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We show Akari data, Herschel data and data from the SCUBA2 camera on JCMT, of molecular clouds. We focus on pre-stellar cores within the clouds. We present Akari data of the L1147-1157 ring in Cepheus and show how the data indicate that the cores are being externally heated. We present SCUBA2 and Herschel data of the Ophiuchus region and show how the environment is also affecting core evolution in this region. We discuss the effects of the magnetic field in the Lupus I region, and how this lends support to a model for the formation and evolution of cores in filamentary molecular clouds.
High levels of deuterium fractionation of $rm N_2H^+$ (i.e., $rm D_{frac}^{N_2H^+} gtrsim 0.1$) are often observed in pre-stellar cores (PSCs) and detection of $rm N_2D^+$ is a promising method to identify elusive massive PSCs. However, the physical
Dust grains are the building {blocks} of future planets. They evolve in size, shape and composition during the life cycle of the interstellar medium. We seek to understand the process which leads from diffuse medium grains to dust grains in the vicin
Stars like our Sun and planets like our Earth form in dense regions within interstellar molecular clouds, called pre-stellar cores (PSCs). PSCs provide the initial conditions in the process of star and planet formation. In the past 15 years, detailed
High levels of deuterium fraction in N$_2$H$^+$ are observed in some pre-stellar cores. Single-zone chemical models find that the timescale required to reach observed values ($D_{rm frac}^{{rm N}_2{rm H}^+} equiv {rm N}_2{rm D}^+/{rm N}_2{rm H}^+ gtr
We present observations of L1155 and L1148 in the Cepheus molecular cloud, taken using the FIS instrument on the Akari satellite. We compare these data to submillimetre data taken using the SCUBA camera on the JCMT, and far-infrared data taken with t