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Table 3.

Flux densities for known sources from FULLCONCAT dataset.

Source Spectral type RA Dec FluxFULLCONCAT (mJy)
WR A WN7b+OB? 16 47 8.36412 −45 50 45.5948 0.89 ± 0.06
1.38 ± 0.09
WR D WN7o 16 47 6.29738 −45 51 26.6985 0.71 ± 0.05
WR B WN7o+OB? 16 47 5.34956 −45 51 5.3995 3.38 ± 0.03c
16.53 ± 0.15t
WR G WN7o 16 47 4.05743 −45 51 23.7000 0.34 ± 0.04
WR P WN7o 16 47 1.61624 −45 51 45.5984 0.05 ± 0.02m
WR I WN8o 16 47 0.89863 −45 51 20.6974 0.42 ± 0.02
WR L WN9h+OB? 16 47 4.20100 −45 51 7.5000 0.55 ± 0.04
WR S WN10−11h/BHG 16 47 2.96652 −45 50 19.7997 0.16 ± 0.04
WR E WC9 16 47 6.06807 −45 52 8.6988 0.13 ± 0.02
WR F WC9d+OB? 16 47 5.20647 −45 52 25.1996 0.29 ± 0.02
WR M WC9d 16 47 3.94256 −45 51 38.1000 0.24 ± 0.04

W16a A5Ia+ 16 47 6.69880 −45 50 41.0980 2.70 ± 0.11
W12a F1Ia+ 16 47 2.19106 −45 50 59.3991 1.76 ± 0.03c
3.77 ± 0.07t
W4a F3Ia+ 16 47 1.44479 −45 50 37.4982 3.18 ± 0.04c
4.72 ± 0.07t
W32 F5Ia+ 16 47 3.71289 −45 50 43.8000 0.18 ± 0.04
W265 F5Ia+ 16 47 6.29597 −45 49 24.2985 1.02 ± 0.04c
3.34 ± 0.11t
W237 M3Ia 16 47 3.10953 −45 52 19.1998 1.31 ± 0.02c
9.57 ± 0.19t
W75 M4Ia 16 47 8.93719 −45 49 58.7933 0.34 ± 0.03
W20 M5Ia 16 47 4.68920 −45 51 24.2999 2.54 ± 0.03c
20.65 ± 0.23t
W26 M5−6Ia 16 47 5.40679 −45 50 36.5994 153.11 ± 0.17

W17 O9Iab 16 47 6.18210 −45 50 49.4987 0.98 ± 0.04c
2.04±0.08t
W243 A2Ia (LBV) 16 47 7.50460 −45 52 29.3966 1.38 ± 0.04

W9 sgB[e] 16 47 4.14355 −45 50 31.5000 27.38 ± 0.06c
83.14 ± 0.41t
D09-R1 BSG 16 47 9.08253 −45 51 10.1929 1.29 ± 0.03c
5.44 ± 0.10t
D09-R2 BSG 16 47 6.89972 −45 50 37.1977 0.96 ± 0.06

W15 O9Ib 16 47 6.72735 −45 50 28.7980 1.65 ± 0.09
W10 B0.5I+OB 16 47 3.42580 −45 50 35.3999 0.16 ± 0.05
W18 B0.5Ia 16 47 5.60787 −45 50 50.3993 0.36 ± 0.06
W19 B1Ia 16 47 4.86139 −45 50 57.8998 0.08 ± 0.03
W1031 O9III 16 47 1.96137 −45 50 57.8988 0.90 ± 0.05
W1056 O9.5II 16 47 8.70904 −45 51 2.0939 0.09 ± 0.02

Notes. Flux densities are from the FULLCONCAT dataset, measured by SEAC (with flood threshold, σf = 3, and seed threshold, σs = 5), with consideration of segmentation where necessary. Flux densities are given in mJy. For extended sources, where possible, core flux densities are denoted by the superscript, c, and total flux densities are denoted by the superscript, t. A marginal flux detection is indicated with the superscript m. Spectral type identifications are taken from Crowther et al. (2006) for the WR stars, Clark et al. (2010) for the YHGs and RSGs, D10 for D09-R1 and D09-R2, and Clark et al. (2019b) for the OB stars.

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