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tokens: components, respectively. The solid red curve is the sum of these two models. Fig. 8 Schematic representation of the spherically symmetric model for the molecular components of Arp 299A showing approximate spatial scales. Most of the molecular absorption is formed in the outer layers of the dense, most compact C component while the HO emission in the submillimeter seems to originate in the more optically thin C component. A tentative inflowing C component is included to account for the redshifted ground state OH doublet at m. Fig. 9 Reduced for the observed high-lying HO lines in our grid of models with . Fig. 10 for the OH at m with different values of applied to the best fit model of the inner component found using the HO lines. 3.3. Outer component Even in the best fit model for the inner component there is flux missing in the low-lying OH and and HO lines detected with PACS and, especially, the low-lying HO lines detected with SPIRE. To account for this missing flux in the models, a less excited and more extended component is required. To constrain the parameters of this outer component we have followed the same general procedure as for the inner component, but now for the low-lying lines normalized to the flux of the HO m line. In this process we have also taken the best fit model for the inner component into account. The observed line ratios are best reproduced with a dust opacity in the range . In this component collisional excitation becomes non-negligible for cm, but in these models the undetected HO m line goes into emission, favoring models with lower where collisional excitation is negligible. The reduced for our grid of models at the preferred dust opacity is presented in Fig. 11 . The line ratios are best reproduced with dust temperatures between and K, and HO columns between and cm. To also account for the absolute fluxes, the component should have a radius of pc. The best fit is achieved with , K, cm and pc. Fig. 11 Reduced for the observed low-lying HO lines in our grid of models with for the outer component, taking the contribution from the inner component into account. In Fig. 12 we present the reduced for the OH doublets in the outer component for different values of applied to the best fit model found for HO, now taking the OH contribution from the inner component into account. The OH m doublet which is redshifted by km s is not included here. The best fit is achieved with a column density of OH in the range to cm, corresponding to an OH/HO ratio in the range to . Applying a similar process to the upper limits of the OH doublets we get an upper limit to the OH column density of cm. Fig. 12 Reduced for the OH doublets, except for OH m , with different values of applied to the best fit model of the outer component found using the HO lines. 3.4. Extended component Most of the flux in both the HO and the OH lines is reproduced with the two components described in Sects. 3.2 and 3.3 . The ground state OH doublet at m is,