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We present the results of Herschel HOBYS photometric mapping combined withBIMA observations and additional archival data, and perform an in-depth studyof the evolutionary phases of the star-forming clumps in W 48A and theirsurroundings. Age estimates for the compact sources were derived frombolometric luminosities and envelope masses, which were obtained from the dustcontinuum emission, and agree within an order of magnitude with age estimatesfrom molecular line and radio data. The clumps in W 48A are linearly aligned byage (east-old to west-young): we find a ultra compact (UC) HII region, a youngstellar object (YSO) with class II methanol maser emission, a YSO with amassive outflow, and finally the NH_2D prestellar cores from Pillai et al. Thisremarkable positioning reflects the (star) formation history of the region. Wefind that it is unlikely that the star formation in the W 48A molecular cloudwas triggered by the UCHII region and discuss the Aquila supershell expansionas a mayor influence on the evolution of W 48A. We conclude that thecombination of Herschel continuum data with interferometric molecular line andradio continuum data is important to derive trustworthy age estimates andinterpret the origin of large scale structures through kinematic information.

A Herschel and BIMA study of the sequential star formation near the W48A HII region