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Table 1.

Radio sources and H II region information.

l, b coord. Ident. VHα VRadio ( * ) dadopted Radio cont. log(NLyc)
Flux density ( * *)
4.85–5 GHz
(Degrees) (km s −1) (km s −1) (kpc) (mJy) (s−1)
281.013−1.528 −5 −5(1); −9.7 ± 0.1(4) 3.2 8200(1) 48.93
281.162−1.640 −6 −7(1); −7.1 ± 0.2(4) 3.1 1986.7(3) 48.30
281.595−0.969 +2(1); −3.4 ± 0.1(4) 4.1 1000(1) 48.25
281.840−1.600 −8.2 ± 0.5(4) 2.76 210.2(4) 47.24
282.015−0.997 +1.4 ± 0.2(4) 4.5 1080.68(4) 48.38
282.025−1.178 RCW 46 −11 4.4
282.026−1.181 +19(1); +22.1 ± 0.1(4) 6.5 33 096.86(3) 50.18
282.240−1.099 −2(1) 4 (14 000)(1) 49.39
282.260−1.810 −15(1); −15 ± 2.5(4) 1.8 1628.93(3) 47.75
282.632−0.853 0(1); 0 ± 2.5(4) 4.6 1768.40(1) 48.62
282.709−2.477 RCW 47 −5 2.3 791.2(2) 47.66
282.808−1.338 BRAN 293 −6 −4.2 ± 0.3(4) 3.9 654.1(4) 48.03
283.131−0.984 −1(1); −1 ± 2.5(4) 4.4 4228.89(3) 48.93
283.146−0.604 BRAN 299; H2 −12 1.9
283.312−0.566 +6(1); −6 ± 2.5(4) 5.3 2121.79(3) 48.84
283.329−1.050 +16(1) 6.3 6400(1) 49.49
283.524−1.004 RCW48 −7.2 +3(1) 3.9 17 800(1) 49.49
283.832−0.730 +6.3 ± 0.3(4) 5.4 513.7(4) 48.21
283.978−0.920 +3(1); +3 ± 2.5(4) 5 8148.24(3) 49.34
284.014−0.857 +8.6 ± 0.1(4) 5.7 980.2(4) 48.54
284.114−1.505 BRAN 302 −6.4 2.3
284.308−0.334 RCW49 −5.4 0(1); 0 ± 2.5(4) 4.1 1.61 × 105(1) 50.47
284.260+0.400 +1(1) 4.9 8300(1) 49.37
284.373+0.402 RCW 50 −7 3.6
284.559−0.183 +7 +9(1) 5.7 7800(1) 49.50
284.650−0.484 −4.7 +5(1); +5 ± 2.5(4) 4.3 987.5(3) 48.30
284.723+0.313 +14.2 +10(1); +8.5 ± 0.1(4) 6.2 4106.95(3) 49.28
284.902+0.06 +3.4 ± 1.2(4) 5.4 128.13(4) 47.61
285.253−0.053 +3.8 −2(1); −0.1 ± 0.1(4) 4.7 16 207.84(4) 49.59
285.353+0.004 −4.5 ± 0.9(4) 4.8
285.860+0.074 GUM 30 −19 2.35 48.59 ( * * * )

Notes. ( * ) The typical uncertainty is 1 km s−1 for reference (1). ( * *) The typical beam size is 4.3′ for (1), 4.9′ for (3) and ∼2′ for (4) respectively. ( * * * ) Evaluated from the stellar content (stars earlier than B3) of the cluster NGC 3293 listed by Göppl & Preibisch (2022) and using Panagia (1973).

References. (1)Caswell & Haynes (1987), (2)Gregory et al. (1994), (3)Kuchar & Clark (1997), (4)Wenger et al. (2021).

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