Molecular genetics of Meckel syndrome : Ciliary genes are defective in MKS

Meckel syndrome (MKS, MIM 249000) is a severe developmental disorder that leads to death already in utero or shortly after birth. MKS diagnosis can be established by a careful ultrasound examination already at 11-14 weeks of gestation. The main features of MKS are occipital meningoencephalocele, cystic kidney dysplasia and fibrotic changes of the liver. In addition, polydactyly is frequently reported in the cases. The aim of the study was to characterize the molecular and functional defects in MKS. In this study we were able to identify two major MKS mutations in Finnish population, which cover over 90% of the cases. The first mutation is a 29 bp intronic deletion in the MKS1 gene (c.1483-7_35del) that is found in 70% of the families and the second is a C>T substitution in the coding region of CC2D2A (c.1762C>T), that is found in 20% of the MKS families. Both of these mutations result in abnormal splicing. The discovery of the disease genes has revealed that MKS is caused by primary cilia dysfunction. MKS1 gene has a conserved B9 domain, and it is found in the predicted ciliary proteome. CC2D2A protein is also found in the predicted ciliary proteome and it has a Ca2+ binding domain. The number of genes behind MKS has increased rapidly in the past years and to date, mutations have been identified in five genes (MKS1, TMEM67/MKS3, CEP290/MKS4, RPGRIP1L/MKS5 and CC2D2A/MKS6). Identification of the disease genes mutations has also revealed that MKS is an allelic disorder with other syndromes with overlapping phenotypes. Disorders that are caused by primary cilia dysfunction are collectively known as ciliopathies. Sequence analysis of all the known MKS genes in Finnish and non-Finnish families available to us, where the mutation was still unknown, revealed mutations in 14 out of the 30 families included in the study. When we collected all the reported mutations in MKS genes in different syndromes we could see that there was clearly a genotype-syndrome correlation between the mutations and the syndromes, since the same pair of mutations has never been reported in different syndromes. The basic molecular events behind MKS will not only give us information of this syndrome, but also significant novel information on early fetal development in general.

Molecular line and continuum studies of the early stages of star formation

New stars form in dense interstellar clouds of gas and dust called molecular clouds. The actual sites where the process of star formation takes place are the dense clumps and cores deeply embedded in molecular clouds. The details of the star formation process are complex and not completely understood. Thus, determining the physical and chemical properties of molecular cloud cores is necessary for a better understanding of how stars are formed. Some of the main features of the origin of low-mass stars, like the Sun, are already relatively well-known, though many details of the process are still under debate. The mechanism through which high-mass stars form, on the other hand, is poorly understood. Although it is likely that the formation of high-mass stars shares many properties similar to those of low-mass stars, the very first steps of the evolutionary sequence are unclear. Observational studies of star formation are carried out particularly at infrared, submillimetre, millimetre, and radio wavelengths. Much of our knowledge about the early stages of star formation in our Milky Way galaxy is obtained through molecular spectral line and dust continuum observations. The continuum emission of cold dust is one of the best tracers of the column density of molecular hydrogen, the main constituent of molecular clouds. Consequently, dust continuum observations provide a powerful tool to map large portions across molecular clouds, and to identify the dense star-forming sites within them. Molecular line observations, on the other hand, provide information on the gas kinematics and temperature. Together, these two observational tools provide an efficient way to study the dense interstellar gas and the associated dust that form new stars. The properties of highly obscured young stars can be further examined through radio continuum observations at centimetre wavelengths. For example, radio continuum emission carries useful information on conditions in the protostar+disk interaction region where protostellar jets are launched. In this PhD thesis, we study the physical and chemical properties of dense clumps and cores in both low- and high-mass star-forming regions. The sources are mainly studied in a statistical sense, but also in more detail. In this way, we are able to examine the general characteristics of the early stages of star formation, cloud properties on large scales (such as fragmentation), and some of the initial conditions of the collapse process that leads to the formation of a star. The studies presented in this thesis are mainly based on molecular line and dust continuum observations. These are combined with archival observations at infrared wavelengths in order to study the protostellar content of the cloud cores. In addition, centimetre radio continuum emission from young stellar objects (YSOs; i.e., protostars and pre-main sequence stars) is studied in this thesis to determine their evolutionary stages. The main results of this thesis are as follows: i) filamentary and sheet-like molecular cloud structures, such as infrared dark clouds (IRDCs), are likely to be caused by supersonic turbulence but their fragmentation at the scale of cores could be due to gravo-thermal instability; ii) the core evolution in the Orion B9 star-forming region appears to be dynamic and the role played by slow ambipolar diffusion in the formation and collapse of the cores may not be significant; iii) the study of the R CrA star-forming region suggests that the centimetre radio emission properties of a YSO are likely to change with its evolutionary stage; iv) the IRDC G304.74+01.32 contains candidate high-mass starless cores which may represent the very first steps of high-mass star and star cluster formation; v) SiO outflow signatures are seen in several high-mass star-forming regions which suggest that high-mass stars form in a similar way as their low-mass counterparts, i.e., via disk accretion. The results presented in this thesis provide constraints on the initial conditions and early stages of both low- and high-mass star formation. In particular, this thesis presents several observational results on the early stages of clustered star formation, which is the dominant mode of star formation in our Galaxy.