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Table 1

X-ray-detected Wolf–Rayet stars in Wd1.

Name ID Other RA Dec Net counts Spectral type Info P P (this work)
names h m s ° ′ ″ days days
(1) (2) (3) (4) (5) (6) (7) (8) (9) (10)
A 3972 WR77sc, W72 16:47:08.35 −45:50:45.4 10295 ± 102 (l) WN7b earlyBIa 7.63(a) 81.75 ± 4.63
5412.8±74.3 (s) 7.70 ± 0.04
B 3299 WR77o 16:47:05.36 −15:51:04.8 3046.2±55.9 WN7o SB1 3.52(b) 3.514±0.009
2.222 ± 0.004
U 3577 WR77s, #1(c) 16:47:06.53 −45:50:39.1 1996.9±45.2 WN6o
L 3012 WR77k, W44 16:47:04.19 −45:51:07.2 1221.9±35.5 WN9h binary 53.95(d) 46.41±1.38
F 3252 WR77n, W239 16:47:05.20 −45:52:25.0 903.3±30.3 WC9d SB1 5.05(e) 2.263 ± 0.004
5.15 ± 0.02
O 3830 WR77sb 16:47:07.65 −45:52:36.0 387.7±20.0 WN6o
N 2015 WR77b 16:46:59.91 −45:55:25.6 375.2±20.0 WC9d SB2?, O? 58.61 ± 2.79
W 3815 WR77sa, #3(c) 16:47:07.61 −45:49:22.1 243.1±16.0 WN6h
J 2579 WR77e 16:47:02.47 −45:50:59.9 233.5±16.0 WN5h 5.15±0.02 (u)
R 3488 WR77q, W14c 16:47:06.09 −45:50:22.4 192.9±14.8 WN5o
X 4798 WR77sd,#2(c) 16:47:14.13 −45:48:32.0 154.2±13.0 WN5o 9.01 ± 0.05 (u)
G 2967 WR77j, W39b 16:47:04.00 −45:51:25.1 146.8±13.0 WN7o
P 2381 WR77d, W57c 16:47:01.59 −45:51:45.2 88.9±10.0 WN7o 5.19 ± 0.01
I 2198 WR77c 16:47:00.87 −45:51:20.6 86.6±10.0 WN8o
Q 1416 WR77a 16:46:55.54 −45:51:34.5 86.5±9.7 WN6o 7.4 ± 0.04 (u)
D 3523 WR77r 16:47:06.25 −45:51:26.4 69.3±9.5 WN7o
V 2918 WR77h 16:47:03.79 −45:50:38.7 66.8±9.0 WN8o
E 3445 WR77p, W241 16:47:05.96 −45:52:08.3 56.3±8.0 WC9 (f) RVbinary?
H 3019 WR77l 16:47:04.23 −45:51:20.2 26.3±7.3 WC9d
S 2708 WR77f, W5 16:47:02.98 −45:50:18.5 23.7±5.8 WN10-11h/B0.5Ia+

Notes. Column 1 reports the most common names for the WR stars in Wd1. Column 2 reports the EWOCS catalogue source identification number (Guarcello et al. 2024). Column 3 reports other WR names used in the literature. Columns 4 and 5 report the coordinates obtained from the X-ray source detection. Column 6 reports the net counts in the broad band (0.5–8.0 keV) and the corresponding errors adopted from Guarcello et al. (2024). For star A we also report the net counts corresponding to the large extraction region noted with (l). Column 7 presents the WR spectral type originally reported in Crowther et al. (2006a) unless otherwise indicated. Column 8 presents some information on source binarity and companion properties adopted by Crowther et al. (2006a), Clark et al. (2020), and Ritchie et al. (2022). Columns 9 and 10 report the measured periods from other and this work, respectively. For the cases where we detect two periods for the same source, both are reported in order of highest significance. The letter (u) signifies that the measured period is uncertain (a detailed description is provided in Sec. 3.3). (a)Bonanos (2007) (b)Koumpia & Bonanos (2012) (c)as reported in Groh et al. (2006)(d)Ritchie et al. (2022) (e)Clark et al. (2011) (f)Clark & Negueruela (2002).

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