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Table 4

Differences between needed ionizing photon rates and those expected from nearby massive Cygnus OB2 stars.

Source #9 ΔNi #9 #22 ΔNi #22 #8 ΔNi #8 MT 516 ΔNi MT 516
(s−1) (s−1) (%) (s−1) (%) (s−1) (%) (s−1) (%)
(1) (2) (3) (4) (5) (6) (7) (8) (9) (10)
WDDGGHK2 7.32 × 1044 6.19 × 1044 −15 5.02 × 1044 −31 4.30 × 1044 −41 1.31 × 1044 −82
WDDGGHK3 7.19 × 1045 4.25 × 1045 −41 3.47 × 1045 −52 2.90 × 1045 −60 9.35 × 1044 −87
WDDGGHK4 2.02 × 1045 2.21 × 1045 9 1.81 × 1045 −10 1.49 × 1045 −26 4.88 × 1044 −76
WDDGGHK6 9.05 × 1045 8.35 × 1045 −8 7.93 × 1045 −12 4.48 × 1045 −50 2.85 × 1045 −68
WDDGGHK7 2.63 × 1045 4.16 × 1045 58 3.37 × 1045 28 2.69 × 1045 2 1.18 × 1045 −55
WDDGGHK8 2.02 × 1045 3.71 × 1045 84 3.07 × 1045 52 2.33 × 1045 15 1.16 × 1045 −42
WDDGGHK9 5.32 × 1043 9.43 × 1044 1671 7.66 × 1044 1338 6.26 × 1044 1075 2.54 × 1044 377
WDDGGHK10 1.31 × 1045 3.37 × 1045 157 2.44 × 1045 86 2.85 × 1045 118 5.39 × 1044 −59

Notes.The distances between the ionizing candidates and the WDDGGHK 3 group range 1300′′ –1900′′ (~ 13 pc); to WDDGGHK 6, distances range 600′′ –1200′′ (~ 7.5 pc); to the WDDGGHK 7 group, distances range 550′′ –900′′ (~ 6 pc); to WDDGGHK 10, distances range 1000′′ –1100′′ (~ 8.5 pc). (1) Name of thesource. (2) Rate of ionizing Lyman photons needed to produce the measured radio emission. (3), (5), (7) and (9) Rates of Lyman photons incident at each of the frEGGs (see text) and produced by Cygnus OB2 stars #9 (O5 I and O3.5 III), #22 (O5 I and O3.5 III), #8 (considering #8A and #8B, which comprises an O6 I plus an O5.5 III, and an O6.5 III), and the star RPL 841 (O5.5 V), respectively. The spectral type of the stars were adopted from Wright et al. (2015). The ionizing photon rates from the corresponding spectral type, using the models based on observational Teff scales by Martins et al. (2005). (4), (6), (8) and (10) Difference in % of the needed and the provided ionizing photon rates, . Negative percentages indicate a deficit of ionizing photons from the star, while positive percentages indicate the opposite, an excess of ionizing photons (or a larger than projected distance to the object).

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