Distribution of gas, dust and the lambda 6613 angstrom DIB carrier in the Perseus OB2 association

We present a study of the spatial distribution of the lambda 6613 Angstrom DIB carrier in the Perseus OB2 association based on high resolution observa tions toward lines of sight representing different interstellar environment s. We determined that in the studied region, the lambda 6613 Angstrom DIB c arrier is concentrated in two distinct clouds with velocities of 1.4 (+/- 0 .4) and 12.0 (+/- 0.9) km s(-1). We compared the lambda 6613 Angstrom DIB c arrier's velocity with the Na I velocity distribution derived from our surv ey measurements, as well as with CO, OH, H I and Ca II measurements from th e literature. We conclude that the behaviour of the carrier of the lambda 6 613 Angstrom DIB follows the overall expansion motion of the gas in the ass ociation. The DIB velocity is directly linked to that of Ca II and H I. The DIB total column density is proportional to the total column density of Ca II and H I making those atoms good tracers of the lambda 6613 Angstrom DIB carrier Those new results support the assumption that the lambda 6613 Angs trom DIB would arise from a gas phase molecule, possibly single-ionized (So nnentrucker et al. 1997). We also conclude that the DIB carrier is distribu ted in shell structures over the whole association. We finally show from th e DIB velocity structure that the DIB carrier, gas and dust are well mixed toward the association but that the DIB shells have an angular extent twice larger than that of the dust.