Radio observations of evaporating objects in the Cygnus OB2 region

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Table 4

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

Source		#9	ΔN_i #9	#22	ΔN_i #22	#8	ΔN_i #8	MT 516	ΔN_i 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 T_eff 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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