisk indicates the most extended object among the 8 sources with HST imaging (see text). Right panel: Log (MgFe) plotted vs. V for three samples of compact objects. Green filled circles indicate the Centaurus compact objects from the left panel. Blue open circles are the Virgo UCDs (Evstigneeva et al. 2007). Magenta open circles indicate Fornax compact objects (Mieske et al. 2006a). |
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Figure 10:
Radial velocity histogram of Centaurus compact objects (solid line). The (blue) curve indicates the expected velocity distribution if the Cen30 and Cen45 sample had mean velocities and velocity dispersion identical to the early-type galaxy population in both sub-clusters (Stein et al. 1997). The dotted tick at 4000 km s-1 indicates the adopted separation between Cen30 and Cen45. The two solid ticks indicate the radial velocities of NGC 4696 (2960 km s-1, NED) and NGC 4709 (4680 km s-1, NED). The dashed ticks indicate the ![]() ![]() |
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Figure 11:
Top: Two
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Figure 12:
HST based half light radius measurements of compact objects in various environments plotted vs. their absolute magnitude MV. Green filled circles indicate Centaurus compact objects (this paper). The dotted line indicates the
resolution limit of the Centaurus ACS images. This value
(
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