Table 4
Differences between needed ionizing photon rates and those expected from nearby massive Cygnus OB2 stars.
Source | ![]() |
![]() |
ΔNi #9 | ![]() |
ΔNi #22 | ![]() |
ΔNi #8 | ![]() |
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).
Current usage metrics show cumulative count of Article Views (full-text article views including HTML views, PDF and ePub downloads, according to the available data) and Abstracts Views on Vision4Press platform.
Data correspond to usage on the plateform after 2015. The current usage metrics is available 48-96 hours after online publication and is updated daily on week days.
Initial download of the metrics may take a while.