(1) | (2) | (3) | (4) | (5) | (6) | (7) | (8) | (9) | (10) | (11) | (12) |
Cluster | log ![]() |
![]() |
d | ![]() |
![]() |
![]() |
Source | Background | Member | IDs. | Referencea |
(
![]() |
(
![]() |
(kpc) | |||||||||
NGC 6266 | 5.14 | 10.8 | 6.9 | -9.19 | 37.07 | 8.24 | 51 | 2-3 | 48-49 | 2c | 1, 2, 3 |
47 Tuc | 4.81 | 24.0 | 4.5 | -9.4 | 24.91 | 10.0 | 79 | ![]() |
![]() |
53-63 | 4 |
M 28 | 4.75 | 14.4 | 5.6 | -8.33 | 11.29 | 3.73 | 26 | 2-3 | 23-24 | 2c | 1, 5 |
M 4 | 4.01 | 49.8 | 1.73 | -6.9 | 1.0 | 1.0 | 6 | 1-3 | 3-5 | 5 | 1, 6 |
M 71 | 3.05 | 37.8 | 4.0 | -5.6 | 0.11 | 0.30 | 14 | 1-7 | 10 ![]() |
4-9 | 7 |
NGC 6366 | 2.42 | 109.8 | 3.6 | -5.77 | 0.08 | 0.33 | 5 | 2-5 | 1+2-1 | ![]() |
8 |
M 55 | 2.15 | 169.8 | 5.3 | -7.6 | 0.18 | 1.82 | 16 | 5-12 | 8+3-4 | 2-4 | 8 |
NGC 288b | 1.80 | 85.0 | 8.4 | -6.7 | 0.03 | 0.83 | 11 | 4-11 | 4+3-4 | 2-5 | 9 |
Notes. Columns 2-5 give the values
for central density (),
core-radius (
),
distance (d), and absolute visual magnitude (
)
come from Harris (1996, version of
February 2003). For M 4, the values of
and
are computed for the distance and reddening of Richer
et al. (1997). Columns 6 and 7 are
the collision number, which is computed from
and the half mass from
(Kong et al. 2006).
Values for
and
are normalized to the value of M 4. Column 8 shows
the total number of sources detected within the half-mass radius.
Column 9 is the number of expected fore/background sources.
Column 10 gives the number of expected cluster members plus
error. Column 11 shows the number of X-ray sources (with
erg s-1)
which have optical or/and radio counterparts associated with the
cluster, or spectrally confirmed qLMXBs. The last column gives the
reference paper. These globular clusters are ordered on the central
density.
(a) For each
cluster, the basic data for this table were extracted from: 1. Pooley et al. (2003);
2. Cocozza et al. (2008);
3. Trepl (2007); 4. Heinke et al. (2005);
5. Becker et al. (2003);
6. Bassa et al. (2004);
7. this work; 8. Bassa
et al. (2008); 9. Kong
et al. (2006). (b) NGC 288
was not observed long enough to reach this luminosity limit of
erg s-1 in the 0.5-6.0 keV
range. Its limiting luminosity is
erg s-1.
However, we keep this cluster's data, as a lower limit, since we have
so few constraints on low-density clusters. (c) No
information about the optical counterparts to X-ray sources.
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